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12473133 | 1607.01526 | Globular clusters as tracers of the host galaxy mass distribution: the Fornax dSph test case | The Fornax dwarf spheroidal galaxy is the most massive satellites of the Milky Way, claimed to be embedded in a huge dark matter halo, and the only among the Milky Way satellites hosting five globular clusters. Interestingly, their estimated masses, ages and positions seem hardly compatible with the presence of a significant dark matter component, as expected in the ΛCDM scheme. Indeed, if Fornax would have a CDM halo with a standard density profile, all its globular clusters should have sunk to the galactic centre many Gyr ago due to dynamical friction. Due to this, some authors proposed that the most massive clusters may have formed out of Fornax and later tidally captured. In this paper, we investigate the past evolution of the Fornax GC system by using both a recently developed, semi-analytical treatment of dynamical friction and direct N-body simulations of the orbital evolution of the globular clusters within Fornax and of Fornax galaxy around the Milky Way. Our results suggest that an `in situ' origin for all the clusters is likely if their observed positions are close to their spatial ones and their orbits are almost circular. Moreover, the Milky Way seems to accelerate the GC decay reducing the decay time of 15 per cent. Nevertheless, our results indicate that the GCs survival probability exceeds 50 per cent, even in the case of cuspy density profiles. We conclude that more detailed data are required to shed light on the Fornax dark matter content, to distinguish between a cuspy or a cored profile. | [
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-0.... | 9.992026 | 7.407736 | 2016-07-01 | 17 | 2016MNRAS.461.4335A | [
"cuspy density profiles",
"dynamical friction",
"Fornax GC",
"Fornax",
"the Fornax dark matter content",
"five globular clusters",
"the globular clusters",
"direct N-body simulations",
"the Fornax GC system",
"a huge dark matter halo",
"a standard density profile",
"the Milky Way satellites",
... | [
"methods: numerical",
"galaxies: individual: Fornax",
"galaxies: nuclei",
"galaxies: star clusters: general",
"Astrophysics - Astrophysics of Galaxies"
] | 1 | [
"10.1093/mnras/stw1647",
"10.48550/arXiv.1607.01526"
] | [
"Arca-Sedda, M.",
"Capuzzo-Dolcetta, R."
] | [
"Department of Physics, Sapienza, University of Rome, Piazzale Aldo Moro 5, I-00185 Rome, Italy",
"Department of Physics, Sapienza, University of Rome, Piazzale Aldo Moro 5, I-00185 Rome, Italy"
] | [
"2017MNRAS.464.3060A",
"2017MNRAS.471..478A",
"2018A&A...615A..91B",
"2018MNRAS.477..480Z",
"2018MNRAS.477.4423A",
"2018MNRAS.479..900A",
"2018MNRAS.480..927P",
"2019ApJ...877..133D",
"2019MNRAS.485.2546B",
"2019MNRAS.488.2977O",
"2020MNRAS.493..320L",
"2020arXiv200906133A",
"2021MNRAS.503..... | [
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5209849 | 1607.03009 | Impacts of fragmented accretion streams onto classical T Tauri stars: UV and X-ray emission lines | Context. The accretion process in classical T Tauri stars (CTTSs) can be studied through the analysis of some UV and X-ray emission lines which trace hot gas flows and act as diagnostics of the post-shock downfalling plasma. In the UV-band, where higher spectral resolution is available, these lines are characterized by rather complex profiles whose origin is still not clear. <BR /> Aims: We investigate the origin of UV and X-ray emission at impact regions of density structured (fragmented) accretion streams. We study if and how the stream fragmentation and the resulting structure of the post-shock region determine the observed profiles of UV and X-ray emission lines. <BR /> Methods: We modeled the impact of an accretion stream consisting of a series of dense blobs onto the chromosphere of a CTTS through two-dimensional (2D) magnetohydrodynamic (MHD) simulations. We explored different levels of stream fragmentation and accretion rates. From the model results, we synthesize C IV (1550 Å) and O VIII (18.97 Å) line profiles. <BR /> Results: The impacts of accreting blobs onto the stellar chromosphere produce reverse shocks propagating through the blobs and shocked upflows. These upflows, in turn, hit and shock the subsequent downfalling fragments. As a result, several plasma components differing for the downfalling velocity, density, and temperature are present altoghether. The profiles of C IV doublet are characterized by two main components: one narrow and redshifted to speed ≈ 50 km s<SUP>-1</SUP> and the other broader and consisting of subcomponents with redshift to speed in the range 200-400 km s<SUP>-1</SUP>. The profiles of O VIII lines appear more symmetric than C IV and are redshifted to speed ≈ 150 km s<SUP>-1</SUP>. <BR /> Conclusions: Our model predicts profiles of C IV line remarkably similar to those observed and explains their origin in a natural way as due to stream fragmentation. <P />Movies are available at <A href="http://www.aanda.org/10.1051/0004-6361/201628858/olm">http://www.aanda.org</A> | [
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-0.0... | 9.33351 | 12.213435 | 2016-07-01 | 15 | 2016A&A...594A..93C | [
"line profiles",
"C IV line",
"stream fragmentation",
"O VIII lines",
"accretion rates",
"UV and X-ray emission lines",
"dense blobs",
"the post-shock downfalling plasma",
"C IV doublet",
"C IV",
"fragmentation",
"speed",
"shocked upflows",
"impact regions",
"several plasma components",
... | [
"accretion",
"accretion disks",
"magnetohydrodynamics (MHD)",
"stars: pre-main sequence",
"shock waves",
"X-rays: stars",
"ultraviolet: stars",
"Astrophysics - Solar and Stellar Astrophysics"
] | 3 | [
"10.1051/0004-6361/201628858",
"10.48550/arXiv.1607.03009"
] | [
"Colombo, S.",
"Orlando, S.",
"Peres, G.",
"Argiroffi, C.",
"Reale, F."
] | [
"INAF-Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134, Palermo, Italy",
"INAF-Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134, Palermo, Italy",
"INAF-Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134, Palermo, Italy; Dipartimento di Fisica & Chimica,... | [
"2017A&A...598L...8P",
"2017A&A...602A..10G",
"2017A&A...607A..14A",
"2017SciA....3E0982R",
"2018MNRAS.475.4367D",
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"2019ASPC..519...21I",
"2019ASSP...55...29D",
"2019ASSP...55...43O",
"2019arXiv190409156D",
"2020A&A...640A.... | [
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12586989 | 1607.06240 | Hybrid entropy stable HLL-type Riemann solvers for hyperbolic conservation laws | It is known that HLL-type schemes are more dissipative than schemes based on characteristic decompositions. However, HLL-type methods offer greater flexibility to large systems of hyperbolic conservation laws because the eigenstructure of the flux Jacobian is not needed. We demonstrate in the present work that several HLL-type Riemann solvers are provably entropy stable. Further, we provide convex combinations of standard dissipation terms to create hybrid HLL-type methods that have less dissipation while retaining entropy stability. The decrease in dissipation is demonstrated for the ideal MHD equations with a numerical example. | [
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... | 8.773089 | 4.468664 | 2016-07-01 | 7 | 2017JCoPh.330..566S | [
"hyperbolic conservation laws",
"entropy stability",
"characteristic decompositions",
"standard dissipation terms",
"less dissipation",
"large systems",
"Jacobian",
"HLL",
"greater flexibility",
"dissipation",
"several HLL-type Riemann solvers",
"hybrid HLL-type methods",
"HLL-type schemes",... | [
"Entropy stability",
"Ideal magnetohydrodynamics",
"HLL",
"Riemann solver",
"Discrete entropy inequality",
"Mathematics - Numerical Analysis",
"Astrophysics - Instrumentation and Methods for Astrophysics"
] | 1 | [
"10.1016/j.jcp.2016.10.034",
"10.48550/arXiv.1607.06240"
] | [
"Schmidtmann, Birte",
"Winters, Andrew R."
] | [
"MathCCES, RWTH Aachen University, Schinkelstr. 2, 52062 Aachen, Germany",
"Mathematisches Institut, Universität zu Köln, Weyertal 86-90, 50931 Köln, Germany"
] | [
"2019JCoPh.378..477S",
"2019ShWav..29..755P",
"2020JCoPh.41609545T",
"2021ApJS..257...24L",
"2021ApJS..257...34F",
"2022JCoPh.46811521W",
"2023JCoPh.49312505H"
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168897 | 1607.07246 | Dynamics of Saturn’s great storm of 2010-2011 from Cassini ISS and RPWS | Saturn’s quasi-periodic planet-encircling storms are the largest convecting cumulus outbursts in the Solar System. The last eruption was in 1990 (Sánchez-Lavega, A. [1994]. Chaos 4, 341-353). A new eruption started in December 2010 and presented the first-ever opportunity to observe such episodic storms from a spacecraft in orbit around Saturn (Fischer, G. et al. [2011]. Nature 475, 75-77; Sánchez-Lavega, A. et al. [2011]. Nature 475, 71-74; Fletcher, L.N. et al. [2011]. Science 332, 1413). Here, we analyze images acquired with the Cassini Imaging Science Subsystem (ISS), which captured the storm’s birth, evolution, and demise. In studying the end of the convective activity, we also analyze the Saturn Electrostatic Discharge (SED) signals detected by the Radio and Plasma Wave Science (RPWS) instrument. The storm’s initial position coincided with that of a previously known feature called the String of Pearls (SoPs) at 33°N planetocentric latitude. Intense cumulus convection at the westernmost point of the storm formed a particularly bright “head” that drifted at -26.9 ± 0.8 m s<SUP>-1</SUP> (negative denotes westward motion). On January 11, 2011, the size of the head was 9200 km and up to 34,000 km in the north-south and east-west dimensions, respectively. RPWS measurements show that the longitudinal extent of the lightning source expanded with the storm’s growth. The storm spawned the largest tropospheric vortex ever seen on Saturn. On January 11, 2011, the anticyclone was sized 11,000 km by 12,000 km in the north-south and east-west directions, respectively. Between January and September 2011, the vortex drifted at an average speed of -8.4 m s<SUP>-1</SUP>. We detect anticyclonic circulation in the new vortex. The vortex’s size gradually decreased after its formation, and its central latitude shifted to the north. The storm’s head moved westward and encountered the new anticyclone from the east in June 2011. After the head-vortex collision, the RPWS instrument detected that the SED activities became intermittent and declined over ∼40 days until the signals became undetectable in early August. In late August, the SED radio signals resurged for 9 days. The storm left a vast dark area between 32°N and 38°N latitudes, surrounded by a highly disturbed region that resembles the mid-latitudes of Jupiter. Using ISS images, we also made cloud-tracking wind measurements that reveal differences in the cloud-level zonal wind profiles before and after the storm. | [
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-0.... | 8.500903 | 15.534467 | 2016-07-01 | 74 | 2013Icar..223..460S | [
"such episodic storms",
"early August",
"G. et al",
"∼40 days",
"L.N. et al",
"A. et al",
"late August",
"Plasma Wave Science",
"SED",
"Jupiter",
"Saturn",
"the SED radio signals",
"motion",
"demise",
"latitudes",
"Saturn’s quasi-periodic planet-encircling storms",
"RPWS",
"-",
"... | [
"Astrophysics - Earth and Planetary Astrophysics"
] | 18 | [
"10.1016/j.icarus.2012.12.013",
"10.48550/arXiv.1607.07246"
] | [
"Sayanagi, Kunio M.",
"Dyudina, Ulyana A.",
"Ewald, Shawn P.",
"Fischer, Georg",
"Ingersoll, Andrew P.",
"Kurth, William S.",
"Muro, Gabriel D.",
"Porco, Carolyn C.",
"West, Robert A."
] | [
"Department of Atmospheric and Planetary Sciences, Hampton University, Hampton, VA 23668, USA; Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA",
"Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA",
... | [
"2013Icar..226..641L",
"2013Icar..226.1020D",
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"2014Icar..241..313D",
"2014Icar..242..122T",
"2014MNRAS.444.1369H",
"2014Natur.505..625S",
"2015A&A...580A.... | [
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"1992Icar..100..... |
12408831 | 1607.07888 | Observed Variability at 1 and 4 μm in the Y0 Brown Dwarf WISEP J173835.52+273258.9 | We have monitored photometrically the Y0 brown dwarf WISEP J173835.52+273258.9 (W1738) at both near- and mid-infrared wavelengths. This ≲1 Gyr old 400 K dwarf is at a distance of 8 pc and has a mass around 5 M <SUB>Jupiter</SUB>. We observed W1738 using two near-infrared filters at λ ≈ 1 μm, Y and J, on Gemini Observatory and two mid-infrared filters at λ ≈ 4 μm, [3.6] and [4.5], on the Spitzer observatory. Twenty-four hours were spent on the source by Spitzer on each of 2013 June 30 and October 30 UT. Between these observations, around 5 hr were spent on the source by Gemini on each of 2013 July 17 and August 23 UT. The mid-infrared light curves show significant evolution between the two observations separated by 4 months. We find that a double sinusoid can be fit to the [4.5] data, where one sinusoid has a period of 6.0 ± 0.1 hr and the other a period of 3.0 ± 0.1 hr. The near-infrared observations suggest variability with a ∼3.0 hr period, although only at a ≲2σ confidence level. We interpret our results as showing that the Y dwarf has a 6.0 ± 0.1 hr rotation period, with one or more large-scale surface features being the source of variability. The peak-to-peak amplitude of the light curve at [4.5] is 3%. The amplitude of the near-infrared variability, if real, may be as high as 5%-30%. Intriguingly, this size of variability and the wavelength dependence can be reproduced by atmospheric models that include patchy KCl and Na<SUB>2</SUB>S clouds and associated small changes in surface temperature. The small number of large features, as well as the timescale for evolution of the features, is very similar to what is seen in the atmospheres of the solar system gas giants. | [
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... | 7.153717 | 12.541796 | 2016-07-01 | 31 | 2016ApJ...830..141L | [
"large features",
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"surface temperature",
"-infrared wavelengths",
"significant evolution",
"patchy KCl",
"atmospheric models",
"Jupiter</SUB",
"variability",
"evolution",
"The mid-infrared light curves",
"the solar system gas giants",
"a ∼3.0 hr period",
"Gemini... | [
"brown dwarfs",
"stars: atmospheres",
"stars: individual: WISEP J173835.52+273258.9",
"Astrophysics - Solar and Stellar Astrophysics"
] | 10 | [
"10.3847/0004-637X/830/2/141",
"10.48550/arXiv.1607.07888"
] | [
"Leggett, S. K.",
"Cushing, Michael C.",
"Hardegree-Ullman, Kevin K.",
"Trucks, Jesica L.",
"Marley, M. S.",
"Morley, Caroline V.",
"Saumon, D.",
"Carey, S. J.",
"Fortney, J. J.",
"Gelino, C. R.",
"Gizis, J. E.",
"Kirkpatrick, J. D.",
"Mace, G. N."
] | [
"Gemini Observatory, Northern Operations Center, 670 N. A'ohoku Place, Hilo, HI 96720, USA",
"The University of Toledo, 2801 West Bancroft Street, Mailstop 111, Toledo, OH 43606, USA",
"The University of Toledo, 2801 West Bancroft Street, Mailstop 111, Toledo, OH 43606, USA",
"The University of Toledo, 2801 W... | [
"2016ApJ...832...58E",
"2017ApJ...842...78V",
"2017ApJ...842..118L",
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12518466 | 1607.08820 | Dispersion by pulsars, magnetars, fast radio bursts and massive electromagnetism at very low radio frequencies | Our understanding of the universe relies mostly on electromagnetism. As photons are the messengers, fundamental physics is concerned in testing their properties. Photon mass upper limits have been earlier set through pulsar observations, but new investigations are offered by the excess of dispersion measure (DM), sometimes observed with pulsar and magnetar data at low frequencies, or with the fast radio bursts (FRBs), of yet unknown origin. Arguments for the excess of DM do not reach a consensus, but are not mutually exclusive. Thus, we remind that for massive electromagnetism, dispersion goes as the inverse of the frequency squared. Thereby, new avenues are offered also by the recently operating ground observatories in 10-80 MHz domain and by the proposed Orbiting Low Frequency Antennas for Radio astronomy (OLFAR). The latter acts as a large aperture dish by employing a swarm of nano-satellites observing the sky for the first time in the 0.1-15 MHz spectrum. The swarm must be deployed sufficiently away from the ionosphere to avoid distorsions from terrestrial interference, especially during solar maxima, and offer stable conditions for calibration during observations. | [
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0.0... | 6.522832 | 3.614386 | 2016-07-01 | 28 | 2017AdSpR..59..736B | [
"unknown origin",
"pulsar observations",
"Radio astronomy",
"OLFAR",
"observations",
"low frequencies",
"new investigations",
"dispersion measure",
"stable conditions",
"the proposed Orbiting Low Frequency Antennas",
"solar maxima",
"new avenues",
"dispersion",
"terrestrial interference",
... | [
"Photons",
"Radio astronomy",
"Satellites",
"Pulsars",
"Magnetars",
"Fast radio bursts",
"Astrophysics - Instrumentation and Methods for Astrophysics",
"Astrophysics - High Energy Astrophysical Phenomena",
"General Relativity and Quantum Cosmology",
"High Energy Physics - Phenomenology"
] | 6 | [
"10.1016/j.asr.2016.10.018",
"10.48550/arXiv.1607.08820"
] | [
"Bentum, Mark J.",
"Bonetti, Luca",
"Spallicci, Alessandro D. A. M."
] | [
"Universiteit van Twente, Faculteit van Elektrotechniek, Wiskunde en Informatica, Telecommunication Engineering Postbus 217, 7500 AE Enschede, The Netherlands; ASTRON, Postbus 2, 7900 AA Dwingeloo, The Netherlands",
"Université d'Orléans, Observatoire des Sciences de l'Univers en région Centre, 1A rue de la Férol... | [
"2017ApJ...842...23Y",
"2017CQGra..34u5006S",
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"2019EPJC...79..590H",
"2019PhRvD..99l4001C",
"2019arXiv191206288S",
"2020RAA....20..... | [
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12406228 | 1607.06710 | Setting the volatile composition of (exo)planet-building material. Does chemical evolution in disk midplanes matter? | Context. The atmospheres of extrasolar planets are thought to be built largely through accretion of pebbles and planetesimals. Such pebbles are also the building blocks of comets. The chemical composition of their volatiles are usually taken to be inherited from the ices in the collapsing cloud. However, chemistry in the protoplanetary disk midplane can modify the composition of ices and gases. <BR /> Aims: To investigate if and how chemical evolution affects the abundances and distributions of key volatile species in the midplane of a protoplanetary disk in the 0.2-30 AU range. <BR /> Methods: A disk model used in planet population synthesis models is adopted, providing temperature, density and ionisation rate at different radial distances in the disk midplane. A full chemical network including gas-phase, gas-grain interactions and grain-surface chemistry is used to evolve chemistry in time, for 1 Myr. Both molecular (inheritance from the parent cloud) and atomic (chemical reset) initial conditions are investigated. <BR /> Results: Great diversity is observed in the relative abundance ratios of the main considered species: H<SUB>2</SUB>O, CO, CO<SUB>2</SUB>, CH<SUB>4</SUB>, O<SUB>2</SUB>, NH<SUB>3</SUB> and N<SUB>2</SUB>. The choice of ionisation level, the choice of initial abundances, as well as the extent of chemical reaction types included are all factors that affect the chemical evolution. The only exception is the inheritance scenario with a low ionisation level, which results in negligible changes compared with the initial abundances, regardless of whether or not grain-surface chemistry is included. The grain temperature plays an important role, especially in the critical 20-28 K region where atomic H no longer sticks long enough to the surface to react, but atomic O does. Above 28 K, efficient grain-surface production of CO<SUB>2</SUB> ice is seen, as well as O<SUB>2</SUB> gas and ice under certain conditions, at the expense of H<SUB>2</SUB>O and CO. H<SUB>2</SUB>O ice is produced on grain surfaces only below 28 K. For high ionisation levels at intermediate disk radii, CH<SUB>4</SUB> gas is destroyed and converted into CO and CO<SUB>2</SUB> (in contrast with previous models), and similarly NH<SUB>3</SUB> gas is converted into N<SUB>2</SUB>. At large radii around 30 AU, CH<SUB>4</SUB> ice is enhanced leading to a low gaseous CO abundance. As a result, the overall C/O ratios for gas and ice change significantly with radius and with model assumptions. For high ionisation levels, chemical processing becomes significant after a few times 10<SUP>5</SUP> yr. <BR /> Conclusions: Chemistry in the disk midplane needs to be considered in the determination of the volatile composition of planetesimals. In the inner <30 AU disk, interstellar ice abundances are preserved only if the ionisation level is low, or if these species are included in larger bodies within 10<SUP>5</SUP> yr. | [
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0.00... | 10.068603 | 13.044076 | 2016-07-01 | 146 | 2016A&A...595A..83E | [
"SUB>2</SUB",
"interstellar ice abundances",
"grain surfaces",
"CO",
"initial abundances",
"ices",
"atomic H",
"intermediate disk radii",
"ionisation level",
"high ionisation levels",
"CO<SUB>2</SUB>",
"gases",
"key volatile species",
"CO. H<SUB>2</SUB>O ice",
"chemical evolution",
"pr... | [
"astrochemistry",
"planets and satellites: formation",
"protoplanetary disks",
"planets and satellites: atmospheres",
"molecular processes",
"Astrophysics - Earth and Planetary Astrophysics"
] | 12 | [
"10.1051/0004-6361/201628509",
"10.48550/arXiv.1607.06710"
] | [
"Eistrup, Christian",
"Walsh, Catherine",
"van Dishoeck, Ewine F."
] | [
"Leiden Observatory, Leiden University, PO Box 9513, 2300 RA, Leiden, The Netherlands",
"Leiden Observatory, Leiden University, PO Box 9513, 2300 RA, Leiden, The Netherlands ; School of Physics and Astronomy, University of Leeds, Leeds, LS2 9JT, UK",
"Leiden Observatory, Leiden University, PO Box 9513, 2300 RA,... | [
"2017A&A...599A.101V",
"2017A&A...599A.113M",
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2774767 | 1607.08619 | The Data Reduction Pipeline for the SDSS-IV MaNGA IFU Galaxy Survey | Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) is an optical fiber-bundle integral-field unit (IFU) spectroscopic survey that is one of three core programs in the fourth-generation Sloan Digital Sky Survey (SDSS-IV). With a spectral coverage of 3622-10354 Å and an average footprint of ∼500 arcsec<SUP>2</SUP> per IFU the scientific data products derived from MaNGA will permit exploration of the internal structure of a statistically large sample of 10,000 low-redshift galaxies in unprecedented detail. Comprising 174 individually pluggable science and calibration IFUs with a near-constant data stream, MaNGA is expected to obtain ∼100 million raw-frame spectra and ∼10 million reduced galaxy spectra over the six-year lifetime of the survey. In this contribution, we describe the MaNGA Data Reduction Pipeline algorithms and centralized metadata framework that produce sky-subtracted spectrophotometrically calibrated spectra and rectified three-dimensional data cubes that combine individual dithered observations. For the 1390 galaxy data cubes released in Summer 2016 as part of SDSS-IV Data Release 13, we demonstrate that the MaNGA data have nearly Poisson-limited sky subtraction shortward of ∼8500 Å and reach a typical 10σ limiting continuum surface brightness μ = 23.5 AB arcsec<SUP>-2</SUP> in a five-arcsecond-diameter aperture in the g-band. The wavelength calibration of the MaNGA data is accurate to 5 km s<SUP>-1</SUP> rms, with a median spatial resolution of 2.54 arcsec FWHM (1.8 kpc at the median redshift of 0.037) and a median spectral resolution of σ = 72 km s<SUP>-1</SUP>. | [
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"individual dithered observations",
"SDSS-IV Data Release",
"centralized metadata framework",
"unprecedented detail",
"the MaNGA Data Reduction Pipeline algorithms",
"∼8500 Å",
"SDSS-IV Data",
"the MaNGA Data Reduction Pipeline",
"Mapping Nearby Galaxies",
... | [
"methods: data analysis",
"surveys",
"techniques: imaging spectroscopy",
"Astrophysics - Instrumentation and Methods for Astrophysics"
] | 32 | [
"10.3847/0004-6256/152/4/83",
"10.48550/arXiv.1607.08619"
] | [
"Law, David R.",
"Cherinka, Brian",
"Yan, Renbin",
"Andrews, Brett H.",
"Bershady, Matthew A.",
"Bizyaev, Dmitry",
"Blanc, Guillermo A.",
"Blanton, Michael R.",
"Bolton, Adam S.",
"Brownstein, Joel R.",
"Bundy, Kevin",
"Chen, Yanmei",
"Drory, Niv",
"D'Souza, Richard",
"Fu, Hai",
"Jones... | [
"Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA",
"Center for Astrophysical Sciences, Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA",
"Department of Physics and Astronomy, University of Kentucky, 505 Rose Street, Lexington, KY 40506-0... | [
"2016AJ....152..197Y",
"2016MNRAS.463.2513B",
"2017AJ....154...28B",
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"2017ApJ...838...77L",
"2017ApJ...839...87B",
"2017ApJ...844...80B",
"2017ApJ...850..136S",
"2017ApJ...851...18L",
"2017ApJ...851L..33G",
"2017ApJS..233...25A",
"2017MNRAS.464L..46S",
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12585901 | 1607.08157 | Dark matter directional detection: comparison of the track direction determination | Several directional techniques have been proposed for a directional detection of Dark matter, among others anisotropic crystal detectors, nuclear emulsion plates, and low-pressure gaseous TPCs. The key point is to get access to the initial direction of the nucleus recoiling due to the elastic scattering by a WIMP. In this article, we aim at estimating, for each method, how the information of the recoil track initial direction is preserved in different detector materials. We use the SRIM simulation code to emulate the motion of the first recoiling nucleus in each material. We propose the use of a new observable, D, to quantify the preservation of the initial direction of the recoiling nucleus in the detector. We show that in an emulsion mix and an anisotropic crystal, the initial direction is lost very early, while in a typical TPC gas mix, the direction is well preserved. | [
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"initial direction",
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"the recoiling nucleus",
"Dark matter",
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"Several directional techn... | [
"Astrophysics - Instrumentation and Methods for Astrophysics",
"Physics - Instrumentation and Detectors"
] | 3 | [
"10.1088/1475-7516/2017/01/027",
"10.48550/arXiv.1607.08157"
] | [
"Couturier, C.",
"Zopounidis, J. P.",
"Sauzet, N.",
"Naraghi, F.",
"Santos, D."
] | [
"LPSC, CNRS/IN2P3, UJF, INP, Avenue des Martyrs, 38000, Grenoble, France",
"LPSC, CNRS/IN2P3, UJF, INP, Avenue des Martyrs, 38000, Grenoble, France",
"LPSC, CNRS/IN2P3, UJF, INP, Avenue des Martyrs, 38000, Grenoble, France",
"LPSC, CNRS/IN2P3, UJF, INP, Avenue des Martyrs, 38000, Grenoble, France",
"LPSC, C... | [
"2016arXiv160708765C",
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12509827 | 1607.01847 | Oscillating chiral tensor spectrum from axionic inflation | We study axionic inflation with a modulated potential and examine if the primordial tensor power spectrum exhibits oscillatory feature, which is testable with future space-based gravitational-wave experiments such as DECIGO and BBO. In the case of single-field axion monodromy inflation, it turns out that it is difficult to detect an oscillation in the spectrum due to the suppression of the sub-Planckian decay constant of the axion. On the other hand, in the case of aligned chromo-natural inflation where the axion is coupled to a SU(2) gauge field, it turns out that a sizable oscillation in the tensor spectrum can occur due to the enhancement of chiral gravitational waves sourced by the gauge field. We expect that this feature will be a new probe for axion phenomenologies in the early Universe through chiral gravitational waves. | [
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-0.03988135978579521... | 10.62901 | -1.476708 | 2016-07-01 | 42 | 2016PhRvD..94d4062O | [
"chiral gravitational waves",
"axion phenomenologies",
"BBO",
"single-field axion monodromy inflation",
"oscillatory feature",
"axionic inflation",
"DECIGO",
"future space-based gravitational-wave experiments",
"the sub-Planckian decay constant",
"the gauge field",
"the tensor spectrum",
"Plan... | [
"Astrophysics - Cosmology and Nongalactic Astrophysics",
"General Relativity and Quantum Cosmology",
"High Energy Physics - Phenomenology",
"High Energy Physics - Theory"
] | 6 | [
"10.1103/PhysRevD.94.044062",
"10.48550/arXiv.1607.01847"
] | [
"Obata, Ippei",
"Soda, Jiro"
] | [
"Department of Physics, Kyoto University, Kyoto 606-8502, Japan",
"Department of Physics, Kobe University, Kobe 657-8501, Japan"
] | [
"2016JCAP...12..031G",
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"2018JCAP...07..023F",
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2775537 | 1607.07699 | A High-velocity Cloud Impact Forming a Supershell in the Milky Way | Neutral atomic hydrogen (H I) gas in interstellar space is largely organized into filaments, loops, and shells, the most prominent of which are “supershells.” These gigantic structures, which require ≳ 3× {10}<SUP>52</SUP> erg to form, are generally thought to be produced by either the explosion of multiple supernovae (SNe) in OB associations or, alternatively, by the impact of high-velocity clouds (HVCs) falling into the Galactic disk. Here, we report the detection of a kiloparsec (kpc)-size supershell in the outskirts of the Milky Way with the compact HVC 040 + 01-282 (hereafter, CHVC040) at its geometrical center using the “Inner-Galaxy Arecibo L-band Feed Array” H I 21 cm survey data. The morphological and physical properties of both objects suggest that CHVC040, which is either a fragment of a nearby disrupted galaxy or a cloud that originated from an intergalactic accreting flow, collided with the disk ∼5 Myr ago to form the supershell. Our results show that some compact HVCs can survive their trip through the Galactic halo and inject energy and momentum into the Milky Way disk. | [
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-0.002... | 11.281891 | 9.068976 | 2016-07-01 | 10 | 2016ApJ...827L..27P | [
"supershells",
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"the Galactic disk",
"interstellar space",
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"high-velocity clouds",
"shells",
"loops",
"filaments",
"the disk",
"SNe",
"the Milky Way",
"an interga... | [
"Galaxy: disk",
"ISM: clouds",
"radio lines: ISM",
"Astrophysics - Astrophysics of Galaxies"
] | 7 | [
"10.3847/2041-8205/827/2/L27",
"10.48550/arXiv.1607.07699"
] | [
"Park, Geumsook",
"Koo, Bon-Chul",
"Kang, Ji-hyun",
"Gibson, Steven J.",
"Peek, J. E. G.",
"Douglas, Kevin A.",
"Korpela, Eric J.",
"Heiles, Carl E."
] | [
"Department of Physics and Astronomy, Seoul National University Seoul 151-747, Korea",
"Department of Physics and Astronomy, Seoul National University Seoul 151-747, Korea",
"Korea Astronomy and Space Science Institute Daejeon 305-348, Korea",
"Department of Physics and Astronomy, Western Kentucky University ... | [
"2017AIPC.1792d0007M",
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"2020AJ....160...66P",
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4552757 | 1607.02243 | Diffuse gas in retired galaxies: nebular emission templates and constraints on the sources of ionization | We present emission-line templates for passively-evolving (`retired') galaxies, useful for investigation of the evolution of the interstellar medium in these galaxies, and characterization of their high-temperature source populations. The templates are based on high signal-to-noise (>800) co-added spectra (3700-6800 Å) of ∼11 500 gas-rich Sloan Digital Sky Survey galaxies devoid of star formation and active galactic nuclei. Stacked spectra are provided for the entire sample and sub-samples binned by mean stellar age. In our previous paper, Johansson et al., these spectra provided the first measurements of the He II 4686 Å line in passively-evolving galaxies, and the observed He II/Hβ ratio constrained the contribution of accreting white dwarfs (the `single-degenerate' scenario) to the Type Ia supernova rate. In this paper, the full range of unambiguously detected emission lines are presented. Comparison of the observed [O I] 6300 Å/Hα ratio with photoionization models further constrains any high-temperature single-degenerate scenario for Type Ia supernovae (with 1.5 ≲ T/10<SUP>5</SUP> K ≲ 10) to ≲3-6 per cent of the observed rate in the youngest age bin (I.e. highest SN Ia rate). Hence, for the same temperatures, in the presence of an ambient population of post-asymptotic giant branch stars, we exclude additional high-temperature sources with a combined ionizing luminosity of ≈1.35 × 10<SUP>30</SUP> L<SUB>⊙</SUB>/M<SUB>⊙,*</SUB> for stellar populations with mean ages of 1-4 Gyr. Furthermore, we investigate the extinction affecting both the stellar and nebular continuum. The latter shows about five times higher values. This contradicts isotropically distributed dust and gas that renders similar extinction values for both cases. | [
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... | 12.531031 | 7.864967 | 2016-07-01 | 28 | 2016MNRAS.461.4505J | [
"stellar age",
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"stellar populations",
"active galactic nuclei",
"the Type Ia supernova rate",
"additional high-temperature sources",
"star formation",
"the youngest age bin",
"(I.e. highest SN Ia rate",
"SN",
"similar extinction v... | [
"galaxies: elliptical and lenticular",
"cD",
"galaxies: ISM",
"Astrophysics - Astrophysics of Galaxies"
] | 5 | [
"10.1093/mnras/stw1668",
"10.48550/arXiv.1607.02243"
] | [
"Johansson, Jonas",
"Woods, Tyrone E.",
"Gilfanov, Marat",
"Sarzi, Marc",
"Chen, Yan-Mei",
"Oh, Kyuseok"
] | [
"Max-Planck Institut für Astrophysik, Karl-Schwarzschild-Str. 1, D-85741 Garching, Germany; Department of Biological and Environmental Sciences, University of Gothenburg, Medicinaregatan 18, SE-40530 Gothenburg, Sweden",
"Max-Planck Institut für Astrophysik, Karl-Schwarzschild-Str. 1, D-85741 Garching, Germany; M... | [
"2017ApJ...835...70Z",
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"2017NatAs...1..800W",
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12410206 | 1607.02596 | Large-scale fluctuations in the number density of galaxies in independent surveys of deep fields | New arguments supporting the reality of large-scale fluctuations in the density of the visible matter in deep galaxy surveys are presented. A statistical analysis of the radial distributions of galaxies in the COSMOS and HDF-N deep fields is presented. Independent spectral and photometric surveys exist for each field, carried out in different wavelength ranges and using different observing methods. Catalogs of photometric redshifts in the optical (COSMOS-Zphot) and infrared (UltraVISTA) were used for the COSMOS field in the redshift interval 0.1 < z < 3.5, as well as the zCOSMOS (10kZ) spectroscopic survey and the XMM-COSMOS and ALHAMBRA-F4 photometric redshift surveys. The HDFN-Zphot and ALHAMBRA-F5 catalogs of photometric redshifts were used for the HDF-N field. The Pearson correlation coefficient for the fluctuations in the numbers of galaxies obtained for independent surveys of the same deep field reaches R = 0.70 ± 0.16. The presence of this positive correlation supports the reality of fluctuations in the density of visible matter with sizes of up to 1000 Mpc and amplitudes of up to 20% at redshifts z ~ 2. The absence of correlations between the fluctuations in different fields (the correlation coefficient between COSMOS and HDF-N is R = -0.20 ± 0.31) testifies to the independence of structures visible in different directions on the celestial sphere. This also indicates an absence of any influence from universal systematic errors (such as "spectral voids"), which could imitate the detection of correlated structures. | [
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0.... | 11.799792 | 3.5501 | 2016-07-01 | 8 | 2016ARep...60..563S | [
"different fields",
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"different observing methods",
"different wavelength ranges",
"R = -0.20 ±",
"photometric redshifts",
"correlated structures",
"visible matter",
"independent surveys",
"HDF-N",
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"structures",
"R =",
"redshifts",
... | [
"Astrophysics - Cosmology and Nongalactic Astrophysics",
"85A40",
"85A35"
] | 3 | [
"10.1134/S1063772916040107",
"10.48550/arXiv.1607.02596"
] | [
"Shirokov, S. I.",
"Lovyagin, N. Yu.",
"Baryshev, Yu. V.",
"Gorokhov, V. L."
] | [
"Saint-Petersburg State University, St. Petersburg, Russia",
"Saint-Petersburg State University, St. Petersburg, Russia",
"Saint-Petersburg State University, St. Petersburg, Russia",
"Saint-Petersburg State University of Architecture and Civil Engineering, St. Petersburg, Russia"
] | [
"2017Ap.....60..484S",
"2020AstBu..75..207S",
"2020MNRAS.496.1530S",
"2020Univ....6..212B",
"2020Univ....6..215N",
"2021A&A...651A.114D",
"2021Univ....7..289R",
"2022Galax..10..108L"
] | [
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"2007Natur.445..286M",
"2008A&A...477..381S",
"2009A&A...505..463M",
"2009ApJ...690.1... |
12593510 | 1607.00841 | H I absorption towards low-luminosity radio-loud active galactic nuclei of different accretion modes and WISE colours | H I absorption studies of active galaxies enable us to probe their circumnuclear regions and the general interstellar medium and study the supply of gas that may trigger nuclear activity. In this article, we investigate the dependence of the detection rate of H I absorption on the nature of radio galaxies based on their emission-line spectra and on the nature of host galaxies based on WISE colours and their radio structure, which may help us understand the different accretion modes. We find significant differences in the distributions of W2-W3 colour for sources with H I absorption detections and non-detections. We report a high detection rate of H I absorption in those galaxies with WISE infrared colours W2-W3 > 2, typical of gas-rich systems, along with a compact radio structure. The H I detection rate for low-excitation radio galaxies (LERGs) with W2-W3 > 2 and compact radio structure is high (70.6 ± 20.4 per cent). In high-excitation radio galaxies (HERGs), compact radio structure in the nuclear or circumnuclear region could give rise to absorption by gas in the dusty torus, in addition to gas in the interstellar medium. However, the higher specific star-formation rate (sSFR) for LERGs with W2-W3 > 2 suggests that H I absorption may be largely due to star-forming gas in their hosts. LERGs with extended radio structure tend to have significantly lower values of W2-W3 compared with those with compact structure. Extended radio sources and those with W2-W3 < 2 have low H I detection rates. | [
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-... | 13.755699 | 8.490065 | 2016-07-01 | 13 | 2017MNRAS.465..997C | [
"compact radio structure",
"low H I detection rates",
"radio galaxies",
"extended radio structure",
"compact structure",
"H I absorption detections",
"gas",
"H I absorption studies",
"host galaxies",
"Extended radio sources",
"nuclear activity",
"detections",
"W2",
"active galaxies",
"a ... | [
"galaxies: active",
"galaxies: general",
"galaxies: nuclei",
"infrared: galaxies",
"radio continuum: galaxies",
"radio lines: galaxies",
"Astrophysics - Astrophysics of Galaxies",
"Astrophysics - Cosmology and Nongalactic Astrophysics"
] | 12 | [
"10.1093/mnras/stw2705",
"10.48550/arXiv.1607.00841"
] | [
"Chandola, Yogesh",
"Saikia, D. J."
] | [
"National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China",
"Cotton College State University, Panbazar, Guwahati 781 001, India; NCRA, TIFR, Post Bag 3, Ganeshkhind, Pune 411 007, India"
] | [
"2017A&A...604A..43M",
"2017MNRAS.467.2766G",
"2018A&ARv..26....4M",
"2018MNRAS.476.3580C",
"2018MNRAS.480..947D",
"2019MNRAS.482.5597A",
"2020MNRAS.491..838D",
"2020MNRAS.494.5161C",
"2021A&ARv..29....3O",
"2021ApJ...918...65S",
"2022JApA...43..103D",
"2022PASA...39...10A",
"2023A&A...675A.... | [
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"2000AJ....120.1579Y",
"2001ApJ...556..... |
12409080 | 1607.05713 | Disk Detective: Discovery of New Circumstellar Disk Candidates through Citizen Science | The Disk Detective citizen science project aims to find new stars with 22 μm excess emission from circumstellar dust using data from NASA’s Wide-field Infrared Survey Explorer (WISE) mission. Initial cuts on the AllWISE catalog provide an input catalog of 277,686 sources. Volunteers then view images of each source online in 10 different bands to identify false positives (galaxies, interstellar matter, image artifacts, etc.). Sources that survive this online vetting are followed up with spectroscopy on the FLWO Tillinghast telescope. This approach should allow us to unleash the full potential of WISE for finding new debris disks and protoplanetary disks. We announce a first list of 37 new disk candidates discovered by the project, and we describe our vetting and follow-up process. One of these systems appears to contain the first debris disk discovered around a star with a white dwarf companion: HD 74389. We also report four newly discovered classical Be stars (HD 6612, HD 7406, HD 164137, and HD 218546) and a new detection of 22 μm excess around the previously known debris disk host star HD 22128. | [
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-0.... | 8.898128 | 12.924279 | 2016-07-01 | 24 | 2016ApJ...830...84K | [
"new debris disks",
"HD",
"new stars",
"protoplanetary disks",
"Infrared Survey Explorer",
"the previously known debris disk host star HD",
"image artifacts",
"37 new disk candidates",
"interstellar matter",
"circumstellar dust",
"WISE",
"false positives",
"the first debris disk",
"FLWO Ti... | [
"catalogs",
"infrared: planetary systems",
"methods: data analysis",
"protoplanetary disks",
"stars: emission-line",
"Be",
"surveys",
"Astrophysics - Earth and Planetary Astrophysics",
"Astrophysics - Instrumentation and Methods for Astrophysics",
"Astrophysics - Solar and Stellar Astrophysics"
] | 8 | [
"10.3847/0004-637X/830/2/84",
"10.48550/arXiv.1607.05713"
] | [
"Kuchner, Marc J.",
"Silverberg, Steven M.",
"Bans, Alissa S.",
"Bhattacharjee, Shambo",
"Kenyon, Scott J.",
"Debes, John H.",
"Currie, Thayne",
"García, Luciano",
"Jung, Dawoon",
"Lintott, Chris",
"McElwain, Michael",
"Padgett, Deborah L.",
"Rebull, Luisa M.",
"Wisniewski, John P.",
"Ne... | [
"NASA Goddard Space Flight Center Exoplanets and Stellar Astrophysics Laboratory, Code 667 Greenbelt, MD 21230, USA",
"Homer L. Dodge Department of Physics and Astronomy The University of Oklahoma 440 W. Brooks St. Norman, OK 73019, USA",
"Valparaiso University, Department of Physics & Astronomy, Neils Scie... | [
"2016ApJ...830L..28S",
"2017ApJ...839...38K",
"2017ApJ...841L..19K",
"2017MNRAS.471.3419M",
"2018A&A...609A.108S",
"2018A&C....23...72N",
"2018ApJ...868...43S",
"2018MNRAS.476.3290M",
"2019clrp.2020...26R",
"2020AJ....160..156S",
"2020ApJ...890..106S",
"2020PASP..132e4401Z",
"2021AJ....161..... | [
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"1988ApJ...328..315M",
"1990PASP..102..440S",
"1993BICDS..43....5T",
"1994A&A...290..... |
12406007 | 1607.07534 | K band SINFONI spectra of two z ~ 5 submillimeter galaxy systems: upper limits to the unobscured star formation from [O II] optical emission line searches | We present deep SINFONI K-band integral field spectra of two submillimeter galaxy systems (SMG): BR 1202-0725 and J1000+0234, at z = 4.69 and 4.55, respectively. Spectra extracted for each object in the two systems do not show any signature of the [O II]λλ3726, 29 Å emission-lines, placing upper flux limits of 3.9 and 2.5 × 10<SUP>-18</SUP>erg s<SUP>-1</SUP> cm<SUP>-2</SUP>for BR 1202-0725 and J1000+0234, respectively. Using the relation between the star formation rate (SFR) and the luminosity of the [O II] doublet, we estimate unobscured SFR upper limits of ~ 10-15 M<SUB>⊙</SUB> yr<SUP>-1</SUP>and ~30-40 M<SUB>⊙</SUB> yr<SUP>-1</SUP>for the objects of the two systems, respectively. For the SMGs, these values are at least two orders of magnitude lower than those derived from SED and IR luminosities. The differences on the SFR values would correspond to internal extinction of, at least, 3.4-4.9 and 2.1-3.6 mag in the visual for BR 1202-0725 and J1000+0234 SMGs, respectively. The upper limit for the [O II]-derived SFR in one of the LAEs (Lyα2) in the BR1202-0725 system is at least one order of magnitude lower than the previous SFR derived from infrared tracers, while both estimates are in good agreement for Lyα1. The lower limits to the internal extinction in these two Lyman-alpha emitters are 0.6 mag and 1.3 mag, respectively. No evidence for [O II] emission associated with Lyα1 is identified in our data, implying that residuals of the K-band sky emission lines after subtraction in medium-band imaging data could provide the adequate flux. | [
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-0.039917971938848495,... | 13.379037 | 7.22061 | 2016-07-01 | 1 | 2016A&A...594A..74C | [
"SFR upper limits",
"upper flux limits",
"SFR",
"BR",
"z",
"Lyα1",
"internal extinction",
"magnitude",
"good agreement",
"medium-band imaging data",
"SUP>-18</SUP",
"infrared tracers",
"cm",
"residuals",
"the K-band sky emission lines",
"SINFONI K-band",
"two submillimeter galaxy sys... | [
"galaxies: high-redshift",
"galaxies: individual: BR 1202",
"0725",
"galaxies: individual: J1000+0234",
"galaxies: starburst",
"galaxies: star formation",
"Astrophysics - Astrophysics of Galaxies"
] | 3 | [
"10.1051/0004-6361/201628952",
"10.48550/arXiv.1607.07534"
] | [
"Couto, Guilherme S.",
"Colina, Luis",
"López, Javier Piqueras",
"Storchi-Bergmann, Thaisa",
"Arribas, Santiago"
] | [
"Universidade Federal do Rio Grande do Sul, IF, CP 15051, 91501-970, Porto Alegre, RS, Brazil ; Centro de Astrobiología (INTA-CSIC), Ctra de Torrejón a Ajalvir, km 4, 28850 Torrejón de Ardoz, Madrid, Spain",
"Centro de Astrobiología (INTA-CSIC), Ctra de Torrejón a Ajalvir, km 4, 28850 Torrejón de Ardoz, Madrid, S... | [
"2017ApJ...837..147H"
] | [
"1988ApJ...328L..35S",
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"2004AJ....128.2704O",
"2005ASSL..327...41C",
"2006ApJ...645L..97I",
"2007ApJ...657..... |
1093440 | 1607.07969 | The Automatic Calibration of Korean VLBI Network Data | The calibration of Very Long Baseline Interferometry (VLBI) data has long been a time consuming process. The Korean VLBI Network (KVN) is a simple array consisting of three identical antennas. Because four frequencies are observed simultaneously, phase solutions can be transferred from lower frequencies to higher frequencies in order to improve phase coherence and hence sensitivity at higher frequencies. Due to the homogeneous nature of the array, the KVN is also well suited for automatic calibration. In this paper we describe the automatic calibration of single-polarisation KVN data using the KVN Pipeline and comparing the results against VLBI data that has been manually reduced. We find that the pipelined data using phase transfer produces better results than a manually reduced dataset not using the phase transfer. Additionally we compared the pipeline results with a manually reduced phase-transferred dataset and found the results to be identical. | [
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0.020363636314868927,
-0.012048270553350449,
-... | 10.671652 | 3.791145 | 2016-07-01 | 20 | 2016JKAS...49..137H | [
"higher frequencies",
"phase transfer",
"phase coherence",
"phase solutions",
"lower frequencies",
"better results",
"VLBI data",
"KVN",
"automatic calibration",
"single-polarisation KVN data",
"Very Long Baseline Interferometry",
"order",
"the phase transfer",
"a manually reduced phase-tr... | [
"Astrophysics - Instrumentation and Methods for Astrophysics"
] | 3 | [
"10.5303/JKAS.2016.49.4.137",
"10.48550/arXiv.1607.07969"
] | [
"Hodgson, Jeffrey A.",
"Lee, Sang-Sung",
"Zhao, Guang-Yao",
"Algaba, Juan-Carlos",
"Yun, Youngjoo",
"Jung, Taehyun",
"Byun, Do-Young"
] | [
"Korea Astronomy and Space Science Institute, 776 Daedeokdae-ro, Yuseong-gu, Daejeon 34055, Korea",
"University of Science and Technology, 217 Gajeong-ro, Yuseong-gu, Daejeon 34113, Korea",
"-",
"-",
"-",
"-",
"-"
] | [
"2016ApJS..227....8L",
"2017ApJ...841..119L",
"2017JKAS...50..167K",
"2018A&A...610L...5K",
"2018AJ....155...26Z",
"2018ApJ...852...30A",
"2018ApJ...859..128A",
"2018MNRAS.480.2324K",
"2018arXiv180202766H",
"2019ApJ...877..106P",
"2019JKAS...52...31A",
"2020ApJ...902..104L",
"2020MNRAS.495L.... | [
"1980A&A....89..377C",
"1984ARA&A..22...97P",
"2002astro.ph..5118R",
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"2013EPJWC..6107007L",
"2014AJ....147...77L",
"2014AJ....148...84R",
"2015JKAS...48..229L",
"2015JKAS...48..237A"
] |
11492261 | 1607.06368 | The Eruption of the Candidate Young Star ASASSN-15QI | Outbursts on young stars are usually interpreted as accretion bursts caused by instabilities in the disk or the star-disk connection. However, some protostellar outbursts may not fit into this framework. In this paper, we analyze optical and near-infrared spectra and photometry to characterize the 2015 outburst of the probable young star ASASSN-15qi. The ∼3.5 mag brightening in the V band was sudden, with an unresolved rise time of less than one day. The outburst decayed exponentially by 1 mag for 6 days and then gradually back to the pre-outburst level after 200 days. The outburst is dominated by emission from ∼10,000 K gas. An explosive release of energy accelerated matter from the star in all directions, seen in a spectacular cool, spherical wind with a maximum velocity of 1000 km s<SUP>-1</SUP>. The wind and hot gas both disappeared as the outburst faded and the source returned to its quiescent F-star spectrum. Nebulosity near the star brightened with a delay of 10-20 days. Fluorescent excitation of H<SUB>2</SUB> is detected in emission from vibrational levels as high as v = 11, also with a possible time delay in flux increase. The mid-infrared spectral energy distribution does not indicate the presence of warm dust emission, though the optical photospheric absorption and CO overtone emission could be related to a gaseous disk. Archival photometry reveals a prior outburst in 1976. Although we speculate about possible causes for this outburst, none of the explanations are compelling. | [
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-0.0639759823679924,
... | 9.681632 | 11.623852 | 2016-07-01 | 21 | 2016ApJ...831..133H | [
"young stars",
"warm dust emission",
"vibrational levels",
"Outbursts",
"flux increase",
"emission",
"the pre-outburst level",
"∼10,000 K gas",
"hot gas",
"the probable young star ASASSN-15qi",
"accretion bursts",
"v",
"possible causes",
"the star-disk connection",
"The mid-infrared spec... | [
"stars: formation",
"stars: pre-main sequence",
"stars: variables: general",
"stars: winds",
"outflows",
"Astrophysics - Solar and Stellar Astrophysics"
] | 14 | [
"10.3847/0004-637X/831/2/133",
"10.48550/arXiv.1607.06368"
] | [
"Herczeg, Gregory J.",
"Dong, Subo",
"Shappee, Benjamin J.",
"Chen, Ping",
"Hillenbrand, Lynne A.",
"Jose, Jessy",
"Kochanek, Christopher S.",
"Prieto, Jose L.",
"Stanek, K. Z.",
"Kaplan, Kyle",
"Holoien, Thomas W. -S.",
"Mairs, Steve",
"Johnstone, Doug",
"Gully-Santiago, Michael",
"Zhu,... | [
"Kavli Institute for Astronomy and Astrophysics, Peking University, Yi He Yuan Lu 5, Haidian Qu, 100871 Beijing, People's Republic of China",
"Kavli Institute for Astronomy and Astrophysics, Peking University, Yi He Yuan Lu 5, Haidian Qu, 100871 Beijing, People's Republic of China",
"Carnegie Observatories, 813... | [
"2017A&A...607A.127S",
"2017MNRAS.464.2672H",
"2017MNRAS.467.1098H",
"2017MNRAS.468.4938K",
"2017MNRAS.471.4966H",
"2017PASP..129j4502K",
"2017SPIE10117E..0JR",
"2018ApJ...861..145C",
"2018Galax...6...82K",
"2019ApJ...874...82H",
"2019ApJ...876..115S",
"2019Galax...8....2K",
"2019MNRAS.484.1... | [
"1864MNRAS..24...65H",
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"1992AJ....104..725W",
"1992ApJS...82..247H",
"1993ASPC...52..173T",
"1993ApJ...405..... |
2246995 | 1607.01062 | A Deep X-Ray View of the Bare AGN Ark 120. I. Revealing the Soft X-Ray Line Emission | The Seyfert 1 galaxy Ark 120 is a prototype example of the so-called class of bare nucleus active galactic nuclei (AGNs), whereby there is no known evidence for the presence of ionized gas along the direct line of sight. Here deep (>400 ks exposure), high-resolution X-ray spectroscopy of Ark 120 is presented from XMM-Newton observations that were carried out in 2014 March, together with simultaneous Chandra/High Energy Transmission Grating exposures. The high-resolution spectra confirmed the lack of intrinsic absorbing gas associated with Ark 120, with the only X-ray absorption present originating from the interstellar medium (ISM) of our own Galaxy, with a possible slight enhancement of the oxygen abundance required with respect to the expected ISM values in the solar neighborhood. However, the presence of several soft X-ray emission lines are revealed for the first time in the XMM-Newton RGS spectrum, associated with the AGN and arising from the He- and H-like ions of N, O, Ne, and Mg. The He-like line profiles of N, O, and Ne appear velocity broadened, with typical FWHMs of ∼5000 km s<SUP>-1</SUP>, whereas the H-like profiles are unresolved. From the clean measurement of the He-like triplets, we deduce that the broad lines arise from a gas of density n <SUB>e</SUB> ∼ 10<SUP>11</SUP> cm<SUP>-3</SUP>, while the photoionization calculations infer that the emitting gas covers at least 10% of 4π steradian. Thus the broad soft X-ray profiles appear coincident with an X-ray component of the optical-UV broad-line region on sub-parsec scales, whereas the narrow profiles originate on larger parsec scales, perhaps coincident with the AGN narrow-line region. The observations show that Ark 120 is not intrinsically bare and substantial X-ray-emitting gas exists out of our direct line of sight toward this AGN. | [
-0.030549822375178337,
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0.009097195230424404,
... | 15.980777 | 7.975695 | 2016-07-01 | 24 | 2016ApJ...828...98R | [
"several soft X-ray emission lines",
"ionized gas",
"sub-parsec scales",
"intrinsic absorbing gas",
"AGN",
"the broad soft X-ray profiles",
"larger parsec scales",
"-",
"high-resolution X-ray spectroscopy",
"the only X-ray absorption",
"an X-ray component",
"bare nucleus active galactic nuclei... | [
"galaxies: active",
"galaxies: individual: Ark 120",
"galaxies: Seyfert",
"X-rays: galaxies",
"Astrophysics - High Energy Astrophysical Phenomena",
"Astrophysics - Astrophysics of Galaxies"
] | 7 | [
"10.3847/0004-637X/828/2/98",
"10.48550/arXiv.1607.01062"
] | [
"Reeves, J. N.",
"Porquet, D.",
"Braito, V.",
"Nardini, E.",
"Lobban, A.",
"Turner, T. J."
] | [
"Center for Space Science and Technology, University of Maryland Baltimore County, 1000 Hilltop Circle, Baltimore, MD 21250, USA ; Astrophysics Group, School of Physical and Geographical Sciences, Keele University, Keele, Staffordshire, ST5 5BG, UK;",
"Observatoire Astronomique de Strasbourg, Université de Strasb... | [
"2016ApJ...832...45N",
"2017A&A...601A..17B",
"2017ApJ...837...23R",
"2017MNRAS.472..174M",
"2018A&A...609A..42P",
"2018MNRAS.474.3237L",
"2018MNRAS.474.3782K",
"2018MNRAS.478..950M",
"2019A&A...623A..11P",
"2019A&A...623A..12M",
"2019A&A...630A..94G",
"2019ApJS..241...33L",
"2019MNRAS.489.3... | [
"1977PASP...89..251O",
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"1994ApJ...434..570T",
"1995ApJ...455L.119B",
"1995ApJS...99..461N",
"1995PASP..107..803U",
"1997MNRAS.286..... |
12594280 | 1607.08005 | Similarities and uniqueness of Ly α emitters among star-forming galaxies at z = 2.5 | We conducted a deep narrow-band imaging survey with the Subaru Prime Focus Camera on the Subaru Telescope and constructed a sample of Lyα emitters (LAEs) at z = 2.53 in the UDS-CANDELS field, where a sample of Hα emitters (HAEs) at the same redshift is already obtained from our previous narrow-band observation at near-infrared. The deep narrow-band and multibroad-band data allow us to find LAEs of stellar masses and star formation rates (SFRs) down to ≳10<SUP>8</SUP> M<SUB>⊙</SUB> and ≳0.2 M<SUB>⊙</SUB> yr<SUP>-1</SUP>, respectively. We show that the LAEs are located along the same mass-SFR sequence traced by normal star-forming galaxies such as HAEs, but towards a significantly lower mass regime. Likewise, LAEs seem to share the same mass-size relation with typical star-forming galaxies, except for the massive LAEs that tend to show significantly compact sizes. We identify a vigorous mass growth in the central part of LAEs: the stellar mass density in the central region of LAEs increases as their total galaxy mass grows. On the other hand, we see no Lyα line in emission for most of the HAEs. Rather, we find that the Lyα feature is either absent or in absorption (Lyα absorbers, LAAs), and its absorption strength may increase with reddening of the UV continuum slope. We demonstrate that a deep Lyα narrow-band imaging like this study is able to search for not only LAEs but also LAAs in a certain redshift slice. This work suggests that LAEs trace normal star-forming galaxies in the low-mass regime, while they remain as a unique population because the majority of HAEs are not LAEs. | [
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-0... | 13.462973 | 6.428069 | 2016-07-01 | 17 | 2017MNRAS.468.1123S | [
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"Hα emitters",
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"Lyα",
"stellar masses",
"LAAs",
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"a certain redshift slice",... | [
"galaxies: evolution",
"galaxies: formation",
"galaxies: high-redshift",
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] | 12 | [
"10.1093/mnras/stx091",
"10.48550/arXiv.1607.08005"
] | [
"Shimakawa, Rhythm",
"Kodama, Tadayuki",
"Shibuya, Takatoshi",
"Kashikawa, Nobunari",
"Tanaka, Ichi",
"Matsuda, Yuichi",
"Tadaki, Ken-ichi",
"Koyama, Yusei",
"Hayashi, Masao",
"Suzuki, Tomoko L.",
"Yamamoto, Moegi"
] | [
"Department of Astronomical Science, SOKENDAI, Osawa, Mitaka, Tokyo 181-8588, Japan; National Astronomical Observatory of Japan, Osawa, Mitaka, Tokyo 181-8588, Japan",
"Department of Astronomical Science, SOKENDAI, Osawa, Mitaka, Tokyo 181-8588, Japan; National Astronomical Observatory of Japan, Osawa, Mitaka, To... | [
"2016arXiv161001163H",
"2018ApJ...859...84H",
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"2020MNRAS.491.3266G",
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2219791 | 1607.06829 | A perturbation study of axisymmetric strongly magnetic degenerate stars: the case of super-Chandrasekhar white dwarfs | In the presence of a strong magnetic field, a stellar equilibrium configuration, aided by the Lorentz force, can support a larger mass than a non-magnetic one. This has been considered a possible explanation of the super-Chandrasekhar mass white dwarfs giving rise to overluminous Type-Ia supernovae. We present here linear and non-linear perturbation studies of such strongly magetized configurations and show that axisymmetric configurations with poloidal or toroidal fields are unstable. The numerical evolution of the perturbations shows instability after about an Alfvén crossing time. This time-scale is very short for the magnetically supported super-Chandrasekhar mass white dwarfs. Uniform rotation about the symmetry axis can reduce the growth rate but cannot stabilize the super-massive configurations. It is concluded that long-lived super-Chandrasekhar mass white dwarfs supported by magnetic field are unlikely to occur in nature. | [
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0... | 4.619769 | 3.167871 | 2016-07-01 | 6 | 2017MNRAS.465.4026B | [
"axisymmetric configurations",
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"the magnetically supported super-Chandrasekhar mass white dwarfs",
"nature",
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"long-lived super-Chandr... | [
"instabilities",
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"methods: numerical",
"stars: magnetic field",
"white dwarfs",
"Astrophysics - Solar and Stellar Astrophysics",
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] | 2 | [
"10.1093/mnras/stw2979",
"10.48550/arXiv.1607.06829"
] | [
"Bera, Prasanta",
"Bhattacharya, Dipankar"
] | [
"Inter University Centre for Astronomy and Astrophysics, Post Bag 4, Pune 411007, India",
"Inter University Centre for Astronomy and Astrophysics, Post Bag 4, Pune 411007, India"
] | [
"2017ASPC..509..395B",
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"2018CoSka..48..250M",
"2019PhLB..79734859P",
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] | [
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1243490 | 1607.02707 | The radio spectral energy distribution of infrared-faint radio sources | Context. Infrared-faint radio sources (IFRS) are a class of radio-loud (RL) active galactic nuclei (AGN) at high redshifts (z ≥ 1.7) that are characterised by their relative infrared faintness, resulting in enormous radio-to-infrared flux density ratios of up to several thousand. <BR /> Aims: Because of their optical and infrared faintness, it is very challenging to study IFRS at these wavelengths. However, IFRS are relatively bright in the radio regime with 1.4 GHz flux densities of a few to a few tens of mJy. Therefore, the radio regime is the most promising wavelength regime in which to constrain their nature. We aim to test the hypothesis that IFRS are young AGN, particularly GHz peaked-spectrum (GPS) and compact steep-spectrum (CSS) sources that have a low frequency turnover. <BR /> Methods: We use the rich radio data set available for the Australia Telescope Large Area Survey fields, covering the frequency range between 150 MHz and 34 GHz with up to 19 wavebands from different telescopes, and build radio spectral energy distributions (SEDs) for 34 IFRS. We then study the radio properties of this class of object with respect to turnover, spectral index, and behaviour towards higher frequencies. We also present the highest-frequency radio observations of an IFRS, observed with the Plateau de Bure Interferometer at 105 GHz, and model the multi-wavelength and radio-far-infrared SED of this source. <BR /> Results: We find IFRS usually follow single power laws down to observed frequencies of around 150 MHz. Mostly, the radio SEDs are steep (α < -0.8; %), but we also find ultra-steep SEDs (α < -1.3; %). In particular, IFRS show statistically significantly steeper radio SEDs than the broader RL AGN population. Our analysis reveals that the fractions of GPS and CSS sources in the population of IFRS are consistent with the fractions in the broader RL AGN population. We find that at least % of IFRS contain young AGN, although the fraction might be significantly higher as suggested by the steep SEDs and the compact morphology of IFRS. The detailed multi-wavelength SED modelling of one IFRS shows that it is different from ordinary AGN, although it is consistent with a composite starburst-AGN model with a star formation rate of 170 M<SUB>⊙</SUB> yr<SUP>-1</SUP>. <P />Based on observations carried out with the IRAM Plateau de Bure Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). | [
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"galaxies: active",
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] | 6 | [
"10.1051/0004-6361/201527000",
"10.48550/arXiv.1607.02707"
] | [
"Herzog, A.",
"Norris, R. P.",
"Middelberg, E.",
"Seymour, N.",
"Spitler, L. R.",
"Emonts, B. H. C.",
"Franzen, T. M. O.",
"Hunstead, R.",
"Intema, H. T.",
"Marvil, J.",
"Parker, Q. A.",
"Sirothia, S. K.",
"Hurley-Walker, N.",
"Bell, M.",
"Bernardi, G.",
"Bowman, J. D.",
"Briggs, F."... | [
"Astronomisches Institut, Ruhr-Universität Bochum, Universitätsstr. 150, 44801, Bochum, Germany ; Macquarie University, Sydney, NSW, 2109, Australia; CSIRO Astronomy and Space Science, Marsfield, PO Box 76, Epping, NSW, 1710, Australia",
"CSIRO Astronomy and Space Science, Marsfield, PO Box 76, Epping, NSW, 1710,... | [
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12518234 | 1607.00228 | The Appearance of Non-Spherical Systems. Application to LMXB | We study the appearance of the neutron star-accretion disk system as seen by a distant observer in the UV/X-ray domain. The observed intensity spectra are computed assuming non-spherical geometry of the whole system, in which outgoing spectrum is not represented by the flux spectrum, the latter being valid for spherically symmetric objects. Intensity spectra of our model display double bumps in UV/X-ray energy domains. Such structure is caused by the fact that the the source is not spherically symmetric, and the proper integration of intensity over emitted area is needed to reproduce observed spectral shape. Relative normalization of double bump is self consistently computed by our model. X-ray spectra of such a type were often observed in LMXB with accretion disk, ultra luminous X-ray sources, and accreting black hole systems with hot inner compact corona. Our model naturally explains high energy broadening of the disk spectrum observed in some binaries. We attempted to fit our model to X-ray data of XTE J1709-267 from XMM-Newton. Unfortunately, the double intensity bump predicted by our model for LMXB is located in soft X-ray domain, uncovered by existing data for this source. | [
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-0.04687043651938438... | 6.253361 | 6.572081 | 2016-07-01 | 3 | 2017AcA....67...51R | [
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"UV/X-ray energy domains",
"existing data",
"accretion disk",
"non-spherical geometry",
"emitted area",
"the... | [
"Accretion",
"accretion disks",
"Stars: neutron",
"X-rays: binaries",
"Astrophysics - High Energy Astrophysical Phenomena"
] | 4 | [
"10.32023/0001-5237/67.1.3",
"10.48550/arXiv.1607.00228"
] | [
"Różańska, A.",
"Bełdycki, B.",
"Madej, J.",
"Adhikari, T. P.",
"You, B."
] | [
"N. Copernicus Astronomical Center, Bartycka 18, 00-716 Warsaw, Poland",
"N. Copernicus Astronomical Center, Bartycka 18, 00-716 Warsaw, Poland",
"Warsaw University Observatory, Al. Ujazdowskie 4, 00-478 Warszawa, Poland",
"-",
"-"
] | [
"2018A&A...612L..12R",
"2022ApJ...925..206M",
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12472610 | 1607.02477 | Is there substructure around M87? | We present a general method to identify infalling substructure in discrete data sets with position and line-of-sight velocity data. We exploit the fact that galaxies falling on to a brightest cluster galaxy (BCG) in a virialized cluster, or dwarf satellites falling on to a central galaxy like the Milky Way, follow nearly radial orbits. If the orbits are exactly radial, we show how to find the probability distribution for a satellite's energy, given a tracer density for the satellite population, by solving an Abel integral equation. This is an extension of Eddington's classical formula for the isotropic distribution function. When applied to a system of galaxies, clustering in energy space can then be quantified using the Kullback-Leibler divergence, and groups of objects can be identified which, though separated in the sky, may be falling in on the same orbit. This method is tested using mock data and applied to the satellite galaxy population around M87, the BCG in Virgo, and a number of associations that are found, which may represent infalling galaxy groups. | [
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-0.... | 10.674732 | 6.126083 | 2016-07-01 | 7 | 2016MNRAS.462..298O | [
"galaxy groups",
"dwarf satellites",
"galaxies",
"the satellite galaxy population",
"mock data",
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"discrete data sets",
"groups",
"a brightest cluster galaxy",
"BCG",
"the satellite population",
"a central galaxy",
"objects",
"nearly radial orbits",
"an Abel integral equat... | [
"galaxies: individual: M87",
"galaxies: kinematics and dynamics",
"galaxies: structure",
"Astrophysics - Astrophysics of Galaxies"
] | 3 | [
"10.1093/mnras/stw1574",
"10.48550/arXiv.1607.02477"
] | [
"Oldham, L. J.",
"Evans, N. W."
] | [
"Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK",
"Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK"
] | [
"2018ApJ...864...36L",
"2018MNRAS.473.5476C",
"2018MNRAS.474.4169O",
"2019MNRAS.484.1702P",
"2022ApJ...931..120K",
"2022MNRAS.512.2266B",
"2023MNRAS.519.6065B"
] | [
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2241475 | 1607.03701 | Ionization and Dust Charging in Protoplanetary Disks | Ionization-recombination balance in dense interstellar and circumstellar environments is a key factor for a variety of important physical processes, such as chemical reactions, dust charging and coagulation, coupling of the gas with magnetic field, and development of instabilities in protoplanetary disks. We determine a critical gas density above which the recombination of electrons and ions on the grain surface dominates over the gas-phase recombination. For this regime, we present a self-consistent analytical model, which allows us to calculate exactly the abundances of charged species in dusty gas, without making assumptions on the grain charge distribution. To demonstrate the importance of the proposed approach, we check whether the conventional approximation of low grain charges is valid for typical protoplanetary disks, and discuss the implications for dust coagulation and development of the “dead zone” in the disk. The presented model is applicable for arbitrary grain-size distributions and, for given dust properties and conditions of the disk, has only one free parameter—the effective mass of the ions, shown to have a small effect on the results. The model can be easily included in numerical simulations following the dust evolution in dense molecular clouds and protoplanetary disks. | [
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... | 10.12242 | 13.419773 | 2016-07-01 | 25 | 2016ApJ...833...92I | [
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"low grain charges",
"dusty gas",
"coagulation",
"ions",
"dense molecular clouds",
"development",
"important physical processes",
"magnetic field",
"chemical reactions",
"the d... | [
"astrochemistry",
"cosmic rays",
"dust",
"extinction",
"ISM: clouds",
"protoplanetary disks",
"Astrophysics - Solar and Stellar Astrophysics",
"Astrophysics - Earth and Planetary Astrophysics",
"Astrophysics - Astrophysics of Galaxies"
] | 9 | [
"10.3847/1538-4357/833/1/92",
"10.48550/arXiv.1607.03701"
] | [
"Ivlev, A. V.",
"Akimkin, V. V.",
"Caselli, P."
] | [
"Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstr. 1, D-85748 Garching, Germany",
"Institute of Astronomy of the Russian Academy of Sciences, Pyatnitskaya Street 48, 119017 Moscow, Russia",
"Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstr. 1, D-85748 Garching, Germany"
] | [
"2016ApJS..226...12T",
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"2018MNRAS.478.2723Z",
"2019A&A...632A..44T",
"2019MNRAS.484..161G",
"2019MNRAS.487.5405S",
"2020A&A...643A.... | [
"1962pfig.book.....S",
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12521732 | 1607.03537 | Hubble Parameter Measurement Constraints on the Redshift of the Deceleration-Acceleration Transition, Dynamical Dark Energy, and Space Curvature | We compile an updated list of 38 measurements of the Hubble parameter H(z) between redshifts 0.07 ≤ z ≤ 2.36 and use them to place constraints on model parameters of constant and time-varying dark energy cosmological models, both spatially flat and curved. We use five models to measure the redshift of the cosmological deceleration-acceleration transition, z<SUB>da</SUB>, from these H(z) data. Within the error bars, the measured z<SUB>da</SUB> are insensitive to the model used, depending only on the value assumed for the Hubble constant H<SUB>0</SUB>. The weighted mean of our measurements is z<SUB>da</SUB> = 0.72 ± 0.05 (0.84 ± 0.03) for H<SUB>0</SUB> = 68 ± 2.8 (73.24 ± 1.74) km s<SUP>-1</SUP> Mpc<SUP>-1</SUP> and should provide a reasonably model-independent estimate of this cosmological parameter. The H(z) data are consistent with the standard spatially flat ΛCDM cosmological model but do not rule out nonflat models or dynamical dark energy models. | [
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0.... | 11.635274 | 1.368594 | 2016-07-01 | 325 | 2017ApJ...835...26F | [
"model parameters",
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"±",
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"the standard spatially flat ΛCDM cosmological model",
"the Hubble constant H<SUB>0</SUB",
"da</SUB",
"this cosmological parameter",
"redshifts",
"z",
"five m... | [
"cosmological parameters",
"cosmology: observations",
"dark energy",
"Astrophysics - Cosmology and Nongalactic Astrophysics",
"Astrophysics - Astrophysics of Galaxies",
"General Relativity and Quantum Cosmology"
] | 14 | [
"10.3847/1538-4357/835/1/26",
"10.48550/arXiv.1607.03537"
] | [
"Farooq, Omer",
"Ranjeet Madiyar, Foram",
"Crandall, Sara",
"Ratra, Bharat"
] | [
"Department of Physical Sciences, Embry-Riddle Aeronautical University, 600 Clyde Morris Boulevard, Daytona Beach, FL 32114, USA",
"Department of Physical Sciences, Embry-Riddle Aeronautical University, 600 Clyde Morris Boulevard, Daytona Beach, FL 32114, USA",
"Department of Physics, Kansas State University, 1... | [
"2016Univ....2...27F",
"2017ApJ...835...86C",
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"2017MPLA...3230019V",
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12408878 | 1607.01829 | The Hot Companion and Circumbinary Disk of the Be Star HR 2142 | We present a spectroscopic investigation of the Be+sdO binary system HR 2142 that is based upon large sets of ultraviolet observations from the International Ultraviolet Explorer (IUE) and ground-based Hα observations. We measured radial velocities for the Be star component from these spectra and computed a revised orbit. In order to search for the spectral signature of the hot subdwarf, we cross-correlated the short wavelength end of each IUE spectrum with a model hot star spectrum, and then we used the predicted Doppler shifts of the subdwarf to shift-and-add all the cross-correlation functions to the frame of the subdwarf. This merged function shows the weak signal from the spectral lines of the hot star, and a best fit is obtained with a mass ratio {M}<SUB>2</SUB>/{M}<SUB>1</SUB>=0.07+/- 0.02, companion temperature {T}<SUB>{{eff</SUB>}}≥slant 43+/- 5 kK, projected rotational velocity V\sin I\lt 30 km s<SUP>-1</SUP>, and a monochromatic flux ratio near 1170 Å of {f}<SUB>2</SUB>/{f}<SUB>1</SUB>\gt 0.009+/- 0.001. This hot subdwarf creates a one-armed spiral, tidal wake in the disk of the Be star, and we present a circumbinary disk model that can explain the occurrence of shell absorption lines by gas enhancements that occur where gas crossing the gap created by the subdwarf strikes the disk boundaries. The faint companion of HR 2142 may be representative of a significant fraction of Be stars with undetected former mass donor companion stars. | [
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0.... | 7.576323 | 11.040377 | 2016-07-01 | 41 | 2016ApJ...828...47P | [
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"HD 41335",
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] | 13 | [
"10.3847/0004-637X/828/1/47",
"10.48550/arXiv.1607.01829"
] | [
"Peters, Geraldine J.",
"Wang, Luqian",
"Gies, Douglas R.",
"Grundstrom, Erika D."
] | [
"Space Sciences Center, University of Southern California, Los Angeles, CA 90089-1341, USA ;;",
"Center for High Angular Resolution Astronomy and Department of Physics and Astronomy, Georgia State University, P.O. Box 5060, Atlanta, GA 30302-5060, USA",
"Center for High Angular Resolution Astronomy and Departme... | [
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2068556 | 1607.05726 | An Improved Distance and Mass Estimate for Sgr A* from a Multistar Orbit Analysis | We present new, more precise measurements of the mass and distance of our Galaxy’s central supermassive black hole, Sgr A*. These results stem from a new analysis that more than doubles the time baseline for astrometry of faint stars orbiting Sgr A*, combining 2 decades of speckle imaging and adaptive optics data. Specifically, we improve our analysis of the speckle images by using information about a star’s orbit from the deep adaptive optics data (2005-2013) to inform the search for the star in the speckle years (1995-2005). When this new analysis technique is combined with the first complete re-reduction of Keck Galactic Center speckle images using speckle holography, we are able to track the short-period star S0-38 (K-band magnitude = 17, orbital period = 19 yr) through the speckle years. We use the kinematic measurements from speckle holography and adaptive optics to estimate the orbits of S0-38 and S0-2 and thereby improve our constraints of the mass (M <SUB>bh</SUB>) and distance (R <SUB> o </SUB>) of Sgr A*: M <SUB>bh</SUB> = (4.02 ± 0.16 ± 0.04) × 10<SUP>6</SUP> M <SUB>⊙</SUB> and 7.86 ± 0.14 ± 0.04 kpc. The uncertainties in M <SUB>bh</SUB> and R <SUB> o </SUB> as determined by the combined orbital fit of S0-2 and S0-38 are improved by a factor of 2 and 2.5, respectively, compared to an orbital fit of S0-2 alone and a factor of ∼2.5 compared to previous results from stellar orbits. This analysis also limits the extended dark mass within 0.01 pc to less than 0.13 × 10<SUP>6</SUP> M <SUB>⊙</SUB> at 99.7% confidence, a factor of 3 lower compared to prior work. | [
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-0... | 8.661275 | 5.997828 | 2016-07-01 | 306 | 2016ApJ...830...17B | [
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"infrared: stars",
"quasars: supermassive black holes",
"techniques: high angular resolution",
"Astrophysics - Astrophysics of Galaxies"
] | 17 | [
"10.3847/0004-637X/830/1/17",
"10.48550/arXiv.1607.05726"
] | [
"Boehle, A.",
"Ghez, A. M.",
"Schödel, R.",
"Meyer, L.",
"Yelda, S.",
"Albers, S.",
"Martinez, G. D.",
"Becklin, E. E.",
"Do, T.",
"Lu, J. R.",
"Matthews, K.",
"Morris, M. R.",
"Sitarski, B.",
"Witzel, G."
] | [
"UCLA, Department of Physics and Astronomy, Los Angeles, CA 90095, USA",
"UCLA, Department of Physics and Astronomy, Los Angeles, CA 90095, USA",
"Instituto de Astrofísica de Andalucía (CSIC), Glorieta de la Astronomía S/N, E-18008 Granada, Spain",
"UCLA, Department of Physics and Astronomy, Los Angeles, CA 9... | [
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12434581 | 1607.02094 | Magneto-optic effects of the Cosmic Microwave Background | Generation of magneto-optic effects by the interaction of the CMB with cosmic magnetic fields is studied. Effects which generate polarization such as the Cotton-Mouton effect, vacuum polarization and photon-pseudoscalar mixing in external magnetic field are studied. Considering the CMB linearly polarized at decoupling time, it is shown that photon-pseudoscalar mixing in external magnetic field, the Cotton-Mouton effect in plasma and the vacuum polarization in cosmic magnetic field, would generate elliptic polarization of the CMB depending on the photon frequency and magnetic field strength. Among standard magneto-optic effects, the Cotton-Mouton effect in plasma turns out to be the dominant effect in the generation of CMB elliptic polarization in the low frequency part $\nu_0 \sim 10^8-10^9$ Hz with degree of circular polarization $P_C(T_0)\simeq 10^{-10}-10^{-6}$ for magnetic field amplitude $B_{e0}\sim 100\, \text{nG}-1$ nG. The vacuum polarization in magnetic field is the dominant process in the high frequency part $\nu_0\geq 10^{10}$ Hz where the degree of circular polarization at present is $P_C(T_0)\lesssim 10^{-11}$ in the best scenario. It is shown that photon-pseudoscalar particle mixing in cosmic magnetic field generates elliptic polarization of the CMB as well and even in the case of initially unpolarized CMB. New limits/constraints on the pseudoscalar parameter space are found. By using current limit on the degree of circular polarization of the CMB, the upper limit of $|g_{\phi\gamma}|<4.29\times 10^{-19}(\text{G}/B_{e0})$ GeV$^{-1}$ for $m_\phi<1.6\times 10^{-14}$ eV in the weak mixing case is found. If $|g_{\phi\gamma}| < 1.17\times 10^{-24}(\text{G}/B_{e0})$ GeV$^{-1}$, a value of the order $|g_{\phi\gamma}|\simeq 10^{-26}(\text{G}/B_{e0})$ GeV$^{-1}$ for $m_\phi\simeq 1.6\times 10^{-14}$ eV in the resonant case, from large scale temperature anisotropy is obtained. | [
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0.... | 12.582679 | 0.152251 | 2016-07-01 | 6 | 2016arXiv160702094E | [
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"Astrophysics - Cosmology and Nongalactic Astrophysics",
"General Relativity and Quantum Cosmology",
"High Energy Physics - Phenomenology",
"Quantum Physics"
] | 2 | [
"10.48550/arXiv.1607.02094"
] | [
"Ejlli, Damian"
] | [
"-"
] | [
"2017PhRvD..96b3540E",
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1486962 | 1607.07723 | Probing the physics and history of cosmic reionization with the Sunyaev-Zel'dovich effect | Context. The evolution of the Universe during the dark ages (DA) and the epoch of reonization (EoR) marks an important transition in the history of the Universe but it is not yet fully understood. <BR /> Aims: We study here an alternative technique to probe the DA and EoR that makes use of the Comptonization of the CMB spectrum modified by physical effects occurring during this epoch related to the emergence of the 21-cm radiation background. Inverse Compton scattering of 21-cm photon background by thermal and non-thermal electrons residing in the atmospheres of cosmic structures like galaxy clusters, radiogalaxy lobes and galaxy halos, produces a specific form of Sunyaev-Zel'dovich effect (SZE) that we refer to as SZE-21 cm. <BR /> Methods: We derived the SZE-21 cm in a general relativistic approach, which is required to describe the correct spectral features of this astrophysical effect. We calculated the spectral features of the thermal and non-thermal SZE-21 cm in galaxy clusters and in radiogalaxy lobes, and their dependence on the history of physical mechanisms occurring during the DA and EoR. We studied how the spectral shape of the SZE-21 cm can be used to establish the global features in the mean 21-cm spectrum generated during and prior to the EoR, and how it depends on the properties of the (thermal and non-thermal) plasma in cosmic structures. <BR /> Results: We found that the thermal and non-thermal SZE-21 cm have peculiar spectral shapes that allow to investigate the physics and history of the EoR and DA. Its spectrum depends on the gas temperature (for the thermal SZE-21 cm) and on the electrons minimum momentum (for the non-thermal SZE-21 cm). The global SZE-21 cm signal can be detected (in ~ 1000 h) by SKA1-low in the frequency range ν ≳ 75-90 MHz, for clusters in the temperature range 5 to 20 keV, and the difference between the SZE-21 cm and the standard SZE can be detected by SKA1 or SKA2 at frequencies depending on the background model and the cluster temperature. <BR /> Conclusions: We have shown that the detection of the SZE-21 cm can provide unique information on the DA and EoR, and on the cosmic structures that produce the scattering; the frequencies at which the SZE-21 cm shows its main spectral features will indicate the epoch at which the physical processes related to the cosmological 21-cm signal occurred and shed light on the cosmic history during the DA and EoR by using local, well-known cosmic structures like galaxy clusters and radio galaxies. | [
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0.... | 13.296888 | 3.253237 | 2016-07-01 | 5 | 2016A&A...595A..21C | [
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"... | [
"dark ages",
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] | 3 | [
"10.1051/0004-6361/201424904",
"10.48550/arXiv.1607.07723"
] | [
"Colafrancesco, S.",
"Marchegiani, P.",
"Emritte, M. S."
] | [
"INAF-Osservatorio Astronomico di Roma via Frascati 33, 00040, Monteporzio, Italy ; School of Physics, University of the Witwatersrand, Private Bag 3, 2050, Johannesburg, South Africa",
"INAF-Osservatorio Astronomico di Roma via Frascati 33, 00040, Monteporzio, Italy; School of Physics, University of the Witwater... | [
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11492527 | 1607.05383 | The Clustering of Luminous Red Galaxies at z ∼ 0.7 from EBOSS and BOSS Data | We present the first scientific results from the luminous red galaxy (LRG) sample of the extended Baryon Oscillation Spectroscopic Survey (eBOSS) combined with the high-redshift galaxies of the previous BOSS sample. We measure the small- and intermediate-scale clustering from a sample of more than 97,000 galaxies in the redshift range 0.6< z< 0.9. We interpret these measurements in the framework of the Halo Occupation Distribution. The bias of this sample of LRGs is 2.30 ± 0.03, with a satellite fraction of 13% ± 3% and a mean halo mass of 2.5× {10}<SUP>13</SUP> {h}<SUP>-1</SUP> {M}<SUB>⊙ </SUB>. These results are consistent with expectations, demonstrating that these LRGs will be reliable tracers of large-scale structure at z∼ 0.7. The galaxy bias implies a scatter of luminosity at fixed halo mass, {σ }<SUB>{log</SUB>L}, of 0.19 dex. Using the clustering of massive galaxies from BOSS CMASS, BOSS LOWZ, and SDSS, we find that {σ }<SUB>{log</SUB>L}=0.19 is consistent with observations over the full redshift range that these samples cover. The addition of eBOSS to previous surveys allows the investigation of the evolution of massive galaxies over the past ∼7 Gyr. | [
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"cosmology: observations",
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] | 6 | [
"10.3847/1538-4357/aa8eee",
"10.48550/arXiv.1607.05383"
] | [
"Zhai, Zhongxu",
"Tinker, Jeremy L.",
"Hahn, ChangHoon",
"Seo, Hee-Jong",
"Blanton, Michael R.",
"Tojeiro, Rita",
"Camacho, Hugo O.",
"Lima, Marcos",
"Carnero Rosell, Aurelio",
"Sobreira, Flavia",
"da Costa, Luiz N.",
"Bautista, Julian E.",
"Brownstein, Joel R.",
"Comparat, Johan",
"Daws... | [
"Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003, USA",
"Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003, USA",
"Center for Cosmology and Particle Physics, ... | [
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12408147 | 1607.00874 | Probabilistic Inference of Basic Stellar Parameters: Application to Flickering Stars | The relations between observable stellar parameters are usually assumed to be deterministic. That is, given an infinitely precise measurement of independent variable, “x”, and some model, the value of dependent variable, “y” can be known exactly. In practice this assumption is rarely valid and intrinsic stochasticity means that two stars with exactly the same “x” will have slightly different “y”s. The relation between short-timescale brightness fluctuations (flicker) of stars and both surface gravity and stellar density are two such stochastic relations that have until now been treated as deterministic ones. We recalibrate these relations in a probabilistic framework, using hierarchical Bayesian modeling to constrain the instrinsic scatter in the relations. We find evidence for additional scatter in the relationship, that cannot be accounted for by the observational uncertainties alone. The scatter in surface gravity and stellar density does not depend on flicker, suggesting that using flicker as a proxy for {log}g and ρ <SUB>⋆</SUB> is equally valid for dwarf and giant stars, despite the fact that the observational uncertainties tend to be larger for dwarfs. <P />Based on archival data of the Kepler telescope. | [
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0... | 7.612182 | 12.071368 | 2016-07-01 | 1 | 2016ApJ...823L...9A | [
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"y",
"dwarf",
"the ... | [
"methods: statistical",
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"Astrophysics - Solar and Stellar Astrophysics"
] | 5 | [
"10.3847/2041-8205/823/1/L9",
"10.48550/arXiv.1607.00874"
] | [
"Angus, Ruth",
"Kipping, David. M."
] | [
"Department of Physics, University of Oxford, UK",
"Department of Astronomy, Columbia University, 550 W 120th Street, New York, NY 10027, USA"
] | [
"2017A&C....19....1T"
] | [
"2003ApJ...585.1038S",
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12408259 | 1607.08162 | Realistic Detectability of Close Interstellar Comets | During the planet formation process, billions of comets are created and ejected into interstellar space. The detection and characterization of such interstellar comets (ICs) (also known as extra-solar planetesimals or extra-solar comets) would give us in situ information about the efficiency and properties of planet formation throughout the galaxy. However, no ICs have ever been detected, despite the fact that their hyperbolic orbits would make them readily identifiable as unrelated to the solar system. Moro-Martín et al. have made a detailed and reasonable estimate of the properties of the IC population. We extend their estimates of detectability with a numerical model that allows us to consider “close” ICs, e.g., those that come within the orbit of Jupiter. We include several constraints on a “detectable” object that allow for realistic estimates of the frequency of detections expected from the Large Synoptic Survey Telescope (LSST) and other surveys. The influence of several of the assumed model parameters on the frequency of detections is explored in detail. Based on the expectation from Moro-Martín et al., we expect that LSST will detect 0.001-10 ICs during its nominal 10 year lifetime, with most of the uncertainty from the unknown number density of small (nuclei of ∼0.1-1 km) ICs. Both asteroid and comet cases are considered, where the latter includes various empirical prescriptions of brightening. Using simulated LSST-like astrometric data, we study the problem of orbit determination for these bodies, finding that LSST could identify their orbits as hyperbolic and determine an ephemeris sufficiently accurate for follow-up in about 4-7 days. We give the hyperbolic orbital parameters of the most detectable ICs. Taking the results into consideration, we give recommendations to future searches for ICs. | [
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-0... | 8.332028 | 16.487818 | 2016-07-01 | 53 | 2016ApJ...825...51C | [
"extra-solar comets",
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"orbit determination",
"such interstellar comets",
"interstellar space",
"comets",
"LSST",
"other surveys",
"realistic estimates",
"planet formation",
"various empirical prescriptions",
"situ information",
"properties",
"Jupiter",... | [
"comets: general",
"ISM: general",
"methods: observational",
"planetary systems",
"Astrophysics - Earth and Planetary Astrophysics"
] | 10 | [
"10.3847/0004-637X/825/1/51",
"10.48550/arXiv.1607.08162"
] | [
"Cook, Nathaniel V.",
"Ragozzine, Darin",
"Granvik, Mikael",
"Stephens, Denise C."
] | [
"Brigham Young University, BYU Department of Physics and Astronomy N283 ESC, Provo, UT 84602, USA",
"Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA ; University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611, USA ; Florida Institute of Technology, 150 W... | [
"2016ApJ...833...78M",
"2017AJ....153..133E",
"2017AJ....153..203L",
"2017ApJ...850L..38T",
"2017ApJ...851L...5Y",
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"2018AJ....155..217S",
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12500421 | 1607.04385 | Sulfur and zinc abundances of red giant stars† | Sulfur and zinc are chemically volatile elements, which play significant roles as depletion-free tracers in studying galactic chemical evolution. However, regarding red giants having evolved off the main sequence, reliable abundance determinations of S and Zn seem to be difficult, despite the several studies that have been reported so far. Given this situation, we tried to establish the abundances of these elements for an extensive sample of 239 field GK giants ( - 0.8 ≲ [Fe/H] ≲ +0.2), by applying the spectrum-fitting technique to S I 8694-5, S I 6757, and Zn I 6362 lines and by taking into account the non-LTE effect. Besides, similar abundance analysis was done for 160 FGK dwarfs to be used for comparison. The non-LTE corrections for the S and Zn abundances derived from these lines turned out to be ≲ 0.1(-0.2) dex for most cases and not very significant. It revealed that the S I 6757 feature is more reliable as an abundance indicator than S I 8694-5 for the case of red giants, because the latter suffers blending of unidentified lines. The finally resulting [S/Fe]-[Fe/H] and [Zn/Fe]-[Fe/H] relations for GK giants were confirmed to be in good agreement with those for FGK dwarfs, indicating that S and Zn abundances of red giants are reliably determinable from the S I 6757 and Zn I 6362 lines. Accordingly, not only main-sequence stars but also evolved red giant stars are usable for tracing the chemical evolution history of S and Zn in the regime of disk metallicity by using these lines. | [
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-0.... | 8.707664 | 9.233992 | 2016-07-01 | 20 | 2016PASJ...68...81T | [
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... | [
"stars: abundances",
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"Astrophysics - Solar and Stellar Astrophysics"
] | 7 | [
"10.1093/pasj/psw071",
"10.48550/arXiv.1607.04385"
] | [
"Takeda, Yoichi",
"Omiya, Masashi",
"Harakawa, Hiroki",
"Sato, Bun'ei"
] | [
"National Astronomical Observatory, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; SOKENDAI, The Graduate University for Advanced Studies, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan",
"National Astronomical Observatory, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan",
"National Astronomical Observatory, 2-21-1 Osaw... | [
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2526299 | 1607.03100 | Size matters: abundance matching, galaxy sizes, and the Tully-Fisher relation in EAGLE | The Tully-Fisher relation (TFR) links the stellar mass of a disc galaxy, M<SUB>str</SUB>, to its rotation speed: it is well approximated by a power law, shows little scatter, and evolves weakly with redshift. The relation has been interpreted as reflecting the mass-velocity scaling (M ∝ V<SUP>3</SUP>) of dark matter haloes, but this interpretation has been called into question by abundance-matching (AM) models, which predict the galaxy-halo mass relation to deviate substantially from a single power law and to evolve rapidly with redshift. We study the TFR of luminous spirals and its relation to AM using the EAGLE set of Λ cold dark matter (ΛCDM) cosmological simulations. Matching both relations requires disc sizes to satisfy constraints given by the concentration of haloes and their response to galaxy assembly. EAGLE galaxies approximately match these constraints and show a tight mass-velocity scaling that compares favourably with the observed TFR. The TFR is degenerate to changes in galaxy formation efficiency and the mass-size relation; simulations that fail to match the galaxy stellar mass function may fit the observed TFR if galaxies follow a different mass-size relation. The small scatter in the simulated TFR results because, at fixed halo mass, galaxy mass and rotation speed correlate strongly, scattering galaxies along the main relation. EAGLE galaxies evolve with lookback time following approximately the prescriptions of AM models and the observed mass-size relation of bright spirals, leading to a weak TFR evolution consistent with observation out to z = 1. ΛCDM models that match both the abundance and size of galaxies as a function of stellar mass have no difficulty reproducing the observed TFR and its evolution. | [
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-0.035... | 11.191223 | 6.156008 | 2016-07-01 | 45 | 2017MNRAS.464.4736F | [
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"the galaxy stellar mass function",
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"size",
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... | [
"Galaxy: formation",
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"Astrophysics - Astrophysics of Galaxies"
] | 16 | [
"10.1093/mnras/stw2691",
"10.48550/arXiv.1607.03100"
] | [
"Ferrero, Ismael",
"Navarro, Julio F.",
"Abadi, Mario G.",
"Sales, Laura V.",
"Bower, Richard G.",
"Crain, Robert A.",
"Frenk, Carlos S.",
"Schaller, Matthieu",
"Schaye, Joop",
"Theuns, Tom"
] | [
"Instituto de Astronomía Teórica y Experimental, CONICET-UNC, Laprida 854, X5000BGR, Córdoba, Argentina; Observatorio Astronómico de Córdoba, Universidad Nacional de Córdoba, Laprida 854, X5000BGR, Córdoba, Argentina",
"Department of Physics and Astronomy, University of Victoria, Victoria, BC V8P 5C2, Canada",
... | [
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12465617 | 1607.01105 | Using the PPML approach for constructing a low-dissipation, operator-splitting scheme for numerical simulations of hydrodynamic flows | An approach for constructing a low-dissipation numerical method is described. The method is based on a combination of the operator-splitting method, Godunov method, and piecewise-parabolic method on the local stencil. Numerical method was tested on a standard suite of hydrodynamic test problems. In addition, the performance of the method is demonstrated on a global test problem showing the development of a spiral structure in a gravitationally unstable gaseous galactic disk. | [
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0.0... | 8.939051 | 4.610072 | 2016-07-01 | 18 | 2016JCoPh.317..318K | [
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"a low-dissipation numerical method",
"the operator-splitting method",
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"... | [
"Computational astrophysics",
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"Operator-splitting methods",
"Piecewise-parabolic method on the local stencil",
"Astrophysics - Instrumentation and Methods for Astrophysics",
"Astrophysics - Astrophysics of Galaxies"
] | 7 | [
"10.1016/j.jcp.2016.04.057",
"10.48550/arXiv.1607.01105"
] | [
"Kulikov, Igor",
"Vorobyov, Eduard"
] | [
"Institute of Computational Mathematics and Mathematical Geophysics SB RAS, Prospect Akademika Lavrentjeva, 6, Novosibirsk, 630090, Russia",
"Department of Astrophysics, University of Vienna, Turkenschanzstrasse, 17, Vienna, 1180, Austria"
] | [
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2944614 | 1607.08738 | Spectroscopic Characterisation of CARMENES Target Candidates from FEROS, CAFE and HRS High-Resolution Spectra | CARMENES (Calar Alto high-Resolution search for M dwarfs with Exoearths with Near-infrared and optical Échelle Spectrographs) started a new planet survey on M-dwarfs in January this year. The new high-resolution spectrographs are operating in the visible and near-infrared at Calar Alto Observatory. They will perform high-accuracy radial-velocity measurements (goal 1 m s-1) of about 300 M-dwarfs with the aim to detect low-mass planets within habitable zones. We characterised the candidate sample for CARMENES and provide fundamental parameters for these stars in order to constrain planetary properties and understand star-planet systems. Using state-of-the-art model atmospheres (PHOENIX-ACES) and χ2-minimization with a downhill-simplex method we determine effective temperature, surface gravity and metallicity [Fe/H] for high-resolution spectra of around 480 stars of spectral types M0.0-6.5V taken with FEROS, CAFE and HRS. We find good agreement between the models and our observed high-resolution spectra. We show the performance of the algorithm, as well as results, parameter and spectral type distributions for the CARMENES candidate sample, which is used to define the CARMENES target sample. We also present first preliminary results obtained from CARMENES spectra. | [
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-... | 7.398715 | 12.717311 | 2016-07-01 | 0 | 2016csss.confE.109P | [
"spectral type distributions",
"habitable zones",
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"spectral types",
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"CARMENES",
"m",
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"surface gravity",
"Échelle Spectrographs",
"HRS",
"effective temperature",
"fundamental parameters",
"planetary properties",
"star-planet syst... | [
"Zenodo community cs19",
"Astrophysics - Solar and Stellar Astrophysics"
] | 5 | [
"10.5281/zenodo.59007",
"10.48550/arXiv.1607.08738"
] | [
"Passegger, Vera Maria",
"Reiners, Ansgar",
"Jeffers, Sandra V.",
"Wende, Sebastian",
"Schöfer, Patrick",
"Amado, Pedro J.",
"Caballero, Jose A.",
"Montes, David",
"Mundt, Reinhard",
"Ribas, Ignasi",
"Quirrenbach, Andreas"
] | [
"Institut für Astrophysik, Georg-August-Universität Göttingen",
"Institut für Astrophysik, Georg-August-Universität Göttingen",
"Institut für Astrophysik, Georg-August-Universität Göttingen",
"Institut für Astrophysik, Georg-August-Universität Göttingen",
"Institut für Astrophysik, Georg-August-Universität ... | null | [
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] |
12472778 | 1607.05795 | The anatomy of a star-forming galaxy: pressure-driven regulation of star formation in simulated galaxies | We explore the regulation of star formation in star-forming galaxies through a suite of high-resolution isolated galaxy simulations. We use the smoothed particle hydrodynamics code GASOLINE, including photoelectric heating and metal cooling, which produces a multi-phase interstellar medium (ISM). We show that representative star formation and feedback sub-grid models naturally lead to a weak, sub-linear dependence between the amount of star formation and changes to star formation parameters. We incorporate these sub-grid models into an equilibrium pressure-driven regulation framework. We show that the sub-linear scaling arises as a consequence of the non-linear relationship between scaleheight and the effective pressure generated by stellar feedback. Thus, simulated star formation regulation is sensitive to how well vertical structure in the ISM is resolved. Full galaxy discs experience density waves which drive locally time-dependent star formation. We develop a simple time-dependent, pressure-driven model that reproduces the response extremely well. | [
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-0... | 11.714225 | 8.613326 | 2016-07-01 | 38 | 2016MNRAS.462.3053B | [
"feedback sub-grid models",
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"ISM",
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"the non-linear relationship",
"Full galaxy discs",
"metal cooling",
... | [
"methods: numerical",
"ISM: clouds",
"ISM: evolution",
"galaxies: evolution",
"galaxies: ISM",
"galaxies: star formation",
"Astrophysics - Astrophysics of Galaxies"
] | 5 | [
"10.1093/mnras/stw1741",
"10.48550/arXiv.1607.05795"
] | [
"Benincasa, S. M.",
"Wadsley, J.",
"Couchman, H. M. P.",
"Keller, B. W."
] | [
"Department of Physics and Astronomy, McMaster University, Hamilton, ON L8S 4M1, Canada",
"Department of Physics and Astronomy, McMaster University, Hamilton, ON L8S 4M1, Canada",
"Department of Physics and Astronomy, McMaster University, Hamilton, ON L8S 4M1, Canada",
"Department of Physics and Astronomy, Mc... | [
"2017ApJ...845..133S",
"2017MNRAS.468.4189P",
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12593906 | 1607.00386 | The global 21-cm signal in the context of the high- z galaxy luminosity function | We build a new model for the global 21-cm signal that is calibrated to measurements of the high-z galaxy luminosity function (LF) and further tuned to match the Thomson scattering optical depth of the cosmic microwave background, τ<SUB>e</SUB>. Assuming that the z ≲ 8 galaxy population can be smoothly extrapolated to higher redshifts, the recent decline in best-fitting values of τ<SUB>e</SUB> and the inefficient heating induced by X-ray binaries (the presumptive sources of the high-z X-ray background) imply that the entirety of cosmic reionization and reheating occurs at z ≲ 12. In contrast to past global 21-cm models, whose z ∼ 20 (ν ∼ 70 MHz) absorption features and strong ∼25 mK emission features were driven largely by the assumption of efficient early star formation and X-ray heating, our new models peak in absorption at ν ∼ 110 MHz at depths ∼-160 mK and have negligible emission components. Current uncertainties in the faint-end of the LF, binary populations in star-forming galaxies, and UV and X-ray escape fractions introduce ∼20 MHz (∼50 mK) deviations in the trough's frequency (amplitude), while emission signals remain weak (≲10 mK) and are confined to ν ≳ 140 MHz. These predictions, which are intentionally conservative, suggest that the detection of a 21-cm absorption minimum at frequencies below ∼90 MHz and/or emission signals stronger than ∼10mK at ν ≲ 140 MHz would provide strong evidence for `new' sources at high redshifts, such as Population III stars and their remnants. | [
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0... | 13.183392 | 3.472462 | 2016-07-01 | 108 | 2017MNRAS.464.1365M | [
"X-ray heating",
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"∼20 MHz",
"∼90 MHz",
"strong ∼25",
"efficient early star formation",
"UV and X-ray escape fractions",
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"galaxies: high-redshift",
"intergalactic medium",
"galaxies: luminosity function",
"mass function",
"dark ages",
"reionization",
"first stars",
"diffuse radiation",
"Astrophysics - Astrophysics of Galaxies"
] | 12 | [
"10.1093/mnras/stw2412",
"10.48550/arXiv.1607.00386"
] | [
"Mirocha, Jordan",
"Furlanetto, Steven R.",
"Sun, Guochao"
] | [
"Department of Physics and Astronomy, University of California, Los Angeles, CA 90024, USA",
"Department of Physics and Astronomy, University of California, Los Angeles, CA 90024, USA",
"Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA"
] | [
"2016ApJ...832....7A",
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12473291 | 1607.07874 | Resistive tearing instability in electron MHD: application to neutron star crusts | We study a resistive tearing instability developing in a system evolving through the combined effect of Hall drift in the electron magnetohydrodynamic limit and Ohmic dissipation. We explore first the exponential growth of the instability in the linear case and we find the fastest growing mode, the corresponding eigenvalues and dispersion relation. The instability growth rate scales as γ ∝ B<SUP>2/3</SUP>σ<SUP>-1/3</SUP>, where B is the magnetic field and σ the electrical conductivity. We confirm the development of the tearing resistive instability in the fully non-linear case, in a plane-parallel configuration where the magnetic field polarity reverses, through simulations of systems initiating in Hall equilibrium with some superimposed perturbation. Following a transient phase, during which there is some minor rearrangement of the magnetic field, the perturbation grows exponentially. Once the instability is fully developed, the magnetic field forms the characteristic islands and X-type reconnection points, where Ohmic decay is enhanced. We discuss the implications of this instability for the local magnetic field evolution in neutron stars' crusts, proposing that it can contribute to heating near the surface of the star, as suggested by models of magnetar post-burst cooling. In particular, we find that a current sheet a few metres thick, covering as little as 1 per cent of the total surface, can provide 10<SUP>42</SUP> erg in thermal energy within a few days. We briefly discuss applications of this instability in other systems where the Hall effect operates such as protoplanetary discs and space plasmas. | [
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0... | 5.069378 | 3.10706 | 2016-07-01 | 19 | 2016MNRAS.463.3381G | [
"dispersion relation",
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"space plasmas",
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"Hall equilibrium",
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"Hall",
"other systems",
"protoplanetary discs",
"the local magnetic field evolution",
"systems",
"the magnetic field polarity",
"the fast... | [
"magnetic fields",
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"methods: numerical",
"stars: magnetars",
"stars: neutron",
"Astrophysics - High Energy Astrophysical Phenomena",
"Astrophysics - Solar and Stellar Astrophysics",
"Physics - Plasma Physics"
] | 4 | [
"10.1093/mnras/stw2309",
"10.48550/arXiv.1607.07874"
] | [
"Gourgouliatos, Konstantinos N.",
"Hollerbach, Rainer"
] | [
"Department of Applied Mathematics, University of Leeds, Leeds LS2 9JT, UK",
"Department of Applied Mathematics, University of Leeds, Leeds LS2 9JT, UK"
] | [
"2017AstL...43..624K",
"2018A&G....59e5.37G",
"2018ASSL..457...57G",
"2018ApJ...852...21G",
"2018EPJA...54..191H",
"2019AN....340..475K",
"2019MNRAS.486.4130L",
"2019PASP..131e4201W",
"2019PhRvR...1c2049G",
"2019RPPh...82j6901E",
"2020MNRAS.495.1692G",
"2020arXiv200103335G",
"2021JPlPh..87d9... | [
"1932ZPhy...74..295B",
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"1985RPPh...48..955P",
"1986PhFl...29..512M",
"1988MNRAS.233..875J",
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12510816 | 1607.05040 | Effective theory for electroweak doublet dark matter | We perform a detailed study of an effective field theory which includes the standard model particle content extended by a pair of Weyl fermionic SU(2) doublets with opposite hypercharges. A discrete symmetry guarantees that a linear combination of the doublet components is stable and can act as a candidate particle for dark matter. The dark sector fermions interact with the Higgs and gauge bosons through renormalizable d =4 operators, and nonrenormalizable d =5 operators that appear after integrating out extra degrees of freedom above the TeV scale. We study collider, cosmological and astrophysical probes for this effective theory of dark matter. We find that a weakly interacting dark matter particle with a mass nearby the electroweak scale, and thus observable at the LHC, is consistent with collider and astrophysical data only when fairly large magnetic dipole moment transition operators with the gauge bosons exist, together with moderate Yukawa interactions. | [
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-0.0... | 8.523992 | -1.606507 | 2016-07-01 | 10 | 2016PhRvD..94i5008D | [
"opposite hypercharges",
"gauge bosons",
"moderate Yukawa interactions",
"dark matter",
"fairly large magnetic dipole moment transition operators",
"Weyl fermionic SU(2",
"extra degrees",
"collider and astrophysical data",
"TeV",
"the standard model particle content",
"freedom",
"Yukawa",
"t... | [
"High Energy Physics - Phenomenology",
"Astrophysics - Cosmology and Nongalactic Astrophysics"
] | 5 | [
"10.1103/PhysRevD.94.095008",
"10.48550/arXiv.1607.05040"
] | [
"Dedes, A.",
"Karamitros, D.",
"Spanos, V. C."
] | [
"Department of Physics, Division of Theoretical Physics, University of Ioannina, GR 45110 Ioannina, Greece",
"Department of Physics, Division of Theoretical Physics, University of Ioannina, GR 45110 Ioannina, Greece",
"Section of Nuclear & Particle Physics, Department of Physics, National and Kapodistrian U... | [
"2017JHEP...03..025N",
"2017JHEP...09..160B",
"2017PhRvD..95k5037D",
"2017PhRvD..96k5006C",
"2017arXiv170310916K",
"2018PhRvD..98i5003B",
"2019PhRvD..99i5036K",
"2021JHEP...07..081C",
"2022PhRvD.106e5031F",
"2023PhRvD.108k6023C"
] | [
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"1997PhRvD..56.1... |
3829677 | 1607.05089 | Absolute kinematics of radio-source components in the complete S5 polar cap sample. IV. Proper motions of the radio cores over a decade and spectral properties | We have carried out a high-precision astrometric analysis of two very-long-baseline-interferometry (VLBI) epochs of observation of the 13 extragalactic radio sources in the complete S5 polar cap sample. The VLBI epochs span a time baseline of ten years and enable us to achieve precisions in the proper motions of the source cores up to a few micro-arcseconds per year. The observations were performed at 14.4 GHz and 43.1 GHz, and enable us to estimate the frequency core-shifts in a subset of sources, for which the spectral-index distributions can be computed. We study the source-position stability by analysing the changes in the relative positions of fiducial source points (the jet cores) over a decade. We find motions of 0.1-0.9 mas among close-by sources between the two epochs, which imply drifts in the jet cores of approximately a few tens of μas per year. These results have implications for the standard Active Galactic Nucleus (AGN) jet model (where the core locations are supposed to be stable in time). For one of our sources, 0615+820, the morphological and spectral properties in year 2010, as well as the relative astrometry between years 2000 and 2010, suggest the possibility of either a strong parsec-scale interaction of the AGN jet with the ISM, a gravitational lens with 1 mas diameter, or a resolved massive binary black hole. <P />Reduced images as FITS files are only available at the CDS via anonymous ftp to <A href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A> (<A href="http://130.79.128.5">http://130.79.128.5</A>) or via <A href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/596/A27">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/596/A27</A> | [
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... | 15.580625 | 5.351726 | 2016-07-01 | 6 | 2016A&A...596A..27M | [
"year",
"years",
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"sources",
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"anonymous ftp",
"a resolved massive binary black hole",
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"the jet cores",
"Active Galactic Nucleus",
"the AGN jet",
"the complete S5 polar cap sample",
"ten years",
"year 2010",
"motions",
"ISM",
"μa... | [
"astrometry",
"quasars: general",
"techniques: interferometric",
"BL Lacertae objects: general",
"radio continuum: general",
"Astrophysics - Astrophysics of Galaxies",
"Astrophysics - Instrumentation and Methods for Astrophysics"
] | 4 | [
"10.1051/0004-6361/201628149",
"10.48550/arXiv.1607.05089"
] | [
"Martí-Vidal, I.",
"Abellán, F. J.",
"Marcaide, J. M.",
"Guirado, J. C.",
"Pérez-Torres, M. A.",
"Ros, E."
] | [
"Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, 43992, Onsala, Sweden",
"Departament d'Astronomia i Astrofísica, Universitat de València, C/Dr. Moliner 50, 46100, Burjassot, Spain",
"Departament d'Astronomia i Astrofísica, Universitat de València, C/Dr. Moli... | [
"2017A&A...598L...1K",
"2017ApJ...841..119L",
"2017NewAR..79...85D",
"2018A&A...614A..74A",
"2019SCPMA..6269511C",
"2020A&ARv..28....6R"
] | [
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"2004AJ....127.3587F",
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12408911 | 1607.03982 | Galaxy Groups in the 2Mass Redshift Survey | A galaxy group catalog is constructed from the 2MASS Redshift Survey (2MRS) with the use of a halo-based group finder. The halo mass associated with a group is estimated using a “GAP” method based on the luminosity of the central galaxy and its gap with other member galaxies. Tests using mock samples show that this method is reliable, particularly for poor systems containing only a few members. On average, 80% of all the groups have completeness \gt 0.8, and about 65% of the groups have zero contamination. Halo masses are estimated with a typical uncertainty of ∼ 0.35 {dex}. The application of the group finder to the 2MRS gives 29,904 groups from a total of 43,246 galaxies at z≤slant 0.08, with 5286 groups having two or more members. Some basic properties of this group catalog is presented, and comparisons are made with other group catalogs in overlap regions. With a depth to z∼ 0.08 and uniformly covering about 91% of the whole sky, this group catalog provides a useful database to study galaxies in the local cosmic web, and to reconstruct the mass distribution in the local universe. | [
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... | 12.206766 | 5.244895 | 2016-07-01 | 26 | 2016ApJ...832...39L | [
"other member galaxies",
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"this group catalog",
"overlap regions",
"the central galaxy",
"Redshift Survey",
"the group finder",
"the local cosmic web",
"a halo-based group finder",
"43,246 galaxies",
"poor systems",
"29,904 group... | [
"dark matter",
"galaxies: halos",
"large-scale structure of universe",
"methods: statistical",
"Astrophysics - Astrophysics of Galaxies",
"Astrophysics - Cosmology and Nongalactic Astrophysics"
] | 10 | [
"10.3847/0004-637X/832/1/39",
"10.48550/arXiv.1607.03982"
] | [
"Lu, Yi",
"Yang, Xiaohu",
"Shi, Feng",
"Mo, H. J.",
"Tweed, Dylan",
"Wang, Huiyuan",
"Zhang, Youcai",
"Li, Shijie",
"Lim, S. H."
] | [
"Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Nandan Road 80, Shanghai 200030, China",
"Center for Astronomy and Astrophysics, Shanghai Jiao Tong University, Shanghai 200240, China ; IFSA Collaborative Innovation Center, Shanghai Jiao Tong University, Shanghai 200240, ... | [
"2017MNRAS.470.2982L",
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"2018ApJ...858..110P",
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"2020MNRAS.494.2090J",
"2020MNRAS.496.2516M",
"2020MNRAS.497.2954L",
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"1998ApJ...494....1J",
"1999MNRAS.304..175M",
"2000AJ....119.2498J",
"2000MNRAS.318.1... |
12436396 | 1607.06105 | A Monodromy from London | We focus on the massive gauge theory formulation of axion monodromy inflation. We argue that a gauge symmetry hidden in these models is the key protection mechanism from dangerous corrections from both field theory and gravitational dynamics. The effective theory of large field inflation is a dual to a massive U(1) 4-form gauge theory, which is similar to a massive gauge theory description of superconductivity. The gauge theory explicitly realizes the old Julia-Toulouse proposal for a low energy description of a gauge theory in a defect condensate. While we work mostly with the example of quadratic axion potential induced by flux monodromy, we discuss how other types of potentials can arise from inclusion of gauge invariant corrections to the theory. | [
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... | 10.572262 | -1.467464 | 2016-07-01 | 17 | 2016arXiv160706105K | [
"gauge invariant corrections",
"axion monodromy inflation",
"a massive gauge theory description",
"the massive gauge theory formulation",
"large field inflation",
"dangerous corrections",
"gravitational dynamics",
"quadratic axion potential",
"The gauge theory",
"a gauge theory",
"flux monodromy... | [
"High Energy Physics - Theory",
"Astrophysics - Cosmology and Nongalactic Astrophysics",
"General Relativity and Quantum Cosmology",
"High Energy Physics - Phenomenology"
] | 2 | [
"10.48550/arXiv.1607.06105"
] | [
"Kaloper, Nemanja",
"Lawrence, Albion"
] | [
"-",
"-"
] | [
"2016arXiv161005320M",
"2017JHEP...02..097H",
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"2018JHEP...06..006K",
"2018JHEP...10..146N",
"2018JHEP...12..032M",
"2019JHEP...05..065D",
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"2005hep.th....7215D",
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12583815 | 1607.08610 | Bouncing cosmology inspired by regular black holes | In this article, we present a bouncing cosmology inspired by a family of regular black holes. This scale-dependent cosmology deviates from the cosmological principle by means of a scale factor which depends on the time and the radial coordinate as well. The model is isotropic but not perfectly homogeneous. That is, this cosmology describes a universe almost homogeneous only for large scales, such as our observable universe. | [
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"large scales",
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"our observable universe",
"means",
"a scale factor",
"the radial coordinate",
"This scale-dependent cosmology deviates",
"a universe",
"the cosmological principle",
"a bouncing cosmology",
"the time",
"this cosmology",
"a family",
"The model",
"thi... | [
"Bouncing cosmology",
"Singularity",
"Regular black holes",
"Cosmological principle",
"General Relativity and Quantum Cosmology",
"Astrophysics - Cosmology and Nongalactic Astrophysics"
] | 6 | [
"10.1007/s10714-017-2288-6",
"10.48550/arXiv.1607.08610"
] | [
"Neves, J. C. S."
] | [
"Instituto de Matemática, Estatística e Computação Científica, Universidade Estadual de Campinas, Campinas, SP, Brazil"
] | [
"2018AN....339..298N",
"2018arXiv180307995N",
"2024EPJC...84...73F"
] | [
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12509665 | 1607.01677 | Current and future constraints on Bekenstein-type models for varying couplings | Astrophysical tests of the stability of dimensionless fundamental couplings, such as the fine-structure constant α and the proton-to-electron mass ratio μ , are an optimal probe of new physics. There is a growing interest in these tests, following indications of possible spacetime variations at the few parts per million level. Here we make use of the latest astrophysical measurements, combined with background cosmological observations, to obtain improved constraints on Bekenstein-type models for the evolution of both couplings. These are arguably the simplest models allowing for α and μ variations, and are characterized by a single free dimensionless parameter, ζ , describing the coupling of the underlying dynamical degree of freedom to the electromagnetic sector. In the former case we find that this parameter is constrained to be |ζ<SUB>α</SUB>|<4.8 ×10<SUP>-6</SUP> (improving previous constraints by a factor of 6), while in the latter (which we quantitatively compare to astrophysical measurements for the first time) we find ζ<SUB>μ</SUB>=(2.7 ±3.1 )×10<SUP>-7</SUP> ; both of these are at the 99.7% confidence level. For ζ<SUB>α</SUB> this constraint is about 20 times stronger than the one obtained from local weak equivalence principle tests, while for ζ<SUB>μ</SUB> it is about 2 orders of magnitude weaker. We also discuss the improvements on these constraints to be expected from the forthcoming ESPRESSO and ELT-HIRES spectrographs, conservatively finding a factor of around 5 for the former and around 50 for the latter. | [
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0... | 9.209813 | 0.311204 | 2016-07-01 | 12 | 2016PhRvD..94b3503L | [
"local weak equivalence principle tests",
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"previous constraints",
"astrophysical measurements",
"possible spacetime variations",
"ζ",
"background cosmological observations",
"electron",
"freedo... | [
"Astrophysics - Cosmology and Nongalactic Astrophysics",
"General Relativity and Quantum Cosmology",
"High Energy Physics - Phenomenology",
"High Energy Physics - Theory"
] | 3 | [
"10.1103/PhysRevD.94.023503",
"10.48550/arXiv.1607.01677"
] | [
"Leite, A. C. O.",
"Martins, C. J. A. P."
] | [
"Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal; Instituto de Astrofísica e Ciências do Espaço, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal; Faculdade de Ciências, Universidade do Porto, Rua do Campo Alegre, 4150-007 Porto, Portugal",
"Centro de Astrofísica, Universi... | [
"2017CoTPh..68..632W",
"2017PhLB..770...93A",
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12593997 | 1607.01394 | Merger-driven evolution of the effective stellar initial mass function of massive early-type galaxies | The stellar initial mass function (IMF) of early-type galaxies is the combination of the IMF of the stellar population formed in situ and that of accreted stellar populations. Using as an observable the effective IMF α<SUB>IMF</SUB>, defined as the ratio between the true stellar mass of a galaxy and the stellar mass inferred assuming a Salpeter IMF, we present a theoretical model for its evolution as a result of dry mergers. We use a simple dry-merger evolution model, based on cosmological N-body simulations, together with empirically motivated prescriptions for the IMF to make predictions on how the effective IMF of massive early-type galaxies changes from z = 2 to z = 0. We find that the IMF normalization of individual galaxies becomes lighter with time. At fixed velocity dispersion, α<SUB>IMF</SUB> is predicted to be constant with redshift. Current dynamical constraints on the evolution of the IMF are in slight tension with this prediction, even though systematic uncertainties, including the effect of radial gradients in the IMF, prevent a conclusive statement. The correlation of α<SUB>IMF</SUB> with stellar mass becomes shallower with time, while the correlation between α<SUB>IMF</SUB> and velocity dispersion is mostly preserved by dry mergers. We also find that dry mergers can mix the dependence of the IMF on stellar mass and velocity dispersion, making it challenging to infer, from z = 0 observations of global galactic properties, what is the quantity that is originally coupled with the IMF. | [
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"IMF",
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"accreted stellar populations",
"dry mergers",
"individual galaxies",
"stellar mass and velocity dispersion",
"global galactic properties",
"The stellar initial mass function",
"IMF</SUB",
"fixed velocity dispersion",
"the true stellar mass",
"z",
"a Salpeter IMF",
"... | [
"stars: luminosity function",
"mass function",
"galaxies: elliptical and lenticular",
"cD",
"galaxies: evolution",
"galaxies: stellar content",
"Astrophysics - Astrophysics of Galaxies",
"Astrophysics - Cosmology and Nongalactic Astrophysics"
] | 3 | [
"10.1093/mnras/stw2919",
"10.48550/arXiv.1607.01394"
] | [
"Sonnenfeld, Alessandro",
"Nipoti, Carlo",
"Treu, Tommaso"
] | [
"Kavli IPMU (WPI), UTIAS, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan; Department of Physics and Astronomy, University of California, Los Angeles, 430 Portola Plaza, Los Angeles, CA 90025, USA",
"Department of Physics and Astronomy, Bologna University, viale Berti-Pichat 6/2, I-40127 Bologna, Italy",
... | [
"2017A&A...600L...3C",
"2017ApJ...841...68V",
"2017ApJ...845..136B",
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"2018MNRAS.475.2878S",
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"2018PASA...35...39H",
"2020MNRAS.499..559N",
"2021MNRAS.500.4153L",
"2022MNRAS.513.3893M",
"2023MNRAS.520.5... | [
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"2010ARA&A..48..339B",
"2010ApJ...709.1... |
12473435 | 1607.04264 | Evidence for the magnetar nature of 1E 161348-5055 in RCW 103 | We report on the detection of a bright, short, structured X-ray burst coming from the supernova remnant RCW 103 on 2016 June 22 caught by the Swift/Burst Alert Telescope (BAT) monitor, and on the follow-up campaign made with Swift/X-ray Telescope, Swift/UV/Optical Telescope, and the optical/near-infrared (NIR) Gamma-Ray burst Optical and Near-infrared Detector. The characteristics of this flash, such as duration and spectral shape, are consistent with typical short bursts observed from soft gamma repeaters. The BAT error circle at 68 per cent confidence range encloses the point-like X-ray source at the centre of the nebula, 1E 161348-5055. Its nature has been long debated due to a periodicity of 6.67 h in X-rays, which could indicate either an extremely slow pulsating neutron star, or the orbital period of a very compact X-ray binary system. We found that 20 min before the BAT trigger, the soft X-ray emission of 1E 161348-5055 was a factor of ∼100 higher than measured 2 yr earlier, indicating that an outburst had already started. By comparing the spectral and timing characteristics of the source in the 2 yr before the outburst and after the BAT event, we find that, besides a change in luminosity and spectral shape, also the 6.67 h pulsed profile has significantly changed with a clear phase shift with respect to its low-flux profile. The UV/optical/NIR observations did not reveal any counterpart at the position of 1E 161348-5055. Based on these findings, we associate the BAT burst with 1E 161348-5055, we classify it as a magnetar, and pinpoint the 6.67 h periodicity as the magnetar spin period. | [
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... | 5.192254 | 4.426284 | 2016-07-01 | 55 | 2016MNRAS.463.2394D | [
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"X-rays: general",
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] | 11 | [
"10.1093/mnras/stw2023",
"10.48550/arXiv.1607.04264"
] | [
"D'Aì, A.",
"Evans, P. A.",
"Burrows, D. N.",
"Kuin, N. P. M.",
"Kann, D. A.",
"Campana, S.",
"Maselli, A.",
"Romano, P.",
"Cusumano, G.",
"La Parola, V.",
"Barthelmy, S. D.",
"Beardmore, A. P.",
"Cenko, S. B.",
"De Pasquale, M.",
"Gehrels, N.",
"Greiner, J.",
"Kennea, J. A.",
"Klo... | [
"INAF/IASF Palermo, via Ugo La Malfa 153, I-90146 Palermo, Italy",
"Department of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, UK",
"Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA",
"Mullard Space Science Laboratory,... | [
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12464691 | 1607.02442 | The tau of galaxy clusters | The recent emergence of detections of the kinetic Sunyeav-Zel'dovich (kSZ) effect through cross-correlation techniques is encouraging for the prospects of future cosmic microwave background (CMB) experiments. Extracting information on the large-scale velocity fields and constraining cosmological parameters from such kSZ measurements requires an understanding of the optical depth to CMB photons through halos. Using cosmological hydrodynamic simulations we find that there exists a low-scatter relation between the optical depth and thermal Sunyeav-Zel'dovich (tSZ) signal of halos within a physical aperture. We propose that such a relation can be used to break the degeneracy between optical depth and line-of-sight velocity in kSZ measurements. The limiting factors in our proposal are systematic uncertainties associated with the sub-grid physics models in the simulations, which we calculate to be less than 10 percent. We discuss future observational measurements that could potentially be used to mitigate the systematic uncertainties in this scaling relation. | [
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0... | 13.300249 | 2.775191 | 2016-07-01 | 65 | 2016JCAP...08..058B | [
"optical depth",
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"halos",
"future cosmic microwave background",
"cosmological hydrodynamic simulations",
"CMB",
"systematic uncertainties",
"cosmological parameters"... | [
"Astrophysics - Cosmology and Nongalactic Astrophysics"
] | 15 | [
"10.1088/1475-7516/2016/08/058",
"10.48550/arXiv.1607.02442"
] | [
"Battaglia, N."
] | [
"Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, U.S.A."
] | [
"2016PhRvD..94d3522A",
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"2018arXiv181013423S",
"2019BAAS...51c.... | [
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12473523 | 1607.05324 | Dark matter inside early-type galaxies as function of mass and redshift | We study the behaviour of the dynamical and stellar mass inside the effective radius (r<SUB>e</SUB>) of early-type galaxies (ETGs). We use several samples of ETGs - ranging from 19 000 to 98 000 objects - from the ninth data release of the Sloan Digital Sky Survey. We consider Newtonian dynamics, different light profiles and different initial mass functions (IMF) to calculate the dynamical and stellar mass. We assume that any difference between these two masses is due to dark matter and/or a non-universal IMF. The main results for galaxies in the redshift range 0.0024 < z < 0.3500 and in the dynamical mass range 9.5 < log(M) < 12.5 are: (I) a significant part of the intrinsic dispersion of the distribution of dynamical versus stellar mass is due to redshift; (II) the difference between dynamical and stellar mass increases as a function of dynamical mass and decreases as a function of redshift; (III) the difference between dynamical and stellar mass goes from approximately 0 to 70 per cent of the dynamical mass depending on mass and redshift; (IV) these differences could be due to dark matter or a non-universal IMF or a combination of both; (v) the amount of dark matter inside ETGs would be equal to or less than the difference between dynamical and stellar mass depending on the impact of the IMF on the stellar mass estimation; (VI) the previous results go in the same direction of some results of the Fundamental Plane (FP) found in the literature in the sense that they could be interpreted as an increase of dark matter along the FP and a dependence of the FP on redshift. | [
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0.001... | 11.483376 | 6.044522 | 2016-07-01 | 7 | 2016MNRAS.462..951N | [
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"dynamical versus stellar mass",
"the dynamical mass range",
"redshift",
"the stellar mass estimation",
"the dynamical mass",
"IMF",
"lt",
"the... | [
"galaxies: elliptical and lenticular",
"cD",
"galaxies: fundamental parameters",
"dark matter",
"Astrophysics - Astrophysics of Galaxies"
] | 3 | [
"10.1093/mnras/stw1661",
"10.48550/arXiv.1607.05324"
] | [
"Nigoche-Netro, A.",
"Ramos-Larios, G.",
"Lagos, P.",
"Ruelas-Mayorga, A.",
"de la Fuente, E.",
"Kemp, S. N.",
"Navarro, S. G.",
"Corral, L. J.",
"Hidalgo-Gámez, A. M."
] | [
"Instituto de Astronomía y Meteorología, Universidad de Guadalajara, Guadalajara, Jalisco 44130, México",
"Instituto de Astronomía y Meteorología, Universidad de Guadalajara, Guadalajara, Jalisco 44130, México",
"Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, Rua das Estrelas, P-4150-762 ... | [
"2018MNRAS.473..969T",
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"2019MNRAS.488.1320N",
"2020ApJ...903...38C",
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"2022MNRAS.516.3924V"
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3458517 | 1607.03114 | V346 Normae: first post-outburst observations of an FU Orionis star | During their formation phase, stars gain most of their mass in violent episodic accretion events, such as observed in FU Orionis (FUor) and EXor stars. V346 Normae is a well-studied FUor that underwent a strong outburst beginning around 1980. Here, we report on photometric and spectroscopic observations, which show that the visual/near-infrared brightness has decreased dramatically between the 1990s and 2010 (ΔR ≈ 10.9 mag, ΔJ ≈ 7.8 mag and ΔK ≈ 5.8 mag). The spectral properties of this fading event cannot be explained by variable extinction alone, but indicate a drop in accretion rate by two to three orders of magnitude. This is the first time that a member of the FUor class has been observed to switch to a very low accretion phase. Remarkably, in the last few years (2011-2015) V346 Nor has brightened again at all near-infrared wavelengths, indicating the onset of a new outburst event. The observed behaviour might be consistent with the clustered luminosity bursts that have been predicted by recent gravitational instability and fragmentation models for the early stages of protostellar evolution. Given V346 Nor's unique characteristics (concerning outburst duration, repetition frequency and spectroscopic diagnostics), our results also highlight the need to revisit the FUor/EXor classification scheme. | [
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"accretion",
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"stars: individual: V346 Normae",
"stars: pre-main sequence",
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"Astrophysics - Solar and Stellar Astrophysics"
] | 6 | [
"10.1093/mnrasl/slw126",
"10.48550/arXiv.1607.03114"
] | [
"Kraus, S.",
"Caratti o Garatti, A.",
"Garcia-Lopez, R.",
"Kreplin, A.",
"Aarnio, A.",
"Monnier, J. D.",
"Naylor, T.",
"Weigelt, G."
] | [
"School of Physics, Astrophysics Group, University of Exeter, Stocker Road, Exeter EX4 4QL, UK",
"Dublin Institute for Advanced Studies, School of Cosmic Physics, Astronomy and Astrophysics Section, 31 Fitzwilliam Place, Dublin 2, Ireland",
"Dublin Institute for Advanced Studies, School of Cosmic Physics, Astro... | [
"2017A&A...597L..10K",
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"2019ApJ...873..130Z",
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"2019MNRAS.485.1843W",
"2020ApJ...889..148K",
"2020MNRAS.492..... | [
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1683108 | 1607.06394 | Outbursts in ultracompact X-ray binaries | Context. Very faint X-ray binaries appear to be transient in many cases with peak luminosities much fainter than that of usual soft X-ray transients, but their nature still remains elusive. <BR /> Aims: We investigate the possibility that this transient behaviour is due to the same thermal/viscous instability which is responsible for outbursts of bright soft X-ray transients, occurring in ultracompact binaries for adequately low mass-transfer rates. More generally, we investigate the observational consequences of this instability when it occurs in ultracompact binaries. <BR /> Methods: We use our code for modelling the thermal-viscous instability of the accretion disc, assumed here to be hydrogen poor. We also take into account the effects of disc X-ray irradiation, and consider the impact of the mass-transfer rate on the outburst brightness. <BR /> Results: We find that one can reproduce the observed properties of both the very faint and the brighter short transients (peak luminosity, duration, recurrence times), provided that the viscosity parameter in quiescence is slightly smaller (typically a factor of between two and four) than in bright soft X-ray transients and normal dwarf nova outbursts, the viscosity in outburst being unchanged. This possibly reflects the impact of chemical composition on non-ideal magnetohydrodynamic effects affecting magnetically driven turbulence in poorly ionized discs. | [
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... | 6.496911 | 6.344964 | 2016-07-01 | 14 | 2016A&A...594A..87H | [
"bright soft X-ray transients",
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"Very faint X-ray binaries",
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"peak luminosity",
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"outbursts",
"non-ideal magnetohydrodynamic effects",
"many cases",
... | [
"accretion",
"accretion disks",
"X-rays: binaries",
"instabilities",
"Astrophysics - High Energy Astrophysical Phenomena"
] | 3 | [
"10.1051/0004-6361/201628434",
"10.48550/arXiv.1607.06394"
] | [
"Hameury, J. -M.",
"Lasota, J. -P."
] | [
"Observatoire Astronomique de Strasbourg, Université de Strasbourg, CNRS UMR 7550, 67000, Strasbourg, France",
"Institut d'Astrophysique de Paris, CNRS et Sorbonne Universités, UPMC Paris 06, UMR 7095, 98bis Bd Arago, 75014, Paris, France; Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, Barty... | [
"2017ApJ...851..114R",
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"2020A&A...644A..63A",
"2020AdSpR..66.1004H",
"2020MNRAS.492.4344S",
"2021A&A...650A.... | [
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3221474 | 1607.01782 | Approximate Bayesian computation in large-scale structure: constraining the galaxy-halo connection | Standard approaches to Bayesian parameter inference in large-scale structure assume a Gaussian functional form (chi-squared form) for the likelihood. This assumption, in detail, cannot be correct. Likelihood free inferences such as approximate Bayesian computation (ABC) relax these restrictions and make inference possible without making any assumptions on the likelihood. Instead ABC relies on a forward generative model of the data and a metric for measuring the distance between the model and data. In this work, we demonstrate that ABC is feasible for LSS parameter inference by using it to constrain parameters of the halo occupation distribution (HOD) model for populating dark matter haloes with galaxies. Using specific implementation of ABC supplemented with population Monte Carlo importance sampling, a generative forward model using HOD and a distance metric based on galaxy number density, two-point correlation function and galaxy group multiplicity function, we constrain the HOD parameters of mock observation generated from selected 'true' HOD parameters. The parameter constraints we obtain from ABC are consistent with the 'true' HOD parameters, demonstrating that ABC can be reliably used for parameter inference in LSS. Furthermore, we compare our ABC constraints to constraints we obtain using a pseudo-likelihood function of Gaussian form with MCMC and find consistent HOD parameter constraints. Ultimately, our results suggest that ABC can and should be applied in parameter inference for LSS analyses. | [
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0.024... | 11.644382 | 3.301285 | 2016-07-01 | 44 | 2017MNRAS.469.2791H | [
"consistent HOD parameter constraints",
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"parameters",
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"galaxy number density",
"Gaussian form",
"galaxies",
"dark matter haloes",
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"free inferences",
"the HOD parameters",
"ABC",
"LSS ana... | [
"methods: data analysis",
"methods: statistical",
"galaxies: haloes",
"dark matter",
"large-scale structure of Universe",
"Astrophysics - Cosmology and Nongalactic Astrophysics"
] | 3 | [
"10.1093/mnras/stx894",
"10.48550/arXiv.1607.01782"
] | [
"Hahn, ChangHoon",
"Vakili, Mohammadjavad",
"Walsh, Kilian",
"Hearin, Andrew P.",
"Hogg, David W.",
"Campbell, Duncan"
] | [
"Center for Cosmology and Particle Physics, Department of Physics, New York University, 726 Broadway, New York, NY 10003, USA",
"Center for Cosmology and Particle Physics, Department of Physics, New York University, 726 Broadway, New York, NY 10003, USA",
"Center for Cosmology and Particle Physics, Department o... | [
"2016arXiv161204041L",
"2017A&A...605A...9C",
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1267015 | 1607.06488 | Global Energetics of Solar Flares. III. Nonthermal Energies | This study entails the third part of a global flare energetics project, in which Ramaty High-Energy Solar Spectroscopic Imager (RHESSI) data of 191 M and X-class flare events from the first 3.5 years of the Solar Dynamics Observatory mission are analyzed. We fit a thermal and a nonthermal component to RHESSI spectra, yielding the temperature of the differential emission measure (DEM) tail, the nonthermal power-law slope and flux, and the thermal/nonthermal cross-over energy e <SUB>co</SUB>. From these parameters, we calculate the total nonthermal energy E <SUB>nt</SUB> in electrons with two different methods: (1) using the observed cross-over energy e <SUB>co</SUB> as low-energy cutoff, and (2) using the low-energy cutoff e <SUB>wt</SUB> predicted by the warm thick-target bremsstrahlung model of Kontar et al. Based on a mean temperature of T <SUB> e </SUB> = 8.6 MK in active regions, we find low-energy cutoff energies of {e}<SUB>{wt</SUB>}=6.2+/- 1.6 {keV} for the warm-target model, which is significantly lower than the cross-over energies {e}<SUB>{co</SUB>}=21+/- 6 {keV}. Comparing with the statistics of magnetically dissipated energies E <SUB>mag</SUB> and thermal energies E <SUB>th</SUB> from the two previous studies, we find the following mean (logarithmic) energy ratios with the warm-target model: {E}<SUB>{nt</SUB>}=0.41 {E}<SUB>{mag</SUB>}, {E}<SUB>{th</SUB>}=0.08 {E}<SUB>{mag</SUB>}, and {E}<SUB>{th</SUB>}=0.15 {E}<SUB>{nt</SUB>}. The total dissipated magnetic energy exceeds the thermal energy in 95% and the nonthermal energy in 71% of the flare events, which confirms that magnetic reconnection processes are sufficient to explain flare energies. The nonthermal energy exceeds the thermal energy in 85% of the events, which largely confirms the warm thick-target model. | [
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0.044347... | 13.258176 | 15.646975 | 2016-07-01 | 58 | 2016ApJ...832...27A | [
"thermal energies",
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"energy",
"low-energy cutoff energies",
"SUB",
"low-energy cutoff",
"Kontar et al",
"The nonthermal energy",
"the nonthermal energy",
"the thermal energy",
"The total dissipated magnetic energy",
"the total nonthermal energy E <SUB",
"magne... | [
"radiation mechanisms: nonthermal",
"Sun: flares",
"Sun: particle emission",
"Sun: X-rays",
"gamma rays",
"Astrophysics - Solar and Stellar Astrophysics"
] | 8 | [
"10.3847/0004-637X/832/1/27",
"10.48550/arXiv.1607.06488"
] | [
"Aschwanden, Markus J.",
"Holman, Gordon",
"O'Flannagain, Aidan",
"Caspi, Amir",
"McTiernan, James M.",
"Kontar, Eduard P."
] | [
"Lockheed Martin, Solar and Astrophysics Laboratory, Org. A021S, Bldg. 252, 3251 Hanover Street, Palo Alto, CA 94304, USA",
"Code 671, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA",
"Astrophysics Research Group, School of Physics, Trinity College Dublin, Dublin 2, Ireland",
"Planetary Science Di... | [
"2017Ap&SS.362..113F",
"2017ApJ...836...17A",
"2017ApJ...841..124V",
"2017ApJ...847...27A",
"2017ApJ...847...84F",
"2017ApJ...848..116B",
"2017AstL...43..614G",
"2017Ge&Ae..57..916T",
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"2017IAUS..327...94D",
"2017MNRAS.471.4677K",
"2017arXiv170100619C",
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12594329 | 1607.05442 | Density and metallicity of the Milky Way circumgalactic gas | The halo of the Milky Way circumgalactic gas extends up to the virial radius of the Galaxy, ∼250 kpc. The halo properties may be deduced from X-ray spectroscopic observations and from studies of the ram-pressure stripping of satellite dwarf galaxies. The former method is more precise, but its results depend crucially on the assumed metallicity of the circumgalactic gas; the latter one does not need these assumptions. Here, the information from both approaches is combined to constrain observationally the gas metallicity and density as functions of the galactocentric distance. It is demonstrated that the two kinds of data could be reconciled if the metallicity decreased to Z ∼ 0.1 Z<SUB>⊙</SUB> in the outer parts of the extended halo. The corresponding gas density profile is rather flat, falling as r<SUP>-(0.45-0.75)</SUP> at large galactocentric distances r. | [
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... | 12.595534 | 8.25086 | 2016-07-01 | 7 | 2017MNRAS.468L..36T | [
"satellite dwarf galaxies",
"large galactocentric distances",
"r.",
"X-ray spectroscopic observations",
"the Milky Way circumgalactic gas",
"∼250",
"studies",
"Galaxy",
"the galactocentric distance",
"The corresponding gas density profile",
"density",
"the gas metallicity",
"r",
"the circu... | [
"ISM: structure",
"Galaxy: halo",
"Galaxy: structure",
"Astrophysics - Astrophysics of Galaxies",
"Astrophysics - High Energy Astrophysical Phenomena"
] | 6 | [
"10.1093/mnrasl/slx022",
"10.48550/arXiv.1607.05442"
] | [
"Troitsky, Sergey"
] | [
"Institute for Nuclear Research of the Russian Academy of Sciences, 60th October Anniversary prospect 7a, 117312 Moscow, Russia; Moscow Institute for Physics and Technology, Institutskii per. 9, 141700 Dolgoprudny, Moscow Region, Russia"
] | [
"2016PhRvD..94f3013K",
"2017MNRAS.467.3544S",
"2018JCAP...07..063B",
"2020ApJ...894....1F",
"2022MNRAS.511..843M",
"2023MNRAS.524.4091B",
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] | [
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12472567 | 1607.02054 | [O III] emission line as a tracer of star-forming galaxies at high redshifts: comparison between Hα and [O III] emitters at z=2.23 in HiZELS | We investigate the properties of z = 2.23 Hα and [O III] λ5007 emitters using the narrow-band-selected samples obtained from the High-z Emission Line Survey. We construct two samples of the Hα and [O III] emitters and compare their integrated physical properties. We find that the distribution of stellar masses, dust extinction, star formation rates (SFRs), and specific SFRs (sSFRs) is not statistically different between the two samples. When we separate the full galaxy sample into three subsamples according to the detections of the Hα and/or [O III] emission lines, most of the sources detected with both Hα and [O III] show log(sSFR<SUB>UV</SUB>) ≳ -9.5. The comparison of the three subsamples suggests that sources with strong [O III] line emission tend to have the highest star-forming activity out all galaxies that we study. We argue that the [O III] emission line can be used as a tracer of star-forming galaxies at high redshift, and that it is especially useful to investigate star-forming galaxies at z > 3, for which Hα emission is no longer observable from the ground. | [
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0.00... | 12.829719 | 7.016621 | 2016-07-01 | 24 | 2016MNRAS.462..181S | [
"Hα emission",
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"star formation rates",
"high redshift",
"specific SFRs",
"star-forming galaxies",
"strong [O III] line emission",
"[O III",
"SFRs",
"UV</SUB",
"the full galaxy sample",
"emitters",
"the High-z Emission Line Survey",
"the highest star-forming activity",
"... | [
"galaxies: evolution",
"galaxies: high-redshift",
"Astrophysics - Astrophysics of Galaxies"
] | 6 | [
"10.1093/mnras/stw1655",
"10.48550/arXiv.1607.02054"
] | [
"Suzuki, T. L.",
"Kodama, T.",
"Sobral, D.",
"Khostovan, A. A.",
"Hayashi, M.",
"Shimakawa, R.",
"Koyama, Y.",
"Tadaki, K. -i.",
"Tanaka, I.",
"Minowa, Y.",
"Yamamoto, M.",
"Smail, I.",
"Best, P. N."
] | [
"Department of Astronomical Science, SOKENDAI (The Graduate University for Advanced Studies), Mitaka, Tokyo 181-8588, Japan; Optical and Infrared Astronomy Division, National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan",
"Department of Astronomical Science, SOKENDAI (The Graduate University f... | [
"2017ApJ...849...39S",
"2018AAS...23132805K",
"2018ApJ...858...96C",
"2018ApJ...859...38N",
"2018MNRAS.475.1587S",
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"2019sf2a.conf..115V",
"2020A&A...635A..35B",
"2020ApJ...895....9O",
"2020ApJ...904..... | [
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"2000ApJ...533..682C",
"2000MNRAS.312..813S",
"2002PASJ...54..... |
12409154 | 1607.07447 | Complete Element Abundances of Nine Stars in the r-process Galaxy Reticulum II | We present chemical abundances derived from high-resolution Magellan/Magellan Inamori Kyocera Echelle spectra of the nine brightest known red giant members of the ultra-faint dwarf galaxy Reticulum II (Ret II). These stars span the full metallicity range of Ret II (-3.5 < [Fe/H] < -2). Seven of the nine stars have extremely high levels of r-process material ([Eu/Fe] ∼ 1.7), in contrast to the extremely low neutron-capture element abundances found in every other ultra-faint dwarf galaxy studied to date. The other two stars are the most metal-poor stars in the system ([Fe/H] < -3), and they have neutron-capture element abundance limits similar to those in other ultra-faint dwarf galaxies. We confirm that the relative abundances of Sr, Y, and Zr in these stars are similar to those found in r-process halo stars, but they are ∼0.5 dex lower than the solar r-process pattern. If the universal r-process pattern extends to those elements, the stars in Ret II display the least contaminated known r-process pattern. The abundances of lighter elements up to the iron peak are otherwise similar to abundances of stars in the halo and in other ultra-faint dwarf galaxies. However, the scatter in abundance ratios is large enough to suggest that inhomogeneous metal mixing is required to explain the chemical evolution of this galaxy. The presence of low amounts of neutron-capture elements in other ultra-faint dwarf galaxies may imply the existence of additional r-process sites besides the source of r-process elements in Ret II. Galaxies like Ret II may be the original birth sites of r-process enhanced stars now found in the halo. <P />This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. | [
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0.... | 7.951599 | 8.825322 | 2016-07-01 | 158 | 2016ApJ...830...93J | [
"other ultra-faint dwarf galaxies",
"Ret II",
"Reticulum II",
"Galaxies",
"every other ultra-faint dwarf galaxy",
"r-process halo stars",
"stars",
"r-process enhanced stars",
"r-process elements",
"known r-process pattern",
"lighter elements",
"additional r-process sites",
"r-process materia... | [
"galaxies: dwarf",
"galaxies: individual: Ret II",
"Local Group",
"nuclear reactions",
"nucleosynthesis",
"abundances",
"stars: abundances",
"Astrophysics - Astrophysics of Galaxies",
"Astrophysics - Solar and Stellar Astrophysics"
] | 26 | [
"10.3847/0004-637X/830/2/93",
"10.48550/arXiv.1607.07447"
] | [
"Ji, Alexander P.",
"Frebel, Anna",
"Simon, Joshua D.",
"Chiti, Anirudh"
] | [
"Department of Physics and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA ; Joint Institute for Nuclear Astrophysics—Center for Evolution of the Elements, East Lansing, MI:48824, USA;",
"Department of Physics and Kavli Institute for Astrophysic... | [
"2016ApJ...832..149B",
"2016ApJ...832L...3J",
"2017A&A...604A.128D",
"2017A&A...606A.112S",
"2017A&A...608A..46R",
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"2017ApJ...842...24J",
"2017ApJ...850..179C",
"2017MNRAS.466.2... | [
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"1995MNRAS.277.1354I",
"1996ApJ...466L.109W",
"2000ApJ...530..783W",
"2000ApJ...544..302B",
"2001ApJ...548..592S",
"2002A&A...387..... |
5170993 | 1607.02781 | Infrared Observations of the Quintuplet Proper Members using SOFIA/FORCAST and Gemini/TReCS | Since their discovery, the Quintuplet proper members (QPMs) have been somewhat mysterious in nature. Originally dubbed the “cocoon stars” due to their cool featureless spectra, high-resolution near-infrared imaging observations have shown that at least two of the objects exhibit “pinwheel” nebulae consistent with binary systems with a carbon-rich Wolf-Rayet star and O/B companion. In this paper, we present 19.7, 25.2, 31.5, and 37.1 μm observations of the QPMs (with an angular resolution of 3.2″-3.8″) taken with the Faint Object Infrared Camera for the SOFIA Telescope (FORCAST) in conjunction with high-resolution (∼0.1″-0.2″) images at 8.8 and 11.7 μm from the Thermal-Region Camera Spectrograph (TReCS). DUSTY models of the thermal dust emission of two of the four detected QPMs, Q2 and Q3, are fitted by radial density profiles that are consistent with constant mass-loss rates ({ρ }<SUB>d</SUB>\propto {r}<SUP>-2</SUP>). For the two remaining sources, Q1 and Q9, extended structures (∼1″) are detected around these objects in high-resolution imaging data. Based on the fitted dust masses, Q9 has an unusually large dust reservoir ({M}<SUB>{{d</SUB>}}={1.3}<SUB>-0.4</SUB><SUP>+0.8</SUP>× {10}<SUP>-3</SUP>{M}<SUB>⊙ </SUB>) compared to typical dusty Wolf-Rayet stars, which suggests that it may have recently undergone an episode of enhanced mass loss. | [
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-... | 8.697518 | 8.321824 | 2016-07-01 | 5 | 2016ApJ...827..136H | [
"enhanced mass loss",
"r}<SUP>-2</SUP",
"high-resolution imaging data",
"typical dusty Wolf-Rayet stars",
"binary systems",
"radial density profiles",
"TReCS",
"constant mass-loss rates",
"the Faint Object Infrared Camera",
"conjunction",
"nature",
"extended structures",
"∼0.1″-0.2″",
"QPM... | [
"Galaxy: center",
"stars: evolution",
"stars: massive",
"stars: Wolf-Rayet",
"Astrophysics - Astrophysics of Galaxies",
"Astrophysics - Solar and Stellar Astrophysics"
] | 4 | [
"10.3847/0004-637X/827/2/136",
"10.48550/arXiv.1607.02781"
] | [
"Hankins, M. J.",
"Lau, R. M.",
"Morris, M. R.",
"Sanchez-Bermudez, J.",
"Pott, J. U.",
"Adams, J. D.",
"Herter, T. L."
] | [
"Astronomy Department, 202 Space Sciences Building, Cornell University, Ithaca, NY 14853-6801, USA",
"Astronomy Department, 202 Space Sciences Building, Cornell University, Ithaca, NY 14853-6801, USA; Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109-8099, USA... | [
"2017ApJ...845..127N",
"2020ApJ...894...55H",
"2020ApJ...898...74L",
"2020MNRAS.496.2776H",
"2024ApJ...963..127L"
] | [
"1972JOSA...62...55R",
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"1994PASP..106.1025H",
"1998MNRAS.295..109Z",
"1999ApJ...514..202F",
"1999Natur.398..... |
12408595 | 1607.03567 | Constraining Warm Dark Matter Mass with Cosmic Reionization and Gravitational Waves | We constrain the warm dark matter (WDM) particle mass with observations of cosmic reionization and CMB optical depth. We suggest that the gravitational waves (GWs) from stellar-mass black holes (BHs) could give a further constraint on WDM particle mass for future observations. The star formation rates (SFRs) of Population I/II (Pop I/II) and Population III (Pop III) stars are also derived. If the metallicity of the universe is enriched beyond the critical value of {Z}<SUB>{{crit</SUB>}}={10}<SUP>-3.5</SUP> {Z}<SUB>⊙ </SUB>, the star formation shifts from Pop III to Pop I/II stars. Our results show that the SFRs are quite dependent on the WDM particle mass, especially at high redshifts. Combined with the reionization history and CMB optical depth derived from the recent Planck mission, we find that the current data require the WDM particle mass to be in a narrow range of 1 {{keV}}≲ {m}<SUB>{{x</SUB>}}≲ 3 {{keV}}. Furthermore, we suggest that the stochastic gravitational wave background (SGWB) produced by stellar BHs could give a further constraint on the WDM particle mass for future observations. For {m}<SUB>{{x</SUB>}}=3 {{keV}}, with Salpeter (Chabrier) initial mass function (IMF), the SGWB from Pop I/II BHs has a peak amplitude of {{{Ω }}}<SUB>{{GW</SUB>}}≈ 2.8× {10}<SUP>-9</SUP> (5.0× {10}<SUP>-9</SUP>) at f=316{{Hz}}, while the GW radiation at f\lt 10 Hz is seriously suppressed. For {m}<SUB>{{x</SUB>}}=1 {{keV}}, the SGWB peak amplitude is the same as that for {m}<SUB>{{x</SUB>}}=1 {{keV}}, but a little lower at low frequencies. Therefore, it is hard to constrain the WDM particle mass by the SGWB from Pop I/II BHs. To assess the detectability of the GW signal, we also calculate the signal-to-noise ratios (S/N), which are {{S}}/{{N}}=37.7 (66.5) and 27 (47.7) for {m}<SUB>{{x</SUB>}}=3 {{keV}} and {m}<SUB>{{x</SUB>}}=1 {{keV}} for the Einstein Telescope with Salpeter (Chabrier) IMF, respectively. The SGWB from Pop III BHs is very dependent on the WDM particle mass, the GW strength could be an order of magnitude different, and the frequency band could be two times different for {m}<SUB>{{x</SUB>}}=1 {{keV}} and {m}<SUB>{{x</SUB>}}=3 {{keV}}. Moreover, the SGWB from Pop III BHs with {m}<SUB>{{x</SUB>}}=1 {{keV}} could be detected by the Laser Interferometer Space Antenna for one year of observation, but it cannot be detected for those with {m}<SUB>{{x</SUB>}}=3 {{keV}}. | [
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0.015... | 8.770711 | -0.721419 | 2016-07-01 | 15 | 2016ApJ...829...29T | [
"WDM particle mass",
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"future observations",
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"CMB optical depth",
"stellar BHs",
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"Population III",
"the WDM particle mass",
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... | [
"cosmology: theory",
"dark ages",
"reionization",
"first stars",
"dark matter",
"gravitational waves",
"Astrophysics - Cosmology and Nongalactic Astrophysics"
] | 6 | [
"10.3847/0004-637X/829/1/29",
"10.48550/arXiv.1607.03567"
] | [
"Tan, Wei-Wei",
"Wang, F. Y.",
"Cheng, K. S."
] | [
"School of Astronomy and Space Science, Nanjing University, Nanjing 210093, China ; Key laboratory of Modern Astronomy and Astrophysics (Nanjing University), Nanjing 210093, China;",
"School of Astronomy and Space Science, Nanjing University, Nanjing 210093, China ; Key laboratory of Modern Astronomy and Astrophy... | [
"2016Nanot..27X5602C",
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"2017ChPhB..26h8101Z",
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"2019MNRAS.489..487S",
"2019Nanot..30W5703T",
"2020JCAP...03..042B",
"2020PDU....2800476N",
"2020SeScT..35b5020S",
"2021MNRAS.506.5... | [
"1955ApJ...121..161S",
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2583156 | 1607.05732 | Setting firmer constraints on the evolution of the most massive, central galaxies from their local abundances and ages | There is still much debate surrounding how the most massive, central galaxies in the local universe have assembled their stellar mass, especially the relative roles of in situ growth versus later accretion via mergers. In this paper, we set firmer constraints on the evolutionary pathways of the most massive central galaxies by making use of empirical estimates on their abundances and stellar ages. The most recent abundance matching and direct measurements strongly favour that a substantial fraction of massive galaxies with M<SUB>star</SUB>>3 × 10<SUP>11</SUP> M<SUB>⊙</SUB> reside at the centre of clusters with mass M<SUB>halo</SUB>>3 × 10<SUP>13</SUP> M<SUB>⊙</SUB>. Spectral analysis supports ages >10 Gyr, corresponding to a formation redshift z<SUB>form</SUB>>2. We combine these two pieces of observationally based evidence with the mass accretion history of their host dark matter haloes. We find that in these massive haloes, the stellar mass locked up in the central galaxy is comparable to, if not greater than, the total baryonic mass at z<SUB>form</SUB>. These findings indicate that either only a relatively minor fraction of their present-day stellar mass was formed in situ at z<SUB>form</SUB>, or that these massive, central galaxies form in the extreme scenario where almost all of the baryons in the progenitor halo are converted into stars. Interestingly, the latter scenario would not allow for any substantial size growth since the galaxy's formation epoch either via mergers or expansion. We show our results hold irrespective of systematic uncertainties in stellar mass, abundances, galaxy merger rates, stellar initial mass function, star formation rate and dark matter accretion histories. | [
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-0.02... | 11.69136 | 6.049311 | 2016-07-01 | 13 | 2016MNRAS.462.2001B | [
"dark matter accretion histories",
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"stellar ages",
"merger rates",
"later accretion",
"mass M<SUB",
"the mass accretion history",
"mergers",
"situ growth",
"M<SUB",
"their host dark matter",
"star... | [
"galaxies: abundances",
"galaxies: evolution",
"galaxies: formation",
"galaxies: statistics",
"galaxies: structure",
"Astrophysics - Astrophysics of Galaxies",
"Astrophysics - Cosmology and Nongalactic Astrophysics"
] | 6 | [
"10.1093/mnras/stw1771",
"10.48550/arXiv.1607.05732"
] | [
"Buchan, Stewart",
"Shankar, Francesco"
] | [
"School of Physics and Astronomy, University of Southampton, Southampton SO17 1BJ, UK",
"School of Physics and Astronomy, University of Southampton, Southampton SO17 1BJ, UK"
] | [
"2017ApJ...840...34S",
"2017MNRAS.467..661N",
"2018ApJ...863...42C",
"2018MNRAS.475.2878S",
"2018MNRAS.476..705N",
"2018MNRAS.480..521H",
"2019A&A...622A..30S",
"2019MNRAS.483.2506G",
"2020MNRAS.491..634G",
"2022MNRAS.510.5639M",
"2022MNRAS.511..506C",
"2023ApJ...954...97B",
"2024MNRAS.tmp.1... | [
"1991ApJ...379...52W",
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12406183 | 1607.02975 | The faint end of the 250 μm luminosity function at z < 0.5 | <BR /> Aims: We aim to study the 250 μm luminosity function (LF) down to much fainter luminosities than achieved by previous efforts. <BR /> Methods: We developed a modified stacking method to reconstruct the 250 μm LF using optically selected galaxies from the SDSS survey and Herschel maps of the GAMA equatorial fields and Stripe 82. Our stacking method not only recovers the mean 250 μm luminosities of galaxies that are too faint to be individually detected, but also their underlying distribution functions. <BR /> Results: We find very good agreement with previous measurements in the overlapping luminosity range. More importantly, we are able to derive the LF down to much fainter luminosities (~ 25 times fainter) than achieved by previous studies. We find strong positive luminosity evolution L<SUP>*</SUP><SUB>250</SUB>(z)∝(1+z)<SUP>4.89±1.07</SUP> and moderate negative density evolution Φ<SUP>*</SUP><SUB>250</SUB>(z)∝(1+z)<SUP>-1.02±0.54</SUP> over the redshift range 0.02 <z< 0.5. | [
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... | 12.556497 | 6.26449 | 2016-07-01 | 7 | 2016A&A...592L...5W | [
"much fainter luminosities",
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"previous studies",
"previous efforts",
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"previous measurements",
"moderate negative density",
"Stripe",
"Herschel maps",
"LF",
"the overlapping luminosity range",
"evolution",
"galaxies",
"their underlying dist... | [
"submillimeter: galaxies",
"galaxies: statistics",
"methods: statistical",
"galaxies: evolution",
"galaxies: abundances",
"galaxies: luminosity function",
"mass function",
"Astrophysics - Astrophysics of Galaxies"
] | 3 | [
"10.1051/0004-6361/201629076",
"10.48550/arXiv.1607.02975"
] | [
"Wang, L.",
"Norberg, P.",
"Bethermin, M.",
"Bourne, N.",
"Cooray, A.",
"Cowley, W.",
"Dunne, L.",
"Dye, S.",
"Eales, S.",
"Farrah, D.",
"Lacey, C.",
"Loveday, J.",
"Maddox, S.",
"Oliver, S.",
"Viero, M."
] | [
"SRON Netherlands Institute for Space Research, Landleven 12, 9747 AD, Groningen, The Netherlands ; Kapteyn Astronomical Institute, University of Groningen, Postbus 800, 9700 AV, Groningen, The Netherlands; ICC & CEA, Department of Physics, Durham University, Durham, DH1 3LE, UK",
"ICC & CEA, Department o... | [
"2018A&A...615A.146P",
"2018A&A...617A..33A",
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12473475 | 1607.02144 | Black holes in stellar-mass binary systems: expiating original spin? | We investigate systematically whether accreting black hole systems are likely to reach global alignment of the black hole spin and its accretion disc with the binary plane. In low-mass X-ray binaries (LMXBs), there is only a modest tendency to reach such global alignment, and it is difficult to achieve fully: except for special initial conditions, we expect misalignment of the spin and orbital planes by ∼1 rad for most of the LMXB lifetime. The same is expected in high-mass X-ray binaries. A fairly close approach to global alignment is likely in most stellar-mass ultraluminous X-ray binary systems (ULXs) where the companion star fills its Roche lobe and transfers mass on a thermal or nuclear time-scale to a black hole of lower mass. These systems are unlikely to show orbital eclipses, as their emission cones are close to the hole's spin axis. This offers a potential observational test, as models for ULXs invoking intermediate-mass black holes do predict eclipses for ensembles of ≳ 10 systems. Recent observational work shows that eclipses are either absent or extremely rare in ULXs, supporting the picture that most ULXs are stellar-mass binaries with companion stars more massive than the accretor. | [
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0.... | 6.792903 | 6.535344 | 2016-07-01 | 14 | 2016MNRAS.462..464K | [
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"orbital eclipses",
"intermediate-mass black holes",
"most stellar-mass ultraluminous X-ray binary... | [
"accretion",
"accretion discs",
"black hole physics",
"binaries: close",
"X-rays: binaries",
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] | 5 | [
"10.1093/mnras/stw1598",
"10.48550/arXiv.1607.02144"
] | [
"King, Andrew",
"Nixon, Chris"
] | [
"Theoretical Astrophysics Group, Department of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, UK; Astronomical Institute Anton Pannekoek, University of Amsterdam, Science Park 904, NL-1098 XH Amsterdam, Netherlands; Leiden Observatory, Leiden University, Niels Bohrweg 2, NL-2333 CA Leiden, Nethe... | [
"2017MNRAS.472.3821R",
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12594146 | 1607.08250 | Dust traps as planetary birthsites: basics and vortex formation | We present a simple model for low-mass planet formation and subsequent evolution within 'transition' discs. We demonstrate quantitatively that the predicted and observed structures of such discs are prime birthsites of planets. Planet formation is likely to proceed through pebble accretion, should a planetary embryo (M ≳ 10<SUP>-4</SUP> M<SUB>⊕</SUB>) form. Efficient pebble accretion is likely to be unavoidable in transition disc dust traps, as the dust particles required for pebble accretion are those which are most efficiently trapped in the transition disc dust trap. Rapid pebble accretion within the dust trap gives rise not only to low-mass planets, but also to a large accretion luminosity. This accretion luminosity is sufficient to heat the disc outside the gravitational influence of the planet and makes the disc locally baroclinic, and a source of vorticity. Using numerical simulations, we demonstrate that this source of vorticity can lead to the growth of a single large-scale vortex in ∼100 orbits, which is capable of trapping particles. Finally, we suggest an evolutionary cycle: Planet formation proceeds through pebble accretion, followed by vortex formation and particle trapping in the vortex quenching the planetary accretion and thus removing the vorticity source. After the vortex is destroyed, the process can begin anew. This means transition discs should present with large-scale vortices for a significant fraction of their lifetimes, and remnant planets at large 10 au radii should be a common outcome of this cycle. | [
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"transition disc dust traps",
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"transition discs",
"remnant planets",
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"Efficient pebble accretion",
"Rapid pebble accretion",
"planets",
"such discs",
"the transition disc dust trap",
"vorticity",
"low-mass planet formation",
"part... | [
"accretion",
"accretion discs",
"planets and satellites: formation",
"planet-disc interactions",
"protoplanetary discs",
"Astrophysics - Solar and Stellar Astrophysics",
"Astrophysics - Earth and Planetary Astrophysics"
] | 2 | [
"10.1093/mnras/stx302",
"10.48550/arXiv.1607.08250"
] | [
"Owen, James E.",
"Kollmeier, Juna A."
] | [
"Institute for Advanced Study, Einstein Drive, Princeton, NJ 08540, USA",
"Institute for Advanced Study, Einstein Drive, Princeton, NJ 08540, USA; Observatories of the Carnegie Institution of Washington, 813 Santa Barbara Street, Pasadena, CA 91101, USA"
] | [
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4331519 | 1607.07918 | Investigating the dusty torus of Seyfert galaxies using SOFIA/FORCAST photometry | We present 31.5 μm imaging photometry of 11 nearby Seyfert galaxies observed from the Stratospheric Observatory For Infrared Astronomy (SOFIA) using the Faint Object infraRed CAmera for the SOFIA Telescope (FORCAST). We tentatively detect extended 31 μm emission for the first time in our sample. In combination with this new data set, subarcsecond resolution 1-18 μm imaging and 7.5-13 μm spectroscopic observations were used to compute the nuclear spectral energy distribution (SED) of each galaxy. We found that the turnover of the torus emission does not occur at wavelengths ≤31.5 μm, which we interpret as a lower-limit for the wavelength of peak emission. We used CLUMPY torus models to fit the nuclear infrared (IR) SED and infer trends in the physical parameters of the AGN torus for the galaxies in the sample. Including the 31.5 μm nuclear flux in the SED (1) reduces the number of clumpy torus models compatible with the data, and (2) modifies the model output for the outer radial extent of the torus for 10 of the 11 objects. Specifically, six (60 per cent) objects show a decrease in radial extent while four (40 per cent) show an increase. We find torus outer radii ranging from <1 to 8.4 pc. | [
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... | 14.912519 | 7.970968 | 2016-07-01 | 24 | 2016MNRAS.462.2618F | [
"clumpy torus models",
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"subarcsecond resolution",
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"31 μm emission",
"the nuclear spectral energy distribution",
"the AGN torus",
"the out... | [
"galaxies: active",
"galaxies: nuclei",
"galaxies: Seyfert",
"Astrophysics - Astrophysics of Galaxies"
] | 9 | [
"10.1093/mnras/stw1780",
"10.48550/arXiv.1607.07918"
] | [
"Fuller, L.",
"Lopez-Rodriguez, E.",
"Packham, C.",
"Ramos-Almeida, C.",
"Alonso-Herrero, A.",
"Levenson, N. A.",
"Radomski, J.",
"Ichikawa, K.",
"García-Bernete, I.",
"González-Martín, O.",
"Díaz-Santos, T.",
"Martínez-Paredes, M."
] | [
"Department of Physics & Astronomy, University of Texas at San Antonio, One UTSA Circle, San Antonio, TX 78249, USA",
"Department of Astronomy, University of Texas at Austin, 2515 Speedway, Stop C1402, Austin, TX 78712, USA; McDonald Observatory, University of Texas at Austin, 2515 Speedway, Stop C1402, Austi... | [
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"2019ApJ...870...31I",
"2019ApJ...872..... | [
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12510124 | 1607.03973 | Observable cosmological vector mode in the dark ages | The second-order vector mode is inevitably induced from the coupling of first-order scalar modes in cosmological perturbation theory and might hinder a possible detection of primordial gravitational waves from inflation through 21 cm lensing observations. Here, we investigate the weak lensing signal in 21 cm photons emitted by neutral hydrogen atoms in the dark ages induced by the second-order vector mode by decomposing the deflection angle of the 21 cm lensing signal into the gradient and curl modes. The curl mode is a good tracer of the cosmological vector and tensor modes since the scalar mode does not induce the curl one. By comparing angular power spectra of the 21 cm lensing curl mode induced by the second-order vector mode and primordial gravitational waves whose amplitude is parametrized by the tensor-to-scalar ratio r , we find that the 21 cm curl mode from the second-order vector mode dominates over that from primordial gravitational waves on almost all scales if r ≲10<SUP>-5</SUP>. If we use the multipoles of the power spectrum up to ℓma<SUB>x</SUB>=1 0<SUP>5</SUP> and 1 0<SUP>6</SUP> in reconstructing the curl mode from 21 cm temperature maps, the signal-to-noise ratios of the 21 cm curl mode from the second-order vector mode achieve S /N ≈0.46 and 73, respectively. Observation of 21 cm radiation is, in principle, a powerful tool to explore not only the tensor mode but also the cosmological vector mode. | [
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... | 12.113307 | 0.362762 | 2016-07-01 | 5 | 2016PhRvD..94f3523S | [
"primordial gravitational waves",
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"first-order scalar modes",
"The second-order vector mode",
"the second-order vector mode",
"the curl mode",
"second",
"the scalar mode",
"cosmological perturbation theory",
"the cosmological vector and tensor modes",
"the 21 cm l... | [
"Astrophysics - Cosmology and Nongalactic Astrophysics"
] | 2 | [
"10.1103/PhysRevD.94.063523",
"10.48550/arXiv.1607.03973"
] | [
"Saga, Shohei"
] | [
"Department of Physics and Astrophysics, Nagoya University, Aichi 464-8602, Japan"
] | [
"2017MNRAS.470.3131T",
"2017PhRvD..95l3524S",
"2017PhRvD..96f3508S",
"2018arXiv181009572C",
"2020CQGra..37o4001A"
] | [
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3016013 | 1607.06621 | Signatures of nonlinear mode interactions in the pulsating hot B subdwarf star KIC 10139564 | Context. The unprecedented photometric quality and time coverage offered by the Kepler spacecraft has opened up new opportunities to search for signatures of nonlinear effects that affect oscillation modes in pulsating stars. <BR /> Aims: The data accumulated on the pulsating hot B subdwarf KIC 10139564 are used to explore in detail the stability of its oscillation modes, focusing in particular on evidences of nonlinear behaviors. <BR /> Methods: We analyzed 38 months of contiguous short-cadence data, concentrating on mode multiplets induced by the star rotation and on frequencies forming linear combinations that show intriguing behaviors during the course of the observations. <BR /> Results: We find clear signatures that point toward nonlinear effects predicted by resonant mode coupling mechanisms. These couplings can induce various mode behaviors for the components of multiplets and for frequencies related by linear relationships. We find that a triplet at 5760 μHz, a quintuplet at 5287 μHz and a (ℓ > 2) multiplet at 5412 μHz, all induced by rotation, show clear frequency and amplitude modulations which are typical of the so-called intermediate regime of a resonance between the components. One triplet at 316 μHz and a doublet at 394 μHz show modulated amplitude and constant frequency which can be associated with a narrow transitory regime of the resonance. Another triplet at 519 μHz appears to be in a frequency-locked regime where both frequency and amplitude are constant. Additionally, three linear combinations of frequencies near 6076 μHz also show amplitude and frequency modulations, which are likely related to a three-mode direct resonance of the type ν<SUB>0</SUB> ~ ν<SUB>1</SUB> + ν<SUB>2</SUB>. <BR /> Conclusions: The identified frequency and amplitude modulations are the first clear-cut signatures of nonlinear resonant couplings occurring in pulsating hot B subdwarf stars. However, the observed behaviors suggest that the resonances occurring in these stars usually follow more complicated patterns than the simple predictions from current nonlinear theoretical frameworks. These results should therefore motivate further work to develop the theory of nonlinear stellar pulsations, considering that stars such as KIC 10139564 now offer remarkable testbeds to do so. | [
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-0.01312... | 6.904308 | 11.488626 | 2016-07-01 | 45 | 2016A&A...594A..46Z | [
"nonlinear behaviors",
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"techniques: photometric",
"stars: variables: general",
"stars: individual: KIC 10139564",
"Astrophysics - Solar and Stellar Astrophysics"
] | 2 | [
"10.1051/0004-6361/201629132",
"10.48550/arXiv.1607.06621"
] | [
"Zong, W.",
"Charpinet, S.",
"Vauclair, G."
] | [
"Université de Toulouse, UPS-OMP, IRAP, 31400, Toulouse, France ; CNRS, IRAP, 14 avenue Edouard Belin, 31400, Toulouse, France",
"Université de Toulouse, UPS-OMP, IRAP, 31400, Toulouse, France ; CNRS, IRAP, 14 avenue Edouard Belin, 31400, Toulouse, France",
"Université de Toulouse, UPS-OMP, IRAP, 31400, Toulous... | [
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"2020A&A...643A.... | [
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2263112 | 1607.04412 | High-precision astrometry towards ELTs | With the aim of paving the road for future accurate astrometry with MICADO at the European-ELT, we performed an astrometric study using two different but complementary approaches to investigate two critical components that contribute to the total astrometric accuracy. First, we tested the predicted improvement in the astrometric measurements with the use of an atmospheric dispersion corrector (ADC) by simulating realistic images of a crowded Galactic globular cluster. We found that the positional measurement accuracy should be improved by up to 2 mas with the ADC, making this component fundamental for high-precision astrometry. Second, we analysed observations of a globular cluster taken with the only currently available Multi-Conjugate Adaptive Optics assisted camera, GeMS/GSAOI at Gemini South. Making use of previously measured proper motions of stars in the field of view, we were able to model the distortions affecting the stellar positions. We found that they can be as large as 200 mas, and that our best model corrects them to an accuracy of 1 mas. We conclude that future astrometric studies with MICADO requires both an ADC and an accurate modelling of distortions to the field of view, either through an a-priori calibration or an a-posteriori correction. | [
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-0... | 14.041121 | 10.465379 | 2016-07-01 | 7 | 2016SPIE.9909E..1GM | [
"Gemini South",
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"future astrometric studies",
"future accurate astrometry",
"ADC",
"realistic images",
"MICADO",
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"the total astrometric accuracy",
"view",
"the only currently available Multi-Conjugate Adaptive Optics",
"a crowded Galactic globu... | [
"Astrophysics - Instrumentation and Methods for Astrophysics"
] | 3 | [
"10.1117/12.2232478",
"10.48550/arXiv.1607.04412"
] | [
"Massari, Davide",
"Fiorentino, Giuliana",
"Tolstoy, Eline",
"McConnachie, Alan",
"Stuik, Remko",
"Schreiber, Laura",
"Andersen, David",
"Clénet, Yann",
"Davies, Richard",
"Gratadour, Damien",
"Kuijken, Konrad",
"Navarro, Ramon",
"Pott, Jörg-Uwe",
"Rodeghiero, Gabriele",
"Turri, Paolo",
... | [
"INAF - Osservatorio Astronomico di Bologna (Italy)",
"INAF - Osservatorio Astronomico di Bologna (Italy)",
"Univ. of Groningen (Netherlands)",
"Herzberg Astronomy and Astrophysics, National Research Council Canada (Canada)",
"Leiden Observatory (Netherlands)",
"INAF - Osservatorio Astronomico di Bologna ... | [
"2016SPIE.9908E..1ZD",
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"2017ApJ...840...30F",
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5398407 | 1607.07377 | Frames of most uniform Hubble flow | It has been observed [1,2] that the locally measured Hubble parameter converges quickest to the background value and the dipole structure of the velocity field is smallest in the reference frame of the Local Group of galaxies. We study the statistical properties of Lorentz boosts with respect to the Cosmic Microwave Background frame which make the Hubble flow look most uniform around a particular observer. We use a very large N-Body simulation to extract the dependence of the boost velocities on the local environment such as underdensities, overdensities, and bulk flows. We find that the observation [1,2] is not unexpected if we are located in an underdensity, which is indeed the case for our position in the universe. The amplitude of the measured boost velocity for our location is consistent with the expectation in the standard cosmology. | [
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0... | 11.508515 | 1.900224 | 2016-07-01 | 12 | 2016JCAP...10..016K | [
"bulk flows",
"galaxies",
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"Hubble",
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"overdensities",
"the Hubble flow",
"underdensities",
"the measured boost velocity",
"the boost velocities",
"the velocity field",
"the reference frame",
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"Astrophysics - Cosmology and Nongalactic Astrophysics"
] | 9 | [
"10.1088/1475-7516/2016/10/016",
"10.48550/arXiv.1607.07377"
] | [
"Kraljic, David",
"Sarkar, Subir"
] | [
"Rudolf Peierls Centre for Theoretical Physics, University of Oxford, 1 Keble Road, Oxford, OX1 3NP, U.K.",
"Rudolf Peierls Centre for Theoretical Physics, University of Oxford, 1 Keble Road, Oxford, OX1 3NP, U.K.; Niels Bohr International Academy, University of Copenhagen, Blegdamsvej 17, 2100 Copenhagen, Denmar... | [
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3360123 | 1607.03554 | Metallicity and Age of the Stellar Stream around the Disk Galaxy NGC 5907 | Stellar streams have become central to studies of the interaction histories of nearby galaxies. To characterize the most prominent parts of the stellar stream around the well-known nearby (d = 17 Mpc) edge-on disk galaxy NGC 5907, we have obtained and analyzed new, deep gri Subaru/Suprime-Cam and 3.6 μm Spitzer/Infrared Array Camera observations. Combining the near-infrared 3.6 μm data with visible-light images allows us to use a long wavelength baseline to estimate the metallicity and age of the stellar population along an ∼60 kpc long segment of the stream. We have fitted the stellar spectral energy distribution with a single-burst stellar population synthesis model and we use it to distinguish between the proposed satellite accretion and minor/major merger formation models of the stellar stream around this galaxy. We conclude that a massive minor merger (stellar mass ratio of at least 1:8) can best account for the metallicity of -0.3 inferred along the brightest parts of the stream. | [
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"galaxies: evolution",
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"Astrophysics - Astrophysics of Galaxies"
] | 5 | [
"10.3847/0004-6256/152/3/72",
"10.48550/arXiv.1607.03554"
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"Laine, Seppo",
"Grillmair, Carl J.",
"Capak, Peter",
"Arendt, Richard G.",
"Romanowsky, Aaron J.",
"Martínez-Delgado, David",
"Ashby, Matthew L. N.",
"Davies, James E.",
"Majewski, Stephen R.",
"Brodie, Jean P.",
"GaBany, R. Jay",
"Arnold, Jacob A."
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"CRESST/UMBC/NASA GSFC, Code 665, Greenbelt, MD 20771, USA",
"Department of Physics and Astronomy, Sa... | [
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2417729 | 1607.03886 | Kepler Flares. IV. A Comprehensive Analysis of the Activity of the dM4e Star GJ 1243 | We present a comprehensive study of the active dM4e star GJ 1243. We use previous observations and ground-based echelle spectroscopy to determine that GJ 1243 is a member of the Argus association of field stars, suggesting it is ∼ 30{--}50 {{Myr}} old. We analyze 11 months of 1 minute cadence data from Kepler, presenting Kepler flare frequency distributions, as well as determining correlations between flare energy, amplitude, duration, and decay time. We find that the exponent α of the power-law flare energy distribution varies in time, primarily due to completeness of sample and the low frequency of high-energy flares. We also find a deviation from a single power law at high energy. We use ground-based spectroscopic observations that were simultaneous with the Kepler data to provide simultaneous photometric and spectroscopic analysis of three low-energy flares, the lowest-energy dMe flares with detailed spectral analysis to date on any star. The spectroscopic data from these flares extend constraints for radiative hydrodynamic flare models to a lower energy regime than has previously been studied. We use this simultaneous spectroscopy and Kepler photometry to develop approximate conversions from the Kepler bandpass to the traditional U and B bands. This conversion will be a critical factor in comparing any Kepler flare analyses to the canon of previous ground-based flare studies. | [
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"10.3847/0004-637X/829/2/129",
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"Silverberg, Steven M.",
"Kowalski, Adam F.",
"Davenport, James R. A.",
"Wisniewski, John P.",
"Hawley, Suzanne L.",
"Hilton, Eric J."
] | [
"Homer L. Dodge Department of Physics and Astronomy, University of Oklahoma, 440 W. Brooks Street, Norman, OK 73019, USA",
"Department of Astronomy, University of Maryland, College Park, MD 20742, USA ; NASA Goddard Space Flight Center, Code 671, Greenbelt, MD 20771, USA",
"Western Washington University, Bellin... | [
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12409068 | 1607.03909 | The Evolution of Galaxy Number Density at z < 8 and Its Implications | The evolution of the number density of galaxies in the universe, and thus also the total number of galaxies, is a fundamental question with implications for a host of astrophysical problems including galaxy evolution and cosmology. However, there has never been a detailed study of this important measurement, nor a clear path to answer it. To address this we use observed galaxy stellar mass functions up to z ∼ 8 to determine how the number densities of galaxies change as a function of time and mass limit. We show that the increase in the total number density of galaxies (ϕ <SUB>T</SUB>), more massive than M <SUB>*</SUB> = 10<SUP>6</SUP> M <SUB>⊙</SUB>, decreases as ϕ <SUB>T</SUB> ∼ t <SUP>-1</SUP>, where t is the age of the universe. We further show that this evolution turns over and rather increases with time at higher mass lower limits of M <SUB>*</SUB> > 10<SUP>7</SUP> M <SUB>⊙</SUB>. By using the M <SUB>*</SUB> = 10<SUP>6</SUP> M <SUB>⊙</SUB> lower limit we further show that the total number of galaxies in the universe up to z = 8 is {2.0}<SUB>-0.6</SUB><SUP>+0.7</SUP>× {10}<SUP>12</SUP> (2 trillion), almost a factor of 10 higher than would be seen in an all sky survey at Hubble Ultra-Deep Field depth. We discuss the implications for these results for galaxy evolution, as well as compare our results with the latest models of galaxy formation. These results also reveal that the cosmic background light in the optical and near-infrared likely arise from these unobserved faint galaxies. We also show how these results solve the question of why the sky at night is dark, otherwise known as Olbers’ paradox. | [
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"10.3847/0004-637X/830/2/83",
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"Conselice, Christopher J.",
"Wilkinson, Aaron",
"Duncan, Kenneth",
"Mortlock, Alice"
] | [
"University of Nottingham, School of Physics & Astronomy, Nottingham, NG7 2RD, UK",
"University of Nottingham, School of Physics & Astronomy, Nottingham, NG7 2RD, UK",
"University of Nottingham, School of Physics & Astronomy, Nottingham, NG7 2RD, UK",
"University of Nottingham, School of Physics &... | [
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1187815 | 1607.03412 | An innovative silicon photomultiplier digitizing camera for gamma-ray astronomy | The single-mirror small-size telescope (SST-1M) is one of the three proposed designs for the small-size telescopes (SSTs) of the Cherenkov Telescope Array (CTA) project. The SST-1M will be equipped with a 4 m-diameter segmented reflector dish and an innovative fully digital camera based on silicon photo-multipliers. Since the SST sub-array will consist of up to 70 telescopes, the challenge is not only to build telescopes with excellent performance, but also to design them so that their components can be commissioned, assembled and tested by industry. In this paper we review the basic steps that led to the design concepts for the SST-1M camera and the ongoing realization of the first prototype, with focus on the innovative solutions adopted for the photodetector plane and the readout and trigger parts of the camera. In addition, we report on results of laboratory measurements on real scale elements that validate the camera design and show that it is capable of matching the CTA requirements of operating up to high moonlight background conditions. | [
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"10.1140/epjc/s10052-017-4609-z",
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"Heller, M.",
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"Aguilar, J. A.",
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"Prandini, E.",
"Rajda, P.",
"Rameez, M.",
"Bilnik, W.",
"Błocki, J.",
"Bogacz, L.",
"Borkowski,... | [
"DPNC-Université de Genève, Geneva, Switzerland",
"DPNC-Université de Genève, Geneva, Switzerland",
"DPNC-Université de Genève, Geneva, Switzerland",
"DPNC-Université de Genève, Geneva, Switzerland",
"Astronomical Observatory, Jagellonian University, Kraków, Poland",
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2775547 | 1607.01403 | H0LiCOW - IV. Lens mass model of HE 0435-1223 and blind measurement of its time-delay distance for cosmology | Strong gravitational lenses with measured time delays between the multiple images allow a direct measurement of the time-delay distance to the lens, and thus a measure of cosmological parameters, particularly the Hubble constant, H<SUB>0</SUB>. We present a blind lens model analysis of the quadruply imaged quasar lens HE 0435-1223 using deep Hubble Space Telescope imaging, updated time-delay measurements from the COSmological MOnitoring of GRAvItational Lenses (COSMOGRAIL), a measurement of the velocity dispersion of the lens galaxy based on Keck data, and a characterization of the mass distribution along the line of sight. HE 0435-1223 is the third lens analysed as a part of the H<SUB>0</SUB> Lenses in COSMOGRAIL's Wellspring (H0LiCOW) project. We account for various sources of systematic uncertainty, including the detailed treatment of nearby perturbers, the parametrization of the galaxy light and mass profile, and the regions used for lens modelling. We constrain the effective time-delay distance to be D_{Δ t}= 2612_{-191}^{+208} Mpc, a precision of 7.6 per cent. From HE 0435-1223 alone, we infer a Hubble constant of H<SUB>0</SUB> = 73.1_{-6.0}^{+5.7} km s^{-1 Mpc^{-1}} assuming a flat ΛCDM cosmology. The cosmographic inference based on the three lenses analysed by H0LiCOW to date is presented in a companion paper (H0LiCOW Paper V). | [
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"gravitational lensing: strong",
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] | 28 | [
"10.1093/mnras/stw3077",
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"Wong, Kenneth C.",
"Suyu, Sherry H.",
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"Courbin, Frederic",
"Fassnacht, Christopher D.",
"Halkola, Aleksi",
"Rusu, Cristian E.",
"Sluse, Dominique",
"Sonnenfeld, Alessandro",
"Treu, Tommaso",
"Collett, Thomas E.",
"Hilbert, Stefan",
"Koopmans, Leon V.... | [
"National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; Institute of Astronomy and Astrophysics, Academia Sinica (ASIAA), PO Box 23-141, Taipei 10617, Taiwan",
"Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, D-85748 Garching, Germany; Institute of Astronomy and A... | [
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12511007 | 1607.04226 | Arrival times of gravitational radiation peaks for binary inspiral | Modeling of gravitational waves (GWs) from binary black hole inspiral brings together early post-Newtonian waveforms and late quasinormal ringing waveforms. Attempts to bridge the two limits without recourse to numerical relativity involve predicting the time of the peak GW amplitude. This prediction will require solving the question of why the peak of the "source," i.e., the peak of the binary angular velocity, does not correspond to the peak of the GW amplitude. We show here that this offset can be understood as due to the existence of two distinct components of the radiation: the "direct" radiation analogous to that in flat spacetime and "scattered" radiation associated with curved spacetime. The time dependence of these two components and of their relative phases determines the location of the peak amplitude. We use a highly simplified model to clarify the two-component nature of the source, then demonstrate that the explanation is valid also for an extreme mass-ratio binary inspiral. | [
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... | 8.009014 | 2.524879 | 2016-07-01 | 4 | 2016PhRvD..94j4026P | [
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"General Relativity and Quantum Cosmology",
"Astrophysics - High Energy Astrophysical Phenomena"
] | 3 | [
"10.1103/PhysRevD.94.104026",
"10.48550/arXiv.1607.04226"
] | [
"Price, Richard H.",
"Khanna, Gaurav"
] | [
"Department of Physics, MIT, 77 Massachusetts Ave., Cambridge, Massachusetts 02139 and Department of Physics, University of Massachusetts, Dartmouth, Massachusetts 02747",
"Department of Physics, University of Massachusetts, Dartmouth, Massachusetts 02747"
] | [
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4842242 | 1607.06479 | The cold dark matter content of Galactic dwarf spheroidals: no cores, no failures, no problem | We examine the dark matter content of satellite galaxies in Lambda-CDM cosmological hydrodynamical simulations of the Local Group from the APOSTLE project. We find excellent agreement between simulation results and estimates for the 9 brightest Galactic dwarf spheroidals (dSphs) derived from their stellar velocity dispersions and half-light radii. Tidal stripping plays an important role by gradually removing dark matter from the outside in, affecting in particular fainter satellites and systems of larger-than-average size for their luminosity. Our models suggest that tides have significantly reduced the dark matter content of Can Ven I, Sextans, Carina, and Fornax, a prediction that may be tested by comparing them with field galaxies of matching luminosity and size. Uncertainties in observational estimates of the dark matter content of individual dwarfs have been underestimated in the past, at times substantially. We use our improved estimates to revisit the `too-big-to-fail' problem highlighted in earlier N-body work. We reinforce and extend our previous conclusion that the APOSTLE simulations show no sign of this problem. The resolution does not require `cores' in the dark mass profiles, but, rather, relies on revising assumptions and uncertainties in the interpretation of observational data and accounting for `baryon effects' in the theoretical modelling. | [
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"size",
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"Astrophysics - Astrophysics of Galaxies",
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] | 9 | [
"10.48550/arXiv.1607.06479"
] | [
"Fattahi, Azadeh",
"Navarro, Julio F.",
"Sawala, Till",
"Frenk, Carlos S.",
"Sales, Laura V.",
"Oman, Kyle",
"Schaller, Matthieu",
"Wang, Jie"
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"-",
"-",
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12626389 | 1607.03540 | Binary neutron star mergers: a review of Einstein’s richest laboratory | In a single process, the merger of binary neutron star systems combines extreme gravity, the copious emission of gravitational waves, complex microphysics and electromagnetic processes, which can lead to astrophysical signatures observable at the largest redshifts. We review here the recent progress in understanding what could be considered Einstein’s richest laboratory, highlighting in particular the numerous significant advances of the last decade. Although special attention is paid to the status of models, techniques and results for fully general-relativistic dynamical simulations, a review is also offered on the initial data and advanced simulations with approximate treatments of gravity. Finally, we review the considerable amount of work carried out on the post-merger phase, including black-hole formation, torus accretion onto the merged compact object, the connection with gamma-ray burst engines, ejected material, and its nucleosynthesis. | [
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... | 6.693792 | 2.402728 | 2016-07-01 | 421 | 2017RPPh...80i6901B | [
"binary neutron star systems combines extreme gravity",
"extreme gravity",
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"gravity",
"advanced simulations",
"astrophysical signatures",
"approximate treatments",
"binary neutron star systems",
"torus accretion",
"mat... | [
"General Relativity and Quantum Cosmology",
"Astrophysics - High Energy Astrophysical Phenomena",
"Astrophysics - Solar and Stellar Astrophysics"
] | 24 | [
"10.1088/1361-6633/aa67bb",
"10.48550/arXiv.1607.03540"
] | [
"Baiotti, Luca",
"Rezzolla, Luciano"
] | [
"Graduate School of Science, Osaka University, Toyonaka, 560-0043, Japan",
"Institute for Theoretical Physics, Max-von-Laue-Str. 1, 60438 Frankfurt, Germany ; Frankfurt Institute for Advanced Studies, Ruth-Moufang-Str. 1, 60438 Frankfurt, Germany"
] | [
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12593803 | 1607.03149 | The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: baryon acoustic oscillations in the Fourier space | We analyse the baryon acoustic oscillation (BAO) signal of the final Baryon Oscillation Spectroscopic Survey (BOSS) data release (DR12). Our analysis is performed in the Fourier space, using the power spectrum monopole and quadrupole. The data set includes 1198 006 galaxies over the redshift range 0.2 < z < 0.75. We divide this data set into three (overlapping) redshift bins with the effective redshifts z<SUB>eff</SUB> = 0.38, 0.51 and 0.61. We demonstrate the reliability of our analysis pipeline using N-body simulations as well as ∼1000 MultiDark-Patchy mock catalogues that mimic the BOSS-DR12 target selection. We apply density field reconstruction to enhance the BAO signal-to-noise ratio. By including the power spectrum quadrupole we can separate the line of sight and angular modes, which allows us to constrain the angular diameter distance D<SUB>A</SUB>(z) and the Hubble parameter H(z) separately. We obtain two independent 1.6 and 1.5 per cent constraints on D<SUB>A</SUB>(z) and 2.9 and 2.3 per cent constraints on H(z) for the low (z<SUB>eff</SUB> = 0.38) and high (z<SUB>eff</SUB> = 0.61) redshift bin, respectively. We obtain two independent 1 and 0.9 per cent constraints on the angular averaged distance D<SUB>V</SUB>(z), when ignoring the Alcock-Paczynski effect. The detection significance of the BAO signal is of the order of 8σ (post-reconstruction) for each of the three redshift bins. Our results are in good agreement with the Planck prediction within Λ cold dark matter. This paper is part of a set that analyses the final galaxy clustering data set from BOSS. The measurements and likelihoods presented here are combined with others in Alam et al. to produce the final cosmological constraints from BOSS. | [
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"gravitation",
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] | 33 | [
"10.1093/mnras/stw2373",
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"Beutler, Florian",
"Seo, Hee-Jong",
"Ross, Ashley J.",
"McDonald, Patrick",
"Saito, Shun",
"Bolton, Adam S.",
"Brownstein, Joel R.",
"Chuang, Chia-Hsun",
"Cuesta, Antonio J.",
"Eisenstein, Daniel J.",
"Font-Ribera, Andreu",
"Grieb, Jan Niklas",
"Hand, Nick",
"Kitaura, Francisco-Shu",
"M... | [
"Institute of Cosmology and Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK; Lawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley, CA 94720, USA",
"Department of Physics and Astronomy, Ohio University, 251B Clippinger Labs, Athens, OH 45701, USA",
"Department of Physics... | [
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12408270 | 1607.01290 | Caught in the Act: Direct Detection of Galactic Bars in the Buckling Phase | The majority of massive disk galaxies, including our own, have stellar bars with vertically thick inner region, known as “boxy/peanut-shaped” (B/P) bulges. The most commonly suggested mechanism for the formation of B/P bulges is a violent vertical “buckling” instability in the bar, something that has been seen in N-body simulations for over 20 years, but never identified in real galaxies. Here, we present the first direct observational evidence for ongoing buckling in two nearby galaxies (NGC 3227 and NGC 4569), including characteristic asymmetric isophotes and (in NGC 4569) stellar kinematic asymmetries that match buckling in simulations. This confirms that the buckling instability takes place and produces B/P bulges in real galaxies. A toy model of bar evolution yields a local fraction of buckling bars consistent with observations if the buckling phase lasts ∼0.5-1 Gyr, in agreement with simulations. | [
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"galaxies: bulges",
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] | 12 | [
"10.3847/2041-8205/825/2/L30",
"10.48550/arXiv.1607.01290"
] | [
"Erwin, Peter",
"Debattista, Victor P."
] | [
"Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse, D-85748 Garching, Germany ; Universitäts-Sternwarte München, Scheinerstrasse 1, D-81679 München, Germany;",
"Jeremiah Horrocks Institute, University of Central Lancashire, Preston PR1 2HE, UK"
] | [
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12472902 | 1607.06365 | Viscous time lags between starburst and AGN activity | There is strong observational evidence indicating a time lag of order of some 100 Myr between the onset of starburst and AGN activity in galaxies. Dynamical time lags have been invoked to explain this. We extend this approach by introducing a viscous time lag the gas additionally needs to flow through the AGN's accretion disc before it reaches the central black hole. Our calculations reproduce the observed time lags and are in accordance with the observed correlation between black hole mass and stellar velocity dispersion. | [
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-... | 15.912522 | 7.675403 | 2016-07-01 | 9 | 2016MNRAS.462.2246B | [
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"galaxies: active",
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"quasars: general",
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"Astrophysics - Astrophysics of Galaxies"
] | 2 | [
"10.1093/mnras/stw1804",
"10.48550/arXiv.1607.06365"
] | [
"Blank, Marvin",
"Duschl, Wolfgang J."
] | [
"Institut für Theoretische Physik und Astrophysik, Christian-Albrechts-Universität zu Kiel, Leibnizstr. 15, D-24118 Kiel, Germany",
"Institut für Theoretische Physik und Astrophysik, Christian-Albrechts-Universität zu Kiel, Leibnizstr. 15, D-24118 Kiel, Germany; Steward Observatory, The University of Arizona, 933... | [
"2016acps.confE..33E",
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12472835 | 1607.06686 | The analemma criterion: accidental quasi-satellites are indeed true quasi-satellites | In the Solar system, a quasi-satellite is an object that follows a heliocentric path with an orbital period that matches almost exactly with that of a host body (planetary or not). The trajectory is of such nature that, without being gravitationally attached, the value of the angular separation between host and quasi-satellite as seen from the Sun remains confined within relatively narrow limits for time-spans that exceed the length of the host's sidereal orbital period. Here, we show that under these conditions, a quasi-satellite traces an analemma in the sky as observed from the host in a manner similar to that found for geosynchronous orbits. The analemmatic curve (figure-eight-, teardrop-, ellipse-shaped) results from the interplay between the tilt of the rotational axis of the host and the properties of the orbit of the quasi-satellite. The analemma criterion can be applied to identify true quasi-satellite dynamical behaviour using observational or synthetic astrometry and it is tested for several well-documented quasi-satellites. For the particular case of 15810 (1994 JR<SUB>1</SUB>), a putative accidental quasi-satellite of dwarf planet Pluto, we show explicitly that this object describes a complex analemmatic curve for several Plutonian sidereal periods, confirming its transient quasi-satellite status. | [
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"its transient quasi-satellite status",
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"methods: numerical",
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"asteroids: individual: 63252 (2001 BL<SUB>41</SUB>)",
"Astrophysics - Earth and Planetary Astrophysics"
] | 9 | [
"10.1093/mnras/stw1833",
"10.48550/arXiv.1607.06686"
] | [
"de la Fuente Marcos, C.",
"de la Fuente Marcos, R."
] | [
"Apartado de Correos 3413, E-28080 Madrid, Spain",
"Apartado de Correos 3413, E-28080 Madrid, Spain"
] | [
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12583834 | 1607.00775 | The magnetic part of the Weyl tensor, and the expansion of discrete universes | We examine the effect that the magnetic part of the Weyl tensor has on the large-scale expansion of space. This is done within the context of a class of cosmological models that contain regularly arranged discrete masses, rather than a continuous perfect fluid. The natural set of geodesic curves that one should use to consider the cosmological expansion of these models requires the existence of a non-zero magnetic part of the Weyl tensor. We include this object in the evolution equations of these models by performing a Taylor series expansion about a hypersurface where it initially vanishes. At the same cosmological time, measured as a fraction of the age of the universe, we find that the influence of the magnetic part of the Weyl tensor increases as the number of masses in the universe is increased. We also find that the influence of the magnetic part of the Weyl tensor increases with time, relative to the leading-order electric part, so that its contribution to the scale of the universe can reach values of ∼ 1%, before the Taylor series approximation starts to break down. | [
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... | 10.419729 | 0.264016 | 2016-07-01 | 16 | 2017GReGr..49...30C | [
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"a non-zero magnetic part",
"geodesic curves",
... | [
"Black holes",
"Cosmology",
"Silent universes",
"General Relativity and Quantum Cosmology",
"Astrophysics - Cosmology and Nongalactic Astrophysics"
] | 3 | [
"10.1007/s10714-017-2192-0",
"10.48550/arXiv.1607.00775"
] | [
"Clifton, Timothy",
"Gregoris, Daniele",
"Rosquist, Kjell"
] | [
"School of Physics and Astronomy, Queen Mary University of London, London, UK",
"Department of Mathematics and Statistics, Dalhousie University, Halifax, Canada",
"Department of Physics, Stockholm University, Stockholm, Sweden"
] | [
"2017CQGra..34f5003S",
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12409147 | 1607.05961 | Projection Effects in Coronal Dimmings and Associated EUV Wave Event | We investigate the high-speed (v > 1000 km s<SUP>-1</SUP>) extreme-ultraviolet (EUV) wave associated with an X1.2 flare and coronal mass ejection (CME) from NOAA active region 11283 on 2011 September 6 (SOL2011-09-06T22:12). This EUV wave features peculiar on-disk signatures in particular, we observe an intermittent “disappearance” of the front for 120 s in Solar Dynamics Observatory (SDO)/AIA 171, 193, 211 Å data, whereas the 335 Å filter, sensitive to hotter plasmas (T ∼ 2.5 MK), shows a continuous evolution of the wave front. The eruption was also accompanied by localized coronal dimming regions. We exploit the multi-point quadrature position of SDO and STEREO-A, to make a thorough analysis of the EUV wave evolution, with respect to its kinematics and amplitude evolution and reconstruct the SDO line-of-sight (LOS) direction of the identified coronal dimming regions in STEREO-A. We show that the observed intensities of the dimming regions in SDO/AIA depend on the structures that are lying along their LOS and are the combination of their individual intensities, e.g., the expanding CME body, the enhanced EUV wave, and the CME front. In this context, we conclude that the intermittent disappearance of the EUV wave in the AIA 171, 193, and 211 Å filters, which are channels sensitive to plasma with temperatures below ∼2 MK is also caused by such LOS integration effects. These observations clearly demonstrate that single-view image data provide us with limited insight to correctly interpret coronal features. | [
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-0.01540... | 13.333632 | 15.926162 | 2016-07-01 | 11 | 2016ApJ...830...92D | [
"localized coronal dimming regions",
"NOAA active region",
"such LOS integration effects",
"coronal features",
"Solar Dynamics Observatory",
"EUV",
"LOS",
"CME",
"hotter plasmas",
"the identified coronal dimming regions",
"evolution",
"the EUV wave evolution",
"the enhanced EUV wave",
"MK"... | [
"Sun: activity",
"Sun: corona",
"Sun: coronal mass ejections: CMEs",
"Sun: flares",
"Astrophysics - Solar and Stellar Astrophysics"
] | 7 | [
"10.3847/0004-637X/830/2/92",
"10.48550/arXiv.1607.05961"
] | [
"Dissauer, K.",
"Temmer, M.",
"Veronig, A. M.",
"Vanninathan, K.",
"Magdalenić, J."
] | [
"IGAM/Institute of Physics, University of Graz, Universitätsplatz 5/II, A-8010 Graz, Austria",
"IGAM/Institute of Physics, University of Graz, Universitätsplatz 5/II, A-8010 Graz, Austria",
"IGAM/Institute of Physics, University of Graz, Universitätsplatz 5/II, A-8010 Graz, Austria; Kanzelhöhe Observatory/Insti... | [
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14122128 | 1607.02546 | Interpreting the cosmic far-infrared background anisotropies using a gas regulator model | Cosmic far-infrared background (CFIRB) is a powerful probe of the history of star formation rate (SFR) and the connection between baryons and dark matter across cosmic time. In this work, we explore to which extent the CFIRB anisotropies can be reproduced by a simple physical framework for galaxy evolution, the gas regulator (bathtub) model. This model is based on continuity equations for gas, stars, and metals, taking into account cosmic gas accretion, star formation, and gas ejection. We model the large-scale galaxy bias and small-scale shot noise self-consistently, and we constrain our model using the CFIRB power spectra measured by Planck. Because of the simplicity of the physical model, the goodness of fit is limited. We compare our model predictions with the observed correlation between CFIRB and gravitational lensing, bolometric infrared luminosity functions, and submillimetre source counts. The strong clustering of CFIRB indicates a large galaxy bias, which corresponds to haloes of mass 10<SUP>12.5</SUP> M<SUB>⊙</SUB> at z = 2, higher than the mass associated with the peak of the star formation efficiency. We also find that the far-infrared luminosities of haloes above 10<SUP>12</SUP> M<SUB>⊙</SUB> are higher than the expectation from the SFR observed in ultraviolet and optical surveys. | [
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... | 13.257123 | 7.083963 | 2016-07-01 | 9 | 2018MNRAS.475.3974W | [
"star formation rate",
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"cosmic time",
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"dark matter",
"galaxy evolution",
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"the star formation efficiency",
"Planck",
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"continuity equations",
"baryons",
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... | [
"galaxies: haloes",
"galaxies: star formation",
"submillimetre: diffuse background",
"submillimetre: galaxies",
"Astrophysics - Cosmology and Nongalactic Astrophysics",
"Astrophysics - Astrophysics of Galaxies"
] | 6 | [
"10.1093/mnras/sty071",
"10.48550/arXiv.1607.02546"
] | [
"Wu, Hao-Yi",
"Doré, Olivier",
"Teyssier, Romain",
"Serra, Paolo"
] | [
"California Institute of Technology, MC 367-17, Pasadena, CA 91125, USA; Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USA;",
"California Institute of Technology, MC 367-17, Pasadena, CA 91125, USA; Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USA",
"Institute for ... | [
"2016ApJ...833..153S",
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"2020ApJ...890..140S",
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12594106 | 1607.05199 | Gravitational wave signals from 3D neutrino hydrodynamics simulations of core-collapse supernovae | We present gravitational wave (GW) signal predictions from four 3D multigroup neutrino hydrodynamics simulations of core-collapse supernovae of progenitors with 11.2, 20 and 27 M<SUB>⊙</SUB>. GW emission in the pre-explosion phase strongly depends on whether the post-shock flow is dominated by the standing accretion shock instability (SASI) or convection and differs considerably from 2D models. SASI activity produces a strong signal component below 250 Hz through asymmetric mass motions in the gain layer and a non-resonant coupling to the proto-neutron star (PNS). Both convection- and SASI-dominated models show GW emission above 250 Hz, but with considerably lower amplitudes than in 2D. This is due to a different excitation mechanism for high-frequency l = 2 motions in the PNS surface, which are predominantly excited by PNS convection in 3D. Resonant excitation of high-frequency surface g modes in 3D by mass motions in the gain layer is suppressed compared to 2D because of smaller downflow velocities and a lack of high-frequency variability in the downflows. In the exploding 20 M<SUB>⊙</SUB> model, shock revival results in enhanced low-frequency emission due to a change of the preferred scale of the convective eddies in the PNS convection zone. Estimates of the expected excess power in two frequency bands suggest that second-generation detectors will only be able to detect very nearby events, but that third-generation detectors could distinguish SASI- and convection-dominated models at distances of ∼ 10 kpc. | [
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"smaller downflow velocities",
"enhanced low-frequency emission",
"high-frequency variability"... | [
"gravitational waves",
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"Astrophysics - High Energy Astrophysical Phenomena",
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] | 18 | [
"10.1093/mnras/stx618",
"10.48550/arXiv.1607.05199"
] | [
"Andresen, H.",
"Müller, B.",
"Müller, E.",
"Janka, H. -Th."
] | [
"Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, D-85748 Garching, Germany; Physik Department, Technische Universität München, James-Franck-Str. 1, D-85748 Garching, Germany",
"Astrophysics Research Centre, School of Mathematics and Physics, Queen's University Belfast, Belfast BT7 1NN, UK; Monash ... | [
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12408923 | 1607.02400 | GRB 090510: A Genuine Short GRB from a Binary Neutron Star Coalescing into a Kerr-Newman Black Hole | In a new classification of merging binary neutron stars (NSs) we separate short gamma-ray bursts (GRBs) into two subclasses. The ones with {E}<SUB>{iso</SUB>}≲ {10}<SUP>52</SUP> erg coalesce to form a massive NS and are indicated as short gamma-ray flashes (S-GRFs). The hardest, with {E}<SUB>{iso</SUB>}≳ {10}<SUP>52</SUP> erg, coalesce to form a black hole (BH) and are indicated as genuine short GRBs (S-GRBs). Within the fireshell model, S-GRBs exhibit three different components: the proper GRB (P-GRB) emission, observed at the transparency of a self-accelerating baryon-{e}<SUP>+</SUP>{e}<SUP>-</SUP> plasma; the prompt emission, originating from the interaction of the accelerated baryons with the circumburst medium; and the high-energy (GeV) emission, observed after the P-GRB and indicating the formation of a BH. GRB 090510 gives the first evidence for the formation of a Kerr BH or, possibly, a Kerr-Newman BH. Its P-GRB spectrum can be fitted by a convolution of thermal spectra whose origin can be traced back to an axially symmetric dyadotorus. A large value of the angular momentum of the newborn BH is consistent with the large energetics of this S-GRB, which reach in the 1-10,000 keV range {E}<SUB>{iso</SUB>}=(3.95+/- 0.21)× {10}<SUP>52</SUP> erg and in the 0.1-100 GeV range {E}<SUB>{LAT</SUB>}=(5.78+/- 0.60)× {10}<SUP>52</SUP> erg, the most energetic GeV emission ever observed in S-GRBs. The theoretical redshift {z}<SUB>{th</SUB>}=0.75+/- 0.17 that we derive from the fireshell theory is consistent with the spectroscopic measurement z=0.903+/- 0.003, showing the self-consistency of the theoretical approach. All S-GRBs exhibit GeV emission, when inside the Fermi-LAT field of view, unlike S-GRFs, which never evidence it. The GeV emission appears to be the discriminant for the formation of a BH in GRBs, confirmed by their observed overall energetics. | [
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-0... | 16.102983 | 0.608687 | 2016-07-01 | 21 | 2016ApJ...831..178R | [
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"gamma-ray burst: general",
"gamma-ray burst: individual: GRB 090510",
"Astrophysics - High Energy Astrophysical Phenomena",
"Astrophysics - Cosmology and Nongalactic Astrophysics"
] | 9 | [
"10.3847/0004-637X/831/2/178",
"10.48550/arXiv.1607.02400"
] | [
"Ruffini, R.",
"Muccino, M.",
"Aimuratov, Y.",
"Bianco, C. L.",
"Cherubini, C.",
"Enderli, M.",
"Kovacevic, M.",
"Moradi, R.",
"Penacchioni, A. V.",
"Pisani, G. B.",
"Rueda, J. A.",
"Wang, Y."
] | [
"Dipartimento di Fisica, Sapienza Università di Roma and ICRA, Piazzale Aldo Moro 5, I-00185 Roma, Italy ; ICRANet, Piazza della Repubblica 10, I-65122 Pescara, Italy ; Université de Nice Sophia-Antipolis, Grand Château Parc Valrose, Nice, CEDEX 2, France ; ICRANet-Rio, Centro Brasileiro de Pesquisas Fisicas, Rua D... | [
"2016ApJ...832..136R",
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12472712 | 1607.07822 | Blazar flaring patterns (B-FlaP) classifying blazar candidate of uncertain type in the third Fermi-LAT catalogue by artificial neural networks | The Fermi-Large Area Telescope (LAT) is currently the most important facility for investigating the GeV γ-ray sky. With Fermi-LAT, more than three thousand γ-ray sources have been discovered so far. 1144 (∼40 per cent) of the sources are active galaxies of the blazar class, and 573 (∼20 per cent) are listed as blazar candidate of uncertain type (BCU), or sources without a conclusive classification. We use the empirical cumulative distribution functions and the artificial neural networks for a fast method of screening and classification for BCUs based on data collected at γ-ray energies only, when rigorous multiwavelength analysis is not available. Based on our method, we classify 342 BCUs as BL Lacs and 154 as flat-spectrum radio quasars, while 77 objects remain uncertain. Moreover, radio analysis and direct observations in ground-based optical observatories are used as counterparts to the statistical classifications to validate the method. This approach is of interest because of the increasing number of unclassified sources in Fermi catalogues and because blazars and in particular their subclass high synchrotron peak objects are the main targets of atmospheric Cherenkov telescopes. | [
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0.0... | 16.485292 | 4.53846 | 2016-07-01 | 48 | 2016MNRAS.462.3180C | [
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"methods: statistical",
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"Astrophysics - High Energy Astrophysical Phenomena"
] | 12 | [
"10.1093/mnras/stw1830",
"10.48550/arXiv.1607.07822"
] | [
"Chiaro, G.",
"Salvetti, D.",
"La Mura, G.",
"Giroletti, M.",
"Thompson, D. J.",
"Bastieri, D."
] | [
"Dip. Fisica and Astronomia G. Galilei - Università di Padova, I-35131 Padova, Italy",
"INAF-Istituto di Astrofisica Spaziale e Fisica Cosmica, I-20133 Milano, Italy",
"Dip. Fisica and Astronomia G. Galilei - Università di Padova, I-35131 Padova, Italy",
"INAF-Institute of Radioastronomy, I-40129 Bologna, Ita... | [
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12471923 | 1607.06129 | Braking indices of pulsars obtained in the presence of an effective force | Braking indices of pulsars present a scientific challenge as their theoretical calculation is still an open problem. In this paper, we report results of a study regarding such calculation which adapts the canonical model (which admits that pulsars are rotating magnetic dipoles) basically by introducing a compensating component in the energy conservation equation of the system. This component would correspond to an effective force that varies with the first power of the tangential velocity of the pulsar's crust. We test the proposed model using data available and predict braking indices values for different stars. We comment on the high braking index recently measured of the pulsar J1640-4631. | [
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-0... | 5.495424 | 3.660727 | 2016-07-01 | 10 | 2016MNRAS.461.3993M | [
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"PSR B0540-69",
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"Astrophysics - High Energy Astrophysical Phenomena",
"As... | 2 | [
"10.1093/mnras/stw1636",
"10.48550/arXiv.1607.06129"
] | [
"Magalhaes, N. S.",
"Okada, A. S.",
"Frajuca, C."
] | [
"Department of Exact and Earth Sciences, Federal University of Sao Paulo Rua Sao Nicolau 210, Diadema, SP 09913-030, Brazil",
"Scientific Initiation Program, Federal University of Sao Paulo Rua Sao Nicolau 210, Diadema, SP 09913-030, Brazil",
"Federal Institute of Education, Science and Technology of Sao Paulo ... | [
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12595569 | 1607.01824 | The infrared-dark dust content of high redshift galaxies | We present a theoretical model aimed at explaining the IRX-β relation for high redshift (z ≳ 5) galaxies. Recent observations have shown that early Lyman-Break Galaxies, although characterized by a large ultraviolet (UV) attenuation (e.g. flat UV β slopes), show a striking far-infrared (FIR) deficit, I.e. they are `infrared-dark'. This marked deviation from the local IRX-β relation can be explained by the larger molecular gas content of these systems. While dust in the diffuse interstellar medium attains relatively high temperatures (T<SUB>d</SUB> ≃ 45 K for typical size a = 0.1 μm; smaller grains can reach T<SUB>d</SUB> ≳ 60 K), a sizable fraction of the dust mass is embedded in dense gas, and therefore remains cold. If confirmed, the FIR deficit might represent a novel, powerful indicator of the molecular content of high-z galaxies which can be used to pre-select candidates for follow-up deep CO observations. Thus, high-z CO line searches with ALMA might be much more promising than currently thought. | [
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"typical size",
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"high-z galaxies",
"early Lyman-Break Galaxies",
"Lyman-Break Galaxies",
"FIR",
"ALMA",
... | [
"dust",
"extinction",
"Astrophysics - Astrophysics of Galaxies"
] | 5 | [
"10.1093/mnras/stx1898",
"10.48550/arXiv.1607.01824"
] | [
"Ferrara, A.",
"Hirashita, H.",
"Ouchi, M.",
"Fujimoto, S."
] | [
"Scuola Normale Superiore, Piazza dei Cavalieri 7, I-56126 Pisa, Italy; Kavli IPMU, WPI, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan",
"Institute of Astronomy and Astrophysics, Academia Sinica, No. 1, Sec. 4, Roosevelt Rd., Taipei 10617, Taiwan",
"Institute for Cosmic Ray Research, The University of... | [
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12473132 | 1607.08591 | Tidal spin down rates of homogeneous triaxial viscoelastic bodies | We use numerical simulations to measure the sensitivity of the tidal spin-down rate of a homogeneous triaxial ellipsoid to its axis ratios by comparing the drift rate in orbital semimajor axis to that of a spherical body with the same mass, volume and simulated rheology. We use a mass-spring model approximating a viscoelastic body spinning around its shortest body axis, with spin aligned with orbital spin axis, and in circular orbit about a point mass. The torque or drift rate can be estimated from that predicted for a sphere with equivalent volume if multiplied by 0.5 (1 + b^4/a^4)(b/a)^{-4/3} (c/a)^{-α _c} where b/a and c/a are the body axis ratios and index α<SUB>c</SUB> ≈ 1.05 is consistent with the random lattice mass-spring model simulations but α<SUB>c</SUB> = 4/3 suggested by scaling estimates. A homogeneous body with axis ratios 0.5 and 0.8, like Haumea, has orbital semimajor axis drift rate about twice as fast as a spherical body with the same mass, volume and material properties. A simulation approximating a mostly rocky body but with 20 per cent of its mass as ice concentrated at its ends has a drift rate 10 times faster than the equivalent homogeneous rocky sphere. However, this increase in drift rate is not enough to allow Haumea's satellite, Hi'iaka, to have tidally drifted away from Haumea to its current orbital semimajor axis. | [
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-0.01... | 8.380346 | 14.843683 | 2016-07-01 | 15 | 2016MNRAS.463.1543Q | [
"orbital semimajor axis drift rate",
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"its current orbital semimajor axis",
"its shortest body axis",
"estimates",
"Haumea",
"spin",
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"c</SUB",
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"planets and satellites: dynamical evolution and stability",
"Planetary Systems",
"minor planets",
"asteroids",
"general",
"asteroids: individual: Haumea",
"asteroids: general",
"Astrophysics - Earth and Planetary Astrophysics"
] | 4 | [
"10.1093/mnras/stw2094",
"10.48550/arXiv.1607.08591"
] | [
"Quillen, Alice C.",
"Kueter-Young, Andrea",
"Frouard, Julien",
"Ragozzine, Darin"
] | [
"Department of Physics and Astronomy, University of Rochester, Rochester, NY 14627, USA",
"Department of Physics and Astronomy, University of Rochester, Rochester, NY 14627, USA; Physics Department, Siena College, Loudonville, NY 12211, USA,",
"US Naval Observatory, 3450 Massachusetts Ave NW, Washington DC 2039... | [
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5100913 | 1607.06773 | The ALMA Spectroscopic Survey in the Hubble Ultra Deep Field: Implications for Spectral Line Intensity Mapping at Millimeter Wavelengths and CMB Spectral Distortions | We present direct estimates of the mean sky brightness temperature in observing bands around 99 and 242 GHz due to line emission from distant galaxies. These values are calculated from the summed line emission observed in a blind, deep survey for spectral line emission from high redshift galaxies using ALMA (the ALMA spectral deep field observations “ASPECS” survey). In the 99 GHz band, the mean brightness will be dominated by rotational transitions of CO from intermediate and high redshift galaxies. In the 242 GHz band, the emission could be a combination of higher order CO lines, and possibly [C II] 158 μm line emission from very high redshift galaxies (z ∼ 6-7). The mean line surface brightness is a quantity that is relevant to measurements of spectral distortions of the cosmic microwave background, and as a potential tool for studying large-scale structures in the early universe using intensity mapping. While the cosmic volume and the number of detections are admittedly small, this pilot survey provides a direct measure of the mean line surface brightness, independent of conversion factors, excitation, or other galaxy formation model assumptions. The mean surface brightness in the 99 GHZ band is: T <SUB> B </SUB> = 0.94 ± 0.09 μK. In the 242 GHz band, the mean brightness is: T <SUB> B </SUB> = 0.55 ± 0.033 μK. These should be interpreted as lower limits on the average sky signal, since we only include lines detected individually in the blind survey, while in a low resolution intensity mapping experiment, there will also be the summed contribution from lower luminosity galaxies that cannot be detected individually in the current blind survey. | [
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... | 13.151997 | 7.511482 | 2016-07-01 | 28 | 2016ApJ...833...73C | [
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"distant galaxies",
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"lines",
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"cosmic background radiation",
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"reionization",
"first stars",
"galaxies: formation",
"molecular data",
"radio lines: general",
"techniques: imaging spectroscopy",
"Astrophysics - Astrophysics of Galaxies"
] | 9 | [
"10.3847/1538-4357/833/1/73",
"10.48550/arXiv.1607.06773"
] | [
"Carilli, C. L.",
"Chluba, J.",
"Decarli, R.",
"Walter, F.",
"Aravena, M.",
"Wagg, J.",
"Popping, G.",
"Cortes, P.",
"Hodge, J.",
"Weiss, A.",
"Bertoldi, F.",
"Riechers, D."
] | [
"National Radio Astronomy Observatory, P.O. Box 0, Socorro, NM 87801, USA ; Astrophysics Group, Cavendish Laboratory, JJ Thomson Avenue, Cambridge CB3 0HE, UK;",
"Jodrell Bank Centre for Astrophysics, University of Manchester, Oxford Road, M13 9PL, UK",
"Max-Planck Institute for Astronomy, D-69117 Heidelberg, G... | [
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12434275 | 1607.01365 | Second order singular pertubative theory for gravitational lenses | The extension of the singular perturbative approach to the second order is presented in this paper. The general expansion to the second order is derived. The second order expansion is considered as a small correction to the first order expansion. Using this approach it is demonstrated that the second order expansion is reducible to a first order expansion via a re-definition of the first order pertubative fields. Even if in practice the second order correction is small the reducibility of the second order expansion to the first order expansion indicates a degeneracy problem. In general this degeneracy is hard to break. A useful and simple second order approximation is the thin source approximation which offers a direct estimation of the correction. The practical application of the corrections derived in this paper are illustrated by using an elliptical NFW lens model. The second order pertubative expansion provides a noticeable improvement, even for the simplest case of thin source approximation. To conclude it is clear that for accurate modelisation of gravitational lenses using the perturbative method the second order perturbative expansion should be considered. In particular an evaluation of the degeneracy due to the second order term should be performed, for which the thin source approximation is particularly useful. | [
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0.... | 12.600745 | 3.706642 | 2016-07-01 | 1 | 2016arXiv160701365A | [
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"Astrophysics - Astrophysics of Galaxies",
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] | 3 | [
"10.48550/arXiv.1607.01365"
] | [
"Alard, C."
] | [
"-"
] | [
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12593827 | 1607.07296 | Matter density perturbation and power spectrum in running vacuum model | We investigate the matter density perturbation δ<SUB>m</SUB> and power spectrum P(k) in the running vacuum model, with the cosmological constant being a function of the Hubble parameter, given by Λ = Λ<SUB>0</SUB> + 6σHH<SUB>0</SUB> + 3νH<SUP>2</SUP>, in which the linear and quadratic terms of H would originate from the QCD vacuum condensation and cosmological renormalization group, respectively. Taking the dark energy perturbation into consideration, we derive the evolution equation for δ<SUB>m</SUB> and find a specific scale d<SUB>cr</SUB> = 2π/k<SUB>cr</SUB>, which divides the evolution of the universe into the sub-interaction and super-interaction regimes, corresponding to k ≪ k<SUB>cr</SUB> and k ≫ k<SUB>cr</SUB>, respectively. For the former, the evolution of δ<SUB>m</SUB> has the same behaviour as that in the Λ cold dark model, while for the latter, the growth of δ<SUB>m</SUB> is frozen (greatly enhanced) when ν + σ > (<)0 due to the couplings between radiation, matter and dark energy. It is clear that the observational data rule out the cases with ν < 0 and ν + σ < 0, while the allowed window for the model parameters is extremely narrow with ν , |σ | ≲ O(10^{-7}). | [
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... | 10.913698 | 0.603303 | 2016-07-01 | 5 | 2017MNRAS.464.2462G | [
"k",
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"Λ",
"<SUB>cr</SUB",
"energy",
"the dark... | [
"dark energy",
"Astrophysics - Cosmology and Nongalactic Astrophysics",
"General Relativity and Quantum Cosmology"
] | 4 | [
"10.1093/mnras/stw2549",
"10.48550/arXiv.1607.07296"
] | [
"Geng, Chao-Qiang",
"Lee, Chung-Chi"
] | [
"Chongqing University of Posts and Telecommunications, Chongqing 400065, China; National Center for Theoretical Sciences, Hsinchu, Taiwan 30043, Republic of China; Department of Physics, National Tsing Hua University, Hsinchu, Taiwan 30013, Republic of China",
"National Center for Theoretical Sciences, Hsinchu, T... | [
"2017JCAP...08..026P",
"2017JCAP...08..032G",
"2019ChPhC..43b5102Z",
"2020ChPhC..44j5104G",
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12408329 | 1607.02150 | Foreground Bias from Parametric Models of Far-IR Dust Emission | We use simple toy models of far-IR dust emission to estimate the accuracy to which the polarization of the cosmic microwave background can be recovered using multi-frequency fits, if the parametric form chosen for the fitted dust model differs from the actual dust emission. Commonly used approximations to the far-IR dust spectrum yield CMB residuals comparable to or larger than the sensitivities expected for the next generation of CMB missions, despite fitting the combined CMB + foreground emission to precision 0.1% or better. The Rayleigh-Jeans approximation to the dust spectrum biases the fitted dust spectral index by {{Δ }}{β }<SUB>d</SUB>=0.2 and the inflationary B-mode amplitude by {{Δ }}r=0.03. Fitting the dust to a modified blackbody at a single temperature biases the best-fit CMB by {{Δ }}r\gt 0.003 if the true dust spectrum contains multiple temperature components. A 13-parameter model fitting two temperature components reduces this bias by an order of magnitude if the true dust spectrum is in fact a simple superposition of emission at different temperatures, but fails at the level {{Δ }}r=0.006 for dust whose spectral index varies with frequency. Restricting the observing frequencies to a narrow region near the foreground minimum reduces these biases for some dust spectra but can increase the bias for others. Data at THz frequencies surrounding the peak of the dust emission can mitigate these biases while providing a direct determination of the dust temperature profile. | [
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... | 13.134475 | 1.697792 | 2016-07-01 | 11 | 2016ApJ...826..101K | [
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"cosmology: observations",
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"Astrophysics - Cosmology and Nongalactic Astrophysics"
] | 3 | [
"10.3847/0004-637X/826/2/101",
"10.48550/arXiv.1607.02150"
] | [
"Kogut, A.",
"Fixsen, D. J."
] | [
"Code 665, Goddard Space Flight Center, Greenbelt, MD 20771, USA",
"Code 665, Goddard Space Flight Center, Greenbelt, MD 20771, USA; University of Maryland, College Park, MD 20742, USA"
] | [
"2016PhRvD..94h3526S",
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2426651 | 1607.00013 | ZFIRE: A KECK/MOSFIRE Spectroscopic Survey of Galaxies in Rich Environments at z ∼ 2 | We present an overview and the first data release of ZFIRE, a spectroscopic redshift survey of star-forming galaxies that utilizes the MOSFIRE instrument on Keck-I to study galaxy properties in rich environments at 1.5 < z < 2.5. ZFIRE measures accurate spectroscopic redshifts and basic galaxy properties derived from multiple emission lines. The galaxies are selected from a stellar mass limited sample based on deep near infrared imaging ({K}<SUB>{AB</SUB>}\lt 25) and precise photometric redshifts from the ZFOURGE and UKIDSS surveys as well as grism redshifts from 3DHST. Between 2013 and 2015, ZFIRE has observed the COSMOS and UDS legacy fields over 13 nights and has obtained 211 galaxy redshifts over 1.57 < z < 2.66 from a combination of nebular emission lines (such as Hα, [N II], Hβ, [O II], [O III], and [S II]) observed at 1-2 μm. Based on our medium-band near infrared photometry, we are able to spectrophotometrically flux calibrate our spectra to ∼10% accuracy. ZFIRE reaches 5σ emission line flux limits of ∼3 × 10<SUP>-18</SUP> erg s<SUP>-1</SUP> cm<SUP>-2</SUP> with a resolving power of R = 3500 and reaches masses down to ∼10<SUP>9</SUP> M <SUB>⊙</SUB>. We confirm that the primary input survey, ZFOURGE, has produced photometric redshifts for star-forming galaxies (including highly attenuated ones) accurate to {{Δ }}z/(1+{z}<SUB>{spec</SUB>})=0.015 with 0.7% outliers. We measure a slight redshift bias of <0.001, and we note that the redshift bias tends to be larger at higher masses. We also examine the role of redshift on the derivation of rest-frame colors and stellar population parameters from SED fitting techniques. The ZFIRE survey extends spectroscopically confirmed z ∼ 2 samples across a richer range of environments, here we make available the first public release of the data for use by the community.<SUP>7</SUP> | [
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-... | 12.685656 | 7.040785 | 2016-07-01 | 63 | 2016ApJ...828...21N | [
"photometric redshifts",
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"lt",
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"catalogs",
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"galaxies: distances and redshifts",
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"galaxies: high-redshift",
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] | 18 | [
"10.3847/0004-637X/828/1/21",
"10.48550/arXiv.1607.00013"
] | [
"Nanayakkara, Themiya",
"Glazebrook, Karl",
"Kacprzak, Glenn G.",
"Yuan, Tiantian",
"Tran, Kim-Vy",
"Spitler, Lee",
"Kewley, Lisa",
"Straatman, Caroline",
"Cowley, Michael",
"Fisher, David",
"Labbe, Ivo",
"Tomczak, Adam",
"Allen, Rebecca",
"Alcorn, Leo"
] | [
"Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia",
"Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia",
"Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawth... | [
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1797939 | 1607.03427 | Propeller Effect in the Transient X-Ray Pulsar SMC X-2 | We report the results of the monitoring campaign of the transient X-ray pulsar SMC X-2 performed with the Swift/XRT telescope over the period of 2015 September-2016 January during the Type II outburst. During this event, the bolometric luminosity of the source ranged from ≃10<SUP>39</SUP> down to several ×10<SUP>34</SUP> erg s<SUP>-1</SUP>. Moreover, we discovered its dramatic drop by a factor of more than 100 below the limiting value of {L}<SUB>{lim</SUB>}≃ 4× {10}<SUP>36</SUP> erg s<SUP>-1</SUP>, which can be interpreted as a transition to the propeller regime. These measurements make SMC X-2 the sixth pulsating X-ray source where such a transition is observed and allow us to estimate the magnetic field of the neutron star in the system B ≃ 3 × 10<SUP>12</SUP> G, which is in agreement with independent results of the spectral analysis. | [
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0... | 5.675789 | 5.937639 | 2016-07-01 | 33 | 2017ApJ...834..209L | [
"independent results",
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"several ×10<SUP>34</SUP> erg s",
"the spectral analysis",
"SUP>39</SUP",
"≃10",
"the system B",
"s... | [
"accretion",
"accretion disks",
"magnetic fields",
"stars: individual: SMC X-2",
"X-rays: binaries",
"Astrophysics - High Energy Astrophysical Phenomena"
] | 8 | [
"10.3847/1538-4357/834/2/209",
"10.48550/arXiv.1607.03427"
] | [
"Lutovinov, Alexander A.",
"Tsygankov, Sergey S.",
"Krivonos, Roman A.",
"Molkov, Sergey V.",
"Poutanen, Juri"
] | [
"Space Research Institute, Russian Academy of Sciences, Profsoyuznaya 84/32, 117997 Moscow, Russia; Moscow Institute of Physics and Technology, Moscow region, Dolgoprudnyi, Russia",
"Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Väisäläntie 20, FI-21500 Piikkiö, Finland",
"Space ... | [
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12409546 | 1607.08818 | An Opportunistic Search for Extraterrestrial Intelligence (SETI) with the Murchison Widefield Array | A spectral line image cube generated from 115 minutes of MWA data that covers a field of view of 400 sq, deg. around the Galactic Center is used to perform the first Search for ExtraTerrestrial Intelligence (SETI) with the Murchison Widefield Array (MWA). Our work constitutes the first modern SETI experiment at low radio frequencies, here between 103 and 133 MHz, paving the way for large-scale searches with the MWA and, in the future, the low-frequency Square Kilometre Array. Limits of a few hundred mJy beam<SUP>-1</SUP> for narrowband emission (10 kHz) are derived from our data, across our 400 sq. deg. field of view. Within this field, 45 exoplanets in 38 planetary systems are known. We extract spectra at the locations of these systems from our image cube to place limits on the presence of narrow line emission from these systems. We then derive minimum isotropic transmitter powers for these exoplanets; a small handful of the closest objects (10 s of pc) yield our best limits of order 10<SUP>14</SUP> W (Equivalent Isotropic Radiated Power). These limits lie above the highest power directional transmitters near these frequencies currently operational on Earth. A SETI experiment with the MWA covering the full accessible sky and its full frequency range would require approximately one month of observing time. The MWA frequency range, its southern hemisphere location on an extraordinarily radio quiet site, its very large field of view, and its high sensitivity make it a unique facility for SETI. | [
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"instrumentation: interferometers",
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] | 2 | [
"10.3847/2041-8205/827/2/L22",
"10.48550/arXiv.1607.08818"
] | [
"Tingay, S. J.",
"Tremblay, C.",
"Walsh, A.",
"Urquhart, R."
] | [
"International Centre for Radio Astronomy Research (ICRAR), Curtin University, Bentley, WA 6102, Australia ; Istituto di Radioastronomia, Istituto Nazionale di Astrofisica, I-40129 Bologna, Italy",
"International Centre for Radio Astronomy Research (ICRAR), Curtin University, Bentley, WA 6102, Australia",
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11492362 | 1607.06458 | Constraining the dark energy equation of state with H II galaxies | We use the H II galaxies L-σ relation and the resulting Hubble expansion cosmological probe of a sample of just 25 high-z (up to z ∼ 2.33) H II galaxies, in a joint likelihood analysis with other well tested cosmological probes (cosmic microwave background, CMB, Baryon Acoustic Oscillations, BAOs) in an attempt to constrain the dark energy equation of state (EoS). The constraints, although still weak, are in excellent agreement with those of a similar joint analysis using the well established SNIa Hubble expansion probe. Interestingly, even with the current small number of available high redshift H II galaxies, the H II/BAO/CMB joint analysis gives a 13 per cent improvement of the quintessence dark energy cosmological constraints compared to the BAO/CMB joint analysis. We have further performed extensive Monte Carlo simulations, with a realistic redshift sampling, to explore the extent to which the use of the L-σ relation, observed in H II galaxies, can constrain effectively the parameter space of the dark energy EoS. The simulations predict substantial improvement in the constraints when increasing the sample of high-z H II galaxies to 500, a goal that can be achieved in reasonable observing times with existing large telescopes and state-of-the-art instrumentation. | [
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0... | 11.586074 | 1.305392 | 2016-07-01 | 64 | 2016MNRAS.462.2431C | [
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] | 4 | [
"10.1093/mnras/stw1813",
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] | [
"Chávez, R.",
"Plionis, M.",
"Basilakos, S.",
"Terlevich, R.",
"Terlevich, E.",
"Melnick, J.",
"Bresolin, F.",
"González-Morán, A. L."
] | [
"Instituto Nacional de Astrofísica Óptica y Electrónica, AP 51 y 216, 72000 Puebla, México; Cavendish Laboratory, University of Cambridge, 19 J. J. Thomson Ave, Cambridge CB3 0HE, UK; Kavli Institute for Cosmology, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK",
"Physics Department, Aristotle Uni... | [
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2073369 | 1607.06172 | The Primordial Inflation Polarization Explorer (PIPER) | The Primordial Inflation Polarization ExploreR (PIPER) is a balloon-borne telescope designed to measure the polarization of the Cosmic Microwave Background on large angular scales. PIPER will map 85% of the sky at 200, 270, 350, and 600 GHz over a series of 8 conventional balloon flights from the northern and southern hemispheres. The first science flight will use two 32 × 40 arrays of backshort-under-grid transition edge sensors, multiplexed in the time domain, and maintained at 100 mK by a Continuous Adiabatic Demagnetization Refrigerator. Front- end cryogenic Variable-delay Polarization Modulators provide systematic control by rotating linear to circular polarization at 3 Hz. Twin telescopes allow PIPER to measure Stokes I, Q, U , and V simultaneously. The telescope is maintained at 1.5 K in an LHe bucket dewar. Cold optics and the lack of a warm window permit sensitivity at the sky-background limit. The ultimate science target is a limit on the tensor-to-scalar ratio of r ∼ 0.007, from the reionization bump to l ∼ 300. PIPER's first flight will be from the Northern hemisphere, and overlap with the CLASS survey at lower frequencies. We describe the current status of the PIPER instrument. | [
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"10.1117/12.2231109",
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"Gandilo, Natalie N.",
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"Chuss, David T.",
"Dotson, Jessie L.",
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"Fixsen, Dale J.",
"Halpern, Mark",
"Hilton, Gene",
"Hinshaw, Gary F.",
"Irwin, Kent",
"Jhabvala, Christine",
"Kimball, Mark",
"Kogut, Alan",
... | [
"Johns Hopkins Univ. (United States)",
"Cardiff Univ. (United Kingdom)",
"NASA Goddard Space Flight Ctr. (United States)",
"Johns Hopkins Univ. (United States)",
"Villanova Univ. (United States)",
"NASA Ames Research Ctr. (United States)",
"Johns Hopkins Univ. (United States)",
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12408854 | 1607.06491 | Radiation and Polarization Signatures of the 3D Multizone Time-dependent Hadronic Blazar Model | We present a newly developed time-dependent three-dimensional multizone hadronic blazar emission model. By coupling a Fokker-Planck-based lepto-hadronic particle evolution code, 3DHad, with a polarization-dependent radiation transfer code, 3DPol, we are able to study the time-dependent radiation and polarization signatures of a hadronic blazar model for the first time. Our current code is limited to parameter regimes in which the hadronic γ-ray output is dominated by proton synchrotron emission, neglecting pion production. Our results demonstrate that the time-dependent flux and polarization signatures are generally dominated by the relation between the synchrotron cooling and the light-crossing timescale, which is largely independent of the exact model parameters. We find that unlike the low-energy polarization signatures, which can vary rapidly in time, the high-energy polarization signatures appear stable. As a result, future high-energy polarimeters may be able to distinguish such signatures from the lower and more rapidly variable polarization signatures expected in leptonic models. | [
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... | 16.577076 | 5.100655 | 2016-07-01 | 30 | 2016ApJ...829...69Z | [
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"the first time",
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"galaxies: active",
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] | 4 | [
"10.3847/0004-637X/829/2/69",
"10.48550/arXiv.1607.06491"
] | [
"Zhang, Haocheng",
"Diltz, Chris",
"Böttcher, Markus"
] | [
"Department of Physics and Astronomy, University of New Mexico, Albuquerque, NM 87131, USA ; Theoretical Division, Los Alamos National Laboratory, Los Alamos, NM 87545, USA",
"Astrophysical Institute, Department of Physics and Astronomy, Ohio University, Athens, OH 45701, USA",
"Centre for Space Research, North... | [
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12500420 | 1607.00879 | Origin of the characteristic X-ray spectral variations of IRAS 13224-3809 | The narrow-line Seyfert 1 galaxy (NLS1) IRAS 13224-3809 is known to exhibit significant X-ray spectral variation, a sharp spectral drop at ∼7 keV, strong soft excess emission, and a hint of an iron L-edge feature, which is very similar to the NLS1 1H 0707-495. We have proposed the "Variable Double Partial Covering (VDPC) model" to explain the energy spectra and spectral variability of 1H 0707-495 (Mizumoto et al. 2014, PASJ, 66, 122). In this model, the observed flux/spectral variations below 10 keV within ∼ a day are primarily caused by change of the partial covering fraction of patchy clouds composed by double absorption layers in the line of sight. In this paper, we apply the VDPC model to IRAS 13224-3809. Consequently, we have found that the VDPC model can explain the observed spectral variations of IRAS 13224-3809 in the 0.5-10 keV band. In particular, we can explain the observed root mean square (RMS) spectra (energy dependence of the fractional flux variation) in the entire 0.5-10 keV band. In addition to the well-known significant drop in the iron K-band, we have found intriguing iron L-peaks in the RMS spectra when the iron L-edge is particularly deep. This feature, which is also found in 1H 0707-495, is naturally explained with the VDPC model, such that the RMS variations increase at the energies where optical depths of the partial absorbers are large. The absorbers have a larger optical depth at the iron L-edge than in the adjacent energy bands, and thus a characteristic iron L-peak appears. On the other hand, just below the iron K-edge, the optical depth is the lowest and the RMS spectrum has a broad dip. | [
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] | 3 | [
"10.1093/pasj/psw070",
"10.48550/arXiv.1607.00879"
] | [
"Yamasaki, Hiroki",
"Mizumoto, Misaki",
"Ebisawa, Ken",
"Sameshima, Hiroaki"
] | [
"Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa 252-5210, Japan; Department of Astronomy, Graduate School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan",
"Institute of Space and Astronautical Sc... | [
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