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12473133 | [
"Arca-Sedda, M.",
"Capuzzo-Dolcetta, R."
] | 2016MNRAS.461.4335A | [
"Globular clusters as tracers of the host galaxy mass distribution: the Fornax dSph test case"
] | 17 | [
"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"
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] | 1607 | 1607.01526_arXiv.txt | The Fornax galaxy is the brightest dwarf spheroidal galaxy (dSph) satellite of the Milky Way (MW) and is, among all of the MW satellites, the only one that hosts five globular clusters, located within $1$ kpc from its center, named Fornax 1,2,3,4 and 5. Moreover, Fornax does not show any bright nucleus. As the other M... | \label{end} In this paper we revisited the so called ``timing problem'' for the stellar clusters in the Fornax dwarf spheroidal galaxy. Using two complementary approaches, a simple semi-analytic investigation of the dynamical friction decay times and a more sophisticated and detailed series of numerical simulations for... | 16 | 7 | 1607.01526 | 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 signi... | false | [
"cuspy density profiles",
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"a huge dark matter halo",
"a standard density profile",
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... | 10.009286 | 7.42452 | 167 |
5209849 | [
"Colombo, S.",
"Orlando, S.",
"Peres, G.",
"Argiroffi, C.",
"Reale, F."
] | 2016A&A...594A..93C | [
"Impacts of fragmented accretion streams onto classical T Tauri stars: UV and X-ray emission lines"
] | 15 | [
"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,... | [
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"2019ASSP...55...43O",
"2019arXiv190409156D",
"2020A&A...640A.... | [
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] | 3 | [
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"10.1051/0004-6361/201628858",
"10.48550/arXiv.1607.03009"
] | 1607 | 1607.03009_arXiv.txt | Classical T Tauri Stars (CTTS) are young stars surrounded by \salvo{an accretion} disk. \salvo{According to the magnetospheric accretion scenario, gas from the disk accretes onto the star through accretion columns \citep{1991Apj...370L..39K}. Several lines of evidence support this picture especially in the optical and ... | \label{sec4} In this work we investigated the effects of \salvo{stream fragmentation} on C\,IV and O\,VIII emission lines. We developed a model that describes \salvo{a stream composed by a series of dense blobs} impacting onto the surface of a CTTS. Our model \salvo{takes} into account the stellar magnetic field, the ... | 16 | 7 | 1607.03009 | 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... | false | [
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... | 9.324092 | 12.202207 | 147 |
12586989 | [
"Schmidtmann, Birte",
"Winters, Andrew R."
] | 2017JCoPh.330..566S | [
"Hybrid entropy stable HLL-type Riemann solvers for hyperbolic conservation laws"
] | 7 | [
"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",
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"2021ApJS..257...24L",
"2021ApJS..257...34F",
"2022JCoPh.46811521W",
"2023JCoPh.49312505H"
] | [
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"10.1016/j.jcp.2016.10.034",
"10.48550/arXiv.1607.06240"
] | 1607 | 1607.06240_arXiv.txt | We consider the numerical solution of systems of hyperbolic conservation laws of the form \begin{equation} \label{eq:hypLaw} \pderivative{\vec{q}}{t} + \nabla\cdot\vec{f} = 0, \end{equation} on a domain $\Omega$. For a one-dimensional approximation we divide $\Omega$ into $K$ non-overlapping grid cells $C_i = [x_{i-1/2... | \label{scn:Conclusion} In this work we constructed two one-parameter families of hybrid entropy stable numerical fluxes. An advantage of the new numerical flux functions is that they remain applicable even when the eigenstructure of the flux Jacobian matrix is unknown. % The derivations and proofs in this work are kept... | 16 | 7 | 1607.06240 | 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 ... | false | [
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"several HLL-type Riemann solvers",
"hybrid HLL-type methods",
"HLL-type schemes",... | 8.789782 | 4.468701 | 28 |
168897 | [
"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."
] | 2013Icar..223..460S | [
"Dynamics of Saturn’s great storm of 2010-2011 from Cassini ISS and RPWS"
] | 74 | [
"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",
... | [
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"2014Natur.505..625S",
"2015A&A...580A.... | [
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] | 18 | [
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"10.1016/j.icarus.2012.12.013",
"10.48550/arXiv.1607.07246"
] | 1607 | 1607.07246_arXiv.txt | } Cumulus convecting storms on Saturn are known for their episodic behavior. Convective events on Saturn can be identified visually and through radio noise. The events occur intermittently within a small range of latitudes and are interspersed with quiescent periods that last for a year or longer \citep{Sromovsky_etal_... | We have reported the evolution of Saturn's latest planet-encircling storm of 2010-2011 using two of the instruments aboard Cassini spacecraft, ISS and RPWS. Our observational coverage enabled us to study the preconditions of the storm, in which we show that the storm erupted out of a previously known feature called the... | 16 | 7 | 1607.07246 | 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 spacecra... | false | [
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"... | 8.50624 | 15.511942 | 96 |
12408831 | [
"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."
] | 2016ApJ...830..141L | [
"Observed Variability at 1 and 4 μm in the Y0 Brown Dwarf WISEP J173835.52+273258.9"
] | 31 | [
"Gemini Observatory, Northern Operations Center, 670 N. A'ohoku Place, Hilo, HI 96720, USA",
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"The University of Toledo, 2801 West Bancroft Street, Mailstop 111, Toledo, OH 43606, USA",
"The University of Toledo, 2801 W... | [
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"2019ApJ...874..111T",
"2019ApJ...875L..15M",
"2019ApJ...877..... | [
"astronomy"
] | 10 | [
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"10.3847/0004-637X/830/2/141",
"10.48550/arXiv.1607.07888"
] | 1607 | 1607.07888_arXiv.txt | There are now more than twenty brown dwarfs known in the solar neighborhood that have effective temperatures ($T_{\rm eff}$) lower than 500~K (Cushing et al. 2011, 2014; Kirkpatrick et al. 2012; Liu et al. 2012; Luhman 2014; Luhman, Burgasser \& Bochanski 2011, Pinfield et al. 2014; Schneider et al. 2015; Tinney et al... | We obtained 12 hours of continuous {\em Spitzer} data on the Y0 brown dwarf W1738 at [3.6], followed by another 12 hours at [4.5]. Two sets of data were obtained four months apart, on June 30 and October 30 2013. We also obtained interspersed Gemini $Y$ and $J$ data on W1738, with about 1.4 hours on-source at $Y$ and 2... | 16 | 7 | 1607.07888 | 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 Observat... | false | [
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"the solar system gas giants",
"a ∼3.0 hr period",
"Gemini... | 7.209815 | 12.589618 | 102 |
12518466 | [
"Bentum, Mark J.",
"Bonetti, Luca",
"Spallicci, Alessandro D. A. M."
] | 2017AdSpR..59..736B | [
"Dispersion by pulsars, magnetars, fast radio bursts and massive electromagnetism at very low radio frequencies"
] | 28 | [
"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... | [
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"2019arXiv191206288S",
"2020RAA....20..... | [
"astronomy",
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] | 6 | [
"Photons",
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"Astrophysics - High Energy Astrophysical Phenomena",
"General Relativity and Quantum Cosmology",
"High Energy Physics - Phenomenology"
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"10.1016/j.asr.2016.10.018",
"10.48550/arXiv.1607.08820"
] | 1607 | 1607.08820_arXiv.txt | For many years, many of us have worked, see {\it e.g.}, \cite{spalliccietal2005}, for the opening of one of the gravitational wave windows on the universe, that has finally occurred \cite{abbottetal2016}, while for other windows we still have to wait \cite{spallicci2013}. Nevertheless, we can genuinely state that even ... | We have focused on the interest raised by the newly operating and future ground and space detectors at very low radio frequencies. The foundations of electromagnetism could be tested, confirming our beliefs or else contributing to establish new physics. Studies on dispersion appear crucial to unveil the causes of the e... | 16 | 7 | 1607.08820 | 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), somet... | false | [
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"solar maxima",
"new avenues",
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... | 6.506097 | 3.84499 | -1 |
12406228 | [
"Eistrup, Christian",
"Walsh, Catherine",
"van Dishoeck, Ewine F."
] | 2016A&A...595A..83E | [
"Setting the volatile composition of (exo)planet-building material. Does chemical evolution in disk midplanes matter?"
] | 146 | [
"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,... | [
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"10.1051/0004-6361/201628509",
"10.48550/arXiv.1607.06710"
] | 1607 | 1607.06710_arXiv.txt | \label{intr} The discovery of more than 2000 extrasolar planets by the radial velocity and transiting techniques \citep[e.g.,][]{udry2007,borucki2011,batalha2013,fischer2014} has signaled the next phase in exoplanet research: the characterization of their atmospheres. Simple molecules such as CO, \ce{H2O} and perhaps ... | \label{conclusions} The models presented in this work have examined the importance of kinetic chemistry on the molecular composition (gas and ice) in protoplanetary disk midplanes. The main conclusions are listed below. \begin{itemize} \item The disk midplane composition reflects that of interstellar ices only for t... | 16 | 7 | 1607.06710 | 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 t... | false | [
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"key volatile species",
"CO. H<SUB>2</SUB>O ice",
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2774767 | [
"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... | 2016AJ....152...83L | [
"The Data Reduction Pipeline for the SDSS-IV MaNGA IFU Galaxy Survey"
] | 359 | [
"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... | [
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"10.3847/0004-6256/152/4/83",
"10.48550/arXiv.1607.08619"
] | 1607 | 1607.08619.txt | Over the last twenty years, multiplexed spectroscopic surveys have been valuable tools for bringing the power of statistics to bear on the study of galaxy formation. Using large samples of tens to hundreds of thousands of galaxies with optical spectroscopy from the Sloan Digital Sky Survey \citep{york00,dr1.ref} for i... | \label{summary.sec} The 13th data release of the Sloan Digital Sky Survey includes the raw MaNGA spectroscopic data, the fully reduced spectrophotometrically calibrated data, and the pipeline software and metadata required for individual users to re-reduce the data themselves. In this work, we have described the frame... | 16 | 7 | 1607.08619 | 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</SU... | false | [
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12585901 | [
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"Department of Physics and Astronomy, Seoul National University Seoul 151-747, Korea",
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12593510 | [
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] | 1607 | 1607.05713_arXiv.txt | \label{sec:introduction} All-sky mid-infrared surveys have revolutionized the science of planet formation by discovering populations of young stars and main sequence stars with excess infrared radiation indicating the presence of dusty circumstellar disks. These disks, which include gas-rich protoplanetary disks aroun... | \label{sec:conclusions} We have outlined and demonstrated a novel process for identifying new candidate circumstellar disks in the WISE survey data. This paper reports only results from the first 10\% of the search, so it might be premature to try to derive any statistically meaningful inferences about the population... | 16 | 7 | 1607.05713 | 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 onli... | false | [
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12406007 | [
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] | 2016A&A...594A..74C | [
"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"
] | 1 | [
"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... | [
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] | 1607 | 1607.07534_arXiv.txt | \begin{figure*} \centering \includegraphics[width=\textwidth]{figs/HST_image.eps} \caption{Left panel: {\it HST-NICMOS 2} image of the BR1202-0725 system, using the F160W filter, covering the SINFONI FoV of $8\arcsec \times 8\arcsec$. White crosses mark the positions of the SMG, quasar, Ly$\alpha1$ and Ly$\alpha2$ as l... | \label{conc} In this work we presented deep SINFONI {\it K}-band integral field spectroscopy of two SMG systems at $z \sim 5$, BR1202-0725 and J1000+0234. BR1202-0725 consists of the SMG, a QSO and two LAEs while J1000+0234 appears to have a complex extended structure as traced by multiband optical and near-infrared i... | 16 | 7 | 1607.07534 | 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 ... | false | [
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1093440 | [
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"Algaba, Juan-Carlos",
"Yun, Youngjoo",
"Jung, Taehyun",
"Byun, Do-Young"
] | 2016JKAS...49..137H | [
"The Automatic Calibration of Korean VLBI Network Data"
] | 20 | [
"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",
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"10.5303/JKAS.2016.49.4.137",
"10.48550/arXiv.1607.07969"
] | 1607 | 1607.07969_arXiv.txt | } The calibration and analysis of Very Long Baseline Interferometry (VLBI) data has long been a time consuming process. However, with increases in computing power and hardware, it is becoming increasingly feasible to largely automate the process. The Korean VLBI Network (KVN) is an homogeneous radio array comprising o... | } The KVN pipeline has demonstrated its ability to automatically reduce a single polarisation KVN datset without direct human intervention. The performance of the KVN Pipeline is consistently superiour to manually reduced data without FPT being applied. While the KVN is a simple network consisting of 3 identical teles... | 16 | 7 | 1607.07969 | 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 frequ... | false | [
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11492261 | [
"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,... | 2016ApJ...831..133H | [
"The Eruption of the Candidate Young Star ASASSN-15QI"
] | 21 | [
"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... | [
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"10.3847/0004-637X/831/2/133",
"10.48550/arXiv.1607.06368"
] | 1607 | 1607.06368_arXiv.txt | Large brightness changes of young stars were seen long before the class of objects was understood to be related to star formation, or even that stars formed \citep{hind,ceraski06}. The largest and most prominent physical changes are decades-long bursts of accretion at rates of $10^{-4}-10^{-5}$ M$_\odot$ yr$^{-1}$, c... | 16 | 7 | 1607.06368 | 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 ... | false | [
"young stars",
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2246995 | [
"Reeves, J. N.",
"Porquet, D.",
"Braito, V.",
"Nardini, E.",
"Lobban, A.",
"Turner, T. J."
] | 2016ApJ...828...98R | [
"A Deep X-Ray View of the Bare AGN Ark 120. I. Revealing the Soft X-Ray Line Emission"
] | 24 | [
"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... | [
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"10.3847/0004-637X/828/2/98",
"10.48550/arXiv.1607.01062"
] | 1607 | 1607.01062_arXiv.txt | Photo-ionised or ``warm'' absorbers are commonly observed in at least 50\% of the UV/X-ray spectra of Seyfert 1s and type-1 QSO and are an important constituent of AGN (Reynolds 1997, Crenshaw, Kraemer \& George 2003, Porquet et al.\ 2004, Blustin et al. 2005, McKernan et al. 2007, Turner \& Miller 2009). Indeed the Se... | \label{sec:discussion} \subsection{The Origins of the Ionized Soft X-ray Emission in Ark\,120} While there is no intrinsic X-ray absorption towards Ark 120 (aside from the neutral ISM absorption due to the Milkyway), the high signal to noise RGS spectrum has revealed several broad and narrow emission line profiles as... | 16 | 7 | 1607.01062 | 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 XM... | false | [
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12594280 | [
"Shimakawa, Rhythm",
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"Shibuya, Takatoshi",
"Kashikawa, Nobunari",
"Tanaka, Ichi",
"Matsuda, Yuichi",
"Tadaki, Ken-ichi",
"Koyama, Yusei",
"Hayashi, Masao",
"Suzuki, Tomoko L.",
"Yamamoto, Moegi"
] | 2017MNRAS.468.1123S | [
"Similarities and uniqueness of Ly α emitters among star-forming galaxies at z = 2.5"
] | 17 | [
"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... | [
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"10.1093/mnras/stx091",
"10.48550/arXiv.1607.08005"
] | 1607 | 1607.08005_arXiv.txt | The redshift interval of $z$=2.1--2.6 is the key epoch for us to understand the formation mechanisms of star-forming galaxies. In this era, the cosmic star-formation density is peaked \citep{Hopkins:2006}, galaxy morphology is still under construction \citep{Papovich:2005}, and gaseous flows (feeding and feedback) are ... | We have conducted an optical narrow-band imaging survey with the Suprime-Cam to search for LAEs at $z=2.5$ in the UDS-CANDELS field where we have already identified many HAEs in the same redshift slice by our previous narrow-band imaging survey at NIR. Together with existing WFC3/IR data from the HST and multi-band pho... | 16 | 7 | 1607.08005 | 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-... | false | [
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2219791 | [
"Bera, Prasanta",
"Bhattacharya, Dipankar"
] | 2017MNRAS.465.4026B | [
"A perturbation study of axisymmetric strongly magnetic degenerate stars: the case of super-Chandrasekhar white dwarfs"
] | 6 | [
"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"
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"2018CoSka..48..250M",
"2019PhLB..79734859P",
"2020MNRAS.499.2636B",
"2021MNRAS.500..763M"
] | [
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] | 2 | [
"instabilities",
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"methods: numerical",
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"white dwarfs",
"Astrophysics - Solar and Stellar Astrophysics",
"Astrophysics - High Energy Astrophysical Phenomena"
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"10.1093/mnras/stw2979",
"10.48550/arXiv.1607.06829"
] | 1607 | 1607.06829_arXiv.txt | White dwarfs, compact object supported by electron degeneracy pressure, have the well known maximum mass limit of 1.4 M$_\odot$ \citep{Chandrasekhar1931}. If accretion raises the mass above this Chandrasekhar limit, the white dwarf is no longer able to support itself against gravitational collapse, and the resulting r... | \label{conclusion} In this paper, we have studied the linear and non-linear evolution of perturbations to an axisymmetric, strongly magnetized object. Our main results are: \begin{enumerate} \item Axisymmetric magnetic configurations with pure poloidal or pure toroidal field suffer from magnetic instabilities with ti... | 16 | 7 | 1607.06829 | 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 lin... | false | [
"axisymmetric configurations",
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1243490 | [
"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."... | 2016A&A...593A.130H | [
"The radio spectral energy distribution of infrared-faint radio sources"
] | 10 | [
"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,... | [
"2016A&A...596A..80M",
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"2022ApJ...934...26P",
"2023ApJ...958..176W"
] | [
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"1998AJ....115.1... | [
"10.1051/0004-6361/201527000",
"10.48550/arXiv.1607.02707"
] | 1607 | 1607.02707_arXiv.txt | \label{introduction} Infrared-faint radio sources~(IFRS) are comparatively bright radio sources with a faint or absent near-infrared counterpart. They were serendipitously discovered in the Chandra Deep Field-South~(CDFS) by \citet{Norris2006} in the Australia Telescope Large Area Survey~(ATLAS) 1.4\,GHz map and the c... | \label{conclusion} We built radio SEDs for 34~IFRS in the CDFS and ELAIS-S1 fields, covering the frequency range between 150\,MHz and 34\,GHz. Based on these SEDs, we found the vast majority of IFRS ($74^{+6}_{-9}$\%) to show steep radio SEDs defined by $\alpha < -0.8$. $6^{+7}_{-2}$\% of the IFRS in our sample are cl... | 16 | 7 | 1607.02707 | 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 a... | false | [
"radio spectral energy distributions",
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"higher frequencies",
"RL AGN",
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"spectral index",
"CSS sources",
"different telescopes",
"SEDs",
"significantly steeper radio SEDs",
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12518234 | [
"Różańska, A.",
"Bełdycki, B.",
"Madej, J.",
"Adhikari, T. P.",
"You, B."
] | 2017AcA....67...51R | [
"The Appearance of Non-Spherical Systems. Application to LMXB"
] | 3 | [
"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",
"2024ApJ...966..223M"
] | [
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] | 4 | [
"Accretion",
"accretion disks",
"Stars: neutron",
"X-rays: binaries",
"Astrophysics - High Energy Astrophysical Phenomena"
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"2005ApJ...621..372D",
"2011A&A...527A..47R",
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"2013ApJ...767L.... | [
"10.32023/0001-5237/67.1.3",
"10.48550/arXiv.1607.00228"
] | 1607 | 1607.00228_arXiv.txt | Low mass X-ray binaries (LMXB) are binary systems, where the primary star is a compact object, being the black hole or the neutron star. The secondary is a late type main sequence star, classified as K or M of low mass slightly less than the solar mass, $M_{\odot}$. In many of those sources accretion of matter ont... | \label{sec:concl} In this paper we theoretically explained the appearance of non-spherical emission by proper computation of the amount of energy which goes directly towards observer. We defined full set of terms for observed intensity of a non-spherical system, consisting of a neutron star and the accretion disk. We ... | 16 | 7 | 1607.00228 | 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 spherica... | false | [
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"black hole systems",
"outgoing spectrum",
"UV/X-ray energy domains",
"existing data",
"accretion disk",
"non-spherical geometry",
"emitted area",
"the... | 6.060791 | 6.444291 | 48 |
12472610 | [
"Oldham, L. J.",
"Evans, N. W."
] | 2016MNRAS.462..298O | [
"Is there substructure around M87?"
] | 7 | [
"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"
] | [
"astronomy"
] | 3 | [
"galaxies: individual: M87",
"galaxies: kinematics and dynamics",
"galaxies: structure",
"Astrophysics - Astrophysics of Galaxies"
] | [
"1916MNRAS..76..572E",
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"2003MNRAS.343..978S",
"2005ApJ...618..195G",
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"2007ApJ...655..144M",
"2007ApJ...671.1135K",
"2007MNRAS.382..109T",
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"2008MNRAS.388..... | [
"10.1093/mnras/stw1574",
"10.48550/arXiv.1607.02477"
] | 1607 | 1607.02477_arXiv.txt | \label{sec:introduction} In the hierarchical model of galaxy formation, elliptical galaxies and the stellar haloes of spiral galaxies are built up gradually by prolonged periods of accretion. In this picture, early-type galaxies form during an early phase of dissipational star formation fed by gas-rich mergers, creati... | Strong tests of the current cosmological paradigm are provided by the abundance of substructure. As larger structures are assembled hierarchically from mergers and accretion, we should be able to identify fossil signatures of these events in galaxies and clusters. In particular, galaxy clusters are characterised by a v... | 16 | 7 | 1607.02477 | 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 near... | false | [
"galaxy groups",
"dwarf satellites",
"galaxies",
"the satellite galaxy population",
"mock data",
"energy space",
"discrete data sets",
"groups",
"a brightest cluster galaxy",
"BCG",
"the satellite population",
"a central galaxy",
"objects",
"nearly radial orbits",
"an Abel integral equat... | 10.610939 | 6.177447 | -1 |
2241475 | [
"Ivlev, A. V.",
"Akimkin, V. V.",
"Caselli, P."
] | 2016ApJ...833...92I | [
"Ionization and Dust Charging in Protoplanetary Disks"
] | 25 | [
"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",
"2016PASA...33...53H",
"2017ASPC..510...63A",
"2017ApJ...845...75B",
"2017ApJ...849..130M",
"2017NJPh...19j3019S",
"2018A&A...614A..98V",
"2018ApJ...855...23I",
"2018MNRAS.478.2723Z",
"2019A&A...632A..44T",
"2019MNRAS.484..161G",
"2019MNRAS.487.5405S",
"2020A&A...643A.... | [
"astronomy"
] | 9 | [
"astrochemistry",
"cosmic rays",
"dust",
"extinction",
"ISM: clouds",
"protoplanetary disks",
"Astrophysics - Solar and Stellar Astrophysics",
"Astrophysics - Earth and Planetary Astrophysics",
"Astrophysics - Astrophysics of Galaxies"
] | [
"1962pfig.book.....S",
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"1983PThPh..69..480U",
"1987ApJ...320..803D",
"1990MNRAS.243..103U",
"1991ApJ...368..181N",
"1991ApJ...376..214B",
"1994ApJ...422..164K",
"1999ApJ...517..292W",
"2000ApJ...543..486S",
"2001ApJ...548..... | [
"10.3847/1538-4357/833/1/92",
"10.48550/arXiv.1607.03701"
] | 1607 | 1607.03701_arXiv.txt | \label{intro} An accurate calculation of ionization-recombination balance in dense protoplanetary conditions is essential for understanding various fundamental problems, such as coupling of the gas with magnetic field \citep{Li2014}, accretion processes \citep{Turner2014}, chemistry \citep{Semenov2004,Larsson2012} and... | \label{conclusion} We have developed an exact analytical model which describes ionization and dust charging in dense protoplanetary disk conditions, for arbitrary grain-size distribution. Unlike previously developed approaches \citep[][]{Ilgner2006,Okuzumi2009,Fujii2011,Dzyurkevich2013,Mori2016}, our model does not ma... | 16 | 7 | 1607.03701 | 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 ... | false | [
"protoplanetary disks",
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"dust coagulation",
"dust properties",
"dust charging",
"low grain charges",
"dusty gas",
"coagulation",
"ions",
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"development",
"important physical processes",
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12521732 | [
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"Hubble Parameter Measurement Constraints on the Redshift of the Deceleration-Acceleration Transition, Dynamical Dark Energy, and Space Curvature"
] | 325 | [
"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",
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12408878 | [
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"The Hot Companion and Circumbinary Disk of the Be Star HR 2142"
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] | 1607 | 1607.01829_arXiv.txt | % Close binary stars are progressively more common among stars of higher mass \citep{duchene2013}, so we expect that binary interactions will play a fundamental role in the evolution of a significant fraction of massive stars \citep{demink2014}. Roche lobe overflow (RLOF) in close binaries with extreme mass ratios ma... | % Our investigation of the UV and optical spectrum of HR~2142 has led to a new understanding of the nature of this binary system and its circumbinary disk. We used the revised spectroscopic orbit of the Be star to establish the orbital geometry and to predict the radial velocity of the faint companion at the times of ... | 16 | 7 | 1607.01829 | 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 orb... | false | [
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2068556 | [
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"An Improved Distance and Mass Estimate for Sgr A* from a Multistar Orbit Analysis"
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] | 1607 | 1607.05726_arXiv.txt | \label{intro} Following the motions of stars in the center of our Galaxy has given many insights into the properties of the gravitational potential in which they move. The measurement of the high proper motions, and later, accelerations of these stars implies that they move in the gravitational potential of a concentr... | \label{discussion} \subsection{Improvements with the Additional Information from S0-38} \label{discussion1} We have demonstrated the power of our new methodology of searching for speckle holography detections of S0-38 using the information in the AO detections by applying it to S0-38. The combination of S0-2 and S0-... | 16 | 7 | 1607.05726 | 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. Spec... | false | [
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12434581 | [
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"Magneto-optic effects of the Cosmic Microwave Background"
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] | 1607 | 1607.02094.txt | The interaction of light with matter and fields has been intensively studied in the literature and first quantitative studies dates back to Galileo, Newton, Faraday and Maxwell. Among the interesting effects that such interaction represents, there is one class of phenomena which includes the interaction of light (elect... | \label{sec:7} In this work we have studied the most important magneto-optic effects and their impact in the generation of CMB polarization. We presented a systematic study of each of them where we mostly focused on the generation of CMB circular polarization. In this work we found the equations of motion for photon a... | 16 | 7 | 1607.02094 | 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 ... | false | [
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1486962 | [
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"Probing the physics and history of cosmic reionization with the Sunyaev-Zel'dovich effect"
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"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",
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] | 1607 | 1607.07723_arXiv.txt | Departures of the Cosmic Microwave Background (CMB) frequency spectrum from a pure blackbody encode information about the thermal history of the early universe before the epoch of recombination when it emerged from the last scattering surface. The evolution of the universe after this epoch proceeds through the period o... | The goal of obtaining information on the physical processes occurred during the DA and EoR by measuring the SZE-21 cm with SKA is challenging, but possible if pursued with good theoretical and observational strategies. Observations have to be carried out towards high temperature and high optical depth clusters to maxi... | 16 | 7 | 1607.07723 | 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... | false | [
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11492527 | [
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"The Clustering of Luminous Red Galaxies at z ∼ 0.7 from EBOSS and BOSS Data"
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"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",
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] | 1607 | 1607.05383_arXiv.txt | Galaxy redshift surveys have been fundamental in advancing our understanding of the universe. The successes of the past decade, varying from 2dFGRS \citep{Cole_2005}, SDSS \citep{Eisenstein_2005, Zehavi_2011}, and BOSS \citep{Anderson_2012}, have spawned even larger investments in mapping the universe through the three... | This paper marks the first scientific results from the eBOSS LRG program. Although the observing strategy for eBOSS LRGs differs substantially from its predecessors in BOSS and SDSS, we have demonstrated that the combination of the bright-end of the BOSS CMASS sample with the eBOSS LRGs over the redshift range $0.6<z<0... | 16 | 7 | 1607.05383 | 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 th... | false | [
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12408147 | [
"Angus, Ruth",
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] | 2016ApJ...823L...9A | [
"Probabilistic Inference of Basic Stellar Parameters: Application to Flickering Stars"
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"Department of Physics, University of Oxford, UK",
"Department of Astronomy, Columbia University, 550 W 120th Street, New York, NY 10027, USA"
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] | 1607 | 1607.00874_arXiv.txt | \label{sec:intro} Accurate stellar characterization plays a vital role for many active research fields within astronomy. For example, stellar populations, galactic archaeology, the study of binary stars, asteroseismology and exoplanet studies all rely on inferences of basic stellar parameters to varying degrees. Empi... | \label{sec:discussion} We have recalibrated the relation between short timescale brightness fluctuations in the {\it Kepler} light curves of stars (flicker) with both stellar density and surface gravity, whilst including parameters to describe the intrinsic scatter in these relationships, presented in table \ref{tab:... | 16 | 7 | 1607.00874 | 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 m... | false | [
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12408259 | [
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] | 2016ApJ...825...51C | [
"Realistic Detectability of Close Interstellar Comets"
] | 53 | [
"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... | [
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] | 1607 | 1607.08162_arXiv.txt | The current understanding of planet formation suggests that very large numbers of minor bodies are ejected into interstellar space by planets during and after formation \citep[e.g.,][]{1972IAUS...45..329S,1987AJ.....94.1330D,2004come.book..153D}. In typical simulations of solar system formation, only a small fraction o... | \label{sec:discussion} The likelihood of detecting interstellar planetesimals has had a long and varied history. A modern understanding of the properties of the IC population was recently proposed by M09. In this work, we've studied the realistic observational aspects of detecting and characterizing this unknown popul... | 16 | 7 | 1607.08162 | 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 fo... | false | [
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12500421 | [
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] | 2016PASJ...68...81T | [
"Sulfur and zinc abundances of red giant stars†"
] | 20 | [
"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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] | 1607 | 1607.04385_arXiv.txt | Sulfur and zinc are counted as important elements in stellar spectroscopy. Owing to their ``volatile'' characteristics, they are hardly affected by condensation process (unlike refractory elements such as Fe, which may suffer gas--dust depletion). For this reason, S ($\alpha$ group) and Zn (Fe-group element) are regard... | Since sulfur and zinc belong to chemically volatile species, they play important roles in stellar spectroscopy because of being usable as depletion-free tracers for studying the galactic chemical evolution. However, regarding stars of disk population, spectroscopic studies of S and Zn abundances have been mostly direc... | 16 | 7 | 1607.04385 | 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 ... | false | [
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... | 8.692615 | 9.19563 | 140 |
2526299 | [
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"Crain, Robert A.",
"Frenk, Carlos S.",
"Schaller, Matthieu",
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"Theuns, Tom"
] | 2017MNRAS.464.4736F | [
"Size matters: abundance matching, galaxy sizes, and the Tully-Fisher relation in EAGLE"
] | 45 | [
"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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] | 1607 | 1607.03100_arXiv.txt | \label{SecIntro} The Tully-Fisher relation (TFR) links the luminosity of disk galaxies with their characteristic rotation speed. First noted by \citet{Tully-Fisher1977} using photographic magnitudes and HI velocity widths, it has become one of the best studied galaxy scaling relations and a powerful secondary distance... | \label{SecConc} We have used the EAGLE set of $\Lambda$CDM cosmological hydrodynamical simulations to study the relation between abundance matching, galaxy sizes, and the Tully-Fisher relation (TFR). Our main findings may be summarized as follows: \begin{itemize} \item Galaxies that match the predictions of abundanc... | 16 | 7 | 1607.03100 | 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 ha... | false | [
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12465617 | [
"Kulikov, Igor",
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"Using the PPML approach for constructing a low-dissipation, operator-splitting scheme for numerical simulations of hydrodynamic flows"
] | 18 | [
"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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] | 1607 | 1607.01105_arXiv.txt | During the last two decades, two main approaches have been used for numeral hydrodynamics simulations of astrophysical flows: the Lagrangian smooth particle hydrodynamics methods (hereafter, the SPH method) and Eulerian mesh-based methods. Numerous comparisons between the SPH and mesh-based methods have been performed ... | {\bf The limiter problem.} The main trend in constructing accurate numerical methods (e.g. PPM, TVD and WENO) has been the use of high-order polynomials in the interpolation schemes. However, this practice often produces unphysical oscillations around discontinuous solutions. To resolve this problem, the limiters are i... | 16 | 7 | 1607.01105 | 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 perfor... | false | [
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2944614 | [
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"Caballero, Jose A.",
"Montes, David",
"Mundt, Reinhard",
"Ribas, Ignasi",
"Quirrenbach, Andreas"
] | 2016csss.confE.109P | [
"Spectroscopic Characterisation of CARMENES Target Candidates from FEROS, CAFE and HRS High-Resolution Spectra"
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"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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] | 1607 | 1607.08738_arXiv.txt | The new CARMENES instrument is mounted at the 3.5 m telescope at Calar Alto Observatory, located in the Sierra de los Filabres in southern Spain. It consists of two fibre-fed high-resolution spectrographs, operating in the visible wavelength range from 0.52 to 0.96 $\mu$m and in the near-infrared from 0.96 to 1.71 $\mu... | We obtained stellar parameters for 351 stars from 977 spectra. We find that most stars lie within 3200-3900 K, corresponding to spectral types M1V-M5V, as shown in the upper left panel of Figure~\ref{fig:results}. The higher the metallicity the higher the temperature for each spectral type (Figure~\ref{fig:results}, lo... | 16 | 7 | 1607.08738 | CARMENES (Calar Alto high-Resolution search for M dwarfs with Exoearths with Near-infrared and optical Échelle Spectrographs) started a new planet survey on M-dwarfs in January this year. The new high-resolution spectrographs are operating in the visible and near-infrared at Calar Alto Observatory. They will perform hi... | false | [
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12472778 | [
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] | 2016MNRAS.462.3053B | [
"The anatomy of a star-forming galaxy: pressure-driven regulation of star formation in simulated galaxies"
] | 38 | [
"Department of Physics and Astronomy, McMaster University, Hamilton, ON L8S 4M1, Canada",
"Department of Physics and Astronomy, McMaster University, Hamilton, ON L8S 4M1, Canada",
"Department of Physics and Astronomy, McMaster University, Hamilton, ON L8S 4M1, Canada",
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] | 1607 | 1607.05795_arXiv.txt | The process of star formation is limited, in principle, by the availability of cold, dense gas fuel. However, in typical disk galaxies it proceeds inefficiently relative to characteristic time-scales for the gas, such as the local free-fall time in Giant Molecular Clouds ($\sim 10$ Myr). In fact, globally, star forma... | \label{sec:conclusions} We have presented a suite of high resolution isolated galaxies that include a purposefully simple feedback scheme. We use a wide range of parameter choices to explore both the implications of these choices and the process of regulation of star formation. We find a sub-linear scaling between pa... | 16 | 7 | 1607.05795 | 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 represent... | false | [
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... | 11.671693 | 8.556044 | 192 |
12593906 | [
"Mirocha, Jordan",
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"Sun, Guochao"
] | 2017MNRAS.464.1365M | [
"The global 21-cm signal in the context of the high- z galaxy luminosity function"
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"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"
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] | 1607 | 1607.00386_arXiv.txt | \label{sec:Introduction} Galaxy evolution in the early Universe is most often studied from two distinct vantage points: through direct observations of high-$z$ galaxies and measurements of the thermal and ionization history of the intergalactic medium (IGM). These two approaches are exceptionally complementary, at leas... | \label{sec:conclusions} We have shown that linking models of the global 21-cm signal to recent measurements of the high-$z$ galaxy LF leads to a strong preference for models with late heating and reionization ($z \lesssim 12$). At the formalism level, we assume that the $\fstar$-based model is the true model for the ga... | 16 | 7 | 1607.00386 | 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 h... | false | [
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12473291 | [
"Gourgouliatos, Konstantinos N.",
"Hollerbach, Rainer"
] | 2016MNRAS.463.3381G | [
"Resistive tearing instability in electron MHD: application to neutron star crusts"
] | 19 | [
"Department of Applied Mathematics, University of Leeds, Leeds LS2 9JT, UK",
"Department of Applied Mathematics, University of Leeds, Leeds LS2 9JT, UK"
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] | 1607 | 1607.07874_arXiv.txt | A plethora of observations of strongly magnetised neutron stars \citep{Olausen:2014} has revealed that their temperatures are higher than what conventional cooling of a hot proto-neutron star suggests. A solution to this puzzle is that the extra thermal energy needed for these systems is provided by the Ohmic decay of... | In this work we have shown that the tearing mode instability operates under the Hall effect and resistivity in the Electron-MHD description. The appearance of the instability is similar to the usual MHD case, developing the characteristic reconnection islands, even though the mechanism is physically different, as the u... | 16 | 7 | 1607.07874 | 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 eigenv... | false | [
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12510816 | [
"Dedes, A.",
"Karamitros, D.",
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] | 2016PhRvD..94i5008D | [
"Effective theory for electroweak doublet dark matter"
] | 10 | [
"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... | [
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"10.1103/PhysRevD.94.095008",
"10.48550/arXiv.1607.05040"
] | 1607 | 1607.05040_arXiv.txt | The conventional way to produce non-relativistic (cold) DM relic particle abundance, is the so called freeze-out mechanism~\cite{Lee:1977ua,Hut:1977zn}. Although this mechanism is well reviewed in the literature\cite{Hooper:2009zm, Jungman:1995df,Kolb:1990vq,Dodelson:2003ft,Weinberg:2008zzc,Lisanti:2016jxe}, it would... | \setcounter{equation}{0} \label{sec:concl} We have introduced in the SM particle spectrum a fermionic bi-doublet: a pair of Weyl fermion $SU(2)_L$-doublets, $\mathbf{D}_1$ and $\mathbf{D}_2$, with opposite hypercharges. In addition, we assume a discrete $Z_2$-symmetry that distinguishes $\mathbf{D}_1$ and $\mathbf{D}_... | 16 | 7 | 1607.05040 | 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... | false | [
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3829677 | [
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"Guirado, J. C.",
"Pérez-Torres, M. A.",
"Ros, E."
] | 2016A&A...596A..27M | [
"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"
] | 6 | [
"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... | [
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"10.1051/0004-6361/201628149",
"10.48550/arXiv.1607.05089"
] | 1607 | 1607.05089_arXiv.txt | Distant Active Galactic Nuclei (AGN), like quasars and BL Lacs, are currently used as position references in the definition of astronomical inertial frames, from radio \citep[the international celestial reference frame, ICRF][]{Fey,Fey2} to the optical (e.g., {\em Gaia}, \citealt{Linde}). The consolidation of reference... | \label{conclusions} We report on quasi-simultaneous 14.4\,GHz and 43.1\,GHz VLBA observations of the S5 polar cap sample, performed in December 2010 in phase-referencing mode, using the fast-frequency-switching (FFS) capabilities of the VLBA, and compare them to earlier results at 15\,GHz band. We have performed a hi... | 16 | 7 | 1607.05089 | 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 so... | false | [
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12408911 | [
"Lu, Yi",
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"Shi, Feng",
"Mo, H. J.",
"Tweed, Dylan",
"Wang, Huiyuan",
"Zhang, Youcai",
"Li, Shijie",
"Lim, S. H."
] | 2016ApJ...832...39L | [
"Galaxy Groups in the 2Mass Redshift Survey"
] | 26 | [
"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, ... | [
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] | 1607 | 1607.03982_arXiv.txt | \label{sec:mass} One of the key steps in the halo-based group finder \citep{Yang2005a,Yang2007} is to have accurate estimates of the halo masses of candidate galaxy groups. As demonstrated in \citet{Yang2007}, halo mass is tightly correlated with the total luminosity of member galaxies. In practice, however, one can o... | In this paper, we have implemented, tested and applied a modified version of the halo-based group finder developed in \citet{Yang2005a, Yang2007} to extract galaxy groups from the 2MRS. Covering uniformly about 91\% of the sky, the 2MRS provides the best available representation of the structures in local universe, an... | 16 | 7 | 1607.03982 | 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 met... | false | [
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12593997 | [
"Sonnenfeld, Alessandro",
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"Merger-driven evolution of the effective stellar initial mass function of massive early-type galaxies"
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"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",
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] | 1607 | 1607.01394_arXiv.txt | \label{sect:intro} Understanding the properties and the origin of the stellar initial mass function (IMF) is currently one of the biggest challenges in galaxy formation theory. Observational constraints on the IMF provide us with a puzzling scenario. On the one hand the IMF appears to be remarkably self-similar acros... | \label{sect:concl} Using empirically motivated recipes for describing the IMF of massive galaxies together with the dry merger evolution model developed by \citet{Nip++12} we studied the time evolution of the effective IMF, defined as the ratio between the true stellar mass and the stellar mass one would infer assumin... | 16 | 7 | 1607.01394 | 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 in... | false | [
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12473435 | [
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"Evidence for the magnetar nature of 1E 161348-5055 in RCW 103"
] | 55 | [
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"Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA",
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] | 1607 | 1607.04264_arXiv.txt | RCW\,103 is a shell supernova remnant (SNR) of $\sim$\,9 arcmin apparent diameter, expanding at around 1100 km s$^{-1}$, with an estimated age between 1350 and 3050 yr \citep{carter97}, and at a distance of 3.3 kpc \citep{caswell75}. \citet{frank15} gave a detailed, spatially resolved, accou... | We have reported on the characteristics of the \emph{Swift}/BAT bright X-ray burst coming from the direction of the RCW 103 nebula observed on 2016 June 22. At the same time, we have also presented spectral and timing results concerning the X-ray activation of the CCO at the centre of the RCW~103 nebula, \oneE... | 16 | 7 | 1607.04264 | 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-Ra... | false | [
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12464691 | [
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"10.1088/1475-7516/2016/08/058",
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] | 1607 | 1607.02442_arXiv.txt | A focal problem today in the dynamics of globular clusters is core collapse. It has been predicted by theory for decades \citep{hen61,lyn68,spi85}, but observation has been less alert to the phenomenon. For many years the central brightness peak in M15 \citep{kin75,new78} seemed a unique anomaly. Then \citet{aur82} sug... | 16 | 7 | 1607.02442 | 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 kS... | false | [
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] | 2016MNRAS.462..951N | [
"Dark matter inside early-type galaxies as function of mass and redshift"
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"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 ... | [
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"10.1093/mnras/stw1661",
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] | 1607 | 1607.05324_arXiv.txt | \label{sec:intro} The measurement of masses of galaxies has been, over a long period of time, an interesting and difficult problem, which has elicited the application of various and diverse techniques \citep{spi75,bur75,sof01,sim07}. Since the determination of rotation curves for a large number of spiral galaxies \cit... | The analysis of the distribution of stellar mass with respect to virial mass on several samples of ETGs from the SDSS DR9 in the redshift range $0.0024 < z < 0.3500$ and in the dynamical mass range $9.5 < log({\bf M_{virial}}/{\bf M_{\odot}}) < 12.5$ has yielded the following results: \begin{itemize} \item A signific... | 16 | 7 | 1607.05324 | 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 profil... | false | [
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3458517 | [
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"Naylor, T.",
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] | 2016MNRAS.462L..61K | [
"V346 Normae: first post-outburst observations of an FU Orionis star"
] | 21 | [
"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... | [
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"10.1093/mnrasl/slw126",
"10.48550/arXiv.1607.03114"
] | 1607 | 1607.03114_arXiv.txt | FU\,Orionis stars (FUors) are pre-main-sequence stars that undergo optical outbursts, interpreted as extremely active phases of mass accretion ($\sim10^{-4}\,$M$_{\sun}$\,yr$^{-1}$). These sources are classified by the observation of outbursts that increase the optical/infrared brightness by up to 6\,mag for several de... | \label{sec:conclusions} Our study shows that V346\,Nor has switched from an extreme FUor-type outburst into a much less active phase, consistent with a change in the accretion rate by 2-3 orders of magnitude. With ${\Delta}R=10.9$\,mag and ${\Delta}K=5.8$\,mag, the observed dimming event far exceeded the variability t... | 16 | 7 | 1607.03114 | 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 tha... | false | [
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1683108 | [
"Hameury, J. -M.",
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] | 2016A&A...594A..87H | [
"Outbursts in ultracompact X-ray binaries"
] | 14 | [
"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... | [
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"10.48550/arXiv.1607.06394"
] | 1607 | 1607.06394_arXiv.txt | Soft X-ray transients (SXTs) are a subclass of low mass X-ray binaries (LMXBs) which alternate between quiescent periods lasting years and bright outbursts which can reach the Eddington limit and last typically for weeks \citep[see e.g.][for reviews of the observations]{ts96,csl97,yy15}. These bright sources were disco... | We have shown that the disc instability model applied to ultracompact binaries produces outbursts whose characteristics are very similar to those of the faint and very faint outbursts observed in VFXBs, provided we use the same value of the viscosity parameter $\alpha_{\rm h}$ as in cataclysmic variables and in longer ... | 16 | 7 | 1607.06394 | 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 ... | false | [
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... | 6.519248 | 6.502261 | -1 |
3221474 | [
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"Campbell, Duncan"
] | 2017MNRAS.469.2791H | [
"Approximate Bayesian computation in large-scale structure: constraining the galaxy-halo connection"
] | 44 | [
"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... | [
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] | 1607 | 1607.01782_arXiv.txt | Cosmology was revolutionized in the 1990s with the introduction of likelihoods---% pro\-ba\-bil\-ities for the data given the theoretical model---% for combining data from different surveys and performing principled inferences of the cosmological parameters (\citealt{White:1996aa, Riess:1998aa}). Nowhere has this been ... | \label{sec:discussion} Approximate Bayesian Computation, ABC, is a generative, simulation-based inference that can deliver correct parameter estimation with appropriate choices for its design. It has the advantage over the standard approach in that it does not require explicit knowledge of the likelihood function. It ... | 16 | 7 | 1607.01782 | 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 possi... | false | [
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1267015 | [
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] | 2016ApJ...832...27A | [
"Global Energetics of Solar Flares. III. Nonthermal Energies"
] | 58 | [
"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... | [
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"10.3847/0004-637X/832/1/27",
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] | 1607 | 1607.06488_arXiv.txt | We undertake a systematic survey of the global energetics of solar flares and coronal mass ejections (CME) observed during the SDO era, which includes all M and X-class flares during the first 3.5 years of the SDO mission, covering some 400 flare events. This project embodies the most comprehensive survey about variou... | The energy partition study of Emslie et al.~(2012) was restricted to 38 large solar eruptive events (SEE). In a more comprehensive study on the global flare energetics we choose a dataset that contains the 400 largest (GOES M and X-class) flare events observed during the first 3.5 years of the SDO era. Previously we de... | 16 | 7 | 1607.06488 | 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, y... | false | [
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12594329 | [
"Troitsky, Sergey"
] | 2017MNRAS.468L..36T | [
"Density and metallicity of the Milky Way circumgalactic gas"
] | 7 | [
"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"
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"2020ApJ...894....1F",
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"10.1093/mnrasl/slx022",
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] | 1607 | 1607.05442_arXiv.txt | \label{sec:intro} Recently, considerable attention has been attracted to studies of gas coronae of galaxies, that is of reservoirs of gas extending up to the galaxies' virial radii. This circumgalactic gas represents, thanks to the large volume it fills, a substantial contribution to the mass budget of a galaxy. This g... | \label{sec:concl} The results of this work eliminate the apparent discrepancy, see Fig.~\ref{fig:2contours}, in parameters of the Milky-Way circumgalactic gas estimated from X-ray spectroscopy and from studies of ram-pressure stripping of Galactic dwarf satellites. A combined analysis of the observational constraints, ... | 16 | 7 | 1607.05442 | 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 o... | false | [
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12472567 | [
"Suzuki, T. L.",
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"Hayashi, M.",
"Shimakawa, R.",
"Koyama, Y.",
"Tadaki, K. -i.",
"Tanaka, I.",
"Minowa, Y.",
"Yamamoto, M.",
"Smail, I.",
"Best, P. N."
] | 2016MNRAS.462..181S | [
"[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"
] | 24 | [
"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... | [
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"2020ApJ...895....9O",
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] | 6 | [
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"10.1093/mnras/stw1655",
"10.48550/arXiv.1607.02054"
] | 1607 | 1607.02054_arXiv.txt | \label{intro} Emission lines from regions ionized by hot, young massive stars are useful as indicators of star formation in distant galaxies. Imaging observations with narrow-band (NB) filters, which can capture redshifted strong emission lines, are a powerful method to construct a star-forming galaxy sample at a part... | \label{summary} We use the NB-selected galaxy catalog at $z$=2.23 obtained by the HiZELS project, and construct the two galaxy samples of \ha\ and \oiii\ emission line galaxies by applying the same line flux limit. We derive the global physical properties of these emitters, and compare the number distribution of a ste... | 16 | 7 | 1607.02054 | 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 ex... | false | [
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"the full galaxy sample",
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"... | 12.826963 | 7.009368 | -1 |
12409154 | [
"Ji, Alexander P.",
"Frebel, Anna",
"Simon, Joshua D.",
"Chiti, Anirudh"
] | 2016ApJ...830...93J | [
"Complete Element Abundances of Nine Stars in the r-process Galaxy Reticulum II"
] | 158 | [
"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... | [
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"10.3847/0004-637X/830/2/93",
"10.48550/arXiv.1607.07447"
] | 1607 | 1607.07447_arXiv.txt | \label{s:intro} Ultra-faint dwarf galaxies (UFDs) probe extreme astrophysical regimes. They are the faintest and most metal-poor galaxies known \citep{Kirby08,Kirby13b}. Their high velocity dispersions imply they are the most dark matter dominated galaxies \citep{Simon07,Strigari08,Simon11}, making them attractive targ... | 16 | 7 | 1607.07447 | 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 hav... | false | [
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5170993 | [
"Hankins, M. J.",
"Lau, R. M.",
"Morris, M. R.",
"Sanchez-Bermudez, J.",
"Pott, J. U.",
"Adams, J. D.",
"Herter, T. L."
] | 2016ApJ...827..136H | [
"Infrared Observations of the Quintuplet Proper Members using SOFIA/FORCAST and Gemini/TReCS"
] | 5 | [
"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",
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"10.3847/0004-637X/827/2/136",
"10.48550/arXiv.1607.02781"
] | 1607 | 1607.02781_arXiv.txt | Five very luminous infrared sources reside in the young, massive Quintuplet cluster in the Galactic center (Okuda et al. 1990). These five objects, for which the cluster is named, are referred to as the Quintuplet proper members (QPMs). The QPMs are sources of great interest, given their enigmatic nature exhibiting hig... | In this paper, infrared observations taken with SOFIA/FORCAST and Gemini/TReCS were used to study the thermal dust emission from the QPMs. DUSTY models of the SEDs were used to determine properties of the dust reservoirs present in each object. Best-fit model parameters indicate that the near-IR pinwheel stars (Q2 and ... | 16 | 7 | 1607.02781 | 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 binar... | false | [
"enhanced mass loss",
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"conjunction",
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12408595 | [
"Tan, Wei-Wei",
"Wang, F. Y.",
"Cheng, K. S."
] | 2016ApJ...829...29T | [
"Constraining Warm Dark Matter Mass with Cosmic Reionization and Gravitational Waves"
] | 15 | [
"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... | [
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"2020PDU....2800476N",
"2020SeScT..35b5020S",
"2021MNRAS.506.5... | [
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] | 6 | [
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"10.3847/0004-637X/829/1/29",
"10.48550/arXiv.1607.03567"
] | 1607 | 1607.03567.txt | The astrophysical and cosmological probes have confirmed that baryons constitute only some $16\%$ of the total matter in the Universe. The rest of the mass is in the form of `dark matter' (DM). The nature of DM particles is poorly understood, as they do not interact with baryons. Many indirect searches have been carrie... | Although the CDM paradigm has great success in explaining the large scale structure of the universe, it still have some problems on small scales. An alternatively WDM paradigm could ease these problems by employing the $\kev$ WDM particles. In this paper, we calculate the SFRs of Pop I/II and Pop III stars in the frame... | 16 | 7 | 1607.03567 | 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 Populat... | false | [
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"m}<SUB>{{x</SUB>}}=3",
... | 8.761995 | -0.73356 | 50 |
2583156 | [
"Buchan, Stewart",
"Shankar, Francesco"
] | 2016MNRAS.462.2001B | [
"Setting firmer constraints on the evolution of the most massive, central galaxies from their local abundances and ages"
] | 13 | [
"School of Physics and Astronomy, University of Southampton, Southampton SO17 1BJ, UK",
"School of Physics and Astronomy, University of Southampton, Southampton SO17 1BJ, UK"
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"2022MNRAS.510.5639M",
"2022MNRAS.511..506C",
"2023ApJ...954...97B",
"2024MNRAS.tmp.1... | [
"astronomy"
] | 6 | [
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"galaxies: formation",
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"galaxies: structure",
"Astrophysics - Astrophysics of Galaxies",
"Astrophysics - Cosmology and Nongalactic Astrophysics"
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"2004ApJ...614...17G",
"2005ApJ...621..673T",
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"10.1093/mnras/stw1771",
"10.48550/arXiv.1607.05732"
] | 1607 | 1607.05732_arXiv.txt | The mechanisms both to form and evolve massive early-type galaxies are still highly debated. Early-type galaxies (ETG) dominate the red population of objects in the observed bimodal distribution of galaxy colours \citep{Baldry2004,Cassata2008}. However, how ETGs form, evolve and transition in the colour-mass plane rema... | In this work, we have set tighter constrains on the assembly and evolution of massive, central galaxies. We utilise a catalogue of dark matter haloes created from the Bolshoi simulation. We populate these haloes with a stellar mass using recent rendition of the stellar mass to halo mass relation by \cite{Kravtsov2014} ... | 16 | 7 | 1607.05732 | 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 gal... | false | [
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"the mass accretion history",
"mergers",
"situ growth",
"M<SUB",
"their host dark matter",
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12406183 | [
"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."
] | 2016A&A...592L...5W | [
"The faint end of the 250 μm luminosity function at z < 0.5"
] | 7 | [
"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... | [
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"10.1051/0004-6361/201629076",
"10.48550/arXiv.1607.02975"
] | 1607 | 1607.02975_arXiv.txt | Luminosity functions (LF) are fundamental properties of the observed galaxy populations that provide important constraints on models of galaxy formation and evolution (e.g. Lacey et al. 2015; Schaye et al. 2015). Studying the LF at far-infrared (FIR) and sub-millimetre (sub-mm) wavelengths is critical. Half of the ene... | We study the low-redshift, rest-frame 250 $\mu$m LF using stacking of deep optically selected galaxies from the SDSS survey on the {\it Herschel}-SPIRE maps of the GAMA fields and the Stripe 82 area. Our method not only recovers the mean 250 $\mu$m luminosities $L_{250}$ of galaxies that are too faint to be individuall... | 16 | 7 | 1607.02975 | <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 field... | false | [
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12473475 | [
"King, Andrew",
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] | 2016MNRAS.462..464K | [
"Black holes in stellar-mass binary systems: expiating original spin?"
] | 14 | [
"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... | [
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"10.1093/mnras/stw1598",
"10.48550/arXiv.1607.02144"
] | 1607 | 1607.02144_arXiv.txt | \label{intro} Accreting black holes frequently have their spins at least initially misaligned from the angular momentum of the mass reservoir feeding them. This is generic for supermassive black holes (SMBH) \citep[cf][]{King:2006aa} and is possible in stellar--mass binary systems, particularly if they have undergone a... | We have investigated whether various accreting black hole systems are likely to reach global alignment of the black hole spin and its accretion disc with the binary plane. A fairly close approach to this state is likely in systems where the companion star fills its Roche lobe and transfers mass to a lower--mass black h... | 16 | 7 | 1607.02144 | 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 fo... | false | [
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12594146 | [
"Owen, James E.",
"Kollmeier, Juna A."
] | 2017MNRAS.467.3379O | [
"Dust traps as planetary birthsites: basics and vortex formation"
] | 20 | [
"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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] | 1607 | 1607.08250_arXiv.txt | Despite observational advances in characterising exoplanets and the environments in which they form (protoplanetary discs), a coherent picture that explains the origin and diversity of planets from their disky forebears remains elusive. We know planets must sculpt the discs in which they form, and indeed we see structu... | \label{sec:results} We have shown that ``transition'' discs are prime sites for the growth of low-mass planets by pebble accretion. This planet formation scenario has two important -- perhaps mutually exclusive -- implications. Firstly, if the planet were able to accrete pebbles at the standard rate for the entire tim... | 16 | 7 | 1607.08250 | 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... | false | [
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4331519 | [
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"Levenson, N. A.",
"Radomski, J.",
"Ichikawa, K.",
"García-Bernete, I.",
"González-Martín, O.",
"Díaz-Santos, T.",
"Martínez-Paredes, M."
] | 2016MNRAS.462.2618F | [
"Investigating the dusty torus of Seyfert galaxies using SOFIA/FORCAST photometry"
] | 24 | [
"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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"10.1093/mnras/stw1780",
"10.48550/arXiv.1607.07918"
] | 1607 | 1607.07918.txt | The unified model \citep{A1993,UP1995} of active galactic nuclei (AGN) posits that all AGN are essentially the same type of object viewed from different lines of sight. This orientation-based model depends on a circumnuclear toroidal region of optically and geometrically thick dust which can obscure a central region o... | \label{CON} We present new 31.5 \um~imaging data from NASA's SOFIA/FORCAST for 11 nearby Seyfert galaxies. To derive AGN-dominated fluxes within the 3.4 arcsec SOFIA aperture, we used the PSF scaling method of \citet{Radomski2003,RA09,Mason2012}. We then performed a spectral decomposition using the routine of \citet... | 16 | 7 | 1607.07918 | 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 thi... | false | [
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12510124 | [
"Saga, Shohei"
] | 2016PhRvD..94f3523S | [
"Observable cosmological vector mode in the dark ages"
] | 5 | [
"Department of Physics and Astrophysics, Nagoya University, Aichi 464-8602, Japan"
] | [
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"2018arXiv181009572C",
"2020CQGra..37o4001A"
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"10.1103/PhysRevD.94.063523",
"10.48550/arXiv.1607.03973"
] | 1607 | 1607.03973_arXiv.txt | Recent development of cosmological observations plays an important role in establishing standard cosmology, namely, the $\Lambda$CDM model. In the current states of observations of cosmological perturbations, for example, we have detected the cosmic microwave background (CMB) temperature anisotropy, the CMB E-mode pola... | \label{sec: results} In Fig.~\ref{fig: cls}, we show the angular power spectra of the curl mode induced from PGWs with $r = 0.1$ and the second-order vector mode. \begin{figure}[t] \begin{center} \includegraphics[width=0.49\textwidth]{Signal_PGW} \includegraphics[width=0.49\textwidth]{Signal_VEC} \end{center} \caption{... | 16 | 7 | 1607.03973 | 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 em... | false | [
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3016013 | [
"Zong, W.",
"Charpinet, S.",
"Vauclair, G."
] | 2016A&A...594A..46Z | [
"Signatures of nonlinear mode interactions in the pulsating hot B subdwarf star KIC 10139564"
] | 45 | [
"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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"2019OAst...28...61P",
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"10.1051/0004-6361/201629132",
"10.48550/arXiv.1607.06621"
] | 1607 | 1607.06621_arXiv.txt | Hot B subdwarf (sdB) stars are helium core burning objects that populate the so-called Extreme Horizontal Branch (EHB). They are expected to have a mass around 0.47 $M_{\odot}$ and are characterized by a very thin hydrogen-rich residual envelope containing at most $\sim 0.02$ $M_{\odot}$. For this reason, they remain h... | While studying the high-quality and long-duration photometric data provided by the {\sl Kepler} spacecraft on the pulsating sdB star KIC\,10139564, we have identified different patterns in the frequency and amplitude modulations of the oscillation modes belonging to several rotationally split multiplets or linear combi... | 16 | 7 | 1607.06621 | 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 exp... | false | [
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2263112 | [
"Massari, Davide",
"Fiorentino, Giuliana",
"Tolstoy, Eline",
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"Stuik, Remko",
"Schreiber, Laura",
"Andersen, David",
"Clénet, Yann",
"Davies, Richard",
"Gratadour, Damien",
"Kuijken, Konrad",
"Navarro, Ramon",
"Pott, Jörg-Uwe",
"Rodeghiero, Gabriele",
"Turri, Paolo",
... | 2016SPIE.9909E..1GM | [
"High-precision astrometry towards ELTs"
] | 7 | [
"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 ... | [
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"10.48550/arXiv.1607.04412"
] | 1607 | 1607.04412_arXiv.txt | \label{sec:intro} % Accurate astrometry is one of the major drivers for diffraction limited Extremely Large Telescopes (ELTs). To reach diffraction limited observations, the Multi-AO Imaging Camera for Deep Observations (MICADO), one of the first light instruments for the European-ELT, will be assisted by an Adaptive... | 16 | 7 | 1607.04412 | 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 a... | false | [
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"a crowded Galactic globu... | 14.053365 | 10.484058 | 10 | |
5398407 | [
"Kraljic, David",
"Sarkar, Subir"
] | 2016JCAP...10..016K | [
"Frames of most uniform Hubble flow"
] | 12 | [
"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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"2023CQGra..40i4001K",
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] | 9 | [
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"10.1088/1475-7516/2016/10/016",
"10.48550/arXiv.1607.07377"
] | 1607 | 1607.07377_arXiv.txt | The standard Lambda Cold Dark Matter ($\Lambda$CDM) cosmological model is based on an assumed background Friedmann-Lema\^itre-Robertson-Walker (FLRW) geometry that is isotropic and homogeneous. The structure in the universe is modelled as statistically isotropic and homogeneous, initially Gaussian distributed perturbat... | \label{sec:conclusion} We have studied the properties of boost velocities of observers with respect to the CMB frame that make the spherically averaged Hubble flow converge the quickest to its background value. We place observers at different locations in a Hubble volume N-body simulation and find that the distributio... | 16 | 7 | 1607.07377 | 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 Ba... | false | [
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3360123 | [
"Laine, Seppo",
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"Ashby, Matthew L. N.",
"Davies, James E.",
"Majewski, Stephen R.",
"Brodie, Jean P.",
"GaBany, R. Jay",
"Arnold, Jacob A."
] | 2016AJ....152...72L | [
"Metallicity and Age of the Stellar Stream around the Disk Galaxy NGC 5907"
] | 13 | [
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"Spitzer Science Center-Caltech, MS 314-6, Pasadena, CA 91125, USA",
"Spitzer Science Center-Caltech, MS 314-6, Pasadena, CA 91125, USA",
"CRESST/UMBC/NASA GSFC, Code 665, Greenbelt, MD 20771, USA",
"Department of Physics and Astronomy, Sa... | [
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] | 5 | [
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] | 1607 | 1607.03554_arXiv.txt | \label{s:intro} Major mergers, mergers that take place between galaxies of comparable mass (say stellar or total mass ratios of 1:3 -- 1:5 or larger, with the ratio being the mass of the lower mass galaxy over the mass of the more massive galaxy), have attracted attention in the past \citep*[e.g.,][]{arp66,schweizer82... | \label{concl} We have studied the brightest part of the stellar stream around NGC~5907 with both visible-light ($g$, $i$, and $r$) and IRAC near-infrared 3.6 $\mu$m images. While the stream is very faint, we have managed to generate color index profiles and an SED for the brightest part of the stream. Our results show... | 16 | 7 | 1607.03554 | 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/Infrare... | false | [
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"Kepler Flares. IV. A Comprehensive Analysis of the Activity of the dM4e Star GJ 1243"
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] | 1607 | 1607.03886_arXiv.txt | M dwarfs are well known for their high magnetic activity, most notably their powerful, frequent flares. These are believed to be magnetic reconnection events analogous to the flares observed on the Sun, but occur much more frequently, and with much greater energies. Observational studies of flares on these stars have b... | \label{sec:Conclusions} In this paper, we have presented a comprehensive study of the star GJ 1243, using previous data in the literature, 11 months of short-cadence wide-band photometry from \textit{Kepler}, and simultaneous spectroscopy for three flares. We calculated and analyzed the cumulative frequency of flares ... | 16 | 7 | 1607.03886 | 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, presenti... | false | [
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2775547 | [
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] | 1607 | 1607.01403_arXiv.txt | \label{sec:intro} The flat $\Lambda$CDM cosmological model is the concordance model of our Universe today. It is consistent with a variety of independent experiments, including an analysis of the cosmic microwave background (CMB) by the {\it Planck} mission \citep{planck2015}. The {\it Planck} results provide the mo... | 16 | 7 | 1607.01403 | 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 ... | false | [
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12511007 | [
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] | 1607 | 1607.04226_arXiv.txt | \label{sec:overview} \subsection{Introduction and Summary} \medskip The recent detections of gravitational radiation events GW150914~\cite{GWPRL1} and GW151226~\cite{GWPRL2} from black hole binary inspiral has underscored the importance of understanding the theoretical predictions of the waveforms for such processes. ... | \label{sec:conc} Though peak time offsets have been important in waveform construction, all that has been known is that such a time offset exists and that it is different (a) in the Schwarzschild background for gravitational waves in different multipole modes, and also (b) in the Kerr background for even a given multi... | 16 | 7 | 1607.04226 | 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 solvi... | false | [
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"The cold dark matter content of Galactic dwarf spheroidals: no cores, no failures, no problem"
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] | 1607 | 1607.06479_arXiv.txt | \label{SecIntro} The steep slope of the dark matter halo mass function at the low-mass end is a defining characteristic of the $\Lambda$CDM cosmological paradigm. It is much steeper than the faint-end slope of the galaxy stellar mass function, implying that low-mass CDM haloes are significantly more abundant than fain... | \label{SecConc} We use the APOSTLE suite of $\Lambda$CDM cosmological hydrodynamical simulations of the Local Group to examine the masses of satellite galaxies brighter than $M_V=-8$ (i.e., $M_{\rm str}>10^5 \Msun$). Our analysis extends that of \citet{Sawala2016}, were we showed that our simulations reproduce the Ga... | 16 | 7 | 1607.06479 | 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 disp... | false | [
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12626389 | [
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"Graduate School of Science, Osaka University, Toyonaka, 560-0043, Japan",
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] | 1607 | 1607.03540_arXiv.txt | \label{sec:Introduction} Neutron stars are believed to be born in supernova explosions triggered by the collapse of the iron core in massive stars. Many astronomical observations have revealed that binary neutron stars\footnote{\lrn{With \textit{``binary neutron-star''} systems we here refer to binary systems composed... | \label{sec:sao} As anticipated in the Introduction, there is little doubt that this is a particularly exciting and highly dynamical time for research on neutron stars, in general, and on BNS mergers, in particular. In less than 10 years, \ie starting approximately from 2008, a considerable effort by several groups acr... | 16 | 7 | 1607.03540 | 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 wh... | false | [
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] | 1607 | 1607.03149.txt | \label{sec:intro} The baryon acoustic oscillation (BAO) signal in the distribution of galaxies is an imprint of primordial sound waves that have propagated in the very early Universe through the plasma of tightly coupled photons and baryons (e.g.~\citealt{Peebles:1970ag, Sunyaev:1970eu}). The corresponding BAO signal ... | \label{sec:conclusion} We have measured the power spectrum multipoles from the final BOSS DR12 dataset in three (overlapping) redshift bins, covering the total redshift range $0.2 < z < 0.75$. Our analysis focuses on measuring the isotropic and anisotropic Baryon Acoustic Oscillation signal in Fourier-space. Our main ... | 16 | 7 | 1607.03149 | 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.... | false | [
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12408270 | [
"Erwin, Peter",
"Debattista, Victor P."
] | 2016ApJ...825L..30E | [
"Caught in the Act: Direct Detection of Galactic Bars in the Buckling Phase"
] | 41 | [
"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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] | 1607 | 1607.01290_arXiv.txt | % Approximately 60--70\% of disk galaxies in the local universe have stellar bars \citep[e.g.,][]{eskridge00,menendez-delmestre07}. A wide variety of observational evidence indicates that many bars are vertically thickened in their inner regions, appearing as ``boxy'' or ``peanut-shaped'' (B/P) bulges when seen edge-o... | 16 | 7 | 1607.01290 | 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-bod... | false | [
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12472902 | [
"Blank, Marvin",
"Duschl, Wolfgang J."
] | 2016MNRAS.462.2246B | [
"Viscous time lags between starburst and AGN activity"
] | 9 | [
"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... | [
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] | 1607 | 1607.06365_arXiv.txt | Motivated by, for instance, observed correlations between the mass of an AGN's central black hole and the host galaxy's velocity dispersion \citep[e.g.,][]{2000_Gebhardt_Bender_Bower} and between black hole mass and bulge mass \citep[e.g.,][]{1995ARA&A..33..581K}, there is an ongoing debate whether, and if so, how star... | \label{sec:summary} With only one model setup we were able to reproduce three observational findings that have been identified in galaxies: (i) The observed time lag between starburst and AGN activity is, in our work, principally caused by a viscous time lag the gas needs to flow through the AGN's accretion disc until... | 16 | 7 | 1607.06365 | 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 accreti... | false | [
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12472835 | [
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] | 2016MNRAS.462.3344D | [
"The analemma criterion: accidental quasi-satellites are indeed true quasi-satellites"
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] | 1607 | 1607.06686_arXiv.txt | Objects trapped in a 1:1 mean motion resonance with a host (planetary or not) are classified as co-orbitals of the host, independently of the shape and orientation of their paths (Morais \& Morbidelli 2002); in other words, to be classed as co-orbitals their orbits do not have to resemble that of the host as long as th... | In this paper, we have explored a new criterion to identify quasi-satellites. In sharp contrast with the numerical strategies customarily applied in the study of co-orbital bodies, the criterion described here can make direct use of observational astrometric data. Our conclusions can be summarized as follows. \begin{en... | 16 | 7 | 1607.06686 | 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-s... | false | [
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12583834 | [
"Clifton, Timothy",
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] | 2017GReGr..49...30C | [
"The magnetic part of the Weyl tensor, and the expansion of discrete universes"
] | 16 | [
"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"
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] | 1607 | 1607.00775_arXiv.txt | The large-scale expansion of the Universe is usually taken to be dominated by the Newtonian part of the gravitational field. This idea probably originates from the close correspondence between the Friedmann equations of general relativity and the equations that govern Newtonian cosmologies \cite{milne}, but also has st... | \l{sec:discussion} We have considered the effect of $H_{ab}$ on the evolution of LRS curves in lattice models of the universe. These models treat the matter in the Universe as a collection of point-like sources, and allow the formulation of cosmology as an initial value problem. They are therefore particularly well su... | 16 | 7 | 1607.00775 | 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 ... | false | [
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... | 10.511437 | 0.329424 | 89 |
12409147 | [
"Dissauer, K.",
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"Veronig, A. M.",
"Vanninathan, K.",
"Magdalenić, J."
] | 2016ApJ...830...92D | [
"Projection Effects in Coronal Dimmings and Associated EUV Wave Event"
] | 11 | [
"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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"10.3847/0004-637X/830/2/92",
"10.48550/arXiv.1607.05961"
] | 1607 | 1607.05961_arXiv.txt | Coronal mass ejections (CMEs) are large-scale coronal magnetic field structures expelled into the heliosphere. They are the main causes of space weather disturbances since they may drive interplanetary shocks and produce geomagnetic storms. Accompanied with CMEs we observe activities low in the solar atmosphere includi... | \label{discussion} The EUV wave/CME/coronal dimming event on September 6, 2011 shows several peculiar features. Only by complementing the results of SDO observations with ST-A, we were able to disentangle real signatures from signatures arising from LOS integration and projection effects. Furthermore, we were able to ... | 16 | 7 | 1607.05961 | 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... | false | [
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14122128 | [
"Wu, Hao-Yi",
"Doré, Olivier",
"Teyssier, Romain",
"Serra, Paolo"
] | 2018MNRAS.475.3974W | [
"Interpreting the cosmic far-infrared background anisotropies using a gas regulator model"
] | 9 | [
"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",
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"10.1093/mnras/sty071",
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] | 1607 | 1607.02546_arXiv.txt | Cosmic far-infrared background (CFIRB) originates from unresolved dusty star-forming galaxies across cosmic time. In these galaxies, the ultraviolet (UV) photons associated with newly formed, massive stars are absorbed by dust and re-emitted in far-infrared (FIR), and the FIR emission serves as an indicator of the star... | \label{sec:discussion} In this work, we show that the gas regulator model provides a qualitative description for the CFIRB power spectra but is unable to produce all the details in observations. In this section, we discuss the limitations of our implementation of the gas regulator model and possible improvements. In ... | 16 | 7 | 1607.02546 | 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 reg... | false | [
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... | 13.294259 | 7.068842 | 132 |
12594106 | [
"Andresen, H.",
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"Müller, E.",
"Janka, H. -Th."
] | 2017MNRAS.468.2032A | [
"Gravitational wave signals from 3D neutrino hydrodynamics simulations of core-collapse supernovae"
] | 148 | [
"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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"10.1093/mnras/stx618",
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] | 1607 | 1607.05199_arXiv.txt | Despite impressive progress during recent years, the explosion mechanism powering core-collapse supernovae is still not fully understood. For ordinary supernovae with explosion energies up to $\mathord{\sim}10^{51} \,\mathrm{erg}$, the prevailing theory is the delayed neutrino-driven mechanism (see \citealp{janka_12,bu... | \label{sec:con} We have studied the GW signal from the accretion phase and the early explosion phase of core-collapse supernovae based on four recent 3D multi-group neutrino hydrodynamics simulations. We considered four models based on three progenitors with ZAMS masses of $11.2 M_\odot$, $20 M_\odot$, and $27 M_\odot$... | 16 | 7 | 1607.05199 | 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 sh... | false | [
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"high-frequency surface g modes",
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"enhanced low-frequency emission",
"high-frequency variability"... | 5.70114 | 2.208929 | 62 |
12408923 | [
"Ruffini, R.",
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"Enderli, M.",
"Kovacevic, M.",
"Moradi, R.",
"Penacchioni, A. V.",
"Pisani, G. B.",
"Rueda, J. A.",
"Wang, Y."
] | 2016ApJ...831..178R | [
"GRB 090510: A Genuine Short GRB from a Binary Neutron Star Coalescing into a Kerr-Newman Black Hole"
] | 21 | [
"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... | [
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"10.3847/0004-637X/831/2/178",
"10.48550/arXiv.1607.02400"
] | 1607 | 1607.02400_arXiv.txt | Thanks to a fortunate coincidence of observations by AGILE, \textit{Fermi}, and \textit{Swift} satellites, together with the optical observations by the VLT/FORS2 and the Nordic Optical Telescope, it has been possible to obtain an unprecedented set of data, extending from the optical-UV, through the X-rays, all the way... | It is interesting to recall some of the main novelties introduced in this paper with respect to previous works on GRB 090510. Particularly noteworthy are the differences from the previous review of short bursts by \citet{2007PhR...442..166N}, made possible by the discovery of the high energy emission by the Fermi team ... | 16 | 7 | 1607.02400 | 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</S... | false | [
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"short gamma-ray bursts",
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"thermal spectra",
"binary neutron stars",
"their observed overall energetics",
"the prompt emission",
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12472712 | [
"Chiaro, G.",
"Salvetti, D.",
"La Mura, G.",
"Giroletti, M.",
"Thompson, D. J.",
"Bastieri, D."
] | 2016MNRAS.462.3180C | [
"Blazar flaring patterns (B-FlaP) classifying blazar candidate of uncertain type in the third Fermi-LAT catalogue by artificial neural networks"
] | 48 | [
"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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"astronomy"
] | 12 | [
"methods: statistical",
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] | 1607 | 1607.07822_arXiv.txt | Blazars are active galactic nuclei (AGN) with a radio-loud behavior and a relativistic jet pointing toward the observer. \citep{Abdo01} These sources are divided into two main classes: BL Lacertae objects (BL Lacs) and Flat Spectrum Radio Quasars (FSRQs), which show very different optical spectra even if in other waveb... | \label{sec:conclusions} We developed an Artificial Neural Network technique based on B-FlaP information to assess the likelihood that a $\gamma$-ray source can belong to the BL Lac or FSRQ family, or more interestingly to the HSP blazar subclass, using only $\gamma$-ray data. We tested the method on sources that are c... | 16 | 7 | 1607.07822 | 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 c... | false | [
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12471923 | [
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] | 2016MNRAS.461.3993M | [
"Braking indices of pulsars obtained in the presence of an effective force"
] | 10 | [
"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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] | 1607 | 1607.06129_arXiv.txt | Pulsars are normally modelled as rapidly rotating, highly magnetized stars composed mainly of neutrons. It has been observed that their rotation frequencies are decaying, this spin-down being quantified by the braking index (BI), $n$, defined by: \eqnn{eq:def_n}{n \equiv \frac{{\Omega \ddot \Omega }} {{\dot \Omega ^2... | We analysed a modification of the canonical model for pulsars' spin-down that introduces an effective force that is tangential to the star's rotation motion. Our goal was to provide more precise predictions of pulsars' BI. The effective force involves all yet unknown physical contributions that make pulsars' BI less th... | 16 | 7 | 1607.06129 | 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 c... | false | [
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12595569 | [
"Ferrara, A.",
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] | 2017MNRAS.471.5018F | [
"The infrared-dark dust content of high redshift galaxies"
] | 48 | [
"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",
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"10.1093/mnras/stx1898",
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] | 1607 | 1607.01824_arXiv.txt | \label{Mot} Dust grains are a fundamental constituent of the interstellar medium (ISM) of galaxies. A large fraction ($\approx $ 50\% in the Milky Way) of the heavy elements produced by nucleosynthetic processes in stellar interiors can be locked into these solid particles. They are vital elements of the ISM multiphas... | \label{Con} We have presented a dust extinction and FIR emission model that is aimed at explaining the IRX-$\beta$ relation for high redshift ($z \simgt 5$) galaxies. We have first derived the dust mass vs. UV spectral slope, $\beta$ relation. Then the temperature of grains exposed to the typical range of internal UV f... | 16 | 7 | 1607.01824 | 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 `inf... | false | [
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12473132 | [
"Quillen, Alice C.",
"Kueter-Young, Andrea",
"Frouard, Julien",
"Ragozzine, Darin"
] | 2016MNRAS.463.1543Q | [
"Tidal spin down rates of homogeneous triaxial viscoelastic bodies"
] | 15 | [
"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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"10.1093/mnras/stw2094",
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] | 1607 | 1607.08591_arXiv.txt | The simplicity of analytic formulae for tidal spin down of spherical bodies and the associated drift rate in semi-major axis \citep{goldreich63,goldreich68,kaula64,efroimsky09,efroimsky13} has made it possible to estimate tidal spin-down rates in diverse settings, including stars, exoplanets, satellites, and asteroid... | \begin{table} \vbox to90mm{\vfil \caption{\large Information about Haumea and Hi'iaka \label{tab:haumea}} \begin{tabular}{@{}lllllll} \hline Haumea: && \\ Semi-major axis of ellipsoid & $a_H$ & 960 km \\ Axis ratio & $b_H/a_H$ & 0.80 \\ Axis ratio & $c_H/a_H$ & 0.52 \\ Volumetric radius & $R_{vH}$ & 716.6 km \\ Mass... | 16 | 7 | 1607.08591 | 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 visco... | false | [
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5100913 | [
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"Aravena, M.",
"Wagg, J.",
"Popping, G.",
"Cortes, P.",
"Hodge, J.",
"Weiss, A.",
"Bertoldi, F.",
"Riechers, D."
] | 2016ApJ...833...73C | [
"The ALMA Spectroscopic Survey in the Hubble Ultra Deep Field: Implications for Spectral Line Intensity Mapping at Millimeter Wavelengths and CMB Spectral Distortions"
] | 28 | [
"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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"10.3847/1538-4357/833/1/73",
"10.48550/arXiv.1607.06773"
] | 1607 | 1607.06773_arXiv.txt | Intensity mapping of the cumulative CO and other millimeter and submillimeter line emission from early galaxies has been proposed as a new means to probe very large-scale structures in the distant Universe (Carilli 2011; Gong et al. 2011; Gong et al. 2012; Yue et al. 2015). Intensity mapping entails low spatial and spe... | \subsection{Limits} As a pilot ALMA study, we reemphasize that the volumes in question are small, as are the number of detections. Hence, our conclusions and uncertainties are dominated by cosmic variance and simple shot noise (Poisson statistics). Aravena et al. (2016b) consider the issue of cosmic variance in the c... | 16 | 7 | 1607.06773 | 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 s... | false | [
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"a low resolution inten... | 13.209164 | 7.52868 | 132 |
12434275 | [
"Alard, C."
] | 2016arXiv160701365A | [
"Second order singular pertubative theory for gravitational lenses"
] | 1 | [
"-"
] | [
"2017MNRAS.467.1997A"
] | [
"astronomy"
] | 3 | [
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] | [
"2002MNRAS.332..951W",
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"2003MNRAS.340..105M",
"2006ApJ...653..936S",
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"2009A&A...506..609A",
"2010A&A...513A..39A"
] | [
"10.48550/arXiv.1607.01365"
] | 1607 | 1607.01365_arXiv.txt | The singular perturbative method is a non parametric approach to gravitational lenses offering a direct relation between the description of the lens and the observations. The direct relation between the lens and the data minimize the degeneracy problems generally encountered in gravitational lenses modeling (see for in... | It is relatively simple to estimate the second order perturbative expansion as a correction of the first order expansion. In particular the correction in the thin source limit is simple and provide a noticeable improvement over the first order pertubative expansion. The full iterative second order correction converge t... | 16 | 7 | 1607.01365 | 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... | false | [
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"the first order pertubativ... | 12.571441 | 3.801993 | 162 |
12593827 | [
"Geng, Chao-Qiang",
"Lee, Chung-Chi"
] | 2017MNRAS.464.2462G | [
"Matter density perturbation and power spectrum in running vacuum model"
] | 5 | [
"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",
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"2019ChPhC..43b5102Z",
"2020ChPhC..44j5104G",
"2020EPJC...80...69G"
] | [
"astronomy"
] | 4 | [
"dark energy",
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"10.1093/mnras/stw2549",
"10.48550/arXiv.1607.07296"
] | 1607 | 1607.07296_arXiv.txt | \label{sec:introduction} It is well-known that the Type-Ia supernova observations (Riess et al. \citep{Riess:1998cb}; Perlmutter et al. \citep{Perlmutter:1998np}) have revealed the late-time accelerating expansion of our universe. To realize the accelerating universe, it is necessary to introduce a negative pressure f... | \label{sec:conclusion} We have studied the matter density perturbation $\delta_m$ and matter power spectrum $P(k)$ in the RVM with $\Lambda = \Lambda_0 + 6 \sigma H H_0+ 3\nu H^2$. By rewriting $\Lambda$ to be a function of the covariant derivative of four-velocity as $\Lambda = \Lambda_0+ 2 \sigma \nabla_{\mu} U^{\... | 16 | 7 | 1607.07296 | 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 th... | false | [
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12408329 | [
"Kogut, A.",
"Fixsen, D. J."
] | 2016ApJ...826..101K | [
"Foreground Bias from Parametric Models of Far-IR Dust Emission"
] | 11 | [
"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"
] | [
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"2017MNRAS.471.1126A",
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"2023PhRvD.107f3506N",
"2024MNRAS.527.5751A"
] | [
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] | 3 | [
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] | [
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"10.3847/0004-637X/826/2/101",
"10.48550/arXiv.1607.02150"
] | 1607 | 1607.02150_arXiv.txt | Polarization of the cosmic microwave background (CMB) provides a critical test for models of inflation. The primary signature is is a parity-odd curl component in the polarization on angular scales of a few degrees or larger \citep{kamionkowski/etal:1997, seljak/zaldarriaga:1997}. The amplitude of this ``B-mode'' signa... | Parametric modeling of the diffuse dust foreground can bias estimates of CMB polarization if the chosen dust model cannot adequately represent the true emission spectrum. For the commonly used one- or two-component modified blackbody models, the bias can exceed levels $\Delta r \sim {\rm few} \times 10^{-3}$, large com... | 16 | 7 | 1607.02150 | 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 du... | false | [
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2426651 | [
"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"
] | 2016ApJ...828...21N | [
"ZFIRE: A KECK/MOSFIRE Spectroscopic Survey of Galaxies in Rich Environments at z ∼ 2"
] | 63 | [
"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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] | 18 | [
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"2003MNRAS.344.1... | [
"10.3847/0004-637X/828/1/21",
"10.48550/arXiv.1607.00013"
] | 1607 | 1607.00013_arXiv.txt | The rapid development of very deep multi-wavelength imaging surveys from the ground and space in the past decade has greatly enhanced our understanding of important questions in galaxy evolution particularly through the provision of `photometric redshift' estimates (and hence the evolutionary sequencing of galaxies) ... | \label{sec:summary} Here we present the ZFIRE survey of galaxies in rich environments and our first public data release. A detailed description of the data reduction used by ZFIRE is provided. The use of a flux standard star along with photometric data from ZFOURGE and UKIDSS has made it possible to flux calibrate ... | 16 | 7 | 1607.00013 | 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 ... | false | [
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1797939 | [
"Lutovinov, Alexander A.",
"Tsygankov, Sergey S.",
"Krivonos, Roman A.",
"Molkov, Sergey V.",
"Poutanen, Juri"
] | 2017ApJ...834..209L | [
"Propeller Effect in the Transient X-Ray Pulsar SMC X-2"
] | 33 | [
"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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"2018A&A...610A..46C",
"2018ApJ...861L...7B",
"2018MNRAS.479L.134T",
"2019A&A...621A.134T",
"2019A&A...622A.... | [
"astronomy"
] | 8 | [
"accretion",
"accretion disks",
"magnetic fields",
"stars: individual: SMC X-2",
"X-rays: binaries",
"Astrophysics - High Energy Astrophysical Phenomena"
] | [
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"10.3847/1538-4357/834/2/209",
"10.48550/arXiv.1607.03427"
] | 1607 | 1607.03427_arXiv.txt | \label{sec:intro} The Small Magellanic Cloud (SMC) is the satellite of the Milky Way situated at the distance of $d\simeq62$~kpc \citep{2012AJ....144..107H}. This galaxy is extremely rich in Be X-ray binary systems, harboring a neutron star orbiting around an OBe companion \citep[see recent review of ][and references ... | In this paper we have reported the discovery of the propeller effect in the bright transient X-ray pulsar \smc. The dramatic drop of the source luminosity (by a factor of more than 100) on the time scale of a few days was revealed thanks to the monitoring campaign with the {\it Swift}/XRT telescope, organized during th... | 16 | 7 | 1607.03427 | 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</SU... | false | [
"independent results",
"the transient X-ray pulsar SMC X-2",
"the sixth pulsating X-ray source",
"L}<SUB>{lim</SUB>}≃ 4×",
"agreement",
"the Type II outburst",
"SMC",
"the propeller regime",
"several ×10<SUP>34</SUP> erg s",
"the spectral analysis",
"SUP>39</SUP",
"≃10",
"the system B",
"s... | 5.6891 | 5.959013 | 46 |
12409546 | [
"Tingay, S. J.",
"Tremblay, C.",
"Walsh, A.",
"Urquhart, R."
] | 2016ApJ...827L..22T | [
"An Opportunistic Search for Extraterrestrial Intelligence (SETI) with the Murchison Widefield Array"
] | 21 | [
"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",
"Inte... | [
"2018AJ....156..260W",
"2018ApJ...856...31T",
"2018ApJ...857...11T",
"2018PASP..130d4502M",
"2018exha.book.....P",
"2019AcAau.155...51H",
"2019PASA...36...50B",
"2020AJ....159...86P",
"2020ApJ...891..174Z",
"2020IJAsB..19..299G",
"2020PASA...37...35T",
"2021AJ....162...33G",
"2021AJ....162..... | [
"astronomy"
] | 2 | [
"instrumentation: interferometers",
"planets and satellites: detection",
"radio lines: planetary systems",
"techniques: spectroscopic",
"Astrophysics - Earth and Planetary Astrophysics",
"Astrophysics - Instrumentation and Methods for Astrophysics"
] | [
"1975Icar...26..462.",
"1981MNRAS.194..693L",
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"1995ASPC...77..433S",
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"1998AJ....115.1693C",
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"2001SPIE.4273..104W",
"2007JCAP...01..020L",
"2009ASPC..420..431K",
"2009IEEEP..97.1... | [
"10.3847/2041-8205/827/2/L22",
"10.48550/arXiv.1607.08818"
] | 1607 | 1607.08818_arXiv.txt | The first modern Search for ExtraTerrestrial Intelligence (SETI) was undertaken at radio wavelengths in 1960 at Green Bank, West Virginia \citep{dra08}, targeting two stars, Tau Ceti and Epsilon Eridani at frequencies near the 21-cm line of neutral hydrogen. In the decades since, SETI programs have continued to be und... | The great majority of exoplanet systems listed in Table 1 are at large distances, yielded from microlensing experiments toward the Galactic Centre, meaning that the observational limits on detectable transmitter power from the MWA are very high, inferred isotropic powers of $10^{17} - 10^{19}$ W. Even if a directional... | 16 | 7 | 1607.08818 | 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 rad... | false | [
"MWA data",
"MWA",
"low radio frequencies",
"Square Kilometre Array",
"Equivalent Isotropic Radiated Power",
". deg",
"observing time",
"SETI",
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"The MWA frequency range",
"narrow line emission",
"isotropic transmitter powers",
"field",
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... | 12.837073 | 12.860886 | 6 |
11492362 | [
"Chávez, R.",
"Plionis, M.",
"Basilakos, S.",
"Terlevich, R.",
"Terlevich, E.",
"Melnick, J.",
"Bresolin, F.",
"González-Morán, A. L."
] | 2016MNRAS.462.2431C | [
"Constraining the dark energy equation of state with H II galaxies"
] | 64 | [
"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... | [
"2016A&A...592L...7T",
"2016MNRAS.463.1144W",
"2017A&A...599A..76M",
"2017ApJ...843..100W",
"2017JCAP...11..029Y",
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"2018A&A...615A..55T",
"2018ApJ...866...31R",
"2018JCAP...08..008B",
"2018MNRAS.474.1250F",
"2018MNRAS.474.4... | [
"astronomy"
] | 4 | [
"galaxies: starburst",
"cosmological parameters",
"dark energy",
"Astrophysics - Cosmology and Nongalactic Astrophysics"
] | [
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"10.1093/mnras/stw1813",
"10.48550/arXiv.1607.06458"
] | 1607 | 1607.06458_arXiv.txt | The observational evidence for an accelerated cosmic expansion was first given by Type Ia Supernovae (SNIa) \citep{Riess1998, Perlmutter1999}. Since then, measurements of the cosmic microwave background (CMB) anisotropies \citep[e.g.][]{Jaffe2001, Pryke2002, Spergel2007, Planck2015} and of Baryon Acoustic Oscillations ... | \begin{itemize} \item The FoM of the QDE EoS constraints, provided by the joint HII/BAO/CMB analysis, was found to be larger by 13 percent than those provided by the BAO/CMB joint analysis, even with the very small sample of only 25 high-z HII galaxies. \item Both the QDE and CPL EoS constraints of the HII/BAO/CMB and... | 16 | 7 | 1607.06458 | 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 cons... | false | [
"H II galaxies",
"available high redshift H II galaxies",
"H II",
"high-z H II galaxies",
"cosmic microwave background",
"Baryon Acoustic Oscillations",
"the quintessence dark energy cosmological constraints",
"the resulting Hubble expansion cosmological probe",
"reasonable observing times",
"CMB"... | 11.617276 | 1.371424 | 89 |
2073369 | [
"Gandilo, Natalie N.",
"Ade, Peter A. R.",
"Benford, Dominic",
"Bennett, Charles L.",
"Chuss, David T.",
"Dotson, Jessie L.",
"Eimer, Joseph R.",
"Fixsen, Dale J.",
"Halpern, Mark",
"Hilton, Gene",
"Hinshaw, Gary F.",
"Irwin, Kent",
"Jhabvala, Christine",
"Kimball, Mark",
"Kogut, Alan",
... | 2016SPIE.9914E..1JG | [
"The Primordial Inflation Polarization Explorer (PIPER)"
] | 25 | [
"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)",
"NASA Goddard Space Fli... | [
"2016NCimR..39..399G",
"2016arXiv160501615C",
"2016arXiv160803707Z",
"2017arXiv170602464A",
"2017arXiv170902389F",
"2018ApJ...863..121W",
"2018JCAP...04..016F",
"2019MNRAS.484.1616Z",
"2019arXiv190304592M",
"2020ApJ...891..134X",
"2020JLTP..199.1027A",
"2020PASJ...72....6N",
"2020SPIE11453E.... | [
"astronomy",
"physics"
] | 4 | [
"Astrophysics - Instrumentation and Methods for Astrophysics"
] | [
"2011ApJ...730..138S",
"2013ApOpt..52.8747D"
] | [
"10.1117/12.2231109",
"10.48550/arXiv.1607.06172"
] | 1607 | 1607.06172_arXiv.txt | \label{sec:intro} \begin{figure} [ht] \begin{center} \includegraphics[height=6cm]{Figure1.png} \end{center} \caption[power spectrum] { \label{fig:piperplaincl} Left: The polarization of the CMB can be decomposed into E- and B-modes. Right: B-mode power spectrum assuming a tensor-to-scalar ratio $r=0.02$ from inflationa... | PIPER will map the polarization of the CMB in four frequency bands (200, 270, 350, and 600\,GHz) over 85\% of the sky over a series of conventional balloon flights from the Northern and Southern Hemisphere. This will allow the shape of the B-mode power spectrum to be measured at angular scales up to $90^{\circ}$, const... | 16 | 7 | 1607.06172 | 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 ... | false | [
"large angular scales",
"Continuous Adiabatic Demagnetization",
"circular polarization",
"lower frequencies",
"V",
"l",
"systematic control",
"a Continuous Adiabatic Demagnetization Refrigerator",
"Polarization Modulators",
"PIPER",
"r",
"l ∼ 300",
"U",
"Twin telescopes",
"8 conventional... | 10.593943 | 2.856915 | 68 |
12408854 | [
"Zhang, Haocheng",
"Diltz, Chris",
"Böttcher, Markus"
] | 2016ApJ...829...69Z | [
"Radiation and Polarization Signatures of the 3D Multizone Time-dependent Hadronic Blazar Model"
] | 30 | [
"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... | [
"2016Galax...4...22B",
"2017ApJ...835..125Z",
"2017Galax...5...32Z",
"2018ApJ...863...98P",
"2018JATIS...4a1003T",
"2018MNRAS.473.4107P",
"2018arXiv180711069Z",
"2019ASSL..460..109T",
"2019ApJ...876..109Z",
"2019BAAS...51c..92R",
"2019BAAS...51c.291M",
"2019BAAS...51c.348R",
"2019BAAS...51c.... | [
"astronomy"
] | 4 | [
"galaxies: active",
"galaxies: jets",
"gamma rays: galaxies",
"polarization",
"radiation mechanisms: nonthermal",
"relativistic processes",
"Astrophysics - High Energy Astrophysical Phenomena"
] | [
"1977MNRAS.179..433B",
"1985ApJ...298..114M",
"1992A&A...253L..21M",
"1992A&A...256L..27D",
"1992ApJ...397L...5M",
"1994ApJ...421..153S",
"1995A&A...295..613M",
"1995MNRAS.273..583D",
"1997ApJ...488..669H",
"2000NewA....5..377A",
"2001APh....15..121M",
"2007ApJ...664L..71A",
"2008Natur.452..... | [
"10.3847/0004-637X/829/2/69",
"10.48550/arXiv.1607.06491"
] | 1607 | 1607.06491_arXiv.txt | Blazars are the most violent class of active galactic nuclei. Their emission is known to be nonthermal-dominated, covering the entire electromagnetic spectrum from radio up to TeV $\gamma$-rays, with strong variability on all time scales \citep[e.g.,][]{Aharonian07}. Blazar spectral energy distributions (SEDs) are char... | } In this paper, we have presented the first 3D multi-zone time-dependent lepto-hadronic blazar code, 3DHad, describing a lepto-hadronic model in a parameter regime in which the high-energy emission is dominated by proton synchrotron radiation. By coupling with the 3DPol code, we are able to derive the time-dependent ... | 16 | 7 | 1607.06491 | 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 signat... | false | [
"time",
"leptonic models",
"such signatures",
"neglecting pion production",
"proton synchrotron emission",
"a hadronic blazar model",
"the exact model parameters",
"first",
"the time-dependent radiation and polarization signatures",
"the first time",
"the time-dependent flux and polarization sig... | 16.644976 | 5.061895 | 115 |
12500420 | [
"Yamasaki, Hiroki",
"Mizumoto, Misaki",
"Ebisawa, Ken",
"Sameshima, Hiroaki"
] | 2016PASJ...68...80Y | [
"Origin of the characteristic X-ray spectral variations of IRAS 13224-3809"
] | 12 | [
"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... | [
"2017MNRAS.466.3259M",
"2018PASJ...70...42M",
"2019MNRAS.482.5316M",
"2019MNRAS.486..227G",
"2020MNRAS.492.1363P",
"2020NatAs...4..597A",
"2021MNRAS.500.4506H",
"2022MNRAS.509.3599T",
"2022MNRAS.513.5020M",
"2023ApJ...954...47M",
"2023MNRAS.525..922M",
"2024IAUS..380...82H"
] | [
"astronomy"
] | 3 | [
"galaxies: active",
"galaxies: Seyfert",
"X-rays: galaxies",
"Astrophysics - High Energy Astrophysical Phenomena"
] | [
"1990ApJ...361..440M",
"2001A&A...365L...1J",
"2001A&A...365L...7D",
"2001A&A...365L..18S",
"2002ApJ...568..610E",
"2002MNRAS.335L...1F",
"2003MNRAS.340L..28F",
"2003MNRAS.343L..89B",
"2003PASJ...55..615M",
"2003PASJ...55..625I",
"2004ApJS..155..675K",
"2004MNRAS.347..269G",
"2004MNRAS.349.1... | [
"10.1093/pasj/psw070",
"10.48550/arXiv.1607.00879"
] | 1607 | 1607.00879_arXiv.txt | Among Active Galactic Nuclei (AGNs), Narrow-line Seyfert 1 galaxies (NLS1s) are characterized by their particular X-ray spectral and timing properties. A strong soft excess below $\sim$2 keV and remarkable X-ray variations are often observed, and high-energy spectral drops at $\sim$7 keV and seemingly broadened and ske... | We have studied spectral variations of NLS1 IRAS 13224$-$3809, using all the currently available XMM-Newton and Suzaku archival data. Following Paper I, we examined if the observed spectral variation is explained by the Variable Double Partial Covering (VDPC) model. Consequently, we have found that the VDPC model can s... | 16 | 7 | 1607.00879 | 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 (VDP... | false | [
"significant X-ray spectral variation",
"optical depths",
"spectral variability",
"intriguing iron L-peaks",
"energy dependence",
"double absorption layers",
"strong soft excess emission",
"patchy clouds",
"PASJ",
"keV",
"RMS",
"1H",
"an iron L-edge feature",
"a characteristic iron L-peak"... | 15.983583 | 7.822195 | 118 |
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