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12501480 | [
"Geng, Chao-Qiang",
"Lee, Chung-Chi",
"Zhang, Kaituo"
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"Running cosmological constant with observational tests"
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"Chongqing University of Posts & Telecommunications, Chongqing, 400065, China",
"National Center for Theoretical Sciences, Hsinchu, 300, Taiwan",
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] | 1607 | 1607.02567_arXiv.txt | \label{sec:introduction} The type-Ia supernova observations~\cite{Riess:1998cb,Perlmutter:1998np} have shown that our universe is undergoing a late-time accelerating expansion, which is caused by Dark Energy~\cite{Copeland:2006wr}. The simplest way to realize such a late-time accelerating mechanism is to introduce a c... | \label{sec:conclusion} We have investigated the $\Lambda(t)$CDM model with the dark energy decaying to both matter and radiation, in which $\Lambda(t)= \sigma H + \Lambda_0$. Although this scenario is suitable to describe the late-time accelerating universe at the background level, the linear perturbation analyses of ... | 16 | 7 | 1607.02567 | We investigate the running cosmological constant model with dark energy linearly proportional to the Hubble parameter, Λ = σH +Λ<SUB>0</SUB>, in which the ΛCDM limit is recovered by taking σ = 0. We derive the linear perturbation equations of gravity under the Friedmann-Lemaïtre-Robertson-Walker cosmology, and show the... | false | [
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12458738 | [
"Eroshenko, Yu. N."
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"Dark matter density spikes around primordial black holes"
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] | 1607 | 1607.00612_arXiv.txt | Primordial black holes (PBHs), the possibility of whose formation was predicted in \cite{p41} and \cite{p22}, can give valuable information about processes in the early Universe \cite{p12,p14,p3}, in particular, about the shape of the perturbation spectrum on small scales \cite{p24}. The quantum evaporation of low-mass... | DM clumps can be produced by various mechanisms \cite{p6}. They can be formed both from cosmological density perturbations in the dark matter itself and around compact seed masses, for example, around cosmic strings \cite{p27} or PBHs \cite{p15,p35,p30,p36,p28,p38}. Secondary accretion, the infall and virialization of... | 16 | 7 | 1607.00612 | We show that density spikes begin to form from dark matter particles around primordial black holes immediately after their formation at the radiation-dominated cosmological stage. This stems from the fact that in the thermal velocity distribution of particles there are particles with low velocities that remain in finit... | false | [
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12614143 | [
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"Spallicci, Alessandro D. A. M."
] | 2017PhLB..764..203B | [
"Effective photon mass by Super and Lorentz symmetry breaking"
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"Université d'Orléans, Observatoire des Sciences de l'Univers en région Centre (OSUC), UMS 3116, 1A rue de la Férollerie, 45071 Orléans, France",
"Centro Brasileiro de Pesquisas Físicas (CBPF), Rua Xavier Sigaud 150, 22290-180 Urca, Rio de Janeiro, RJ, Brasil",
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] | 1607 | 1607.08786_arXiv.txt | 16 | 7 | 1607.08786 | In the context of Standard Model Extensions (SMEs), we analyse four general classes of Super Symmetry (SuSy) and Lorentz Symmetry (LoSy) breaking, leading to observable imprints at our energy scales. The photon dispersion relations show a non-Maxwellian behaviour for the CPT (Charge-Parity-Time reversal symmetry) odd a... | false | [
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900376 | [
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"Pala, A. F.",
"Dhillon, V. S.",... | 2016Natur.537..374M | [
"A radio-pulsing white dwarf binary star"
] | 135 | [
"Department of Physics, Gibbet Hill Road, University of Warwick, Coventry CV4 7AL, UK;",
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"Bundesdeutsche Arbeitsgemeinschaft für Veränderliche Sterne e.V. (BAV), Berlin, Germany; American Association of Variable Star Observe... | [
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] | 1607 | 1607.08265_arXiv.txt | 16 | 7 | 1607.08265 | White dwarfs are compact stars, similar in size to Earth but approximately 200,000 times more massive. Isolated white dwarfs emit most of their power from ultraviolet to near-infrared wavelengths, but when in close orbits with less dense stars, white dwarfs can strip material from their companions and the resulting mas... | false | [
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2417607 | [
"Davenport, James R. A."
] | 2016ApJ...829...23D | [
"The Kepler Catalog of Stellar Flares"
] | 254 | [
"Department of Physics & Astronomy, Western Washington University, Bellingham, WA 98225, USA"
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"10.3847/0004-637X/829/1/23",
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] | 1607 | 1607.03494_arXiv.txt | Flares occur on nearly all main sequence stars with outer convective envelopes as a generic result of magnetic reconnection \citep{pettersen1989}. These events occur stochastically, and are most frequently observed on low-mass stars with the deepest convective zones such as M dwarfs. Solar and stellar flares are believ... | I have presented a homogeneous search for stellar flares using every available light curve from the primary 4-year \Kepler mission. A final sample of 4041 flare stars was recovered, with 851168 flare events having energies above the locally determined completeness limit. This analysis included extensive completeness te... | 16 | 7 | 1607.03494 | A homogeneous search for stellar flares has been performed using every available Kepler light curve. An iterative light curve de-trending approach was used to filter out both astrophysical and systematic variability to detect flares. The flare recovery completeness has also been computed throughout each light curve usi... | false | [
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... | 8.526059 | 13.27945 | 130 |
12620005 | [
"Taylor, Andrew M.",
"Giacinti, Gwenael"
] | 2017PhRvD..95b3001T | [
"Cosmic rays in a galactic breeze"
] | 13 | [
"Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Ireland",
"Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, D-69117 Heidelberg, Germany"
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"10.1103/PhysRevD.95.023001",
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] | 1607 | 1607.08862_arXiv.txt | \label{intro} The presence of a Galactic wind has considerable impact on an array of topics connected to describing the Galactic \lq\lq halo\rq\rq\/ environment. With little knowledge about such outer regions of the Galaxy, information provided by non-thermal probes hold the first clues to revealing new information a... | \label{conclusion} We first investigated a scenario in which an advective outflow, emanating from the Galactic center region, carries pre-accelerated CR. These CR produce secondary $\gamma$-rays via $pp$ interactions on target gas. We have demonstrated that one can reproduce a flat $\gamma$-ray surface brightness pr... | 16 | 7 | 1607.08862 | Motivated by the discovery of the nonthermal Fermi bubble features both below and above the Galactic plane, we investigate a scenario in which these bubbles are formed through galacto-centric outflow. Cosmic rays (CR) both diffusing and advecting within a galactic breeze outflow, interacting with the ambient gas presen... | false | [
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12406391 | [
"Di Gesu, L.",
"Costantini, E."
] | 2016A&A...594A..88D | [
"The warm absorber in the radio-loud quasar 4C +74.26"
] | 9 | [
"SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA, Utrecht, The Netherlands; Department of Astronomy, University of Geneva, 16 Ch. d' Ecogia, 1290, Versoix, Switzerland",
"SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA, Utrecht, The Netherlands"
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"2023arXiv230210930G",
"2024arXiv240502391Y"
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"10.48550/arXiv.1607.01943"
] | 1607 | 1607.01943_arXiv.txt | \label{intro5} In the last fifteen years, thanks to the advent of high-resolution X-ray spectrometers, such as the \xmm \th \th Reflection Grating Spectrometer (RGS) or the \chandra Low and High Energy Transmission Grating Spectrometers (LETGS and HETGS), our knowledge of the circumnuclear gaseous environment of active... | \label{dsou} We have presented a joint analysis of the RGS and HETGS spectra of the heavily X-ray absorbed radio-loud quasar 4C +74.26. Thanks to the high spectral resolution of these grating spectra, we were able to reveal a rich spectrum of absorption features originating from both Galactic and intrinsic material.... | 16 | 7 | 1607.01943 | Outflows of photoionized gas are commonly detected in the X-ray spectra of Seyfert 1 galaxies. However, the evidence for this phenomenon in broad line radio galaxies, which are analogous to Seyfert 1 galaxies in the radio-loud regime, has so far been scarce. Here, we present the analysis of the X-ray absorption in the ... | false | [
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12473067 | [
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] | 2016MNRAS.461.4215M | [
"Finding binaries from phase modulation of pulsating stars with Kepler - IV. Detection limits and radial velocity verification"
] | 30 | [
"Sydney Institute for Astronomy (SIfA), School of Physics, The University of Sydney, NSW 2006, Australia; Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, DK-8000 Aarhus C, Denmark; Department of Astronomy, The University of Tokyo, Tokyo 113-0033, Japan",
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"10.48550/arXiv.1607.07879"
] | 1607 | 1607.07879_arXiv.txt | Two methods are traditionally used to detect and characterise binary companions to stars: radial velocities (RVs) from spectroscopy and eclipse measurements from photometry. The availability of four years of high-precision photometry from the \textit{Kepler} Mission has facilitated a third method, namely measuring the ... | We have developed MCMC software to solve binary orbits based on a series of time delay observations, and to provide robust uncertainties. We simulated orbits covering a range of parameters to explore the sensitivity limits of the method, the factors governing those limits, and to predict the lowest mass companions dete... | 16 | 7 | 1607.07879 | We explore the detection limits of the phase modulation (PM) method of finding binary systems among multiperiodic pulsating stars. The method is an attractive way of finding non-transiting planets in the habitable zones of intermediate-mass stars, whose rapid rotation inhibits detections via the radial velocity (RV) me... | false | [
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12614315 | [
"Bridle, Sarah",
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"Fernandez, Susana",
"Guzowski, Pawel",
"Söldner-Rembold, Stefan"
] | 2017PhLB..764..322B | [
"A combined view of sterile-neutrino constraints from CMB and neutrino oscillation measurements"
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"The University of Manchester, School of Physics and Astronomy, Manchester, M13 9PL, United Kingdom",
"The University of Manchester, School of Physics and Astronomy, Manchester, M13 9PL, United Kingdom",
"The University of Manchester, School of Physics and Astronomy, Manchester, M13 9PL, United Kingdom",
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] | 1607 | 1607.00032_arXiv.txt | \label{intro} The search for low-mass sterile neutrinos is motivated by several experimental anomalies that are not consistent with the three-flavour paradigm. Sterile neutrinos would change the oscillation probabilities observed by detecting neutrinos from accelerators, nuclear reactors, or produced in the atmosphere... | \label{sec:conclusions} In conclusion, we compare sterile neutrino constraints from oscillation experiments and cosmological constraints. We use the quantum kinetic equations to convert between the standard oscillation parameterization of neutrinos (the mass-squared difference and mixing angle) and the cosmology param... | 16 | 7 | 1607.00032 | We perform a comparative analysis of constraints on sterile neutrinos from the Planck experiment and from current and future neutrino oscillation experiments (MINOS, IceCube, SBN). For the first time, we express joint constraints on N<SUB>eff</SUB> and m<SUB>eff</SUB><SUP>sterile</SUP> from the CMB in the Δm<SUP>2</SUP... | false | [
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12462050 | [
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] | 1607 | 1607.05329_arXiv.txt | \label{intro} Baryon acoustic oscillations (BAO) are widely used to establish the distance-redshift relation enabling to constrain the expansion history and the composition of the Universe \cite{Eisenstein:1998tu,Eisenstein:2005su}. BAO measurements aim at providing (sub-) percent precision in the near future and thus... | \label{sec:conclus} In these notes we discussed the non-linear effects in the BAO and sketched the way how one can systematically take them into account within time-sliced perturbation theory. We outlined the physical picture behind the interactions with large scale bulk flows and argued the need for IR resummation if... | 16 | 7 | 1607.05329 | In this contribution we will discuss the non-linear effects in the baryon acoustic oscillations and present a systematic and controllable way to account for them within time-sliced perturbation theory. | false | [
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12511163 | [
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12435851 | [
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1513670 | [
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] | 1607 | 1607.02353_arXiv.txt | \label{sec:intro} The last six years have seen the surprising discovery of new classes of intrinsically bright supernovae. They show absolute peak magnitudes of M$\sim-21$ \citep[e.g.][]{qu11,2011ApJ...743..114C,in14} and a tendency to occur in dwarf, metal poor galaxies \citep[e.g.][]{ch13,lu14,le15a,ch16}. They do n... | We have presented the first spectropolarimetric data for a SLSN. We have gathered two epochs, one pre-peak at -23.7d and the second 27.5 days after maximum light in the rest-frame. Our analysis of these data indicates: \begin{enumerate} \item the presence of a dominant axis and no physical departure from it; \item a s... | 16 | 7 | 1607.02353 | We present the first spectropolarimetric observations of a hydrogen-free superluminous supernova (SLSN) at z = 0.1136, namely SN 2015bn. The transient shows significant polarization at both of the observed epochs: one 24 days before maximum light in the rest-frame, and the other at 27 days after peak luminosity. Analys... | false | [
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] | 1607 | 1607.07740_arXiv.txt | While pulsars are primarily detected and observed with high time resolution in order to resolve their narrow pulses, the phase-averaged emissions of many pulsars can be detected in previous radio continuum surveys~\citep[e.g.,][]{kca+98,ht99,k00}. More importantly, continuum surveys are equally sensitive to all pulsars... | \label{discussion} We investigated the variation of pulsar intensity caused by DISS in variance images. Through simulations, we studied the sensitivity of variance images on detecting pulsars and compared it with Stokes I images. Using data taken with MWA, we demonstrated that variance images can lead to the detection... | 16 | 7 | 1607.07740 | Pulsars are the only cosmic radio sources known to be sufficiently compact to show diffractive interstellar scintillations. Images of the variance of radio signals in both time and frequency can be used to detect pulsars in large-scale continuum surveys using the next generation of synthesis radio telescopes. This tech... | false | [
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12595183 | [
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"Chernyakova, Maria",
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] | 2017MNRAS.471.3657Z | [
"High-energy gamma-rays from Cyg X-1"
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"Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, Bartycka 18, PL-00-716 Warszawa, Poland",
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"School of Physical Sciences, Dublin City University, Glasnevin, Dublin 9, Ireland; DIAS, F... | [
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] | 1607 | 1607.05059_arXiv.txt | \label{intro} Cyg X-1, an archetypical black-hole binary, shows two main spectral states, hard and soft. In the hard state, the main component of its X-ray spectrum appears to be thermal Comptonization in a plasma with the electron temperature of $k T_{\rm e}\sim 100$ keV, which features a sharp cutoff [in the $EF(E)$... | \label{conclusions} We have obtained measurements and upper limits of the flux from Cyg X-1 in the 0.04--200 GeV energy band based on observations of the \fermi/LAT. Our observational results confirm, and significantly extend, the independent results of \citet{zanin16}. We have detected a steady emission in the 0.04--... | 16 | 7 | 1607.05059 | We have obtained a firm detection of Cyg X-1 during its hard and intermediate spectral states in the energy range of 40 MeV-60 GeV based on observations by the Fermi Large Area Telescope, confirming the independent results at ≥60 MeV of a previous work. The detection significance is ≃8σ in the 0.1-10 GeV range. In the ... | false | [
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12473004 | [
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] | 1607 | 1607.00951_arXiv.txt | \label{sec:introduction} Many spectroscopic, spectrophotometric and photometric observational studies have revealed that globular clusters (GCs) host multiple stellar populations characterized by different chemical properties. While the first stellar generation (FG) has a chemical composition equal to that of the prist... | \label{sec:conc} We proposed a scheme for the interaction of the GC wind powered by the SNe II with the surrounding ambient medium. This interaction provides a viable mechanism to supply pristine gas and dilutes AGB ejecta during the SG star formation phase in early Globular Clusters. We have shown that our proposed m... | 16 | 7 | 1607.00951 | We study the interaction of the early spherical GC wind powered by Type II supernovae (SNe II) with the surrounding ambient medium consisting of the gaseous disc of a star-forming galaxy at redshift z ≳ 2. The bubble formed by the wind eventually breaks out of the disc, and most of the wind moves directly out of the ga... | false | [
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12510952 | [
"Korsmeier, Michael",
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] | 2016PhRvD..94l3019K | [
"Galactic cosmic-ray propagation in the light of AMS-02: Analysis of protons, helium, and antiprotons"
] | 63 | [
"Institute for Theoretical Particle Physics and Cosmology, RWTH Aachen University, 52056 Aachen, Germany",
"Institute for Theoretical Particle Physics and Cosmology, RWTH Aachen University, 52056 Aachen, Germany"
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"10.1103/PhysRevD.94.123019",
"10.48550/arXiv.1607.06093"
] | 1607 | 1607.06093_arXiv.txt | Theory} The propagation of CR can be described by the well-known diffusion equation \cite{StrongMoskalenko_CR_rewview_2007} for the particle density $\psi_i$ of species $i$ per volume and absolute value of momentum $p$ \begin{eqnarray} \label{eqn::PropagationEquation} \frac{\partial \psi_i (\bm{x}, p, t)}{\partial t}... | Summary and Conclusion} We have presented new constraints on the propagation of Galactic CRs from an (up to) 11-dimensional parameter fit to the latest AMS-02 spectra for $p$, He, and $\bar{p}/p$. Solar modulation is treated within the force-field approximation, but the modulation potential is constrained with a nov... | 16 | 7 | 1607.06093 | We present novel constraints on cosmic-ray propagation in the Galaxy using the recent precise measurements of proton and helium spectra from AMS-02, together with preliminary AMS-02 data on the antiproton over proton ratio. To explore efficiently the large (up to 11-dimensional) parameter space we employ the nested-sam... | false | [
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12465028 | [
"Algoner, W. C.",
"Velten, H. E. S.",
"Zimdahl, W."
] | 2016JCAP...11..034A | [
"Scalar-tensor extension of the ΛCDM model"
] | 6 | [
"Departamento de Física, Universidade Federal do Espírito Santo, Av. Fernando Ferrari, 514, Campus de Goiabeiras, CEP 29075-910, Vitória, Espírito Santo, Brazil",
"Departamento de Física, Universidade Federal do Espírito Santo, Av. Fernando Ferrari, 514, Campus de Goiabeiras, CEP 29075-910, Vitória, Espírito Sant... | [
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] | 5 | [
"General Relativity and Quantum Cosmology",
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"10.1088/1475-7516/2016/11/034",
"10.48550/arXiv.1607.03952"
] | 1607 | 1607.03952_arXiv.txt | \label{Introduction} In scalar-tensor theories the gravitational interaction is mediated both by a metric tensor and a scalar field. The interest in this type of theories of gravity is connected with the expectation that the observed late-time accelerated expansion of the Universe may be understood without a dark-ene... | \label{conclusions} We have established a class of scalar-tensor-theory-based cosmological models which are simple extensions of the $\Lambda$CDM model. The background dynamics of this class has been discussed in detail. Our main result is an analytic expression (\ref{H2Phi}) for the Hubble rate which explicitly quant... | 16 | 7 | 1607.03952 | We construct a cosmological scalar-tensor-theory model in which the Brans-Dicke type scalar Φ enters the effective (Jordan-frame) Hubble rate as a simple modification of the Hubble rate of the ΛCDM model. This allows us to quantify differences between the background dynamics of scalar-tensor theories and general relati... | false | [
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5079399 | [
"Smith, Matthew W. L.",
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"Ciesla, Laure",
"Clemens, Marcel",
"Clements, David L.",
"Cooray, Asantha R.",
"Cortese, Luca",
"Davies, J... | 2016MNRAS.462..331S | [
"Far-reaching dust distribution in galaxy discs"
] | 27 | [
"School of Physics and Astronomy, Cardiff University, The Parade, Cardiff CF24 3AA, UK",
"School of Physics and Astronomy, Cardiff University, The Parade, Cardiff CF24 3AA, UK",
"Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281 S9, B-9000 Gent, Belgium; Institute of Astronomy, University of Cambri... | [
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] | 1607 | 1607.01020_arXiv.txt | Recent studies of the extinction of quasars \citep{Menard2010} and the reddening of galaxies \citep{Peek2015} imply that approximately 50\% of the interstellar dust in the universe lies outside galactic disks. However, we still know remarkably little about how far out the dust in galactic disks extends. Spiral galaxie... | \label{sec:conc} In this paper we present the results of combining images of a large sample of nearby galaxies made from observations with the \textit{Herschel Space Observatory}. By combining the images, we determine how the average surface-density of dust depends on radius. We find the following results: \begin{enum... | 16 | 7 | 1607.01020 | In most studies of dust in galaxies, dust is only detected from its emission to approximately the optical radius of the galaxy. By combining the signal of 110 spiral galaxies observed as part of the Herschel Reference Survey, we are able to improve our sensitivity by an order of magnitude over that for a single object.... | false | [
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"... | 12.389791 | 8.0452 | 187 |
3996362 | [
"Du, X.",
"Landecker, T. L.",
"Robishaw, T.",
"Gray, A. D.",
"Douglas, K. A.",
"Wolleben, M."
] | 2016PASP..128k5006D | [
"Gain and Polarization Properties of a Large Radio Telescope from Calculation and Measurement: The John A. Galt Telescope"
] | 12 | [
"National Research Council Canada, Dominion Radio Astrophysical Observatory, P.O. Box 248, Penticton, British Columbia, V2A 6J9, Canada ; Department of Electrical Engineering, University of Victoria, Canada ; School of Engineering, University of British Columbia, Kelowna, Canada;",
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"10.1088/1538-3873/128/969/115006",
"10.48550/arXiv.1607.06436"
] | 1607 | 1607.06436_arXiv.txt | \label{intro} Full exploitation of a radio telescope requires detailed and accurate knowledge of its radiation properties. Modern tools of antenna engineering, electromagnetic simulators, offer the ability to analyze telescope performance. To what extent can they deliver a true picture of telescope characteristics? Ca... | \label{disc} We have used GRASP-10 to calculate the properties of a large radio telescope, and have compared the results of those calculations with measurements wherever possible. The GRASP-10 evaluation of aperture efficiency of the Galt Telescope has successfully predicted the frequency dependence of that parameter,... | 16 | 7 | 1607.06436 | Measurement of the brightness temperature of extended radio emission demands knowledge of the gain (or aperture efficiency) of the telescope and measurement of the polarized component of the emission requires correction for the conversion of unpolarized emission from sky and ground to apparently polarized signal. Radia... | false | [
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12406343 | [
"Dafonte, C.",
"Fustes, D.",
"Manteiga, M.",
"Garabato, D.",
"Álvarez, M. A.",
"Ulla, A.",
"Allende Prieto, C."
] | 2016A&A...594A..68D | [
"On the estimation of stellar parameters with uncertainty prediction from Generative Artificial Neural Networks: application to Gaia RVS simulated spectra"
] | 17 | [
"Universidade da Coruña (UDC), Dept. de Tecnologías de la Información y las Comunicaciones, Elviña, 15071, A Coruña, Spain",
"Universidade da Coruña (UDC), Dept. de Tecnologías de la Información y las Comunicaciones, Elviña, 15071, A Coruña, Spain",
"Universidade da Coruña (UDC), Dept. de Ciencias de la Navegac... | [
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"10.1051/0004-6361/201527045",
"10.48550/arXiv.1607.05954"
] | 1607 | 1607.05954_arXiv.txt | } The first automatic systems for spectral classification were developed in the 80s and based on two paradigms: expert systems and pattern recognition. Knowledge-based systems were created by defining a set of rules/models that relate, for the case of astronomical objects, spectral indexes (absorption line equivalent ... | } ANNs are a great tool that offer nonlinear regression capabilities to any degree of complexity. Furthermore, they can provide accurate predictions when new data is presented to them, since they can generalize their solutions. However, in principle, they are not able to give a measure of uncertainty over their predic... | 16 | 7 | 1607.05954 | <BR /> Aims: We present an innovative artificial neural network (ANN) architecture, called Generative ANN (GANN), that computes the forward model, that is it learns the function that relates the unknown outputs (stellar atmospheric parameters, in this case) to the given inputs (spectra). Such a model can be integrated ... | false | [
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2409424 | [
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"Chiang, H. C.",
"Cliche, J. F.",
"Davé, R.",
"Dobbs, M.",
"Clarkson, C.",
"Ganga, K. M.",
"Gogo, T.",
"Gumba, A.",
"Gupta, N.",
"Hilton, M.",
"Johnstone, B.",
"Karastergiou, A.",
"Kunz, M.",
"Lokhorst, D.",
"Maa... | 2016SPIE.9906E..5XN | [
"HIRAX: a probe of dark energy and radio transients"
] | 211 | [
"Univ. of Toronto (Canada)",
"West Virginia Univ. (United States)",
"APC, Univ. Paris Diderot, CNRS (France)",
"Institute of Astronomy and Astrophysics (Taiwan)",
"National Institute for Theoretical Physics (South Africa)",
"McGill Univ. (Canada)",
"Univ. of the Western Cape (South Africa)",
"McGill U... | [
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"2016A&A...594A.... | [
"10.1117/12.2234286",
"10.48550/arXiv.1607.02059"
] | 1607 | 1607.02059_arXiv.txt | \label{sec:intro} % Measurements from Type Ia supernovae (SN1a)~\cite{SN1a}, Baryon Acoustic Oscillations (BAO)~\cite{2016MNRAS.457.1770C}, and the Cosmic Microwave Background (CMB)~\cite{2015arXiv150201589P} have shown that the energy density of the Universe is now dominated by Dark Energy, an unknown component caus... | 16 | 7 | 1607.02059 | The Hydrogen Intensity and Real-time Analysis eXperiment (HIRAX) is a new 400{800MHz radio interferometer under development for deployment in South Africa. HIRAX will comprise 1024 six meter parabolic dishes on a compact grid and will map most of the southern sky over the course of four years. HIRAX has two primary sci... | false | [
"new radio transient phenomena searches",
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"higher redshift",
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"fast radio bursts",
"Dark Energy",
"redshifts",
"current BAO measurements",
"new opportunities",
"BAO",
"galaxy surveys",
"many wavelengths",
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"long... | 12.290406 | 3.292618 | 161 | |
1208119 | [
"Roy, Arpita",
"Chakraborty, Abhijit",
"Mahadevan, Suvrath",
"Chaturvedi, Priyanka",
"Prasad, Neelam J. S. S. V.",
"Shah, Vishal",
"Pathan, F. M.",
"Anandarao, B. G."
] | 2016SPIE.9908E..6RR | [
"Precision velocimetry planet hunting with PARAS: current performance and lessons to inform future extreme precision radial velocity instruments"
] | 4 | [
"The Pennsylvania State Univ. (United States)",
"Physical Research Lab. (India)",
"The Pennsylvania State Univ. (United States)",
"Physical Research Lab. (India)",
"Physical Research Lab. (India)",
"Physical Research Lab. (India)",
"Physical Research Lab. (India)",
"Physical Research Lab. (India)"
] | [
"2018AJ....156....3C",
"2019PASP..131l4503C",
"2020AJ....159..161R",
"2021A&A...649A..17D"
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"astronomy",
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] | 8 | [
"Astrophysics - Instrumentation and Methods for Astrophysics",
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"2014SPIE.9147E.... | [
"10.1117/12.2232833",
"10.48550/arXiv.1607.06485"
] | 1607 | 1607.06485_arXiv.txt | \label{sec:intro} % As we await the bounty of sources expected from space-based missions like TESS and GAIA, it is imperative that we tool up for the efficient and widespread ground-based follow-up of exoplanet candidates that will be required in complement. While confirmation of the most promising, and likely Earth a... | 16 | 7 | 1607.06485 | The PRL Advanced Radial-velocity Abu-sky Search (PARAS) instrument is a fiber-fed stabilized high-resolution cross-dispersed echelle spectrograph, located on the 1.2 m telescope in Mt. Abu India. Designed for exoplanet detection, PARAS is capable of single-shot spectral coverage of 3800 - 9600 Å, and currently achievin... | false | [
"RV analysis pipeline",
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"RV",
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"precision velocimeters",
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"longer baselines",
"Mt. Abu India",
"telescopes",
"simultaneous ThAr calibration",
"M dwarfs",
"scientific surveys",
"pipeline prototypes",
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3941943 | [
"Hayes, L. A.",
"Gallagher, P. T.",
"Dennis, B. R.",
"Ireland, J.",
"Inglis, A. R.",
"Ryan, D. F."
] | 2016ApJ...827L..30H | [
"Quasi-periodic Pulsations during the Impulsive and Decay phases of an X-class Flare"
] | 44 | [
"School of Physics, Trinity College Dublin, Dublin 2, Ireland ; Solar Physics Laboratory, Heliophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA ; ADNET Systems, Inc., USA",
"School of Physics, Trinity College Dublin, Dublin 2, Ireland",
"Solar Physics Laboratory, Heliophysics... | [
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"astronomy"
] | 12 | [
"Sun: flares",
"Sun: oscillations",
"Sun: X-rays",
"gamma rays",
"Astrophysics - Solar and Stellar Astrophysics"
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"10.3847/2041-8205/827/2/L30",
"10.48550/arXiv.1607.06957"
] | 1607 | 1607.06957_arXiv.txt | \label{sec:intro} During a solar flare, the X-ray flux from the Sun can increase by several orders of magnitude and be accompanied by pulsations in the flare emission. These pulsations, known as quasi-periodic pulsations (QPP), are variations of flux as a function of time. Their nature has been examined in many previo... | We have detected and analysed pulsations observed at multiple wavelengths during the X1.0 flare of 2013 October 28. Throughout the impulsive phase of the flare, highly correlated common features are observed at HXR, SXR, and microwave wavelengths with minimal time delay between peaks. Wavelet analysis of this impulsive... | 16 | 7 | 1607.06957 | Quasi-periodic pulsations (QPPs) are often observed in X-ray emission from solar flares. To date, it is unclear what their physical origins are. Here, we present a multi-instrument investigation of the nature of QPP during the impulsive and decay phases of the X1.0 flare of 2013 October 28. We focus on the character of... | false | [
"X-ray emission",
"solar flares",
"thermal pulsations",
"the vertical kink mode",
"the non-thermal emission",
"the non-thermal emissions",
"the co-existing multi-wavelength QPPs",
"hard X-ray and microwave emission",
"the thermal and non-thermal emissions",
"the fast sausage mode",
"SXR pulsatio... | 13.558462 | 15.665303 | 2 |
12511058 | [
"Jia, Lian-Bao"
] | 2016PhRvD..94i5028J | [
"Study of WIMP annihilations into a pair of on-shell scalar mediators"
] | 7 | [
"School of Science, Southwest University of Science and Technology, Mianyang 621010, People's Republic of China"
] | [
"2016JHEP...12..033K",
"2017JCAP...02..037B",
"2017JHEP...06..077L",
"2017PhRvD..96e5009J",
"2018JHEP...02..121A",
"2020EPJC...80..143J",
"2022ChPhC..46h3111J"
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"astronomy",
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] | 5 | [
"High Energy Physics - Phenomenology",
"Astrophysics - Cosmology and Nongalactic Astrophysics"
] | [
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"2009JCAP...08..017I",
"2009JCAP...12..007C",
"2009PhLB..671..... | [
"10.1103/PhysRevD.94.095028",
"10.48550/arXiv.1607.00737"
] | 1607 | 1607.00737.txt | The weakly interacting massive particle (WIMP) type dark matter (DM) attracts much attention in DM direct detections, and the cold DM relic density can be derived from thermally freeze-out WIMPs. Today, the compatible confident events are still absent in DM direct detection experiments, and the recent search results of... | The scalar and vectorial WIMPs have been studied in this article, with a new scalar $\phi$ as the mediator and the mass of $\phi$ being slightly below the WIMP mass. The dominant annihilation products of WIMPs are on-shell $\phi \phi$ pairs with $\phi$ mainly decaying into $\tau \bar \tau$, and the WIMP annihilations a... | 16 | 7 | 1607.00737 | In this article, we focus on new scalar ϕ mediated scalar/vectorial weakly interacting massive particles (WIMPs) with ϕ 's mass slightly below the WIMP mass. To explain the Galactic center 1-3 GeV gamma-ray excess, here we consider the case that a WIMP pair predominantly annihilates into an on-shell ϕ ϕ pair with ϕ mai... | false | [
"e",
"ϕ",
"DM direct detection",
"new scalar ϕ",
"direct detections",
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"scalar DM",
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"the upgraded DM direct detection experiment",
"the future high-luminosity e",
"the ϕ -SM particles",
"ϕ s mass",
"the next few years",
"WIMPs",
"today",
"t... | 8.206857 | -1.69794 | 54 |
12471532 | [
"Giersz, M.",
"Leigh, N.",
"Hypki, A.",
"Askar, A.",
"Lützgendorf, N."
] | 2016MmSAI..87..555G | [
"Formation mechanisms of IMBH in globular clusters"
] | 7 | [
"Nicolaus Copernicus Astronomical Centre, Polish Academy of Sciences, ul. Bartycka 18, 00-716 Warsaw, Poland,",
"Department of Astrophysics, American Museum of Natural History, Central Park West and 79th Street, New York, NY 10024",
"Leiden Observatory, Leiden University, PO Box 9513, NL-2300 RA Leiden, the Net... | [
"2017JCAP...04..036D",
"2017PhRvD..96b2001A",
"2018PhyU...61..115D",
"2019MNRAS.482.3669G",
"2020arXiv200210332D",
"2022MNRAS.511.4060K",
"2024PTEP.2024e3E01B"
] | [
"astronomy"
] | 4 | [
"Stars: black holes",
"star clusters: general",
"Methods: numerical",
"Astrophysics - Astrophysics of Galaxies"
] | [
"1971Ap&SS..14..151H",
"1986AcA....36...19S",
"1995MNRAS.277.1507K",
"1996AJ....112.1487H",
"2001ApJ...550..372F",
"2001ApJ...551L..27M",
"2001MNRAS.322..231K",
"2002ApJ...572..407B",
"2004Natur.428..724P",
"2005MNRAS.360..974H",
"2009ApJ...706..404G",
"2013MNRAS.431.2184G",
"2013MNRAS.433.1... | [
"10.48550/arXiv.1607.08384"
] | 1607 | 1607.08384_arXiv.txt | Intermediate mass black holes (IMBH) are thought to be a missing link between stellar-mass black holes (BH) and supermassive BHs (SMBH). There are many theoretical arguments in favor of the formation of IMBHs in the centers of globular clusters (GCs) \citep[e.g.][and reference therein]{Lutzgendorfetal2013}. Observation... | The MOCCA code shows clearly its ability to model in a very efficient way a large number (thousands) of GC models. The observation of any events connected with accretion of matter on IMBHs or connected with mergers due to gravitational radiation is very improbable. We will have to have a lot of luck to see one of them.... | 16 | 7 | 1607.08384 | We very briefly discuss proposed in the literature possible scenarios for intermediate mass black holes formation in globular clusters. We also discuss the results of the MOCCA simulations of about 2000 models (BigSurvey) regarding the distribution of events connected with electromagnetic and gravitational radiations, ... | false | [
"IMBH",
"gravitational radiation",
"mergers",
"globular clusters",
"intermediate mass black holes formation",
"collisions",
"electromagnetic and gravitational radiations",
"events",
"possible scenarios",
"BigSurvey",
"namely: mass transfer",
"the MOCCA simulations",
"these events",
"the di... | 8.727796 | 6.69257 | -1 |
12585774 | [
"Fauvarque, Olivier",
"Neichel, Benoit",
"Fusco, Thierry",
"Sauvage, Jean-Francois",
"Girault, Orion"
] | 2017JATIS...3a9001F | [
"General formalism for Fourier-based wave front sensing: application to the pyramid wave front sensors"
] | 11 | [
"Aix-Marseille Université, CNRS, Laboratoire d'Astrophysique de Marseille, UMR 7326, Marseille, France",
"Aix-Marseille Université, CNRS, Laboratoire d'Astrophysique de Marseille, UMR 7326, Marseille, France",
"ONERA-the French Aerospace Laboratory, Châtillon, France",
"ONERA-the French Aerospace Laboratory, ... | [
"2017arXiv170809044F",
"2018ApOpt..57.8790H",
"2018JOSAA..35..594F",
"2018MNRAS.481.2829H",
"2019JATIS...5c9001J",
"2019JOSAA..36.1241F",
"2020MNRAS.495.4380C",
"2022A&A...664A..71N",
"2022SPIE12185E..3DH",
"2022SPIE12185E..89L",
"2024A&A...683A.113H"
] | [
"astronomy"
] | 7 | [
"Astrophysics - Instrumentation and Methods for Astrophysics"
] | [
"1934MNRAS..94..377Z",
"1996JMOp...43..289R",
"1999A&A...350L..23R",
"2001A&A...369L...9E",
"2004OptCo.233...27V",
"2005ApJ...629..592G",
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"10.1117/1.JATIS.3.1.019001",
"10.48550/arXiv.1607.03269"
] | 1607 | 1607.03269_arXiv.txt | \label{sec:intro} By placing amplitude or phase masks in a focal plane, it is possible to filter the light from a pupil plane to another. Those masks are able, in particular, to transform incoming phase fluctuations into intensity variations on a detector. Such optical designs (see figure \ref{ff_bench}) are thus part... | The numerous parameters of the sensors of the Pyramid class thus allows to consider the \textbf{optimization} of the element \emph{sensor} in an Adaptive Optics loop. The comparison of the different WFSs of this class, following unified performance criteria, shows that: -- The \textbf {number of faces} is essentially ... | 16 | 7 | 1607.03269 | We compare a set of wave front sensors (WFS) based on Fourier filtering technique. In particular, this study explores the "class of pyramidal WFS" defined as the 4-faces pyramid WFS, all its recent variations, and also some WFSs as the 3-faces pyramid WFS. First, we describe such a sensors class due to the optical para... | false | [
"linear range",
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2523945 | [
"Sakari, Charli M.",
"Shetrone, Matthew D.",
"Schiavon, Ricardo P.",
"Bizyaev, Dmitry",
"Allende Prieto, Carlos",
"Beers, Timothy C.",
"Caldwell, Nelson",
"García-Hernández, D. A.",
"Lucatello, Sara",
"Majewski, Steven",
"O'Connell, Robert W.",
"Pan, Kaike",
"Strader, Jay"
] | 2016ApJ...829..116S | [
"Infrared High-resolution Integrated Light Spectral Analyses of M31 Globular Clusters from APOGEE"
] | 34 | [
"Department of Astronomy, University of Washington, Seattle WA 98195-1580, USA",
"McDonald Observatory, University of Texas at Austin, HC75 Box 1337-MCD, Fort Davis, TX 79734, USA",
"Gemini Observatory, 670 N. A'Ohoku Place, Hilo, HI 96720, USA ; Astrophysics Research Institute, Liverpool John Moores University... | [
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] | 8 | [
"galaxies: abundances",
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"10.3847/0004-637X/829/2/116",
"10.48550/arXiv.1607.06811"
] | 1607 | 1607.06811_arXiv.txt | \label{sec:Intro} Integrated Light (IL) spectroscopy of globular clusters (GCs) provides valuable clues about the assembly histories of distant galaxies and their GC systems. An IL spectrum comes from an entire stellar population---integrated chemical abundances therefore represent flux-weighted averages from the indi... | \label{sec:Conclusion} This paper has presented an $H$-band integrated light spectroscopic analysis of 25 bright GCs that are associated with M31. The target GCs span a wide range in metallicity (from $[\rm{Fe/H}] = -1.8$ to $-0.2$), a moderate range in total mass (from $\log \rm{mass} \sim 5.4$ to $\sim 6.5$), and a s... | 16 | 7 | 1607.06811 | Chemical abundances are presented for 25 M31 globular clusters (GCs), based on moderately high resolution (R = 22,500) H-band integrated light (IL) spectra from the Apache Point Observatory Galactic Evolution Experiment (APOGEE). Infrared (IR) spectra offer lines from new elements, lines of different strengths, and lin... | false | [
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4188624 | [
"Raouafi, N. E.",
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"Sterling, A. C.",
"Savcheva, A.",
"Shimojo, M.",
"Moreno-Insertis, F.",
"DeVore, C. R.",
"Archontis, V.",
"Török, T.",
"Mason, H.",
"Curdt, W.",
"Meyer, K.",
"Dalmasse, K.",
"Matsui, Y."
] | 2016SSRv..201....1R | [
"Solar Coronal Jets: Observations, Theory, and Modeling"
] | 261 | [
"The Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA",
"Department of Physics, University of Ioannina, Ioannina, Greece",
"LESIA, Observatoire de Paris, Meudon, France",
"College of Science, George Mason University, Fairfax, VA, USA; NASA/Goddard Space Flight Center, Greenbelt, MD, USA",
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"10.1007/s11214-016-0260-5",
"10.48550/arXiv.1607.02108"
] | 1607 | 1607.02108.txt | The wide variety of transient phenomena in the solar corona first became apparent in the 1970s with the discovery of coronal transients in ground-based, green-line observations \citep{1973SoPh...31..449D}; discovery of macro-spicules in Skylab EUV observations \citep{1975ApJ...197L.133B,1976ApJ...203..528W}; and the di... | Imaging and spectroscopic observations over the last two decades have provided unprecedented insights into the formation and evolution of solar coronal transients, particularly coronal jets. Recent space missions, such as {\it{Hinode}}, {\it{STEREO}}, {\it{SDO}}, {\it{IRIS}} and are instrumental in advancing our unders... | 16 | 7 | 1607.02108 | Coronal jets represent important manifestations of ubiquitous solar transients, which may be the source of significant mass and energy input to the upper solar atmosphere and the solar wind. While the energy involved in a jet-like event is smaller than that of "nominal" solar flares and coronal mass ejections (CMEs), j... | false | [
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"the solar activity",
"important clues",
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12408793 | [
"Fang, Ke",
"Olinto, Angela V."
] | 2016ApJ...828...37F | [
"High-energy Neutrinos from Sources in Clusters of Galaxies"
] | 31 | [
"University of Maryland, Department of Astronomy, 1105 PSC, College Park, MD 20742, USA ; Joint Space-Science Institute, College Park, MD 20742, USA",
"Department of Astronomy & Astrophysics, Kavli Institute for Cosmological Physics, The University of Chicago, Chicago, Illinois 60637, USA"
] | [
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"2020SCPMA..6319501A",
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"astronomy"
] | 2 | [
"astroparticle physics",
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] | [
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"2003ApJ...584..... | [
"10.3847/0004-637X/828/1/37",
"10.48550/arXiv.1607.00380"
] | 1607 | 1607.00380_arXiv.txt | \label{sec:introduction} The IceCube Observatory has observed the first high-energy astrophysical neutrinos \citep{Aartsen:2013jdh, Aartsen:2013bka, Aartsen:2013uuv}. The all-flavor diffuse neutrino flux is reported to be $\Phi_\nu=2.06\times10^{-18}\,(E_\nu/10^5\,\rm GeV)^{-2.46}\,\rm GeV^{-1}cm^{-2}sr^{-1}s^{-1}$... | \label{sec:discussion} Unlike other astrophysical sources, galaxy clusters offer a unique environment for TeV-PeV neutrino production through efficient acceleration and confinement of high-energy cosmic rays. By propagating particles in three-dimensional turbulent magnetic fields and recording their interactions with ... | 16 | 7 | 1607.00380 | High-energy cosmic rays can be accelerated in clusters of galaxies, by mega-parsec scale shocks induced by the accretion of gas during the formation of large-scale structures, or by powerful sources harbored in clusters. Once accelerated, the highest energy particles leave the cluster via almost rectilinear trajectorie... | false | [
"galaxy clusters",
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"high-energy cosmic rays",
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12464610 | [
"Cai, Yi-Fu",
"Gong, Jinn-Ouk",
"Wang, Dong-Gang",
"Wang, Ziwei"
] | 2016JCAP...10..017C | [
"Features from the non-attractor beginning of inflation"
] | 45 | [
"CAS Key Laboratory for Researches in Galaxies and Cosmology, University of Science and Technology of China, Chinese Academy of Sciences, Hefei, Anhui 230026, China",
"Asia Pacific Center for Theoretical Physics, Pohang 37673, Korea ; Department of Physics, Postech, Pohang 37673, Korea;",
"CAS Key Laboratory fo... | [
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"General Relativity and Quantum Cosmology",
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] | [
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"10.1088/1475-7516/2016/10/017",
"10.48550/arXiv.1607.07872"
] | 1607 | 1607.07872_arXiv.txt | \label{intro} Inflationary scenario is the most popular paradigm for the very early universe which successfully resolves the puzzles of standard big bang cosmology~\cite{Starobinsky:1980te,Fang:1980wi,Guth:1980zm,Sato:1980yn,Linde:1981mu, Albrecht:1982wi}. Conventionally, inflation is driven by the potential of ... | \label{sec:discussions} There are two interesting directions regarding the non-attractor phase during inflation. First, non-attractor inflation models have aroused a lot theoretical concerns, since in this case the curvature perturbation grows after horizon-exit and the non-Gaussianity consistency relation is vio... | 16 | 7 | 1607.07872 | We study the effects of the non-attractor initial conditions for the canonical single-field inflation. The non-attractor stage can last only several e-folding numbers, and should be followed by hilltop inflation. This two-stage evolution leads to large scale suppression in the primordial power spectrum, which is favore... | false | [
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"only several e-folding numbers",
"the primordial power spectrum",
"the canonical s... | 11.128139 | -0.739333 | 89 |
1093459 | [
"Hodgson, J. A.",
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"Marscher, A. P.",
"Jorstad, S. G.",
"Rani, B.",
"Marti-Vidal, I.",
"Bach, U.",
"Sanchez, S.",
"Bremer, M.",
"Lindqvist, M.",
"Uunila, M.",
"Kallunki, J.",
"Vicente, P.",
"Fuhrmann, L.",
"Angelakis, E.",
"Karamanavis, V.",
"Myserlis, I.",
"Nest... | 2017A&A...597A..80H | [
"Location of γ-ray emission and magnetic field strengths in OJ 287"
] | 71 | [
"Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121, Bonn, Germany; Korea Astronomy and Space Institute, 776 Daedeokdae-ro, Yuseong-gu, 34055, Daejeon, Korea",
"Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121, Bonn, Germany",
"Institute for Astrophysical Research, Boston Universit... | [
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"astronomy"
] | 13 | [
"BL Lacertae objects: individual: OJ 287",
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"magnetic fields",
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"techniques: interferometric",
"galaxies: jets",
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"10.1051/0004-6361/201526727",
"10.48550/arXiv.1607.00725"
] | 1607 | 1607.00725_arXiv.txt | Radio loud active galactic nuclei (AGN) feature highly energised relativistic jets which are likely produced by the conversion of gravitational energy around a central super-massive black hole (SMBH) \citep{BZ77,BP82}. Blazars are a subclass of AGN with the jet direction being nearly parallel to our line of sight \cite... | We have used multi-frequency VLBI data at 2\,cm, 7\,mm and 3\,mm, total intensity radio data at 2\,cm, 7\,mm, 3\,mm, 1\,mm, 0.85\,mm and $\gamma$-ray data from the \emph{Fermi}/LAT space telescope to perform a detailed kinematic and spectral analysis of the highly variable BL Lac OJ\,287. We have used the 2\,cm MOJAVE,... | 16 | 7 | 1607.00725 | Context. The γ-ray BL Lac object OJ 287 is known to exhibit inner-parsec "jet-wobbling", high degrees of variability at all wavelengths and quasi-stationary features, including an apparent (≈100°) position-angle change in projection on the sky plane. <BR /> Aims: Sub-50 micro-arcsecond resolution 86 GHz observations wi... | false | [
"quasi-stationary features",
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"spectral changes",
"lower frequencies",
"ongoing multi-frequency VLBI blazar",
"the downstream quasi-stationary feature",
"Magnetic field estimates",
"a downstream stationary feature",
"projection",
"multiple locations",
"radio flares",
"radi... | 16.592764 | 5.50577 | -1 |
12578451 | [
"Tarnopolski, Mariusz"
] | 2017CeMDA.127..121T | [
"Influence of a second satellite on the rotational dynamics of an oblate moon"
] | 6 | [
"Astronomical Observatory of the Jagiellonian University, Kraków, Poland"
] | [
"2017A&A...606A..43T",
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"2019CeMDA.131...33G",
"2020ApJ...899..103M",
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] | 4 | [
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"Rotation",
"Bifurcation diagrams",
"Astrophysics - Earth and Planetary Astrophysics",
"Nonlinear Sciences - Chaotic Dynamics",
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"1982Sci...215..504S",
"1983PhyD....9..... | [
"10.1007/s10569-016-9719-7",
"10.48550/arXiv.1607.07333"
] | 1607 | 1607.07333_arXiv.txt | Saturn's seventh moon, Hyperion (also known as Saturn VII), was discovered in the XIX century by \citet{bond} and \citet{lassel}, but only due to Voyager~2 \citep{smith} and Cassini \citep{thomas10} missions it became apparent that it is the biggest known highly aspherical celestial body in the Solar System, with a hig... | \label{disc} The aim of this paper was to investigate how does the gravitational interaction with a second satellite influence the rotational dynamics of an oblate moon. A simplified model was designed, resulting in the equation on motion given in Eq.~(\ref{eq21}), being basically a perturbation of the well known Eq.~... | 16 | 7 | 1607.07333 | The gravitational influence of a second satellite on the rotation of an oblate moon is numerically examined. A simplified model, assuming the axis of rotation perpendicular to the (Keplerian) orbit plane, is derived. The differences between the two models, i.e. in the absence and presence of the second satellite, are i... | false | [
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"The gravitational influence",
"the gravitational influence",
"a second satellite",
"the second satellite",
"the phase space",
"Keplerian",
"the oblate bo... | 8.014376 | 15.362032 | -1 |
12472585 | [
"Belloni, Diogo",
"Giersz, Mirek",
"Askar, Abbas",
"Leigh, Nathan",
"Hypki, Arkadiusz"
] | 2016MNRAS.462.2950B | [
"MOCCA-SURVEY database I. Accreting white dwarf binary systems in globular clusters - I. Cataclysmic variables - present-day population"
] | 33 | [
"Nicolaus Copernicus Astronomical Centre, Polish Academy of Sciences, ul. Bartycka 18, PL-00-716 Warsaw, Poland; CAPES Foundation, Ministry of Education of Brazil, DF 70040-020 Brasilia, Brazil",
"Nicolaus Copernicus Astronomical Centre, Polish Academy of Sciences, ul. Bartycka 18, PL-00-716 Warsaw, Poland",
"N... | [
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"2019A&A...631A.118G",
"2019MNRAS.483..315B",
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] | 7 | [
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"10.1093/mnras/stw1841",
"10.48550/arXiv.1607.07619"
] | 1607 | 1607.07619_arXiv.txt | \label{introduction} The study of star clusters plays an important role in our understanding of the Universe since these systems are natural laboratories for testing theories of stellar dynamics and evolution. Particularly, globular clusters (GCs) are one of the most important objects for studying the formation and th... | \label{conclusion} So far, we have exposed in this paper part of the first results obtained from the analysis of six models simulated by MOCCA using the CATUABA code as well as description of the code itself. The PDP of CVs in GC are in the last stage of their evolution! This, maybe, is the leading characteristic of ... | 16 | 7 | 1607.07619 | In this paper, which is the first in a series of papers associated with cataclysmic variables and related objects, we introduce the CATUABA code, a numerical machinery written for analysis of the MOCCA simulations, and show some first results by investigating the present-day population of cataclysmic variables in globu... | false | [
"cataclysmic variables",
"observed cataclysmic variables",
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"observational selection effects",
"binary stellar evolution",
"no single cataclysmic variable",
"outbursts",
"strong dynamical interactions",
"place",
"Kroupa initial distributions",
"related objects",
"quiescence... | 5.466553 | 10.010388 | 24 |
1622440 | [
"Oman, Kyle A.",
"Hudson, Michael J."
] | 2016MNRAS.463.3083O | [
"Satellite quenching time-scales in clusters from projected phase space measurements matched to simulated orbits"
] | 89 | [
"Department of Physics and Astronomy, University of Victoria, Victoria, BC V8P 5C2, Canada; Department of Physics and Astronomy, University of Waterloo, Waterloo, ON N2L 3G1, Canada",
"Department of Physics and Astronomy, University of Waterloo, Waterloo, ON N2L 3G1, Canada; Perimeter Institute for Theoretical Ph... | [
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"2018A&A...614A..57F",
"2018ApJ...857...71B",
"2018ApJ...862..... | [
"astronomy"
] | 13 | [
"galaxies: clusters: general",
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] | 1607 | 1607.07934_arXiv.txt | A detailed understanding of the mechanisms that quench star formation in galaxies remains elusive. It now seems clear that quenching is strongly correlated with an `internal' parameter that is closely related to galaxy mass: stellar mass \citep{2003MNRAS.341...33K, 2004ApJ...600..681B}, velocity dispersion \citep{SmiLu... | \label{sec-conclusions} In the results of fitting our model, shown in Fig.~\ref{mstar_trends}, we note the expected trend in $f_{\rm passive,out}$, with higher stellar mass galaxies outside the clusters that are more affected by `internal quenching' having higher $f_{\rm passive,out}$. Interestingly, in all cases we r... | 16 | 7 | 1607.07934 | We measure the star formation quenching efficiency and time-scale in cluster environments. Our method uses N-body simulations to estimate the probability distribution of possible orbits for a sample of observed Sloan Digital Sky Survey galaxies in and around clusters based on their position and velocity offsets from th... | false | [
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12473122 | [
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] | 2016MNRAS.462.2542A | [
"Using baseline-dependent window functions for data compression and field-of-interest shaping in radio interferometry"
] | 10 | [
"Department of Physics and Electronics, Rhodes University, PO Box 94, Grahamstown 6140, South Africa",
"Department of Physics and Electronics, Rhodes University, PO Box 94, Grahamstown 6140, South Africa; SKA South Africa, 3rd Floor, The Park, Park Road, Pinelands 7405, South Africa",
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] | 1607 | 1607.04106_arXiv.txt | \newcommand{\VV}{\mathcal{V}} \newcommand{\PP}{\mathcal{P}} \newcommand{\VVM}{\textcolor{black}{\widehat{\mathcal{V}}}}% \newcommand{\WW}{\mathcal{W}} \newcommand{\II}{\mathcal{I}} \newcommand{\IID}{\mathcal{I}^\mathrm{D}} \newcommand{\IIDI}{\mathcal{I}^\mathrm{DI}} \newcommand{\EE}{\mathcal{E}} \newcommand{\FF}{\mathc... | The goal of this work was to demonstrate the application of baseline-dependent window functions to radio interferometry. We have demonstrated that BDWFs offer a number of interesting advantages over conventional averaging. The first of these is data compression -- i.e. visibilities can be sampled at a lower rate, while... | 16 | 7 | 1607.04106 | In radio interferometry, observed visibilities are intrinsically sampled at some interval in time and frequency. Modern interferometers are capable of producing data at very high time and frequency resolution; practical limits on storage and computation costs require that some form of data compression be imposed. The t... | false | [
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... | 11.106184 | 3.779708 | 171 |
12409587 | [
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"Shi, Jianrong",
"Luo, Ali",
"Zhang, Haotong",
"Dong, Subo",
"Zhang, Ruyuan",
"Zhang, Yong",
"Hou, Yonghui",
"Wang, Yuefei",
"Cao, Zihuang",
"Du, Bing"
] | 2016ApJS..225...28R | [
"LAMOST Observations in the Kepler Field. Analysis of the Stellar Parameters Measured with LASP Based on Low-resolution Spectra"
] | 41 | [
"Department of Astronomy, Beijing Normal University, No. 19 Xinjiekouwai Street, Haidian District, Beijing 100875, China",
"Department of Astronomy, Beijing Normal University, No. 19 Xinjiekouwai Street, Haidian District, Beijing 100875, China",
"Royal observatory of Belgium, Ringlaan 3, B-1180 Brussel, Belgium... | [
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"10.48550/arXiv.1607.01453"
] | 1607 | 1607.01453_arXiv.txt | The main scientific objective of the NASA (National Aeronautics and Space Administration) space mission \kepler\ are to detect the Earth-size and even larger planets in the habitable zone \citep{Kas1993,Bor2007} of solar-like stars by using the method of photometric transits \citep{Bor2009}, and to determine the proper... | 16 | 7 | 1607.01453 | All 14 subfields of the Kepler field were observed at least once with the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (lamost, Xinglong Observatory, China) during the 2012-2014 observation seasons. There are 88,628 reduced spectra with a signal-to-noise ratio in the g band (S/N<SUB> g </SUB>) ≥ 6 after th... | false | [
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12464875 | [
"Arbañil, José D. V.",
"Malheiro, M."
] | 2016JCAP...11..012A | [
"Radial stability of anisotropic strange quark stars"
] | 80 | [
"ITA—Instituto Tecnológico de Aeronáutica—Departamento de Física, 12228-900, São José dos Campos, São Paulo, Brazil ; UPN—Universidad Privada del Norte—Departamento de Ciencias, Av. Alfredo Mendiola 6062 Urb. Los Olivos, Lima, Lima, Perú;",
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"10.1088/1475-7516/2016/11/012",
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] | 1607 | 1607.03984_arXiv.txt | In astrophysics, the study of compact stars is vitally important because it provides an excellent laboratory for the study of highly dense matter on extreme conditions. Theoretically, it is largely considered that these objects are composed of a perfect fluid. However, strong theoretical evidences suggest that in a hig... | The radial stability of anisotropic strange quark stars is studied in the present article. This is possible through the numerical solution of the hydrostatic equilibrium equation and the radial pulsation equation, which are modified from their original form to the inclusion of anisotropy. We consider that the matter co... | 16 | 7 | 1607.03984 | The influence of the anisotropy in the equilibrium and stability of strange stars is investigated through the numerical solution of the hydrostatic equilibrium equation and the radial oscillation equation, both modified from their original version to include this effect. The strange matter inside the quark stars is des... | false | [
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12408858 | [
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"Shimakawa, Rhythm",
"Koyama, Yusei",
"Tadaki, Ken-ichi",
"Suzuki, Tomoko L.",
"Yamamoto, Moegi"
] | 2016ApJ...826L..28H | [
"Enhanced Star Formation of Less Massive Galaxies in a Protocluster at z = 2.5"
] | 29 | [
"Optical and Infrared Astronomy Division, National Astronomical Observatory, Mitaka, Tokyo 181-8588, Japan",
"Optical and Infrared Astronomy Division, National Astronomical Observatory, Mitaka, Tokyo 181-8588, Japan; Department of Astronomical Science, SOKENDAI (The Graduate University for Advanced Studies), Mita... | [
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"astronomy"
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"10.3847/2041-8205/826/2/L28",
"10.48550/arXiv.1607.04040"
] | 1607 | 1607.04040_arXiv.txt | Since the last decade, the question of a positive correlation between SFR and stellar mass in star-forming galaxies (SFGs), which is called the main sequence (MS) of SFGs, has been one among hot topics in the field of galaxy evolution \citep[e.g.,][]{Noeske2007,Daddi2007,Elbaz2007}. The tight correlation provides us wi... | \label{sec:discussion} Until now, there have been a number of previous studies that investigated the MS of SFGs at $z\ga2$ \citep[e.g.,][]{Dunne2009,Karim2011,Reddy2012}. Figure \ref{fig:MS} also compares the MSs derived from the previous studies. Our HAEs with stellar masses of $\ga10^{10}$ \Msun\ seem to be located r... | 16 | 7 | 1607.04040 | We investigate a correlation between star formation rate (SFR) and stellar mass for Hα emission-line galaxies (HAEs) in one of the richest protoclusters ever known at z ∼ 2.5, the USS 1558-003 protocluster. This study is based on a 9.7 hr narrowband imaging data with MOIRCS on the Subaru telescope. We are able to const... | false | [
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12436863 | [
"Berdyugina, S. V."
] | 2016arXiv160706874B | [
"Polarized Scattering and Biosignatures in Exoplanetary Atmospheres"
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"-"
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"2017NatSR...714141A",
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"10.48550/arXiv.1607.06874"
] | 1607 | 1607.06874_arXiv.txt | \label{sec:prt} Radiative processes in planetary atmospheres is a classical subject, simply for the reason that we live in one. Extensive theoretical studies were carried out during the second half of the twentieth century by such giants as Sobolev \cite{Sobolev1956} and Chandrasekhar \cite{Chandra1960} as well as the... | 16 | 7 | 1607.06874 | Polarized scattering in planetary atmospheres is computed in the context of exoplanets. The problem of polarized radiative transfer is solved for a general case of absorption and scattering, while Rayleigh and Mie polarized scattering are considered as most relevant examples. We show that (1) relative contributions of ... | false | [
"visible polarized spectra",
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... | 7.207616 | 14.876241 | -1 | |
12593828 | [
"Repp, A.",
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] | 2017MNRAS.464L..21R | [
"Precision prediction of the log power spectrum"
] | 15 | [
"Institute for Astronomy, 2680 Woodlawn Dr., Honolulu, Hawaii 96822, USA",
"Institute for Astronomy, 2680 Woodlawn Dr., Honolulu, Hawaii 96822, USA"
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] | 4 | [
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"10.1093/mnrasl/slw178",
"10.48550/arXiv.1607.01386"
] | 1607 | 1607.01386_arXiv.txt | \label{sec-intro} Three-dimensional galaxy surveys can potentially yield significant gains in our understanding of cosmological parameters. Realizing this potential, however, depends on our ability to extract the cosmological information inherent in translinear modes. The power spectrum $P(k)$ is the standard means of... | \label{sec:concl} Based on the Millennium Simulation, we have provided a prescription (Equations~\ref{eq:sigA} and \ref{eq:PA}) for calculating the log power spectrum $P_A(k)$. This prescription is accurate to a few percent when one includes a slope modulation parameter $\alpha$ (Equations~\ref{eq:slopemod}--\ref{eq:N... | 16 | 7 | 1607.01386 | At translinear scales, the log power spectrum captures significantly more cosmological information than the standard power spectrum. At high wavenumbers k, the Fisher information in the standard power spectrum P(k) fails to increase in proportion to k, in part due to correlations between large- and small-scale modes. A... | false | [
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12594710 | [
"Mohammed, Irshad",
"Seljak, Uroš",
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] | 2017MNRAS.466..780M | [
"Perturbative approach to covariance matrix of the matter power spectrum"
] | 56 | [
"Fermilab Center for Particle Astrophysics, Fermi National Accelerator Laboratory, Batavia, IL 60510-0500, USA",
"Physics, Astronomy Department, University of California, Berkeley, CA 94720, USA; Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA",
"Stanford Institute for Theoretical Physics and Dep... | [
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"10.1093/mnras/stw3196",
"10.48550/arXiv.1607.00043"
] | 1607 | 1607.00043_arXiv.txt | \label{sec:intro} The distribution of matter in the Universe contains a wealth of information about the energy content of the Universe, its properties, and evolution. Initial distribution is thought to be a Gaussian random field, but as a result of the gravitational instability the tiny fluctuations in the initial mat... | \label{sec:discussion} In this paper, we developed a perturbative model for the covariance matrix of the power spectrum, going up to 1-loop in PT, but without including all the 1-loop terms (see \cite{2015arXiv151207630B} for the full 1-loop calculation). In addition, we go beyond 1-loop by including the nonlinear da... | 16 | 7 | 1607.00043 | We evaluate the covariance matrix of the matter power spectrum using perturbation theory up to dominant terms at 1-loop order and compare it to numerical simulations. We decompose the covariance matrix into the disconnected (Gaussian) part, trispectrum from the modes outside the survey (supersample variance) and trispe... | false | [
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12472971 | [
"Banasiński, P.",
"Bednarek, W.",
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] | 2016MNRAS.463L..26B | [
"Orphan γ-ray flares from relativistic blobs encountering luminous stars"
] | 14 | [
"Department of Astrophysics, The University of Łódź, ul. Pomorska 149/153, PL-90-236 Łódź, Poland",
"Department of Astrophysics, The University of Łódź, ul. Pomorska 149/153, PL-90-236 Łódź, Poland",
"Department of Astrophysics, The University of Łódź, ul. Pomorska 149/153, PL-90-236 Łódź, Poland"
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] | 1607 | 1607.07725_arXiv.txt | It is widely accepted that the non-thermal radiation in blazars is produced within a relativistic jet directed towards the observer. However, the mechanism of energization of particles and their radiation is not fully understood. Recently, simple scenarios exploiting collisions of compact objects with the jet plasma re... | \label{sec5} We propose that blobs of relativistic plasma, moving in jets of AGNs, can encounter from time to time luminous stars which form a quasi-spherical halo around the central super-massive black hole. The transit time of a star through a conical jet can be estimated as $T_{\rm transit} = R_{\bot}/v_\star\appro... | 16 | 7 | 1607.07725 | We propose that γ-rays in blazars can be produced during encounters of relativistic blobs of plasma with radiation field produced by luminous stars within (or close to) the jet. The blob is expected to contain relativistic electrons which Comptonize stellar radiation to the GeV-TeV energies. Produced γ-rays can initiat... | false | [
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12594003 | [
"Storch, Natalia I.",
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] | 2017MNRAS.465.3927S | [
"Dynamics of stellar spin driven by planets undergoing Lidov-Kozai migration: paths to spin-orbit misalignment"
] | 25 | [
"TAPIR, Walter Burke Institute for Theoretical Physics, Mailcode 350-17, Caltech, Pasadena, CA 91125, USA; Cornell Center for Astrophysics and Planetary Science, Department of Astronomy, Cornell University, Ithaca, NY 14853, USA",
"Cornell Center for Astrophysics and Planetary Science, Department of Astronomy, Co... | [
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] | 1607 | 1607.03937_arXiv.txt | The discovery of the misalignment between the orbital axes of hot Jupiters (HJs; giant planets with orbital periods of $\sim 3$~days) and the spin axes of their host stars (e.g. Hebrard et al. 2008, 2010; Narita et al. 2009; Triaud et al. 2010; Winn et al. 2009; Albrecht et al. 2012; Winn \& Fabrycky 2015) continues to... | \subsection{Complications due to Spin Feedback on Orbit} As explained in Section \ref{SRFsec}, a major assumption in the analysis laid out in this paper, as well as in SL15, is the omission of the extra precession the planet's orbit experiences due to perturbation from the stellar quadrupole. This omission enables us... | 16 | 7 | 1607.03937 | Many exoplanetary systems containing hot Jupiters (HJs) exhibit significant misalignment between the spin axes of the host stars and the orbital angular momentum axes of the planets ('spin-orbit misalignment'). High-eccentricity migration involving Lidov-Kozai oscillations of the planet's orbit induced by a distant per... | false | [
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12518205 | [
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] | 2017A&C....20..120M | [
"JUDE: An Ultraviolet Imaging Telescope pipeline"
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"Indian Institute of Astrophysics, Bengaluru, India",
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"Indian Institute of Astrophysics, Bengaluru, India",
"M. P. Birla Institute of Fundamental Research, Bengaluru, India",
"Department of Physics, Christ University, Bengaluru, India",
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] | 1607 | 1607.01874_arXiv.txt | The Ultraviolet Imaging Telescope (UVIT) was first proposed as part of the multi-wavelength \astrosat mission in the late $20^{th}$ century \citep{Pati1998,Pati1999} and was launched on 28 September, 2015 into a low Earth orbit (650 km, $6^{\circ}$ inclination) by an ISRO (Indian Space Research Organization) PSLV (Pola... | We have designed a set of software routines that begin with Level~1 UVIT data from the ISSDC and produces images suitable for scientific purposes. We have tested the software on all our GT observations, and have produced Level~2 event lists and images for all observations through an automated process. A few observation... | 16 | 7 | 1607.01874 | The Ultraviolet Imaging Telescope (UVIT) was launched as part of the multi-wavelength Indian AstroSat mission on 28 September, 2015 into a low Earth orbit. A 6-month performance verification (PV) phase ended in March 2016, and the instrument is now in the general observing phase. UVIT operates in three channels: visibl... | false | [
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12473014 | [
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] | 1607 | 1607.06453_arXiv.txt | In astrophysical context, the process in which diffuse gas or matter is accumulated around a compact object under an influence of gravity is called accretion. The importance of accretion as the source of steady or unsteady emission of radiation was first widely recognized in explaining observations of binary systems, e... | In this paper, we presented extensive time dependent numerical simulations of two quadrant accretion flow around a black hole. In earlier studies, such as in MLC94 and GC10, similar type of simulations were carried out in one quadrant using SPH and TVD schemes respectively. In these earlier simulations, our goal was t... | 16 | 7 | 1607.06453 | We study time evolution of rotating, axisymmetric, two-dimensional inviscid accretion flows around black holes using a grid-based finite difference method. We do not use reflection symmetry on the equatorial plane in order to inspect if the disc along with the centrifugal barrier oscillated vertically. In the inviscid ... | false | [
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12406286 | [
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"Taking stock of superluminous supernovae and long gamma-ray burst host galaxy comparison using a complete sample of LGRBs"
] | 25 | [
"INAF-Osservatorio Astronomico di Trieste, via G. B. Tiepolo 11, 34131, Trieste, Italy",
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] | 1607 | 1607.01045_arXiv.txt | Distinctly more luminous than ordinary supernovae, the recently established class of superluminous supernovae \citep[SLSN;][]{Quimby2011} is associated with the deaths of very massive stars \citep[e.g.][]{GalYam2009} and is being recognized as a new class of cosmic beacons that pinpoints distant star-forming galaxies \... | We compared the properties of the host galaxies of SLSNe to those of LGRBs with the aim of looking for similarities and possible differences of the two populations, to try to understand the different results found in the literature on this topic and with the final goal to shed some light on the progenitors of these two... | 16 | 7 | 1607.01045 | Long gamma-ray bursts (LGRBs) and superluminous supernovae (SLSNe) are both explosive transients with very massive progenitor stars. Clues about the nature of the progenitors can be found by investigating environments in which such transients occur. While studies of LGRB host galaxies have a long history, dedicated obs... | false | [
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12408841 | [
"Amano, Takanobu"
] | 2016ApJ...831..100A | [
"A Second-order Divergence-constrained Multidimensional Numerical Scheme for Relativistic Two-fluid Electrodynamics"
] | 9 | [
"Department of Earth & Planetary Science, University of Tokyo, 113-0033, Japan"
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"10.3847/0004-637X/831/1/100",
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] | 1607 | 1607.08487_arXiv.txt | \label{intro} There is growing evidence that the magnetic field plays a crucial role in many astrophysical phenomena. In particular, it is now widely accepted that relativistic outflows from compact objects involve magnetic fields. Examples include pulsar winds, and jets from active galactic nuclei and gamma-ray burst... | \label{conclusion} In this paper, we have discussed the relativistic two-fluid electrodynamics (RTFED) equations, which are an extension of relativistic magnetohydrodynamics (RMHD). The advantage of the RTFED model is obviously its capability for a wider range of applications. In contrast to RMHD, there is no inherent... | 16 | 7 | 1607.08487 | A new multidimensional simulation code for relativistic two-fluid electrodynamics (RTFED) is described. The basic equations consist of the full set of Maxwell’s equations coupled with relativistic hydrodynamic equations for separate two charged fluids, representing the dynamics of either an electron-positron or an elec... | false | [
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12593957 | [
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"Wong, K. C.",
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"Fassnacht, C. D.",
"Treu, T.",
"Auger, M. W.",
"Hilbert, S.",
"Koopmans, L. V. E.",
"Meylan, G.",
"Rumbaugh, N.",
"Sonnenfeld, A.",
"Spiniello, C."... | 2017MNRAS.465.4914B | [
"H0LiCOW - V. New COSMOGRAIL time delays of HE 0435-1223: H<SUB>0</SUB> to 3.8 per cent precision from strong lensing in a flat ΛCDM model"
] | 406 | [
"Laboratory of Astrophysics, Institute of Physics, Ecole Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, CH-1290 Versoix, Switzerland",
"Laboratory of Astrophysics, Institute of Physics, Ecole Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, CH-1290 Versoix, Switzerland",
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] | 1607 | 1607.01790_arXiv.txt | \label{sec:intro} In the past decade, the Standard Cosmological Model, \LCDM, which assumes the existence of either a cosmological constant or a form of dark energy with equation of state $w = -1$, and large scale structure predominantly composed of Cold Dark Matter, has been firmly established given observations to d... | \label{sec:conclusion} Using multiple telescopes in the Southern and Northern hemispheres, we have monitored the quadruple imaged strong gravitational lens \hequad\ for 13 years with an average cadence of one observing epoch every 3.6 days. We analyse the imaging data using the MCS deconvolution algorithm \citep{Magai... | 16 | 7 | 1607.01790 | We present a new measurement of the Hubble Constant H<SUB>0</SUB> and other cosmological parameters based on the joint analysis of three multiply imaged quasar systems with measured gravitational time delays. First, we measure the time delay of HE 0435-1223 from 13-yr light curves obtained as part of the COSMOGRAIL pro... | false | [
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] | 2016AJ....152..146N | [
"Star-forming Activity in the H II Regions Associated with the IRAS 17160-3707 Complex"
] | 14 | [
"Indian Institute of Space Science and Technology, Thiruvananthapuram 695 547, India",
"Indian Institute of Space Science and Technology, Thiruvananthapuram 695 547, India",
"Indian Institute of Space Science and Technology, Thiruvananthapuram 695 547, India",
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"10.3847/0004-6256/152/5/146",
"10.48550/arXiv.1607.01267"
] | 1607 | 1607.01267_arXiv.txt | \hii~regions are the first reliable pointers announcing the formation of massive O and B stars embedded in their natal molecular clouds. The hypercompact (size $<0.01$~pc) and ultracompact (size $<0.1$~pc) \hii~region phases with large electron densities ($n_e\ge 10^4$~cm$^{-3}$) are indicative of the early evolutionar... | \par We examined the star formation activity in the \hii~region complex associated with IRAS~17160--3707 using a range of wavelengths spanning from 3.6~$\mu$m to 870~$\mu$m. Based on our analysis, we arrive at the following conclusions: \begin{itemize} \item[(a)] The radio continuum maps show the presence of twelve ... | 16 | 7 | 1607.01267 | We present a multiwavelength investigation of star formation activity toward the southern H II regions associated with IRAS 17160-3707, located at a distance of 6.2 kpc with a bolometric luminosity of 8.3 × 10<SUP>5</SUP> L <SUB>⊙</SUB>. The ionized gas distribution and dust clumps in the parental molecular cloud are e... | false | [
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12408731 | [
"Kreisch, C. D.",
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] | 2016ApJ...830...39K | [
"Merger Hydrodynamics of the Luminous Cluster RX J1347.5-1145"
] | 12 | [
"Max Planck Institute for Astrophysics, Karl-Schwarzschild-Strasse 1, D-85748 Garching bei München, Germany; Department of Physics, Washington University in St. Louis, One Brookings Drive, St. Louis, MO 63130, USA;",
"Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA",
"Har... | [
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] | 1607 | 1607.04674_arXiv.txt | \label{sec:introduction} The growth of structure across cosmic time provides an important probe of cosmology. The evolution of the galaxy cluster mass function with redshift places significant constraints on the dark energy equation of state, with the greatest sensitivity found at the high mass end \citep{mass_functio... | \label{sec:conclude} With~$2.5$~times the exposure of previous analyses, we are able to study the gas hydrodynamics of RXJ1347 and its merging subcluster in unprecedented detail. We briefly summarize our key results. \begin{itemize} \item{A series of four cold fronts west, southeast, east, and northeast located at~$5\... | 16 | 7 | 1607.04674 | We present an analysis of the complex gas hydrodynamics in the X-ray-luminous galaxy cluster RX J1347.5-1145 caught in the act of merging with a subcluster to its southeast using a combined 186 ks Chandra exposure, 2.5 times greater than previous analyses. The primary cluster hosts a sloshing cold front spiral traced b... | false | [
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12473116 | [
"Adams, Fred C.",
"Bloch, Anthony M."
] | 2016MNRAS.462.2527A | [
"The stability of tidal equilibrium for hierarchical star-planet-moon systems"
] | 10 | [
"Physics Department, University of Michigan, Ann Arbor, MI 48109, USA; Astronomy Department, University of Michigan, Ann Arbor, MI 48109, USA",
"Math Department, University of Michigan, Ann Arbor, MI 48109, USA"
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"2020MNRAS.499.4195T",
"2021AJ....162..154D",
"2022ApJ...929L...2T"
] | [
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] | 8 | [
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"10.1093/mnras/stw1883",
"10.48550/arXiv.1607.08170"
] | 1607 | 1607.08170_arXiv.txt | \label{sec:intro} A classic dynamical problem is to consider the tidal equilibrium states for self-gravitating systems that include both rotational and orbital motion \citep{darwin1,darwin2}. The conditions required for the existence of such equilibrium states has been determined previously for binary star systems \c... | \label{sec:conclude} This paper considers the issue of tidal equilibrium for hierarchical star-planet-moon systems, which are described by 16 variables that specify the energy and angular momentum of the stellar spin, planetary spin, planetary orbit, lunar orbit, and lunar spin. The optimization procedure is subject t... | 16 | 7 | 1607.08170 | Motivated by the current search for exomoons, this paper considers the stability of tidal equilibrium for hierarchical three-body systems containing a star, a planet, and a moon. In this treatment, the energy and angular momentum budgets include contributions from the planetary orbit, lunar orbit, stellar spin, planeta... | false | [
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12520904 | [
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"Self-consistent Modeling of Reionization in Cosmological Hydrodynamical Simulations"
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] | 1607 | 1607.04218_arXiv.txt | \label{sec:intro} In our current standard model of the universe, hydrogen and helium account for 99\% of the baryonic mass density \citep{Planck:2015}. After the recombination epoch, these elements remain neutral until ultraviolet radiation from star-forming galaxies and active galactic nuclei reionizes them. Therefo... | \label{sec:conc} In this paper we have presented results from optically thin cosmological hydrodynamical simulations using the Nyx code \citep{Almgren:2013,Lukic:2015}. As commonly done in multiple IGM and galaxy formation studies, the UV background is modeled as a uniform and isotropic field that evolves with redshi... | 16 | 7 | 1607.04218 | The ultraviolet background (UVB) emitted by quasars and galaxies governs the ionization and thermal state of the intergalactic medium (IGM), regulates the formation of high-redshift galaxies, and is thus a key quantity for modeling cosmic reionization. The vast majority of cosmological hydrodynamical simulations implem... | false | [
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12409116 | [
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] | 1607 | 1607.08036_arXiv.txt | } By a factor of more than $10^4$, \htwo\ is the most abundant molecule in the universe, found in diverse environments ranging from planet atmospheres to quasars hosts \citep{Hanel79, Hanel81, Walter03, Genzel14}. It was the first neutral molecule to form in the Universe and hence dominated the cooling of pristine gas... | \subsection{What are the typical molecular gas temperatures in galaxies?} UV pumping sets the level populations of upper level states, J $\geqslant$ 3, in particular at low column densities of \htwo. As a result, these states may result in rotational temperatures well in excess of their kinetic temperatures. For our pu... | 16 | 7 | 1607.08036 | Robust knowledge of molecular gas mass is critical for understanding star formation in galaxies. The {{{H}}}<SUB>2</SUB> molecule does not emit efficiently in the cold interstellar medium, hence the molecular gas content of galaxies is typically inferred using indirect tracers. At low metallicity and in other extreme e... | false | [
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] | 53 | [
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] | 1607 | 1607.05996_arXiv.txt | \label{sec:introduction} The CE phase is usually invoked to explain the formation of close binary systems with at least one compact star: the compact star is born as a core of a giant with a much larger radius than the separation of the observed binary. During the CE phase, angular momentum and energy is extracted fro... | \label{sec:discussion} The first MHD simulations of the CE phase show that magnetic fields are strongly amplified in the direct vicinity of the companion star on dynamical timescales during the spiral-in. The temporal and spatial scales are compatible with the MRI operating in the accretion flow around the companion. ... | 16 | 7 | 1607.05996 | During the common envelope (CE) phase, a giant star in a binary system overflows its Roche lobe and unstable mass transfer leads to a spiral-in of the companion, resulting in a close binary system or in a merger of the stellar cores. Dynamo processes during the CE phase have been proposed as a mechanism to generate mag... | false | [
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1073937 | [
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3330704 | [
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] | 1607 | 1607.02787_arXiv.txt | % Understanding the gas cycle in galaxies -- how galaxies acquire, process, and expel their gas -- is the central goal of most studies of galaxy evolution. Our current understanding is that this cycle is a balance between the accretion of gas onto the galaxy, the efficiency of turning the accreted and ``recycled'' gas ... | \label{discussion} % Further discussion and analysis of the data presented here will be given in future papers in this series (e.g., Paper II; Butcher et al., in prep.; Healy et al., in prep.). Our goal was to observe a total of 3000 galaxies in the local Universe, distributed as uniformly as possible over the full ra... | 16 | 7 | 1607.02787 | To investigate galaxy properties as a function of their total stellar mass, we obtained 21 cm H I line observations at the 100-m class Nançay Radio Telescope of 2839 galaxies from the Sloan Digital Sky Survey (SDSS) in the Local Volume (900 < cz < 12 000 km s<SUP>-1</SUP>), dubbed the Nançay Interstellar Baryons ... | false | [
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"High-velocity extended molecular outflow in the star-formation dominated luminous infrared galaxy ESO 320-G030"
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"Centro de Astrobiología (CSIC/INTA), Ctra de Torrejón a Ajalvir, km 4, 28850, Torrejón de Ardoz, Madrid, Spain; ASTRO-UAM, UAM, Unidad Asociada CSIC, 28049, Madrid, Spain; Department of Physics, University of Oxford, Keble Road, Oxford, OX1 3RH, UK",
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] | 1607 | 1607.03674_arXiv.txt | \label{s:intro} Theoretical models predict that massive gas outflows, driven by starbursts or active galactic nuclei (AGN), are fundamental actors in shaping the observed properties of galaxies (e.g., galaxy mass function, mass-metallicity relation). This is because massive outflows can regulate both the accretion rat... | \label{s:conclusions} We present high spatial resolution ($\sim$60\,pc) ALMA CO(2--1) observations of the local spiral LIRG ESO~320-G030. We study the morphology and kinematics of the cold molecular gas traced by the CO(2--1) emission and combine these data with ancillary \textit{HST} optical and near-IR imaging as w... | 16 | 7 | 1607.03674 | We analyze new high spatial resolution (~60 pc) ALMA CO(2-1) observations of the isolated luminous infrared galaxy ESO 320-G030 (d = 48 Mpc) in combination with ancillary Hubble Space Telescope optical and near infrared (IR) imaging, as well as VLT/SINFONI near-IR integral field spectroscopy. We detect a high-velocity ... | false | [
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3332979 | [
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"Steeghs, D.",
"Maccarone, T. J.",
"Heinke, C.",
"Hynes, R. I.",
"Udalski, A.",
"Kostrzewa-Rutkowska, Z.",
"Groot, P. J.",
"Gazer, R.",
"Szymański, M. K.",
"Britt, C. T.",
"Wyrzykowski, Ł.",
"Poleski... | 2016MNRAS.462L.106W | [
"Discovery of a high state AM CVn binary in the Galactic Bulge Survey"
] | 19 | [
"Department of Astrophysics/IMAPP, Radboud University, PO Box 9010, NL-6500 GL Nijmegen, the Netherlands",
"Department of Astrophysics/IMAPP, Radboud University, PO Box 9010, NL-6500 GL Nijmegen, the Netherlands; SRON, Netherlands Institute for Space Research, Sorbonnelaan 2, NL-3584 CA Utrecht, the Netherlands",... | [
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"10.1093/mnrasl/slw141",
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] | 1607 | 1607.04262_arXiv.txt | \label{sec:introduction} AM Canum Venaticorum (AM CVn) systems are a class of binary stars, consisting of a white dwarf (WD) accreting H-deficient material from a low mass companion. These binaries are in a very compact configuration with observed orbital periods ranging from 5 to 65 min, suggesting the companion is a ... | \label{sec:discussion} We have discovered a persistent X-ray source, CX361, in the Galactic Bulge Survey. We obtained optical spectroscopy, presented in Figure \ref{fig:opticalspectra}. The spectrum shows shallow, broad and asymmetric He\,\textsc{i} absorption lines, lacking signatures of hydrogen. This is typical for ... | 16 | 7 | 1607.04262 | We report on the discovery of a hydrogen-deficient compact binary (CXOGBS J175107.6-294037) belonging to the AM CVn class in the Galactic Bulge Survey. Deep archival X-ray observations constrain the X-ray positional uncertainty of the source to 0.57 arcsec, and allow us to uniquely identify the optical and UV counterpa... | false | [
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1649322 | [
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"Dennihy, E.",
"Gianninas, A.",
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"Chote, P.",
"Winget, K. I."
] | 2016ApJ...829...82B | [
"Outbursts in Two New Cool Pulsating DA White Dwarfs"
] | 26 | [
"Department of Astronomy, University of Texas at Austin, Austin, TX-78712, USA ; McDonald Observatory, Fort Davis, TX-79734, USA;",
"Department of Physics and Astronomy, University of North Carolina, Chapel Hill, NC-27599, USA ;",
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] | 1607 | 1607.01392_arXiv.txt | White dwarf stars are the remnant products of 97\% of Galactic stellar evolution. About 80\% of white dwarfs spectroscopically display atmospheres dominated by hydrogen \citep[DA;][]{Tremblay2008}. Convective driving \citep{Brickhill1991,Goldreich1999} of nonradial gravity-mode pulsations \citep{Robinson1982} in DA whi... | \label{sec:conc} The four confirmed members of the outbursting class of DAV have three distinct commonalities: (1) repeated outbursts, recurring on irregular intervals of order days and lasting for several hours; (2) effective temperatures that put them near the cool, red edge of the DAV instability strip; and (3) ric... | 16 | 7 | 1607.01392 | The unprecedented extent of coverage provided by Kepler observations recently revealed outbursts in two hydrogen-atmosphere pulsating white dwarfs (DAVs) that cause hours-long increases in the overall mean flux of up to 14%. We have identified two new outbursting pulsating white dwarfs in K2, bringing the total number ... | false | [
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13975199 | [
"Slepian, Zachary",
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"Chuang, Chia-Hsun",
"Gil-Marín, Héctor",
"Ho, Shirley",
"Kitaura, Francisco-Shu",
"McEwen, Joseph E.",
"Percival, Will J.",
"Ross, Ashley J.",
"Rossi, Graziano",
"Seo, Hee-Jong",
"Slosar, Anže",
"... | 2018MNRAS.474.2109S | [
"Constraining the baryon-dark matter relative velocity with the large-scale three-point correlation function of the SDSS BOSS DR12 CMASS galaxies"
] | 47 | [
"Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA",
"Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA",
"Center for Cosmology and Astroparticle Physics, Department of Physics, The Ohio State University, OH 43210, USA",
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"10.1093/mnras/stx2723",
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] | 1607 | 1607.06098_arXiv.txt | \label{sec:intro} Prior to decoupling at redshift $z\sim 1020$, baryons and dark matter behave differently because they experience different forces. The Universe is ionized, and the electrons are tightly coupled to the photons through Thomson scattering, while the protons follow the electrons under the Coulomb force. ... | \label{sec:concs} We have shown that the 3PCF permits a $0.01$ precision measurement of the relative velocity bias, translating to about $0.5\%$ of the linear bias. We have shown three different estimates of this error bar that are all consistent with each other. For the data we find $b_v$ consistent with zero within... | 16 | 7 | 1607.06098 | We search for a galaxy clustering bias due to a modulation of galaxy number with the baryon-dark matter relative velocity resulting from recombination-era physics. We find no detected signal and place the constraint b<SUB>v</SUB> < 0.01 on the relative velocity bias for the CMASS galaxies. This bias is an important ... | false | [
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"the relative velocity",
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12408761 | [
"Corlies, Lauren",
"Schiminovich, David"
] | 2016ApJ...827..148C | [
"Empirically Constrained Predictions for Metal-line Emission from the Circumgalactic Medium"
] | 26 | [
"Department of Astronomy, Columbia University, New York, NY 10027, USA",
"Department of Astronomy, Columbia University, New York, NY 10027, USA"
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] | 10 | [
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"10.3847/0004-637X/827/2/148",
"10.48550/arXiv.1607.08616"
] | 1607 | 1607.08616_arXiv.txt | Perhaps the most basic process of galaxy formation, the flow of gas into and out of a galaxy, remains as one of the least understood. The key seems to lie in our lack of understanding of the circumgalactic medium (CGM). Roughly defined as the gas surrounding galaxies at 10 to 300 kpc, the CGM encompasses all gas in tr... | Observing the predicted gas halos of nearby galaxies has long been a goal of observations but the need to study this gas in the space ultraviolet coupled with the diffuse nature of the gas in question has made this challenging. Now, studies of the CGM at low redshift are entering an unprecedented age of sensitivity. ... | 16 | 7 | 1607.08616 | The circumgalactic medium (CGM) is one of the remaining least constrained components of galaxies and as such has significant potential for advancing galaxy formation theories. In this work, we vary the extragalactic ultraviolet background for a high-resolution cosmological simulation of a Milky-Way-like galaxy and exam... | false | [
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12472750 | [
"Wahl, Haley M.",
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] | 2016MNRAS.461.3740W | [
"Quasi-periodicities in the anomalous emission events in pulsars B1859+07 and B0919+06"
] | 21 | [
"Physics Department, University of Vermont, Burlington, VT 05405, USA",
"Physics Department, University of Vermont, Burlington, VT 05405, USA",
"Physics Department, University of Vermont, Burlington, VT 05405, USA",
"Physics and Astronomy Department, Carleton College, Northfield, MN 55057, USA"
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"2020MNRAS.493.3608J",
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] | 8 | [
"radiation mechanisms: non-thermal",
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"pulsars: individual: B1859+07 and B0919+06",
"Astrophysics - High Energy Astrophysical Phenomena",
"Astrophysics - Solar and Stellar Astrophysics"
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"10.1093/mnras/stw1589",
"10.48550/arXiv.1607.01737"
] | 1607 | 1607.01737_arXiv.txt | Pulsars are rapidly-rotating, highly-magnetized neutron stars that emit electromagnetic radiation along their magnetic axes which are tilted with respect to their rotation axes. This circumstance causes their radio signals to sweep across our sightline as the star rotates, producing discrete, regular pulses. Such pulse... | We report extensive new Arecibo observations and analyses studying the strange swooshes in pulsars B0919+06 and B1859+07. We find much more complexity that was earlier reported by Rankin \etal\ (2006); however, we confirm the basic effect involving usually gradual, temporary, about 10\degr\ shifts in the emission wind... | 16 | 7 | 1607.01737 | A quasi-periodicity has been identified in the strange emission shifts in pulsar B1859+07 and possibly B0919+06. These events, first investigated by Rankin, Rodriguez & Wright in 2006, originally appeared disordered or random, but further mapping as well as Fourier analysis has revealed that they occur on a fairly ... | false | [
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2152772 | [
"Robert, Jasmin",
"Gagné, Jonathan",
"Artigau, Étienne",
"Lafrenière, David",
"Nadeau, Daniel",
"Doyon, René",
"Malo, Lison",
"Albert, Loïc",
"Simard, Corinne",
"Bardalez Gagliuffi, Daniella C.",
"Burgasser, Adam J."
] | 2016ApJ...830..144R | [
"A Brown Dwarf Census from the SIMP Survey"
] | 37 | [
"Département de physique and Observatoire du Mont-Mégantic, Université de Montréal, Montréal, QC H3C 3J7, Canada ; Département de Physique, Université de Montréal, C.P. 6128 Succ. Centre-ville, Montréal, QC, H3C 3J7, Canada ;;",
"Département de physique and Observatoire du Mont-Mégantic, Université de Montréal, M... | [
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] | 13 | [
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"10.3847/0004-637X/830/2/144",
"10.48550/arXiv.1607.06117"
] | 1607 | 1607.06117_arXiv.txt | Ever since the discovery of the high proper motion of Barnard's star (\citealt{bar16}), proper motion has proved to be an effective method to identify faint stars in the solar neighborhood. Even thin disk stars, which are comoving with the Sun, have residual velocities of the order of tens of km\,s$^{-1}$. This arises ... | \label{Summary} A sample of 169 spectra have been obtained from different observatories for UCD candidates found through proper motion detection by comparing source position from the SIMP survey to 2MASS. From this sample, 164 UCDs, with spectral types from M8 to T6.5, were found, including 2 young field brown dwarfs,... | 16 | 7 | 1607.06117 | We have conducted a near-infrared (NIR) proper motion survey, the Sondage Infrarouge de Mouvement Propre, in order to discover field ultracool dwarfs (UCD) in the solar neighborhood. The survey was conducted by imaging ∼28% of the sky with the Caméra PAnoramique Proche-InfraRouge both in the southern hemisphere at the ... | false | [
"2MASS PSC",
"unwanted astrophysical sources",
"field ultracool dwarfs",
"L",
"the Cerro Tololo Inter-American Observatory",
"2 young field brown dwarfs",
"imaging ∼28%",
"the Two Micron All-Sky Survey Point Source Catalog",
"UCD",
"the source positions",
"2 candidate unresolved L+T binaries",
... | 6.987643 | 12.340874 | 102 |
2932983 | [
"Kóspál, Á.",
"Ábrahám, P.",
"Acosta-Pulido, J. A.",
"Dunham, M. M.",
"García-Álvarez, D.",
"Hogerheijde, M. R.",
"Kun, M.",
"Moór, A.",
"Farkas, A.",
"Hajdu, G.",
"Hodosán, G.",
"Kovács, T.",
"Kriskovics, L.",
"Marton, G.",
"Molnár, L.",
"Pál, A.",
"Sárneczky, K.",
"Sódor, Á.",
... | 2016A&A...596A..52K | [
"Multiwavelength study of the low-luminosity outbursting young star HBC 722"
] | 35 | [
"Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Hungarian Academy of Sciences, PO Box 67, 1525, Budapest, Hungary",
"Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Hungarian Academy of Sciences, PO Box 67, 1525, Budapest, Hungary",
"Instituto de Astrofísica de Can... | [
"2017A&A...597L..10K",
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"2020ApJ...899..130S",
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] | 7 | [
"stars: formation",
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"stars: individual: HBC 722",
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"10.1051/0004-6361/201528061",
"10.48550/arXiv.1607.05925"
] | 1607 | 1607.05925_arXiv.txt | Sun-like pre-main sequence stars are surrounded by circumstellar disks, from which material is accreted onto the growing protostar. The accretion rate is variable: the protostar's normal accretion at a low rate may be occasionally interspersed by brief episodes of highly enhanced accretion \citep{kenyon1990}. FU Orioni... | \label{sec:con} Based on our optical-infrared monitoring, spectroscopic observations, and millimeter mapping, we performed a detailed study of the first six years of the outburst of the low-mass T\,Tauri star HBC\,722. We interpreted the first brightness peak, lasting several months, as the rapid fall of piled-up mate... | 16 | 7 | 1607.05925 | Context. HBC 722 (V2493 Cyg) is a young eruptive star in outburst since 2010. Spectroscopic evidence suggests that the source is an FU Orionis-type object, with an atypically low outburst luminosity. <BR /> Aims: Because it was well characterized in the pre-outburst phase, HBC 722 is one of the few FUors from which we ... | false | [
"steady accretion disk models",
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"other epochs",
"many epochs",
"HBC",
"millimeter wavelengths",
"processes",
"mass",
"accretion-related outbursts",
"the late Class II phase",
"NASA",
"the pre-outburst phase",
"California Institute",
"Spitzer",
"a constant plateau... | 9.487344 | 11.69418 | 139 |
12406078 | [
"Luna, M.",
"Díaz, A. J.",
"Oliver, R.",
"Terradas, J.",
"Karpen, J."
] | 2016A&A...593A..64L | [
"The effects of magnetic-field geometry on longitudinal oscillations of solar prominences: Cross-sectional area variation for thin tubes"
] | 9 | [
"Instituto de Astrofísica de Canarias, 38205 La Laguna, Tenerife, Spain; Universidad de La Laguna, Dept. Astrofísica, 38206 La Laguna, Tenerife, Spain",
"Departament Física, Universitat de les Illes Balears, 07122 Palma de Mallorca, Spain",
"Departament Física, Universitat de les Illes Balears, 07122 Palma de M... | [
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"10.1051/0004-6361/201628845",
"10.48550/arXiv.1607.02996"
] | 1607 | 1607.02996_arXiv.txt | \label{sec:intro} Solar prominences are subject to various types of oscillatory motions \citep[see review by][]{arregui2012}. In general these oscillations are a combination of movements transverse and longitudinal to the local magnetic field. In early magnetohydrodynamic (MHD) descriptions of longitudinal oscillations... | \label{sec:conclusions} In this work we investigated the influence of the cross-sectional area, i.e., magnetic field, variations on the frequencies and velocity profiles of the normal modes in a flux tube containing a prominence thread surrounded by hot corona. We characterized the area variations with two parameters:... | 16 | 7 | 1607.02996 | Context. Solar prominences are subject to both field-aligned (longitudinal) and transverse oscillatory motions, as evidenced by an increasing number of observations. Large-amplitude longitudinal motions provide valuable information on the geometry of the filament-channel magnetic structure that supports the cool promin... | false | [
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12472551 | [
"Mazzalay, Ximena",
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"Saglia, Roberto P.",
"Wegner, Gary A.",
"Bender, Ralf",
"Erwin, Peter",
"Fabricius, Maximilian H.",
"Rusli, Stephanie P."
] | 2016MNRAS.462.2847M | [
"The supermassive black hole and double nucleus of the core elliptical NGC 5419"
] | 16 | [
"Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, D-85741 Garching, Germany",
"Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, D-85741 Garching, Germany; Universitätssternwarte, Scheinerstrasse 1, D-81679 München, Germany",
"Max-Planck-Institut für extraterrestrische Physik, P... | [
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"10.1093/mnras/stw1802",
"10.48550/arXiv.1607.06466"
] | 1607 | 1607.06466_arXiv.txt | It is now well established that super massive black holes (SMBHs) are present at the centres of galaxies with bulges. The observational correlations found between the black-hole mass and various parameters of the host galaxy, e.g., velocity dispersion, bulge mass, and bulge luminosity, have led to the idea that the for... | \label{s_summary} We have presented high-resolution \Kb\ \S/VLT IFS and optical long-slit spectroscopic observations of the galaxy \n5419. The kinematics derived from these data show that \n5419 is a dispersion-dominated galaxy. The rotational velocity does not exceed 50\kms; although a clear rotational pattern is obs... | 16 | 7 | 1607.06466 | We obtained adaptive-optics assisted SINFONI observations of the central regions of the giant elliptical galaxy NGC 5419 with a spatial resolution of 0.2 arcsec (≈55 pc). NGC 5419 has a large depleted stellar core with a radius of 1.58 arcsec (430 pc). HST and SINFONI images show a point source located at the galaxy's ... | false | [
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12460150 | [
"Cardoso, Vitor",
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] | 2016CQGra..33q4001C | [
"Testing the black hole ‘no-hair’ hypothesis"
] | 186 | [
"CENTRA, Departamento de Física, Instituto Superior Técnico, Universidade de Lisboa, Avenida Rovisco Pais 1, 1049 Lisboa, Portugal ; Perimeter Institute for Theoretical Physics, 31 Caroline Street North Waterloo, Ontario N2L 2Y5, Canada ; Theoretical Physics Department, CERN, CH-1211 Genève 23, Switzerland ;;",
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"10.1088/0264-9381/33/17/174001",
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] | 1607 | 1607.03133_arXiv.txt | the no-hair hypothesis (and why should we care)?} \subsection{The simplicity of black holes in General Relativity\label{sec:Sch}} We celebrate this year the first direct detection of gravitational waves (GWs) and the first detection of a black hole (BH) binary, in its last stages of coalescence~\cite{Abbott:2016blz}.... | It is by now well-known that the Kerr family is {\it not} the most general solution of Einstein's field equations in the presence of reasonable forms of matter. However, there are good reasons to believe that BHs which do not belong to the Kerr family are either dynamically unstable or do not form out of realistic coll... | 16 | 7 | 1607.03133 | Black holes (BHs) in general relativity (GR) are very simple objects. This property, that goes under the name of ‘no-hair’, has been refined in the last few decades and admits several versions. The simplicity of BHs makes them ideal testbeds of fundamental physics and of GR itself. Here we discuss the no-hair property ... | false | [
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12408842 | [
"Deng, Na",
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"Tian, Hui",
"Kleint, Lucia",
"Liu, Chang",
"Xu, Yan",
"Wang, Haimin"
] | 2016ApJ...829..103D | [
"Multi-wavelength Study of Transition Region Penumbral Subarcsecond Bright Dots Using IRIS and NST"
] | 15 | [
"Space Weather Research Laboratory, New Jersey Institute of Technology, University Heights, Newark, NJ 07102-1982, USA ; Big Bear Solar Observatory, New Jersey Institute of Technology, 40386 North Shore Lane, Big Bear City, CA 92314-9672, USA;",
"Big Bear Solar Observatory, New Jersey Institute of Technology, 403... | [
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"10.3847/0004-637X/829/2/103",
"10.48550/arXiv.1607.00306"
] | 1607 | 1607.00306_arXiv.txt | While sunspots have been observed for a long time, their fine structure and vertical extension are only revealed in recent decades by high-resolution and multi-wavelength (beyond visible) observations. Sunspots are concentrations of strong magnetic fields emerged from the convection zone. The magnetic fields are more v... | \label{sec:summary} We have presented a statistical study of TR penumbral subarcsecond BDs using multi-wavelength observations from IRIS and NST. A total of 2692 BDs are automatically identified from a 37-minute time series of IRIS 1400~\AA\ SJIs. They have a mean size of $\sim$400~km and a mean lifetime of $\sim$43~s... | 16 | 7 | 1607.00306 | Using high-resolution transition region (TR) observations taken by the Interface Region Imaging Spectrograph (IRIS) mission, Tian et al. revealed numerous short-lived subarcsecond bright dots (BDs) above sunspots (mostly located in the penumbrae), which indicate yet unexplained small-scale energy releases. Moreover, wh... | false | [
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2301789 | [
"Rujopakarn, W.",
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"Jagannathan, P.",
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"Alexander, D. M.",
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"Bhatnagar, S.",
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"Elbaz, D.",
"Geach, J. E.",
"Hayward, C. C.",
"Kirkpatri... | 2016ApJ...833...12R | [
"VLA and ALMA Imaging of Intense Galaxy-wide Star Formation in z ∼ 2 Galaxies"
] | 119 | [
"Kavli Institute for the Physics and Mathematics of the universe (WPI), The University of Tokyo Institutes for Advanced Study, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan ; Department of Physics, Faculty of Science, Chulalongkorn University, 254 Phayathai Road, Pathumwan, Bangkok 10330, Thailand;",
"I... | [
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"Astrophysics - Cosmology and Nongalactic Astrophysics"
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"10.3847/0004-637X/833/1/12",
"10.48550/arXiv.1607.07710"
] | 1607 | 1607.07710_arXiv.txt | \label{sec:intro} Numerical simulations and observational inferences suggest that typical star-forming galaxies (SFGs) at the peak of galaxy assembly activity, $z \simeq 1 - 3$, assembled most of their stellar mass via accretion of cold gas, which led to gas-rich, unstable disks and disk-wide star formation \citep[e.g... | \label{conclude} We have made the first comparison between ultra-deep VLA and ALMA imaging of $z \sim 2$ main-sequence SFGs. The far-infrared/radio correlation appears to hold for individual main-sequence SFGs with SFR $\sim$ 100 \Msunyr\ at $z \sim 2$ and the extinction-independent distributions of star formation are... | 16 | 7 | 1607.07710 | We present ≃0.″4 resolution extinction-independent distributions of star formation and dust in 11 star-forming galaxies (SFGs) at z = 1.3-3.0. These galaxies are selected from sensitive blank-field surveys of the 2‧ × 2‧ Hubble Ultra-Deep Field at λ = 5 cm and 1.3 mm using the Karl G. Jansky Very Large Array and Atacam... | false | [
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12464727 | [
"Alho, Artur",
"Carloni, Sante",
"Uggla, Claes"
] | 2016JCAP...08..064A | [
"On dynamical systems approaches and methods in f(R) cosmology"
] | 48 | [
"Center for Mathematical Analysis, Geometry and Dynamical Systems, Instituto Superior Técnico, Universidade de Lisboa, Av. Rovisco Pais, 1049-001 Lisboa, Portugal",
"Centro Multidisciplinar de Astrofisica – CENTRA, Instituto Superior Técnico, Universidade de Lisboa, Av. Rovisco Pais, 1049-001 Lisboa, Portugal",
... | [
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"10.1088/1475-7516/2016/08/064",
"10.48550/arXiv.1607.05715"
] | 1607 | 1607.05715_arXiv.txt | The simplest class of fourth order metric gravity theories is based on an action \begin{equation}\label{actionJ} \mathcal{S} = \int\left\{\frac{f(R)}{2\kappa^2} + \mathcal{L}_{m} \right\} \sqrt{-\det{g}}\, d^{4}x \end{equation} where $\kappa^2 = 8\pi G$; the speed of light, $c$, is set to one; $\det{g}$ is the determin... | \label{sec:disc} The global regular system we have presented for the Jordan frame naturally conveys the global properties of the models at hand, as illustrated by Figure~\ref{fig:VacuumJF}. Nevertheless, it is by no means an optimal dynamical system for all aspects one might want to investigate: there are other dynami... | 16 | 7 | 1607.05715 | We discuss dynamical systems approaches and methods applied to flat Robertson-Walker models in f(R)-gravity. We argue that a complete description of the solution space of a model requires a global state space analysis that motivates globally covering state space adapted variables. This is shown explicitly by an illustr... | false | [
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1469802 | [
"Vagnetti, F.",
"Middei, R.",
"Antonucci, M.",
"Paolillo, M.",
"Serafinelli, R."
] | 2016A&A...593A..55V | [
"Ensemble X-ray variability of active galactic nuclei. II. Excess variance and updated structure function"
] | 52 | [
"Dipartimento di FisicaUniversità di Roma \"Tor Vergata\", via della Ricerca Scientifica 1, 00133, Roma, Italy",
"Dipartimento di FisicaUniversità di Roma \"Tor Vergata\", via della Ricerca Scientifica 1, 00133, Roma, Italy; Dipartimento di Matematica e Fisica, Università Roma Tre, via della Vasca Navale 84, 0014... | [
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] | 12 | [
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"10.1051/0004-6361/201629057",
"10.48550/arXiv.1607.02629"
] | 1607 | 1607.02629_arXiv.txt | Variability is a distinctive feature shared by all classes of active galactic nuclei (AGN), occurring in all the wavebands and on different timescales from a fraction of a day up to years. In the X-ray band, variability is observed on timescales as short as hours, giving insight into the innermost AGN regions, but als... | The normalised excess variance is popularly used as a variability estimator. In most cases the method is applied correctly, using monitoring time intervals of fixed duration, for AGN samples at low redshift \citep[e.g. as in][]{pont12}. But this estimator depends on the length of the time interval in the rest frame and... | 16 | 7 | 1607.02629 | Context. Most investigations of the X-ray variability of active galactic nuclei (AGN) have been concentrated on the detailed analyses of individual, nearby sources. A relatively small number of studies have treated the ensemble behaviour of the more general AGN population in wider regions of the luminosity-redshift pla... | false | [
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1491627 | [
"Owocki, Stanley P.",
"ud-Doula, Asif",
"Sundqvist, Jon O.",
"Petit, Veronique",
"Cohen, David H.",
"Townsend, Richard H. D."
] | 2016MNRAS.462.3830O | [
"An `analytic dynamical magnetosphere' formalism for X-ray and optical emission from slowly rotating magnetic massive stars"
] | 60 | [
"Department of Physics and Astronomy, Bartol Research Institute, University of Delaware, Newark, DE 19716, USA",
"Penn State Worthington Scranton, Dunmore, PA 18512, USA",
"Centro de Astrobiología, CSIC-INTA, Ctra. Torrejón a Ajalvir km.4, E-28850 Madrid, Spain; Instituut voor Sterrenkunde, KU Leuven, Celestijn... | [
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] | 4 | [
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"10.1093/mnras/stw1894",
"10.48550/arXiv.1607.08568"
] | 1607 | 1607.08568.txt | Hot luminous, massive stars of spectral type O and B have dense, high-speed, radiatively driven stellar winds \citep{Castor75}. In the subset ($\sim$10\%) of massive stars with strong ($> 1$kG), globally ordered (often significantly dipolar) magnetic fields \citep{Petit13}, the trapping of the wind outflow by closed ma... | \label{sec:conclusions} The ADM analysis here provides readily computable formulae for the basic hydrodynamic quantities -- density, temperature, and velocity -- for each of the three components of a wind-fed dynamical magnetosphere -- wind upflow, hot post-shock gas, and cooled downflow. Comparison with time-averaged... | 16 | 7 | 1607.08568 | Slowly rotating magnetic massive stars develop `dynamical magnetospheres' (DMs), characterized by trapping of stellar wind outflow in closed magnetic loops, shock heating from collision of the upflow from opposite loop footpoints, and subsequent gravitational infall of radiatively cooled material. In 2D and 3D magnetoh... | false | [
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... | 8.788651 | 11.689974 | -1 |
12594336 | [
"Klencki, Jakub",
"Wiktorowicz, Grzegorz",
"Gładysz, Wojciech",
"Belczynski, Krzysztof"
] | 2017MNRAS.469.3088K | [
"Dynamical formation of black hole low-mass X-ray binaries in the field: an alternative to the common envelope"
] | 12 | [
"Astronomical Observatory, University of Warsaw, Al. Ujazdowskie 4, 00-478 Warsaw, Poland",
"Astronomical Observatory, University of Warsaw, Al. Ujazdowskie 4, 00-478 Warsaw, Poland",
"Astronomical Observatory, University of Warsaw, Al. Ujazdowskie 4, 00-478 Warsaw, Poland",
"Astronomical Observatory, Univers... | [
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] | 1607 | 1607.05186_arXiv.txt | There are currently 19 Galactic X-ray binary systems in which black holes (BHs) have been confirmed dynamically, with a few more extragalactic sources observed \citep{Remillard2006, Casares2014, Wiktorowicz2014, Tetarenko2016B}. They are all close binaries (with the majority of orbital periods $P_{\rm orb} < 1$ day), f... | \begin{enumerate} \item \textbf{The number of BH LMXBs:} we find that dynamical formation of LMXBs from primordial binaries in the Galactic field can lead to a population of $\sim$ 60--220 BH LMXBs, depending on the model of tidal circularization. This number could possibly be higher by a factor of about 4.5 if the d... | 16 | 7 | 1607.05186 | Very wide binaries (>500 au) are subject to numerous encounters with fly-by stars in the Galactic field and can be perturbed into highly eccentric orbits (e ∼ 0.99). For such systems, the tidal interactions at close pericentre passages can lead to orbit circularization and, possibly, to mass transfer, consequently p... | false | [
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12406321 | [
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"Evren, S.",
"Weber, M.",
"Granzer, T."
] | 2016A&A...593A.123O | [
"Time-series Doppler imaging of the red giant HD 208472. Active longitudes and differential rotation"
] | 10 | [
"Leibniz Institute for Astrophysics Potsdam (AIP), An der Sternwarte 16, 14482, Potsdam, Germany; Ege University, Faculty of Science, Astronomy and Space Sciences Department, 35100 Bornova, İzmir, Turkey",
"Leibniz Institute for Astrophysics Potsdam (AIP), An der Sternwarte 16, 14482, Potsdam, Germany",
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"2020ApJ...893..164X",
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"2021ApJ...907...89H"
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"10.1051/0004-6361/201628545",
"10.48550/arXiv.1607.06841"
] | 1607 | 1607.06841_arXiv.txt | \label{S1} Well-sampled photometric monitoring of spotted cool stars allows tracing photospheric brightness variations that are caused by rotational modulation. Long-term photometric data moreover allow investigating spot activity cycles and relate inherent changes of the surface spot distribution to photometric perio... | Three years of high-resolution time-series STELLA spectra enabled us to not only refine precise spectroscopic orbital elements and atmospheric parameters of HD~208472, but reconstruct 13 separate surface images from three observing seasons through multiple-line inversions. Surface reconstructions were made by tracing t... | 16 | 7 | 1607.06841 | Context. HD 208472 is among the most active RS CVn binaries with cool starspots. Decade-long photometry has shown that the spots seem to change their longitudinal appearance with a period of about six years, coherent with brightness variations. <BR /> Aims: Our aim is to spatially resolve the stellar surface of <ASTROB... | false | [
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12593805 | [
"Pjanka, Patryk",
"Zdziarski, Andrzej A.",
"Sikora, Marek"
] | 2017MNRAS.465.3506P | [
"The power and production efficiency of blazar jets"
] | 39 | [
"Department of Astrophysical Sciences, Princeton University, 4 Ivy Lane, Princeton, NJ 08544, USA",
"Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, Bartycka 18, PL-00-716 Warsaw, Poland",
"Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, Bartycka 18, PL-00-716 Warsaw, P... | [
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] | 1607 | 1607.08895_arXiv.txt | Starting with the seminal paper by \citet{Rawlings1991}, it has become common to use energetics and lifetimes of extended double radio sources to calculate jet powers in radio galaxies and quasars. Such studies indicated that in radio-loudest objects the jet power, $P_{\rm j}$, is comparable or even exceeds the accreti... | 16 | 7 | 1607.08895 | We use published data on the power and production efficiency of jets in blazars with double radio lobes in order to compare results obtained using different methods. In order to eliminate selection effects, we use cross-matched sub-samples containing only luminous blazars. We compare the three main existing methods, na... | false | [
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12406880 | [
"Wong, Ian",
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] | 2016AJ....152...90W | [
"A Hypothesis for the Color Bimodality of Jupiter Trojans"
] | 60 | [
"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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"10.3847/0004-6256/152/4/90",
"10.48550/arXiv.1607.04133"
] | 1607 | 1607.04133_arXiv.txt | In the past decade, Jupiter Trojans have been the subject of increasing scientific interest, and understanding their origin and surface properties promises to unlock many of the fundamental aspects of Solar System formation and evolution. These minor bodies share Jupiter's orbit around the Sun at 5.2~AU and reside in t... | We have proposed a simple hypothesis for the two color sub-populations within the Trojans. The main feature of our proposal is location-dependent sublimation of volatile ices within a primordial planetesimal disk in the outer Solar System, which divided objects in this region into two groups --- those that retained H$_... | 16 | 7 | 1607.04133 | One of the most enigmatic and hitherto unexplained properties of Jupiter Trojans is their bimodal color distribution. This bimodality is indicative of two sub-populations within the Trojans, which have distinct size distributions. In this paper, we present a simple, plausible hypothesis for the origin and evolution of ... | false | [
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"this primordial color bimodal... | 8.056985 | 16.306089 | -1 |
12473104 | [
"Sesto, Leandro A.",
"Faifer, Favio R.",
"Forte, Juan C."
] | 2016MNRAS.461.4260S | [
"The complex star cluster system of NGC 1316 (Fornax A)"
] | 26 | [
"Facultad de Cs. Astronómicas y Geofísicas, Univ. Nac. de La Plata, Paseo del bosque S/N, B1900FWA LA Plata, Argentina; Instituto de Astrofísica de La Plata, Paseo del bosque S/N, B1900FWA LA Plata, Argentina; Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET), Rivadavia 1917, C1033AAJ Ciudad Autó... | [
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"2019MNRAS.483.4371C",
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"10.1093/mnras/stw1627",
"10.48550/arXiv.1607.04305"
] | 1607 | 1607.04305_arXiv.txt | \label{Intro} Once considered as `simple systems', Globular Clusters (GCs) are steadily leaving that characterization as more complex features of their stellar populations are discovered, e.g., \citet{Carretta2015}. This situation emphasizes the problem of not only understanding their formation as individuals but also... | \label{sec8} The discussion of the $gri'$ photometry of cluster candidates in $NGC~1316$ presented in this paper, confirms earlier results that pointed out the complexity of the cluster system in this galaxy.\\ We identify four cluster subpopulations with distinct characteristics, namely:\\ a) Very blue clusters. \no... | 16 | 7 | 1607.04305 | This paper presents Gemini-gri' high-quality photometry for cluster candidates in the field of NGC 1316 (Fornax A) as part of a study that also includes GMOS spectroscopy. A preliminary discussion of the photometric data indicates the presence of four stellar cluster populations with distinctive features in terms of ag... | false | [
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12405904 | [
"McLaughlin, J. A.",
"Botha, G. J. J.",
"Régnier, S.",
"Spoors, D. L."
] | 2016A&A...591A.103M | [
"3D WKB solution for fast magnetoacoustic wave behaviour around an X-line"
] | 1 | [
"Department of Mathematics and Information Sciences, Northumbria University, Newcastle upon Tyne, NE1 8ST, UK",
"Department of Mathematics and Information Sciences, Northumbria University, Newcastle upon Tyne, NE1 8ST, UK",
"Department of Mathematics and Information Sciences, Northumbria University, Newcastle u... | [
"2017ApJ...837...94T"
] | [
"astronomy"
] | 6 | [
"magnetic fields",
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"1999A&A...346..... | [
"10.1051/0004-6361/201527789",
"10.48550/arXiv.1607.02379"
] | 1607 | 1607.02379_arXiv.txt | It is now clear that magnetohydrodynamic (MHD) wave motions (e.g. Roberts \cite{Bernie}; Nakariakov \& Verwichte \cite{NV2005}; De Moortel \cite{DeMoortel2005}) are ubiquitous throughout the solar atmosphere (Tomczyk et al. \cite{Tomczyk}). Several different types of MHD wave motions have been observed by various so... | This paper describes an investigation into the behaviour of fast magnetoacoustic waves in the neighbourhood of two magnetic dipoles, under the assumptions of ideal and cold plasma. We have demonstrated how the WKB approximation can be used to help solve the linearised MHD equations and we have utilised Charpit's meth... | 16 | 7 | 1607.02379 | Context. We study the propagation of a fast magnetoacoustic wave in a 3D magnetic field created from two magnetic dipoles. The magnetic topology contains an X-line. <BR /> Aims: We aim to contribute to the overall understanding of MHD wave propagation within inhomogeneous media, specifically around X-lines. <BR /> Meth... | false | [
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"the fast magnetoacoustic wave... | 12.452478 | 14.642676 | 2 |
12509811 | [
"Kastaun, W.",
"Ciolfi, R.",
"Giacomazzo, B."
] | 2016PhRvD..94d4060K | [
"Structure of stable binary neutron star merger remnants: A case study"
] | 84 | [
"Physics Department, University of Trento, via Sommarive 14, I-38123 Trento, Italy and INFN-TIFPA, Trento Institute for Fundamental Physics and Applications, via Sommarive 14, I-38123 Trento, Italy",
"Physics Department, University of Trento, via Sommarive 14, I-38123 Trento, Italy and INFN-TIFPA, Trento Institut... | [
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"10.1103/PhysRevD.94.044060",
"10.48550/arXiv.1607.02186"
] | 1607 | 1607.02186_arXiv.txt | \label{sec:intro} Binary neutron star (BNS) mergers are one of the most interesting astrophysical scenarios since their description requires both general relativity (GR) in the strong field regime as well as nuclear physics for matter above nuclear density, in particular the equation of state (EOS) and neutrino physic... | \label{sec:summary} In this work, we investigated the merger of two NSs, each with a mass of $1.4 \usk M_\odot$, employing the Shen-Horowitz-Teige EOS. Because of the atypically large maximum mass allowed by this EOS, the result is a stable NS. We followed in detail the fluid flow during and after merger and found tha... | 16 | 7 | 1607.02186 | In this work, we study the merger of two neutron stars with a gravitational mass of 1.4 M<SUB>⊙</SUB> each, employing the Shen-Horowitz-Teige equation of state. This equation of state is a corner case, allowing the formation of a stable neutron star with the given total baryonic mass of 3.03 M<SUB>⊙</SUB>. We investiga... | false | [
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"short gamma-ray burst models",
"numeric simulations",
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"compactness",
"Ke... | 6.357708 | 2.352713 | 62 |
12521800 | [
"Estes, John",
"Kavic, Michael",
"Lippert, Matthew",
"Simonetti, John H."
] | 2017ApJ...837...87E | [
"Shining Light on Quantum Gravity with Pulsar-Black hole Binaries"
] | 10 | [
"Department of Physics, Long Island University, Brooklyn, NY 11201, USA",
"Department of Physics, Long Island University, Brooklyn, NY 11201, USA",
"Department of Physics, Long Island University, Brooklyn, NY 11201, USA",
"Department of Physics, Virginia Tech, Blacksburg, VA, USA"
] | [
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"2020MNRAS.495..600K",
"2021MNRAS.504.3682C"
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"2008CQGra..25n5... | [
"10.3847/1538-4357/aa610e",
"10.48550/arXiv.1607.00018"
] | 1607 | 1607.00018_arXiv.txt | Observable effects of quantum gravity are highly elusive. One reason is that the Planck scale, where such effects are expected to be manifest, is well beyond the reach of current experiments. In addition, regions of strong spacetime curvature, in which general relativity is expected to break down and be superseded by... | \label{sec:Discussion} In this paper we have argued that PSR--BH binaries are ideally suited to probe metric fluctuations near the event horizons of black holes. More specifically, we have demonstrated that a particular version of the nonviolent nonlocality proposal to resolve the BH information loss paradox predicts... | 16 | 7 | 1607.00018 | Pulsars are some of the most accurate clocks found in nature, while black holes offer a unique arena for the study of quantum gravity. As such, pulsar-black hole (PSR-BH) binaries provide ideal astrophysical systems for detecting the effects of quantum gravity. With the success of aLIGO and the advent of instruments li... | false | [
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... | 7.005116 | 3.429298 | -1 |
12406323 | [
"Majaess, D.",
"Turner, D.",
"Dékány, I.",
"Minniti, D.",
"Gieren, W."
] | 2016A&A...593A.124M | [
"Constraining dust extinction properties via the VVV survey"
] | 30 | [
"Mount Saint Vincent University, Halifax, NS B3M 2J6, Canada ; Department of Astronomy & Physics, Saint Mary's University, Halifax, NS, B3H 3C3, Canada",
"Department of Astronomy & Physics, Saint Mary's University, Halifax, NS, B3H 3C3, Canada",
"Astronomisches Rechen-Institut, Zentrum für Astronomie de... | [
"2016ApJ...830L..14M",
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"2018ApJ...863...79C",
"2019A&A...628A..36D",
"2019ApJ...883..... | [
"astronomy"
] | 2 | [
"dust",
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"10.1051/0004-6361/201628763",
"10.48550/arXiv.1607.08623"
] | 1607 | 1607.08623_arXiv.txt | Applying corrections for dust extinction is a ubiquitous task executed in disciplines throughout astronomy, yet key concerns persist regarding the topic. Cited color-excess and total-to-selective extinction ratios are contested \citep{tu12,na16}, and a debate continues regarding the compositional nature of dust and th... | \label{s-conclusion} New near-infrared observations from the $VVV$ survey were employed to help establish color-excess and total extinction ratios across the Galaxy. To that end, Type II Cepheids and RR Lyrae variables were identified throughout the bulge and an adjacent region of the disk. The $VVV$ observations wer... | 16 | 7 | 1607.08623 | Near-infrared color-excess and extinction ratios are essential for establishing the cosmic distance scale and probing the Galaxy, particularly when analyzing targets attenuated by significant dust. A robust determination of those ratios followed from leveraging new infrared observations from the VVV survey, wherein num... | false | [
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12437107 | [
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12520464 | [
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12436113 | [
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"Properties of strongly magnetized ultradense matter and their imprints on magnetar pulsations"
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] | 1607 | 1607.04707_arXiv.txt | \label{sec:intro} Compact stars have a large number of pulsation modes that have been extensively studied since the seminal work of Chandrasekhar on radial oscillations \cite{APJ140:417:1964,PRL12:114:1964}. In general, these modes are very difficult to observe in the electromagnetic spectrum; therefore most efforts ... | In this section we analyse the effect that a strong magnetic field could produce on the fundamental mode of the radial oscillations of hadronic stars. As mentioned before, we consider that the magnetic field decays with the density following the fast and slow profiles presented in Section \ref{B-density-depndence}. A... | 16 | 7 | 1607.04707 | We investigate the effect of strong magnetic fields on the adiabatic radial oscillations of hadronic stars. We describe magnetized hadronic matter within the framework of the relativistic nonlinear Walecka model and integrate the equations of relativistic radial oscillations to determine the fundamental pulsation mode.... | false | [
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12623290 | [
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"Gravitational Waves from Oscillons after Inflation"
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"Deparment of Physics, University of Basel, Klingelbergstr. 82, CH-4056 Basel, Switzerland; Max-Planck-Institut für Physik (Werner-Heisenberg-Institut), Föhringer Ring 6, D-80805 München, Germany",
"Deparment of Physics, University of Basel, Klingelbergstr. 82, CH-4056 Basel, Switzerland",
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1497653 | [
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"Departamento de Investigación Básica, CIEMAT, 28040, Madrid. Spain",
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"E.A. Milne Centre for Astrophysics, Dept. of Physics & Mathematics, University of Hull, Hull, HU6 7RX, United Kingdom",
"Instituto de Física e Química, Universidade Federal de Ita... | null | [
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] | 1607 | 1607.06228_arXiv.txt | Chemical evolution models are the classical tool by which to interpret observed elemental abundances, and associated quantities such as gas and stellar surface densities, star formation histories, and the distribution of stellar ages. Elemental patterns carry the fingerprint of star formation timescales from their bir... | \begin{itemize} \item A grid of chemical evolution models with 16 dynamical masses in the range 10$^{10}$ to 10$^{13}\,M_{\odot}$ is calculated. A MWG-like model reproduces very well the observed radial distributions, as shown in \cite{molla15} and \cite{molla16b}. \item Prescriptions from \cite{bli} and \cite{fu10} fo... | 16 | 7 | 1607.06228 | We summarize the results obtained from our suite of chemical evolution models for spiral disks, computed for different total masses and star formation efficiencies. Once the gas, stars and star formation radial distributions are reproduced, we analyze the Oxygen abundances radial profiles for gas and stars, in addition... | false | [
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12594074 | [
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] | 2017MNRAS.467.2019R | [
"The stellar mass-halo mass relation of isolated field dwarfs: a critical test of ΛCDM at the edge of galaxy formation"
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"Dipartimento di Fisica e Astronomia, Università di Bologna, Viale Berti Pichat 6/2, I-40127, Bologna, Italy; INAF - Osservatorio Astronomico di Bologna, via Ranzani 1, I-40127, Bologna, Italy",
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] | 1607 | 1607.03127_arXiv.txt | \label{sec:intro} The standard $\Lambda$ Cold Dark Matter ($\Lambda$CDM) cosmological model gives an excellent description of the growth of structure in the Universe, matching the observed temperature fluctuations in the cosmic microwave background radiation \citep[e.g.][]{1992ApJ...396L...1S,2013arXiv1303.5076P}; the ... | \label{sec:conclusions} We have presented a clean probe of cosmology on small scales that follows from the comparison of \MstarMrot, measured from the rotation curves of isolated dwarf galaxies in the field, and \MstarMabund\ calculated from abundance matching (see \S\ref{sec:newprobe}). These should agree if the cosm... | 16 | 7 | 1607.03127 | We fit the rotation curves of isolated dwarf galaxies to directly measure the stellar mass-halo mass relation (M<SUB>⋆</SUB>-M<SUB>200</SUB>) over the mass range 5 × 10<SUP>5</SUP> ≲ M<SUB>⋆</SUB>/M<SUB>⊙</SUB> ≲ 10<SUP>8</SUP>. By accounting for cusp-core transformations due to stellar feedback, we find a monotonic re... | false | [
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12621568 | [
"Anber, Mohamed M.",
"Sabancilar, Eray"
] | 2017PhRvD..96b3501A | [
"Chiral gravitational waves from chiral fermions"
] | 13 | [
"Lewis & Clark College, Portland, Oregon 97219, USA; Institute of Physics, Ecole Polytechnique Fédérale de Lausanne CH-1015 Lausanne Switzerland",
"Institute of Physics, Ecole Polytechnique Fédérale de Lausanne CH-1015 Lausanne Switzerland; Bielefeld University, D-33615 Bielefeld, Germany"
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"10.1103/PhysRevD.96.023501",
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] | 1607 | 1607.03916_arXiv.txt | \label{sec:introduction} Gravitational waves (GW) are an invaluable probe for studying the early Universe as well as various astrophysical events. Recently, there has been a tremendous effort to detect them using both direct and indirect methods. Primordial gravitational waves, i.e., GW of cosmological origin, leave ... | \label{sec:discussion} In this work, we reported on a new mechanism to generate chiral gravitational waves from the imbalance between left and right-handed fermions. This imbalance breaks $\cal P$ and leads to an enhancement of a certain helicity mode of gravitational waves. In particular, we showed that the nonpertur... | 16 | 7 | 1607.03916 | We report on a new mechanism that leads to the generation of primordial chiral gravitational waves, and hence, the violation of the parity symmetry in the Universe. We show that nonperturbative production of fermions with a definite helicity is accompanied by the generation of chiral gravitational waves. This is a gene... | false | [
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12473126 | [
"Botteon, A.",
"Gastaldello, F.",
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] | 2016MNRAS.463.1534B | [
"A M ≳ 3 shock in `El Gordo' cluster and the origin of the radio relic"
] | 67 | [
"Dipartimento di Fisica e Astronomia, Università di Bologna, via C. Ranzani 1, I-40127 Bologna, Italy; INAF - IRA, via P. Gobetti 101, I-40129 Bologna, Italy",
"INAF - IASF Milano, via E. Bassini 15, I-20133 Milano, Italy",
"INAF - IRA, via P. Gobetti 101, I-40129 Bologna, Italy",
"National Centre for Radio A... | [
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"2017MNRAS.471.1107H",
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"2017MNRAS.471.4587D",
"2017MNRAS.471.4747C",
"2017MNRAS.472.3... | [
"astronomy"
] | 14 | [
"shock waves",
"X-rays: galaxies: clusters",
"galaxies: clusters: individual: ACT-CL J0102-4915",
"radio continuum: general",
"radiation mechanisms: non-thermal",
"Astrophysics - High Energy Astrophysical Phenomena",
"Astrophysics - Cosmology and Nongalactic Astrophysics"
] | [
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"2004ApJ...602L..73F",
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"10.1093/mnras/stw2089",
"10.48550/arXiv.1607.04641"
] | 1607 | 1607.04641_arXiv.txt | Galaxy clusters are the largest virialized structures in the Universe and form via aggregation of less massive systems \citep[\eg][]{press74}. During merger events, the intra-cluster medium (ICM) is heated by shocks and is believed to become turbulent. Part of the energy involved in these processes is converted into no... | We presented an X-ray/radio study of the famous `El Gordo' cluster located at $z=0.87$ focusing on the non-thermal activity in the cluster. \\ \indent Our GMRT radio observations at 610 and 327~$\rm{MHz}$ confirmed the presence of a halo and a system of double relics. These represent the most distant diffuse radio sour... | 16 | 7 | 1607.04641 | We present an X-ray and radio study of the famous `El Gordo', a massive and distant (z = 0.87) galaxy cluster. In the deep (340 ks) Chandra observation, the cluster appears with an elongated and cometary morphology, a sign of its current merging state. The GMRT radio observations at 610 MHz confirm the presence of a ra... | false | [
"radio relics",
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"The GMRT radio observations",
"an X-ray and radio study",
"a radio halo",
"these radio sources",
"its current merging state",
"Chandra observation",
"a galaxy cluster",
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12473130 | [
"Bodo, G.",
"Mamatsashvili, G.",
"Rossi, P.",
"Mignone, A."
] | 2016MNRAS.462.3031B | [
"Linear stability analysis of magnetized jets: the rotating case"
] | 19 | [
"INAF/Osservatorio Astrofisico di Torino, Strada Osservatorio 20, I-10025 Pino Torinese, Italy",
"Helmholtz-Zentrum Dresden-Rossendorf, PO Box 510119, D-01314 Dresden, Germany; Department of Physics, Faculty of Exact and Natural Sciences, Tbilisi State University, Il. Chavchavadze ave 3, Tbilisi 0179, Georgia; Ab... | [
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"2022A&A...667A.138K",
"2022ApJS..261...22C",
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"10.1093/mnras/stw1650",
"10.48550/arXiv.1607.01587"
] | 1607 | 1607.01587_arXiv.txt | An important step for understanding the dynamics and phenomenology of astrophysical jets is the study of their instabilities. Instabilities have a substantial importance, on one hand for the formation and evolution of various observed structures and, on the other hand, for dissipating part of the jet energy and leading... | \label{summary} \begin{figure} \centering \includegraphics[width=15cm]{fig19.eps} % \caption{\small The dominant instability types for $ka=0.1$, in the different regions of the parameter plane $(\Omega_c, P_c)$. In the region marked by a green shading, the instability with the largest growth rate is the CDI, while ... | 16 | 7 | 1607.01587 | We perform a linear stability analysis of magnetized rotating cylindrical jet flows in the approximation of zero thermal pressure. We focus our analysis on the effect of rotation on the current driven mode and on the unstable modes introduced by rotation. We find that rotation has a stabilizing effect on the current dr... | false | [
"rotation velocities",
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"Alfvén",
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"the current driven mode",
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12473489 | [
"Maxted, Nigel I.",
"de Wilt, Phoebe",
"Rowell, Gavin P.",
"Nicholas, Brent P.",
"Burton, Michael. G.",
"Walsh, Andrew",
"Fukui, Yasuo",
"Kawamura, Akiko"
] | 2016MNRAS.462..532M | [
"Ammonia excitation imaging of shocked gas towards the W28 gamma-ray source HESS J1801-233"
] | 9 | [
"School of Physics, University of New South Wales, Sydney 2052, Australia",
"School of Physical Sciences, Adelaide University, Adelaide 5005, Australia",
"School of Physical Sciences, Adelaide University, Adelaide 5005, Australia",
"School of Physical Sciences, Adelaide University, Adelaide 5005, Australia",
... | [
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"2020MNRAS.495.2909R",
"2023ApJ...950...64I",
"2024ApJ...966..178T"
] | [
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"cosmic rays",
"gamma-rays: ISM",
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"10.1093/mnras/stw1687",
"10.48550/arXiv.1607.03061"
] | 1607 | 1607.03061_arXiv.txt | W28 is a mature ($>10^{4}$\,yr, \citealt{kaspi1993}) mixed-morphology supernova remnant (SNR) and a prime example of a region of TeV (10$^{12}$\,eV) gamma-ray excess overlapping with molecular gas \citep{hess:w28}; one indicator of a hadronic production mechanism. W28 is estimated to be at a distance of 1.2-3.3\,kpc (e... | \label{sec:conc} We reported on deep mapping observations towards the shocked molecular cloud north-east of W28, with a focus on detecting multiple \nh3 inversion transitions. % The NE cloud has a remarkable spatial match with the gamma-ray source HESS J1801-233, so constraints on the mass distribution are important fo... | 16 | 7 | 1607.03061 | We present 12 mm Mopra observations of the dense (>10<SUP>3</SUP> cm<SUP>-3</SUP>) molecular gas towards the north-east of the W28 supernova remnant (SNR). This cloud is spatially well matched to the TeV gamma-ray source HESS J1801-233 and is known to be an SNR-molecular cloud interaction region. Shock-disruption is... | false | [
"NH",
"SNR",
"SUB>3</SUB",
"molecular gas",
"W28",
"an SNR-molecular cloud interaction region",
"the W28 SNR shock",
"strong detections",
"high temperatures",
"this molecular cloud",
"regions",
"the W28 SNR",
"cloud-disruption",
"disruption",
"spatially extended NH",
"a hot, dense mole... | 4.292176 | 4.891167 | 60 |
12435444 | [
"Chang, Chia-Feng"
] | 2016arXiv160703347C | [
"Hidden Photon Compton and Bremsstrahlung in White Dwarf Anomalous Cooling and Luminosity Functions"
] | 5 | [
"-"
] | [
"2017IJMPA..3250138H",
"2017JHEP...03..139H",
"2018JHEP...03..139H",
"2019arXiv190201055D",
"2020PhR...870....1D"
] | [
"astronomy",
"physics"
] | 3 | [
"High Energy Physics - Phenomenology",
"Astrophysics - High Energy Astrophysical Phenomena"
] | [
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"1968ARA&A...6..351W",
"1969fecg.book.....B",
"1973ApJ...180..911F",
"1976ApJ...203..297S",
"1986PhLB..166..196H",
"1986PhLB..178...65H",
"1989ApJ...340..661G",
"1991ApJ...378L..45K",
"1991PhLB..267..509F",
"1991PhRvD..44.2118H",
"1992ApJ...386..539W",
"1992ApJ...392L.... | [
"10.48550/arXiv.1607.03347"
] | 1607 | 1607.03347_arXiv.txt | The addition of an extra $U(1)_D$ gauge symmetry, implying the existence of an exotic massive neutral gauge boson, is one of the much investigated extensions of the Standard Model (SM) \cite{SM}. This exotic gauge boson is called hidden(dark) photon and denoted by $\gamma_D$ in literatures \cite{Holdom,Nath,HeCalculati... | In this paper we have derived an improved value of the kinetic mixing parameter $\epsilon$, assuming that the mass of the hidden photon $\gamma_D$ is smaller than the core temperature of white dwarfs ($\approx$ keV), and also assuming that the enhanced rate of cooling of the pulsating white dwarf is entirely due to the... | 16 | 7 | 1607.03347 | We computed the contribution of the Compton and Bremsstrahlung processes with a hidden light $U(1)_D$ neutral boson $\gamma_D$ to the white dwarf G117-B15A anomalous cooling rate, as well as the white dwarf luminosity functions (WDLF). We demonstrated that for a light mass of hidden photon ($m_{\gamma_D} \ll$ a few keV... | false | [
"white dwarf",
"WDLF",
"Sky Survey",
"different kinetic",
"\\times",
"the white dwarf luminosity functions",
"a constant star formation rate",
"the white dwarf G117-B15A anomalous cooling rate",
"the recent Sloan Digital Sky Survey",
"compatible results",
"the oldest computed stars",
"an anoma... | 8.381916 | -1.145562 | -1 |
12516896 | [
"Defrère, D.",
"Hinz, P.",
"Downey, E.",
"Böhm, M.",
"Danchi, W. C.",
"Durney, O.",
"Ertel, S.",
"Hill, J. M.",
"Hoffmann, W. F.",
"Mennesson, B.",
"Millan-Gabet, R.",
"Montoya, M.",
"Pott, J. -U.",
"Skemer, A.",
"Spalding, E.",
"Stone, J.",
"Vaz, A."
] | 2016SPIE.9907E..1GD | [
"Simultaneous water vapor and dry air optical path length measurements and compensation with the large binocular telescope interferometer"
] | 6 | [
"Univ. of Arizona (United States)",
"Univ. of Arizona (United States)",
"Univ. of Arizona (United States)",
"Univ. of Stuttgart (Germany)",
"NASA Goddard Space Flight Ctr. (United States)",
"Univ. of Arizona (United States)",
"Univ. of Arizona (United States)",
"Univ. of Arizona (United States)",
"U... | [
"2017JOSAA..34A..10B",
"2017PASP..129f5001G",
"2018SPIE10701E..0UD",
"2018SPIE10701E..1MM",
"2020JATIS...6c5001M",
"2022SPIE12183E..02E"
] | [
"astronomy",
"physics"
] | 4 | [
"Astrophysics - Instrumentation and Methods for Astrophysics"
] | [
"2003SPIE.4838..609M",
"2003SPIE.4838..625K",
"2004PASP..116..876C",
"2006A&A...448..787A",
"2006SPIE.6268E..16K",
"2006SPIE.6268E..31H",
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"2010A&A...515A..69M",
"2014A&A...567A..98M",
"2014SPIE.9146E..07D",
"2014SPIE.9146E..09D",
"2016ApJ...824...66D"
] | [
"10.1117/12.2233884",
"10.48550/arXiv.1607.08749"
] | 1607 | 1607.08749_arXiv.txt | \label{sec:intro} % Water vapor turbulence can limit the performance of high dynamic range interferometers that use phase-referenced modes, even though such turbulence is only a small contributor to the total seeing at visible and infrared wavelengths. Indeed, because water vapor is highly dispersive, random fluctuat... | \label{sec:summary} Recent efforts in co-phasing the LBTI were focused on two main areas: (1) improving the performance of the system at K band where the fringe sensor operates and (2) compensating for atmospheric dispersion with the implementation of a new sensing mode. Thanks to an improved real-time control loop, a... | 16 | 7 | 1607.08749 | The Large Binocular Telescope Interferometer uses a near-infrared camera to measure the optical path length variations between the two AO-corrected apertures and provide high-angular resolution observations for all its science channels (1.5-13 microns). There is however a wavelength dependent component to the atmospher... | false | [
"optical path length errors",
"dry air seeing compensation",
"the optical path length fluctuations",
"the optical path length variations",
"the path length fluctuations",
"high-precision infrared interferometric observations",
"high-angular resolution observations",
"Water vapor",
"dry air and water... | 13.981673 | 10.465308 | 11 |
2074416 | [
"Karkare, K. S.",
"Ade, P. A. R.",
"Ahmed, Z.",
"Alexander, K. D.",
"Amiri, M.",
"Barkats, D.",
"Benton, S. J.",
"Bischoff, C. A.",
"Bock, J. J.",
"Boenish, H.",
"Bowens-Rubin, R.",
"Buder, I.",
"Bullock, E.",
"Buza, V.",
"Connors, J.",
"Filippini, J. P.",
"Fliescher, S. T.",
"Gray... | 2016SPIE.9914E..30K | [
"Optical characterization of the BICEP3 CMB polarimeter at the South Pole"
] | 15 | [
"Harvard-Smithsonian Ctr. for Astrophysics (United States)",
"Cardiff Univ. (United Kingdom)",
"Stanford Univ. (United States)",
"Harvard-Smithsonian Ctr. for Astrophysics (United States)",
"The Univ. of British Columbia (Canada)",
"Harvard-Smithsonian Ctr. for Astrophysics (United States)",
"Univ. of T... | [
"2016SPIE.9914E..0SG",
"2016SPIE.9914E..0TH",
"2017arXiv170602464A",
"2018ApOpt..57.2314P",
"2018SPIE10708E..2NK",
"2019AIPA....9a5321M",
"2019ApJ...884..114B",
"2019MNRAS.486.5448D",
"2020JLTP..199..824S",
"2020OExpr..2823075I",
"2020SPIE11453E..27C",
"2020SPIE11453E..2ES",
"2021ITAP...69.3... | [
"astronomy",
"physics"
] | 6 | [
"Astrophysics - Instrumentation and Methods for Astrophysics",
"Astrophysics - Cosmology and Nongalactic Astrophysics"
] | [
"1985SvA....29..607P",
"2012SPIE.8452E..1GO",
"2014ApJ...792...62B",
"2014SPIE.9153E..1NA",
"2015ApJ...806..206B",
"2015ApJ...811..126B",
"2015ApJ...814..110B",
"2015PhRvL.114j1301B",
"2016JLTP..184..765W",
"2016PhRvL.116c1302B"
] | [
"10.1117/12.2231747",
"10.48550/arXiv.1607.04567"
] | 1607 | 1607.04567_arXiv.txt | \label{sec:intro} % A period of accelerated exponential expansion in the early Universe, while a radical extrapolation from understood physics, naturally solves the flatness, horizon, and monopole problems of standard cosmology\cite{planck_p15xx_15}. This inflationary period also explains the origin of structure by ... | \label{sect:conclusions} In these proceedings we have presented a preliminary analysis of \bicepthree's far field beam performance for the 2016 observing season. Measurements were made during the 2015-2016 deployment season using a new chopped thermal microwave source with a 24'' aperture. We find that \bicepthree\ ... | 16 | 7 | 1607.04567 | BICEP3 is a small-aperture refracting cosmic microwave background (CMB) telescope designed to make sensitive polarization maps in pursuit of a potential B-mode signal from inflationary gravitational waves. It is the latest in the Bicep/Keck Array series of CMB experiments located at the South Pole, which has provided t... | false | [
"pair differencing experiments",
"CMB experiments",
"detector",
"detectors",
"inflationary gravitational waves",
"sensitive polarization maps",
"many thousands",
"date",
"Keck Array",
"next-generation CMB experiments",
"CMB",
"differential pointing",
"inflation",
"polarization",
"calibra... | 10.671288 | 2.792256 | 68 |
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