August 2020 (Page 2)

Limits on axion-like particles from Mrk 421 with 4.5-years period observations by ARGO-YBJ and Fermi-LAT. (arXiv:2008.09464v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Li_H/0/1/0/all/0/1">Hai-Jun Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guo_J/0/1/0/all/0/1">Jun-Guang Guo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bi_X/0/1/0/all/0/1">Xiao-Jun Bi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lin_S/0/1/0/all/0/1">Su-Jie Lin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yin_P/0/1/0/all/0/1">Peng-Fei Yin</a> In this work, we investigate the axion-like particle (ALP)-photon oscillation effect in the spectra of the blazar Markarian 421 (Mrk 421) using 4.5 years of the ARGO-YBJ and Fermi-LAT data. These data are collected during the common operation time, which cover ten activity phases of Mrk 421. No significant ALP-photon oscillation effect is confirmed. Only the observations of three phases can be individually used to set the $95%$ $rm C.L.$ constraint onRead More →

One dimensional nexus objects, network of Kibble-Lazarides-Shafi string walls, and their spin dynamic response in polar distorted B-phase of $^3$He. (arXiv:2008.09286v2 [cond-mat.mes-hall] UPDATED) <a href="http://arxiv.org/find/cond-mat/1/au:+Zhang_K/0/1/0/all/0/1">K. Zhang</a> The Kibble-Lazarides-Shafi (KLS) domain wall problem in the axion solution of CP violation in QCD has condensed-matter based analogy in the nafen-distorted superfluid $^3$He. Recent experiment in rotating superfluid $^3$He produced the network of KLS string walls in human controllable system. In this system, KLS string wall appears in two-step symmetry break transition from normal phase to polar-distorted B phase and turn out to be the descendants of HQVs of polar phase. Here we show the KLS string wallRead More →

Measuring the Hubble Constant with a sample of kilonovae. (arXiv:2008.07420v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Coughlin_M/0/1/0/all/0/1">Michael W. Coughlin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Antier_S/0/1/0/all/0/1">Sarah Antier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dietrich_T/0/1/0/all/0/1">Tim Dietrich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Foley_R/0/1/0/all/0/1">Ryan J. Foley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Heinzel_J/0/1/0/all/0/1">Jack Heinzel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bulla_M/0/1/0/all/0/1">Mattia Bulla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Christensen_N/0/1/0/all/0/1">Nelson Christensen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Coulter_D/0/1/0/all/0/1">David A. Coulter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Issa_L/0/1/0/all/0/1">Lina Issa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Khetan_N/0/1/0/all/0/1">Nandita Khetan</a> Kilonovae produced by the coalescence of compact binaries with at least one neutron star are promising standard sirens for an independent measurement of the Hubble constant ($H_0$). Through their detection via follow-up of gravitational-wave (GW), short gamma-ray bursts (sGRBs) or optical surveys, a large sample of kilonovae (even without GW data) can be used for $H_0$ contraints. Here, we showRead More →

Formation of disks with long-lived spiral arms from violent gravitational dynamics. (arXiv:2008.02605v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Labini_F/0/1/0/all/0/1">Francesco Sylos Labini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pinto_L/0/1/0/all/0/1">Luis Diego Pinto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Capuzzo_Dolcetta_R/0/1/0/all/0/1">Roberto Capuzzo-Dolcetta</a> By means of simple dynamical experiments we study the combined effect of gravitational and gas dynamics in the evolution of an initially out-of-equilibrium, uniform and rotating massive over-density thought of as in isolation. The rapid variation of the system mean-field potential makes the point like particles (PPs), which interact only via Newtonian gravity, form a quasistationary thick disk dominated by rotational motions surrounded by far out-of-equilibrium spiral arms. On the other side, the gas component is subjected to compression shocksRead More →

Magnetic Flux of Active Regions Determining the Eruptive Character of Large Solar Flares. (arXiv:2007.08127v2 [astro-ph.SR] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Li_T/0/1/0/all/0/1">Ting Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hou_Y/0/1/0/all/0/1">Yijun Hou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yang_S/0/1/0/all/0/1">Shuhong Yang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_J/0/1/0/all/0/1">Jun Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_L/0/1/0/all/0/1">Lijuan Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Veronig_A/0/1/0/all/0/1">Astrid M. Veronig</a> We establish the largest eruptive/confined flare database to date and analyze 322 flares of emph{GOES} class M1.0 and larger that occurred during 2010$-$2019, i.e., almost spanning the entire solar cycle 24. We find that the total unsigned magnetic flux ($Phi$$_{AR}$) of active regions (ARs) is a key parameter in governing the eruptive character of large flares, with the proportion of eruptive flares exhibiting a strong anti-correlation with $Phi$$_{AR}$. This meansRead More →

Dyson Spheres. (arXiv:2006.16734v2 [astro-ph.EP] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Wright_J/0/1/0/all/0/1">Jason T. Wright</a> I review the origins and development of the idea of Dyson spheres, their purpose, their engineering, and their detectability. I explicate the ways in which the popular imagining of them as monolithic objects would make them dynamically unstable under gravity and radiation pressure, and mechanically unstable to buckling. I develop a model for the radiative coupling between a star and large amounts of material orbiting it, and connect the observational features of a star plus Dyson sphere system to the gross radiative properties of the sphere itself. I discuss the still-unexplored problem of the effects ofRead More →

Special case of the Ba~{n}ados-Silk-West effect. (arXiv:2006.11552v3 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Zaslavskii_O/0/1/0/all/0/1">O. B. Zaslavskii</a> If two particles collide near the rotating extremal black hole and one of them is fine-tuned, the energy in the center of mass frame $E_{c.m.}$ can grow unbounded. This is the so-called Ba~{n}ados-Silk-West (BSW) effect. Recently, another type of high energy collisions was considered in which all processes happen in the Schwarzschild background with free falling particles. If the Killing energy $E$ of one of particle is sufficiently small, $E_{c.m.}$ grows unbounded. We show that, however, such a particle cannot be created in any precedent collision with finite energies, angular momenta andRead More →

The compressional beta-effect: Analytical solution, numerical benchmark, and data analysis. (arXiv:2004.15017v2 [physics.ao-ph] UPDATED) <a href="http://arxiv.org/find/physics/1/au:+Ong_H/0/1/0/all/0/1">Hing Ong</a>, <a href="http://arxiv.org/find/physics/1/au:+Roundy_P/0/1/0/all/0/1">Paul E. Roundy</a> This study derives a complete set of equatorially confined wave solutions from an anelastic equation set with the complete Coriolis terms, which include both the vertical and meridional planetary vorticity. The propagation mechanism can change with the effective static stability. When the effective static stability reduces to neutral, buoyancy ceases, but the role of buoyancy as an eastward-propagation mechanism is replaced by the compressional beta-effect, i.e., vertical density-weighted advection of the meridional planetary vorticity. For example, the Kelvin mode becomes a compressional Rossby mode. CompressionalRead More →

Parametrized test of parity-violating gravity using GWTC-1 events. (arXiv:2006.11086v2 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Yamada_K/0/1/0/all/0/1">Kei Yamada</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Tanaka_T/0/1/0/all/0/1">Takahiro Tanaka</a> Parity-violating (PV) gravity has recently attracted interest in several aspects. One of them is the axion-graviton coupling to test the axion-dark matter model. Moreover, by extending Chern-Simons (CS) gravity to include derivatives of a scalar field up to the second order, a more general class of PV gravity theory, which we call the CNCL model, has been proposed~[M. Crisostomi {it et al.}, Phys. Rev. D, {bf 97}, 044034 (2018)]. The model can be further extended by including even higher derivatives of the scalar field and/or higher curvature terms.Read More →

GAMA+KiDS: Empirical correlations between halo mass and other galaxy properties near the knee of the stellar-to-halo mass relation. (arXiv:2006.10040v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Taylor_E/0/1/0/all/0/1">Edward N. Taylor</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cluver_M/0/1/0/all/0/1">Michelle E. Cluver</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Duffy_A/0/1/0/all/0/1">Alan Duffy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gurri_P/0/1/0/all/0/1">Pol Gurri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hoekstra_H/0/1/0/all/0/1">Henk Hoekstra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sonnenfeld_A/0/1/0/all/0/1">Alessandro Sonnenfeld</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bremer_M/0/1/0/all/0/1">Malcolm N. Bremer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brouwer_M/0/1/0/all/0/1">Margot M. Brouwer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chisari_N/0/1/0/all/0/1">Nora Elisa Chisari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dvornik_A/0/1/0/all/0/1">Andrej Dvornik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Erben_T/0/1/0/all/0/1">Thomas Erben</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hildebrandt_H/0/1/0/all/0/1">Hendrik Hildebrandt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hopkins_A/0/1/0/all/0/1">Andrew M. Hopkins</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kelvin_L/0/1/0/all/0/1">Lee S. Kelvin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Phillipps_S/0/1/0/all/0/1">Steven Phillipps</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Robotham_A/0/1/0/all/0/1">Aaron S. G. Robotham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sifon_C/0/1/0/all/0/1">Cristobal Sifon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vakili_M/0/1/0/all/0/1">Mohammadjavad Vakili</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wright_A/0/1/0/all/0/1">Angus H. Wright</a> We use KiDS weak lensing data to measure variations in mean halo mass as a function ofRead More →

Repeated mergers and ejection of black holes within nuclear star clusters. (arXiv:2006.01867v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Fragione_G/0/1/0/all/0/1">Giacomo Fragione</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Silk_J/0/1/0/all/0/1">Joseph Silk</a> Current stellar evolution models predict a dearth of black holes (BHs) with masses $gtrsim 50$ M$_odot$ and $lesssim 5$ M$_odot$, and intermediate-mass black holes (IMBHs; $sim10^2- 10^5$ M$_odot$) have not yet been detected beyond any reasonable doubt. A natural way to form massive BHs is through repeated mergers, detectable via gravitational wave emission with current LIGO/Virgo or future LISA and ET observations. Nuclear star clusters (NSCs) have masses and densities high enough to retain most of the merger products, which acquire a recoil kick atRead More →

The age distribution of stars in the Milky Way bulge. (arXiv:2006.01158v2 [astro-ph.SR] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Sit_T/0/1/0/all/0/1">Tawny Sit</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ness_M/0/1/0/all/0/1">Melissa Ness</a> The age and chemical characteristics of the Galactic bulge link to the formation and evolutionary history of the Galaxy. Data-driven methods and large surveys enable stellar ages and precision chemical abundances to be determined for vast regions of the Milky Way, including the bulge. Here, we use the data-driven approach of The Cannon, to infer the ages and abundances for 125,367 stars in the Milky Way, using spectra from Apache Point Observatory Galaxy Evolution Experiment (APOGEE) DR14. We examine the ages and metallicities of 1654 bulgeRead More →

Testing gravity using galaxy-galaxy lensing and clustering amplitudes in KiDS-1000, BOSS and 2dFLenS. (arXiv:2005.14351v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Blake_C/0/1/0/all/0/1">Chris Blake</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amon_A/0/1/0/all/0/1">Alexandra Amon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Asgari_M/0/1/0/all/0/1">Marika Asgari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bilicki_M/0/1/0/all/0/1">Maciej Bilicki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dvornik_A/0/1/0/all/0/1">Andrej Dvornik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Erben_T/0/1/0/all/0/1">Thomas Erben</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Giblin_B/0/1/0/all/0/1">Benjamin Giblin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Glazebrook_K/0/1/0/all/0/1">Karl Glazebrook</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Heymans_C/0/1/0/all/0/1">Catherine Heymans</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hildebrandt_H/0/1/0/all/0/1">Hendrik Hildebrandt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Joachimi_B/0/1/0/all/0/1">Benjamin Joachimi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Joudaki_S/0/1/0/all/0/1">Shahab Joudaki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kannawadi_A/0/1/0/all/0/1">Arun Kannawadi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kuijken_K/0/1/0/all/0/1">Konrad Kuijken</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lidman_C/0/1/0/all/0/1">Chris Lidman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Parkinson_D/0/1/0/all/0/1">David Parkinson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shan_H/0/1/0/all/0/1">HuanYuan Shan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Troster_T/0/1/0/all/0/1">Tilman Tr&#xf6;ster</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Busch_J/0/1/0/all/0/1">Jan Luca van den Busch</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wolf_C/0/1/0/all/0/1">Christian Wolf</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wright_A/0/1/0/all/0/1">Angus H. Wright</a> The physics of gravity on cosmological scales affects both the rate of assembly of large-scale structure, and the gravitational lensing of backgroundRead More →

High-Energy Neutrino and Gamma-Ray Emission from Tidal Disruption Events. (arXiv:2005.08937v3 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Murase_K/0/1/0/all/0/1">Kohta Murase</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kimura_S/0/1/0/all/0/1">Shigeo S. Kimura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_B/0/1/0/all/0/1">B. Theodore Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oikonomou_F/0/1/0/all/0/1">Foteini Oikonomou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Petropoulou_M/0/1/0/all/0/1">Maria Petropoulou</a> Tidal disruption events (TDE) have been considered as cosmic-ray and neutrino sources for a decade. We suggest two classes of new scenarios for high-energy multi-messenger emission from TDEs that do not have to harbor powerful jets. First, we investigate high-energy neutrino and gamma-ray production in the core region of a supermassive black hole. In particular, we show that about 1-100 TeV neutrinos and MeV gamma-rays can efficiently be produced in hot coronae around an accretion disk.Read More →

A unified picture of Galactic and cosmological fast radio bursts. (arXiv:2005.06736v4 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Lu_W/0/1/0/all/0/1">Wenbin Lu</a> (Caltech), <a href="http://arxiv.org/find/astro-ph/1/au:+Kumar_P/0/1/0/all/0/1">Pawan Kumar</a> (UT Austin), <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_B/0/1/0/all/0/1">Bing Zhang</a> (UNLV) The discovery of a fast radio burst (FRB) in our galaxy associated with a magnetar (neutron star with strong magnetic field) has provided a critical piece of information to help us finally understand these enigmatic transients. We show that the volumetric rate of Galactic-FRB like events is consistent with the faint end of the cosmological FRB rate, and hence they most likely belong to the same class of transients. The Galactic FRB had an accompanying X-ray burst but manyRead More →

Spectroscopy of binary black hole ringdown using overtones and angular modes. (arXiv:2005.03260v2 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Forteza_X/0/1/0/all/0/1">Xisco Jim&#xe9;nez Forteza</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Bhagwat_S/0/1/0/all/0/1">Swetha Bhagwat</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Pani_P/0/1/0/all/0/1">Paolo Pani</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Ferrari_V/0/1/0/all/0/1">Valeria Ferrari</a> The black hole uniqueness and the no-hair theorems imply that the quasinormal spectrum of any astrophysical black hole is determined solely by its mass and spin. The countably infinite number of quasinormal modes of a Kerr black hole are thus related to each other and any deviations from these relations provide a strong hint for physics beyond the general theory of relativity. To test the no-hair theorem using ringdown signals, it is necessary to detect at least twoRead More →

Data Analysis of Bright Main-Sequence A- and B-type Stars Observed Using the TESS and BRITE Spacecraft. (arXiv:2008.12661v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Guzik_J/0/1/0/all/0/1">Joyce A. Guzik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jackiewicz_J/0/1/0/all/0/1">Jason Jackiewicz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pigulski_A/0/1/0/all/0/1">Andrzej Pigulski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Catanzaro_G/0/1/0/all/0/1">Giovanni Catanzaro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Soukup_M/0/1/0/all/0/1">Michael S. Soukup</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gaulme_P/0/1/0/all/0/1">Patrick Gaulme</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Handler_G/0/1/0/all/0/1">Gerald Handler</a>, the <a href="http://arxiv.org/find/astro-ph/1/au:+Team_BRITE/0/1/0/all/0/1">BRITE Team</a> During the last two years we have received long time-series photometric observations of bright (V mag < 8) main-sequence A- and B-type stars observed by the NASA TESS spacecraft and the Austria-Poland-Canada BRITE satellites. Using TESS observations of metallic-line A (Am) stars having peculiar element abundances, our goal is to determine whether and why these stars pulsate in multiple radialRead More →

ALMA chemical survey of disk-outflow sources in Taurus (ALMA-DOT) II: Vertical stratification of CO, CS, CN, H2CO, and CH3OH in a Class I disk. (arXiv:2008.12648v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Podio_L/0/1/0/all/0/1">L. Podio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garufi_A/0/1/0/all/0/1">A. Garufi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Codella_C/0/1/0/all/0/1">C. Codella</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fedele_D/0/1/0/all/0/1">D. Fedele</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bianchi_E/0/1/0/all/0/1">E. Bianchi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bacciotti_F/0/1/0/all/0/1">F. Bacciotti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ceccarelli_C/0/1/0/all/0/1">C. Ceccarelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Favre_C/0/1/0/all/0/1">C. Favre</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mercimek_S/0/1/0/all/0/1">S. Mercimek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rygl_K/0/1/0/all/0/1">K. Rygl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Testi_L/0/1/0/all/0/1">L. Testi</a> The chemical composition of planets is inherited from the one of protoplanetary disks at the time of their formation. Increasing observational evidence suggests that planet formation occurs in less than $1-2$ Myr. This motivates the need for spatially resolved spectral observations of young Class I disks,Read More →

Cosmological simulations of quasar fueling to sub-parsec scales using Lagrangian hyper-refinement. (arXiv:2008.12303v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Angles_Alcazar_D/0/1/0/all/0/1">Daniel Angles-Alcazar</a> (1 and 2), <a href="http://arxiv.org/find/astro-ph/1/au:+Quataert_E/0/1/0/all/0/1">Eliot Quataert</a> (3 and 4), <a href="http://arxiv.org/find/astro-ph/1/au:+Hopkins_P/0/1/0/all/0/1">Philip Hopkins</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Somerville_R/0/1/0/all/0/1">Rachel Somerville</a> (2 and 6), <a href="http://arxiv.org/find/astro-ph/1/au:+Hayward_C/0/1/0/all/0/1">Christopher Hayward</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Faucher_Giguere_C/0/1/0/all/0/1">Claude-Andre Faucher-Giguere</a> (7), <a href="http://arxiv.org/find/astro-ph/1/au:+Bryan_G/0/1/0/all/0/1">Greg Bryan</a> (8 and 2), <a href="http://arxiv.org/find/astro-ph/1/au:+Keres_D/0/1/0/all/0/1">Dusan Keres</a> (9), <a href="http://arxiv.org/find/astro-ph/1/au:+Hernquist_L/0/1/0/all/0/1">Lars Hernquist</a> (10), <a href="http://arxiv.org/find/astro-ph/1/au:+Stone_J/0/1/0/all/0/1">James Stone</a> (11) ((1) UConn, (2) Flatiron, (3) Berkeley, (4) Princeton, (5) Caltech, (6) Rutgers, (7) Northwestern, (8) Columbia, (9) San Diego, (10) CfA, (11) IAS) We present cosmological hydrodynamic simulations of a quasar-mass halo ($M_{rm halo} approx 10^{12.5},{rm M}_{odot}$ at z=2) that for the first timeRead More →

Candidate Periodically Variable Quasars from the Dark Energy Survey and the Sloan Digital Sky Survey. (arXiv:2008.12329v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_Y/0/1/0/all/0/1">Yu-Ching Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_X/0/1/0/all/0/1">Xin Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liao_W/0/1/0/all/0/1">Wei-Ting Liao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Holgado_A/0/1/0/all/0/1">A. Miguel Holgado</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guo_H/0/1/0/all/0/1">Hengxiao Guo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gruendl_R/0/1/0/all/0/1">Robert A. Gruendl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Morganson_E/0/1/0/all/0/1">Eric Morganson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shen_Y/0/1/0/all/0/1">Yue Shen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_K/0/1/0/all/0/1">Kaiwen Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abbott_T/0/1/0/all/0/1">Tim M. C. Abbott</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aguena_M/0/1/0/all/0/1">Michel Aguena</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Allam_S/0/1/0/all/0/1">Sahar Allam</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Avila_S/0/1/0/all/0/1">Santiago Avila</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bertin_E/0/1/0/all/0/1">Emmanuel Bertin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bhargava_S/0/1/0/all/0/1">Sunayana Bhargava</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brooks_D/0/1/0/all/0/1">David Brooks</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burke_D/0/1/0/all/0/1">David L. Burke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rosell_A/0/1/0/all/0/1">Aurelio Carnero Rosell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carollo_D/0/1/0/all/0/1">Daniela Carollo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kind_M/0/1/0/all/0/1">Matias Carrasco Kind</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carretero_J/0/1/0/all/0/1">Jorge Carretero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Costanzi_M/0/1/0/all/0/1">Matteo Costanzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Costa_L/0/1/0/all/0/1">Luiz N. da Costa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Davis_T/0/1/0/all/0/1">Tamara M. Davis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vicente_J/0/1/0/all/0/1">Juan De Vicente</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Desai_S/0/1/0/all/0/1">ShantanuRead More →