RAS_WEB (Page 2,430)

Modeling particle transport in astrophysical outflows and simulations of associated emissions. (arXiv:2101.02964v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Papadopoulos_D/0/1/0/all/0/1">D. A. Papadopoulos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kosmas_O/0/1/0/all/0/1">O. T. Kosmas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ganatsios_S/0/1/0/all/0/1">S. Ganatsios</a> In this work, after making an attempt to improve the formulation of the model on particle transport within astrophysical plasma outflows and constructing the appropriate algorithms, we test the reliability and effectiveness of our method through numerical simulations on well-studied Galactic microquasars as the SS 433 and the Cyg X-1 systems. Then, we concentrate on predictions of the associated emissions, focusing on detectable high energy neutrinos and $gamma$-rays originated from the extra-galactic M33 X-7 system, which is a recently discoveredRead More →

The Growth of Intracluster Light in XCS-HSC Galaxy Clusters from $0.1 < z < 0.5$. (arXiv:2101.01644v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Furnell_K/0/1/0/all/0/1">Kate E. Furnell</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Collins_C/0/1/0/all/0/1">Chris A. Collins</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Kelvin_L/0/1/0/all/0/1">Lee S. Kelvin</a> (1,2), <a href="http://arxiv.org/find/astro-ph/1/au:+Baldry_I/0/1/0/all/0/1">Ivan K. Baldry</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+James_P/0/1/0/all/0/1">Phil A. James</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Manolopoulou_M/0/1/0/all/0/1">Maria Manolopoulou</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Mann_R/0/1/0/all/0/1">Robert G. Mann</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Giles_P/0/1/0/all/0/1">Paul A. Giles</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Bermeo_A/0/1/0/all/0/1">Alberto Bermeo</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Hilton_M/0/1/0/all/0/1">Matthew Hilton</a> (5,6), <a href="http://arxiv.org/find/astro-ph/1/au:+Wilkinson_R/0/1/0/all/0/1">Reese Wilkinson</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Romer_A/0/1/0/all/0/1">A. Kathy Romer</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Vergara_C/0/1/0/all/0/1">Carlos Vergara</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Bhargava_S/0/1/0/all/0/1">Sunayana Bhargava</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Stott_J/0/1/0/all/0/1">John P. Stott</a> (7), <a href="http://arxiv.org/find/astro-ph/1/au:+Mayers_J/0/1/0/all/0/1">Julian Mayers</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Viana_P/0/1/0/all/0/1">Pedro Viana</a> (8,9) ((1) Astrophysics Research Institute, Liverpool John Moores University, (2) DepartmentRead More →

MUSCLE-UPS: Improved Approximations of the Matter Field with the Extended Press-Schechter Formalism and Lagrangian Perturbation Theory. (arXiv:2012.14446v3 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Tosone_F/0/1/0/all/0/1">Federico Tosone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Neyrinck_M/0/1/0/all/0/1">Mark C. Neyrinck</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Granett_B/0/1/0/all/0/1">Benjamin R. Granett</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guzzo_L/0/1/0/all/0/1">Luigi Guzzo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vittorio_N/0/1/0/all/0/1">Nicola Vittorio</a> Lagrangian algorithms to simulate the evolution of cold dark matter (CDM) are invaluable tools to generate large suites of mock halo catalogues. However, their precision may not be up to the challenge of upcoming surveys. In this paper, we first show that the main limitation of current schemes is their inability to model the evolution of overdensities in the initial density field, a limit that can be circumvented byRead More →

Effective temperatures of red supergiants estimated from line-depth ratios of iron lines in the YJ bands, 0.97–1.32 micron. (arXiv:2012.07856v2 [astro-ph.SR] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Taniguchi_D/0/1/0/all/0/1">Daisuke Taniguchi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matsunaga_N/0/1/0/all/0/1">Noriyuki Matsunaga</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jian_M/0/1/0/all/0/1">Mingjie Jian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kobayashi_N/0/1/0/all/0/1">Naoto Kobayashi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fukue_K/0/1/0/all/0/1">Kei Fukue</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hamano_S/0/1/0/all/0/1">Satoshi Hamano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ikeda_Y/0/1/0/all/0/1">Yuji Ikeda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kawakita_H/0/1/0/all/0/1">Hideyo Kawakita</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kondo_S/0/1/0/all/0/1">Sohei Kondo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Otsubo_S/0/1/0/all/0/1">Shogo Otsubo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sameshima_H/0/1/0/all/0/1">Hiroaki Sameshima</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Takenaka_K/0/1/0/all/0/1">Keiichi Takenaka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yasui_C/0/1/0/all/0/1">Chikako Yasui</a> Determining the effective temperatures (Teff) of red supergiants (RSGs) observationally is important in many fields of stellar physics and galactic astronomy, yet some significant difficulties remain due to model uncertainty originating majorly in the extended atmosphere of RSGs. Here we propose the line-depth ratio (LDR)Read More →

Internal water storage capacity of terrestrial planets and the effect of hydration on the M-R relation. (arXiv:2012.06455v3 [astro-ph.EP] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Shah_O/0/1/0/all/0/1">Oliver Shah</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alibert_Y/0/1/0/all/0/1">Yann Alibert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Helled_R/0/1/0/all/0/1">Ravit Helled</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mezger_K/0/1/0/all/0/1">Klaus Mezger</a> Understanding the chemical interactions between water and Mg-silicates or iron is essential to constrain the interiors of water-rich planets. Hydration effects have, however, been mostly neglected by the astrophysics community so far. As such effects are unlikely to have major impacts on theoretical mass-radius relations this is justified as long as the measurement uncertainties are large. However, upcoming missions, such as the PLATO mission (scheduled launch 2026), are envisaged to reach a precision ofRead More →

Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. I. Confirmation of an Eccentric, Cool Jupiter With an Interior Earth-sized Planet Orbiting Kepler-1514. (arXiv:2012.04676v2 [astro-ph.EP] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Dalba_P/0/1/0/all/0/1">Paul A. Dalba</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kane_S/0/1/0/all/0/1">Stephen R. Kane</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Isaacson_H/0/1/0/all/0/1">Howard Isaacson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Giacalone_S/0/1/0/all/0/1">Steven Giacalone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Howard_A/0/1/0/all/0/1">Andrew W. Howard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rodriguez_J/0/1/0/all/0/1">Joseph E. Rodriguez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vanderburg_A/0/1/0/all/0/1">Andrew Vanderburg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eastman_J/0/1/0/all/0/1">Jason D. Eastman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kraus_A/0/1/0/all/0/1">Adam L. Kraus</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dupuy_T/0/1/0/all/0/1">Trent J. Dupuy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weiss_L/0/1/0/all/0/1">Lauren M. Weiss</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schwieterman_E/0/1/0/all/0/1">Edward W. Schwieterman</a> Despite the severe bias of the transit method of exoplanet discovery toward short orbital periods, a modest sample of transiting exoplanets with orbital periods greater than 100 days is known. Long-term radial velocity (RV) surveysRead More →

Flavour specific neutrino self-interaction: $H_0$ tension and IceCube. (arXiv:2011.13685v2 [hep-ph] UPDATED) <a href="http://arxiv.org/find/hep-ph/1/au:+Mazumdar_A/0/1/0/all/0/1">Arindam Mazumdar</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Mohanty_S/0/1/0/all/0/1">Subhendra Mohanty</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Parashari_P/0/1/0/all/0/1">Priyank Parashari</a> Self-interaction in the active neutrinos is studied in the literature to alleviate the $H_0$ tension. Similar self-interaction can also explain the observed dips in the flux of the neutrinos coming from the distant astro-physical sources in IceCube detectors. In contrast to the flavour universal neutrino interaction considered for solving the $H_0$ tension, which is ruled out from particle physics experiments, we consider flavour specific neutrino interactions. We show that the values of self-interaction coupling constant and mediator mass required for explaining the IceCube dips areRead More →

Unusual chemistry of the C-H-N-O system under pressure and implications for giant planets. (arXiv:2011.12803v2 [cond-mat.mtrl-sci] UPDATED) <a href="http://arxiv.org/find/cond-mat/1/au:+Naumova_A/0/1/0/all/0/1">Anastasia S. Naumova</a>, <a href="http://arxiv.org/find/cond-mat/1/au:+Lepeshkin_S/0/1/0/all/0/1">Sergey V. Lepeshkin</a>, <a href="http://arxiv.org/find/cond-mat/1/au:+Bushlanov_P/0/1/0/all/0/1">Pavel V. Bushlanov</a>, <a href="http://arxiv.org/find/cond-mat/1/au:+Oganov_A/0/1/0/all/0/1">Artem R. Oganov</a> C-H-N-O system is central for organic chemistry and biochemistry, and plays a major role in planetary science (dominating the composition of “ice giants” Uranus and Neptune). The inexhaustible chemical diversity of this system at normal conditions explains it as the basis of all known life, but the chemistry of this system at high pressures and temperatures of planetary interiors is poorly known. Using ab initio evolutionary algorithm USPEX, we performed an extensive studyRead More →

Relevance of jet magnetic field structure for blazar axionlike particle searches. (arXiv:2011.08123v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Davies_J/0/1/0/all/0/1">James Davies</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meyer_M/0/1/0/all/0/1">Manuel Meyer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cotter_G/0/1/0/all/0/1">Garret Cotter</a> Many theories beyond the Standard Model of particle physics predict the existence of axionlike particles (ALPs) that mix with photons in the presence of a magnetic field. One prominent indirect method of searching for ALPs is to look for irregularities in blazar gamma-ray spectra caused by ALP-photon mixing in astrophysical magnetic fields. This requires the modelling of magnetic fields between Earth and the blazar. So far, only very simple models for the magnetic field in the blazar jet have been used. HereRead More →

Constraining the primordial black hole scenario with Bayesian inference and machine learning: the GWTC-2 gravitational wave catalog. (arXiv:2011.01865v2 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Wong_K/0/1/0/all/0/1">Kaze W. K. Wong</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Franciolini_G/0/1/0/all/0/1">Gabriele Franciolini</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Luca_V/0/1/0/all/0/1">Valerio De Luca</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Baibhav_V/0/1/0/all/0/1">Vishal Baibhav</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Berti_E/0/1/0/all/0/1">Emanuele Berti</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:+Riotto_A/0/1/0/all/0/1">Antonio Riotto</a> Primordial black holes (PBHs) might be formed in the early Universe and could comprise at least a fraction of the dark matter. Using the recently released GWTC-2 dataset from the third observing run of the LIGO-Virgo Collaboration, we investigate whether current observations are compatible with the hypothesis that all black hole mergers detected so far are of primordial origin. We constrainRead More →

Spins of primordial black holes formed in the radiation-dominated phase of the universe: first-order effect. (arXiv:2011.00710v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Harada_T/0/1/0/all/0/1">Tomohiro Harada</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yoo_C/0/1/0/all/0/1">Chul-Moon Yoo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kohri_K/0/1/0/all/0/1">Kazunori Kohri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koga_Y/0/1/0/all/0/1">Yasutaka Koga</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Monobe_T/0/1/0/all/0/1">Takeru Monobe</a> The standard deviation of the initial values of the nondimensional Kerr parameter $a_{*}$ of primordial black holes (PBHs) formed in the radiation-dominated phase of the universe is estimated to the first order of perturbation for the narrow power spectrum. Evaluating the angular momentum at turn around based on linearly extrapolated transfer functions and peak theory, we obtain the expression $sqrt{langle a_{*}^{2} rangle} simeq 4.0times 10^{-3} (M/M_{H})^{-1/3}sqrt{1-gamma^{2}}[1-0.072 log_{10}(beta_{0}(M_{H})/(1.3times 10^{-15}))]^{-1}$, where $M_{H}$, $beta_{0}(M_{H})$, andRead More →

Eccentricity evolution of compact binaries and applications to gravitational-wave physics. (arXiv:2010.15151v4 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Cardoso_V/0/1/0/all/0/1">Vitor Cardoso</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Macedo_C/0/1/0/all/0/1">Caio F. B. Macedo</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Vicente_R/0/1/0/all/0/1">Rodrigo Vicente</a> Searches for gravitational waves from compact binaries focus mostly on quasi-circular motion, with the rationale that wave emission circularizes the orbit. Here, we study the generality of this result, when astrophysical environments (e.g., accretion disks) or other fundamental interactions are taken into account. We are motivated by possible electromagnetic counterparts to binary black hole coalescences and orbits, but also by the possible use of eccentricity as a smoking-gun for new physics. We find that: i) backreaction from radiative mechanisms, including scalars,Read More →

Collider Signals of Baryogenesis and Dark Matter from $B$ Mesons: A Roadmap to Discovery. (arXiv:2101.02706v1 [hep-ph]) <a href="http://arxiv.org/find/hep-ph/1/au:+Alonso_Alvarez_G/0/1/0/all/0/1">Gonzalo Alonso-&#xc1;lvarez</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Elor_G/0/1/0/all/0/1">Gilly Elor</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Escudero_M/0/1/0/all/0/1">Miguel Escudero</a> Low-scale baryogenesis could be discovered at $B$-factories and the LHC. In the $B$-Mesogenesis paradigm, the CP violating oscillations and subsequent decays of $B$ mesons in the early Universe simultaneously explain the origin of the baryonic and the dark matter of the Universe. This mechanism for baryo- and dark matter-genesis from $B$ mesons gives rise to distinctive signals at collider experiments, which we scrutinize in this paper. We study CP violating observables in the $B^0_q-bar{B}_q^0$ system, discuss current and expected sensitivitiesRead More →

On the structure of Small Magellanic Cloud star clusters. (arXiv:2101.03157v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Piatti_A/0/1/0/all/0/1">Andr&#xe9;s E. Piatti</a> It has been recently shown from observational data sets the variation of structural parameters and internal dynamical evolution of star clusters in the Milky Way and in the Large Magellanic Cloud (LMC), caused by the different gravitational field strengths that they experience. We report here some hints for such a differential tidal effects in structural parameters of star clusters in the Small Magellanic Cloud (SMC), which is nearly 10 times less massive than the LMC. A key contribution to this study is the consideration of the SMC as a triaxialRead More →

Maximally self-interacting dark matter: models and predictions. (arXiv:2007.15522v2 [hep-ph] UPDATED) <a href="http://arxiv.org/find/hep-ph/1/au:+Kamada_A/0/1/0/all/0/1">Ayuki Kamada</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Kim_H/0/1/0/all/0/1">Hee Jung Kim</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Kuwahara_T/0/1/0/all/0/1">Takumi Kuwahara</a> We study self-interacting dark matter (SIDM) scenarios, where the $s$-wave self-scattering cross section almost saturates the Unitarity bound. Such self-scattering cross sections are singly parameterized by the dark matter mass, and are featured by strong velocity dependence in a wide range of velocities. They may be indicated by observations of dark matter halos in a wide range of masses, from Milky Way’s dwarf spheroidal galaxies to galaxy clusters. We pin down the model parameters that saturates the Unitarity bound in well-motivated SIDM models: the gaugedRead More →

Starspot evolution, Differential Rotation and Correlation between Chromospheric and Photospheric Activities on Kepler-411. (arXiv:2007.07158v5 [astro-ph.SR] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Xu_F/0/1/0/all/0/1">Fukun Xu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gu_S/0/1/0/all/0/1">Shenghong Gu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ioannidis_P/0/1/0/all/0/1">Panogiotis Ioannidis</a> We present an analysis of the starspot evolution, the surface differential rotation (SDR), the correlation between chromospheric activity indicators and the spatial connection between chromospheric and photospheric activities on the active star Kepler-411, using time series photometry over 4 years from Kepler, and spectroscopic data from Keck I 10-m telescope and Lijiang 2.4-m telescope. We constructed the light curve by re-performing photometry and reduction from the Target Pixel Files and Cotrending Basis Vectors with a manually redefined aperture using theRead More →

The Last Journey. I. An Extreme-Scale Simulation on the Mira Supercomputer. (arXiv:2006.01697v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Heitmann_K/0/1/0/all/0/1">Katrin Heitmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Frontiere_N/0/1/0/all/0/1">Nicholas Frontiere</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rangel_E/0/1/0/all/0/1">Esteban Rangel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Larsen_P/0/1/0/all/0/1">Patricia Larsen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pope_A/0/1/0/all/0/1">Adrian Pope</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sultan_I/0/1/0/all/0/1">Imran Sultan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Uram_T/0/1/0/all/0/1">Thomas Uram</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Habib_S/0/1/0/all/0/1">Salman Habib</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Finkel_H/0/1/0/all/0/1">Hal Finkel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Korytov_D/0/1/0/all/0/1">Danila Korytov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kovacs_E/0/1/0/all/0/1">Eve Kovacs</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rizzi_S/0/1/0/all/0/1">Silvio Rizzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Insley_J/0/1/0/all/0/1">Joe Insley</a> The Last Journey is a large-volume, gravity-only, cosmological N-body simulation evolving more than 1.24 trillion particles in a periodic box with a side-length of 5.025Gpc. It was implemented using the HACC simulation and analysis framework on the BG/Q system, Mira. The cosmological parameters are chosen to be consistent with the results fromRead More →

The Formation of Isolated Ultra-Diffuse Galaxies in Romulus25. (arXiv:2005.07634v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Wright_A/0/1/0/all/0/1">Anna C. Wright</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tremmel_M/0/1/0/all/0/1">Michael Tremmel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brooks_A/0/1/0/all/0/1">Alyson M. Brooks</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Munshi_F/0/1/0/all/0/1">Ferah Munshi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nagai_D/0/1/0/all/0/1">Daisuke Nagai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sharma_R/0/1/0/all/0/1">Ray S. Sharma</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Quinn_T/0/1/0/all/0/1">Thomas R. Quinn</a> We use the textsc{Romulus25} cosmological simulation volume to identify the largest-ever simulated sample of {it field} ultra-diffuse galaxies (UDGs). At $z=0$, we find that isolated UDGs have average star formation rates, colors, and virial masses for their stellar masses and environment. UDGs have moderately elevated HI masses, being 70% (300%) more HI-rich than typical isolated dwarf galaxies at luminosities brighter (fainter) than M$_mathrm{B}$=-14. However, UDGs are consistent with theRead More →