RAS_WEB

Mass Estimation of Galaxy Clusters with Deep Learning II: CMB Cluster Lensing. (arXiv:2005.13985v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Gupta_N/0/1/0/all/0/1">N. Gupta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reichardt_C/0/1/0/all/0/1">C. L. Reichardt</a> We present a new application of deep learning to reconstruct the cosmic microwave background (CMB) temperature maps from the images of microwave sky, and to use these reconstructed maps to estimate the masses of galaxy clusters. We use a feed-forward deep learning network, mResUNet, for both steps of the analysis. The first deep learning model, mResUNet-I, is trained to reconstruct foreground and noise suppressed CMB maps from a set of simulated images of the microwave sky that include signals from the cosmic microwaveRead More →

“Direct” Gas-Phase Metallicity in Local Analogs of High-Redshift Galaxies: Empirical Metallicity Calibrations for High-Redshift Star-Forming Galaxies. (arXiv:1805.08224v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Bian_F/0/1/0/all/0/1">Fuyan Bian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kewley_L/0/1/0/all/0/1">Lisa J. Kewley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dopita_M/0/1/0/all/0/1">Michael A. Dopita</a> We study the direct gas-phase oxygen abundance using the well-detected auroral [OIII]4363 line in the stacked spectra of a sample of local analogs of high-redshift galaxies. These local analogs share the same location as $zsim2$ star-forming galaxies on the Baldwin-Phillips-Terlevich diagram. This type of analog has the same ionized interstellar medium (ISM) properties as high-redshift galaxies. We establish empirical metallicity calibrations between the direct gas-phase oxygen abundances ($7.8<12+log(rm{O/H})<8.4$) and the N2/O3N2 indices in our localRead More →

Detecting the radiative decay of the cosmic neutrino background with line-intensity mapping. (arXiv:2103.12099v2 [hep-ph] UPDATED) <a href="http://arxiv.org/find/hep-ph/1/au:+Bernal_J/0/1/0/all/0/1">Jos&#xe9; Luis Bernal</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Caputo_A/0/1/0/all/0/1">Andrea Caputo</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Villaescusa_Navarro_F/0/1/0/all/0/1">Francisco Villaescusa-Navarro</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Kamionkowski_M/0/1/0/all/0/1">Marc Kamionkowski</a> We study the possibility to use line-intensity mapping (LIM) to seek photons from the radiative decay of neutrinos in the cosmic neutrino background. The Standard Model prediction for the rate for these decays is extremely small, but it can be enhanced if new physics increases the neutrino electromagnetic moments. The decay photons will appear as an interloper of astrophysical spectral lines. We propose that the neutrino-decay line can be identified with anisotropies in LIM clustering and alsoRead More →

Detection of OH in the ultra-hot Jupiter WASP-76b. (arXiv:2110.11946v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Landman_R/0/1/0/all/0/1">Rico Landman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sanchez_Lopez_A/0/1/0/all/0/1">Alejandro S&#xe0;nchez-L&#xf3;pez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Molliere_P/0/1/0/all/0/1">Paul Molli&#xe8;re</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kesseli_A/0/1/0/all/0/1">Aurora Kesseli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Louca_A/0/1/0/all/0/1">Amy Louca</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Snellen_I/0/1/0/all/0/1">Ignas Snellen</a> Ultra-hot Jupiters have dayside temperatures at which most molecules are expected to thermally dissociate. The dissociation of water vapour results in the production of the hydroxyl radical (OH). While OH absorption is easily observed in near-infrared spectra of M dwarfs, which have similar effective temperatures as ultra-hot Jupiters, it is often not considered when studying the atmospheres of ultra-hot Jupiters. We use high-resolution spectroscopic observations of a transit of WASP-76b obtained using CARMENES to study the presenceRead More →

Evolution of accretion disc reflection spectra due to a Type I X-ray burst. (arXiv:2110.11931v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Speicher_J/0/1/0/all/0/1">J. Speicher</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Ballantyne_D/0/1/0/all/0/1">D. R. Ballantyne</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Fragile_P/0/1/0/all/0/1">P. C. Fragile</a> (2) ((1) Center for Relativistic Astrophysics, School of Physics, Georgia Institute of Technology, (2) Department of Physics &amp; Astronomy, College of Charleston) Irradiation of the accretion disc causes reflection signatures in the observed X-ray spectrum, encoding important information about the disc structure and density. A Type I X-ray burst will strongly irradiate the accretion disc and alter its properties. Previous numerical simulations predicted the evolution of the accretion disc due to an X-ray burst. Here, we processRead More →

A new perspective on cosmology through Supernovae Ia and Gamma Ray Bursts. (arXiv:2110.11930v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Simone_B/0/1/0/all/0/1">Biagio De Simone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nielson_V/0/1/0/all/0/1">Via Nielson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rinaldi_E/0/1/0/all/0/1">Enrico Rinaldi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dainotti_M/0/1/0/all/0/1">Maria Giovanna Dainotti</a> The actual knowledge of the structure and future evolution of our universe is based on the use of cosmological models, which can be tested through the so-called ‘probes’, namely astrophysical phenomena, objects or structures with peculiar properties that can help to discriminate among different cosmological models. Among all the existing probes, of particular importance are the Supernovae Ia (SNe Ia) and the Gamma Ray Bursts (GRBs): the former are considered among the best standard candles so farRead More →

SELCIE: A tool for investigating the chameleon field of arbitrary sources. (arXiv:2110.11917v1 [gr-qc]) <a href="http://arxiv.org/find/gr-qc/1/au:+Briddon_C/0/1/0/all/0/1">Chad Briddon</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Burrage_C/0/1/0/all/0/1">Clare Burrage</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Moss_A/0/1/0/all/0/1">Adam Moss</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Tamosiunas_A/0/1/0/all/0/1">Andrius Tamosiunas</a> The chameleon model is a modified gravity theory that introduces an additional scalar field that couples to matter through a conformal coupling. This `chameleon field’ possesses a screening mechanism through a nonlinear self-interaction term which allows the field to affect cosmological observables in diffuse environments whilst still being consistent with current local experimental constraints. Due to the self-interaction term the equations of motion of the field are nonlinear and therefore difficult to solve analytically. The analytic solutions that do existRead More →

Radio emission from colliding outflows in high-mass X-ray binaries with strongly magnetized neutron stars. (arXiv:2110.11906v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Chatzis_M/0/1/0/all/0/1">Margaritis Chatzis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Petropoulou_M/0/1/0/all/0/1">Maria Petropoulou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vasilopoulos_G/0/1/0/all/0/1">Georgios Vasilopoulos</a> We present a toy model for radio emission in HMXBs with strongly magnetized neutron stars (NS) where a wind-collision region is formed by the NS outflow and the stellar wind of the massive companion. Radio emission is expected from the synchrotron radiation of shock-accelerated electrons and the free-free emission of the stellar wind. We found that the predicted relation between the GHz luminosity ($L_R$) and the accretion X-ray luminosity ($L_X$) can be written as $L_R propto L_X^b$ for most parameters.Read More →

Black Hole Shadow in Symmergent Gravity. (arXiv:2110.11904v1 [gr-qc]) <a href="http://arxiv.org/find/gr-qc/1/au:+Cimdiker_I/0/1/0/all/0/1">&#x130;rfan &#xc7;imdiker</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Demir_D/0/1/0/all/0/1">Durmu&#x15f; Demir</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Ovgun_A/0/1/0/all/0/1">Ali &#xd6;vg&#xfc;n</a> Symmergent gravity is the $R+R^2$ gravity theory which emerges in a way restoring gauge symmetries broken explicitly by the ultraviolet cutoff in effective field theories. To test symmergent gravity we construct novel black hole solutions in four dimensions, and study their shadow in the vacuum as well as plasma medium. Our detailed analyses show that the horizon radius, Hawking temperature, Bekenstein-Hawking entropy, shadow angular radius, and photon deflection angle are sensitive probes of the symmergent gravity and particle spectrum of the underlying quantum field theory. Symmergent gravity isRead More →

Resolved simulations of jet-ISM interaction: Implications for gas dynamics and star formation. (arXiv:2110.11900v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Mukherjee_D/0/1/0/all/0/1">Dipanjan Mukherjee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bicknell_G/0/1/0/all/0/1">Geoffrey V. Bicknell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wagner_A/0/1/0/all/0/1">Alexander Y. Wagner</a> Relativistic jets can interact with the ambient gas distribution of the host galaxy, before breaking out to larger scales. In the past decade several studies have simulated jet-driven outflows to understand how they affect the nearby environment, and over what spatial and temporal scales such interactions occur. The simulations are able to capture the interaction of the jets with the turbulent clumpy interstellar medium and the resultant energetics of the gas. In this review we summarise the results of suchRead More →

Black Holes and Neutron Stars in an Oscillating Universe. (arXiv:2110.11897v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Gorkavyi_N/0/1/0/all/0/1">Nick Gorkavyi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tyulbashev_S/0/1/0/all/0/1">Sergei Tyul&#x27;bashev</a> One of the problems for the cyclic Universe will be its compatibility with a vast population of indestructible black holes that accumulate from cycle to cycle. The article considers a simple iterative model of the evolution of black holes in a cyclic Universe, independent of specific cosmological theories. The model has two free parameters that determine the iterative decrease in the number of black holes and the increase in their individual mass. It is shown that this model, with wide variations in the parameters, explains the observed numberRead More →

The Galactic metallicity gradient shown by open clusters in the light of radial migration. (arXiv:2110.11893v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Netopil_M/0/1/0/all/0/1">Martin Netopil</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oralhan_I/0/1/0/all/0/1">&#x130;nci Akkaya Oralhan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cakmak_H/0/1/0/all/0/1">Hikmet &#xc7;akmak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Michel_R/0/1/0/all/0/1">Ra&#xfa;l Michel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Karatas_Y/0/1/0/all/0/1">Y&#xfc;ksel Karata&#x15f;</a> During the last years and decades several individual studies and large-scale spectroscopic surveys significantly improved our knowledge of the Galactic metallicity distribution based on open clusters. The availability of Gaia data provided a further step forward in our knowledge. However, still some open issues remain, for example the influence of radial migration on the interpretation of the observed gradients. We used spectroscopic metallicities from individual studies and from the APOGEE survey to compileRead More →

Effect of dust in circumgalactic haloes on the cosmic shear power spectrum. (arXiv:2110.11892v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Silva_M/0/1/0/all/0/1">Makana Silva</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hirata_C/0/1/0/all/0/1">Christopher Hirata</a> Weak gravitational lensing is a powerful statistical tool for probing the growth of cosmic structure and measuring cosmological parameters. However, as shown by studies such as M’enard et al. (2010), dust in the circumgalactic region of haloes dims and reddens background sources. In a weak lensing analysis, this selects against sources behind overdense regions; since there is more structure in overdense regions, we will underestimate the amplitude of density perturbations $sigma_8$ if we do not correct for the effects of circumgalactic dust. To model theRead More →

Primordial neutrino asymmetry evolution with full mean-field effects and collisions. (arXiv:2110.11889v1 [hep-ph]) <a href="http://arxiv.org/find/hep-ph/1/au:+Froustey_J/0/1/0/all/0/1">Julien Froustey</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Pitrou_C/0/1/0/all/0/1">Cyril Pitrou</a> Neutrino oscillations and mean-field effects considerably enrich the phenomenology of neutrino evolution in the early Universe. Taking into account these effects, most notably the neutrino self-interaction mean-field contribution, we revisit the problem of the evolution of primordial neutrino asymmetries including for the first time the complete expression for collisions, which describe scattering and annihilations with electron/positrons and reactions among (anti)neutrinos. We show that a generalisation of the adiabatic transfer of averaged oscillations (ATAO) scheme, a numerical method previously developed without neutrino degeneracy and based on the largeRead More →

A novel fourth-order WENO interpolation technique. A possible new tool designed for radiative transfer. (arXiv:2110.11885v1 [math.NA]) <a href="http://arxiv.org/find/math/1/au:+Janett_G/0/1/0/all/0/1">Gioele Janett</a>, <a href="http://arxiv.org/find/math/1/au:+Steiner_O/0/1/0/all/0/1">Oskar Steiner</a>, <a href="http://arxiv.org/find/math/1/au:+Ballester_E/0/1/0/all/0/1">Ernest Alsina Ballester</a>, <a href="http://arxiv.org/find/math/1/au:+Belluzzi_L/0/1/0/all/0/1">Luca Belluzzi</a>, <a href="http://arxiv.org/find/math/1/au:+Mishra_S/0/1/0/all/0/1">Siddhartha Mishra</a> Context. Several numerical problems require the interpolation of discrete data that present various types of discontinuities. The radiative transfer is a typical example of such a problem. This calls for high-order well-behaved techniques to interpolate both smooth and discontinuous data. Aims. The final aim is to propose new techniques suitable for applications in the context of numerical radiative transfer. Methods. We have proposed and tested two different techniques. Essentially non-oscillatory (ENO) techniques generateRead More →

Sub-millimetre compactness as a critical dimension to understand the Main Sequence of star-forming galaxies. (arXiv:2103.12035v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Puglisi_A/0/1/0/all/0/1">Annagrazia Puglisi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Daddi_E/0/1/0/all/0/1">Emanuele Daddi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Valentino_F/0/1/0/all/0/1">Francesco Valentino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Magdis_G/0/1/0/all/0/1">Georgios Magdis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_D/0/1/0/all/0/1">Daizhong Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kokorev_V/0/1/0/all/0/1">Vasilii Kokorev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Circosta_C/0/1/0/all/0/1">Chiara Circosta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Elbaz_D/0/1/0/all/0/1">David Elbaz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bournaud_F/0/1/0/all/0/1">Frederic Bournaud</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gomez_Guijarro_C/0/1/0/all/0/1">Carlos Gomez-Guijarro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jin_S/0/1/0/all/0/1">Shuowen Jin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Madden_S/0/1/0/all/0/1">Suzanne Madden</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sargent_M/0/1/0/all/0/1">Mark T. Sargent</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Swinbank_M/0/1/0/all/0/1">Mark Swinbank</a> We study the interstellar medium (ISM) properties as a function of the molecular gas size for 77 infrared-selected galaxies at $z sim 1.3$. Molecular gas sizes are measured on ALMA images that combine CO(2-1), CO(5-4) and underlying continuum observations, and include CO(4-3), CO(7-6)+[CI]($^3 P_2-^3P_1$), [CI]($^3Read More →

Meridional Circulation of Dust and Gas in the Circumstellar Disk: Delivery of Solids onto the Circumplanetary Region. (arXiv:2103.12128v2 [astro-ph.EP] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Szulagyi_J/0/1/0/all/0/1">J. Szul&#xe1;gyi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Binkert_F/0/1/0/all/0/1">F. Binkert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Surville_C/0/1/0/all/0/1">C. Surville</a> We carried out 3D dust+gas radiative hydrodynamic simulations of forming planets. We investigated a parameter grid of Neptune-, Saturn-, Jupiter-, and 5 Jupiter-mass planets at 5.2, 30, 50 AU distance from their star. We found that the meridional circulation citep{Szulagyi14,FC16} drives a strong vertical flow for the dust as well, hence the dust is not settled in the midplane, even for mm-sized grains. The meridional circulation will deliver dust and gas vertically onto the circumplanetary region,Read More →

HI-H$_2$ transition: exploring the role of the magnetic field. (arXiv:2110.11878v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Skalidis_R/0/1/0/all/0/1">R. Skalidis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tassis_K/0/1/0/all/0/1">K. Tassis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Panopoulou_G/0/1/0/all/0/1">G. V. Panopoulou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pineda_J/0/1/0/all/0/1">J. L. Pineda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gong_Y/0/1/0/all/0/1">Y. Gong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mandarakas_N/0/1/0/all/0/1">N. Mandarakas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blinov_D/0/1/0/all/0/1">D. Blinov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kiehlmann_S/0/1/0/all/0/1">S. Kiehlmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kypriotakis_J/0/1/0/all/0/1">J. A. Kypriotakis</a> Atomic gas in the diffuse interstellar medium (ISM) is organized in filamentary structures. These structures usually host cold and dense molecular clumps. The Galactic magnetic field is considered to play an important role in the formation of these clumps. Our goal is to explore the role of the magnetic field in the HI – H$_{2}$ transition process. We targeted a filamentary cloud where gasRead More →

Primordial blackholes from Gauss-Bonnet-corrected single field inflation. (arXiv:2108.01340v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Kawai_S/0/1/0/all/0/1">Shinsuke Kawai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_J/0/1/0/all/0/1">Jinsu Kim</a> Primordial blackholes formed in the early Universe via gravitational collapse of over-dense regions may contribute a significant amount to the present dark matter relic density. Inflation provides a natural framework for the production mechanism of primordial blackholes. For example, single field inflation models with a fine-tuned scalar potential may exhibit a period of ultra-slow roll, during which the curvature perturbation may be enhanced to become seeds of the primordial blackholes formed as the corresponding scales reenter the horizon. In this work, we propose an alternative mechanism for the primordialRead More →

Simulations of neutrino and gamma-ray production from relativistic black-hole microquasar jets. (arXiv:2011.12939v1 [hep-ph] CROSS LISTED) <a href="http://arxiv.org/find/hep-ph/1/au:+Papavasileiou_T/0/1/0/all/0/1">Th. V. Papavasileiou</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Kosmas_O/0/1/0/all/0/1">O. T. Kosmas</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Sinatkas_J/0/1/0/all/0/1">J. Sinatkas</a> Recently, microquasar jets have aroused the interest of many researchers focusing on the astrophysical plasma outflows and various jet ejections. In this work, we concentrate on the investigation of electromagnetic radiation and particle emissions from the jets of stellar black hole binary systems characterized by their hadronic content in their jets. Such emissions are reliably described within the context of the relativistic magneto-hydrodynamics. Our model calculations are based on the Fermi acceleration mechanism through which the primary particles (mainlyRead More →