RAS_WEB (Page 2,843)

The variable radio counterpart of Swift J1858.6-0814. (arXiv:2006.06425v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Eijnden_J/0/1/0/all/0/1">J. van den Eijnden</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Degenaar_N/0/1/0/all/0/1">N. Degenaar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Russell_T/0/1/0/all/0/1">T. D. Russell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Buisson_D/0/1/0/all/0/1">D. J. K. Buisson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Altamirano_D/0/1/0/all/0/1">D. Altamirano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Padilla_M/0/1/0/all/0/1">M. Armas Padilla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bahramian_A/0/1/0/all/0/1">A. Bahramian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Segura_N/0/1/0/all/0/1">N. Castro Segura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fogantini_F/0/1/0/all/0/1">F. A. Fogantini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Heinke_C/0/1/0/all/0/1">C. O. Heinke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maccarone_T/0/1/0/all/0/1">T. Maccarone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maitra_D/0/1/0/all/0/1">D. Maitra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Miller_Jones_J/0/1/0/all/0/1">J. C. A. Miller-Jones</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Munoz_Darias_T/0/1/0/all/0/1">T. Mu&#xf1;oz-Darias</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arabaci_M/0/1/0/all/0/1">M. &#xd6;zbey Arabac&#x131;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Russell_D/0/1/0/all/0/1">D. M. Russell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shaw_A/0/1/0/all/0/1">A. W. Shaw</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sivakoff_G/0/1/0/all/0/1">G. Sivakoff</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tetarenko_A/0/1/0/all/0/1">A. J. Tetarenko</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vincentelli_F/0/1/0/all/0/1">F. Vincentelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wijnands_R/0/1/0/all/0/1">R. Wijnands</a> Swift J1858.6-0814 is a transient neutron star X-ray binary discovered in October 2018. Multi-wavelength follow-up observations across theRead More →

Coevolution of primitive methane cycling ecosystems and early Earth atmosphere and climate. (arXiv:2006.06433v1 [q-bio.PE]) <a href="http://arxiv.org/find/q-bio/1/au:+Sauterey_B/0/1/0/all/0/1">Boris Sauterey</a>, <a href="http://arxiv.org/find/q-bio/1/au:+Charnay_B/0/1/0/all/0/1">Benjamin Charnay</a>, <a href="http://arxiv.org/find/q-bio/1/au:+Affholder_A/0/1/0/all/0/1">Antonin Affholder</a>, <a href="http://arxiv.org/find/q-bio/1/au:+Mazevet_S/0/1/0/all/0/1">St&#xe9;phane Mazevet</a>, <a href="http://arxiv.org/find/q-bio/1/au:+Ferriere_R/0/1/0/all/0/1">R&#xe9;gis Ferri&#xe8;re</a> The history of the Earth has been marked by major ecological transitions, driven by metabolic innovation, that radically reshaped the composition of the oceans and atmosphere. The nature and magnitude of the earliest transitions, hundreds of million years before photosynthesis evolved, remain poorly understood. Using a novel ecosystem-planetary model, we find that pre-photosynthetic methane-cycling microbial ecosystems are much less productive than previously thought. In spite of their low productivity, the evolution of methanogenic metabolisms strongly modifiesRead More →

Promoted Mass Growth of Multiple, Distant Giant Planets through Pebble Accretion and Planet-Planet Collision. (arXiv:2006.06451v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Wimarsson_J/0/1/0/all/0/1">John Wimarsson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_B/0/1/0/all/0/1">Beibei Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ogihara_M/0/1/0/all/0/1">Masahiro Ogihara</a> We propose a pebble-driven planet formation scenario to form giant planets with high multiplicity and large orbital distances in the early gas disk phase. We perform N-body simulations to investigate the growth and migration of low-mass protoplanets in the disk with inner viscously heated and outer stellar irradiated regions. The key feature of this model is that the giant planet cores grow rapidly by a combination of pebble accretion and planet-planet collisions. This consequently speeds up their gas accretion. BecauseRead More →

Disforming the Kerr metric. (arXiv:2006.06461v1 [gr-qc]) <a href="http://arxiv.org/find/gr-qc/1/au:+Anson_T/0/1/0/all/0/1">Timothy Anson</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Babichev_E/0/1/0/all/0/1">Eugeny Babichev</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Charmousis_C/0/1/0/all/0/1">Christos Charmousis</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Hassaine_M/0/1/0/all/0/1">Mokhtar Hassaine</a> Starting from a recently constructed stealth Kerr solution of higher order scalar tensor theory involving scalar hair, we analytically construct disformal versions of the Kerr spacetime with a constant degree of disformality and a regular scalar field. While the disformed metric has only a ring singularity and asymptotically is quite similar to Kerr, it is found to be neither Ricci flat nor circular. Non-circularity has far reaching consequences on the structure of the solution. As we approach the rotating compact object from asymptotic infinity we find aRead More →

THESEUS$-$BTA cosmological tests using Multimessenger Gamma-Ray Bursts observations. (arXiv:2006.06488v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Shirokov_S/0/1/0/all/0/1">S. I. Shirokov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sokolov_I/0/1/0/all/0/1">I. V. Sokolov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vlasyuk_V/0/1/0/all/0/1">V. V. Vlasyuk</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amati_L/0/1/0/all/0/1">L. Amati</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sokolov_V/0/1/0/all/0/1">V. V. Sokolov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baryshev_Y/0/1/0/all/0/1">Yu. V. Baryshev</a> Modern Multimessenger Astronomy opens unique possibility for performing cosmological tests of the Standard Cosmological Model in the wide redshift interval up to $z sim 10$. This is principally important for recent discussion related to discrepancies between local and global measurements of cosmological parameters. We present a review of multimessenger Gamma-Ray Bursts observations currently performed and planed for THESEUS-BTA cooperative program. Such observations allow testing the fundamental basis of cosmological models: gravitation theory;Read More →

A Multiwavelength Study of the Massive Cool Core Cluste MACS J1447.4+0827. (arXiv:2006.04815v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Prasow_Emond_M/0/1/0/all/0/1">M. Prasow-&#xc9;mond</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hlavacek_Larrondo_J/0/1/0/all/0/1">J. Hlavacek-Larrondo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rhea_C/0/1/0/all/0/1">C. L. Rhea</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Latulippe_M/0/1/0/all/0/1">M. Latulippe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gendron_Marsolais_M/0/1/0/all/0/1">M.-L. Gendron-Marsolais</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Richard_Laferriere_A/0/1/0/all/0/1">A. Richard-Laferri&#xe8;re</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sanders_J/0/1/0/all/0/1">J. S. Sanders</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Edge_A/0/1/0/all/0/1">A. C. Edge</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Allen_S/0/1/0/all/0/1">S. W. Allen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mantz_A/0/1/0/all/0/1">A. Mantz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Linden_A/0/1/0/all/0/1">A. von der Linden</a> Clusters of galaxies are outstanding laboratories for understanding the physics of supermassive black hole feedback. Here, we present the first textit{Chandra}, Karl G. Janksy Very Large Array and textit{Hubble Space Telescope} analysis of MACS J1447.4+0827 ($z = 0.3755$), one of the strongest cool core clusters known, in which extreme feedback from its centralRead More →

Exploring the small mass ratio binary black hole merger via Zeno’s dichotomy approach. (arXiv:2006.04818v1 [gr-qc]) <a href="http://arxiv.org/find/gr-qc/1/au:+Lousto_C/0/1/0/all/0/1">Carlos O. Lousto</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Healy_J/0/1/0/all/0/1">James Healy</a> We perform a sequence of binary black hole simulations with increasingly small mass ratios, reaching a 128:1 binary that displays 13 orbits before merger. Based on a detailed convergence study of the $q=m_1/m_2=1/15$ nonspinning case, we apply additional mesh refinements levels on the smaller hole horizon to reach the $q=1/32$, $q=1/64$, and $q=1/128$ cases. Roughly linear strong computational scaling with $1/q$ is observed on 8-nodes simulations. We compute the remnant properties of the merger; final mass, spin, and recoil velocity. We also computeRead More →

Testing viscous disc theory using the balance between stellar accretion and external photoevaporation of protoplanetary discs. (arXiv:2006.04819v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Winter_A/0/1/0/all/0/1">Andrew J. Winter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ansdell_M/0/1/0/all/0/1">Megan Ansdell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Haworth_T/0/1/0/all/0/1">Thomas J. Haworth</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kruijssen_J/0/1/0/all/0/1">J. M. Diederik Kruijssen</a> The nature and rate of (viscous) angular momentum transport in protoplanetary discs (PPDs) has important consequences for the formation process of planetary systems. While accretion rates onto the central star yield constraints on such transport in the inner regions of a PPD, empirical constraints on viscous spreading in the outer regions remain challenging to obtain. Here we demonstrate a novel method to probe the angular momentum transport at the outer edgeRead More →

BBN constraints on universally-coupled ultralight scalar dark matter. (arXiv:2006.04820v1 [hep-ph]) <a href="http://arxiv.org/find/hep-ph/1/au:+Sibiryakov_S/0/1/0/all/0/1">Sergey Sibiryakov</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Sorensen_P/0/1/0/all/0/1">Philip S&#xf8;rensen</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Yu_T/0/1/0/all/0/1">Tien-Tien Yu</a> Ultralight scalar dark matter can interact with all massive Standard Model particles through a universal coupling. Such a coupling modifies the Standard Model particle masses and affects the dynamics of Big Bang Nucleosynthesis. We model the cosmological evolution of the dark matter, taking into account the modifications of the scalar mass by the environment as well as the full dynamics of Big Bang Nucleosynthesis. We find that precision measurements of the helium-4 abundance set stringent constraints on the available parameter space, and that these constraints areRead More →

Sensitivity forecasts for the cosmological recombination radiation in the presence of foregrounds. (arXiv:2006.04826v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Hart_L/0/1/0/all/0/1">Luke Hart</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rotti_A/0/1/0/all/0/1">Aditya Rotti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chluba_J/0/1/0/all/0/1">Jens Chluba</a> The cosmological recombination radiation (CRR) is one of the inevitable $Lambda$CDM spectral distortions of the cosmic microwave background (CMB). While it shows a rich spectral structure across dm-mm wavelengths, it is also one of the smallest signals to target. Here we carry out a detailed forecast for the expected sensitivity levels required to not only detect but also extract cosmological information from the CRR in the presence of foregrounds. We use ${tt CosmoSpec}$ to compute the CRR including all important radiative transferRead More →

The Role of Outflows, Radiation Pressure, and Magnetic Fields in Massive Star Formation. (arXiv:2006.04829v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Rosen_A/0/1/0/all/0/1">Anna L. Rosen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Krumholz_M/0/1/0/all/0/1">Mark R. Krumholz</a> Stellar feedback in the form of radiation pressure and magnetically-driven collimated outflows may limit the maximum mass that a star can achieve and affect the star-formation efficiency of massive pre-stellar cores. Here we present a series of 3D adaptive mesh refinement radiation-magnetohydrodynamic simulations of the collapse of initially turbulent, massive pre-stellar cores. Our simulations include radiative feedback from both the direct stellar and dust-reprocessed radiation fields, and collimated outflow feedback from the accreting stars. We find that protostellar outflows punches holes inRead More →

Stochastic re-acceleration and magnetic-field damping in Tycho’s supernova remnant. (arXiv:2006.04832v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Wilhelm_A/0/1/0/all/0/1">A. Wilhelm</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Telezhinsky_I/0/1/0/all/0/1">I. Telezhinsky</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dwarkadas_V/0/1/0/all/0/1">V.V. Dwarkadas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pohl_M/0/1/0/all/0/1">M. Pohl</a> A number of studies suggest that shock acceleration with particle feedback and very efficient magnetic-field amplification combined with Alfv'{e}nic drift are needed to explain the rather soft radio spectrum and the narrow rims observed for Tycho’s SNR. We show that the broadband spectrum of Tycho’s SNR can alternatively be well explained when accounting for stochastic acceleration as a secondary process. The re-acceleration of particles in the turbulent region immediately downstream of the shock should be efficient enough to impact particle spectra overRead More →

Constraining the Rapid Neutron-Capture Process with Meteoritic I-129 and Cm-247. (arXiv:2006.04833v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Cote_B/0/1/0/all/0/1">Benoit C&#xf4;t&#xe9;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eichler_M/0/1/0/all/0/1">Marius Eichler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yague_A/0/1/0/all/0/1">Andr&#xe9;s Yag&#xfc;e</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vassh_N/0/1/0/all/0/1">Nicole Vassh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mumpower_M/0/1/0/all/0/1">Matthew R. Mumpower</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vilagos_B/0/1/0/all/0/1">Blanka Vil&#xe1;gos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Soos_B/0/1/0/all/0/1">Benj&#xe1;min So&#xf3;s</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arcones_A/0/1/0/all/0/1">Almudena Arcones</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sprouse_T/0/1/0/all/0/1">Trevor M. Sprouse</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Surman_R/0/1/0/all/0/1">Rebecca Surman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pignatari_M/0/1/0/all/0/1">Marco Pignatari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wehmeyer_B/0/1/0/all/0/1">Benjamin Wehmeyer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rauscher_T/0/1/0/all/0/1">Thomas Rauscher</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lugaro_M/0/1/0/all/0/1">Maria Lugaro</a> Meteoritic analysis demonstrates that radioactive nuclei heavier than iron were present in the early Solar System. Among them, $^{129}$I and $^{247}$Cm both have a rapid neutron-capture process ($r$ process) origin and decay on the same timescale ($simeq$ 15.6 Myr). We show that the $^{129}$I/$^{247}$Cm abundance ratio in the earlyRead More →

The ALPINE-ALMA [C II] Survey: [C II]158micron Emission Line Luminosity Functions at $z sim 4-6$. (arXiv:2006.04835v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Yan_L/0/1/0/all/0/1">Lin Yan</a> (Caltech), <a href="http://arxiv.org/find/astro-ph/1/au:+Sajina_A/0/1/0/all/0/1">A. Sajina</a> (Tufts University), <a href="http://arxiv.org/find/astro-ph/1/au:+Loiacono_F/0/1/0/all/0/1">F. Loiacono</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lagache_G/0/1/0/all/0/1">G. Lagache</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bethermin_M/0/1/0/all/0/1">M. B&#xe8;thermin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Faisst_A/0/1/0/all/0/1">A. Faisst</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ginolfi_M/0/1/0/all/0/1">M. Ginolfi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fevre_O/0/1/0/all/0/1">O. Le F&#xe8;vre</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gruppioni_C/0/1/0/all/0/1">C. Gruppioni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Capak_P/0/1/0/all/0/1">P.L. Capak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cassata_P/0/1/0/all/0/1">P. Cassata</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schaerer_D/0/1/0/all/0/1">D. Schaerer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Silverman_J/0/1/0/all/0/1">J.D. Silverman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bardelli_S/0/1/0/all/0/1">S. Bardelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dessauges_Zavadsky_M/0/1/0/all/0/1">M. Dessauges-Zavadsky</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cimatti_A/0/1/0/all/0/1">A. Cimatti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hathi_N/0/1/0/all/0/1">N.P. Hathi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lemaux_B/0/1/0/all/0/1">B.C. Lemaux</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ibar_E/0/1/0/all/0/1">E. Ibar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jones_G/0/1/0/all/0/1">G.C. Jones</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koekemoer_A/0/1/0/all/0/1">A.M. Koekemoer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oesch_P/0/1/0/all/0/1">P.A. Oesch</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Talia_M/0/1/0/all/0/1">M. Talia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pozzi_F/0/1/0/all/0/1">F. Pozzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Riechers_D/0/1/0/all/0/1">D.A. Riechers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tasca_L/0/1/0/all/0/1">L.A. Tasca</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Toft_S/0/1/0/all/0/1">S. Toft</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vallini_L/0/1/0/all/0/1">L. Vallini</a>,Read More →

The ALPINE-ALMA [C II] survey: the luminosity function of serendipitous [C II] line emitters at $zsim 5$. (arXiv:2006.04837v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Loiacono_F/0/1/0/all/0/1">Federica Loiacono</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Decarli_R/0/1/0/all/0/1">Roberto Decarli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gruppioni_C/0/1/0/all/0/1">Carlotta Gruppioni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Talia_M/0/1/0/all/0/1">Margherita Talia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cimatti_A/0/1/0/all/0/1">Andrea Cimatti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zamorani_G/0/1/0/all/0/1">Gianni Zamorani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pozzi_F/0/1/0/all/0/1">Francesca Pozzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yan_L/0/1/0/all/0/1">Lin Yan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lemaux_B/0/1/0/all/0/1">Brian C. Lemaux</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Riechers_D/0/1/0/all/0/1">Dominik A. Riechers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fevre_O/0/1/0/all/0/1">Olivier Le F&#xe8;vre</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bethermin_M/0/1/0/all/0/1">Matthieu B&#xe9;thermin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Capak_P/0/1/0/all/0/1">Peter Capak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cassata_P/0/1/0/all/0/1">Paolo Cassata</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Faisst_A/0/1/0/all/0/1">Andreas Faisst</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schaerer_D/0/1/0/all/0/1">Daniel Schaerer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Silverman_J/0/1/0/all/0/1">John D. Silverman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bardelli_S/0/1/0/all/0/1">Sandro Bardelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boquien_M/0/1/0/all/0/1">M&#xe9;d&#xe9;ric Boquien</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burkutean_S/0/1/0/all/0/1">Sandra Burkutean</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dessauges_Zavadsky_M/0/1/0/all/0/1">Miroslava Dessauges-Zavadsky</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fudamoto_Y/0/1/0/all/0/1">Yoshinobu Fudamoto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fujimoto_S/0/1/0/all/0/1">Seiji Fujimoto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ginolfi_M/0/1/0/all/0/1">Michele Ginolfi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hathi_N/0/1/0/all/0/1">Nimish P. Hathi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jones_G/0/1/0/all/0/1">Gareth C. Jones</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Khusanova_Y/0/1/0/all/0/1">YanaRead More →

Wide and Deep Exploration of Radio Galaxies with Subaru HSC (WERGS). III. Discovery of a z = 4.72 Radio Galaxy with Lyman Break Technique. (arXiv:2006.04844v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Yamashita_T/0/1/0/all/0/1">Takuji Yamashita</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nagao_T/0/1/0/all/0/1">Tohru Nagao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ikeda_H/0/1/0/all/0/1">Hiroyuki Ikeda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Toba_Y/0/1/0/all/0/1">Yoshiki Toba</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kajisawa_M/0/1/0/all/0/1">Masaru Kajisawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ono_Y/0/1/0/all/0/1">Yoshiaki Ono</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tanaka_M/0/1/0/all/0/1">Masayuki Tanaka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Akiyama_M/0/1/0/all/0/1">Masayuki Akiyama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Harikane_Y/0/1/0/all/0/1">Yuichi Harikane</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ichikawa_K/0/1/0/all/0/1">Kohei Ichikawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kawaguchi_T/0/1/0/all/0/1">Toshihiro Kawaguchi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kawamuro_T/0/1/0/all/0/1">Taiki Kawamuro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kohno_K/0/1/0/all/0/1">Kotaro Kohno</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_C/0/1/0/all/0/1">Chien-Hsiu Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_K/0/1/0/all/0/1">Kianhong Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matsuoka_Y/0/1/0/all/0/1">Yoshiki Matsuoka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Niida_M/0/1/0/all/0/1">Mana Niida</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ogura_K/0/1/0/all/0/1">Kazuyuki Ogura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Onoue_M/0/1/0/all/0/1">Masafusa Onoue</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Uchiyama_H/0/1/0/all/0/1">Hisakazu Uchiyama</a> We report a discovery of $z = 4.72$ radio galaxy, HSC J083913.17+011308.1, by using the Lyman break technique withRead More →

Interstellar medium properties and feedback in local AGN with the MAGNUM survey. (arXiv:2006.04850v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Mingozzi_M/0/1/0/all/0/1">M. Mingozzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cresci_G/0/1/0/all/0/1">G. Cresci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Venturi_G/0/1/0/all/0/1">G. Venturi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marconi_A/0/1/0/all/0/1">A. Marconi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mannucci_F/0/1/0/all/0/1">F. Mannucci</a> We investigated the interstellar medium (ISM) properties in the central regions of nearby Seyfert galaxies characterised by prominent conical or bi-conical outflows belonging to the MAGNUM survey by exploiting the unprecedented sensitivity, spatial and spectral coverage of the integral field spectrograph MUSE at the Very Large Telescope. We developed a novel approach based on the gas and stars kinematics to disentangle high-velocity gas in the outflow from gas in the disc to spatially track the differencesRead More →

A radiatively-quiet glitch and anti-glitch in the magnetar 1E 2259+586. (arXiv:2006.04854v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Younes_G/0/1/0/all/0/1">G. Younes</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Ray_P/0/1/0/all/0/1">P. S. Ray</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Baring_M/0/1/0/all/0/1">M. G. Baring</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Kouveliotou_C/0/1/0/all/0/1">C. Kouveliotou</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Fletcher_C/0/1/0/all/0/1">C. Fletcher</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Wadiasingh_Z/0/1/0/all/0/1">Z. Wadiasingh</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Harding_A/0/1/0/all/0/1">A. K. Harding</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Goldstein_A/0/1/0/all/0/1">A. Goldstein</a> (4) ((1) George Washington University, (2) Naval Research Lab, (3) Rice University, (4) USRA/NASA/MSFC, (5) NASA/GSFC) We report on the timing and spectral properties of the soft X-ray emission from the magnetar 1E 2259+586 from January 2013, $sim 8$ months after the detection of an anti-glitch, until September 2019, using the Neil Gehrels Swift and NICER observatories. During thisRead More →

Mineral dust increases the habitability of terrestrial planets but confounds biomarker detection. (arXiv:2006.04867v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Boutle_I/0/1/0/all/0/1">Ian A. Boutle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Joshi_M/0/1/0/all/0/1">Manoj Joshi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lambert_F/0/1/0/all/0/1">F. Hugo Lambert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mayne_N/0/1/0/all/0/1">Nathan J. Mayne</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lyster_D/0/1/0/all/0/1">Duncan Lyster</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Manners_J/0/1/0/all/0/1">James Manners</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ridgway_R/0/1/0/all/0/1">Robert Ridgway</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kohary_K/0/1/0/all/0/1">Krisztian Kohary</a> Identification of habitable planets beyond our solar system is a key goal of current and future space missions. Yet habitability depends not only on the stellar irradiance, but equally on constituent parts of the planetary atmosphere. Here we show, for the first time, that radiatively active mineral dust will have a significant impact on the habitability of Earth-like exoplanets. On tidally-locked planets, dust coolsRead More →