RAS_WEB (Page 4,570)

The Galaxy Stellar Mass Function and Low Surface Brightness Galaxies from Core-Collapse Supernovae. (arXiv:1901.05020v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Sedgwick_T/0/1/0/all/0/1">Thomas M. Sedgwick</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baldry_I/0/1/0/all/0/1">Ivan K. Baldry</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+James_P/0/1/0/all/0/1">Philip A. James</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kelvin_L/0/1/0/all/0/1">Lee S. Kelvin</a> We introduce a method for producing a galaxy sample unbiased by surface brightness and stellar mass, by selecting star-forming galaxies via the positions of core-collapse supernovae (CCSNe). Whilst matching $sim$2400 supernovae from the SDSS-II Supernova Survey to their host galaxies using IAC Stripe 82 legacy coadded imaging, we find $sim$150 previously unidentified low surface brightness galaxies (LSBGs). Using a sub-sample of $sim$900 CCSNe, we infer CCSN-rate and star-formation rate densities as a function ofRead More →

Revealing the dust grain size in the inner envelope of the Class I protostar Per-emb-50. (arXiv:1901.05021v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Agurto_Gangas_C/0/1/0/all/0/1">C. Agurto-Gangas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pineda_J/0/1/0/all/0/1">J.E. Pineda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Szucs_L/0/1/0/all/0/1">L. Szucs</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Testi_L/0/1/0/all/0/1">L. Testi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tazzari_M/0/1/0/all/0/1">M. Tazzari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Miotello_A/0/1/0/all/0/1">A. Miotello</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caselli_P/0/1/0/all/0/1">P. Caselli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dunham_M/0/1/0/all/0/1">M. Dunham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stephens_I/0/1/0/all/0/1">I.W. Stephens</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bourke_T/0/1/0/all/0/1">T.L. Bourke</a> A good constraint of when the growth of dust grains from sub-micrometer to millimeter sizes occurs, is crucial for planet formation models. This provides the first step towards the production of pebbles and planetesimals in protoplanetary disks. Currently, it is well established that Class II objects have large dust grains. However, it is not clear when in theRead More →

Resolved young binary systems and their disks. (arXiv:1901.05029v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Akeson_R/0/1/0/all/0/1">Rachel L. Akeson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jensen_E/0/1/0/all/0/1">Eric L. N. Jensen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carpenter_J/0/1/0/all/0/1">John Carpenter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ricci_L/0/1/0/all/0/1">Luca Ricci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Laos_S/0/1/0/all/0/1">Stefan Laos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nogueira_N/0/1/0/all/0/1">Natasha F. Nogueira</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Suen_Lewis_E/0/1/0/all/0/1">Emma M. Suen-Lewis</a> We have conducted a survey of young single and multiple systems in the Taurus-Auriga star-forming region with the Atacama Large Millimeter Array (ALMA), substantially improving both the spatial resolution and sensitivity with which individual protoplanetary disks in these systems have been observed. These ALMA observations can resolve binary separations as small as 25–30 AU and have an average 3$sigma$ detection level of 0.35 mJy, equivalent to a disk mass ofRead More →

Constraining Type Ia Supernova Asymmetry with the Gamma Ray Escape Timescale. (arXiv:1901.05057v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Levanon_N/0/1/0/all/0/1">Naveh Levanon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Soker_N/0/1/0/all/0/1">Noam Soker</a> (Technion, Israel) We calculate the effects of an asymmetric $^{56}mathrm{Ni}$ distribution in Type Ia supernova (SN Ia) ejecta on the late light curve ($>40$ days after peak) using the gamma ray escape timescale ($t_0$) and find it is modest compared to other possible variations in ejecta structure. We parameterize asymmetry in the $^{56}mathrm{Ni}$ distribution and calculate $t_0$ for a grid of SN ejecta models spanning a large volume of the asymmetry parameter space. The models have spherical density profiles while the $^{56}mathrm{Ni}$ distribution in them hasRead More →

Intermediate-Mass Black Holes in binary-rich star clusters. (arXiv:1901.05063v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Subr_L/0/1/0/all/0/1">L. Subr</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fragione_G/0/1/0/all/0/1">G. Fragione</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dabringhausen_J/0/1/0/all/0/1">J. Dabringhausen</a> There is both theoretical expectation and some observational clues that intermediate mass black holes reside in nuclei of globular clusters. In order to find an independent indicator for their existence, we investigate in this paper how an IMBH manifests itself through its dynamical interaction with a binary rich globular cluster of moderate extension and mass. By means of direct $N$-body integration we follow the dynamical evolution of models of such a system over a time span of $approx$ 0.8 Gyr and compare the cases with and withoutRead More →

The Population of Eccentric Binary Black Holes: Implications for mHz Gravitational Wave Experiments. (arXiv:1901.05092v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Fang_X/0/1/0/all/0/1">Xiao Fang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Thompson_T/0/1/0/all/0/1">Todd A. Thompson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hirata_C/0/1/0/all/0/1">Christopher M. Hirata</a> The observed binary black hole (BBH) mergers indicate a large Galactic progenitor population continuously evolving from large orbital separations and low gravitational wave (GW) frequencies to the final merger phase. We investigate the equilibrium distribution of binary black holes in the Galaxy. Given the observed BBH merger rate, we contrast the expected number of systems radiating in the low-frequency $0.1-10,$mHz GW band under two assumptions: (1) that all merging systems originate from near-circular orbits, as may be indicative ofRead More →

Discovery of Standstills in the SU UMa-Type Dwarf Nova NY Serpentis. (arXiv:1901.05100v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Kato_T/0/1/0/all/0/1">Taichi Kato</a> (Kyoto U), <a href="http://arxiv.org/find/astro-ph/1/au:+Pavlenko_E/0/1/0/all/0/1">Elena P. Pavlenko</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pit_N/0/1/0/all/0/1">Nikolaj V. Pit</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Antonyuk_K/0/1/0/all/0/1">Kirill A. Antonyuk</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Antonyuk_O/0/1/0/all/0/1">Oksana I. Antonyuk</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Babina_J/0/1/0/all/0/1">Julia V. Babina</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baklanov_A/0/1/0/all/0/1">Aleksei V. Baklanov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sosnovskij_A/0/1/0/all/0/1">Aleksei A. Sosnovskij</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Belan_S/0/1/0/all/0/1">Sergey P. Belan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maeda_Y/0/1/0/all/0/1">Yutaka Maeda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sugiura_Y/0/1/0/all/0/1">Yuki Sugiura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sumiya_S/0/1/0/all/0/1">Sho Sumiya</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matsumoto_H/0/1/0/all/0/1">Hanami Matsumoto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ito_D/0/1/0/all/0/1">Daiki Ito</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nikai_K/0/1/0/all/0/1">Kengo Nikai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kojiguchi_N/0/1/0/all/0/1">Naoto Kojiguchi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matsumoto_K/0/1/0/all/0/1">Katsura Matsumoto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dubovsky_P/0/1/0/all/0/1">Pavol A. Dubovsky</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kudzej_I/0/1/0/all/0/1">Igor Kudzej</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Medulka_T/0/1/0/all/0/1">Tomas Medulka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wakamatsu_Y/0/1/0/all/0/1">Yasuyuki Wakamatsu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ohnishi_R/0/1/0/all/0/1">Ryuhei Ohnishi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Seki_T/0/1/0/all/0/1">Takaaki Seki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Isogai_K/0/1/0/all/0/1">Keisuke Isogai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Simon_A/0/1/0/all/0/1">Andrii O. Simon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Romanjuk_Y/0/1/0/all/0/1">Yaroslav O. Romanjuk</a>, <aRead More →

AutoRegressive Planet Search: Methodology. (arXiv:1901.05116v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Caceres_G/0/1/0/all/0/1">Gabriel A. Caceres</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Feigelson_E/0/1/0/all/0/1">Eric D. Feigelson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Babu_G/0/1/0/all/0/1">G. Jogesh Babu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bahamonde_N/0/1/0/all/0/1">Natalia Bahamonde</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Christen_A/0/1/0/all/0/1">Alejandra Christen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bertin_K/0/1/0/all/0/1">Karine Bertin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meza_C/0/1/0/all/0/1">Cristian Meza</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cure_M/0/1/0/all/0/1">Michel Cur&#xe9;</a> The detection of periodic signals from transiting exoplanets is often impeded by extraneous aperiodic photometric variability, either intrinsic to the star or arising from the measurement process. Frequently, these variations are autocorrelated wherein later flux values are correlated with previous ones. In this work, we present the methodology of the Autoregessive Planet Search (ARPS) project which uses Autoregressive Integrated Moving Average (ARIMA) and related statistical models that treat a wide variety ofRead More →

SDSS-IV MaNGA: Inside-out vs. outside-in quenching in different local environments. (arXiv:1901.05126v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Lin_L/0/1/0/all/0/1">Lihwai Lin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hsieh_B/0/1/0/all/0/1">Bau-Ching Hsieh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pan_H/0/1/0/all/0/1">Hsi-An Pan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rembold_S/0/1/0/all/0/1">Sandro B. Rembold</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sanchez_S/0/1/0/all/0/1">Sebasti&#xe1;n F. S&#xe1;nchez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Argudo_Fernandez_M/0/1/0/all/0/1">Maria Argudo-Fern&#xe1;ndez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rowlands_K/0/1/0/all/0/1">Kate Rowlands</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Belfiore_F/0/1/0/all/0/1">Francesco Belfiore</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bizyaev_D/0/1/0/all/0/1">Dmitry Bizyaev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lacerna_I/0/1/0/all/0/1">Ivan Lacerna</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Riffel_R/0/1/0/all/0/1">Rogr&#xe9;io Riffel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rong_Y/0/1/0/all/0/1">Yu Rong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yuan_F/0/1/0/all/0/1">Fangting Yuan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Drory_N/0/1/0/all/0/1">Niv Drory</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maiolino_R/0/1/0/all/0/1">Roberto Maiolino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wilcots_E/0/1/0/all/0/1">Eric Wilcots</a> The large Integral Field Spectroscopy (IFS) surveys have allowed the classification of ionizing sources of emission lines on sub-kpc scales. In this work, we define two non-parametric parameters, quiescence (f$_{q}$) and its concentration (c$_{q}$), to quantify the strength and the spatial distribution ofRead More →

Models of a protoplanetary disk forming in-situ the Galilean \ and smaller nearby satellites before Jupiter is fully formed. (arXiv:1901.05131v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Christodoulou_D/0/1/0/all/0/1">D. M. Christodoulou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kazanas_D/0/1/0/all/0/1">D. Kazanas</a> We fit an isothermal oscillatory density model of Jupiter’s protoplanetary disk to the present-day Galilean and other nearby satellites and we determine the radial scale length of the disk, the equation of state and the central density of the primordial gas, and the rotational state of the Jovian nebula. Although the radial density profile of Jupiter’s disk was similar to that of the solar nebula, its rotational support against self-gravity was very low, a property that alsoRead More →

Black Holes as Cosmic Dynamos. (arXiv:1901.05164v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Blandford_R/0/1/0/all/0/1">Roger Blandford</a> An introduction is given to a meeting on the role of massive and stellar black holes in powering non-thermal activity in a rich variety of cosmic sources. Relevant properties of magnetized, spinning black holes are summarized and their observational expression, within galactic nuclei, in terms of radio loudness and Fanaroff-Riley class, is briefly described. The dependence of the accretion mode on the rate and manner of the mass supply beyond the black hole sphere of influence is also discussed. It is argued that hydromagnetic outflows from accretion disks are generally expected over as many asRead More →

Possibility Of Condensation Of Glycine Near The Surface Of Comet 67P/Churyumov-Gerasimenko. (arXiv:1901.05170v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Suzuki_T/0/1/0/all/0/1">Taiki Suzuki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shinnaka_Y/0/1/0/all/0/1">Yoshiharu Shinnaka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shibata_T/0/1/0/all/0/1">Takashi Shibata</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shibaike_Y/0/1/0/all/0/1">Yuhito Shibaike</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Majumdar_L/0/1/0/all/0/1">Liton Majumdar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nomura_H/0/1/0/all/0/1">Hideko Nomura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Minamoto_H/0/1/0/all/0/1">Harumi Minamoto</a> The cometary materials are thought to be the reservoir of primitive materials in the solar system. The recent detection of glycine and CH$_3$NH$_2$ by the ROSINA mass spectrometer in the coma of 67P/Churyumov-Gerasimenko suggests that amino acids and their precursors have been formed in such an early evolutionary phase of the Solar System. We use our chemical modeling for low-mass star-forming regions to investigate if we can explain observed “Glycine/CH$_3$NH$_2$” ratio.Read More →

The CARMENES search for exoplanets around M dwarfs. Period search in H$alpha$, Na I D, and Ca II IRT lines. (arXiv:1901.05173v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Fuhrmeister_B/0/1/0/all/0/1">B. Fuhrmeister</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Czesla_S/0/1/0/all/0/1">S. Czesla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schmitt_J/0/1/0/all/0/1">J. H. M. M. Schmitt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Johnson_E/0/1/0/all/0/1">E. N. Johnson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schofer_P/0/1/0/all/0/1">P. Sch&#xf6;fer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jeffers_S/0/1/0/all/0/1">S. V. Jeffers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caballero_J/0/1/0/all/0/1">J. A. Caballero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zechmeister_M/0/1/0/all/0/1">M. Zechmeister</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reiners_A/0/1/0/all/0/1">A. Reiners</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ribas_I/0/1/0/all/0/1">I. Ribas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amado_P/0/1/0/all/0/1">P. J. Amado</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Quirrenbach_A/0/1/0/all/0/1">A. Quirrenbach</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bauer_F/0/1/0/all/0/1">F. Bauer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bechar_V/0/1/0/all/0/1">V. J. S. B&#xe9;char</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cortes_Contreras_M/0/1/0/all/0/1">M. Cort&#xe9;s-Contreras</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alonso_E/0/1/0/all/0/1">E. D&#xed;ez Alonso</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dreizler_S/0/1/0/all/0/1">S. Dreizler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Galadi_Enriquez_D/0/1/0/all/0/1">D. Galad&#xed;-Enr&#xed;quez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guenther_E/0/1/0/all/0/1">E. W. Guenther</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kaminski_A/0/1/0/all/0/1">A. Kaminski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kurster_M/0/1/0/all/0/1">M. K&#xfc;rster</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lafarga_M/0/1/0/all/0/1">M. Lafarga</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Montes_D/0/1/0/all/0/1">D. Montes</a> We use spectraRead More →

Bar Fraction in Early- and Late-type Spirals. (arXiv:1901.05183v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_Y/0/1/0/all/0/1">Yun Hee Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ann_H/0/1/0/all/0/1">Hong Bae Ann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Park_M/0/1/0/all/0/1">Myeong-Gu Park</a> Bar fractions depend on the properties of the host galaxies, which are closely related to the formation and evolution of bars. However, observational studies do not provide consistent results. We investigate the bar fraction and its dependence on the properties of the host galaxies by using three bar classification methods: visual inspection, ellipse fitting method, and Fourier analysis. Our volume-limited sample consists of 1,698 spiral galaxies brighter than $M_{rm r}=-15.2$ with $z < 0.01$ from SDSS/DR7 visually classified by Ann et al. (2015). We firstRead More →

Local simulations of MRI turbulence with meshless methods. (arXiv:1901.05190v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Deng_H/0/1/0/all/0/1">Hongping Deng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mayer_L/0/1/0/all/0/1">Lucio Mayer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Latter_H/0/1/0/all/0/1">Henrik Latter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hopkins_P/0/1/0/all/0/1">Philip F. Hopkins</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bai_X/0/1/0/all/0/1">Xue-Ning Bai</a> The magneto-rotational instability (MRI) is one of the most important processes in sufficiently ionized astrophysical disks. Grid-based simulations, especially those using the local shearing box approximation, provide a powerful tool to study the ensuing nonlinear turbulence. On the other hand, while meshless methods have been widely used in both cosmology, galactic dynamics, and planet formation they have not been fully deployed on the MRI problem. We present local unstratified and vertically stratified MRI simulations with two meshless MHD schemes:Read More →

Recent insights on the penumbra formation process. (arXiv:1901.05207v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Murabito_M/0/1/0/all/0/1">M. Murabito</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Romano_P/0/1/0/all/0/1">P.Romano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zuccarello_F/0/1/0/all/0/1">F. Zuccarello</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guglielmino_S/0/1/0/all/0/1">S.L.Guglielmino</a> Using high-resolution spectropolarimetric data acquired by textit{IBIS}, as well as textit{SDO}/HMI observations, we studied the penumbra formation in AR NOAA 11490 and in a sample of twelve ARs appeared on the solar disk on 2011 and 2012, which were characterized by $beta$-type magnetic field configuration. The results show that the onset of the classical Evershed flow occurs in a very short time scale, 1-3 hours. Studying the formation of the first penumbral sector around the following proto-spot, we found that a stable penumbra forms in theRead More →

The 2014 TeV Gamma-ray Flare of Mrk 501 Seen with H.E.S.S.: Temporal and Spectral Constraints on Lorentz Invariance Violation. (arXiv:1901.05209v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Collaboration_H%2E_E%2E_S%2E_S%2E/0/1/0/all/0/1">H.E.S.S. Collaboration</a>: <a href="http://arxiv.org/find/astro-ph/1/au:+Abdalla_H/0/1/0/all/0/1">H. Abdalla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aharonian_F/0/1/0/all/0/1">F. Aharonian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Benkhali_F/0/1/0/all/0/1">F. Ait Benkhali</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anguner_E/0/1/0/all/0/1">E. O. Ang&#xfc;ner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arakawa_M/0/1/0/all/0/1">M. Arakawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arcaro_C/0/1/0/all/0/1">C. Arcaro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Armand_C/0/1/0/all/0/1">C. Armand</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arrieta_M/0/1/0/all/0/1">M. Arrieta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Backes_M/0/1/0/all/0/1">M. Backes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barnard_M/0/1/0/all/0/1">M. Barnard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Becherini_Y/0/1/0/all/0/1">Y. Becherini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tjus_J/0/1/0/all/0/1">J. Becker Tjus</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berge_D/0/1/0/all/0/1">D. Berge</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bernhard_S/0/1/0/all/0/1">S. Bernhard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bernlohr_K/0/1/0/all/0/1">K. Bernl&#xf6;hr</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blackwell_R/0/1/0/all/0/1">R. Blackwell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bottcher_M/0/1/0/all/0/1">M. B&#xf6;ttcher</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boisson_C/0/1/0/all/0/1">C. Boisson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bolmont_J/0/1/0/all/0/1">J. Bolmont</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bonnefoy_S/0/1/0/all/0/1">S. Bonnefoy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bordas_P/0/1/0/all/0/1">P. Bordas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bregeon_J/0/1/0/all/0/1">J. Bregeon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brun_F/0/1/0/all/0/1">F. Brun</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brun_P/0/1/0/all/0/1">P. Brun</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bryan_M/0/1/0/all/0/1">M. Bryan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Buchele_M/0/1/0/all/0/1">M. B&#xfc;chele</a>,Read More →

Multi-phase Circum-Galactic Medium probed with MUSE and ALMA. (arXiv:1901.05217v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Peroux_C/0/1/0/all/0/1">Celine Peroux</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Zwaan_M/0/1/0/all/0/1">Martin Zwaan</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Klitsch_A/0/1/0/all/0/1">Anne Klitsch</a> (2,3), <a href="http://arxiv.org/find/astro-ph/1/au:+Augustin_R/0/1/0/all/0/1">Ramona Augustin</a> (1,2), <a href="http://arxiv.org/find/astro-ph/1/au:+Hamanowicz_A/0/1/0/all/0/1">Aleksandra Hamanowicz</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Rahmani_H/0/1/0/all/0/1">Hadi Rahmani</a> (1,4), <a href="http://arxiv.org/find/astro-ph/1/au:+Pettini_M/0/1/0/all/0/1">Max Pettini</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Kulkarni_V/0/1/0/all/0/1">Varsha Kulkarni</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Straka_L/0/1/0/all/0/1">Lorrie Straka</a> (7), <a href="http://arxiv.org/find/astro-ph/1/au:+Biggs_A/0/1/0/all/0/1">Andy Biggs</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+York_D/0/1/0/all/0/1">Donald York</a> (8), <a href="http://arxiv.org/find/astro-ph/1/au:+Milliard_B/0/1/0/all/0/1">Bruno Milliard</a> (1) ((1) Laboratoire d&#x27;Astrophysique de Marseille, France (2) European Southern Observatory, Germany (3) Durham University, UK (4) GEPI, Observatoire de Paris, France (5) IoA, Cambridge, UK (6) University of South Carolina, USA (7) Leiden University, the Netherlands (8) University of Chicago, USA) Galaxy halos appear to be missingRead More →