RAS_WEB (Page 3,784)

Hit or Miss, Arrival Time, and $B_z$ Orientation Predictions of BATS-R-US CME Simulations at 1 AU. (arXiv:1905.08961v1 [physics.space-ph]) <a href="http://arxiv.org/find/physics/1/au:+Schmidt_J/0/1/0/all/0/1">J. M. Schmidt</a>, <a href="http://arxiv.org/find/physics/1/au:+Cairns_I/0/1/0/all/0/1">Iver H. Cairns</a> Using a refined setup process, we simulated the propagation of six observed Coronal Mass Ejections (CMEs) with the 2012 Block-Adaptive-Tree-Solarwind-Roe-Upwind-Scheme (BATS-R-US) code from the Sun to the Earth or STEREO A and compared the outputs with observations. A linear relation between the average CME speed below 6 solar radii and the flux rope current is demonstrated and used to tune the simulations. The simulations correctly predict if and when an observable CME shock reaches one astronomical unit (AU). TheRead More →

GASP. XVI. Does cosmic web enhancement turn on star formation in galaxies?. (arXiv:1905.08971v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Vulcani_B/0/1/0/all/0/1">Benedetta Vulcani</a> (INAF-OaPD), <a href="http://arxiv.org/find/astro-ph/1/au:+Poggianti_B/0/1/0/all/0/1">Bianca M. Poggianti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moretti_A/0/1/0/all/0/1">Alessia Moretti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gullieuszik_M/0/1/0/all/0/1">Marco Gullieuszik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fritz_J/0/1/0/all/0/1">Jacopo Fritz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Franchetto_A/0/1/0/all/0/1">Andrea Franchetto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fasano_G/0/1/0/all/0/1">Giovanni Fasano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bettoni_D/0/1/0/all/0/1">Daniela Bettoni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jaffe_Y/0/1/0/all/0/1">Yara L. Jaffe</a> Galaxy filaments are a peculiar environment, and their impact on the galaxy properties is still controversial. Exploiting the data from the GAs Stripping Phenomena in galaxies with MUSE (GASP), we provide the first characterisation of the spatially resolved properties of galaxies embedded in filaments in the local Universe. The four galaxies we focus on show peculiar ionised gas distributions: Halpha cloudsRead More →

GASP XIX: AGN and their outflows at the center of jellyfish galaxies. (arXiv:1905.08972v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Radovich_M/0/1/0/all/0/1">Mario Radovich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Poggianti_B/0/1/0/all/0/1">Bianca Poggianti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jaffe_Y/0/1/0/all/0/1">Yara L. Jaffe&#x27;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moretti_A/0/1/0/all/0/1">Alessia Moretti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bettoni_D/0/1/0/all/0/1">Daniela Bettoni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gullieuszik_M/0/1/0/all/0/1">Marco Gullieuszik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vulcani_B/0/1/0/all/0/1">Benedetta Vulcani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fritz_J/0/1/0/all/0/1">Jacopo Fritz</a> The GASP survey, based on MUSE data, is unveiling the properties of the gas in the so-called “jellyfish” galaxies: these are cluster galaxies with spectacular evidence of gas stripping by ram pressure. In a previous paper, we selected the seven GASP galaxies with the most extended tentacles of ionized gas, and based on individual diagnostic diagrams concluded that at least five of them present clear evidenceRead More →

GASP XVIII: Star formation quenching due to AGN feedback in the central region of a jellyfish galaxy. (arXiv:1905.08973v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+George_K/0/1/0/all/0/1">Koshy George</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Poggianti_B/0/1/0/all/0/1">B. M. Poggianti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bellhouse_C/0/1/0/all/0/1">C. Bellhouse</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Radovich_M/0/1/0/all/0/1">M. Radovich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fritz_J/0/1/0/all/0/1">J. Fritz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Paladino_R/0/1/0/all/0/1">R. Paladino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bettoni_D/0/1/0/all/0/1">D. Bettoni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jaffe_Y/0/1/0/all/0/1">Y. Jaff&#xe9;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moretti_A/0/1/0/all/0/1">A. Moretti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gullieuszik_M/0/1/0/all/0/1">M. Gullieuszik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vulcani_B/0/1/0/all/0/1">B. Vulcani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fasano_G/0/1/0/all/0/1">G. Fasano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stalin_C/0/1/0/all/0/1">C. S. Stalin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Subramaniam_A/0/1/0/all/0/1">A. Subramaniam</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tandon_S/0/1/0/all/0/1">S.N. Tandon</a> We report evidence for star formation quenching in the central 8.6 kpc region of the jellyfish galaxy JO201 which hosts an active galactic nucleus, while undergoing strong ram pressure stripping. The ultraviolet imaging data of the galaxy disk revealRead More →

Chemical evolution of N2H+ in six massive star-forming regions. (arXiv:1905.08976v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Yu_N/0/1/0/all/0/1">Nai-Ping Yu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xu_J/0/1/0/all/0/1">Jin-Long Xu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_J/0/1/0/all/0/1">Jun-Jie Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_X/0/1/0/all/0/1">Xiao-Lan Liu</a> To investigate how the abundance of N2H+ varies as massive clumps evolve, here we present a multi-wavelength study toward six molecular clouds. All of these clouds contain several massive clumps in different evolutionary stages of star formation. Using archival data of Herschel InfraRed Galactic Plane Survey (Hi-GAL), we made H2 column density and dust temperature maps of these regions by the spectral energy distribution (SED) method. We found all of the six clouds show distinct dust temperature gradients, ranging from 20 KRead More →

Low-mass and High-mass Supermassive Blackholes In Radio-Loud AGNs Are Spun-up in Different Evolution Paths. (arXiv:1905.08978v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_J/0/1/0/all/0/1">J. Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kong_M/0/1/0/all/0/1">M. Z. Kong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_S/0/1/0/all/0/1">S. F. Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xu_D/0/1/0/all/0/1">D. W. Xu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_Q/0/1/0/all/0/1">Q. Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wei_J/0/1/0/all/0/1">J. Y. Wei</a> How Supermassive Blackholes (SMBHs) are spun-up is a key issue of modern astrophysics. As an extension of the study in Wang et al. (2016), we here address the issue by comparing the host galaxy properties of nearby ($z10^{7.9}M_odot$) have a preference for being spun-up in classical bulges, and low-mass SMBHs (i.e., $M_{mathrm{BH}}=10^{6-7}M_odot$) in pseudo-bulges. This dichotomy suggests and confirms that high-mass and low-mass SMBHs are spun-up inRead More →

Weak Lensing Measurement of Filamentary Structure with the SDSS BOSS and Subaru Hyper Suprime-Cam Data. (arXiv:1905.08991v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Kondo_H/0/1/0/all/0/1">Hiroto Kondo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Miyatake_H/0/1/0/all/0/1">Hironao Miyatake</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shirasaki_M/0/1/0/all/0/1">Masato Shirasaki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sugiyama_N/0/1/0/all/0/1">Naoshi Sugiyama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nishizawa_A/0/1/0/all/0/1">Atsushi J. Nishizawa</a> We report the weak lensing measurement of filaments between Sloan Digital Sky Survey (SDSS) III/Baryon Oscillation Spectroscopic Survey (BOSS) CMASS galaxy pairs at $zsim0.55$, using the Subaru Hyper Suprime-Cam (HSC) first-year galaxy shape catalogue. Despite of the small overlap of $140$ deg$^2$ between these surveys we detect the filament lensing signal at 3.9$sigma$ significance, which is the highest signal-to-noise lensing measurement of filaments between galaxy-scale halos at this redshift range. We deriveRead More →

Morphological diversity of spiral galaxies originating in the cold gas inflow from cosmic webs. (arXiv:1905.08993v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Noguchi_M/0/1/0/all/0/1">Masafumi Noguchi</a> Spiral galaxies comprise three major structural components; thin discs, thick discs, and central bulges. Relative dominance of these components is known to correlate with the total mass of the galaxy, and produces a remarkable morphological variety of spiral galaxies. Although there are many formation scenarios regarding individual components, no unified theory exists which explains this systematic variation. The cold-flow hypothesis predicts that galaxies grow by accretion of cold gas from cosmic webs (cold accretion) when their mass is below a certain threshold, whereas in the high-massRead More →

Comparison of Observed Galaxy Properties with Semianalytic Model Predictions using Machine Learning. (arXiv:1905.08996v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Simet_M/0/1/0/all/0/1">Melanie Simet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Soltani_N/0/1/0/all/0/1">Nima Chartab Soltani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lu_Y/0/1/0/all/0/1">Yu Lu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mobasher_B/0/1/0/all/0/1">Bahram Mobasher</a> With large-scale galaxy surveys, we can observe hundreds of thousands of galaxies or more, up to billions with upcoming experiments such as WFIRST, Euclid and LSST. While such surveys cannot obtain spectra for all observed galaxies, we have access to the galaxy magnitudes in color filters. This data set behaves like a high-dimensional nonlinear surface, making it an excellent target for machine learning methods. In this work, we use a lightcone of semianalytic galaxies tuned to match CANDELSRead More →

Comparing extrapolations of the coronal magnetic field structure at 2.5 solar radii with multi-viewpoint coronagraphic observations. (arXiv:1905.09005v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Sasso_C/0/1/0/all/0/1">C. Sasso</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pinto_R/0/1/0/all/0/1">R. F. Pinto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Andretta_V/0/1/0/all/0/1">V. Andretta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Howard_R/0/1/0/all/0/1">R. A. Howard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vourlidas_A/0/1/0/all/0/1">A. Vourlidas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bemporad_A/0/1/0/all/0/1">A. Bemporad</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dolei_S/0/1/0/all/0/1">S. Dolei</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Spadaro_D/0/1/0/all/0/1">D. Spadaro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Susino_R/0/1/0/all/0/1">R. Susino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Antonucci_E/0/1/0/all/0/1">E. Antonucci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abbo_L/0/1/0/all/0/1">L. Abbo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Deppo_V/0/1/0/all/0/1">V. Da Deppo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fineschi_S/0/1/0/all/0/1">S. Fineschi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Frassetto_F/0/1/0/all/0/1">F. Frassetto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Landini_F/0/1/0/all/0/1">F. Landini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Naletto_G/0/1/0/all/0/1">G. Naletto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nicolini_G/0/1/0/all/0/1">G. Nicolini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nicolosi_P/0/1/0/all/0/1">P. Nicolosi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pancrazzi_M/0/1/0/all/0/1">M. Pancrazzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Romoli_M/0/1/0/all/0/1">M. Romoli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Telloni_D/0/1/0/all/0/1">D. Telloni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ventura_R/0/1/0/all/0/1">R. Ventura</a> The magnetic field shapes the structure of the solar corona but we still know little about the interrelationshipsRead More →

Optical Counterparts of an Ultraluminous X-Ray Source X-1 in NGC 2500. (arXiv:1905.09020v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Aksaker_N/0/1/0/all/0/1">N. Aksaker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Akyuz_A/0/1/0/all/0/1">A. Aky&#xfc;z</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Avdan_S/0/1/0/all/0/1">S. Avdan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Avdan_H/0/1/0/all/0/1">H. Avdan</a> We present the results of a search for optical counterparts of ultraluminous X-ray source (ULX) X-1 in the nearby galaxy NGC 2500 by using archival images taken with the Hubble Space Telescope ({it HST}) Wide Field Camera (WFC3)/UVIS. Four optical sources have been identified as possible counterparts within the 2$sigma$ error radius of 0.3 arcsec in the images. However, only two of them were investigated as candidates for counterparts due to their point-like features and their identification in various filters.Read More →

AXS: A framework for fast astronomical data processing based on Apache Spark. (arXiv:1905.09034v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Zecevic_P/0/1/0/all/0/1">Petar Ze&#x10d;evi&#x107;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Slater_C/0/1/0/all/0/1">Colin T. Slater</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Juric_M/0/1/0/all/0/1">Mario Juri&#x107;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Connolly_A/0/1/0/all/0/1">Andrew J. Connolly</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Loncaric_S/0/1/0/all/0/1">Sven Lon&#x10d;ari&#x107;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bellm_E/0/1/0/all/0/1">Eric C. Bellm</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Golkhou_V/0/1/0/all/0/1">V. Zach Golkhou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Suberlack_K/0/1/0/all/0/1">Krzysztof Suberlack</a> We introduce AXS (Astronomy eXtensions for Spark), a scalable open-source astronomical data analysis framework built on Apache Spark, a widely used industry-standard engine for big data processing. Building on capabilities present in Spark, AXS aims to enable querying and analyzing almost arbitrarily large astronomical catalogs using familiar Python/AstroPy concepts, DataFrame APIs, and SQL statements. We achieve this by i) adding support to SparkRead More →

Transit least-squares survey – II. Discovery and validation of 17 new sub- to super-Earth-sized planets in multi-planet systems from K2. (arXiv:1905.09038v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Heller_R/0/1/0/all/0/1">Ren&#xe9; Heller</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Hippke_M/0/1/0/all/0/1">Michael Hippke</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Rodenbeck_K/0/1/0/all/0/1">Kai Rodenbeck</a> (3,1) ((1) Max Planck Institute for Solar System Research, G&#xf6;ttingen (GER), (2) Sonneberg Observatory (GER), (3) Institute for Astrophysics G&#xf6;ttingen, Georg August University G&#xf6;ttingen (GER)) The extended Kepler mission (K2) has revealed more than 500 transiting planets in roughly 500,000 stellar light curves. All of these were found either with the box least-squares algorithm or by visual inspection. Here we use our new transit least-squares (TLS) algorithm to search for additional planetsRead More →

Temperature stability in the sub-milliHertz band with LISA Pathfinder. (arXiv:1905.09060v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Armano_M/0/1/0/all/0/1">M. Armano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Audley_H/0/1/0/all/0/1">H. Audley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baird_J/0/1/0/all/0/1">J. Baird</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Binetruy_P/0/1/0/all/0/1">P. Binetruy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Born_M/0/1/0/all/0/1">M. Born</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bortoluzzi_D/0/1/0/all/0/1">D. Bortoluzzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Castelli_E/0/1/0/all/0/1">E. Castelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cavalleri_A/0/1/0/all/0/1">A. Cavalleri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cesarini_A/0/1/0/all/0/1">A. Cesarini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cruise_A/0/1/0/all/0/1">A. M. Cruise</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Danzmann_K/0/1/0/all/0/1">K. Danzmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Silva_M/0/1/0/all/0/1">M. de Deus Silva</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Diepholz_I/0/1/0/all/0/1">I. Diepholz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dixon_G/0/1/0/all/0/1">G. Dixon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dolesi_R/0/1/0/all/0/1">R. Dolesi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferraioli_L/0/1/0/all/0/1">L. Ferraioli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferroni_V/0/1/0/all/0/1">V. Ferroni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fitzsimons_E/0/1/0/all/0/1">E. D. Fitzsimons</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Freschi_M/0/1/0/all/0/1">M. Freschi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gesa_L/0/1/0/all/0/1">L. Gesa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gibert_F/0/1/0/all/0/1">F. Gibert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Giardini_D/0/1/0/all/0/1">D. Giardini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Giusteri_R/0/1/0/all/0/1">R. Giusteri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grimani_C/0/1/0/all/0/1">C. Grimani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grzymisch_J/0/1/0/all/0/1">J. Grzymisch</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Harrison_I/0/1/0/all/0/1">I. Harrison</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Heinzel_G/0/1/0/all/0/1">G. Heinzel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hewitson_M/0/1/0/all/0/1">M. Hewitson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hollington_D/0/1/0/all/0/1">D. Hollington</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hoyland_D/0/1/0/all/0/1">D. Hoyland</a>,Read More →

Wide Bandwidth Considerations for ALMA Band 2. (arXiv:1905.09064v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Mroczkowski_T/0/1/0/all/0/1">Tony Mroczkowski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Breuck_C/0/1/0/all/0/1">Carlos De Breuck</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kemper_C/0/1/0/all/0/1">Ciska Kemper</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Phillips_N/0/1/0/all/0/1">Neil Phillips</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fuller_G/0/1/0/all/0/1">Gary Fuller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beltran_M/0/1/0/all/0/1">Maite Beltr&#xe1;n</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Laing_R/0/1/0/all/0/1">Robert Laing</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marconi_G/0/1/0/all/0/1">Gianni Marconi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Testi_L/0/1/0/all/0/1">Leonardo Testi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yagoubov_P/0/1/0/all/0/1">Pavel Yagoubov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+George_D/0/1/0/all/0/1">Danielle George</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McGenn_W/0/1/0/all/0/1">William McGenn</a> One of the main considerations in the ALMA Development Roadmap for the future of operations beyond 2030 is to at least double its on-sky instantaneous bandwidth capabilities. Thanks to the technological innovations of the past two decades, we can now produce wider bandwidth receivers than were foreseen at the time of the original ALMA specifications. In several cases, theRead More →

VR CCD photometry of variable stars in globular cluster NGC 4147. (arXiv:1905.08249v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Lata_S/0/1/0/all/0/1">Sneh Lata</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pandey_A/0/1/0/all/0/1">A. K. Pandey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pandey_J/0/1/0/all/0/1">J. C. Pandey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yadav_R/0/1/0/all/0/1">R. K. S. Yadav</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pandey_S/0/1/0/all/0/1">Shashi B. Pandey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gupta_A/0/1/0/all/0/1">Aashish Gupta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bangia_T/0/1/0/all/0/1">Tarun Bangia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chand_H/0/1/0/all/0/1">Hum Chand</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jaiswar_M/0/1/0/all/0/1">Mukesh K. Jaiswar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Joshi_Y/0/1/0/all/0/1">Yogesh C. Joshi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Joshi_M/0/1/0/all/0/1">Mohit Joshi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kumar_B/0/1/0/all/0/1">Brijesh Kumar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kumar_T/0/1/0/all/0/1">T. S. Kumar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Medhi_B/0/1/0/all/0/1">Biman J. Medhi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Misra_K/0/1/0/all/0/1">Kuntal Misra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nanjappa_N/0/1/0/all/0/1">Nandish Nanjappa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pant_J/0/1/0/all/0/1">Jaysreekar Pant</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Purushottam/0/1/0/all/0/1">Purushottam</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reddy_B/0/1/0/all/0/1">B. Krishna Reddy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sahu_S/0/1/0/all/0/1">Sanjeet Sahu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sharma_S/0/1/0/all/0/1">Saurabh Sharma</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Uddin_W/0/1/0/all/0/1">Wahab Uddin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yadav_S/0/1/0/all/0/1">Shobhit Yadav</a> We present results of a search for variable stars in a region of theRead More →

Ultra High Energy Cosmic Rays and the Highest Energies Universe. (arXiv:1905.08250v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Aloisio_R/0/1/0/all/0/1">Roberto Aloisio</a> We will discuss the main relevant aspects of the physics of ultra high energy cosmic rays. After a short recap of the experimental evidences, we will review theoretical models aiming at describing the sources of these extremely energetic particles opening a window on the highest energies universe. We will discuss the production of secondary particles and the possible tests of new physics that ultra high energy cosmic rays could provide. We will discuss the main relevant aspects of the physics of ultra high energy cosmic rays. After a short recapRead More →

Deep into the structure of the first galaxies: SERRA views. (arXiv:1905.08254v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Pallottini_A/0/1/0/all/0/1">A. Pallottini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferrara_A/0/1/0/all/0/1">A. Ferrara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Decataldo_D/0/1/0/all/0/1">D Decataldo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gallerani_S/0/1/0/all/0/1">S. Gallerani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vallini_L/0/1/0/all/0/1">L. Vallini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carniani_S/0/1/0/all/0/1">S. Carniani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Behrens_C/0/1/0/all/0/1">C. Behrens</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kohandel_M/0/1/0/all/0/1">M. Kohandel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Salvadori_S/0/1/0/all/0/1">S. Salvadori</a> We study the formation and evolution of a sample of Lyman Break Galaxies in the Epoch of Reionization by using high-resolution ($sim 10 ,{rm pc}$), cosmological zoom-in simulations part of the SERRA suite. In SERRA, we follow the interstellar medium (ISM) thermo-chemical non-equilibrium evolution, and perform on-the-fly radiative transfer of the interstellar radiation field (ISRF). The simulation outputs are post-processed to compute the emission of farRead More →

Multiple Rings of Millimeter Dust Emission in the HD 15115 Debris Disk. (arXiv:1905.08258v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+MacGregor_M/0/1/0/all/0/1">Meredith A. MacGregor</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weinberger_A/0/1/0/all/0/1">Alycia J. Weinberger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nesvold_E/0/1/0/all/0/1">Erika R. Nesvold</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hughes_A/0/1/0/all/0/1">A. Meredith Hughes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wilner_D/0/1/0/all/0/1">D. J. Wilner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Currie_T/0/1/0/all/0/1">Thayne Currie</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Debes_J/0/1/0/all/0/1">John H. Debes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Donaldson_J/0/1/0/all/0/1">Jessica K. Donaldson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Redfield_S/0/1/0/all/0/1">Seth Redfield</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Roberge_A/0/1/0/all/0/1">Aki Roberge</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schneider_G/0/1/0/all/0/1">Glenn Schneider</a> We present observations of the HD 15115 debris disk from ALMA at 1.3 mm that capture this intriguing system with the highest resolution ($0.!!^{primeprime}6$ or $29$ AU) at millimeter wavelengths to date. This new ALMA image shows evidence for two rings in the disk separated by a cleared gap. By fittingRead More →