RAS_WEB (Page 4,385)

ALMA twenty-six arcmin$^2$ survey of GOODS-S at one-millimeter (ASAGAO): Near-infrared-dark faint ALMA sources. (arXiv:1903.02744v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Yamaguchi_Y/0/1/0/all/0/1">Yuki Yamaguchi</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:+Hatsukade_B/0/1/0/all/0/1">Bunyo Hatsukade</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_T/0/1/0/all/0/1">Tao Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yoshimura_Y/0/1/0/all/0/1">Yuki Yoshimura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ao_Y/0/1/0/all/0/1">Yiping Ao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caputi_K/0/1/0/all/0/1">Karina I. Caputi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dunlop_J/0/1/0/all/0/1">James S. Dunlop</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Egami_E/0/1/0/all/0/1">Eiichi Egami</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Espada_D/0/1/0/all/0/1">Daniel Espada</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:+Hayatsu_N/0/1/0/all/0/1">Natsuki H. Hayatsu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ivison_R/0/1/0/all/0/1">Rob J. Ivison</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kodama_T/0/1/0/all/0/1">Tadayuki Kodama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kusakabe_H/0/1/0/all/0/1">Haruka Kusakabe</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:+Ouchi_M/0/1/0/all/0/1">Masami Ouchi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rujopakarn_W/0/1/0/all/0/1">Wiphu Rujopakarn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tadaki_K/0/1/0/all/0/1">Ken-ichi Tadaki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tamura_Y/0/1/0/all/0/1">Yoichi Tamura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ueda_Y/0/1/0/all/0/1">Yoshihiro Ueda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Umehata_H/0/1/0/all/0/1">Hideki Umehata</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_W/0/1/0/all/0/1">Wei-Hao Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yun_M/0/1/0/all/0/1">Min S. Yun</a> We report detections of two 1.2 mm continuum sources ($S_mathrm{1.2mm}$ ~ 0.6 mJy)Read More →

The PLATO Solar-like Light-curve Simulator: A tool to generate realistic stellar light-curves with instrumental effects representative of the PLATO mission. (arXiv:1903.02747v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Samadi_R/0/1/0/all/0/1">R. Samadi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Deru_A/0/1/0/all/0/1">A. Deru</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reese_D/0/1/0/all/0/1">D. Reese</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marchiori_V/0/1/0/all/0/1">V. Marchiori</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grolleau_E/0/1/0/all/0/1">E. Grolleau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Green_J/0/1/0/all/0/1">J.J. Green</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pertenais_M/0/1/0/all/0/1">M. Pertenais</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lebreton_Y/0/1/0/all/0/1">Y. Lebreton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Deheuvels_S/0/1/0/all/0/1">S. Deheuvels</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mosser_B/0/1/0/all/0/1">B. Mosser</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Belkacem_K/0/1/0/all/0/1">K. Belkacem</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Borner_A/0/1/0/all/0/1">A. Borner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smith_A/0/1/0/all/0/1">A. M. S. Smith</a> The preparation of science objectives of the ESA’s PLATO space mission will require the implementation of hare-and-hound exercises relying on the massive generation of representative simulated light-curves. We developed a light-curve simulator named the PLATO Solar-like Light-curve Simulator (PSLS) in order toRead More →

Origin of Cosmic Ray Electrons and Positrons. (arXiv:1903.02756v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Zhao_Dong_S/0/1/0/all/0/1">Shi Zhao-Dong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Siming_L/0/1/0/all/0/1">Liu Siming</a> With experimental results of AMS on the spectra of cosmic ray (CR) $e^{-}$, $e^{+}$, $e^{-}+e^{+}$ and positron fraction, as well as new measurements of CR $e^{-}+e^{+}$ flux by HESS, one can better understand the CR lepton ($e^{-}$ and $e^{+}$) spectra and the puzzling electron-positron excess above $sim$10 GeV. In this article, spectra of CR $e^{-}$ and $e^{+}$ are fitted with a physically motivated simple model, and their injection spectra are obtained with a one-dimensional propagation model including the diffusion and energy loss processes. Our results show that the electron-positron excessRead More →

Recovering the Star Formation History of IC 1613 Dwarf Galaxy Using Evolved Stars. (arXiv:1903.02767v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Hashemi_S/0/1/0/all/0/1">Seyed Azim Hashemi</a> (Sharif University), <a href="http://arxiv.org/find/astro-ph/1/au:+Javadi_A/0/1/0/all/0/1">Atefeh Javadi</a> (IPM), <a href="http://arxiv.org/find/astro-ph/1/au:+Loon_J/0/1/0/all/0/1">Jacco van Loon</a> (Keele University) Determining the star formation history (SFH) is key to understand the formation and evolution of dwarf galaxies. Recovering the SFH in resolved galaxies is mostly based on deep colour–magnitude diagrams (CMDs), which trace the signatures of multiple evolutionary stages of their stellar populations. In distant and unresolved galaxies, the integrated light of the galaxy can be decomposed, albeit made difficult by an age–metallicity degeneracy. Another solution to determine the SFH of resolved galaxies isRead More →

PRIME: Psf Reconstruction and Identification for Multiple sources characterization Enhancement. Application to Keck NIRC2 imager. (arXiv:1903.02772v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Beltramo_Martin_O/0/1/0/all/0/1">O. Beltramo-Martin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Correia_C/0/1/0/all/0/1">C.M. Correia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ragland_S/0/1/0/all/0/1">S. Ragland</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jolissaint_L/0/1/0/all/0/1">L. Jolissaint</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Neichel_B/0/1/0/all/0/1">B. Neichel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fusco_T/0/1/0/all/0/1">T. Fusco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wizinowich_P/0/1/0/all/0/1">P.L. Wizinowich</a> In order to enhance accuracy of astrophysical estimates obtained on Adaptive-optics (AO) images, such as photometry and astrometry, we investigate a new concept to constrain the Point Spread Function (PSF) model called PSF Reconstruction and Identification for Multi-sources characterization Enhancement (PRIME), that handles jointly the science image and the AO control loop data. We present in this paper the concept of PRIME and validate it on KeckRead More →

Tests of General Relativity and Fundamental Physics with Space-based Gravitational Wave Detectors. (arXiv:1903.02781v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Berti_E/0/1/0/all/0/1">Emanuele Berti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barausse_E/0/1/0/all/0/1">Enrico Barausse</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cholis_I/0/1/0/all/0/1">Ilias Cholis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garcia_Bellido_J/0/1/0/all/0/1">Juan Garcia-Bellido</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Holley_Bockelmann_K/0/1/0/all/0/1">Kelly Holley-Bockelmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hughes_S/0/1/0/all/0/1">Scott A. Hughes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kelly_B/0/1/0/all/0/1">Bernard Kelly</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kovetz_E/0/1/0/all/0/1">Ely D. Kovetz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Littenberg_T/0/1/0/all/0/1">Tyson B. Littenberg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Livas_J/0/1/0/all/0/1">Jeffrey Livas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mueller_G/0/1/0/all/0/1">Guido Mueller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Natarajan_P/0/1/0/all/0/1">Priya Natarajan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shoemaker_D/0/1/0/all/0/1">David H. Shoemaker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shoemaker_D/0/1/0/all/0/1">Deirdre Shoemaker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schnittman_J/0/1/0/all/0/1">Jeremy D. Schnittman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vallisneri_M/0/1/0/all/0/1">Michele Vallisneri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yunes_N/0/1/0/all/0/1">Nicolas Yunes</a> Low-frequency gravitational-wave astronomy can perform precision tests of general relativity and probe fundamental physics in a regime previously inaccessible. A space-based detector will be a formidable tool to explore gravity’s role in the cosmos, potentiallyRead More →

Radio detection of cosmic rays below 10 MHz: the EXTASIS experiment. (arXiv:1903.02792v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Charrier_D/0/1/0/all/0/1">Didier Charrier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dallier_R/0/1/0/all/0/1">Richard Dallier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Escudie_A/0/1/0/all/0/1">Antony Escudie</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garcia_Fernandez_D/0/1/0/all/0/1">Daniel Garc&#xed;a-Fern&#xe1;ndez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lecacheux_A/0/1/0/all/0/1">Alain Lecacheux</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Martin_L/0/1/0/all/0/1">Lilian Martin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Revenu_B/0/1/0/all/0/1">Beno&#xee;t Revenu</a> Since 2003, significant efforts have been devoted to the understanding of the radio emission of extensive air showers above 20 MHz. Despite some studies led until the early nineties, the band available above 20 MHz has remained unused for 20 years. However, it has been claimed by some pioneering experiments that extensive air showers emit a strong electric field in this band and that there is evidence of a large increaseRead More →

Physical properties and transmission spectrum of the WASP-74 planetary system from multi-band photometry. (arXiv:1903.02800v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Mancini_L/0/1/0/all/0/1">L. Mancini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Southworth_J/0/1/0/all/0/1">J. Southworth</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Molliere_P/0/1/0/all/0/1">P. Molliere</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tregloan_Reed_J/0/1/0/all/0/1">J. Tregloan-Reed</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Juvan_I/0/1/0/all/0/1">I. G. Juvan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_G/0/1/0/all/0/1">G. Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sarkis_P/0/1/0/all/0/1">P. Sarkis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bruni_I/0/1/0/all/0/1">I. Bruni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ciceri_S/0/1/0/all/0/1">S. Ciceri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Andersen_M/0/1/0/all/0/1">M. I. Andersen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bozza_V/0/1/0/all/0/1">V. Bozza</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bramich_D/0/1/0/all/0/1">D. M. Bramich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burgdorf_M/0/1/0/all/0/1">M. Burgdorf</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DAgo_G/0/1/0/all/0/1">G. D&#x27;Ago</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dominik_M/0/1/0/all/0/1">M. Dominik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Evans_D/0/1/0/all/0/1">D. F. Evans</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jaimes_R/0/1/0/all/0/1">R. Figuera Jaimes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fossati_L/0/1/0/all/0/1">L. Fossati</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Henning_T/0/1/0/all/0/1">Th. Henning</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hinse_T/0/1/0/all/0/1">T. C. Hinse</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hundertmark_M/0/1/0/all/0/1">M. Hundertmark</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jorgensen_U/0/1/0/all/0/1">U. G. Jorgensen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kerins_E/0/1/0/all/0/1">E. Kerins</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Korhonen_H/0/1/0/all/0/1">H. Korhonen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kuffmeier_M/0/1/0/all/0/1">M. Kuffmeier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Longa_P/0/1/0/all/0/1">P. Longa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Peixinho_N/0/1/0/all/0/1">N. Peixinho</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Popovas_A/0/1/0/all/0/1">A.Read More →

WASP-92, WASP-93 and WASP-118: Transit timing variations and long-term stability of the systems. (arXiv:1903.02804v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Gajdos_P/0/1/0/all/0/1">Pavol Gajdo&#x161;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vanko_M/0/1/0/all/0/1">Martin Va&#x148;ko</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Evans_P/0/1/0/all/0/1">Phil Evans</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bretton_M/0/1/0/all/0/1">Marc Bretton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Molina_D/0/1/0/all/0/1">David Molina</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferratfiat_S/0/1/0/all/0/1">St&#xe9;phane Ferratfiat</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Girardin_E/0/1/0/all/0/1">Eric Girardin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gu%7B%5Cdh%7Dmundsson_S/0/1/0/all/0/1">Sn&#xe6;varr Gu&#xf0;mundsson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Scaggiante_F/0/1/0/all/0/1">Francesco Scaggiante</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Parimucha_S/0/1/0/all/0/1">&#x160;tefan Parimucha</a> We studied three exoplanetary systems with transiting planets: WASP-92, WASP-93 and WASP-118. Using ground-based photometric observations of WASP-92 and WASP-93 and textit{Kepler-K2} observations of WASP-118, we redetermined the orbital and physical parameters of these planets. The precise times of all transits were determined. We constructed O-C diagrams of transits and analysed possible transit timing variations. We did not observe anyRead More →

Looking for ancillary signals around GW150914. (arXiv:1903.02823v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Maroju_R/0/1/0/all/0/1">Rahul Maroju</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dyuthi_S/0/1/0/all/0/1">Sristi Ram Dyuthi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sukrutha_A/0/1/0/all/0/1">Anumandla Sukrutha</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Desai_S/0/1/0/all/0/1">Shantanu Desai</a> We replicated the procedure in Liu and Jackson (arXiv:1609.08346), who had found evidence for a low amplitude signal in the vicinity of GW150914. This was based upon the large correlation between the time integral of the Pearson cross-correlation coefficient in the off-source region of GW150914, and the Pearson cross-correlation in a narrow window around GW150914, for the same time lag between the two LIGO detectors as the gravitational wave signal. Our results mostly agree with those in arXiv:1609.08346. However, we also find a highRead More →

Study of shocks in relativistic viscous accretion flow around Kerr black hole. (arXiv:1903.02856v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Dihingia_I/0/1/0/all/0/1">I. Dihingia</a> (IITG), <a href="http://arxiv.org/find/astro-ph/1/au:+Das_S/0/1/0/all/0/1">Santabrata Das</a> (IITG), <a href="http://arxiv.org/find/astro-ph/1/au:+Maity_D/0/1/0/all/0/1">Debaprasad Maity</a> (IITG), <a href="http://arxiv.org/find/astro-ph/1/au:+Nandi_A/0/1/0/all/0/1">Anuj Nandi</a> (URSC, ISRO) We study the relativistic viscous accretion flows around the Kerr black holes. We present governing equations that describe the flow motion in full general relativity and solve them to obtain the complete set of global transonic solutions in terms of the flow parameters, namely energy (${cal E}$), angular momentum (${cal L}$) and viscosity ($alpha$). We obtain a new type of accretion solution which was not reported earlier. Further, to the best of our knowledge,Read More →

Pre-processing of galaxies in cosmic filaments around AMASCFI clusters in the CFHTLS. (arXiv:1903.02879v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Sarron_F/0/1/0/all/0/1">Florian Sarron</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Adami_C/0/1/0/all/0/1">Christophe Adami</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Durret_F/0/1/0/all/0/1">Florence Durret</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Laigle_C/0/1/0/all/0/1">Clotilde Laigle</a> Galaxy clusters and groups are thought to accrete material along the preferred direction of cosmic filaments. Yet these structures have proven difficult to detect due to their low contrast with few studies focusing on cluster infall regions. In this work, we detected cosmic filaments around galaxy clusters using photometric redshifts in the range 0.15Read More →

Morphology and dynamics of Venus’s middle clouds with Akatsuki/IR1. (arXiv:1903.02883v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Peralta_J/0/1/0/all/0/1">J. Peralta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Iwagami_N/0/1/0/all/0/1">N. Iwagami</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+S%5C%27anchez-Lavega/0/1/0/all/0/1">S&#xe1;nchez-Lavega</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_Y/0/1/0/all/0/1">Y. J. Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hueso_R/0/1/0/all/0/1">R. Hueso</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Narita_M/0/1/0/all/0/1">M. Narita</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Imamura_T/0/1/0/all/0/1">T. Imamura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Miles_P/0/1/0/all/0/1">P. Miles</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wesley_A/0/1/0/all/0/1">A. Wesley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kardasis_E/0/1/0/all/0/1">E. Kardasis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Takagi_S/0/1/0/all/0/1">S. Takagi</a> The Venusian atmosphere is covered by clouds with super-rotating winds whose accelerating mechanism is still not well understood. The fastest winds, occurring at the cloud tops ($sim$70 km height), have been studied for decades thanks to their visual contrast in dayside ultraviolet images. The middle clouds ($sim$50-55 km) can be observed at near-infrared wavelengths (800-950 nm), although with very low contrast.Read More →

Radio detection of atmospheric air showers of particles. (arXiv:1903.02889v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Escudie_A/0/1/0/all/0/1">Antony Escudie</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dallier_R/0/1/0/all/0/1">Richard Dallier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Charrier_D/0/1/0/all/0/1">Didier Charrier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garcia_Fernandez_D/0/1/0/all/0/1">Daniel Garc&#xed;a-Fern&#xe1;ndez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lecacheux_A/0/1/0/all/0/1">Alain Lecacheux</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Martin_L/0/1/0/all/0/1">Lilian Martin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Revenu_B/0/1/0/all/0/1">Beno&#xee;t Revenu</a> Since 2002, the CODALEMA experiment located within the Nanc{c}ay Radio Observatory studies the ultra-high energy cosmic rays (above 10^{17} eV) arriving in the Earth atmosphere. These cosmic rays interact with the component of the atmosphere, inducing an extensive air shower (EAS) composed mainly of charged particles (electrons and positrons). During the development of the shower in the atmosphere, these charged particles in movement generate a fast electric field transient (a few nanoseconds to aRead More →

Accurate mass and radius determinations of a cool subdwarf in an eclipsing binary. (arXiv:1903.02897v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Rebassa_Mansergas_A/0/1/0/all/0/1">Alberto Rebassa-Mansergas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Parsons_S/0/1/0/all/0/1">Steven G. Parsons</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dhillon_V/0/1/0/all/0/1">Vikram S. Dhillon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ren_J/0/1/0/all/0/1">Juanjuan Ren</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Littlefair_S/0/1/0/all/0/1">Stuart P. Littlefair</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marsh_T/0/1/0/all/0/1">Thomas R. Marsh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Torres_S/0/1/0/all/0/1">Santiago Torres</a> Cool subdwarfs are metal-poor low-mass stars that formed during the early stages of the evolution of our Galaxy. Because they are relatively rare in the vicinity of the Sun, we know of few cool subdwarfs in the solar neighbourhood, and none with both the mass and the radius accurately determined. This hampers our understanding of stars at the low-mass end of the main-sequence. Here weRead More →