RAS_WEB (Page 4,386)

The OSIRIS Lens-Amplified Survey (OLAS) I: Dynamical Effects of Stellar Feedback in Low Mass Galaxies at z ~ 2. (arXiv:1811.11768v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Hirtenstein_J/0/1/0/all/0/1">Jessie Hirtenstein</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Jones_T/0/1/0/all/0/1">Tucker Jones</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_X/0/1/0/all/0/1">Xin Wang</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Wetzel_A/0/1/0/all/0/1">Andrew Wetzel</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+El_Badry_K/0/1/0/all/0/1">Kareem El-Badry</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Hoag_A/0/1/0/all/0/1">Austin Hoag</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Treu_T/0/1/0/all/0/1">Tommaso Treu</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Bradac_M/0/1/0/all/0/1">Marusa Bradac</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Morishita_T/0/1/0/all/0/1">Takahiro Morishita</a> (4) ((1) University of California Davis, (2) University of California Los Angeles, (3) University of California Berkeley, (4) Space Telescope Science Institute) We introduce the OSIRIS Lens-Amplified Survey (OLAS), a kinematic survey of gravitationally lensed galaxies at cosmic noon taken with Keck adaptive optics. In this paper we presentRead More →

A SOFIA Survey of [CII] in the galaxy M51 I. [CII] as a tracer of Star Formation. (arXiv:1811.11769v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Pineda_J/0/1/0/all/0/1">Jorge L. Pineda</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Fischer_C/0/1/0/all/0/1">Christian Fischer</a>, (2) <a href="http://arxiv.org/find/astro-ph/1/au:+Kapala_M/0/1/0/all/0/1">Maria Kapala</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Stutzki_J/0/1/0/all/0/1">Juergen Stutzki</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Buchbender_C/0/1/0/all/0/1">Christof Buchbender</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Goldsmith_P/0/1/0/all/0/1">Paul F. Goldsmith</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Ziebart_M/0/1/0/all/0/1">Monika Ziebart</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Glover_S/0/1/0/all/0/1">Simon C. O. Glover</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Klessen_R/0/1/0/all/0/1">Ralf S. Klessen</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Koda_J/0/1/0/all/0/1">Jin Koda</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Kramer_C/0/1/0/all/0/1">Carsten Kramer</a> (7), <a href="http://arxiv.org/find/astro-ph/1/au:+Mookerjea_B/0/1/0/all/0/1">Bhaswati Mookerjea</a> (8), <a href="http://arxiv.org/find/astro-ph/1/au:+Sandstrom_K/0/1/0/all/0/1">Karin Sandstrom</a> (9), <a href="http://arxiv.org/find/astro-ph/1/au:+Scoville_N/0/1/0/all/0/1">Nick Scoville</a> (10), <a href="http://arxiv.org/find/astro-ph/1/au:+Smith_R/0/1/0/all/0/1">Rowan Smith</a> (11), ((1) Jet Propulsion Laboratory, California Institute of Technology,(2) Deutsches SOFIA Institut, (3) University of Cape Town, (4) Universitaet zu Koeln,(5) UniversitaetRead More →

The Extraplanar Type II Supernova ASASSN-14jb in the Nearby Edge-on Galaxy ESO 467-G051. (arXiv:1811.11771v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Meza_N/0/1/0/all/0/1">Nicolas Meza</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prieto_J/0/1/0/all/0/1">J. L. Prieto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Clocchiatti_A/0/1/0/all/0/1">A. Clocchiatti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Galbany_L/0/1/0/all/0/1">L. Galbany</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anderson_J/0/1/0/all/0/1">J. P. Anderson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Falco_E/0/1/0/all/0/1">E. Falco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kochanek_C/0/1/0/all/0/1">C. S. Kochanek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kuncarayakti_H/0/1/0/all/0/1">H. Kuncarayakti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brimacombe_J/0/1/0/all/0/1">J. Brimacombe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Holoien_T/0/1/0/all/0/1">T. W.-S. Holoien</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shappee_B/0/1/0/all/0/1">B. J. Shappee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stanek_K/0/1/0/all/0/1">K. Z. Stanek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Thompson_T/0/1/0/all/0/1">T. A. Thompson</a> We present optical photometry and spectroscopy of the Type II supernova ASASSN-14jb, together with VLT MUSE IFU observations of its host galaxy and a nebular-phase spectrum. This SN, in the nearby galaxy ESO 467-G051 ($z=0.006$), was discovered and followed-up by the All Sky AutomatedRead More →

The host galaxies of FeLoBAL quasars at z$sim$0.9 are not dominated by recent major mergers. (arXiv:1811.11773v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Villforth_C/0/1/0/all/0/1">C. Villforth</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Herbst_H/0/1/0/all/0/1">H. Herbst</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hamann_F/0/1/0/all/0/1">F. Hamann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hamilton_T/0/1/0/all/0/1">T. Hamilton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bertemes_C/0/1/0/all/0/1">C. Bertemes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Efthymiadou_A/0/1/0/all/0/1">A. Efthymiadou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hewlett_T/0/1/0/all/0/1">T. Hewlett</a> Theoretical models have suggested an evolutionary model for quasars, in which most of luminous quasars are triggered by major mergers. It is also postulated that reddening as well as powerful outflows indicate an early phase of activity, close to the merger event. We test this model on a sample of quasars with powerful low ionization outflows seen in broad Iron absorption lines (FeLoBAL). This sample of objectsRead More →

Gravitational waves from spin-3/2 fields — Hunting SUSY in the sky. (arXiv:1811.11774v1 [hep-ph]) <a href="http://arxiv.org/find/hep-ph/1/au:+Benakli_K/0/1/0/all/0/1">Karim Benakli</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Chen_Y/0/1/0/all/0/1">Yifan Chen</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Cheng_P/0/1/0/all/0/1">Peng Cheng</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Lafforgue_Marmet_G/0/1/0/all/0/1">Ga&#xeb;tan Lafforgue-Marmet</a> Stochastic gravitational waves can be produced during the preheating when out-of-equilibrium particles are produced with an anisotropic stress-tensor. We discuss the case where these particles carry spin-3/2. We compute the spectrum of the gravitational waves generated by the transverse and longitudinal components. We find a different scaling of the spectrum near the peak and the longitudinal components lead to an enhancement when compared to spin-1/2 fermions with Yukawa couplings. We note, as expected, that the corresponding typical frequency is tooRead More →

Atmospheric Mass Loss from High Velocity Giant Impacts. (arXiv:1811.11778v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Yalinewich_A/0/1/0/all/0/1">Almog Yalinewich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schlichting_H/0/1/0/all/0/1">Hilke E. Schlichting</a> Using moving mesh hydrodynamic simulations, we determine the shock propagation and resulting ground velocities for a planet hit by a high velocity impactor. We use our results to determine the atmospheric mass loss caused by the resulting ground motion due to the impact shock wave. We find that there are two distinct shock propagation regimes: In the limit in which the impactor is significantly smaller than the target ($R_iRead More →

The large and small scale properties of the intergalactic gas in the Slug Ly-alpha nebula revealed by MUSE HeII emission observations. (arXiv:1811.11783v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Cantalupo_S/0/1/0/all/0/1">Sebastiano Cantalupo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pezzulli_G/0/1/0/all/0/1">Gabriele Pezzulli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lilly_S/0/1/0/all/0/1">Simon J. Lilly</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marino_R/0/1/0/all/0/1">Raffaella A. Marino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gallego_S/0/1/0/all/0/1">Sofia G. Gallego</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schaye_J/0/1/0/all/0/1">Joop Schaye</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bacon_R/0/1/0/all/0/1">Roland Bacon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Feltre_A/0/1/0/all/0/1">Anna Feltre</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kollatschny_W/0/1/0/all/0/1">Wolfram Kollatschny</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nanayakkara_T/0/1/0/all/0/1">Themiya Nanayakkara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Richard_J/0/1/0/all/0/1">Johan Richard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wendt_M/0/1/0/all/0/1">Martin Wendt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wisotzki_L/0/1/0/all/0/1">Lutz Wisotzki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prochaska_J/0/1/0/all/0/1">J. Xavier Prochaska</a> With a projected size of about 450 kpc at z~2.3, the Slug Ly-alpha nebula is a rare laboratory to study, in emission, the properties of the intergalactic gas in the Cosmic Web. Since its discovery, theRead More →

Dwarf Galaxies in CDM, WDM, and SIDM: Disentangling Baryons and Dark Matter Physics. (arXiv:1811.11791v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Fitts_A/0/1/0/all/0/1">Alex Fitts</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boylan_Kolchin_M/0/1/0/all/0/1">Michael Boylan-Kolchin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bozek_B/0/1/0/all/0/1">Brandon Bozek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bullock_J/0/1/0/all/0/1">James S. Bullock</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Graus_A/0/1/0/all/0/1">Andrew Graus</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Robles_V/0/1/0/all/0/1">Victor Robles</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:+El_Badry_K/0/1/0/all/0/1">Kareem El-Badry</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garrison_Kimmel_S/0/1/0/all/0/1">Shea Garrison-Kimmel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Faucher_Giguere_C/0/1/0/all/0/1">Claude-Andr&#xe9; Faucher-Gigu&#xe8;re</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wetzel_A/0/1/0/all/0/1">Andrew Wetzel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Keres_D/0/1/0/all/0/1">Du&#x161;an Kere&#x161;</a> We present a suite of FIRE-2 cosmological zoom-in simulations of isolated field dwarf galaxies, all with masses of $M_mathrm{halo} approx 10^{10},$M$_odot$ at $z=0$, across a range of dark matter models. For the first time, we compare how both self-interacting dark matter (SIDM) and/or warm dark matter (WDM) models affect the assembly historiesRead More →

A wide field map of intracluster globular clusters in Coma. (arXiv:1811.11794v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Madrid_J/0/1/0/all/0/1">Juan P. Madrid</a> (CSIRO), <a href="http://arxiv.org/find/astro-ph/1/au:+ONeill_C/0/1/0/all/0/1">Conor R. O&#x27;Neill</a> (Gemini), <a href="http://arxiv.org/find/astro-ph/1/au:+Gagliano_A/0/1/0/all/0/1">Alexander T. Gagliano</a> (Virginia Tech), <a href="http://arxiv.org/find/astro-ph/1/au:+Marvil_J/0/1/0/all/0/1">Joshua R. Marvil</a> (NRAO) The large-scale distribution of globular clusters in the central region of the Coma cluster of galaxies is derived through the analysis of Hubble Space Telescope/Advanced Camera for Surveys data. Data from three different HST observing programs are combined in order to obtain a full surface density map of globular clusters in the core of Coma. A total of 22,426 Globular cluster candidates were selected through a detailed morphological inspection and the analysisRead More →

Layer formation in double-diffusive convection over resting and moving heated plates. (arXiv:1811.11800v1 [physics.flu-dyn]) <a href="http://arxiv.org/find/physics/1/au:+Zaussinger_F/0/1/0/all/0/1">Florian Zaussinger</a>, <a href="http://arxiv.org/find/physics/1/au:+Kupka_F/0/1/0/all/0/1">Friedrich Kupka</a> We present a numerical study of double-diffusive convection characterized by a stratification unstable to thermal convection while at the same time a mean molecular weight (or solute concentration) difference between top and bottom counteracts this instability. Convective zones can form in this case either by the stratification being locally unstable to the combined action of both temperature and solute gradients or by another process, the oscillatory double-diffusive convective instability, which is triggered by the faster molecular diffusivity of heat in comparison with that one of theRead More →

Dynamical masses of M-dwarf binaries in young moving groups: II – Toward empirical mass-luminosity isochrones. (arXiv:1811.11802v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Janson_M/0/1/0/all/0/1">Markus Janson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Durkan_S/0/1/0/all/0/1">Stephen Durkan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bonnefoy_M/0/1/0/all/0/1">Mickael Bonnefoy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rodet_L/0/1/0/all/0/1">Laetitia Rodet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kohler_R/0/1/0/all/0/1">Rainer Kohler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lacour_S/0/1/0/all/0/1">Sylvestre Lacour</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brandner_W/0/1/0/all/0/1">Wolfgang Brandner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Henning_T/0/1/0/all/0/1">Thomas Henning</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Girard_J/0/1/0/all/0/1">Julien Girard</a> Low-mass stars exhibit substantial pre-main sequence evolution during the first ~100 Myrs of their lives. Thus, young M-type stars are prime targets for isochronal dating, especially in young moving groups (YMGs), which contain large amounts of stars in this mass and age range. If the mass and luminosity of a star can both be directly determined, this allows for a particularlyRead More →

Post-Newtonian Dynamics in Dense Star Clusters: Binary Black Holes in the LISA Band. (arXiv:1811.11812v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Kremer_K/0/1/0/all/0/1">Kyle Kremer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rodriguez_C/0/1/0/all/0/1">Carl L. Rodriguez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amaro_Seoane_P/0/1/0/all/0/1">Pau Amaro-Seoane</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Breivik_K/0/1/0/all/0/1">Katelyn Breivik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chatterjee_S/0/1/0/all/0/1">Sourav Chatterjee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Katz_M/0/1/0/all/0/1">Michael L. Katz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Larson_S/0/1/0/all/0/1">Shane L. Larson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rasio_F/0/1/0/all/0/1">Frederic A. Rasio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Samsing_J/0/1/0/all/0/1">Johan Samsing</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ye_C/0/1/0/all/0/1">Claire S. Ye</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zevin_M/0/1/0/all/0/1">Michael Zevin</a> The dynamical processing of black holes in the dense cores of globular clusters (GCs), makes them efficient factories for producing binary black holes (BBHs). Here we explore the population of BBHs that form dynamically in GCs and may be observable at mHz frequencies or higher with LISA. We use our Monte CarloRead More →

Effect of Induced Seismicity on Advanced Gravitational Wave Interferometers. (arXiv:1811.11817v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Mukund_N/0/1/0/all/0/1">Nikhil Mukund</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+OReilly_B/0/1/0/all/0/1">Brian O&#x27;Reilly</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Somala_S/0/1/0/all/0/1">Surendra Nadh Somala</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mitra_S/0/1/0/all/0/1">Sanjit Mitra</a> Advanced LIGO and the next generation of ground-based detectors aim to capture many more binary coalescences through improving sensitivity and duty cycle. Earthquakes have always been a limiting factor at low frequency where neither the pendulum suspension nor the active controls provide sufficient isolation to the test mass mirrors. Several control strategies have been proposed to reduce the impact of tele-seismic events by switching to a robust configuration with less aggressive feedback. The continental United States has witnessed a huge increaseRead More →

Gamma/Hadron Separation in Imaging Air Cherenkov Telescopes Using Deep Learning Libraries TensorFlow and PyTorch. (arXiv:1811.11822v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Postnikov_E/0/1/0/all/0/1">E. B. Postnikov</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Kryukov_A/0/1/0/all/0/1">A. P. Kryukov</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Polyakov_S/0/1/0/all/0/1">S. P. Polyakov</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Shipilov_D/0/1/0/all/0/1">D. A. Shipilov</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Zhurov_D/0/1/0/all/0/1">D. P. Zhurov</a> (2) ((1) Lomonosov Moscow State University Skobeltsyn Institute of Nuclear Physics (MSU SINP), Moscow, Russia, (2) Irkutsk State University (ISU), Irkutsk, Russia) In this work we compare two open source machine learning libraries, PyTorch and TensorFlow, as software platforms for rejecting hadron background events detected by imaging air Cherenkov telescopes (IACTs). Monte Carlo simulation for the TAIGA-IACT telescope is used to estimate background rejection quality.Read More →

Three years later: gender differences in the advisor’s impact on career choices in astronomy and astrophysics. (arXiv:1811.11836v1 [physics.ed-ph]) <a href="http://arxiv.org/find/physics/1/au:+Ivie_R/0/1/0/all/0/1">Rachel Ivie</a>, <a href="http://arxiv.org/find/physics/1/au:+White_S/0/1/0/all/0/1">Susan White</a>, <a href="http://arxiv.org/find/physics/1/au:+Chu_R/0/1/0/all/0/1">Raymond Y. Chu</a> The Longitudinal Study of Astronomy Graduate Students (LSAGS) arose from the 2003 Women in Astronomy Conference, where it was noted that a majority of young members of the American Astronomical Society were women. The astronomy community wishes to make every effort to retain young women in astronomy, so they commissioned a longitudinal study to be conducted that would pinpoint the factors that contribute to retention in general, with a focus on differences between women and men. TheRead More →

Waiting to make an impact: a probable excess of near-Earth asteroids in 2018 LA-like orbits. (arXiv:1811.11845v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Marcos_C/0/1/0/all/0/1">C. de la Fuente Marcos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marcos_R/0/1/0/all/0/1">R. de la Fuente Marcos</a> Context. The discovery and tracking of 2018 LA marks only the third instance in history that the parent body of a fireball has been identified before its eventual disintegration in our atmosphere. The subsequent recovery of meteorites from 2018 LA was only the second time materials from outer space that reached the ground could be linked with certitude to a particular minor body. However, meteoroids like 2018 LA and its forerunners, 2008 TC3 and 2014 AA,Read More →

Connecting Giant Planet Atmosphere and Interior Modeling: Constraints on Atmospheric Metal Enrichment. (arXiv:1811.11859v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Thorngren%2E_D/0/1/0/all/0/1">Daniel P. Thorngren.</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fortney_J/0/1/0/all/0/1">Jonathan J. Fortney</a> Atmospheric characterization through spectroscopic analysis, an essential tool of modern exoplanet science, can benefit significantly from the context provided by interior structure models. In particular, the planet’s bulk metallicity $Z_p$ places an upper limit on potential atmospheric metallicity. Here we construct interior structure models to derive $Z_p$ and atmospheric metallicity upper limits for 365 known transiting giant exoplanets. These limits are low enough that they can usefully inform atmosphere models. Additionally, we argue that comparing $Z_p$ to the observed atmospheric metallicity gives aRead More →

The Advanced Spectral Library (ASTRAL): Reference Spectra for Evolved M-Stars. (arXiv:1811.11865v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Carpenter_K/0/1/0/all/0/1">Kenneth G. Carpenter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nielsen_K/0/1/0/all/0/1">Krister E. Nielsen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kober_G/0/1/0/all/0/1">Gladys V. Kober</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ayres_T/0/1/0/all/0/1">Thomas R. Ayres</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wahlgren_G/0/1/0/all/0/1">Glenn M. Wahlgren</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rau_G/0/1/0/all/0/1">Gioia Rau</a> The HST Treasury Program “Advanced Spectral Library Project: Cool Stars” was designed to collect representative, high quality ultraviolet spectra of eight evolved F-M type cool stars. The Space Telescope Imaging Spectrograph (STIS) echelle spectra of these objects enable investigations of a broad range of topics including stellar and interstellar astrophysics. This paper provides a guide to the spectra of the two evolved M-stars, the M2Iab supergiant Alpha Ori and theRead More →

Acoustic detection of high energy neutrinos in sea water: status and prospects. (arXiv:1811.11871v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Lahmann_R/0/1/0/all/0/1">Robert Lahmann</a> The acoustic neutrino detection technique is a promising approach for future large-scale detectors with the aim of measuring the small expected flux of neutrinos at energies in the EeV-range and above. The technique is based on the thermo-acoustic model, which implies that the energy deposition by a particle cascade – resulting from a neutrino interaction in a medium with suitable thermal and acoustic properties – leads to a local heating and a subsequent characteristic pressure pulse that propagates in the surrounding medium. Current or recent test setups forRead More →

XMM-Newton and INTEGRAL analysis of the Supergiant Fast X-ray Transient IGR J17354-3255. (arXiv:1811.11882v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Goossens_M/0/1/0/all/0/1">M. E. Goossens</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bird_A/0/1/0/all/0/1">A. J. Bird</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hill_A/0/1/0/all/0/1">A. B. Hill</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sguera_V/0/1/0/all/0/1">V. Sguera</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Drave_S/0/1/0/all/0/1">S. P. Drave</a> We present the results of combined INTEGRAL and XMM-Newton observations of the supergiant fast X-ray transient (SFXT) IGR J17354$-$3255. Three XMM-Newton observations of lengths 33.4 ks, 32.5 ks and 21.9 ks were undertaken, the first an initial pointing to identify the correct source in the field of view and the latter two performed around periastron. Simultaneous INTEGRAL observations across $sim66%$ of the orbital cycle were analysed but the source was neither detectedRead More →