RAS_WEB (Page 4,569)

Dark Matter phenomenology : from simplified WIMP models to refined alternative solutions. (arXiv:1901.05822v1 [hep-ph]) <a href="http://arxiv.org/find/hep-ph/1/au:+Pierre_M/0/1/0/all/0/1">Mathias Pierre</a> One of the most puzzling problems of modern physics is the identification of the nature a non-relativistic matter component present in the universe, contributing to more than 25$%$ of the total energy budget, known as Dark Matter. Weakly Interacting Massive Particles (WIMPs) are among the best motivated dark matter candidates. However, in light of non conclusive detection signals and strong constraints from collider, direct and indirect detection experiments, this thesis presents constraints on several realizations of the WIMP paradigm in the context of simplified dark matter models. MoreRead More →

Concerning pressure and entropy of shock-accelerated heliosheath electrons. (arXiv:1901.05848v1 [physics.space-ph]) <a href="http://arxiv.org/find/physics/1/au:+Fahr_H/0/1/0/all/0/1">Hans J. Fahr</a>, <a href="http://arxiv.org/find/physics/1/au:+Dutta_Roy_R/0/1/0/all/0/1">Robindro Dutta-Roy</a> We study the behaviour of shocked wind-electrons leaving wind-driving stars after undergoing the outer wind termination shock. As an example, we describe the evolution of the keV-energetic electron distribution function downstream of the heliospheric termination shock. We start from a kinetic transport equation in the bulk frame of the heliosheath plasma flow taking into account shock-induced electron injection, convective changes, cooling processes, and whistler wave-induced energy diffusion. From this equation we proceed to an associated pressure moment of the electron distribution function arriving at a corresponding pressure transportRead More →

Spitzer transit follow-up of planet candidates from the K2 mission. (arXiv:1901.05855v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Livingston_J/0/1/0/all/0/1">John H. Livingston</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Crossfield_I/0/1/0/all/0/1">Ian J. M. Crossfield</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Werner_M/0/1/0/all/0/1">Michael W. Werner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gorjian_V/0/1/0/all/0/1">Varoujan Gorjian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Petigura_E/0/1/0/all/0/1">Erik A. Petigura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ciardi_D/0/1/0/all/0/1">David R. Ciardi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dressing_C/0/1/0/all/0/1">Courtney D. Dressing</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fulton_B/0/1/0/all/0/1">Benjamin J. Fulton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hirano_T/0/1/0/all/0/1">Teruyuki Hirano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schlieder_J/0/1/0/all/0/1">Joshua E. Schlieder</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sinukoff_E/0/1/0/all/0/1">Evan Sinukoff</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kosiarek_M/0/1/0/all/0/1">Molly Kosiarek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Akeson_R/0/1/0/all/0/1">Rachel Akeson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beichman_C/0/1/0/all/0/1">Charles A. Beichman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Benneke_B/0/1/0/all/0/1">Bj&#xf6;rn Benneke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Christiansen_J/0/1/0/all/0/1">Jessie L. Christiansen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hansen_B/0/1/0/all/0/1">Bradley M. S. Hansen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Howard_A/0/1/0/all/0/1">Andrew W. Howard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Isaacson_H/0/1/0/all/0/1">Howard Isaacson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Knutson_H/0/1/0/all/0/1">Heather A. Knutson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Krick_J/0/1/0/all/0/1">Jessica Krick</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Martinez_A/0/1/0/all/0/1">Arturo O. Martinez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sato_B/0/1/0/all/0/1">Bun&#x27;ei Sato</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tamura_M/0/1/0/all/0/1">Motohide Tamura</a> We present precision 4.5 $mu$mRead More →

Optimizing the accuracy and efficiency of optical turbulence profiling using adaptive optics telemetry for extremely large telescopes. (arXiv:1901.05860v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Laidlaw_D/0/1/0/all/0/1">Douglas J Laidlaw</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Osborn_J/0/1/0/all/0/1">James Osborn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Morris_T/0/1/0/all/0/1">Timothy J Morris</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Basden_A/0/1/0/all/0/1">Alastair G Basden</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beltramo_Martin_O/0/1/0/all/0/1">Olivier Beltramo-Martin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Butterley_T/0/1/0/all/0/1">Timothy Butterley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gendron_E/0/1/0/all/0/1">Eric Gendron</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reeves_A/0/1/0/all/0/1">Andrew P Reeves</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rousset_G/0/1/0/all/0/1">G&#xe9;rard Rousset</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Townson_M/0/1/0/all/0/1">Matthew J Townson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wilson_R/0/1/0/all/0/1">Richard W Wilson</a> Advanced adaptive optics (AO) instruments on ground-based telescopes require accurate knowledge of the atmospheric turbulence strength as a function of altitude. This information assists point spread function reconstruction, AO temporal control techniques and is required by wide-field AO systems to optimize the reconstruction of an observed wavefront.Read More →

Chemical composition of post-AGB star candidates. (arXiv:1901.05866v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Molina_R/0/1/0/all/0/1">R. E. Molina</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pereira_C/0/1/0/all/0/1">C. B. Pereira</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferro_A/0/1/0/all/0/1">A. Arellano Ferro</a> We present a high resolution detailed abundance analysis for a sample of six post-AGB candidate stars, five of them had not been studied spectroscopically in the optical region. All the analyzed objects are IRAS sources identified as possible post-AGB on the two-colours IRAS diagram. We find three objects with clear signs of evolved stars; IRAS 05338-3051 shows abundances similar to the RV Tauri V453 Oph; the lower-luminosity stars IRAS 18025 – 3906 is O-rich without s-process enrichment and IRAS 18386 – 1253 shows a moderateRead More →

Observations of solar small-scale magnetic flux-sheet emergence. (arXiv:1901.05870v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Fischer_C/0/1/0/all/0/1">C.E. Fischer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Borrero_J/0/1/0/all/0/1">J.M. Borrero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gonzalez_N/0/1/0/all/0/1">N. Bello Gonz&#xe1;lez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kaithakkal_A/0/1/0/all/0/1">A.J. Kaithakkal</a> Aims. Moreno-Insertis et al. (2018) recently discovered two types of flux emergence in their numerical simulations: magnetic loops and magnetic sheet emergence. Whereas magnetic loop emergence has been documented well in the last years, by utilising high-resolution full Stokes data from ground-based telescopes as well as satellites, magnetic sheet emergence is still an understudied process. We report here on the first clear observational evidence of a magnetic sheet emergence and characterise its development. Methods. Full Stokes spectra from the Hinode spectropolarimeter were invertedRead More →

Cross-helically forced and decaying hydromagnetic turbulence. (arXiv:1901.05875v1 [physics.flu-dyn]) <a href="http://arxiv.org/find/physics/1/au:+Brandenburg_A/0/1/0/all/0/1">Axel Brandenburg</a> (Nordita), <a href="http://arxiv.org/find/physics/1/au:+Oughton_S/0/1/0/all/0/1">Sean Oughton</a> (University of Waikato) We study the evolution of kinetic and magnetic energy spectra in magnetohydrodynamic flows in the presence of strong cross helicity. For forced turbulence, we find weak inverse transfer of kinetic energy toward the smallest wavenumber. This is plausibly explained by the finiteness of scale separation between the injection wavenumber and the smallest wavenumber of the domain, which here is a factor of 15. In the decaying case, there is a slight increase at the smallest wavenumber, which is probably explained by the dominance of kinetic energy overRead More →

On the Ubiquity and Stellar Luminosity Dependence of Exocometary CO Gas: Detection around M Dwarf TWA 7. (arXiv:1901.05004v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Matra_L/0/1/0/all/0/1">Luca Matr&#xe0;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oberg_K/0/1/0/all/0/1">Karin I. &#xd6;berg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wilner_D/0/1/0/all/0/1">David J. Wilner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Olofsson_J/0/1/0/all/0/1">Johan Olofsson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bayo_A/0/1/0/all/0/1">Amelia Bayo</a> Millimeter observations of CO gas in planetesimal belts show a high detection rate around A stars, but few detections for later type stars. We present the first CO detection in a planetesimal belt around an M star, TWA 7. The optically thin CO (J=3-2) emission is co-located with previously identified dust emission from the belt, and the emission velocity structure is consistent with Keplerian rotation around the central star.Read More →

Phenotypic redshifts with self-organizing maps: A novel method to characterize redshift distributions of source galaxies for weak lensing. (arXiv:1901.05005v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Buchs_R/0/1/0/all/0/1">R. Buchs</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Davis_C/0/1/0/all/0/1">C. Davis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gruen_D/0/1/0/all/0/1">D. Gruen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DeRose_J/0/1/0/all/0/1">J. DeRose</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alarcon_A/0/1/0/all/0/1">A. Alarcon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bernstein_G/0/1/0/all/0/1">G. M. Bernstein</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sanchez_C/0/1/0/all/0/1">C. S&#xe1;nchez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Myles_J/0/1/0/all/0/1">J. Myles</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Roodman_A/0/1/0/all/0/1">A. Roodman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Allen_S/0/1/0/all/0/1">S. Allen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amon_A/0/1/0/all/0/1">A. Amon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Choi_A/0/1/0/all/0/1">A. Choi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Masters_D/0/1/0/all/0/1">D. C. Masters</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Miquel_R/0/1/0/all/0/1">R. Miquel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Troxel_M/0/1/0/all/0/1">M. A. Troxel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wechsler_R/0/1/0/all/0/1">R. H. Wechsler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abbott_T/0/1/0/all/0/1">T. M. C. Abbott</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Annis_J/0/1/0/all/0/1">J. Annis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Avila_S/0/1/0/all/0/1">S. Avila</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bechtol_K/0/1/0/all/0/1">K. Bechtol</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bridle_S/0/1/0/all/0/1">S. L. Bridle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brooks_D/0/1/0/all/0/1">D. Brooks</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Buckley_Geer_E/0/1/0/all/0/1">E. Buckley-Geer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burke_D/0/1/0/all/0/1">D. L. Burke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rosell_A/0/1/0/all/0/1">A. Carnero Rosell</a>, <aRead More →

Formation of Hot Jupiters through Secular Chaos and Dynamical Tides. (arXiv:1901.05006v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Teyssandier_J/0/1/0/all/0/1">Jean Teyssandier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lai_D/0/1/0/all/0/1">Dong Lai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vick_M/0/1/0/all/0/1">Michelle Vick</a> The population of giant planets on short-period orbits can potentially be explained by some flavours of high-eccentricity migration. In this paper we investigate one such mechanism involving “secular chaos”, in which secular interactions between at least three giant planets push the inner planet to a highly eccentric orbit, followed by tidal circularization and orbital decay. In addition to the equilibrium tidal friction, we incorporate dissipation due to dynamical tides that are excited inside the giant planet. Using the method of Gaussian rings to accountRead More →

Does radiative feedback make faint z>6 galaxies look small?. (arXiv:1901.05007v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Ploeckinger_S/0/1/0/all/0/1">Sylvia Ploeckinger</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:+Hacar_A/0/1/0/all/0/1">Alvaro Hacar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maseda_M/0/1/0/all/0/1">Michael V. Maseda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hodge_J/0/1/0/all/0/1">Jacqueline A. Hodge</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bouwens_R/0/1/0/all/0/1">Rychard J. Bouwens</a> Recent observations of lensed sources have shown that the faintest ($M_{mathrm{UV}} approx -15,mathrm{mag}$) galaxies observed at z=6-8 appear to be extremely compact. Some of them have inferred sizes of less than 40 pc for stellar masses between $10^6$ and $10^7,mathrm{M}_{odot}$, comparable to individual super star clusters or star cluster complexes at low redshift. High-redshift, low-mass galaxies are expected to show a clumpy, irregular morphology and if star clusters form in each of theseRead More →

Detecting Ocean Glint on Exoplanets Using Multiphase Mapping. (arXiv:1901.05011v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Lustig_Yaeger_J/0/1/0/all/0/1">Jacob Lustig-Yaeger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meadows_V/0/1/0/all/0/1">Victoria S. Meadows</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mendoza_G/0/1/0/all/0/1">Guadalupe Tovar Mendoza</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schwieterman_E/0/1/0/all/0/1">Edward W. Schwieterman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fujii_Y/0/1/0/all/0/1">Yuka Fujii</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Luger_R/0/1/0/all/0/1">Rodrigo Luger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Robinson_T/0/1/0/all/0/1">Tyler D. Robinson</a> Rotational mapping and glint are two proposed methods to directly detect liquid water on the surface of habitable exoplanets. However, false positives for both methods may prevent the unambiguous detection of exoplanet oceans. We use simulations of Earth as an exoplanet to introduce a combination of multiwavelength, multiphase, time-series direct-imaging observations and accompanying analyses that may improve the robustness of exoplanet ocean detection by spatially mapping the ocean glint signal.Read More →

Ultraviolet HST Spectroscopy of Planck Cold Clumps. (arXiv:1901.05012v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Dirks_C/0/1/0/all/0/1">Cody Dirks</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meyer_D/0/1/0/all/0/1">David M. Meyer</a> We report results of the first study utilizing the ultraviolet capabilities of the Hubble Space Telescope to investigate a sample of Planck Galactic Cold Clump (PGCC) sources. We have selected high-resolution spectra toward 25 stars that contain a multitude of interstellar absorption lines associated with the interstellar medium (ISM) gas within these PGCC sources, including carbon monoxide (CO), C I and O I. By building cloud-component models of the individual absorption components present in these spectra, we can identify and isolate components associated with the PGCC sources, allowing forRead More →

Deciphering an evolutionary sequence of merger stages in infrared-luminous starburst galaxies at z ~ 0.7. (arXiv:1901.05013v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Calabro_A/0/1/0/all/0/1">Antonello Calabr&#xf2;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Daddi_E/0/1/0/all/0/1">Emanuele Daddi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Puglisi_A/0/1/0/all/0/1">Annagrazia Puglisi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oliva_E/0/1/0/all/0/1">Ernesto Oliva</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gobat_R/0/1/0/all/0/1">Raphael Gobat</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cassata_P/0/1/0/all/0/1">Paolo Cassata</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amorin_R/0/1/0/all/0/1">Ricardo Amor&#xed;n</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arimoto_N/0/1/0/all/0/1">Nobuo Arimoto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boquien_M/0/1/0/all/0/1">M&#xe9;d&#xe9;ric Boquien</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carraro_R/0/1/0/all/0/1">Rosamaria Carraro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Delvecchio_I/0/1/0/all/0/1">Ivan Delvecchio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ibar_E/0/1/0/all/0/1">Eduardo Ibar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jin_S/0/1/0/all/0/1">Shuowen Jin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Juneau_S/0/1/0/all/0/1">St&#xe9;phanie Juneau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_D/0/1/0/all/0/1">Daizhong Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Onodera_M/0/1/0/all/0/1">Masato Onodera</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mannucci_F/0/1/0/all/0/1">Filippo Mannucci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hernanez_H/0/1/0/all/0/1">Hugo M&#xe9;ndez Hern&#xe1;nez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rodighiero_G/0/1/0/all/0/1">Giulia Rodighiero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Valentino_F/0/1/0/all/0/1">Francesco Valentino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zanella_A/0/1/0/all/0/1">Anita Zanella</a> Based on optical/near-IR Magellan FIRE spectra of 25 starburst galaxies at 0.5 < z < 0.9, Calabr`o et al.(2018) showed that their attenuation propertiesRead More →

A mass-dependent slope of the galaxy size-mass relation out to z~3: further evidence for a direct relation between median galaxy size and median halo mass. (arXiv:1901.05014v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Mowla_L/0/1/0/all/0/1">Lamiya Mowla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wel_A/0/1/0/all/0/1">Arjen van der Wel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dokkum_P/0/1/0/all/0/1">Pieter van Dokkum</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Miller_T/0/1/0/all/0/1">Tim Miller</a> We reassess the galaxy size-mass relation out to z~3 using a new definition of size and a sample of >29,000 galaxies from the 3D-HST, CANDELS, and COSMOS-DASH surveys. Instead of the half-light radius r_50 we use r_80, the radius containing 80% of the stellar light. We find that the r_80 — M_star relation has the form of a broken power law, with aRead More →

A Low-Flux State in IRAS 00521-7054 seen with NuSTAR and XMM-Newton: Relativistic Reflection and an Ultrafast Outflow. (arXiv:1901.05016v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Walton_D/0/1/0/all/0/1">D. J. Walton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nardini_E/0/1/0/all/0/1">E. Nardini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gallo_L/0/1/0/all/0/1">L. C. Gallo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reynolds_M/0/1/0/all/0/1">M. T. Reynolds</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ricci_C/0/1/0/all/0/1">C. Ricci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dauser_T/0/1/0/all/0/1">T. Dauser</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fabian_A/0/1/0/all/0/1">A. C. Fabian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garcia_J/0/1/0/all/0/1">J. A. Garcia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Harrison_F/0/1/0/all/0/1">F. A. Harrison</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Risaliti_G/0/1/0/all/0/1">G. Risaliti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stern_D/0/1/0/all/0/1">D. Stern</a> We present results from a deep, coordinated $XMM$-$Newton$+$NuSTAR$ observation of the Seyfert 2 galaxy IRAS 00521-7054. The $NuSTAR$ data provide the first detection of this source in high-energy X-rays ($E > 10$ keV), and the broadband data show this to be a highly complex source which exhibitsRead More →

A New View of the Size-Mass Distribution of Galaxies: Using $r_{20}$ and $r_{80}$ instead of $r_{50}$. (arXiv:1901.05017v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Miller_T/0/1/0/all/0/1">Tim B. Miller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dokkum_P/0/1/0/all/0/1">Pieter van Dokkum</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mowla_L/0/1/0/all/0/1">Lamiya Mowla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wel_A/0/1/0/all/0/1">Arjen van der Wel</a> When investigating the sizes of galaxies it is standard practice to use the half-light radius, $r_{50}$. Here we explore the effects of the size definition on the distribution of galaxies in the size — stellar mass plane. Specifically, we consider $r_{20}$ and $r_{80}$, the radii that contain 20% and 80% of a galaxy’s total luminosity, as determined from a Sersic profile fit, for galaxies in the 3D-HST/CANDELS and COSMOS-DASH surveys. TheseRead More →

A circumbinary protoplanetary disc in a polar configuration. (arXiv:1901.05018v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Kennedy_G/0/1/0/all/0/1">Grant M. Kennedy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matra_L/0/1/0/all/0/1">Luca Matr&#xe0;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Facchini_S/0/1/0/all/0/1">Stefano Facchini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Milli_J/0/1/0/all/0/1">Julien Milli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Panic_O/0/1/0/all/0/1">Olja Pani&#x107;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Price_D/0/1/0/all/0/1">Daniel Price</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wilner_D/0/1/0/all/0/1">David J. Wilner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wyatt_M/0/1/0/all/0/1">Mark C. Wyatt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yelverton_B/0/1/0/all/0/1">Ben M. Yelverton</a> Nearly all young stars are initially surrounded by `protoplanetary’ discs of gas and dust, and in the case of single stars at least 30% of these discs go on to form planets. The process of protoplanetary disc formation can result in initial misalignments, where the disc orbital plane is different to the stellar equator in single star systems, or to the binary orbital planeRead More →

Decorrelating the errors of the galaxy correlation function with compact transformation matrices. (arXiv:1901.05019v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Yuan_S/0/1/0/all/0/1">Sihan Yuan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eisenstein_D/0/1/0/all/0/1">Daniel J. Eisenstein</a> Covariance matrix estimation is a persistent challenge for cosmology, often requiring a large number of synthetic mock catalogues. The off-diagonal components of the covariance matrix also make it difficult to show representative error bars on the 2PCF, since errors computed from the diagonal values of the covariance matrix greatly underestimate the uncertainties. We develop a routine for decorrelating the projected and anisotropic 2PCF with simple and scale-compact transformations on the 2PCF. These transformation matrices are modeled after the Cholesky decomposition and the symmetric squareRead More →

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 →