RAS_WEB (Page 3,811)

Dark Matter Heating vs. Rotochemical Heating in Old Neutron Stars. (arXiv:1905.02991v1 [hep-ph]) <a href="http://arxiv.org/find/hep-ph/1/au:+Hamaguchi_K/0/1/0/all/0/1">Koichi Hamaguchi</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Nagata_N/0/1/0/all/0/1">Natsumi Nagata</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Yanagi_K/0/1/0/all/0/1">Keisuke Yanagi</a> Dark matter (DM) particles in the Universe accumulate in neutron stars (NSs) through their interactions with ordinary matter. It has been known that their annihilation inside the NS core causes late-time heating, with which the surface temperature becomes a constant value of $T_s simeq (2-3) times 10^3$ K for the NS age $t gtrsim 10^{6-7}$ years. This conclusion is, however, drawn based on the assumption that the beta equilibrium is maintained in NSs throughout their life, which turns out to be invalid for rotatingRead More →

The impact of geometric distortions in multiconjugate adaptive optics astrometric observations with future extremely large telescopes. (arXiv:1905.02997v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Patti_M/0/1/0/all/0/1">M. Patti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arcidiacono_C/0/1/0/all/0/1">C. Arcidiacono</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lombini_M/0/1/0/all/0/1">M. Lombini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Diolaiti_E/0/1/0/all/0/1">E. Diolaiti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cortecchia_F/0/1/0/all/0/1">F. Cortecchia</a> Astrometry is one of the main science case which drives the requirements of the next multiconjugate adaptive optics (MCAO) systems for future extremely large telescopes. The small diffraction limited point-spread function (PSF) and the high Signal-to-Noise Ratio (SNR) of these instruments, promise astrometric precision at the level of micro-arcseconds. However, optical distortions have to be as low as possible to achieve the high demanding astrometry requirements. In addition to static distortions, theRead More →

Diurnal variation of dust and gas production in comet 67P/Churyumov-Gerasimenko at the inbound equinox as seen by OSIRIS and VIRTIS-M on board Rosetta. (arXiv:1905.03022v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Tubiana_C/0/1/0/all/0/1">C. Tubiana</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rinaldi_G/0/1/0/all/0/1">G. Rinaldi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guttler_C/0/1/0/all/0/1">C. G&#xfc;ttler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Snodgrass_C/0/1/0/all/0/1">C. Snodgrass</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shi_X/0/1/0/all/0/1">X. Shi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hu_X/0/1/0/all/0/1">X. Hu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marschall_R/0/1/0/all/0/1">R. Marschall</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fulle_M/0/1/0/all/0/1">M. Fulle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bockelee_Morvan_D/0/1/0/all/0/1">D. Bockel&#xe9;e-Morvan</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:+Capaccioni_F/0/1/0/all/0/1">F. Capaccioni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sierks_H/0/1/0/all/0/1">H. Sierks</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arnold_G/0/1/0/all/0/1">G. Arnold</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barucci_M/0/1/0/all/0/1">M. A. Barucci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bertaux_J/0/1/0/all/0/1">J.-L. Bertaux</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bertini_I/0/1/0/all/0/1">I. Bertini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bodewits_D/0/1/0/all/0/1">D. Bodewits</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Capria_M/0/1/0/all/0/1">M. T. Capria</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ciarniello_M/0/1/0/all/0/1">M. Ciarniello</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cremonese_G/0/1/0/all/0/1">G. Cremonese</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Crovisier_J/0/1/0/all/0/1">J. Crovisier</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:+Debei_S/0/1/0/all/0/1">S. Debei</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cecco_M/0/1/0/all/0/1">M. De Cecco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Deller_J/0/1/0/all/0/1">J. Deller</a>, <aRead More →

Rocky Planetesimal Formation Aided by Organics. (arXiv:1905.03029v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Homma_K/0/1/0/all/0/1">Kazuaki Homma</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Okuzumi_S/0/1/0/all/0/1">Satoshi Okuzumi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nakamoto_T/0/1/0/all/0/1">Taishi Nakamoto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ueda_Y/0/1/0/all/0/1">Yuta Ueda</a> The poor stickiness of silicate dust grains is a major obstacle to the formation of rocky planetesimals. In this study, we examine the possibility that silicate grains with an organic mantle, which we call Organic-Mantled Grains (OMGs), form planetesimals through direct coagulation. Organic mantles are commonly found in interplanetary dust particles, and laboratory experiments show that they are softer than silicates, in particular in warm environments. This, combined with the theory of particle adhesion, implies that OMGs are stickier than bare silicate grains. Because organicRead More →

Photoluminescence response of acrylic (PMMA) and polytetrafluoroethylene (PTFE) to ultraviolet light. (arXiv:1905.03044v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Araujo_G/0/1/0/all/0/1">G.R. Araujo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pollmann_T/0/1/0/all/0/1">T. Pollmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ulrich_A/0/1/0/all/0/1">A. Ulrich</a> Some publications indicate that poly(methyl methacrylate) (PMMA) and polytetrafluoroethylene (PTFE) exhibit low levels of photoluminesence (fluorescence and/or phosphorescence) when irradiated with photons in the ultraviolet (UV) to visible range. PMMA (also known as acrylic) and PTFE are commonly used to contain the liquid argon (LAr) or xenon (LXe) target material in rare-event search experiments. LAr and LXe scintillate in the vacuum UV region, and the PMMA and PTFE can be directly illuminated by these photons. Photoluminescence from support materials could cause unexpected signalsRead More →

Identification of Young Stellar Object candidates in the $Gaia$ DR2 x AllWISE catalogue with machine learning methods. (arXiv:1905.03063v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Marton_G/0/1/0/all/0/1">G. Marton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abraham_P/0/1/0/all/0/1">P. &#xc1;brah&#xe1;m</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Szegedi_Elek_E/0/1/0/all/0/1">E. Szegedi-Elek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Varga_J/0/1/0/all/0/1">J. Varga</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kun_M/0/1/0/all/0/1">M. Kun</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kospal_A/0/1/0/all/0/1">&#xc1;. K&#xf3;sp&#xe1;l</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Varga_Verebelyi_E/0/1/0/all/0/1">E. Varga-Vereb&#xe9;lyi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hodgkin_S/0/1/0/all/0/1">S. Hodgkin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Szabados_L/0/1/0/all/0/1">L. Szabados</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beck_R/0/1/0/all/0/1">R. Beck</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kiss_C/0/1/0/all/0/1">Cs. Kiss</a> The second $Gaia$ Data Release (DR2) contains astrometric and photometric data for more than 1.6 billion objects with mean $Gaia$ $G$ magnitude $Read More →

Polarization studies of Rotating Radio Transients. (arXiv:1905.03080v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Caleb_M/0/1/0/all/0/1">M. Caleb</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Straten_W/0/1/0/all/0/1">W. van Straten</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Keane_E/0/1/0/all/0/1">E. F. Keane</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bailes_A/0/1/0/all/0/1">A. Jameson. M. Bailes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barr_E/0/1/0/all/0/1">E.D. Barr</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Flynn_C/0/1/0/all/0/1">C. Flynn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ilie_C/0/1/0/all/0/1">C.D. Ilie</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Petroff_E/0/1/0/all/0/1">E. Petroff</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rogers_A/0/1/0/all/0/1">A. Rogers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stappers_B/0/1/0/all/0/1">B. W. Stappers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Krishnan_V/0/1/0/all/0/1">V. Venkatraman Krishnan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weltevrede_P/0/1/0/all/0/1">P. Weltevrede</a> We study the polarization properties of 22 known rotating radio transients (RRATs) with the 64-m Parkes radio telescope and present the Faraday rotation measures (RMs) for the 17 with linearly polarized flux exceeding the off-pulse noise by 3$sigma$. Each RM was estimated using a brute-force search over trial RMs that spanned the maximum measurable rangeRead More →

BVRI Photometry of the Classic Type II-P Supernova 2017eaw in NGC 6946: Day 3 to Day 594. (arXiv:1905.03084v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Buta_R/0/1/0/all/0/1">Ronald J. Buta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Keel_W/0/1/0/all/0/1">William C. Keel</a> Broadband $BVRI$ light curves of SN 2017eaw in NGC 6946 reveal the classic elements of a Type II-P supernova. The observations were begun on 16 May 2017 (UT), approximately 1 day after the discovery was announced, and the photometric monitoring was carried out over a period of nearly 600 days. The light curves show a well-defined plateau and an exponential tail which curves slightly at later times. An approximation to the bolometric light curve is derived and usedRead More →

J-PLUS: Discovery and characterisation of ultracool dwarfs using Virtual Observatory tools. (arXiv:1905.03139v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Solano_E/0/1/0/all/0/1">E. Solano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Martin_E/0/1/0/all/0/1">E. L. Mart&#xed;n</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caballero_J/0/1/0/all/0/1">J. A. Caballero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rodrigo_C/0/1/0/all/0/1">C. Rodrigo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Angulo_R/0/1/0/all/0/1">R. E. Angulo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alcaniz_J/0/1/0/all/0/1">J. Alcaniz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cenarro_A/0/1/0/all/0/1">A. J. Cenarro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cristobal_Hornillos_D/0/1/0/all/0/1">D. Crist&#xf3;bal-Hornillos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dupke_R/0/1/0/all/0/1">R. A. Dupke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ederoclite_A/0/1/0/all/0/1">A. Ederoclite</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jimenez_Esteban_F/0/1/0/all/0/1">F. Jim&#xe9;nez-Esteban</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hernandez_Jimenez_J/0/1/0/all/0/1">J. A. Hernandez-Jimenez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hernandez_Monteagudo_C/0/1/0/all/0/1">C. Hern&#xe1;ndez-Monteagudo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oliveira_R/0/1/0/all/0/1">R. Lopes de Oliveira</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lopez_Sanjuan_C/0/1/0/all/0/1">C. L&#xf3;pez-Sanjuan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marin_Franch_A/0/1/0/all/0/1">A. Mar&#xed;n-Franch</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oliveira_C/0/1/0/all/0/1">C. Mendes de Oliveira</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moles_M/0/1/0/all/0/1">M. Moles</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Orsi_A/0/1/0/all/0/1">A. Orsi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sobral_D/0/1/0/all/0/1">D. Sobral</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sodre_L/0/1/0/all/0/1">L. Sodr&#xe9; Jr.</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Varela_J/0/1/0/all/0/1">J. Varela</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ramio_H/0/1/0/all/0/1">H. V&#xe1;zquez Rami&#xf3;</a> Ultracool dwarfs (UCDs) are objects with spectral types equal or laterRead More →

Persistence of Technosignatures: A Comment on Lingam and Loeb. (arXiv:1905.03146v1 [physics.pop-ph]) <a href="http://arxiv.org/find/physics/1/au:+Cirkovic_M/0/1/0/all/0/1">Milan M. &#x106;irkovi&#x107;</a>, <a href="http://arxiv.org/find/physics/1/au:+Vukotic_B/0/1/0/all/0/1">Branislav Vukoti&#x107;</a>, <a href="http://arxiv.org/find/physics/1/au:+Stojanovic_M/0/1/0/all/0/1">Milan Stojanovi&#x107;</a> In a recent paper in this journal, Lingam and Loeb (2018) develop an excellent heuristic for searches for biosignatures vs. technosignatures. We consider two ways in which their approach could be extended and sharpened, with focus on durability of technosignatures. We also note an important consequence of the adopted heuristic which offers strong support to the ideas of the Dysonian SETI. In a recent paper in this journal, Lingam and Loeb (2018) develop an excellent heuristic for searches for biosignatures vs. technosignatures. We considerRead More →

Updated orbital ephemeris of the ADC source X 1822-371: a stable orbital expansion over 40 years. (arXiv:1905.03149v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Mazzola_S/0/1/0/all/0/1">S.M. Mazzola</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Iaria_R/0/1/0/all/0/1">R. Iaria</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Salvo_T/0/1/0/all/0/1">T. Di Salvo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gambino_A/0/1/0/all/0/1">A.F. Gambino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marino_A/0/1/0/all/0/1">A. Marino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burderi_L/0/1/0/all/0/1">L. Burderi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sanna_A/0/1/0/all/0/1">A. Sanna</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Riggio_A/0/1/0/all/0/1">A. Riggio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tailo_M/0/1/0/all/0/1">M. Tailo</a> The source X 1822-371 is an eclipsing compact binary system with a period close to 5.57 hr and an orbital period derivative $dot{P}_{rm orb}$ of 1.51(7)$times 10^{-10}$ s s$^{-1}$. The very large value of $dot{P}_{rm orb}$ is compatible with a super-Eddington mass transfer rate from the companion star, as suggested by X-ray and optical data. The XMM-Newton observation takenRead More →

Investigating the Diversity of Type Ia Supernova Spectra with the Open-Source Relational Database Kaepora. (arXiv:1905.02204v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Siebert_M/0/1/0/all/0/1">M. R. Siebert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Foley_R/0/1/0/all/0/1">R. J. Foley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jones_D/0/1/0/all/0/1">D. O. Jones</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Angulo_R/0/1/0/all/0/1">R. Angulo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Davis_K/0/1/0/all/0/1">K. Davis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Duarte_A/0/1/0/all/0/1">A. Duarte</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Strasburger_E/0/1/0/all/0/1">E. Strasburger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Conlon_M/0/1/0/all/0/1">M. Conlon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kazmi_N/0/1/0/all/0/1">N. Kazmi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nishimoto_R/0/1/0/all/0/1">R. Nishimoto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schubert_M/0/1/0/all/0/1">M. Schubert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sun_L/0/1/0/all/0/1">L. Sun</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tippens_R/0/1/0/all/0/1">R. Tippens</a> We present a public, open-source relational database (we name kaepora) containing a sample of 4975 spectra of 777 Type Ia supernovae (SNe Ia). Since we draw from many sources, we significantly improve the spectra by inspecting these data for quality, removing galactic emission lines and cosmic rays,Read More →

The Most Rapidly-Declining Type I Supernova 2019bkc/ATLAS19dqr. (arXiv:1905.02205v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_P/0/1/0/all/0/1">Ping Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dong_S/0/1/0/all/0/1">Subo Dong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stritzinger_M/0/1/0/all/0/1">M. D. Stritzinger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Holmbo_S/0/1/0/all/0/1">Simon Holmbo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Strader_J/0/1/0/all/0/1">Jay Strader</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:+Peng_E/0/1/0/all/0/1">Eric W. Peng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Benetti_S/0/1/0/all/0/1">S. Benetti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bersier_D/0/1/0/all/0/1">D. Bersier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brownsberger_S/0/1/0/all/0/1">Sasha Brownsberger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Buckley_D/0/1/0/all/0/1">David A. H. Buckley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gromadzki_M/0/1/0/all/0/1">Mariusz Gromadzki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moran_S/0/1/0/all/0/1">Shane Moran</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pastorello_A/0/1/0/all/0/1">A. Pastorello</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aydi_E/0/1/0/all/0/1">Elias Aydi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bose_S/0/1/0/all/0/1">Subhash Bose</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Connor_T/0/1/0/all/0/1">Thomas Connor</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Elias_Rosa_N/0/1/0/all/0/1">N. Elias-Rosa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+French_K/0/1/0/all/0/1">K. Decker French</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Holoien_T/0/1/0/all/0/1">Thomas W.-S. Holoien</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mattila_S/0/1/0/all/0/1">Seppo Mattila</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:+Stark_A/0/1/0/all/0/1">Antony A. Stark</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Swihart_S/0/1/0/all/0/1">Samuel J. Swihart</a> We report observations of the hydrogen- and helium-deficient supernova (SN) 2019bkc/ATLAS19dqr. With B- andRead More →

UV Background Fluctuations and Three-Point Correlations in the Large Scale Clustering of the Lyman-alpha Forest. (arXiv:1905.02208v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Tie_S/0/1/0/all/0/1">Suk Sien Tie</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weinberg_D/0/1/0/all/0/1">David H. Weinberg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Martini_P/0/1/0/all/0/1">Paul Martini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhu_W/0/1/0/all/0/1">Wei Zhu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Peirani_S/0/1/0/all/0/1">Sebastien Peirani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Suarez_T/0/1/0/all/0/1">Teresita Suarez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Colombi_S/0/1/0/all/0/1">Stephane Colombi</a> Using the Ly$alpha$ mass assignment scheme (LyMAS), we make theoretical predictions for the 3-dimensional 3-point correlation function (3PCF) of the Ly$alpha$ forest at redshift $z=2.3$. We bootstrap results from the (100 $h^{-1} mbox{ Mpc}$)$^3$ Horizon hydrodynamic simulation to a (1 $h^{-1}$ Gpc)$^3$ $N$-body simulation, considering both a uniform UV background (UVB) and a fluctuating UVB sourced by quasars with a comoving $n_q approx 10^{-5}$ $h^3$Read More →

The Zwicky Transient Facility: Surveys and Scheduler. (arXiv:1905.02209v1 [astro-ph.IM]) <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:+Kulkarni_S/0/1/0/all/0/1">Shrinivas R. Kulkarni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barlow_T/0/1/0/all/0/1">Tom Barlow</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Feindt_U/0/1/0/all/0/1">Ulrich Feindt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Graham_M/0/1/0/all/0/1">Matthew J. Graham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Goobar_A/0/1/0/all/0/1">Ariel Goobar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kupfer_T/0/1/0/all/0/1">Thomas Kupfer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ngeow_C/0/1/0/all/0/1">Chow-Choong Ngeow</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nugent_P/0/1/0/all/0/1">Peter Nugent</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ofek_E/0/1/0/all/0/1">Eran Ofek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prince_T/0/1/0/all/0/1">Thomas A. Prince</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Riddle_R/0/1/0/all/0/1">Reed Riddle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Walters_R/0/1/0/all/0/1">Richard Walters</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ye_Q/0/1/0/all/0/1">Quan-Zhi Ye</a> We present a novel algorithm for scheduling the observations of time-domain imaging surveys. Our Integer Linear Programming approach optimizes an observing plan for an entire night by assigning targets to temporal blocks, enabling strict control of the number of exposures obtained per field and minimizing filter changes. A subsequent optimizationRead More →

Hyper Wide Field Imaging of the Local Group Dwarf Irregular Galaxy IC 1613: An Extended Component of Metal-poor Stars. (arXiv:1905.02210v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Pucha_R/0/1/0/all/0/1">Ragadeepika Pucha</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carlin_J/0/1/0/all/0/1">Jeffrey L. Carlin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Willman_B/0/1/0/all/0/1">Beth Willman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Strader_J/0/1/0/all/0/1">Jay Strader</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sand_D/0/1/0/all/0/1">David J. Sand</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bechtol_K/0/1/0/all/0/1">Keith Bechtol</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brodie_J/0/1/0/all/0/1">Jean P. Brodie</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Crnojevic_D/0/1/0/all/0/1">Denija Crnojevi&#x107;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Forbes_D/0/1/0/all/0/1">Duncan A. Forbes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garling_C/0/1/0/all/0/1">Christopher Garling</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hargis_J/0/1/0/all/0/1">Jonathan Hargis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Peter_A/0/1/0/all/0/1">Annika H. G. Peter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Romanowsky_A/0/1/0/all/0/1">Aaron J. Romanowsky</a> Stellar halos offer direct fossil evidence for hierarchical structure formation. Since halo assembly is predicted to be scale-free, the properties of stellar halos around low-mass galaxies set strong constraints on star formation in the accreted subhalos and onRead More →

COMP2CAT: hunting compact double radio sources in the local Universe. (arXiv:1905.02212v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Jimenez_Gallardo_A/0/1/0/all/0/1">Ana Jimenez-Gallardo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Massaro_F/0/1/0/all/0/1">Francesco Massaro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Capetti_A/0/1/0/all/0/1">Alessandro Capetti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prieto_A/0/1/0/all/0/1">Almudena Prieto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Paggi_A/0/1/0/all/0/1">Alessandro Paggi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baldi_R/0/1/0/all/0/1">Ranieri D. Baldi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grossova_R/0/1/0/all/0/1">Romana Grossova</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ostorero_L/0/1/0/all/0/1">Luisa Ostorero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Siemiginowska_A/0/1/0/all/0/1">Aneta Siemiginowska</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Viada_S/0/1/0/all/0/1">Stefano Viada</a> We present a catalog of compact double radio galaxies (hereafter COMP2$CAT$) listing 43 edge-brightened radio sources whose projected linear size does not exceed 60 kpc, the typical size of their host galaxies. This is the fifth in a series of radio source catalogs recently created, namely: FRI$CAT$, FRII$CAT$, FR0$CAT$ and WAT$CAT$, each focused on a different class of radio galaxies. The mainRead More →