RAS_WEB (Page 2,252)

Star formation scaling relations at ~100 pc from PHANGS: Impact of completeness and spatial scale. (arXiv:2104.09536v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Pessa_I/0/1/0/all/0/1">I. Pessa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schinnerer_E/0/1/0/all/0/1">E. Schinnerer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Belfiore_F/0/1/0/all/0/1">F. Belfiore</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Emsellem_E/0/1/0/all/0/1">E. Emsellem</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Leroy_A/0/1/0/all/0/1">A. K. Leroy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schruba_A/0/1/0/all/0/1">A. Schruba</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kruijssen_J/0/1/0/all/0/1">J. M. D. Kruijssen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pan_H/0/1/0/all/0/1">H.-A. Pan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blanc_G/0/1/0/all/0/1">G. A. Blanc</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sanchez_Blazquez_P/0/1/0/all/0/1">P. Sanchez-Blazquez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bigiel_F/0/1/0/all/0/1">F. Bigiel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chevance_M/0/1/0/all/0/1">M. Chevance</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Congiu_E/0/1/0/all/0/1">E. Congiu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dale_D/0/1/0/all/0/1">D. Dale</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Faesi_C/0/1/0/all/0/1">C. M. Faesi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Glover_S/0/1/0/all/0/1">S. C. O. Glover</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grasha_K/0/1/0/all/0/1">K. Grasha</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Groves_B/0/1/0/all/0/1">B. Groves</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ho_I/0/1/0/all/0/1">I. Ho</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jimenez_Donaire_M/0/1/0/all/0/1">M. Jim&#xe9;nez-Donaire</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Klessen_R/0/1/0/all/0/1">R. Klessen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kreckel_K/0/1/0/all/0/1">K. Kreckel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koch_E/0/1/0/all/0/1">E. W. Koch</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_D/0/1/0/all/0/1">D. Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meidt_S/0/1/0/all/0/1">S. Meidt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pety_J/0/1/0/all/0/1">J. Pety</a>, <aRead More →

Kinematics of MgII Absorbers from the Redshift-space Distortion Around Massive Quiescent Galaxies. (arXiv:2104.09527v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Zu_Y/0/1/0/all/0/1">Ying Zu</a> (SJTU) The kinematics of MgII absorbers is the key to understanding the origin of cool, metal-enriched gas clouds in the circumgalactic medium of massive quiescent galaxies. Exploiting the fact that the cloud line-of-sight velocity distribution is the only unknown for predicting the redshift-space distortion~(RSD) of MgII absorbers from their 3D real-space distribution around galaxies, we develop a novel method to infer the cool cloud kinematics from the redshift-space galaxy-cloud cross-correlation $xi^{s}$. We measure $xi^{s}$ for ${sim}10^4$ MgII absorbers around ${sim}8{times}10^5$ CMASS galaxies at $0.4{<}z{<}0.8$. We discover thatRead More →

Light Curves of Partial Tidal Disruption Events. (arXiv:2104.08827v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_J/0/1/0/all/0/1">Jin-Hong Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shen_R/0/1/0/all/0/1">Rong-Feng Shen</a> Tidal disruption events (TDEs) can uncover the quiescent black holes (BHs) at the center of galaxies and also offer a promising method to study them. In a partial TDE (PTDE), the BH’s tidal force cannot fully disrupt the star, so the stellar core survives and only a varied portion of the stellar mass is bound to the BH and feeds it. We calculate the event rate of PTDEs and full TDEs (FTDEs). In general, the event rate of PTDEs is higher than that of FTDEs, especially for the largerRead More →

Vortex-like kinematic signal, spirals, and beam smearing effect in the HD 142527 disk. (arXiv:2103.13474v3 [astro-ph.EP] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Boehler_Y/0/1/0/all/0/1">Y. Boehler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Menard_F/0/1/0/all/0/1">F. M&#xe9;nard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Robert_C/0/1/0/all/0/1">C.M.T. Robert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Isella_A/0/1/0/all/0/1">A. Isella</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pinte_C/0/1/0/all/0/1">C. Pinte</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gonzalez_J/0/1/0/all/0/1">J.-F. Gonzalez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Plas_G/0/1/0/all/0/1">G. van der Plas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weaver_E/0/1/0/all/0/1">E. Weaver</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Teague_R/0/1/0/all/0/1">R. Teague</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garg_H/0/1/0/all/0/1">H. Garg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meheut_H/0/1/0/all/0/1">H. M&#xe9;heut</a> Vortices are one of the most promising mechanisms to locally concentrate millimeter dust grains and allow the formation of planetesimals through gravitational collapse. The outer disk around the binary system HD 142527 is known for its large horseshoe structure with azimuthal contrasts of 3-5 in the gas surface density and of about 50 inRead More →

The primary proton spectrum of the hadronic PeVatron candidate HAWC J1825-134. (arXiv:2101.10781v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Dzhatdoev_T/0/1/0/all/0/1">Timur Dzhatdoev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Podlesnyi_E/0/1/0/all/0/1">Egor Podlesnyi</a> The $gamma$-ray spectrum of the source HAWC J1825-134 measured with the High Altitude Water Cherenkov (HAWC) observatory extends beyond 200 TeV without any evidence for a steepening or cutoff. There are some indications that the $gamma$-rays detected with HAWC were produced by cosmic ray protons or nuclei colliding with the ambient gas. Assuming primary protons, we inquire which shape of the primary proton spectrum is compatible with the HAWC measurements. We find that the primary proton spectrum with the power-law shape of $gamma_{p}$=2.2 and theRead More →

The CARMENES search for exoplanets around M dwarfs, No evidence for a super-Earth in a 2-day orbit around GJ 1151. (arXiv:2103.10216v2 [astro-ph.EP] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Perger_M/0/1/0/all/0/1">M. Perger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ribas_I/0/1/0/all/0/1">I. Ribas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anglada_Escude_G/0/1/0/all/0/1">G. Anglada-Escud&#xe9;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Morales_J/0/1/0/all/0/1">J. C. Morales</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amado_P/0/1/0/all/0/1">P. J. Amado</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:+Quirrenbach_A/0/1/0/all/0/1">A. Quirrenbach</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reiners_A/0/1/0/all/0/1">A. Reiners</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bejar_V/0/1/0/all/0/1">V. J. S. B&#xe9;jar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dreizler_S/0/1/0/all/0/1">S. Dreizler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Galadi_Enriquez_D/0/1/0/all/0/1">D. Galad&#xed;-Enr&#xed;quez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hatzes_A/0/1/0/all/0/1">A. P. Hatzes</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:+Jeffers_S/0/1/0/all/0/1">S. V. Jeffers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kaminski_A/0/1/0/all/0/1">A. Kaminski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kurster_M/0/1/0/all/0/1">M. K&#xfc;rster</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lafarga_M/0/1/0/all/0/1">M. Lafarga</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Montes_D/0/1/0/all/0/1">D. Montes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pale_E/0/1/0/all/0/1">E. Pal&#xe9;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rodriguez_Lopez_C/0/1/0/all/0/1">C. Rodr&#xed;guez-L&#xf3;pez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schweitzer_A/0/1/0/all/0/1">A. Schweitzer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Osorio_M/0/1/0/all/0/1">M. R. Zapatero Osorio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zechmeister_M/0/1/0/all/0/1">M. Zechmeister</a> The interaction between Earth-likeRead More →

Constraints on the antistar fraction in the Solar system neighborhood from the 10-years Fermi Large Area Telescope gamma-ray source catalog. (arXiv:2103.10073v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Dupourque_S/0/1/0/all/0/1">Simon Dupourqu&#xe9;</a> (IRAP), <a href="http://arxiv.org/find/astro-ph/1/au:+Tibaldo_L/0/1/0/all/0/1">Luigi Tibaldo</a> (IRAP), <a href="http://arxiv.org/find/astro-ph/1/au:+Ballmoos_P/0/1/0/all/0/1">Peter von Ballmoos</a> (IRAP) It is generally taken for granted that our Universe is free of antimatter objects and domains. This certitude has recently been challenged by the possible detection of anti-helium nuclei by AMS-02. Should the observation be confirmed, the existence of nearby antistars would make a plausible hypothesis to explain the origin of the antinuclei. In this paper we use the 10-years Fermi Large Area Telescope (LAT) gamma-ray source catalog toRead More →

Multi-wavelength View of the Type IIn Zoo: Optical to X-ray Emission Model of Interaction-Powered Supernovae. (arXiv:2103.08338v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Tsuna_D/0/1/0/all/0/1">Daichi Tsuna</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kashiyama_K/0/1/0/all/0/1">Kazumi Kashiyama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shigeyama_T/0/1/0/all/0/1">Toshikazu Shigeyama</a> Transients powered by interaction with the circumstellar medium (CSM) are often observed in wavelengths other than optical, and multi-wavelength modelling can be important when inferring the properties of the explosion and CSM, or for distinguishing from other powering mechanisms. We develop a model calculating time dependent emission spectrum of interaction-powered transients. We solve energy equations of electron-proton plasma in the shocked SN ejecta and CSM and a radiation transfer equation out to the outer edge of the CSM,Read More →

Detection of GeV Gamma-Ray Emission of Kepler’s SNR with Fermi-LAT. (arXiv:2103.07824v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Xiang_Y/0/1/0/all/0/1">Yunchuan Xiang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+jiang_Z/0/1/0/all/0/1">Zejun jiang</a> A likely detection of $gamma$-ray emission from the region of Kepler’s SNR is reported by analyzing $sim$12 years of Pass 8 data of textit{Fermi} Large Area Telescope. Its photon flux is $rm (4.85pm0.60)times 10^{-10} ~ ph$ $rm cm^{-2} s^{-1}$ with $sim$4$sigma$ significance in 0.2$-$500 GeV. Moreover, our results show that there is no significant variability in the light curve of $sim$12 years, and its position can well overlap with the observation result of Chandra in hard X-ray band with a good spatial resolution of 0.5$^{”}$, soRead More →

The Be Star 66 Ophiuchi: 60 Years of Disk Evolution. (arXiv:2103.06948v2 [astro-ph.SR] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Marr_K/0/1/0/all/0/1">Keegan C. Marr</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jones_C/0/1/0/all/0/1">Carol E. Jones</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carciofi_A/0/1/0/all/0/1">Alex C. Carciofi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rubio_A/0/1/0/all/0/1">Amanda C. Rubio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mota_B/0/1/0/all/0/1">Bruno C. Mota</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ghoreyshi_M/0/1/0/all/0/1">Mohammad R. Ghoreyshi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hatfield_D/0/1/0/all/0/1">Daniel W. Hatfield</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rimulo_L/0/1/0/all/0/1">Leandro R. R&#xed;mulo</a> We use a time-dependent hydrodynamic code and a non-LTE Monte Carlo code to model disk dissipation for the Be star 66 Ophiuchi. We compiled 63 years of observations from 1957 to 2020 to encompass the complete history of the growth and subsequent dissipation of the star’s disk. Our models are constrained by new and archival photometry, spectroscopy and polarization observations,Read More →

Supernova 1987A: 3D Mixing and light curves for explosion models based on binary-merger progenitors. (arXiv:2102.09686v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Utrobin_V/0/1/0/all/0/1">V. P. Utrobin</a> (1,2,3), <a href="http://arxiv.org/find/astro-ph/1/au:+Wongwathanarat_A/0/1/0/all/0/1">A. Wongwathanarat</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Janka_H/0/1/0/all/0/1">H.-Th. Janka</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Mueller_E/0/1/0/all/0/1">E. Mueller</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Ertl_T/0/1/0/all/0/1">T. Ertl</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Menon_A/0/1/0/all/0/1">A. Menon</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Heger_A/0/1/0/all/0/1">A. Heger</a> (5,6,7,8) ((1) MPA, Garching, (2) ITEP, Moscow, (3) Institute of Astronomy, Moscow, (4) University of Amsterdam, (5) Monash University, Australia, (6) OZGRAV, Melbourne, (7) ASTRO-3D, Melbourne, (8) Michigan State University) Six binary-merger progenitors of Supernova 1987A (SN 1987A) with properties close to those of the blue supergiant Sanduleak -69 202 are exploded by neutrino heating and evolved until long afterRead More →

On the Evolution of Supermassive Primordial Stars in Cosmological Flows. (arXiv:2102.08963v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Woods_T/0/1/0/all/0/1">Tyrone E. Woods</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Patrick_S/0/1/0/all/0/1">Samuel Patrick</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Elford_J/0/1/0/all/0/1">Jacob S. Elford</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Whalen_D/0/1/0/all/0/1">Daniel J. Whalen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Heger_A/0/1/0/all/0/1">Alexander Heger</a> Primordial supermassive stars (SMSs) formed in atomic-cooling halos at z ~ 15 – 20 are leading candidates for the seeds of the first quasars. Past numerical studies of the evolution of SMSs have typically assumed constant accretion rates rather than the highly variable flows in which they form. We model the evolution of SMSs in the cosmological flows that create them using the Kepler stellar evolution and implicit hydrodynamics code. We find that theyRead More →

Neutrino signal dependence on gamma-ray burst emission mechanism. (arXiv:2102.02223v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Pitik_T/0/1/0/all/0/1">Tetyana Pitik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tamborra_I/0/1/0/all/0/1">Irene Tamborra</a> (Niels Bohr Institute), <a href="http://arxiv.org/find/astro-ph/1/au:+Petropoulou_M/0/1/0/all/0/1">Maria Petropoulou</a> (University of Athens) Long duration gamma-ray bursts (GRBs) are among the least understood astrophysical transients powering the high-energy universe. To date, various mechanisms have been proposed to explain the observed electromagnetic GRB emission. In this work, we show that, although different jet models may be equally successful in fitting the observed electromagnetic spectral energy distributions, the neutrino production strongly depends on the adopted emission and dissipation model. To this purpose, we compute the neutrino production for a benchmark high-luminosity GRB in theRead More →

The Supersonic Project: SIGOs, a Proposed Progenitor to Globular Clusters, and their Connections to Gravitational Wave Anisotropies. (arXiv:2104.11226v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Lake_W/0/1/0/all/0/1">William Lake</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Naoz_S/0/1/0/all/0/1">Smadar Naoz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chiou_Y/0/1/0/all/0/1">Yeou S. Chiou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burkhart_B/0/1/0/all/0/1">Blakesley Burkhart</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marinacci_F/0/1/0/all/0/1">Federico Marinacci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vogelsberger_M/0/1/0/all/0/1">Mark Vogelsberger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kremer_K/0/1/0/all/0/1">Kyle Kremer</a> Supersonically Induced Gas Objects (SIGOs), are structures with little to no dark matter component predicted to exist in regions of the Universe with large relative velocities between baryons and dark matter at the time of recombination. They have been suggested to be the progenitors of present-day globular clusters. Using simulations, SIGOs have been studied on small scales (around 2 Mpc), where these relative velocitiesRead More →

First light of a holographic aperture mask: Observation at the Keck OSIRIS Imager. (arXiv:2104.11210v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Doelman_D/0/1/0/all/0/1">David S. Doelman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wardenier_J/0/1/0/all/0/1">Joost P. Wardenier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tuthill_P/0/1/0/all/0/1">Peter Tuthill</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fitzgerald_M/0/1/0/all/0/1">Michael P. Fitzgerald</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lyke_J/0/1/0/all/0/1">Jim Lyke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sallum_S/0/1/0/all/0/1">Steph Sallum</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Norris_B/0/1/0/all/0/1">Barnaby Norris</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Warriner_N/0/1/0/all/0/1">N. Zane Warriner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Keller_C/0/1/0/all/0/1">Christoph Keller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Escuti_M/0/1/0/all/0/1">Michael J. Escuti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Snik_F/0/1/0/all/0/1">Frans Snik</a> We report on the design, construction, and commissioning of a prototype aperture masking technology implemented at the Keck OSIRIS Imager: the holographic aperture mask. Holographic aperture masking (HAM) aims at (i) increasing the throughput of sparse aperture masking (SAM) by selectively combining all subapertures across a telescope pupil in multiple interferograms usingRead More →

HST PanCET Program: A Complete Near-UV to Infrared Transmission Spectrum for the Hot Jupiter WASP-79b. (arXiv:2104.10688v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Rathcke_A/0/1/0/all/0/1">Alexander D. Rathcke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+MacDonald_R/0/1/0/all/0/1">Ryan J. MacDonald</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barstow_J/0/1/0/all/0/1">Joanna K. Barstow</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Goyal_J/0/1/0/all/0/1">Jayesh M. Goyal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lopez_Morales_M/0/1/0/all/0/1">Mercedes Lopez-Morales</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mendonca_J/0/1/0/all/0/1">Jo&#xe3;o M. Mendon&#xe7;a</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sanz_Forcada_J/0/1/0/all/0/1">Jorge Sanz-Forcada</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Henry_G/0/1/0/all/0/1">Gregory W. Henry</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sing_D/0/1/0/all/0/1">David K. Sing</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alam_M/0/1/0/all/0/1">Munazza K. Alam</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lewis_N/0/1/0/all/0/1">Nikole K. Lewis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chubb_K/0/1/0/all/0/1">Katy L. Chubb</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Taylor_J/0/1/0/all/0/1">Jake Taylor</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nikolov_N/0/1/0/all/0/1">Nikolay Nikolov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Buchhave_L/0/1/0/all/0/1">Lars A. Buchhave</a> We present a new optical transmission spectrum of the hot Jupiter WASP-79b. We observed three transits with the STIS instrument mounted on HST, spanning 0.3 – 1.0 um. Combining these transits withRead More →

ExoMol molecular line lists — XLII: Rovibronic molecular line list for the low-lying states of NO. (arXiv:2104.10854v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Qu_Q/0/1/0/all/0/1">Qianwei Qu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yurchenko_S/0/1/0/all/0/1">Sergei N. Yurchenko</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tennyson_J/0/1/0/all/0/1">Jonathan Tennyson</a> An accurate line list, called XABC, is computed for nitric oxide which covers its pure rotational, vibrational and rovibronic spectra. A mixture of empirical and theoretical electronic transition dipole moments are used for the final calculation of $^{14}mathrm{N}^{16}mathrm{O}$ rovibronic $mathrm{A},^2Sigma^+$ — $mathrm{X},^2Pi$, $mathrm{B},^2Pi$ — $mathrm{X}^2Pi$ and $mathrm{C},^2Pi$ — $mathrm{X},^2Pi$ which correspond to the $gamma$, $beta$ and $delta$ band systems, respectively, as well as minor improvements to transitions within the $mathrm{X},^2Pi$ ground state. The work is a majorRead More →

Identification of a new spectral signature at 3 {mu}m over Martian northern high latitudes: implications for surface composition. (arXiv:2104.10924v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Stcherbinine_A/0/1/0/all/0/1">Aur&#xe9;lien Stcherbinine</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vincendon_M/0/1/0/all/0/1">Mathieu Vincendon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Montmessin_F/0/1/0/all/0/1">Franck Montmessin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beck_P/0/1/0/all/0/1">Pierre Beck</a> Mars northern polar latitudes are known to harbor an enhanced 3 ${mu}$m spectral signature when observed from orbit. This may indicate a greater amount of surface adsorbed or bound water, although it has not yet been possible to easily reconcile orbital observations with ground measurements by Phoenix. Here we reprocessed OMEGA/Mars Express observations acquired during the Northern summer to further characterize this 3 ${mu}$m absorption band increase. We identify the presence of aRead More →

Weakened magnetic braking supported by asteroseismic rotation rates of Kepler dwarfs. (arXiv:2104.10919v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Hall_O/0/1/0/all/0/1">Oliver J. Hall</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Davies_G/0/1/0/all/0/1">Guy R. Davies</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Saders_J/0/1/0/all/0/1">Jennifer van Saders</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nielsen_M/0/1/0/all/0/1">Martin B. Nielsen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lund_M/0/1/0/all/0/1">Mikkel N. Lund</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chaplin_W/0/1/0/all/0/1">William J. Chaplin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garcia_R/0/1/0/all/0/1">Rafael A. Garc&#xed;a</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amard_L/0/1/0/all/0/1">Louis Amard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Breimann_A/0/1/0/all/0/1">Angela A. Breimann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Khan_S/0/1/0/all/0/1">Saniya Khan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+See_V/0/1/0/all/0/1">Victor See</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tayar_J/0/1/0/all/0/1">Jamie Tayar</a> Studies using asteroseismic ages and rotation rates from star-spot rotation have indicated that standard age-rotation relations may break down roughly half-way through the main sequence lifetime, a phenomenon referred to as weakened magnetic braking. While rotation rates from spots can be difficult to determine for older, less activeRead More →

PGC 38025: A Star-forming Lenticular Galaxy With an Off-nuclear Star-forming Core. (arXiv:2104.10909v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Zhengyi_C/0/1/0/all/0/1">Chen Zhengyi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Qiu_Sheng_G/0/1/0/all/0/1">Gu Qiu-Sheng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garcia_Benito_R/0/1/0/all/0/1">Rub&#xe9;n Garc&#xed;a-Benito</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhi_Yu_Z/0/1/0/all/0/1">Zhang Zhi-Yu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xue_G/0/1/0/all/0/1">Ge Xue</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mengyuan_X/0/1/0/all/0/1">Xiao Mengyuan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xiaoling_Y/0/1/0/all/0/1">Yu Xiaoling</a> Lenticular galaxies (S0s) were considered mainly as passive evolved spirals due to environmental effects for a long time; however, most S0s in the field cannot fit into this common scenario. In this work, we study one special case, SDSS J120237.07+642235.3 (PGC 38025), a star-forming field S0 galaxy with an off-nuclear blue core. We present optical integral field spectroscopic (IFS) observation with the 3.5 meter telescope at Calar Alto (CAHA) Observatory, andRead More →