Pluto and Charon Don’t Have Enough Small Craters The New Horizons team just shared new findings about the lack of small craters on Pluto and Charon’s surface, which reveal things about the Kuiper Belt. The post Pluto and Charon Don’t Have Enough Small Craters appeared first on Universe Today. Universe Today Go to SourceRead More →
The Analogous Structure of Accretion Flows in Supermassive and Stellar Mass Black Holes. (arXiv:1903.02553v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Ruan_J/0/1/0/all/0/1">John J. Ruan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anderson_S/0/1/0/all/0/1">Scott F. Anderson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eracleous_M/0/1/0/all/0/1">Michael Eracleous</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Green_P/0/1/0/all/0/1">Paul J. Green</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Haggard_D/0/1/0/all/0/1">Daryl Haggard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+MacLeod_C/0/1/0/all/0/1">Chelsea L. MacLeod</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Runnoe_J/0/1/0/all/0/1">Jessie C. Runnoe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sobolewska_M/0/1/0/all/0/1">Malgosia Sobolewska</a> Black holes grow rapidly through the accretion of gas. As the accretion rate onto a black hole decreases, the structure of its surrounding accretion flow is believed to dramatically transition from a luminous thin disc to become quasi-spherical and radiatively inefficient. These accretion state transitions are commonly observed for stellar mass black holes in Galactic X-ray binary systems, but it isRead More →
Ionization age of iron ejecta in the Galactic Type Ia supernova remnant G306.3-0.9. (arXiv:1903.02554v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Sawada_M/0/1/0/all/0/1">Makoto Sawada</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tachibana_K/0/1/0/all/0/1">Katsuhiro Tachibana</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Uchida_H/0/1/0/all/0/1">Hiroyuki Uchida</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ito_Y/0/1/0/all/0/1">Yuta Ito</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matsumura_H/0/1/0/all/0/1">Hideaki Matsumura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bamba_A/0/1/0/all/0/1">Aya Bamba</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tsuru_T/0/1/0/all/0/1">Takeshi Go Tsuru</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tanaka_T/0/1/0/all/0/1">Takaaki Tanaka</a> We present a 190 ks observation of the Galactic supernova remnant (SNR) G306.3-0.9 with Suzaku. To study ejecta properties of this possible Type Ia SNR, the absolute energy scale at the Fe-K band was calibrated to a level of uncertainty less than 10 eV by a cross-calibration with the Hitomi microcalorimeter using the Perseus cluster spectra. This enabled us for the first time to accuratelyRead More →
Evidence of two spectral breaks in the prompt emission of Gamma Ray Bursts. (arXiv:1903.02555v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Ravasio_M/0/1/0/all/0/1">M. E. Ravasio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ghirlanda_G/0/1/0/all/0/1">G. Ghirlanda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nava_L/0/1/0/all/0/1">L. Nava</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ghisellini_G/0/1/0/all/0/1">G. Ghisellini</a> The long-lasting tension between the observed spectra of Gamma Ray Bursts (GRBs) and the predicted synchrotron emission spectrum might be solved if electrons do not completely cool. Evidence for incomplete cooling was recently found in Swift GRBs with prompt observations down to 0.1 keV and in one bright Fermi burst, GRB 160625B. Here we systematically search for evidence of incomplete cooling in the spectra of the ten brightest short and long GRBs observed by Fermi. We findRead More →
DASH: Deep Learning for the Automated Spectral Classification of Supernovae and their Hosts. (arXiv:1903.02557v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Muthukrishna_D/0/1/0/all/0/1">Daniel Muthukrishna</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Parkinson_D/0/1/0/all/0/1">David Parkinson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tucker_B/0/1/0/all/0/1">Brad Tucker</a> We present {tt DASH} (Deep Automated Supernova and Host classifier), a novel software package that automates the classification of the type, age, redshift, and host galaxy of supernova spectra. {tt DASH} makes use of a new approach which does not rely on iterative template matching techniques like all previous software, but instead classifies based on the learned features of each supernova type and age bin. It has achieved this by employing a deep convolutional neural network to train a matching algorithm.Read More →
Early Cosmological Evolution of Primordial Electromagnetic Fields. (arXiv:1903.02561v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Kobayashi_T/0/1/0/all/0/1">Takeshi Kobayashi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sloth_M/0/1/0/all/0/1">Martin S. Sloth</a> It is usually assumed that when Weyl invariance is unbroken in the electromagnetic sector, the energy density of primordial magnetic fields will redshift as radiation. Here we show that primordial magnetic fields do not exhibit radiation-like redshifting in the presence of stronger electric fields, as a consequence of Faraday’s law of induction. In particular for the standard Maxwell theory, magnetic fields on super-horizon scales can redshift as $B^2 propto a^{-6} H^{-2}$, instead of the usually assumed $a^{-4}$. Taking into account this effect for inflationary magnetogenesis can correct previous estimatesRead More →
Planet-planet scattering as the source of the highest eccentricity exoplanets. (arXiv:1903.02564v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Carrera_D/0/1/0/all/0/1">Daniel Carrera</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Raymond_S/0/1/0/all/0/1">Sean R. Raymond</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Davies_M/0/1/0/all/0/1">Melvyn B. Davies</a> Most giant exoplanets discovered by radial velocity surveys have much higher eccentricities than those in the Solar System. The planet-planet scattering mechanism has been shown to match the broad eccentricity distribution, but the highest-eccentricity planets are often attributed to Kozai-Lidov oscillations induced by a stellar companion. Here we investigate whether the highly eccentric exoplanet population can be produced entirely by scattering. We ran 500 N-body simulations of closely packed giant planet systems that became unstable under their own mutual perturbations. We findRead More →
Using Torque to Understand Barred Galaxy Models. (arXiv:1903.02566v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Petersen_M/0/1/0/all/0/1">Michael S. Petersen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weinberg_M/0/1/0/all/0/1">Martin D. Weinberg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Katz_N/0/1/0/all/0/1">Neal Katz</a> We present n-body simulations of barred galaxies to understand the dynamical mechanisms responsible for the evolution of the bar-disc-dark matter halo system. We find evidence for three distinct phases of barred galaxy evolution: assembly, secular growth, and steady-state equilibrium. Using an ensemble decomposition of the disc into orbital families, we track bar mass, geometry, and angular momentum through time and correlate the quantities with the phases of evolution. We follow the angular momentum transfer between particles and identify the dominant torque channels. We find thatRead More →
X-ray Observation of a Magnetized Hot Gas Outflow in the Galactic Center Region. (arXiv:1903.02571v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Nakashima_S/0/1/0/all/0/1">Shinya Nakashima</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koyama_K/0/1/0/all/0/1">Katsuji Koyama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_Q/0/1/0/all/0/1">Q. Daniel Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Enokiya_R/0/1/0/all/0/1">Rei Enokiya</a> We report the discovery of a $1^circ$ scale X-ray plume in the northern Galactic Center (GC) region observed with Suzaku. The plume is located at ($l$, $b$) $sim$ ($0mbox{$.!!^circ$}2$, $0mbox{$.!!^circ$}6$), east of the radio lobe reported by previous studies. No significant X-ray excesses are found inside or to the west of the radio lobe. The spectrum of the plume exhibits strong emission lines from highly ionized Mg, Si, and S that is reproduced by a thin thermalRead More →
WASP-4b Arrived Early for the TESS Mission. (arXiv:1903.02573v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Bouma_L/0/1/0/all/0/1">L. G. Bouma</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Winn_J/0/1/0/all/0/1">J. N. Winn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baxter_C/0/1/0/all/0/1">C. Baxter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bhatti_W/0/1/0/all/0/1">W. Bhatti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dai_F/0/1/0/all/0/1">F. Dai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Daylan_T/0/1/0/all/0/1">T. Daylan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Desert_J/0/1/0/all/0/1">J.-M. Désert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hill_M/0/1/0/all/0/1">M. L. Hill</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kane_S/0/1/0/all/0/1">S. R. Kane</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stassun_K/0/1/0/all/0/1">K. G. Stassun</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Villasenor_J/0/1/0/all/0/1">J. Villasenor</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ricker_G/0/1/0/all/0/1">G. R. Ricker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vanderspek_R/0/1/0/all/0/1">R. Vanderspek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Latham_D/0/1/0/all/0/1">D. W. Latham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Seager_S/0/1/0/all/0/1">S. Seager</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jenkins_J/0/1/0/all/0/1">J. M. Jenkins</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berta_Thompson_Z/0/1/0/all/0/1">Z. Berta-Thompson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Colon_K/0/1/0/all/0/1">K. Colón</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fausnaugh_M/0/1/0/all/0/1">M. Fausnaugh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Glidden_A/0/1/0/all/0/1">Ana Glidden</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guerrero_N/0/1/0/all/0/1">N. Guerrero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rodriguez_J/0/1/0/all/0/1">J. E. Rodriguez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Twicken_J/0/1/0/all/0/1">J. D. Twicken</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wohler_B/0/1/0/all/0/1">B. Wohler</a> The Transiting Exoplanet Survey Satellite (TESS) recently observed 18 transits of the hot JupiterRead More →
X-rays Studies of the Solar System. (arXiv:1903.02574v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Snios_B/0/1/0/all/0/1">Bradford Snios</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dunn_W/0/1/0/all/0/1">William R. Dunn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lisse_C/0/1/0/all/0/1">Carey M. Lisse</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Branduardi_Raymont_G/0/1/0/all/0/1">Graziella Branduardi-Raymont</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dennerl_K/0/1/0/all/0/1">Konrad Dennerl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bhardwaj_A/0/1/0/all/0/1">Anil Bhardwaj</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gladstone_G/0/1/0/all/0/1">G. Randall Gladstone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nulsen_S/0/1/0/all/0/1">Susan Nulsen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bodewits_D/0/1/0/all/0/1">Dennis Bodewits</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jackman_C/0/1/0/all/0/1">Caitriona M. Jackman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alvarado_Gomez_J/0/1/0/all/0/1">Julián D. Alvarado-Gómez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bunce_E/0/1/0/all/0/1">Emma J. Bunce</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Combi_M/0/1/0/all/0/1">Michael R. Combi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cravens_T/0/1/0/all/0/1">Thomas E. Cravens</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cumbee_R/0/1/0/all/0/1">Renata S. Cumbee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Drake_J/0/1/0/all/0/1">Jeremy J. Drake</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Elsner_R/0/1/0/all/0/1">Ronald F. Elsner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grodent_D/0/1/0/all/0/1">Denis Grodent</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hong_J/0/1/0/all/0/1">Jae Sub Hong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kharchenko_V/0/1/0/all/0/1">Vasili Kharchenko</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kraft_R/0/1/0/all/0/1">Ralph P. Kraft</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marler_J/0/1/0/all/0/1">Joan P. Marler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moschou_S/0/1/0/all/0/1">Sofia P. Moschou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mullen_P/0/1/0/all/0/1">Patrick D. Mullen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wolk_S/0/1/0/all/0/1">Scott J. Wolk</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yao_Z/0/1/0/all/0/1">Zhonghua Yao</a> X-ray observatoriesRead More →
Radio Emission from the unbound Debris of Tidal Disruption Events. (arXiv:1903.02575v1 [astro-ph.HE]) <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:+Steinberg_E/0/1/0/all/0/1">Elad Steinberg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Piran_T/0/1/0/all/0/1">Tsvi Piran</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Krolik_J/0/1/0/all/0/1">Julian H. Krolik</a> When a star gets too close to a supermassive black hole, it is torn apart by the tidal forces. Roughly half of the stellar mass becomes unbound and flies away at tremendous velocities. In this work we explore the idea that the shock produced by the interaction of the unbound debris with the ambient medium gives rise to the synchrotron radio emission observed in several TDEs. We use a moving mesh numerical simulation to study the evolution of the unboundRead More →
Helium Absorption at 1083 nm from Extended Exoplanet Atmospheres: Dependence on Stellar Radiation. (arXiv:1903.02576v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Oklopcic_A/0/1/0/all/0/1">Antonija Oklopčić</a> Strong absorption signatures in the helium line at 1083 nm have recently been detected in transmission spectra of several close-in exoplanets. This absorption line originates from neutral helium atoms in an excited, metastable 2$^3$S state. The population of helium atoms in this excited state is governed by the spectral shape and intensity of the incident stellar radiation field. We investigate what kind of stellar environments are most favorable for populating the metastable helium state in extended planetary atmospheres. Our results suggest that planets orbiting at close separationsRead More →
Segregation of Stellar-Mass Black Holes at the Galactic Center. (arXiv:1903.02578v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Emami_R/0/1/0/all/0/1">Razieh Emami</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Loeb_A/0/1/0/all/0/1">Abraham Loeb</a> (Harvard University) We simulate the star cluster near the center of the Milky Way galaxy. Using the Fokker Planck approach we consider the time evolution of the density profile of stars and stellar mass black holes (BHs) for various initial profiles. BHs sink toward the center of the galaxy where they are swallowed by SgrA*. We show that the mass loss increases the mass of SgrA* by up to 20 % for shallow initial radial profile with a power-law slope $gamma = 0.8$, and BH mass of $40Read More →
Gravitational Waves from Stellar Mass Black Holes Around SgrA*. (arXiv:1903.02579v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Emami_R/0/1/0/all/0/1">Razieh Emami</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Loeb_A/0/1/0/all/0/1">Abraham Loeb</a> (Harvard University) We consider the detectability of the gravitational wave (GW) signal from an orbiting stellar-mass black hole (BH) with a mass of order 40 $M_{odot}$ around Sgr A* at the center of the Milky Way galaxy. We simulate the sinking BHs to the center through dynamical friction and GW emission. We predict that LISA will detect of order 10 BHs at any given time with a signal-to-noise ratio $S/N > 10$. We consider the detectability of the gravitational wave (GW) signal from an orbiting stellar-mass black holeRead More →
Probing the Cosmological Evolution of Super-massive Black Holes using Tidal Disruption Flares. (arXiv:1903.02584v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Pasham_D/0/1/0/all/0/1">Dheeraj R. Pasham</a> (MIT), <a href="http://arxiv.org/find/astro-ph/1/au:+Lin_D/0/1/0/all/0/1">Dacheng Lin</a> (University of New Hampshire), <a href="http://arxiv.org/find/astro-ph/1/au:+Saxton_R/0/1/0/all/0/1">Richard Saxton</a> (Telespazio-Vega), <a href="http://arxiv.org/find/astro-ph/1/au:+Jonker_P/0/1/0/all/0/1">Peter Jonker</a> (SRON), <a href="http://arxiv.org/find/astro-ph/1/au:+Kara_E/0/1/0/all/0/1">Erin Kara</a> (UMD), <a href="http://arxiv.org/find/astro-ph/1/au:+Stone_N/0/1/0/all/0/1">Nicholas Stone</a> (Columbia), <a href="http://arxiv.org/find/astro-ph/1/au:+Maksym_P/0/1/0/all/0/1">Peter Maksym</a> (Harvard), <a href="http://arxiv.org/find/astro-ph/1/au:+Auchettl_K/0/1/0/all/0/1">Katie Auchettl</a> (DARK) The question of how supermassive black holes (SMBHs) grow over cosmic time is a major puzzle in high-energy astrophysics. One promising approach to this problem is via the study of tidal disruption flares (TDFs). These are transient events resulting from the disruption of stars by quiescent supermassive black holes at centers of galaxies. A meter-classRead More →
A High-resolution SZ View of the Warm-Hot Universe. (arXiv:1903.02595v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Mroczkowski_T/0/1/0/all/0/1">Tony Mroczkowski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nagai_D/0/1/0/all/0/1">Daisuke Nagai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Andreani_P/0/1/0/all/0/1">Paola Andreani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arnaud_M/0/1/0/all/0/1">Monique Arnaud</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bartlett_J/0/1/0/all/0/1">James Bartlett</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Battaglia_N/0/1/0/all/0/1">Nicholas Battaglia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Basu_K/0/1/0/all/0/1">Kaustuv Basu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bulbul_E/0/1/0/all/0/1">Esra Bulbul</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chluba_J/0/1/0/all/0/1">Jens Chluba</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Churazov_E/0/1/0/all/0/1">Eugene Churazov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cicone_C/0/1/0/all/0/1">Claudia Cicone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Crites_A/0/1/0/all/0/1">Abigail Crites</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DeNigris_N/0/1/0/all/0/1">Nat DeNigris</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Devlin_M/0/1/0/all/0/1">Mark Devlin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mascolo_L/0/1/0/all/0/1">Luca Di Mascolo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dicker_S/0/1/0/all/0/1">Simon Dicker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gaspari_M/0/1/0/all/0/1">Massimo Gaspari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Golwala_S/0/1/0/all/0/1">Sunil Golwala</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guglielmetti_F/0/1/0/all/0/1">Fabrizia Guglielmetti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hill_J/0/1/0/all/0/1">J. Colin Hill</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Klaassen_P/0/1/0/all/0/1">Pamela Klaassen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kitayama_T/0/1/0/all/0/1">Tetsu Kitayama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kneissl_R/0/1/0/all/0/1">Rüdiger Kneissl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kohno_K/0/1/0/all/0/1">Kotaro Kohno</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Komatsu_E/0/1/0/all/0/1">Eiichiro Komatsu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lacy_M/0/1/0/all/0/1">Mark Lacy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mason_B/0/1/0/all/0/1">Brian Mason</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nyland_K/0/1/0/all/0/1">Kristina Nyland</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Romero_C/0/1/0/all/0/1">Charles Romero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sayers_J/0/1/0/all/0/1">Jack Sayers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sehgal_N/0/1/0/all/0/1">Neelima Sehgal</a>,Read More →
The survey of Planetary Nebulae in Andromeda (M31): I. Imaging the disk and halo with MegaCam@CFHT. (arXiv:1903.02597v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Bhattacharya_S/0/1/0/all/0/1">Souradeep Bhattacharya</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arnaboldi_M/0/1/0/all/0/1">Magda Arnaboldi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hartke_J/0/1/0/all/0/1">Johanna Hartke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gerhard_O/0/1/0/all/0/1">Ortwin Gerhard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Comte_V/0/1/0/all/0/1">Valentin Comte</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McConnachie_A/0/1/0/all/0/1">Alan McConnachie</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Harris_W/0/1/0/all/0/1">William E. Harris</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caldwell_N/0/1/0/all/0/1">Nelson Caldwell</a> The Andromeda (M31) galaxy subtends nearly 100 sq. deg. on the sky, with severe contamination from the Milky Way halo stars whose surface density displays a steep gradient across the entire M31 field-of-view. Planetary Nebulae (PNe) are a population of stars firmly associated with M31, that are excellent tracers of light, chemistry and motion in galaxies. We present a 16 sq. deg.Read More →
An ALMA survey of the SCUBA-2 Cosmology Legacy Survey UKIDSS/UDS field: Source catalogue and properties. (arXiv:1903.02602v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Stach_S/0/1/0/all/0/1">S. M. Stach</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Dudzeviciute_U/0/1/0/all/0/1">U. Dudzevičiūtė</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Smail_I/0/1/0/all/0/1">I. Smail</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Swinbank_A/0/1/0/all/0/1">A. M. Swinbank</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Geach_J/0/1/0/all/0/1">J. E. Geach</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Simpson_J/0/1/0/all/0/1">J. M. Simpson</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+An_F/0/1/0/all/0/1">F. X. An</a> (4 and 1), <a href="http://arxiv.org/find/astro-ph/1/au:+Almaini_O/0/1/0/all/0/1">O. Almaini</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Arumugam_V/0/1/0/all/0/1">V. Arumugam</a> (6 and 7), <a href="http://arxiv.org/find/astro-ph/1/au:+Blain_A/0/1/0/all/0/1">A. W. Blain</a> (8), <a href="http://arxiv.org/find/astro-ph/1/au:+Chapman_S/0/1/0/all/0/1">S. C. Chapman</a> (9), <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_C/0/1/0/all/0/1">C. -C. Chen</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Conselice_C/0/1/0/all/0/1">C. J. Conselice</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Cooke_E/0/1/0/all/0/1">E. A. Cooke</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Coppin_K/0/1/0/all/0/1">K. E. K. Coppin</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Cunha_E/0/1/0/all/0/1">E. da Cunha</a> (10), <a href="http://arxiv.org/find/astro-ph/1/au:+Dunlop_J/0/1/0/all/0/1">J. S. Dunlop</a> (7), <a href="http://arxiv.org/find/astro-ph/1/au:+Farrah_D/0/1/0/all/0/1">D.Read More →
Constraining the evolution of stellar rotation using solar twins. (arXiv:1903.02630v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Lorenzo_Oliveira_D/0/1/0/all/0/1">Diego Lorenzo-Oliveira</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Melendez_J/0/1/0/all/0/1">Jorge Meléndez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Galarza_J/0/1/0/all/0/1">Jhon Yana Galarza</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ponte_G/0/1/0/all/0/1">Geisa Ponte</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Santos_L/0/1/0/all/0/1">Leonardo A. dos Santos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Spina_L/0/1/0/all/0/1">Lorenzo Spina</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bedell_M/0/1/0/all/0/1">Megan Bedell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ramirez_I/0/1/0/all/0/1">Iván Ramírez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bean_J/0/1/0/all/0/1">Jacob L. Bean</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Asplund_M/0/1/0/all/0/1">Martin Asplund</a> The stellar Rotation $vs.$ Age relation is commonly considered as a useful tool to derive reliable ages for Sun-like stars. However, in the light of kepler data, the presence of apparently old and fast rotators that do not obey the usual gyrochronology relations led to the hypothesis of weakened magnetic breaking in some stars. In this letter, we constrain theRead More →
