RAS_WEB (Page 3,782)

H0LiCOW XI: Spectroscopic/imaging survey and galaxy-group identification around the strong gravitational lens system WFI2033-4723. (arXiv:1905.08800v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Sluse_D/0/1/0/all/0/1">D. Sluse</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rusu_C/0/1/0/all/0/1">C. E. Rusu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fassnacht_C/0/1/0/all/0/1">C. D. Fassnacht</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sonnenfeld_A/0/1/0/all/0/1">A. Sonnenfeld</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Richard_J/0/1/0/all/0/1">J. Richard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Auger_M/0/1/0/all/0/1">M. W. Auger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Coccato_L/0/1/0/all/0/1">L. Coccato</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wong_K/0/1/0/all/0/1">K. C. Wong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Suyu_S/0/1/0/all/0/1">S. H. Suyu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Treu_T/0/1/0/all/0/1">T. Treu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Agnello_A/0/1/0/all/0/1">A. Agnello</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Birrer_S/0/1/0/all/0/1">S. Birrer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bonvin_V/0/1/0/all/0/1">V. Bonvin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Collett_T/0/1/0/all/0/1">T. Collett</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Courbin_F/0/1/0/all/0/1">F. Courbin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hilbert_S/0/1/0/all/0/1">S. Hilbert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koopmans_L/0/1/0/all/0/1">L. V. E. Koopmans</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tihhanova_O/0/1/0/all/0/1">O. Tihhanova</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marshall_P/0/1/0/all/0/1">P. J. Marshall</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meylan_G/0/1/0/all/0/1">G. Meylan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shajib_A/0/1/0/all/0/1">A. J. Shajib</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:+Bertin_E/0/1/0/all/0/1">E. Bertin</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.Read More →

Fast and inefficient star formation due to short-lived molecular clouds and rapid feedback. (arXiv:1905.08801v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Kruijssen_J/0/1/0/all/0/1">J. M. Diederik Kruijssen</a> (1,2), <a href="http://arxiv.org/find/astro-ph/1/au:+Schruba_A/0/1/0/all/0/1">Andreas Schruba</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Chevance_M/0/1/0/all/0/1">M&#xe9;lanie Chevance</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Longmore_S/0/1/0/all/0/1">Steven N. Longmore</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Hygate_A/0/1/0/all/0/1">Alexander P. S. Hygate</a> (2,1), <a href="http://arxiv.org/find/astro-ph/1/au:+Haydon_D/0/1/0/all/0/1">Daniel T. Haydon</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+McLeod_A/0/1/0/all/0/1">Anna F. McLeod</a> (5,6), <a href="http://arxiv.org/find/astro-ph/1/au:+Dalcanton_J/0/1/0/all/0/1">Julianne J. Dalcanton</a> (7), <a href="http://arxiv.org/find/astro-ph/1/au:+Tacconi_L/0/1/0/all/0/1">Linda J. Tacconi</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Dishoeck_E/0/1/0/all/0/1">Ewine F. van Dishoeck</a> (8,3) ((1) Heidelberg, (2) MPIA, (3) MPE, (4) LJMU, (5) Berkeley, (6) TTU, (7) Washington, (8) Leiden) The physics of star formation and the deposition of mass, momentum, and energy into the interstellar medium by massive stars (`feedback’) are theRead More →

ALMA polarimetry measures magnetically aligned dust grains in the torus of NGC 1068. (arXiv:1905.08802v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Lopez_Rodriguez_E/0/1/0/all/0/1">Enrique Lopez-Rodriguez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alonso_Herrero_A/0/1/0/all/0/1">Almudena Alonso-Herrero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garcia_Burillo_S/0/1/0/all/0/1">Santiago Garc&#xed;a-Burillo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gordon_M/0/1/0/all/0/1">Michael S. Gordon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ichikawa_K/0/1/0/all/0/1">Kohei Ichikawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Imanishi_M/0/1/0/all/0/1">Masatoshi Imanishi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kameno_S/0/1/0/all/0/1">Seiji Kameno</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Levenson_N/0/1/0/all/0/1">Nancy A. Levenson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nikutta_R/0/1/0/all/0/1">Robert Nikutta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Packham_C/0/1/0/all/0/1">Chris Packham</a> The obscuring structure surrounding active galactic nuclei (AGN) can be explained as a dust and gas flow cycle that fundamentally connects the AGN with their host galaxies. Although this structure is usually associated with dusty winds driven by radiation pressure, almost all models for the accretion onto a supermassive blackhole and outflows invoke magnetic fields, which are poorlyRead More →

The Galactic Midplane Is Not a Plane: Implications for Dynamical Analysis with Gaia Data and Beyond. (arXiv:1905.08803v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Beane_A/0/1/0/all/0/1">Angus Beane</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sanderson_R/0/1/0/all/0/1">Robyn E. Sanderson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ness_M/0/1/0/all/0/1">Melissa K. Ness</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Johnston_K/0/1/0/all/0/1">Kathryn V. Johnston</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Filho_D/0/1/0/all/0/1">Douglas Grion Filho</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Low_M/0/1/0/all/0/1">Mordecai-Mark Mac Low</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Angles_Alcazar_D/0/1/0/all/0/1">Daniel Angl&#xe9;s-Alc&#xe1;zar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hogg_D/0/1/0/all/0/1">David W. Hogg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Laporte_C/0/1/0/all/0/1">Chervin F. P. Laporte</a> Orbital properties of stars, computed from their six-dimensional phase space measurements and an assumed Galactic potential, are used to understand the structure and evolution of the Galaxy. Stellar actions, computed from orbits, have the attractive quality of being invariant under certain assumptions and are therefore used as quantitative labels of a star’sRead More →

The Exoplanet Population Observation Simulator. II – Population Synthesis in the Era of Kepler. (arXiv:1905.08804v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Mulders_G/0/1/0/all/0/1">Gijs D. Mulders</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mordasini_C/0/1/0/all/0/1">Christoph Mordasini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pascucci_I/0/1/0/all/0/1">Ilaria Pascucci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ciesla_F/0/1/0/all/0/1">Fred J. Ciesla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Emsenhuber_A/0/1/0/all/0/1">Alexandre Emsenhuber</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Apai_D/0/1/0/all/0/1">Daniel Apai</a> The collection of planetary system properties derived from large surveys such as Kepler provides critical constraints on planet formation and evolution. These constraints can only be applied to planet formation models, however, if the observational biases and selection effects are properly accounted for. Here we show how epos, the Exoplanet Population Observation Simulator, can be used to constrain planet formation models by comparing the Bern planet population synthesis modelsRead More →

Simulating the interstellar medium and stellar feedback on a moving mesh: Implementation and isolated galaxies. (arXiv:1905.08806v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Marinacci_F/0/1/0/all/0/1">Federico Marinacci</a> (1,2,3), <a href="http://arxiv.org/find/astro-ph/1/au:+Sales_L/0/1/0/all/0/1">Laura V. Sales</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Vogelsberger_M/0/1/0/all/0/1">Mark Vogelsberger</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Torrey_P/0/1/0/all/0/1">Paul Torrey</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Springel_V/0/1/0/all/0/1">Volker Springel</a> (6) ((1) Unibo, (2) CfA, (3) MIT, (4) UCR, (5) UFlorida, (6) MPA) We introduce the Stars and MUltiphase Gas in GaLaxiEs — SMUGGLE model, an explicit and comprehensive stellar feedback model for the moving-mesh code Arepo. This novel sub-resolution model resolves the multiphase gas structure of the interstellar medium and self-consistently generates gaseous outflows. The model implements crucial aspects of stellar feedback including photoionization, radiation pressure, energyRead More →

The Globular Cluster Origin of the Milky Way Outer Bulge: Evidence from Sodium Bimodality. (arXiv:1905.08809v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_Y/0/1/0/all/0/1">Young-Wook Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_J/0/1/0/all/0/1">Jenny J. Kim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Johnson_C/0/1/0/all/0/1">Christian I. Johnson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chung_C/0/1/0/all/0/1">Chul Chung</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jang_S/0/1/0/all/0/1">Sohee Jang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lim_D/0/1/0/all/0/1">Dongwook Lim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kang_Y/0/1/0/all/0/1">Yijung Kang</a> Recent investigations of the double red clump in the color-magnitude diagram of the Milky Way bulge cast serious doubts on the structure and formation origin of the outer bulge. Unlike previous interpretation based on an X-shaped bulge, stellar evolution models and CN-band observations have suggested that this feature is another manifestation of the multiple stellar population phenomenon observed in globular clusters (GCs). This new scenario requiresRead More →

The Thermal History of Composite Dark Matter. (arXiv:1905.08810v1 [hep-ph]) <a href="http://arxiv.org/find/hep-ph/1/au:+Dondi_N/0/1/0/all/0/1">Nicola Andrea Dondi</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Sannino_F/0/1/0/all/0/1">Francesco Sannino</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Smirnov_J/0/1/0/all/0/1">Juri Smirnov</a> We study the thermodynamic history of composite Dark Matter models. We start with classifying the models by means of the symmetries partially protecting the composite Dark Matter decays and constrain their lifetimes. For each model, we determine the impact of number-changing and number-conserving operators on its thermal history. We also develop the analytic formalism to calculate the asymptotic abundance of stable relics. We show how the relative strength between number-changing and number-conserving interactions together with the dark plasma lifetime affect the thermal fate of the variousRead More →

Convergence of Fourier-domain templates for inspiraling eccentric compact binaries. (arXiv:1905.08811v1 [gr-qc]) <a href="http://arxiv.org/find/gr-qc/1/au:+Tanay_S/0/1/0/all/0/1">Sashwat Tanay</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Klein_A/0/1/0/all/0/1">Antoine Klein</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Berti_E/0/1/0/all/0/1">Emanuele Berti</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Nishizawa_A/0/1/0/all/0/1">Atsushi Nishizawa</a> The space-based detector LISA may observe gravitational waves from the early inspiral of stellar-mass black hole binaries, some of which could have significant eccentricity. Current gravitational waveform templates are only valid for small orbital velocities (i.e., in a post-Newtonian expansion) and small initial eccentricity $e_0$ (“post-circular” expansion). We conventionally define $e_0$ as the eccentricity corresponding to an orbital frequency of $5 text{ mHz}$, and we study the convergence properties of frequency-domain inspiral templates that are accurate up to 2PN and order $e_0^6$Read More →

Near-Infrared Spectroscopy of Galaxies During Reionization: Measuring C$,$III] in a Galaxy at $mathbf{z=7.5}$. (arXiv:1905.08812v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Hutchison_T/0/1/0/all/0/1">Taylor A. Hutchison</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Papovich_C/0/1/0/all/0/1">Casey Papovich</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Finkelstein_S/0/1/0/all/0/1">Steven L. Finkelstein</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Dickinson_M/0/1/0/all/0/1">Mark Dickinson</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Jung_I/0/1/0/all/0/1">Intae Jung</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Zitrin_A/0/1/0/all/0/1">Adi Zitrin</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Ellis_R/0/1/0/all/0/1">Richard Ellis</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Malhotra_S/0/1/0/all/0/1">Sangeeta Malhotra</a> (6 and 7), <a href="http://arxiv.org/find/astro-ph/1/au:+Rhoads_J/0/1/0/all/0/1">James Rhoads</a> (6 and 7), <a href="http://arxiv.org/find/astro-ph/1/au:+Roberts_Borsani_G/0/1/0/all/0/1">Guido Roberts-Borsani</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Song_M/0/1/0/all/0/1">Mimi Song</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Tilvi_V/0/1/0/all/0/1">Vithal Tilvi</a> (7) ((1) Texas A and M Univ., (2) UT Austin, (3) NOAO, (4) Ben-Gurion Univ. of the Negev, (5) Univ. College London, (6) NASA Goddard, (7) Arizona State Univ.) We present Keck/MOSFIRE $H$-band spectroscopy targeting C$,$III] $lambda$1907,1909Read More →

Confirming Herschel candidate protoclusters from ALMA/VLA CO observations. (arXiv:1905.08813v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Gomez_Guijarro_C/0/1/0/all/0/1">C. G&#xf3;mez-Guijarro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Riechers_D/0/1/0/all/0/1">D. A. Riechers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pavesi_R/0/1/0/all/0/1">R. Pavesi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Magdis_G/0/1/0/all/0/1">G. E. Magdis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Leung_T/0/1/0/all/0/1">T. K. D. Leung</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Valentino_F/0/1/0/all/0/1">F. Valentino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Toft_S/0/1/0/all/0/1">S. Toft</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aravena_M/0/1/0/all/0/1">M. Aravena</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chapman_S/0/1/0/all/0/1">S. C. Chapman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Clements_D/0/1/0/all/0/1">D. L. Clements</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dannerbauer_H/0/1/0/all/0/1">H. Dannerbauer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oliver_S/0/1/0/all/0/1">S. J. Oliver</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perez_Fournon_I/0/1/0/all/0/1">I. P&#xe9;rez-Fournon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Valtchanov_I/0/1/0/all/0/1">I. Valtchanov</a> ALMA 870$mu$m continuum imaging has uncovered a population of blends of multiple dusty star-forming galaxies (DSFGs) in sources originally detected with the Herschel Space Observatory. However, their pairwise separations are much smaller that what is found by ALMA follow-up of other single-dish surveys or expected fromRead More →

A Study of the 20 Day Superorbital Modulation in the High-Mass X-ray Binary IGR J16493-4348. (arXiv:1905.08817v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Coley_J/0/1/0/all/0/1">Joel B. Coley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Corbet_R/0/1/0/all/0/1">Robin H. D. Corbet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fuerst_F/0/1/0/all/0/1">Felix Fuerst</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huxtable_G/0/1/0/all/0/1">Gregory Huxtable</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Krimm_H/0/1/0/all/0/1">Hans A. Krimm</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pearlman_A/0/1/0/all/0/1">Aaron B. Pearlman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pottschmidt_K/0/1/0/all/0/1">Katja Pottschmidt</a> We report on Nuclear Spectroscopic Telescope Array (NuSTAR), Neil Gehrels Swift Observatory (Swift) X-ray Telescope (XRT) and Swift Burst Alert Telescope (BAT) observations of IGR J16493-4348, a wind-fed Supergiant X-ray Binary (SGXB) showing significant superorbital variability. From a discrete Fourier transform of the BAT light curve, we refine its superorbital period to be 20.058 $pm$ 0.007 days. The BAT dynamic power spectrumRead More →

Spatially-resolved stellar populations and kinematics with KCWI: probing the assembly history of the massive early-type galaxy NGC 1407. (arXiv:1905.08818v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Ferre_Mateu_A/0/1/0/all/0/1">Anna Ferre-Mateu</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:+McDermid_R/0/1/0/all/0/1">Richard M. McDermid</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Romanowsky_A/0/1/0/all/0/1">Aaron J. Romanowsky</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brodie_J/0/1/0/all/0/1">Jean P. Brodie</a> Using the newly commissioned KCWI instrument on the Keck-II telescope, we analyse the stellar kinematics and stellar populations of the well-studied massive early-type galaxy (ETG) NGC 1407. We obtained high signal-to-noise integral-field-spectra for a central and an outer (around one effective radius towards the south-east direction) pointing with integration times of just 600s and 2400s, respectively. We confirm the presence of a kinematically distinct core alsoRead More →

Extragalactic Background Light: Inventory of light throughout the cosmic history. (arXiv:1905.08825v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Mattila_K/0/1/0/all/0/1">Kalevi Mattila</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Vaisanen_P/0/1/0/all/0/1">Petri V&#xe4;is&#xe4;nen</a> (2 and 3) ((1) Department of Physics, University of Helsinki, Finland (2) South African Astronomical Observatory, Cape Town, South Africa (3) Southern African Large Telescope, Cape Town, South Africa) The Extragalactic Background Light (EBL) stands for the mean surface brightness of the sky as we would see it from a representative vantage point in the intergalactic space outside of our Milky Way Galaxy. Averaged over the whole 4 pi solid angle it represents the collective light from all luminous matter radiated throughout the cosmic history. PartRead More →

12CO and 13CO J=3-2 observations toward N11 in the Large Magellanic Cloud. (arXiv:1905.08829v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Pena_M/0/1/0/all/0/1">M. Celis Pe&#xf1;a</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Paron_S/0/1/0/all/0/1">S. Paron</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rubio_M/0/1/0/all/0/1">M. Rubio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Herrera_C/0/1/0/all/0/1">C. N. Herrera</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ortega_M/0/1/0/all/0/1">M. E. Ortega</a> After 30 Doradus, N11 is the second largest and brightest nebula in the LMC. This large nebula has several OB associations with bright nebulae at its surroundings. N11 was previously mapped at the lowest rotational transitions of $^{12}$CO (J=1–0 and 2–1), and in some particular regions pointings of the $^{13}$CO J=1–0 and 2–1 lines were also performed. Using ASTE we mapped the whole extension of the N11 nebula in the $^{12}$CO J=3–2 line,Read More →

A definitive merger-AGN connection at z~0 with CFIS: mergers have an excess of AGN and AGN hosts are more frequently disturbed. (arXiv:1905.08830v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Ellison_S/0/1/0/all/0/1">Sara L. Ellison</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Viswanathan_A/0/1/0/all/0/1">Akshara Viswanathan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Patton_D/0/1/0/all/0/1">David R. Patton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bottrell_C/0/1/0/all/0/1">Connor Bottrell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McConnachie_A/0/1/0/all/0/1">Alan W. McConnachie</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gwyn_S/0/1/0/all/0/1">Stephen Gwyn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cuillandre_J/0/1/0/all/0/1">Jean-Charles Cuillandre</a> The question of whether galaxy mergers are linked to the triggering of active galactic nuclei (AGN) continues to be a topic of considerable debate. The issue can be broken down into two distinct questions: 1) Can galaxy mergers trigger AGN? 2) Are galaxy mergers the dominant AGN triggering mechanism? A complete picture of the AGN-merger connection requires thatRead More →

MOBSTER – II. Identification of rotationally variable A stars observed with emph{TESS} in Sectors 1 to 4. (arXiv:1905.08835v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Sikora_J/0/1/0/all/0/1">J. Sikora</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+David_Uraz_A/0/1/0/all/0/1">A. David-Uraz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chowdhury_S/0/1/0/all/0/1">S. Chowdhury</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bowman_D/0/1/0/all/0/1">D. M. Bowman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wade_G/0/1/0/all/0/1">G. A. Wade</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Khalack_V/0/1/0/all/0/1">V. Khalack</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kobzar_O/0/1/0/all/0/1">O. Kobzar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kochukhov_O/0/1/0/all/0/1">O. Kochukhov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Neiner_C/0/1/0/all/0/1">C. Neiner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Paunzen_E/0/1/0/all/0/1">E. Paunzen</a> Recently, high-precision optical 2~min cadence light curves obtained with emph{TESS} for targets located in the mission’s defined first four sectors have been released. The majority of these high-cadence and high-precision measurements currently span $sim28,{rm d}$, thereby allowing periodic variability occurring on timescales $lesssim14,{rm d}$ to potentially be detected. Magnetic chemically peculiar (mCP) A-type starsRead More →

Primordial migration of co-orbital satellites as a mechanism for the horseshoe orbit of Janus-Epimetheus. (arXiv:1905.08839v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Rodriguez_A/0/1/0/all/0/1">Adri&#xe1;n Rodr&#xed;guez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Correa_Otto_J/0/1/0/all/0/1">Jorge Correa-Otto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Michtchenko_T/0/1/0/all/0/1">Tatiana Michtchenko</a> We analyze the orbital motion of two natural satellites initially in co-orbital configuration with a third (guiding) satellite embedded into a circumplanetary gas disc and undergoing tidal interactions with the central planet. By solving the exact equations of motion, including the dissipative effects and the mutual gravitational perturbations, we investigate the configuration of the system soon after the guiding satellite is disrupted when crossing the Roche limit with the central planet during its orbital decay. The application is done forRead More →

Mega-Archive and the EURONEAR Tools for Datamining World Astronomical Images. (arXiv:1905.08847v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Vaduvescu_O/0/1/0/all/0/1">Ovidiu Vaduvescu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Curelaru_L/0/1/0/all/0/1">Lucian Curelaru</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Popescu_M/0/1/0/all/0/1">Marcel Popescu</a> The world astronomical image archives represent huge opportunities to time-domain astronomy sciences and other hot topics such as space defense, and astronomical observatories should improve this wealth and make it more accessible in the big data era. In 2010 we introduced the Mega-Archive database and the Mega-Precovery server for data mining images containing Solar system bodies, with focus on near Earth asteroids (NEAs). This paper presents the improvements and introduces some new related data mining tools developed during the last five years. Currently, theRead More →

The origin of the late-time luminosity of supernova 2011dh. (arXiv:1905.08861v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Maund_J/0/1/0/all/0/1">Justyn R. Maund</a> Due to the small amount of hydrogen (${leq 0.1M_{odot}}$) remaining on the surface of their progenitors, Type IIb supernovae are sensitive probes of the mass loss processes of massive stars towards the ends of their lives, including the role of binarity. We report late-time Hubble Space Telescope observations of SN 2011dh in M51, and a brief period of re-brightening and plateau in the photometric light curve, from $1.8$ to $6.2$ years after the explosion. These observations exclude the role of circumstellar interaction, however a slow rotating magnetar, a significant quantityRead More →