On a possible nonequilibrium imprint in the cosmic background at low frequencies. (arXiv:1908.08876v4 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Baiesi_M/0/1/0/all/0/1">Marco Baiesi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burigana_C/0/1/0/all/0/1">Carlo Burigana</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Conti_L/0/1/0/all/0/1">Livia Conti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Falasco_G/0/1/0/all/0/1">Gianmaria Falasco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maes_C/0/1/0/all/0/1">Christian Maes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rondoni_L/0/1/0/all/0/1">Lamberto Rondoni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Trombetti_T/0/1/0/all/0/1">Tiziana Trombetti</a> The cosmic background radiation has been observed to deviate from the Planck law expected from a blackbody at $sim$ 2.7 K at frequencies below $sim 3$ GHz. We discuss the abundance of the low-energy photons from the perspective of nonequilibrium statistical mechanics. We propose a mechanism of stochastic frequency-diffusion, the counterpart to stochastic acceleration for charged particles in a turbulent plasma, to modify the standard Kompaneets equation. The resultingRead More →

Electron Ionization via Dark Matter-Electron Scattering and the Migdal Effect. (arXiv:1908.00012v3 [hep-ph] UPDATED) <a href="http://arxiv.org/find/hep-ph/1/au:+Baxter_D/0/1/0/all/0/1">Daniel Baxter</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Kahn_Y/0/1/0/all/0/1">Yonatan Kahn</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Krnjaic_G/0/1/0/all/0/1">Gordan Krnjaic</a> There are currently several existing and proposed experiments designed to probe sub-GeV dark matter (DM) using electron ionization in various materials. The projected signal rates for these experiments assume that this ionization yield arises only from DM scattering directly off electron targets, ignoring secondary ionization contributions from DM scattering off nuclear targets. We investigate the validity of this assumption and show that if sub-GeV DM couples with comparable strength to both protons and electrons, as would be the case for a dark photonRead More →

An Informational Approach to Cosmological Parameter Estimation. (arXiv:1905.07472v3 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Stephens_M/0/1/0/all/0/1">Michelle Stephens</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vannah_S/0/1/0/all/0/1">Sara Vannah</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gleiser_M/0/1/0/all/0/1">Marcelo Gleiser</a> We introduce a new approach for cosmological parameter estimation based on the information-theoretical Jensen-Shannon divergence (${cal D}_{rm JS}$), calculating it for models in the restricted parameter space ${H_0, w_0, w_a}$, where $H_0$ is the value of the Hubble constant today, and $w_0$ and $w_a$ are dark energy parameters, with the other parameters held fixed at their best-fit values from the Planck 2018 data. As an application, we investigate the $H_0$ tension between the Planck temperature power spectrum data (TT) and the local astronomical data by comparingRead More →

Understanding the neutrino mass constraints achievable by combining CMB lensing and spectroscopic galaxy surveys. (arXiv:1811.07636v4 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Boyle_A/0/1/0/all/0/1">Aoife Boyle</a> We perform a thorough examination of the neutrino mass ($M_nu$) constraints achievable by combining future spectroscopic galaxy surveys with cosmic microwave background (CMB) experiments, focusing on the contribution of CMB lensing and galaxy-CMB lensing. CMB lensing can help by breaking the $M_nu$-curvature degeneracy when combined with baryon acoustic oscillation (BAO)-only measurements, but we demonstrate this combination wastes a great deal of constraining power, as the broadband shape of the power spectrum contributes significantly to constraints. We also expand on previous work to demonstrate how cosmology-independentRead More →

Gaia Data Release 2: Kinematics of globular clusters and dwarf galaxies around the Milky Way. (arXiv:1804.09381v3 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Collaboration_Gaia/0/1/0/all/0/1">Gaia Collaboration</a>: <a href="http://arxiv.org/find/astro-ph/1/au:+Helmi_A/0/1/0/all/0/1">A. Helmi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Leeuwen_F/0/1/0/all/0/1">F. van Leeuwen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McMillan_P/0/1/0/all/0/1">P.J. McMillan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Massari_D/0/1/0/all/0/1">D. Massari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Antoja_T/0/1/0/all/0/1">T. Antoja</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Robin_A/0/1/0/all/0/1">A. Robin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lindegren_L/0/1/0/all/0/1">L. Lindegren</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bastian_U/0/1/0/all/0/1">U. Bastian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+co_authors_4/0/1/0/all/0/1">445 co-authors</a> The goal of this paper is to demonstrate the outstanding quality of the second data release of the Gaia mission and its power for constraining many different aspects of the dynamics of the satellites of the Milky Way. We focus here on determining the proper motions of 75 Galactic globular clusters, nine dwarf spheroidal galaxies, oneRead More →

Bulge formation through disc instability — I. (arXiv:2011.11629v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Devergne_T/0/1/0/all/0/1">Timoth&#xe9;e Devergne</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cattaneo_A/0/1/0/all/0/1">Andrea Cattaneo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bournaud_F/0/1/0/all/0/1">Fr&#xe9;d&#xe9;ric Bournaud</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koutsouridou_I/0/1/0/all/0/1">Ioanna Koutsouridou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Winter_A/0/1/0/all/0/1">Audrey Winter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dimauro_P/0/1/0/all/0/1">Paola Dimauro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mamon_G/0/1/0/all/0/1">Gary A. Mamon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wacher_W/0/1/0/all/0/1">William Wacher</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Varin_M/0/1/0/all/0/1">Margot Varin</a> We use simulations to study the growth of a pseudobulge in an isolated thin exponential stellar disc embedded in a static spherical halo. We observe a transition from later to earlier morphological types and an increase in bar prominence for higher disc-to-halo mass ratios, for lower disc-to-halo size ratios, and for lower halo concentrations. We compute bulge-to-total stellar mass ratios $B/T$ by fitting a two-component S’ersic-exponential surface-density distribution.Read More →

The Field Substellar Mass Function Based on the Full-sky 20-pc Census of 525 L, T, and Y Dwarfs. (arXiv:2011.11616v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Kirkpatrick_J/0/1/0/all/0/1">J. Davy Kirkpatrick</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gelino_C/0/1/0/all/0/1">Christopher R. Gelino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Faherty_J/0/1/0/all/0/1">Jacqueline K. Faherty</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meisner_A/0/1/0/all/0/1">Aaron M. Meisner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caselden_D/0/1/0/all/0/1">Dan Caselden</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schneider_A/0/1/0/all/0/1">Adam C. Schneider</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marocco_F/0/1/0/all/0/1">Federico Marocco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cayago_A/0/1/0/all/0/1">Alfred J. Cayago</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smart_R/0/1/0/all/0/1">R. L. Smart</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eisenhardt_P/0/1/0/all/0/1">Peter R. Eisenhardt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kuchner_M/0/1/0/all/0/1">Marc J. Kuchner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wright_E/0/1/0/all/0/1">Edward L. Wright</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cushing_M/0/1/0/all/0/1">Michael C. Cushing</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Allers_K/0/1/0/all/0/1">Katelyn N. Allers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gagliuffi_D/0/1/0/all/0/1">Daniella C. Bardalez Gagliuffi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burgasser_A/0/1/0/all/0/1">Adam J. Burgasser</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gagne_J/0/1/0/all/0/1">Jonathan Gagne</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Logsdon_S/0/1/0/all/0/1">Sarah E. Logsdon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Martin_E/0/1/0/all/0/1">Emily C. Martin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ingalls_J/0/1/0/all/0/1">James G. Ingalls</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lowrance_P/0/1/0/all/0/1">Patrick J. Lowrance</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abrahams_E/0/1/0/all/0/1">Ellianna S.Read More →

Detection of spark discharges in an agitated Mars dust simulant isolated from foreign surfaces. (arXiv:2006.01978v3 [astro-ph.EP] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Harper_J/0/1/0/all/0/1">Joshua M&#xe9;ndez Harper</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dufek_J/0/1/0/all/0/1">Josef Dufek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McDonald_G/0/1/0/all/0/1">George McDonald</a> Numerous laboratory experiments, starting in the Viking Lander era, have reported that frictional interactions between Martian analog dust grains can catalyze electrostatic processes (i.e. triboelectrification). Such findings have been cited to suggest that Martian dust devils and dust storms may sustain lightning storms, glow discharges, and other complex electrostatic phenomena. However, in many cases (if not most), these experiments allowed Martian dust simulant grains to contact foreign surfaces (for instance, the wall of an environmental chamber or otherRead More →

Strong detection of the CMB lensingxgalaxy weak lensingcross-correlation from ACT-DR4,PlanckLegacy and KiDS-1000. (arXiv:2011.11613v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Robertson_N/0/1/0/all/0/1">Naomi Clare Robertson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alonso_D/0/1/0/all/0/1">David Alonso</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Harnois_Deraps_J/0/1/0/all/0/1">Joachim Harnois-D&#xe9;raps</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Darwish_O/0/1/0/all/0/1">Omar Darwish</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kannawad_A/0/1/0/all/0/1">Arun Kannawad</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amon_A/0/1/0/all/0/1">Alexandra Amon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Asgari_M/0/1/0/all/0/1">Marika Asgari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bilicki_M/0/1/0/all/0/1">Maciej Bilicki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Calabrese_E/0/1/0/all/0/1">Erminia Calabrese</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Choi_S/0/1/0/all/0/1">Steve K. Choi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Devlin_M/0/1/0/all/0/1">Mark J. Devlin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dunkley_J/0/1/0/all/0/1">Jo Dunkley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dvornik_A/0/1/0/all/0/1">Andrej Dvornik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Erben_T/0/1/0/all/0/1">Thomas Erben</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferraro_S/0/1/0/all/0/1">Simone Ferraro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fortuna_M/0/1/0/all/0/1">Maria Cristina Fortuna</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Giblin_B/0/1/0/all/0/1">Benjamin Giblin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Han_D/0/1/0/all/0/1">Dongwon Han</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Heymans_C/0/1/0/all/0/1">Catherine Heymans</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hildebrandt_H/0/1/0/all/0/1">Hendrik Hildebrandt</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:+Hilton_M/0/1/0/all/0/1">Matt Hilton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ho_S/0/1/0/all/0/1">Shuay-Pwu P. Ho</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hoekstra_H/0/1/0/all/0/1">Henk Hoekstra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hubmayr_J/0/1/0/all/0/1">Johannes Hubmayr</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hughes_J/0/1/0/all/0/1">Jack Hughes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Joachimi_B/0/1/0/all/0/1">Benjamin Joachimi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Joudaki_S/0/1/0/all/0/1">Shahab Joudaki</a>, <aRead More →

HSTCosmicrays: A Python Package for Analyzing Cosmic Rays in HST Calibration Data. (arXiv:2011.11604v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Miles_N/0/1/0/all/0/1">N. D. Miles</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Deustua_S/0/1/0/all/0/1">S. Deustua</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tancredi_G/0/1/0/all/0/1">G. Tancredi</a> HSTCosmicrays is a python-based pipeline designed to find and characterize cosmic rays found in dark frames (exposures taken with the shutter closed). Dark exposures are obtained routinely by all the Hubble Space Telescope (HST) instruments for calibration. The main processing pipeline runs locally or in the cloud on AWS. To date, we have characterized more than 1.2 billion cosmic rays in ~76,000 dark frames obtained with CCDs from the four active instruments ACS/HRC, ACS/WFC, STIS, WFC3/UVIS, and the legacy instrument WFPC2.Read More →

UHECR mass composition at highest energies from anisotropy of their arrival directions. (arXiv:2011.11590v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Kuznetsov_M/0/1/0/all/0/1">M.Yu. Kuznetsov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tinyakov_P/0/1/0/all/0/1">P.G. Tinyakov</a> We propose a new method for the estimation of ultra-high energy cosmic ray (UHECR) mass composition from a distribution of their arrival directions. The method employs a test statistic (TS) based on a characteristic deflection of UHECR events with respect to the distribution of luminous matter in the local Universe. Making realistic simulations of the mock UHECR sets, we show that this TS is robust to the presence of regular Galactic magnetic field and sensitive to the mass composition of events in a set. ThisRead More →

Magnetization of the intergalactic medium in the IllustrisTNG simulations: the importance of extended, outflow-driven bubbles. (arXiv:2011.11581v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Garcia_A/0/1/0/all/0/1">Andres Aramburo Garcia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bondarenko_K/0/1/0/all/0/1">Kyrylo Bondarenko</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boyarsky_A/0/1/0/all/0/1">Alexey Boyarsky</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nelson_D/0/1/0/all/0/1">Dylan Nelson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pillepich_A/0/1/0/all/0/1">Annalisa Pillepich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sokolenko_A/0/1/0/all/0/1">Anastasia Sokolenko</a> We study the effects of galaxy formation physics on the magnetization of the intergalactic medium (IGM) using the IllustrisTNG simulations. We demonstrate that large-scale regions affected by the outflows from galaxies and clusters contain magnetic fields that are several orders of magnitude stronger than in unaffected regions with the same electron density. Moreover, like magnetic fields amplified inside galaxies, these magnetic fields do not depend on the primordial seed,Read More →

A minimal power-spectrum-based moment expansion for CMB B-mode searches. (arXiv:2011.11575v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Azzoni_S/0/1/0/all/0/1">S. Azzoni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abitbol_M/0/1/0/all/0/1">M. H. Abitbol</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alonso_D/0/1/0/all/0/1">D. Alonso</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gough_A/0/1/0/all/0/1">A. Gough</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Katayama_N/0/1/0/all/0/1">N. Katayama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matsumura_T/0/1/0/all/0/1">T. Matsumura</a> The characterization and modeling of polarized foregrounds has become a critical issue in the quest for primordial $B$-modes. A typical method to proceed is to factorize and parametrize the spectral properties of foregrounds and their scale dependence (i.e. assuming that foreground spectra are well described everywhere by their sky average). Since in reality foreground properties vary across the Galaxy, this assumption leads to inaccuracies in the model that manifest themselves as biases in the finalRead More →

Chemical modelling of dust-gas chemistry within AGB outflows III. Photoprocessing of the ice and return to the ISM. (arXiv:2011.11563v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Sande_M/0/1/0/all/0/1">M. Van de Sande</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Walsh_C/0/1/0/all/0/1">C. Walsh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Millar_T/0/1/0/all/0/1">T.J. Millar</a> To explain the properties of dust in the interstellar medium (ISM), the presence of a refractory organic mantle is necessary. The outflows of AGB stars are among the main contributors of stellar dust to the ISM. We present the first study of the refractory organic contribution of AGB stars to the ISM. Based on laboratory experiments, we included a new reaction in our extended chemical kinetics model: the photoprocessing of volatile complex ices intoRead More →

The Magellan-TESS Survey I: Survey Description and Mid-Survey Results. (arXiv:2011.11560v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Teske_J/0/1/0/all/0/1">Johanna Teske</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_S/0/1/0/all/0/1">Sharon Xuesong Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wolfgang_A/0/1/0/all/0/1">Angie Wolfgang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gan_T/0/1/0/all/0/1">Tianjun Gan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Plotnykov_M/0/1/0/all/0/1">Mykhaylo Plotnykov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Armstrong_D/0/1/0/all/0/1">David J. Armstrong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Butler_R/0/1/0/all/0/1">R. Paul Butler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cale_B/0/1/0/all/0/1">Bryson Cale</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Crane_J/0/1/0/all/0/1">Jeffrey D. Crane</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Howard_W/0/1/0/all/0/1">Ward Howard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jensen_E/0/1/0/all/0/1">Eric L. N. Jensen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Law_N/0/1/0/all/0/1">Nicholas Law</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shectman_S/0/1/0/all/0/1">Stephen A. Shectman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Plavchan_P/0/1/0/all/0/1">Peter Plavchan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Valencia_D/0/1/0/all/0/1">Diana Valencia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vanderburg_A/0/1/0/all/0/1">Andrew Vanderburg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ricker_G/0/1/0/all/0/1">George Ricker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vanderspek_R/0/1/0/all/0/1">Roland Vanderspek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Latham_D/0/1/0/all/0/1">Dave W. Latham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Seager_S/0/1/0/all/0/1">Sara Seager</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Winn_J/0/1/0/all/0/1">Joshua W. Winn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jenkins_J/0/1/0/all/0/1">Jon M. Jenkins</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Adibekyan_V/0/1/0/all/0/1">Vardan Adibekyan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barrado_D/0/1/0/all/0/1">David Barrado</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barros_S/0/1/0/all/0/1">Susana C. C. Barros</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brown_D/0/1/0/all/0/1">David J. A. Brown</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bryant_E/0/1/0/all/0/1">EdwardRead More →

Formation and dynamics of water clouds on temperate sub-Neptunes: the example of K2-18b. (arXiv:2011.11553v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Charnay_B/0/1/0/all/0/1">Benjamin Charnay</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blain_D/0/1/0/all/0/1">Doriann Blain</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bezard_B/0/1/0/all/0/1">Bruno B&#xe9;zard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Leconte_J/0/1/0/all/0/1">J&#xe9;r&#xe9;my Leconte</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Turbet_M/0/1/0/all/0/1">Martin Turbet</a> Hubble (HST) spectroscopic transit observations of the temperate sub-Neptune K2-18b were interpreted as the presence of water vapour with potential water clouds. 1D modelling studies also predict the formation of water clouds at some conditions. However, such models cannot predict the cloud cover, driven by atmospheric dynamics and thermal contrasts, and thus their real impact on spectra. The main goal of this study is to understand the formation, distribution and observational consequences of water cloudsRead More →

A new way to test the WIMP dark matter models. (arXiv:2011.11548v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Cheng_W/0/1/0/all/0/1">Wei Cheng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+He_Y/0/1/0/all/0/1">Yuan He</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Diao_J/0/1/0/all/0/1">Jin-Wang Diao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pan_Y/0/1/0/all/0/1">Yu Pan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zeng_J/0/1/0/all/0/1">Jun Zeng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_J/0/1/0/all/0/1">Jia-Wei Zhang</a> In this paper, we investigate the possibility of testing the weakly interacting massive particle (WIMP) dark matter (DM) models by applying the simplest phenomenological model which introduces an interaction term between dark energy (DE) and WIMP DM, i.e., $Q = 3gamma_{DM} Hrho_{DM}$. In general, the coupling strength $gamma_{DE}$ is close to $0$ due to the interaction between DE and WIMP DM is very weak, thus the effect of $gamma_ {DE}$ on the evolution of $Y$Read More →

Primordial Deuterium after LUNA: concordances and error budget. (arXiv:2011.11537v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Pisanti_O/0/1/0/all/0/1">Ofelia Pisanti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mangano_G/0/1/0/all/0/1">Gianpiero Mangano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Miele_G/0/1/0/all/0/1">Gennaro Miele</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mazzella_P/0/1/0/all/0/1">Pierpaolo Mazzella</a> The accurate evaluation of the nuclear reaction rates and corresponding uncertainties is an essential requisite for a precise determination of light nuclide primordial abundances. The recent measurement of the D(p,gamma)3He radiative capture cross section by the LUNA collaboration, with its order 3% error, represents an important step in improving the theoretical prediction for Deuterium produced in the early universe. In view of this recent result, we present in this paper a full analysis of its abundance, which includes a new critical study ofRead More →

Interstellar anatomy of the TeV gamma-ray peak in the IC443 supernova remnant. (arXiv:2011.11515v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+DellOva_P/0/1/0/all/0/1">P. Dell&#x27;Ova</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gusdorf_A/0/1/0/all/0/1">A. Gusdorf</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gerin_M/0/1/0/all/0/1">M. Gerin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Riquelme_D/0/1/0/all/0/1">D. Riquelme</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gusten_R/0/1/0/all/0/1">R. G&#xfc;sten</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Noriega_Crespo_A/0/1/0/all/0/1">A. Noriega-Crespo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tram_L/0/1/0/all/0/1">L.N. Tram</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Houde_M/0/1/0/all/0/1">M. Houde</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guillard_P/0/1/0/all/0/1">P. Guillard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lehmann_A/0/1/0/all/0/1">A. Lehmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lesaffre_P/0/1/0/all/0/1">P. Lesaffre</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Louvet_F/0/1/0/all/0/1">F. Louvet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marcowith_A/0/1/0/all/0/1">A. Marcowith</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Padovani_M/0/1/0/all/0/1">M. Padovani</a> Supernovae remnants (SNRs) represent a major feedback source from stars on the interstellar medium of galaxies. During the latest stage of supernovae explosions, shock waves produced by the initial blast modify the chemistry of gas and dust, inject kinetic energy in the surroundings, and may alter star formation characteristics.Read More →

An N-body population synthesis framework for the formation of moons around Jupiter-like planets. (arXiv:2011.11513v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Cilibrasi_M/0/1/0/all/0/1">Marco Cilibrasi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Szulagyi_J/0/1/0/all/0/1">Judit Szul&#xe1;gyi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grimm_S/0/1/0/all/0/1">Simon L. Grimm</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mayer_L/0/1/0/all/0/1">Lucio Mayer</a> The moons of giant planets are believed to form in situ in Circumplanetary Discs (CPDs). Here we present an N-body population synthesis framework for satellite formation around a Jupiter-like planet, in which the dust-to-gas ratio, the accretion rate of solids from the Protoplanetary Disc, the number, and the initial positions of protosatellites were randomly chosen from realistic distributions. The disc properties were from 3D radiative simulations sampled in 1D and 2D grids and evolved semi-analytically with time.Read More →