RAS_WEB (Page 2,271)

Towards 1% accurate galaxy cluster masses: Including baryons in weak-lensing mass inference. (arXiv:2104.06925v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Cromer_D/0/1/0/all/0/1">Dylan Cromer</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:+Miyatake_H/0/1/0/all/0/1">Hironao Miyatake</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Simet_M/0/1/0/all/0/1">Melanie Simet</a> Galaxy clusters are a promising probe of late-time structure growth, but constraints on cosmology from cluster abundances are currently limited by systematics in their inferred masses. One unmitigated systematic effect in weak-lensing mass inference is ignoring the presence of baryons and treating the entire cluster as a dark matter halo. In this work we present a new flexible model for cluster densities that captures both the baryonic and dark matter profiles, a new general technique for calculating the lensingRead More →

Influence of Ion-Neutral Damping on the Cosmic Ray Streaming Instability: MHD-PIC Simulations. (arXiv:2102.11878v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Plotnikov_I/0/1/0/all/0/1">Illya Plotnikov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ostriker_E/0/1/0/all/0/1">Eve C. Ostriker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bai_X/0/1/0/all/0/1">Xue-Ning Bai</a> We explore the physics of the gyro-resonant cosmic ray streaming instability (CRSI) including the effects of ion-neutral (IN) damping. This is the main damping mechanism in (partially-ionized) atomic and molecular gas, which are the primary components of the interstellar medium (ISM) by mass. Limitation of CRSI by IN damping is important in setting the amplitude of Alfv’en waves that scatter cosmic rays and control galactic-scale transport. Our study employs the MHD-PIC hybrid fluid-kinetic numerical technique to follow linear growth asRead More →

Constructing angular distributions of neutrinos in core collapse supernova from zero-th and first moments calibrated by full Boltzmann neutrino transport. (arXiv:2104.05729v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Nagakura_H/0/1/0/all/0/1">Hiroki Nagakura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Johns_L/0/1/0/all/0/1">Lucas Johns</a> Two-moment neutrino transport methods have been widely used for developing theoretical models of core-collapse supernova (CCSN), since they substantially reduce the computational burden inherent in the multi-dimensional neutrino-radiation hydrodynamical simulations. The approximation, however, comes at a price; the detailed structure of angular distribution of neutrinos is sacrificed, that is the main drawback of this approach. In this paper, we develop a novel method by which to construct angular distributions of neutrinos from the zero-th and firstRead More →

sMILES: A Library of Semi-Empirical MILES Stellar Spectra with Variable [$alpha$/Fe] Abundances. (arXiv:2104.04822v2 [astro-ph.SR] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Knowles_A/0/1/0/all/0/1">Adam T. Knowles</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sansom_A/0/1/0/all/0/1">Anne E. Sansom</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prieto_C/0/1/0/all/0/1">Carlos Allende Prieto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vazdekis_A/0/1/0/all/0/1">Alex Vazdekis</a> We present a new library of semi-empirical stellar spectra that is based on the empirical MILES library. A new, high resolution library of theoretical stellar spectra is generated that is specifically designed for use in stellar population studies. We test these models across their full wavelength range against other model libraries and find reasonable agreement in their predictions of spectral changes due to atmospheric $alpha$-element variations, known as differential corrections. We also test the modelsRead More →

The spatial distribution of Milky Way satellites, gaps in streams and the nature of dark matter. (arXiv:2104.03322v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Lovell_M/0/1/0/all/0/1">Mark R. Lovell</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Cautun_M/0/1/0/all/0/1">Marius Cautun</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Frenk_C/0/1/0/all/0/1">Carlos S. Frenk</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Hellwing_W/0/1/0/all/0/1">Wojciech A. Hellwing</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Newton_O/0/1/0/all/0/1">Oliver Newton</a> (5) ((1) University of Iceland, (2) Leiden, (3) ICC Durham, (4) Warsaw, (5) Lyon) The spatial distribution of Milky Way (MW) subhaloes provides an important set of observables for testing cosmological models. These include the radial distribution of luminous satellites, planar configurations, and the abundance of dark subhaloes whose existence or absence is key to distinguishing amongst dark matter models. We use the COCORead More →

Topological interaction of neutrino with photon in the magnetic field — Electroweak Hall effect. (arXiv:2104.02927v2 [hep-ph] UPDATED) <a href="http://arxiv.org/find/hep-ph/1/au:+Ishikawa_K/0/1/0/all/0/1">Kenzo Ishikawa</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Tobita_Y/0/1/0/all/0/1">Yutaka Tobita</a> Neutrino interaction with photons induced from a strong magnetic field approximation in the electroweak theory is presented. Contrary to the weak filed approximation, the interaction in the magnetized plasma has non-negligible strength and a topological form expressed by the Chern-Simons form of the neutrino current and the electromagnetic vector potential. The derivation of the interaction Lagrangian and its properties are presented. Neutrino interaction with photons induced from a strong magnetic field approximation in the electroweak theory is presented. Contrary to the weakRead More →

HST PanCET program: Non-detection of atmospheric escape in the warm Saturn-sized planet WASP-29 b. (arXiv:2103.15688v2 [astro-ph.EP] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Santos_L/0/1/0/all/0/1">L. A. dos Santos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bourrier_V/0/1/0/all/0/1">V. Bourrier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ehrenreich_D/0/1/0/all/0/1">D. Ehrenreich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sanz_Forcada_J/0/1/0/all/0/1">J. Sanz-Forcada</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lopez_Morales_M/0/1/0/all/0/1">M. L&#xf3;pez-Morales</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sing_D/0/1/0/all/0/1">D. K. Sing</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Munoz_A/0/1/0/all/0/1">A. Garc&#xed;a Mu&#xf1;oz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Henry_G/0/1/0/all/0/1">G. W. Henry</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lavvas_P/0/1/0/all/0/1">P. Lavvas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Etangs_A/0/1/0/all/0/1">A. Lecavelier des Etangs</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mikal_Evans_T/0/1/0/all/0/1">T. Mikal-Evans</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vidal_Madjar_A/0/1/0/all/0/1">A. Vidal-Madjar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wakeford_H/0/1/0/all/0/1">H. R. Wakeford</a> (Abridged) Short-period gas giant exoplanets are susceptible to intense atmospheric escape due to their large scale heights and strong high-energy irradiation. This process is thought to occur ubiquitously, but to date we have only detected direct evidence of atmospheric escape inRead More →

Implementation of Artificial Neural Networks for the Nepta-Uranian Interplanetary (NUIP) Mission. (arXiv:2103.11843v2 [astro-ph.IM] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Gore_S/0/1/0/all/0/1">Saurabh Gore</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ntumba_M/0/1/0/all/0/1">Manuel Ntumba</a> A celestial alignment between Neptune, Uranus, and Jupiter will occur in the early 2030s, allowing a slingshot around Jupiter to gain enough momentum to achieve planetary flyover capability around the two ice giants. The launch of the uranian probe for the departure windows of the NUIP mission is between January 2030 and January 2035, and the duration of the mission is between six and ten years, and the launch of the Nepta probe for the departure windows of the NUIP mission is between February 2031Read More →

Ultra-compact X-ray binaries as dual-line gravitational-wave sources. (arXiv:2103.09858v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Suvorov_A/0/1/0/all/0/1">Arthur G. Suvorov</a> By virtue of their sub-hour orbital periods, ultra-compact X-ray binaries are promising sources for the space-borne gravitational-wave interferometers LISA, Taiji, and TianQin. Some of these systems contain a neutron star primary, whose spin period can be measured directly via pulse timing, or indirectly through rotational modulations of burst phenomena. It is pointed out here that since actively accreting stars, with spin frequencies in the hundreds of Hz, may continuously emit appreciable gravitational waves due to the presence of accretion-built mountains, toroidal magnetic fields, and/or $r$-mode oscillations, such binaries are also candidateRead More →

Detecting and analysing geomorphological structures in images of comet 67P/Churyumov-Gerasimenko using Fourier transform. (arXiv:2103.00970v2 [astro-ph.EP] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Ruzicka_B/0/1/0/all/0/1">Birko-Katarina Ruzicka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schroter_M/0/1/0/all/0/1">Matthias Schr&#xf6;ter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pack_A/0/1/0/all/0/1">Andreas Pack</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boehnhardt_H/0/1/0/all/0/1">Hermann Boehnhardt</a> We present a method for automatised detection and analysis of quasi-periodic lineament structures from images at pixel-precision. The method exploits properties of the images’ frequency domain found by using the Fourier transform. We developed this method with the goal of detecting lineament structures in an image of the Hathor cliff of comet 67P/Churyumov-Gerasimenko, which are caused by layerings and furrows in the nucleus material. Using our method, we determined the orientation and wavelength-range of these structures. TheRead More →

Complexity of non-trivial sound speed in inflation. (arXiv:2102.12014v2 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Liu_L/0/1/0/all/0/1">Lei-Hua Liu</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Li_A/0/1/0/all/0/1">Ai-Chen Li</a> In this paper, we study the impact of non-trivial sound on the evolution of cosmological complexity in inflationary period. The vacuum state of curvature perturbation could be treated as squeezed states with two modes, characterized by the two most essential parameters: angle parameter $phi_k$ and squeezing parameter $r_k$. Through $Schrddot{o}dinger$ equation, one can obtain the corresponding evolution equation of $phi_k$ and $r_k$. Subsequently, the quantum circuit complexity between a squeezed vacuum state and squeezed states are evaluated in scalar curvature perturbation with a type of non-trivial sound speed. OurRead More →

Imaging low-mass planets within the habitable zone of {alpha} Centauri. (arXiv:2102.05159v2 [astro-ph.EP] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Wagner_K/0/1/0/all/0/1">K. Wagner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boehle_A/0/1/0/all/0/1">A. Boehle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pathak_P/0/1/0/all/0/1">P. Pathak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kasper_M/0/1/0/all/0/1">M. Kasper</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arsenault_R/0/1/0/all/0/1">R. Arsenault</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jakob_G/0/1/0/all/0/1">G. Jakob</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kaufl_U/0/1/0/all/0/1">U. Kaufl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Leveratto_S/0/1/0/all/0/1">S. Leveratto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maire_A/0/1/0/all/0/1">A.-L. Maire</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pantin_E/0/1/0/all/0/1">E. Pantin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Siebenmorgen_R/0/1/0/all/0/1">R. Siebenmorgen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zins_G/0/1/0/all/0/1">G. Zins</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Absil_O/0/1/0/all/0/1">O. Absil</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ageorges_N/0/1/0/all/0/1">N. Ageorges</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Apai_D/0/1/0/all/0/1">D. Apai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carlotti_A/0/1/0/all/0/1">A. Carlotti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Choquet_E/0/1/0/all/0/1">&#xc9;. Choquet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Delacroix_C/0/1/0/all/0/1">C. Delacroix</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dohlen_K/0/1/0/all/0/1">K. Dohlen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Duhoux_P/0/1/0/all/0/1">P. Duhoux</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Forsberg_P/0/1/0/all/0/1">P. Forsberg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fuenteseca_E/0/1/0/all/0/1">E. Fuenteseca</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gutruf_S/0/1/0/all/0/1">S. Gutruf</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guyon_O/0/1/0/all/0/1">O. Guyon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huby_E/0/1/0/all/0/1">E. Huby</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kampf_D/0/1/0/all/0/1">D. Kampf</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Karlsson_M/0/1/0/all/0/1">M. Karlsson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kervella_P/0/1/0/all/0/1">P. Kervella</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kirchbauer_J/0/1/0/all/0/1">J.-P. Kirchbauer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Klupar_P/0/1/0/all/0/1">P. Klupar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kolb_J/0/1/0/all/0/1">J.Read More →

The Three Hundred Project: Dynamical state of galaxy clusters and morphology from multi-wavelength synthetic maps. (arXiv:2011.09002v4 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Luca_F/0/1/0/all/0/1">Federico De Luca</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Petris_M/0/1/0/all/0/1">Marco De Petris</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yepes_G/0/1/0/all/0/1">Gustavo Yepes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cui_W/0/1/0/all/0/1">Weiguang Cui</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Knebe_A/0/1/0/all/0/1">Alexander Knebe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rasia_E/0/1/0/all/0/1">Elena Rasia</a> We study the connection between morphology and dynamical state of the simulated galaxy clusters in $zin[0,1.031]$ from THE THREE HUNDRED Project. We quantify cluster dynamical state using a combination of dynamical indicators from theoretical measures and compare this combined parameter, $chi$, with the results from morphological classifications. The dynamical state of the cluster sample shows a continuous distribution from dynamically relaxed, more abundant at lower redshift, toRead More →

Intermittent mildly magnetized jets as the source of GRBs. (arXiv:2102.00005v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Gottlieb_O/0/1/0/all/0/1">Ore Gottlieb</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bromberg_O/0/1/0/all/0/1">Omer Bromberg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Levinson_A/0/1/0/all/0/1">Amir Levinson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nakar_E/0/1/0/all/0/1">Ehud Nakar</a> Gamma-ray bursts (GRBs) are powered by relativistic jets that exhibit intermittency over a broad range of timescales – from $ sim $ ms to seconds. Previous numerical studies have shown that hydrodynamic (i.e., unmagnetized) jets that are expelled from a variable engine are subject to strong mixing of jet and cocoon material, which strongly inhibits the GRB emission. In this paper we conduct 3D RMHD simulations of mildly magnetized jets with power modulation over durations of 0.1 s and 1 s,Read More →

Forecast for cosmological parameter estimation with gravitational-wave standard sirens from the LISA-Taiji network. (arXiv:2101.11882v3 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Wang_L/0/1/0/all/0/1">Ling-Feng Wang</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Jin_S/0/1/0/all/0/1">Shang-Jie Jin</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Zhang_J/0/1/0/all/0/1">Jing-Fei Zhang</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Zhang_X/0/1/0/all/0/1">Xin Zhang</a> LISA and Taiji are expected to form a space-based gravitational-wave (GW) detection network in the future. In this work, we make a preliminary forecast for the cosmological parameter estimation with the GW standard siren observation from the LISA-Taiji network. We simulate the standard siren data based on a scenario with configuration angle of $40^{circ}$ between LISA and Taiji. Three models for the population of massive black hole binary (MBHB), i.e., pop III, Q3nod, and Q3d, are consideredRead More →

The Subarcsecond Mid-Infrared View of Local Active Galactic Nuclei. IV. The L- and M-band Imaging Atlas. (arXiv:2101.07006v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Isbell_J/0/1/0/all/0/1">Jacob W. Isbell</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Burtscher_L/0/1/0/all/0/1">Leonard Burtscher</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Asmus_D/0/1/0/all/0/1">Daniel Asmus</a> (3 and 4), <a href="http://arxiv.org/find/astro-ph/1/au:+Pott_J/0/1/0/all/0/1">J&#xf6;rg-Uwe Pott</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Couzy_P/0/1/0/all/0/1">Paul Couzy</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Stalevski_M/0/1/0/all/0/1">Marko Stalevski</a> (5 and 6), <a href="http://arxiv.org/find/astro-ph/1/au:+Rosas_V/0/1/0/all/0/1">Violeta G&#xe1;mez Rosas</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Meisenheimer_K/0/1/0/all/0/1">Klaus Meisenheimer</a> (1) ((1) Max-Planck Institute for Astronomy, (2) Sterrewacht Leiden, (3) School of Physics and Astronomy, University of Southhampton, (4) Gymnasium Schwarzenbek, (5) Astronomical Observatory, Belgrade, (6) Sterrenkundig Observatorium, Universiteit Ghent) We present the largest currently existing subarcsecond 3-5 $mu$m atlas of 119 local ($z < 0.3$) active galactic nucleiRead More →

Dynamical complexity of the Teleparallel gravity cosmology. (arXiv:2101.06347v2 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Rave_Franco_G/0/1/0/all/0/1">Geovanny A. Rave-Franco</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Escamilla_Rivera_C/0/1/0/all/0/1">Celia Escamilla-Rivera</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Said_J/0/1/0/all/0/1">Jackson Levi Said</a> The exploration of teleparallel gravity has been done from a dynamical systems point of view in order to be tested against the cosmological evolution currently observed. So far, the proposed autonomous systems have been restrictive over a constant dynamical variable, which contains information related to the dynamics on the $H_0$ value. It is therefore that in this paper we consider a generalization of the dynamical system by imposing a nonconstant degree of freedom over it which allows us to rewrite a generic autonomous dynamicalRead More →

A New Method for Aerosol Measurement using Wide-field Photometry. (arXiv:2101.03074v2 [astro-ph.IM] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Ebr_J/0/1/0/all/0/1">Jan Ebr</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Karpov_S/0/1/0/all/0/1">Sergey Karpov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eliasek_J/0/1/0/all/0/1">Ji&#x159;&#xed; Eli&#xe1;&#x161;ek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blazek_J/0/1/0/all/0/1">Ji&#x159;&#xed; Bla&#x17e;ek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cunniffe_R/0/1/0/all/0/1">Ronan Cunniffe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ebrova_I/0/1/0/all/0/1">Ivana Ebrov&#xe1;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Janecek_P/0/1/0/all/0/1">Petr Jane&#x10d;ek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jelinek_M/0/1/0/all/0/1">Martin Jel&#xed;nek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jurysek_J/0/1/0/all/0/1">Jakub Jury&#x161;ek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mandat_D/0/1/0/all/0/1">Du&#x161;an Mandat</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Masek_M/0/1/0/all/0/1">Martin Ma&#x161;ek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pech_M/0/1/0/all/0/1">Miroslav Pech</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prouza_M/0/1/0/all/0/1">Michael Prouza</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Travnicek_P/0/1/0/all/0/1">Petr Travn&#xed;&#x10d;ek</a> We present a new method to measure the vertical aerosol optical depth (VAOD) during clear nights using a wide-field imager – a CCD camera with a photographic lens on an equatorial mount. A series of 30-second exposures taken at different altitudes above the horizon can be used to measure the VAODRead More →

Cosmic antihelium-3 nuclei sensitivity of the GAPS experiment. (arXiv:2012.05834v3 [hep-ph] UPDATED) <a href="http://arxiv.org/find/hep-ph/1/au:+Saffold_N/0/1/0/all/0/1">N. Saffold</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Aramaki_T/0/1/0/all/0/1">T. Aramaki</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Bird_R/0/1/0/all/0/1">R. Bird</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Boezio_M/0/1/0/all/0/1">M. Boezio</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Boggs_S/0/1/0/all/0/1">S. E. Boggs</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Bonvicini_V/0/1/0/all/0/1">V. Bonvicini</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Campana_D/0/1/0/all/0/1">D. Campana</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Craig_W/0/1/0/all/0/1">W. W. Craig</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Doetinchem_P/0/1/0/all/0/1">P. von Doetinchem</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Everson_E/0/1/0/all/0/1">E. Everson</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Fabris_L/0/1/0/all/0/1">L. Fabris</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Fuke_H/0/1/0/all/0/1">H. Fuke</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Gahbauer_F/0/1/0/all/0/1">F. Gahbauer</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Garcia_I/0/1/0/all/0/1">I. Garcia</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Gerrity_C/0/1/0/all/0/1">C. Gerrity</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Hailey_C/0/1/0/all/0/1">C. J. Hailey</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Hayashi_T/0/1/0/all/0/1">T. Hayashi</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Kato_C/0/1/0/all/0/1">C. Kato</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Kawachi_A/0/1/0/all/0/1">A. Kawachi</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Kobayashi_S/0/1/0/all/0/1">S. Kobayashi</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Kozai_M/0/1/0/all/0/1">M. Kozai</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Lenni_A/0/1/0/all/0/1">A. Lenni</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Lowell_A/0/1/0/all/0/1">A. Lowell</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Manghisoni_M/0/1/0/all/0/1">M. Manghisoni</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Marcelli_N/0/1/0/all/0/1">N. Marcelli</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Mognet_S/0/1/0/all/0/1">S. I. Mognet</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Munakata_K/0/1/0/all/0/1">K. Munakata</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Munini_R/0/1/0/all/0/1">R. Munini</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Nakagami_Y/0/1/0/all/0/1">Y. Nakagami</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Olson_J/0/1/0/all/0/1">J.Read More →

Strategies to Detect Dark-Matter Decays with Line-Intensity Mapping. (arXiv:2012.00771v3 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Bernal_J/0/1/0/all/0/1">Jos&#xe9; Luis Bernal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caputo_A/0/1/0/all/0/1">Andrea Caputo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kamionkowski_M/0/1/0/all/0/1">Marc Kamionkowski</a> The nature of dark matter is a longstanding mystery in cosmology, which can be studied with laboratory or collider experiments, as well as astrophysical and cosmological observations. In this work, we propose realistic and efficient strategies to detect radiative products from dark-matter decays with line-intensity mapping (LIM) experiments. This radiation will behave as a line interloper for the atomic and molecular spectral lines targeted by LIM surveys. The most distinctive signatures of the contribution from dark-matter radiative decays are an extra anisotropy on theRead More →