RAS_WEB (Page 2,431)

Design and Sensitivity of the Radio Neutrino Observatory in Greenland (RNO-G). (arXiv:2010.12279v3 [astro-ph.IM] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Aguilar_J/0/1/0/all/0/1">J. A. Aguilar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Allison_P/0/1/0/all/0/1">P. Allison</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beatty_J/0/1/0/all/0/1">J. J. Beatty</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bernhoff_H/0/1/0/all/0/1">H. Bernhoff</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Besson_D/0/1/0/all/0/1">D. Besson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bingefors_N/0/1/0/all/0/1">N. Bingefors</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Botner_O/0/1/0/all/0/1">O. Botner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Buitink_S/0/1/0/all/0/1">S. Buitink</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carter_K/0/1/0/all/0/1">K. Carter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Clark_B/0/1/0/all/0/1">B. A. Clark</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Connolly_A/0/1/0/all/0/1">A. Connolly</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dasgupta_P/0/1/0/all/0/1">P. Dasgupta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kockere_S/0/1/0/all/0/1">S. de Kockere</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vries_K/0/1/0/all/0/1">K. D. de Vries</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Deaconu_C/0/1/0/all/0/1">C. Deaconu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DuVernois_M/0/1/0/all/0/1">M. A. DuVernois</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Feigl_N/0/1/0/all/0/1">N. Feigl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garcia_Fernandez_D/0/1/0/all/0/1">D. Garcia-Fernandez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Glaser_C/0/1/0/all/0/1">C. Glaser</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hallgren_A/0/1/0/all/0/1">A. Hallgren</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hallmann_S/0/1/0/all/0/1">S. Hallmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hanson_J/0/1/0/all/0/1">J. C. Hanson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hendricks_B/0/1/0/all/0/1">B. Hendricks</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hokanson_Fasig_B/0/1/0/all/0/1">B. Hokanson-Fasig</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hornhuber_C/0/1/0/all/0/1">C. Hornhuber</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hughes_K/0/1/0/all/0/1">K. Hughes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Karle_A/0/1/0/all/0/1">A. Karle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kelley_J/0/1/0/all/0/1">J.Read More →

Vector modes in $Lambda$CDM: the gravitomagnetic potential in dark matter haloes from relativistic $N$-body simulations. (arXiv:2010.08257v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Barrera_Hinojosa_C/0/1/0/all/0/1">Cristian Barrera-Hinojosa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_B/0/1/0/all/0/1">Baojiu Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bruni_M/0/1/0/all/0/1">Marco Bruni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+He_J/0/1/0/all/0/1">Jian-hua He</a> We investigate the transverse modes of the gravitational and velocity fields in $Lambda$CDM, based on a high-resolution simulation performed using the adaptive-mesh refinement general-relativistic $N$-body code GRAMSES. We study the generation of vorticity in the dark matter velocity field at low redshift, providing fits to the shape and evolution of its power spectrum over a range of scales. By analysing the gravitomagnetic vector potential, which is absent in Newtonian simulations, in dark matter haloes withRead More →

Bolometric Night Sky Temperature and Subcooling of Telescope Structures. (arXiv:2010.01978v2 [astro-ph.IM] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Holzlohner_R/0/1/0/all/0/1">Ronald Holzl&#xf6;hner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kimeswenger_S/0/1/0/all/0/1">Stefan Kimeswenger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kausch_W/0/1/0/all/0/1">Wolfgang Kausch</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Noll_S/0/1/0/all/0/1">Stefan Noll</a> Context. The term sky temperature is used in the literature in different contexts which often leads to confusion. In this work, we study $T_text{sky}$, the effective bolometric sky temperature at which a hemispherical black body would radiate the same power onto a flat horizontal structure on the ground as the night sky, integrated over the entire thermal wavelength range of $1-100,mu$m. We then analyze the thermal physics of radiative cooling with special focus on telescopes and discuss mitigation strategies. Aims. TheRead More →

The Cosmological Perturbation Theory on the Geodesic Light-Cone background. (arXiv:2009.14134v2 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Fanizza_G/0/1/0/all/0/1">Giuseppe Fanizza</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Marozzi_G/0/1/0/all/0/1">Giovanni Marozzi</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Medeiros_M/0/1/0/all/0/1">Matheus Medeiros</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Schiaffino_G/0/1/0/all/0/1">Gloria Schiaffino</a> Inspired by the fully non-linear Geodesic Light-Cone (GLC) gauge, we consider its analogous set of coordinates which describes the unperturbed Universe. Given this starting point, we then build a cosmological perturbation theory on top of it, study the gauge transformation properties related to this new set of perturbations and show the connection with standard cosmological perturbation theory. In particular, we obtain which gauge in standard perturbation theory corresponds to the GLC gauge, and put in evidence how this is a usefulRead More →

Stellar Tidal Disruption Events with Abundances and Realistic Structures (STARS): Library of Fallback Rates. (arXiv:2007.10996v3 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Law_Smith_J/0/1/0/all/0/1">Jamie A.P. Law-Smith</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Coulter_D/0/1/0/all/0/1">David A. Coulter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guillochon_J/0/1/0/all/0/1">James Guillochon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mockler_B/0/1/0/all/0/1">Brenna Mockler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ramirez_Ruiz_E/0/1/0/all/0/1">Enrico Ramirez-Ruiz</a> We present the STARS library, a grid of tidal disruption event (TDE) simulations interpolated to provide the mass fallback rate ($dM/dt$) to the black hole for a main-sequence star of any stellar mass, stellar age, and impact parameter. We use a one-dimensional stellar evolution code to construct stars with accurate stellar structures and chemical abundances, then perform tidal disruption simulations in a three-dimensional adaptive-mesh hydrodynamics code with a Helmholtz equation ofRead More →

Growth of stellar mass black holes in dense molecular clouds and GW190521. (arXiv:2009.11326v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Rice_J/0/1/0/all/0/1">Jared R. Rice</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_B/0/1/0/all/0/1">Bing Zhang</a> A stellar mass black hole can grow its mass noticeably through Bondi accretion, if it is embedded in an extremely dense and massive molecular cloud with slow motion with respect to the ambient medium for an extended period of time. This provides a novel, yet challenging channel for the formation of massive stellar-mass black holes. We discuss how this channel may account for the massive binary black hole merger system GW190521 as observed by LIGO/Virgo gravitational wave detectors as well as the claimedRead More →

Propagation Effects in Quiet Sun Observations at Meter Wavelengths. (arXiv:2009.10604v2 [astro-ph.SR] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Sharma_R/0/1/0/all/0/1">Rohit Sharma</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oberoi_D/0/1/0/all/0/1">Divya Oberoi</a> Quiet sun meterwave emission arises from thermal bremsstrahlung in the MK corona, and can potentially be a rich source of coronal diagnostics. On its way to the observer, it gets modified substantially due to the propagation effects – primarily refraction and scattering – through the magnetized and turbulent coronal medium, leading to the redistribution of the intensity in the image plane. By comparing the full-disk meterwave solar maps during a quiet solar period and the modelled thermal bremsstrahlung emission, we characterise these propagation effects. The solar radioRead More →

Chondrules from high-velocity collisions: thermal histories and the agglomeration problem. (arXiv:2009.10093v3 [astro-ph.EP] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Choksi_N/0/1/0/all/0/1">Nick Choksi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chiang_E/0/1/0/all/0/1">Eugene Chiang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Connolly_H/0/1/0/all/0/1">Harold C. Connolly Jr.</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gainsforth_Z/0/1/0/all/0/1">Zack Gainsforth</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Westphal_A/0/1/0/all/0/1">Andrew J. Westphal</a> We assess whether chondrules, once-molten mm-sized spheres filling the oldest meteorites, could have formed from super-km/s collisions between planetesimals in the solar nebula. High-velocity collisions release hot and dense clouds of silicate vapor which entrain and heat chondrule precursors. We show how chondrule thermal histories may be reproduced in sufficiently massive vapor clouds. What remains a mystery is how chondrules so dispersed into the nebula agglomerated en masse into meteorite parent bodies, either byRead More →

Addressing $H_0$ tension by means of VCDM. (arXiv:2009.08718v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Felice_A/0/1/0/all/0/1">Antonio De Felice</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mukohyama_S/0/1/0/all/0/1">Shinji Mukohyama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pookkillath_M/0/1/0/all/0/1">Masroor C. Pookkillath</a> In this letter we propose a reduction of the $H_0$ tension puzzle by means of a theory of minimally modified gravity which is dubbed VCDM. After confronting the theory with the data, a transition in the expansion history of the universe in the low-redshift $zsimeq 0.3 $ is found. From the bestfit values the total fitness parameter is improved by $Delta chi^2=33.41$, for the data set considered. We then determine the local Hubble expansion rate today by taking into account proper calibration of theRead More →

Particle acceleration by relativistic magnetic reconnection driven by kink instability turbulence in Poynting flux dominated jets. (arXiv:2009.08516v5 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Medina_Torrejon_T/0/1/0/all/0/1">Tania E. Medina-Torrejon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pino_E/0/1/0/all/0/1">Elisabete M. de Gouveia Dal Pino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kadowaki_L/0/1/0/all/0/1">Luis H.S. Kadowaki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kowal_G/0/1/0/all/0/1">Grzegorz Kowal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Singh_C/0/1/0/all/0/1">Chandra B. Singh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mizuno_Y/0/1/0/all/0/1">Yosuke Mizuno</a> Particle acceleration in magnetized relativistic jets still puzzles theorists, specially when one tries to explain the highly variable emission observed in blazar jets or gamma-ray bursts putting severe constraints on current models. In this work we investigate the acceleration of particles injected in a three-dimensional relativistic magnetohydrodynamical jet subject to current driven kink instability (CDKI), which drives turbulence and fast magneticRead More →

Choked accretion onto a Kerr black hole. (arXiv:2009.06653v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Aguayo_Ortiz_A/0/1/0/all/0/1">Alejandro Aguayo-Ortiz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sarbach_O/0/1/0/all/0/1">Olivier Sarbach</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tejeda_E/0/1/0/all/0/1">Emilio Tejeda</a> The choked accretion model consists of a purely hydrodynamical mechanism in which, by setting an equatorial to polar density contrast, a spherically symmetric accretion flow transitions to an inflow-outflow configuration. This scenario has been studied in the case of a (non-rotating) Schwarzschild black hole as central accretor, as well as in the non-relativistic limit. In this article, we generalize these previous works by studying the accretion of a perfect fluid onto a (rotating) Kerr black hole. We first describe the mechanism by using a steady-state, irrotationalRead More →

Cosmological constraints from BOSS with analytic covariance matrices. (arXiv:2009.00622v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Wadekar_D/0/1/0/all/0/1">Digvijay Wadekar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ivanov_M/0/1/0/all/0/1">Mikhail M. Ivanov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Scoccimarro_R/0/1/0/all/0/1">Roman Scoccimarro</a> We use analytic covariance matrices to carry out a full-shape analysis of the galaxy power spectrum multipoles from the Baryon Oscillation Spectroscopic Survey (BOSS). We obtain parameter estimates that agree well with those based on the sample covariance from two thousand galaxy mock catalogs, thus validating the analytic approach and providing substantial reduction in computational cost. We also highlight a number of additional advantages of analytic covariances. First, the analysis does not suffer from sampling noise, which biases the constraints and typically requires inflatingRead More →

Renyi entropy as a measure of cosmic homogeneity. (arXiv:2008.10266v3 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Pandey_B/0/1/0/all/0/1">Biswajit Pandey</a> We propose a method for testing homogeneity in three dimensional spatial distributions using Renyi entropy. We apply the proposed method to data from cosmological N-body simulations and Monte Carlo simulations of homogeneous Poisson point process. We show that the method can effectively characterize the inhomogeneities and identify any transition scale to homogeneity, if present in such distributions. The proposed method can be used to study the cosmic homogeneity in present and future generation galaxy redshift surveys. We propose a method for testing homogeneity in three dimensional spatial distributions using Renyi entropy.Read More →

Far-Infrared Polarization Spectrum of the OMC-1 Star-Forming Region. (arXiv:2008.00310v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Michail_J/0/1/0/all/0/1">Joseph M. Michail</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ashton_P/0/1/0/all/0/1">Peter C. Ashton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berthoud_M/0/1/0/all/0/1">Marc G. Berthoud</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chuss_D/0/1/0/all/0/1">David T. Chuss</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dowell_C/0/1/0/all/0/1">C. Darren Dowell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guerra_J/0/1/0/all/0/1">Jordan A. Guerra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Harper_D/0/1/0/all/0/1">Doyal A. Harper</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Novak_G/0/1/0/all/0/1">Giles Novak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Santos_F/0/1/0/all/0/1">Fabio P. Santos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Siah_J/0/1/0/all/0/1">Javad Siah</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sukay_E/0/1/0/all/0/1">Ezra Sukay</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Taylor_A/0/1/0/all/0/1">Aster Taylor</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tram_L/0/1/0/all/0/1">Le Ngoc Tram</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vaillancourt_J/0/1/0/all/0/1">John E. Vaillancourt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wollack_E/0/1/0/all/0/1">Edward J. Wollack</a> We analyze the wavelength dependence of the far-infrared polarization fraction toward the OMC-1 star forming region using observations from HAWC+/SOFIA at 53, 89, 154, and 214 $mu$m. We find that the shape of the far-infrared polarization spectrum isRead More →

Results on Low-Mass Weakly Interacting Massive Particles from an 11 kg-day Target Exposure of DAMIC at SNOLAB. (arXiv:2007.15622v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Aguilar_Arevalo_A/0/1/0/all/0/1">A. Aguilar-Arevalo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amidei_D/0/1/0/all/0/1">D. Amidei</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baxter_D/0/1/0/all/0/1">D. Baxter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cancelo_G/0/1/0/all/0/1">G. Cancelo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vergara_B/0/1/0/all/0/1">B.A. Cervantes Vergara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chavarria_A/0/1/0/all/0/1">A.E. Chavarria</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DOlivo_J/0/1/0/all/0/1">J.C. D&#x27;Olivo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Estrada_J/0/1/0/all/0/1">J. Estrada</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Favela_Perez_F/0/1/0/all/0/1">F. Favela-Perez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gaior_R/0/1/0/all/0/1">R. Gaior</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guardincerri_Y/0/1/0/all/0/1">Y. Guardincerri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hoppe_E/0/1/0/all/0/1">E.W. Hoppe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hossbach_T/0/1/0/all/0/1">T.W. Hossbach</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kilminster_B/0/1/0/all/0/1">B. Kilminster</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lawson_I/0/1/0/all/0/1">I. Lawson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_S/0/1/0/all/0/1">S.J. Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Letessier_Selvon_A/0/1/0/all/0/1">A. Letessier-Selvon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matalon_A/0/1/0/all/0/1">A. Matalon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mitra_P/0/1/0/all/0/1">P. Mitra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Overman_C/0/1/0/all/0/1">C.T. Overman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Piers_A/0/1/0/all/0/1">A. Piers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Privitera_P/0/1/0/all/0/1">P. Privitera</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ramanathan_K/0/1/0/all/0/1">K. Ramanathan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rocha_J/0/1/0/all/0/1">J. Da Rocha</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sarkis_Y/0/1/0/all/0/1">Y. Sarkis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Settimo_M/0/1/0/all/0/1">M. Settimo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smida_R/0/1/0/all/0/1">R. Smida</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Thomas_R/0/1/0/all/0/1">R.Read More →

Status of the STUDIO UV balloon mission and platform. (arXiv:2012.14215v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Pahler_A/0/1/0/all/0/1">A. Pahler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+%7B%5CAA%7Dngermann_M/0/1/0/all/0/1">M. &#xc5;ngermann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barnstedt_J/0/1/0/all/0/1">J. Barnstedt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bougueroua_S/0/1/0/all/0/1">S. Bougueroua</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Colin_A/0/1/0/all/0/1">A. Colin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Conti_L/0/1/0/all/0/1">L. Conti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Diebold_S/0/1/0/all/0/1">S. Diebold</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Duffard_R/0/1/0/all/0/1">R. Duffard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Emberger_M/0/1/0/all/0/1">M. Emberger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hanke_L/0/1/0/all/0/1">L. Hanke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kalkuhl_C/0/1/0/all/0/1">C. Kalkuhl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kappelmann_N/0/1/0/all/0/1">N. Kappelmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Keilig_T/0/1/0/all/0/1">T. Keilig</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Klinkner_S/0/1/0/all/0/1">S. Klinkner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Krabbe_A/0/1/0/all/0/1">A. Krabbe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Janson_O/0/1/0/all/0/1">O. Janson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lengowski_M/0/1/0/all/0/1">M. Lengowski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lockowandt_C/0/1/0/all/0/1">C. Lockowandt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maier_P/0/1/0/all/0/1">P. Maier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Muller_T/0/1/0/all/0/1">T. M&#xfc;ller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rauch_T/0/1/0/all/0/1">T. Rauch</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schanz_T/0/1/0/all/0/1">T. Schanz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stelzer_B/0/1/0/all/0/1">B. Stelzer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Taheran_M/0/1/0/all/0/1">M. Taheran</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vaerneus_A/0/1/0/all/0/1">A. Vaerneus</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Werner_K/0/1/0/all/0/1">K. Werner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wolf_J/0/1/0/all/0/1">J. Wolf</a> Stratospheric balloons offer accessible and affordable platforms for observations in atmosphere-constrained wavelength ranges.Read More →