RAS_WEB (Page 2,211)

Spectroscopic Signatures of the Vanishing Natural Coronagraph of eta Carinae. (arXiv:2105.00590v3 [astro-ph.SR] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Damineli_A/0/1/0/all/0/1">A. Damineli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Navarete_F/0/1/0/all/0/1">F. Navarete</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hillier_D/0/1/0/all/0/1">D. J. Hillier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moffat_A/0/1/0/all/0/1">A. F. J. Moffat</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Corcoran_M/0/1/0/all/0/1">M. F. Corcoran</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gull_T/0/1/0/all/0/1">T. R. Gull</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Richardson_N/0/1/0/all/0/1">N. D. Richardson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weigelt_G/0/1/0/all/0/1">G. Weigelt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Morris_P/0/1/0/all/0/1">P. W. Morris</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stevens_I/0/1/0/all/0/1">I. Stevens</a> Eta Carinae is a massive interacting binary system shrouded in a complex circumstellar environment whose evolution is the source of the long-term brightening observed during the last 80 years. An occulter, acting as a natural coronagraph, impacts observations from our perspective, but not from most other directions. Other sight-lines are visible to us through studiesRead More →

REXPACO: an algorithm for high contrast reconstruction of the circumstellar environment by angular differential imaging. (arXiv:2104.09672v2 [astro-ph.IM] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Flasseur_O/0/1/0/all/0/1">Olivier Flasseur</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+The_S/0/1/0/all/0/1">Samuel Th&#xe9;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Denis_L/0/1/0/all/0/1">Lo&#xef;c Denis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Thiebaut_E/0/1/0/all/0/1">&#xc9;ric Thi&#xe9;baut</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Langlois_M/0/1/0/all/0/1">Maud Langlois</a> Aims. The purpose of this paper is to describe a new post-processing algorithm dedicated to the reconstruction of the spatial distribution of light received from off-axis sources, in particular from circumstellar disks. Methods. Built on the recent PACO algorithm dedicated to the detection of point-like sources, the proposed method is based on the local learning of patch covariances capturing the spatial fluctuations of the stellar leakages. From this statistical modeling, we developRead More →

Constraining Black Hole Spin based on the Absence of Lense-Thirring Precession of Megamaser Clumps. (arXiv:2104.05084v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Giner_S/0/1/0/all/0/1">Santiago Giner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Loeb_A/0/1/0/all/0/1">Abraham Loeb</a> We make use of the absence of Lense-Thirring precession of the innermost megamaser clumps around black holes in order to place upper limits on the spin amplitude of seven black holes at the center of megamaser galaxies: NGC 4258, NGC 2273, UGC 3789, NGC 3393, NGC 5495, NGC 5765b, and UGC 6093. The constraints are derived by requiring that the associated precession time-scale be longer than the age of the megamaser clumps, in order to preserve the single-plane geometry of the megamasers.Read More →

The Origin of the Orbital Parameter Distribution of Merging Halos. (arXiv:2104.02160v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Benson_A/0/1/0/all/0/1">A. J. Benson</a> (1) ((1) Carnegie Observatories) We describe a simple model which explains the qualitative and (approximate) quantitative features of the distribution of orbital velocities of merging pairs of dark matter halos. Our model considers a primary dark matter halo as a perturber in a background of secondary halos with velocities described by linear theory. By evaluating the ensemble of secondary halos on orbits within the perturbing halo’s “loss cone” we derive the distribution of orbital parameters of these captured halos. This model is able provide qualitative explanations for theRead More →

Tempestuous life beyond R_500: X-ray view on the Coma cluster with SRG/eROSITA. I. X-ray morphology, recent merger, and radio halo connection. (arXiv:2012.11627v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Churazov_E/0/1/0/all/0/1">E. Churazov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Khabibullin_I/0/1/0/all/0/1">I. Khabibullin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lyskova_N/0/1/0/all/0/1">N. Lyskova</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sunyaev_R/0/1/0/all/0/1">R. Sunyaev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bykov_A/0/1/0/all/0/1">A.M. Bykov</a> This is the first paper in a series of studies of the Coma cluster using the SRG/eROSITA X-ray data obtained in course of the Calibration and Performance Verification observations. The data cover $sim3^circtimes 3^circ$ area around the cluster with a typical exposure time of more than 20 ks. The stability of the instrumental background and operation of the SRG Observatory in the scanning mode provided usRead More →

An exploration of model degeneracies with a unified phase curve retrieval analysis: The light and dark sides of WASP-43 b. (arXiv:2103.14566v2 [astro-ph.EP] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Changeat_Q/0/1/0/all/0/1">Quentin Changeat</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Al_Refaie_A/0/1/0/all/0/1">Ahmed F. Al-Refaie</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Edwards_B/0/1/0/all/0/1">Billy Edwards</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Waldmann_I/0/1/0/all/0/1">Ingo P. Waldmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tinetti_G/0/1/0/all/0/1">Giovanna Tinetti</a> The analysis of exoplanetary atmospheres often relies upon the observation of transit or eclipse events. While very powerful, these snapshots provide mainly 1-dimensional information on the planet structure and do not easily allow precise latitude-longitude characterisations. The phase curve technique, which consists of measuring the planet emission throughout its entire orbit, can break this limitation and provide useful 2-dimensional thermal and chemical constraints on theRead More →

Discrimination of background events in the PolarLight X-ray polarimeter. (arXiv:2103.12962v2 [astro-ph.IM] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Zhu_J/0/1/0/all/0/1">Jiahuan Zhu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_H/0/1/0/all/0/1">Hong Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Feng_H/0/1/0/all/0/1">Hua Feng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huang_J/0/1/0/all/0/1">Jiahui Huang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Long_X/0/1/0/all/0/1">Xiangyun Long</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wu_Q/0/1/0/all/0/1">Qiong Wu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jiang_W/0/1/0/all/0/1">Weichun Jiang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Minuti_M/0/1/0/all/0/1">Massimo Minuti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Citraro_S/0/1/0/all/0/1">Saverio Citraro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nasimi_H/0/1/0/all/0/1">Hikmat Nasimi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yang_D/0/1/0/all/0/1">Dongxin Yang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yu_J/0/1/0/all/0/1">Jiandong Yu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jin_G/0/1/0/all/0/1">Ge Jin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zeng_M/0/1/0/all/0/1">Ming Zeng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+An_P/0/1/0/all/0/1">Peng An</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baldini_L/0/1/0/all/0/1">Luca Baldini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bellazzini_R/0/1/0/all/0/1">Ronaldo Bellazzini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brez_A/0/1/0/all/0/1">Alessandro Brez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Latronico_L/0/1/0/all/0/1">Luca Latronico</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sgro_C/0/1/0/all/0/1">Carmelo Sgro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Spandre_G/0/1/0/all/0/1">Gloria Spandre</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pinchera_M/0/1/0/all/0/1">Michele Pinchera</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Muleri_F/0/1/0/all/0/1">Fabio Muleri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Soffitta_P/0/1/0/all/0/1">Paolo Soffitta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Costa_E/0/1/0/all/0/1">Enrico Costa</a> PolarLight is a space-borne X-ray polarimeter that measures the X-ray polarization via electron tracking in an ionization chamber.Read More →

Binary black hole mergers from young massive and open clusters: comparison to GWTC-2 gravitational wave data. (arXiv:2103.10447v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Fragione_G/0/1/0/all/0/1">Giacomo Fragione</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Banerjee_S/0/1/0/all/0/1">Sambaran Banerjee</a> Several astrophysical scenarios have been proposed to explain the origin of the population of binary black hole (BBH) mergers detected in gravitational waves (GWs) by the LIGO/Virgo Collaboration. Among them, BBH mergers assembled dynamically in young massive and open clusters have been shown to produce merger rate densities consistent with LIGO/Virgo estimated rates. We use the results of a suite of direct, high-precision $N$-body evolutionary models of young massive and open clusters and build the population of BBH mergers, byRead More →

Revisiting FUSE O VI Emission in Galaxy Halos. (arXiv:2103.05008v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Chung_H/0/1/0/all/0/1">Haeun Chung</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vargas_C/0/1/0/all/0/1">Carlos J. Vargas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hamden_E/0/1/0/all/0/1">Erika Hamden</a> A significant fraction of baryons in galaxies are in the form of diffuse gas of the circumgalactic medium (CGM). One critical component of the multi-phases of CGM, the so-called “coronal” warm-hot phase gas ($rm 10^{5}-10^{6}$ K) traced by O VI 1031.93, 1037.62 r{A} resonance lines, has rarely been detected in emission from galaxy halos other than Milky Way. Here we report four additional detections of O VI emission gas in the halos of nearby edge-on galaxies, NGC 4631 and NGC 891, using archival FarRead More →

Inflationary magnetogenesis: solving the strong coupling and its non-Gaussian signatures. (arXiv:2103.03159v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Nandi_D/0/1/0/all/0/1">Debottam Nandi</a> (IISER Mohali) The simplest model of primordial magnetogenesis can provide scale-invariant magnetic fields that can explain the present abundances of it in the cosmic scales. Two kinds of solutions of the coupling function can lead to such phenomena and both of them suffer from the problems of either strong-coupling or large backreaction. In this work, we consider the coupling function as a linear combination of both kinds with a model parameter. We find that the parameter needs to be as small as $sim 10^{-20}$ in order to evade theRead More →

Far UV and Optical Emissions from Three Very Large Supernova Remnants Located at Unusually High Galactic Latitudes. (arXiv:2102.12599v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Fesen_R/0/1/0/all/0/1">Robert A. Fesen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Drechsler_M/0/1/0/all/0/1">Marcel Drechsler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weil_K/0/1/0/all/0/1">Kathryn E. Weil</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Strottner_X/0/1/0/all/0/1">Xavier Strottner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Raymond_J/0/1/0/all/0/1">John C. Raymond</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rupert_J/0/1/0/all/0/1">Justin Rupert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Milisavljevic_D/0/1/0/all/0/1">Dan Milisavljevic</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Subrayan_B/0/1/0/all/0/1">Bhagya M. Subrayan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cicco_D/0/1/0/all/0/1">Dennis di Cicco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Walker_S/0/1/0/all/0/1">Sean Walker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mittelman_D/0/1/0/all/0/1">David Mittelman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ludgate_M/0/1/0/all/0/1">Mathew Ludgate</a> Galactic supernova remnants (SNRs) with angular dimensions greater than a few degrees are relatively rare, as are remnants located more than ten degrees off the Galactic plane. Here we report a UV and optical investigation of two previously suspected SNRs more than ten degreesRead More →

Improved Lyman Alpha Tomography using Optimized Reconstruction with Constraints on Absorption (ORCA). (arXiv:2102.12306v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Li_Z/0/1/0/all/0/1">Zihao Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Horowitz_B/0/1/0/all/0/1">Benjamin Horowitz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cai_Z/0/1/0/all/0/1">Zheng Cai</a> In this work, we propose an improved approach to reconstruct the three-dimensional intergalactic medium from observed Lyman-$alpha$ forest absorption features. We present our new method, the Optimized Reconstruction with Constraints on Absorption (ORCA), which outperforms the current baseline Wiener Filter (WF) when tested on mock Lyman Alpha forest data generated from hydrodynamical simulations. We find that both reconstructed flux errors and cosmic web classification improve substantially with ORCA, equivalent to 30-40% additional sight-lines with the standard WF. We use this methodRead More →

Supernova Constraint on Self-Interacting Dark Sector Particles. (arXiv:2102.04601v2 [hep-ph] UPDATED) <a href="http://arxiv.org/find/hep-ph/1/au:+Sung_A/0/1/0/all/0/1">Allan Sung</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Guo_G/0/1/0/all/0/1">Gang Guo</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Wu_M/0/1/0/all/0/1">Meng-Ru Wu</a> We examine the constraints on sub-GeV dark sector particles set by the proto-neutron star cooling associated with the core-collapse supernova event SN1987a. Considering explicitly a dark photon portal dark sector model, we compute the relevant interaction rates of dark photon ($A’$) and dark fermion ($chi$) with the Standard Model particles as well as their self-interaction inside the dark sector. We find that even with a small dark sector fine structure constant $alpha_Dll 1$, dark sector self-interactions can easily lead to their own self-trapping. This effect stronglyRead More →

The string theory swampland in the Euclid, SKA and Vera Rubin observatory era. (arXiv:2101.02942v3 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Barrau_A/0/1/0/all/0/1">Aur&#xe9;lien Barrau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Renevey_C/0/1/0/all/0/1">Cyril Renevey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Martineau_K/0/1/0/all/0/1">Killian Martineau</a> This article aims at drawing the attention of astronomers on the ability of future cosmological surveys to put constraints on string theory. The fact that “quantum gravity” might be constrained by large scale astrophysical observations is a remarkable fact that has recently concentrated a great amount of interest. In this work, we focus on future observatories and investigate their capability to put string theory, which is sometimes said to be “unfalsifiable”, under serious pressure. We show that the combined analysisRead More →

A one-armed CNN for exoplanet detection from light curves. (arXiv:2105.06292v1 [cs.CV]) <a href="http://arxiv.org/find/cs/1/au:+Visser_K/0/1/0/all/0/1">Koko Visser</a>, <a href="http://arxiv.org/find/cs/1/au:+Bosma_B/0/1/0/all/0/1">Bas Bosma</a>, <a href="http://arxiv.org/find/cs/1/au:+Postma_E/0/1/0/all/0/1">Eric Postma</a> We propose Genesis, a one-armed simplified Convolutional Neural Network (CNN)for exoplanet detection, and compare it to the more complex, two-armed CNN called Astronet. Furthermore, we examine how Monte Carlo cross-validation affects the estimation of the exoplanet detection performance. Finally, we increase the input resolution twofold to assess its effect on performance. The experiments reveal that (i)the reduced complexity of Genesis, i.e., a more than 95% reduction in the number of free parameters, incurs a small performance cost of about 0.5% compared to Astronet, (ii) MonteRead More →

The isotropic attractor solution of axion-SU(2) inflation: Universal isotropization in Bianchi type-I geometory. (arXiv:2105.06259v1 [gr-qc]) <a href="http://arxiv.org/find/gr-qc/1/au:+Wolfson_I/0/1/0/all/0/1">Ira Wolfson</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Maleknejad_A/0/1/0/all/0/1">Azadeh Maleknejad</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Murata_T/0/1/0/all/0/1">Tomoaki Murata</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Komatsu_E/0/1/0/all/0/1">Eiichiro Komatsu</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Kobayashi_T/0/1/0/all/0/1">Tsutomu Kobayashi</a> SU(2) gauge fields coupled to an axion field can acquire an isotropic background solution during inflation. We study homogeneous but anisotropic inflationary solutions in the presence of such (massless) gauge fields. A gauge field in the cosmological background may pose a threat to spatial isotropy. We show, however, that such models $textit{generally}$ isotropize in Bianchi type-I geometry, and the isotropic solution is the attractor. Restricting the setup by adding an axial symmetry, we revisited theRead More →

The cosmological dependence of halo and galaxy assembly bias. (arXiv:2105.05854v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Contreras_S/0/1/0/all/0/1">Sergio Contreras</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chaves_Montero_J/0/1/0/all/0/1">Jon&#xe1;s Chaves-Montero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zennaro_M/0/1/0/all/0/1">Matteo Zennaro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Angulo_R/0/1/0/all/0/1">Raul E. Angulo</a> One of the main predictions of excursion set theory is that the clustering of dark matter haloes only depends on halo mass. However, it has been long established that the clustering of haloes also depends on other properties, including formation time, concentration, and spin; this effect is commonly known as halo assembly bias. We use a suite of gravity-only simulations to study the dependence of halo assembly bias on cosmology; these simulations cover cosmological parameters spanning 10$sigma$ around state-of-the-art best-fitting values,Read More →

Characterizing Spectral Channels of Visible Emission Line Coronagraph of Aditya-L1. (arXiv:2105.05880v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Patel_R/0/1/0/all/0/1">Ritesh Patel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+A%2E_M/0/1/0/all/0/1">Megha A.</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shrivastav_A/0/1/0/all/0/1">Arpit Kumar Shrivastav</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pant_V/0/1/0/all/0/1">Vaibhav Pant</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vishnu_M/0/1/0/all/0/1">M. Vishnu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+K%2E_S/0/1/0/all/0/1">Sankarasubramanian K.</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Banerjee_D/0/1/0/all/0/1">Dipankar Banerjee</a> Aditya-L1 is India’s first solar mission with Visible Emission Line Coronagraph (VELC) consisting of three spectral channels taking high-resolution spectroscopic observations of the inner corona up to 1.5 Rsun at 5303 AA, 7892 AA, and 10747 AA. In this work, we present the strategy for the slit width optimization for the VELC using synthetic line profiles by taking into account the instrument characteristics and coronal conditions for log(T) varying from 6Read More →

Quantum Fisher Cosmology: Confronting Observations and the Trans-Planckian Problem. (arXiv:2105.05251v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Gomez_C/0/1/0/all/0/1">Cesar Gomez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jimenez_R/0/1/0/all/0/1">Raul Jimenez</a> The aim of Quantum Fisher Cosmology is to use the quantum Fisher information about pure de Sitter states to derive model independent observational consequences of the existence of a primordial phase of the Universe of de Sitter accelerated expansion. These quantum features are encoded in a scale dependent quantum cosmological tilt that defines what we can call the de Sitter universality class. The experimental predictions are: i) A phase transition from red into blue tilt at a scale order $k= 1$ Mpc$^{-1}$ that naturally solves the cosmological trans-PlanckianRead More →

AGN STORM 2: I. First results: A Change in the Weather of Mrk 817. (arXiv:2105.05840v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Kara_E/0/1/0/all/0/1">Erin Kara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mehdipour_M/0/1/0/all/0/1">Missagh Mehdipour</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kriss_G/0/1/0/all/0/1">Gerard A. Kriss</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cackett_E/0/1/0/all/0/1">Edward M. Cackett</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arav_N/0/1/0/all/0/1">Nahum Arav</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barth_A/0/1/0/all/0/1">Aaron J. Barth</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Byun_D/0/1/0/all/0/1">Doyee Byun</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brotherton_M/0/1/0/all/0/1">Michael S. Brotherton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rosa_G/0/1/0/all/0/1">Gisella De Rosa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gelbord_J/0/1/0/all/0/1">Jonathan Gelbord</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Santisteban_J/0/1/0/all/0/1">Juan V. Hernandez Santisteban</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hu_C/0/1/0/all/0/1">Chen Hu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kaastra_J/0/1/0/all/0/1">Jelle Kaastra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Landt_H/0/1/0/all/0/1">Hermine Landt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_Y/0/1/0/all/0/1">Yan-Rong Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Miller_J/0/1/0/all/0/1">Jake A. Miller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Montano_J/0/1/0/all/0/1">John Montano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Partington_E/0/1/0/all/0/1">Ethan Partington</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aceituno_J/0/1/0/all/0/1">Jesus Aceituno</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bai_J/0/1/0/all/0/1">Jin-Ming Bai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bao_D/0/1/0/all/0/1">Dongwei Bao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bentz_M/0/1/0/all/0/1">Misty C. Bentz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brink_T/0/1/0/all/0/1">Thomas G. Brink</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chelouche_D/0/1/0/all/0/1">Doron Chelouche</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_Y/0/1/0/all/0/1">Yong-Jie Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bonta_E/0/1/0/all/0/1">Elena Dalla Bonta</a>,Read More →