RAS_WEB (Page 2,678)

Reading between the lines: Disk emission, wind, and accretion during the ZCMa NW outburst. (arXiv:2008.13678v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Sicilia_Aguilar_A/0/1/0/all/0/1">A. Sicilia-Aguilar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bouvier_J/0/1/0/all/0/1">J. Bouvier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dougados_C/0/1/0/all/0/1">C. Dougados</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grankin_K/0/1/0/all/0/1">K. Grankin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Donati_J/0/1/0/all/0/1">J.-F. Donati</a> (Abridged) We use optical spectroscopy to investigate the disk, wind, and accretion during the 2008 ZCMa NW outburst. Over 1000 optical emission lines reveal accretion, a variable, multi-component wind, and double-peaked lines of disk origin. The variable, non-axisymmetric, accretion-powered wind has slow ($sim $0 km s$^{-1}$), intermediate ($sim -$100 km s$^{-1}$) and fast ($geq -$400 km s$^{-1}$) components. The fast components are of stellar origin and disappear in quiescence, while the slow component isRead More →

Simulations of the Early Post-Bounce Phase of Core-Collapse Supernovae in Three-Dimensional Space with Full Boltzmann Neutrino Transport. (arXiv:2004.02091v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Iwakami_W/0/1/0/all/0/1">Wakana Iwakami</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Okawa_H/0/1/0/all/0/1">Hirotada Okawa</a>, <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:+Harada_A/0/1/0/all/0/1">Akira Harada</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Furusawa_S/0/1/0/all/0/1">Shun Furusawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sumiyoshi_K/0/1/0/all/0/1">Kosuke Sumiyoshi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matsufuru_H/0/1/0/all/0/1">Hideo Matsufuru</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yamada_S/0/1/0/all/0/1">Shoichi Yamada</a> We report on the core-collapse supernova simulation we conducted for a 11.2 M progenitor model in three-dimensional space up to 20 ms after bounce, using a radiation hydrodynamics code with full Boltzmann neutrino transport. We solve the six-dimensional Boltzmann equations for three neutrino species and the three-dimensional compressible Euler equations with Furusawa and Togashi’s nuclear equation of state. We focus onRead More →

Discovery of molecular gas fueling galaxy growth in a protocluster at z=1.7. (arXiv:2008.13665v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+DAmato_Q/0/1/0/all/0/1">Q. D&#x27;Amato</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gilli_R/0/1/0/all/0/1">R. Gilli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prandoni_I/0/1/0/all/0/1">I. Prandoni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vignali_C/0/1/0/all/0/1">C. Vignali</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Massardi_M/0/1/0/all/0/1">M. Massardi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mignoli_M/0/1/0/all/0/1">M. Mignoli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cucciati_O/0/1/0/all/0/1">O. Cucciati</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Morishita_T/0/1/0/all/0/1">T. Morishita</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Decarli_R/0/1/0/all/0/1">R. Decarli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brusa_M/0/1/0/all/0/1">M. Brusa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Calura_F/0/1/0/all/0/1">F. Calura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Balmaverde_B/0/1/0/all/0/1">B. Balmaverde</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chiaberge_M/0/1/0/all/0/1">M. Chiaberge</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liuzzo_E/0/1/0/all/0/1">E. Liuzzo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nanni_R/0/1/0/all/0/1">R. Nanni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Peca_A/0/1/0/all/0/1">A. Peca</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pensabene_A/0/1/0/all/0/1">A.Pensabene</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tozzi_P/0/1/0/all/0/1">P. Tozzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Norman_C/0/1/0/all/0/1">C. Norman</a> Based on ALMA Band 3 observations of the CO(2-1) line transition, we report the discovery of three new gas-rich (M_H2 ~ 1.5-4.8 x 10^10 M_sun, SFRs in the range ~5-100 M_sun/yr) galaxies in an overdenseRead More →

Testing the ALP-photon coupling with polarization measurements of Sagittarius A*. (arXiv:2008.13662v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Yuan_G/0/1/0/all/0/1">Guan-Wen Yuan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xia_Z/0/1/0/all/0/1">Ziqing Xia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tang_C/0/1/0/all/0/1">Chengfeng Tang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhao_Y/0/1/0/all/0/1">Yaqi Zhao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cai_Y/0/1/0/all/0/1">Yi-Fu Cai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_Y/0/1/0/all/0/1">Yifan Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shu_J/0/1/0/all/0/1">Jing Shu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yuan_Q/0/1/0/all/0/1">Qiang Yuan</a> Ultra-light bosons such as axions or axion-like particles (ALPs), are promising candidates to solve the dark matter problem. A unique way to detect such ALPs is to search for the periodic oscillation feature of the position angles of linearly polarized photons emitted from the regions where ALP dark matter forms a solitonic core. In this work, we use the high-resolution polarimetric measurements of the radiation near the super-massive blackRead More →

Multi-field dark energy: cosmic acceleration on a steep potential. (arXiv:2008.13660v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Akrami_Y/0/1/0/all/0/1">Yashar Akrami</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sasaki_M/0/1/0/all/0/1">Misao Sasaki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Solomon_A/0/1/0/all/0/1">Adam R. Solomon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vardanyan_V/0/1/0/all/0/1">Valeri Vardanyan</a> We argue that dark energy with multiple fields is theoretically well-motivated and predicts distinct observational signatures, in particular when cosmic acceleration takes place along a trajectory that is highly non-geodesic in field space. Such models provide novel physics compared to $Lambda$CDM and quintessence by allowing cosmic acceleration on steep potentials. From the theoretical point of view, these theories can easily satisfy the conjectured swampland constraints and may in certain cases be technically natural, problems which plague standard single-field dark energy. Observationally,Read More →

Modeling disk fragmentation and multiplicity in massive star formation. (arXiv:2008.13653v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Oliva_G/0/1/0/all/0/1">G. Andr&#xe9; Oliva</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kuiper_R/0/1/0/all/0/1">Rolf Kuiper</a> We investigate the formation and early evolution and fragmentation of an accretion disk around a forming massive protostar. We use a grid-based self-gravity-radiation-hydrodynamics code including a sub-grid module for stellar and dust evolution. On purpose, we do not use sink particles to allow for all paths of fragment formation and destruction, but instead keeping the spatial grid resolution high enough to properly resolve the physical length scales of the problem. We use a 3D grid in spherical coordinates with a logarithmic scaling in the radial direction andRead More →

Pulsation-driven mass loss from massive stars behind stellar mergers in metal-poor dense clusters. (arXiv:2008.13647v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Nakauchi_D/0/1/0/all/0/1">Daisuke Nakauchi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Inayoshi_K/0/1/0/all/0/1">Kohei Inayoshi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Omukai_K/0/1/0/all/0/1">Kazuyuki Omukai</a> The recent discovery of high-redshift (z > 6) supermassive black holes (SMBH) favors the formation of massive seed BHs in protogalaxies. One possible scenario is formation of massive stars ~ 1e3-1e4 Msun via runaway stellar collisions in a dense cluster, leaving behind massive BHs without significant mass loss. We study the pulsational instability of massive stars with the zero-age main-sequence (ZAMS) mass Mzams/Msun = 300-3000 and metallicity Z/Zsun = 0-0.1, and discuss whether or not pulsation-driven mass loss prevents massive BHRead More →

A Survey of 3 to 5.4 Micron Emission From Planetary Nebulae using SOFIA/FLITECAM. (arXiv:2008.13635v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Smith_E/0/1/0/all/0/1">Erin C. Smith</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:+McLean_I/0/1/0/all/0/1">Ian S. McLean</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fletcher_E/0/1/0/all/0/1">Elizabeth Fletcher</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vacca_W/0/1/0/all/0/1">William D. Vacca</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Becklin_E/0/1/0/all/0/1">E. E. Becklin</a>, 5, <a href="http://arxiv.org/find/astro-ph/1/au:+Shenoy_S/0/1/0/all/0/1">Sachindev Shenoy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Savage_M/0/1/0/all/0/1">Maureen Savage</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hamilton_R/0/1/0/all/0/1">Ryan T. Hamilton</a> Here we present the results of an airborne 3-5.4$mu$m spectroscopic study of three young, Carbon-rich planetary nebulae IC 5117, PNG 093.9-00.1, and BD $+$30 3639. These observations were made using the grism spectroscopy mode of the FLITECAM instrument during airborne science operations onboard NASA’s Stratospheric Observatory for Infrared Astronomy (SOFIA). The goal of this study isRead More →

Muonization of supernova matter. (arXiv:2008.13628v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Fischer_T/0/1/0/all/0/1">Tobias Fischer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guo_G/0/1/0/all/0/1">Gang Guo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Martinez_Pinedo_G/0/1/0/all/0/1">Gabriel Mart&#xed;nez-Pinedo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liebendorder_M/0/1/0/all/0/1">Matthias Liebend&#xf6;rder</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mezzacappa_A/0/1/0/all/0/1">Anthony Mezzacappa</a> The present article investigates the impact of muons on core-collapse supernovae, with particular focus on the early muon neutrino emission. While the presence of muons is well understood in the context of neutron stars, until the recent study by Bollig et al. [Phys. Rev. Lett. 119, 242702 (2017)] the role of muons in core-collapse supernovae had been neglected – electrons and neutrinos were the only leptons considered. In their study, Bollig~et~al. disentangled the muon and tau neutrinos and antineutrinos and included a variety ofRead More →

Orbits of 152 Globular Clusters of the Milky Way Galaxy Constructed from the Gaia DR2 data. (arXiv:2008.13624v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Bajkova_A/0/1/0/all/0/1">A.T. Bajkova</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bobylev_V/0/1/0/all/0/1">V.V. Bobylev</a> We present orbits and their properties for 152 globular clusters of the Milky Way galaxy obtained using average Gaia DR2 proper motions and other astrometric data from the list of Vasiliev (2019). For orbit integrating we have used the axisymmetric model of the Galactic potential based on the Navarro-Frenk-White dark halo, and modified by Bajkova and Bobylev (2016) using circular velocities of Galactic objects in wide region of Galactocentric distances (up to 200 kpc) from Bhattacharjee et.al. (2014) catalog. Based onRead More →

A Planck-selected dusty proto-cluster at z=2.16 associated with a strong over-density of massive H$alpha$ emitting galaxies. (arXiv:2008.13614v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Koyama_Y/0/1/0/all/0/1">Yusei Koyama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Polletta_M/0/1/0/all/0/1">Maria del Carmen Polletta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tanaka_I/0/1/0/all/0/1">Ichi Tanaka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kodama_T/0/1/0/all/0/1">Tadayuki Kodama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dole_H/0/1/0/all/0/1">Herv&#xe9; Dole</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Soucail_G/0/1/0/all/0/1">Genevi&#xe8;ve Soucail</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Frye_B/0/1/0/all/0/1">Brenda Frye</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lehnert_M/0/1/0/all/0/1">Matt Lehnert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Scodeggio_M/0/1/0/all/0/1">Marco Scodeggio</a> We discovered an over-density of H-alpha-emitting galaxies associated with a Planck compact source in the COSMOS field (PHzG237.0+42.5) through narrow-band imaging observations with Subaru/MOIRCS. This Planck-selected dusty proto-cluster at z=2.16 has 38 H-alpha emitters including six spectroscopically confirmed galaxies in the observed MOIRCS 4’x7′ field (corresponding to ~2.0×3.5~Mpc^2). We find that massive H-alpha emitters with log(M*/Msun)>10.5 are stronglyRead More →

All known Type Ia supernovae models fail to reproduce the observed $t_0-M_text{Ni56}$ correlation. (arXiv:2008.13612v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Sharon_A/0/1/0/all/0/1">Amir Sharon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kushnir_D/0/1/0/all/0/1">Doron Kushnir</a> Type Ia supernovae (SNe Ia) are likely the thermonuclear explosions of carbon-oxygen white-dwarf stars, but their progenitor systems remain elusive. A few theoretical scenarios for the progenitor systems have been suggested, which have been shown to agree with some observational properties of SNe Ia. However, several computational challenges prohibit a robust comparison to the observations. We focus on the observed $t_0-M_text{Ni56}$ relation, where $t_0$ (the $gamma$-rays’ escape time from the ejecta) is positively correlated with $M_text{Ni56}$ (the synthesized $^{56}$Ni mass). Comparing to the $t_0-M_text{Ni56}$Read More →

Galaxy Morphology Classification using EfficientNet Architectures. (arXiv:2008.13611v1 [cs.CV]) <a href="http://arxiv.org/find/cs/1/au:+Kalvankar_S/0/1/0/all/0/1">Shreyas Kalvankar</a>, <a href="http://arxiv.org/find/cs/1/au:+Pandit_H/0/1/0/all/0/1">Hrushikesh Pandit</a>, <a href="http://arxiv.org/find/cs/1/au:+Parwate_P/0/1/0/all/0/1">Pranav Parwate</a> We study the usage of EfficientNets and their applications to Galaxy Morphology Classification. We explore the usage of EfficientNets into predicting the vote fractions of the 79,975 testing images from the Galaxy Zoo 2 challenge on Kaggle. We evaluate this model using the standard competition metric i.e. rmse score and rank among the top 3 on the public leaderboard with a public score of 0.07765. We propose a fine-tuned architecture using EfficientNetB5 to classify galaxies into seven classes – completely round smooth, in-between smooth, cigarshaped smooth, lenticular, barredRead More →

Medium modifications for light and heavy nuclear clusters in simulations of core collapse supernovae — Impact on equation of state and weak interactions. (arXiv:2008.13608v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Fischer_T/0/1/0/all/0/1">Tobias Fischer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Typel_S/0/1/0/all/0/1">Stefan Typel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ropke_G/0/1/0/all/0/1">Gerd R&#xf6;pke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bastian_N/0/1/0/all/0/1">Niels-Uwe F. Bastian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Martinez_Pinedo_G/0/1/0/all/0/1">Gabriel Mart&#xed;nez-Pinedo</a> The present article investigates the role of heavy nuclear clusters and weakly bound light nuclear clusters based on a newly developed equation of state for core collapse supernova studies. A novel approach is brought forward for the description of nuclear clusters, taking into account the quasiparticle approach and continuum correlations. It demonstrates that the commonly employed nuclear statistical equilibrium approach, based on non-interacting particles,Read More →

Gravitational-wave memory from a propagating relativistic jet: a probe of the interior of gamma-ray burst progenitors. (arXiv:2001.00205v3 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Yu_Y/0/1/0/all/0/1">Yun-Wei Yu</a> It is believed that the relativistic jets of gamma-ray bursts (GRBs) should initially propagate through a heavy envelope of the massive progenitor stars or through a merger ejecta formed from the compact binary mergers. The interaction of a jet with a stellar envelope or a merger ejecta can lead to the deceleration of the head material of the jet and simultaneously the formation of a hot cocoon. However, this jet-envelope/ejecta interaction is actually undetectable with electromagnetic radiation and can only be inferred indirectlyRead More →

Holographic dark energy with non-minimal derivative coupling to gravity effects. (arXiv:2004.06214v3 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Kritpetch_C/0/1/0/all/0/1">Chonticha Kritpetch</a> (IF Naresuan), <a href="http://arxiv.org/find/gr-qc/1/au:+Muhammad_C/0/1/0/all/0/1">Candrasyah Muhammad</a> (IF Naresuan), <a href="http://arxiv.org/find/gr-qc/1/au:+Gumjudpai_B/0/1/0/all/0/1">Burin Gumjudpai</a> (IF Naresuan and ThEP Center) Non-minimal derivative coupling (NMDC) to gravity in flat FLRW universe is investigated in the scenario of holographic dark energy. Kinetic term is coupled to the Einstein tensor under potential $V = (1/2)m^2 phi^2$. The free kinetic term is allowed to be canonical and phantom. Gravitational constant is modified with the NMDC coupling. Holographic cutoff at Hubble horizon gives modification to dark energy density. We evaluate dark energy equation of state and the variation ofRead More →

Extracting the Possible Intrinsic Relation between Radiative Efficiency and Mass of QSOs: a Maximum Likelihood Method and its Application to the SDSS DR7 QSOs. (arXiv:2008.13555v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_F/0/1/0/all/0/1">Fupeng Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lu_Y/0/1/0/all/0/1">Youjun Lu</a> Radiative efficiencies of QSOs and its distribution encode rich information on the evolution of both masses and spins of massive black holes (MBHs) across cosmic time. In this paper, we develop a maximum likelihood method to statistically extract the intrinsic relation between radiative efficiency ($epsilon$) and mass ($M_{bullet}$) of QSOs from their distribution on the luminosity-(empirically estimated virial) mass plane. By using mock samples, we find that strong constraint can be put onRead More →

Structure of neutron stars in massive scalar-tensor gravity. (arXiv:2007.14429v3 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Rosca_Mead_R/0/1/0/all/0/1">Roxana Rosca-Mead</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Moore_C/0/1/0/all/0/1">Christopher J. Moore</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Sperhake_U/0/1/0/all/0/1">Ulrich Sperhake</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Agathos_M/0/1/0/all/0/1">Michalis Agathos</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Gerosa_D/0/1/0/all/0/1">Davide Gerosa</a> We compute families of spherically symmetric neutron-star models in two-derivative scalar-tensor theories of gravity with a massive scalar field. The numerical approach we present allows us to compute the resulting spacetimes out to infinite radius using a relaxation algorithm on a compactified grid. We discuss the structure of the weakly and strongly scalarized branches of neutron-star models thus obtained and their dependence on the linear and quadratic coupling parameters $alpha_0$, $beta_0$ between the scalar and tensor sectors ofRead More →

Pearson cross-correlation in the first four black hole binary mergers. (arXiv:2008.12663v2 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Marcoccia_P/0/1/0/all/0/1">Paolo Marcoccia</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Fredriksson_F/0/1/0/all/0/1">Felicia Fredriksson</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Nielsen_A/0/1/0/all/0/1">Alex B. Nielsen</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Nardini_G/0/1/0/all/0/1">Germano Nardini</a> We adopt the Pearson cross-correlation measure to analyze the LIGO Hanford and LIGO Livingston detector data streams around the events GW150914, GW151012,GW151226 and GW170104. We find that the Pearson cross-correlation method is sensitive to these signals, with correlations peaking when the black hole binaries reconstructed by the LIGO Scientific and Virgo Collaborations, are merging. We compare the obtained cross-correlations with the statistical correlation fluctuations arising in simulated Gaussian noise data and in LIGO data at times when no eventRead More →

Neutrino Counterparts of Fast Radio Bursts. (arXiv:2008.12318v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Metzger_B/0/1/0/all/0/1">Brian D. Metzger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fang_K/0/1/0/all/0/1">Ke Fang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Margalit_B/0/1/0/all/0/1">Ben Margalit</a> The discovery of a luminous radio burst, FRB 200428, with properties similar to those of fast radio bursts (FRB), in coincidence with an X-ray flare from the Galactic magnetar SGR 1935+2154, supports magnetar models for cosmological FRBs. The burst’s X-ray to radio fluence ratio, as well as the X-ray spectral shape and peak energy, are consistent with FRB 200428 being the result of an ultra-relativistic shock (powered, e.g., by an ejected plasmoid) propagating into a magnetized baryon-rich external medium; the shock simultaneously generates X-ray/gamma-rays via thermalRead More →