RAS_WEB (Page 2,436)

Fitting very flexible models: Linear regression with large numbers of parameters. (arXiv:2101.07256v1 [physics.data-an]) <a href="http://arxiv.org/find/physics/1/au:+Hogg_D/0/1/0/all/0/1">David W. Hogg</a> (NYU), <a href="http://arxiv.org/find/physics/1/au:+Villar_S/0/1/0/all/0/1">Soledad Villar</a> (JHU) There are many uses for linear fitting; the context here is interpolation and denoising of data, as when you have calibration data and you want to fit a smooth, flexible function to those data. Or you want to fit a flexible function to de-trend a time series or normalize a spectrum. In these contexts, investigators often choose a polynomial basis, or a Fourier basis, or wavelets, or something equally general. They also choose an order, or number of basis functions to fit, andRead More →

The effects of density inhomogeneities on the radio wave emission in electron beam plasmas. (arXiv:2005.08876v3 [physics.plasm-ph] UPDATED) <a href="http://arxiv.org/find/physics/1/au:+Yao_X/0/1/0/all/0/1">Xin Yao</a>, <a href="http://arxiv.org/find/physics/1/au:+Munoz_P/0/1/0/all/0/1">Patricio A. Mu&#xf1;oz</a>, <a href="http://arxiv.org/find/physics/1/au:+Buchner_J/0/1/0/all/0/1">J&#xf6;rg B&#xfc;chner</a>, <a href="http://arxiv.org/find/physics/1/au:+Zhou_X/0/1/0/all/0/1">Xiaowei Zhou</a>, <a href="http://arxiv.org/find/physics/1/au:+Liu_S/0/1/0/all/0/1">Siming Liu</a> Type III radio bursts are radio emissions associated with solar flares. They are considered to be caused by electron beams traveling from the solar corona to the solar wind. Magnetic reconnection is a possible accelerator of electron beams in the course of solar flares since it causes unstable distribution functions, and density inhomogeneities (cavities). The properties of radio emission by electron beams in an inhomogeneous environment are still poorly understood. We captureRead More →

A Test of the Cosmological Principle with Quasars. (arXiv:2009.14826v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Secrest_N/0/1/0/all/0/1">Nathan Secrest</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hausegger_S/0/1/0/all/0/1">Sebastian von Hausegger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rameez_M/0/1/0/all/0/1">Mohamed Rameez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mohayaee_R/0/1/0/all/0/1">Roya Mohayaee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sarkar_S/0/1/0/all/0/1">Subir Sarkar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Colin_J/0/1/0/all/0/1">Jacques Colin</a> We study the large-scale anisotropy of the Universe by measuring the dipole in the angular distribution of a flux-limited, all-sky sample of 1.36 million quasars observed by the Wide-field Infrared Survey Explorer (WISE). This sample is derived from the new CatWISE2020 catalog, which contains deep photometric measurements at 3.4 and 4.6 $mu$m from the cryogenic, post-cryogenic, and reactivation phases of the WISE mission. While the direction of the dipole in the quasar sky is similarRead More →

Newtonian-like gravity with variable $G$. (arXiv:2009.04434v4 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Fabris_J/0/1/0/all/0/1">J&#xfa;lio C. Fabris</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Gomes_T/0/1/0/all/0/1">Tales Gomes</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Toniato_J/0/1/0/all/0/1">J&#xfa;nior D. Toniato</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Velten_H/0/1/0/all/0/1">Hermano Velten</a> We propose a Lagrangian formulation for a varying $G$ Newtonian-like theory inspired by the Brans-Dicke gravity. Rather than imposing an {it ad hoc} dependence for the gravitational coupling, as previously done in the literature, in our proposal the running of $G$ emerges naturally from the internal dynamical structure of the theory. We explore the features of the resulting gravitational field for static and spherically symmetric mass distributions as well as within the cosmological framework. We propose a Lagrangian formulation for a varying $G$Read More →

The COMBS Survey — II. Distinguishing the Metal-Poor Bulge from the Halo Interlopers. (arXiv:2009.03886v3 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Lucey_M/0/1/0/all/0/1">Madeline Lucey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hawkins_K/0/1/0/all/0/1">Keith Hawkins</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ness_M/0/1/0/all/0/1">Melissa Ness</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Debattista_V/0/1/0/all/0/1">Victor P. Debattista</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Luna_A/0/1/0/all/0/1">Alice Luna</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Asplund_M/0/1/0/all/0/1">Martin Asplund</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bensby_T/0/1/0/all/0/1">Thomas Bensby</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Casagrande_L/0/1/0/all/0/1">Luca Casagrande</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Feltzing_S/0/1/0/all/0/1">Sofia Feltzing</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Freeman_K/0/1/0/all/0/1">Kenneth C. Freeman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kobayashi_C/0/1/0/all/0/1">Chiaki Kobayashi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marino_A/0/1/0/all/0/1">Anna F. Marino</a> The metal-poor stars in the bulge are important relics of the Milky Way’s formation history, as simulations predict that they are some of the oldest stars in the Galaxy. In order to determine if they are truly ancient stars, we must understand the origins of this population. Currently, it isRead More →

The EFT Likelihood for Large-Scale Structure in Redshift Space. (arXiv:2007.14988v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Cabass_G/0/1/0/all/0/1">Giovanni Cabass</a> We study the EFT likelihood for biased tracers in redshift space, for which the bias expansion of the galaxy velocity field $mathbf{v}_g$ plays a fundamental role. The equivalence principle forbids stochastic contributions to $mathbf{v}_g$ to survive at small $k$. Therefore, at leading order in derivatives the form of the likelihood ${cal P}[tilde{delta}_g|delta,!mathbf{v}]$ to observe a redshift-space galaxy overdensity $tilde{delta}_g(tilde{mathbf{x}})$ given a rest-frame matter and velocity fields $delta(mathbf{x})$, $mathbf{v}(mathbf{x})$ is fixed by the rest-frame noise. If this noise is Gaussian with constant power spectrum, ${cal P}[tilde{delta}_g|delta,!mathbf{v}]$ is also a Gaussian inRead More →

Axion quality from the (anti)symmetric of SU(N). (arXiv:2007.12663v3 [hep-ph] UPDATED) <a href="http://arxiv.org/find/hep-ph/1/au:+Ardu_M/0/1/0/all/0/1">Marco Ardu</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Luzio_L/0/1/0/all/0/1">Luca Di Luzio</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Landini_G/0/1/0/all/0/1">Giacomo Landini</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Strumia_A/0/1/0/all/0/1">Alessandro Strumia</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Teresi_D/0/1/0/all/0/1">Daniele Teresi</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Wang_J/0/1/0/all/0/1">Jin-Wei Wang</a> We propose two models where a U(1) Peccei-Quinn global symmetry arises accidentally and is respected up to high-dimensional operators, so that the axion solution to the strong CP problem is successful even in the presence of Planck-suppressed operators. One model is SU$(N)$ gauge interactions with fermions in the fundamental and a scalar in the symmetric. The axion arises from spontaneous symmetry breaking to SO$(N)$, that confines at a lower energy scale. Axion quality in the modelRead More →

Detection of Gravitational Waves Using Bayesian Neural Networks. (arXiv:2007.04176v2 [astro-ph.IM] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Lin_Y/0/1/0/all/0/1">Yu-Chiung Lin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wu_J/0/1/0/all/0/1">Jiun-Huei Proty Wu</a> We propose a new model of Bayesian Neural Networks to not only detect the events of compact binary coalescence in the observational data of gravitational waves (GW) but also identify the full length of the event duration including the inspiral stage. This is achieved by incorporating the Bayesian approach into the CLDNN classifier, which integrates together the Convolutional Neural Network (CNN) and the Long Short-Term Memory Recurrent Neural Network (LSTM). Our model successfully detect all seven BBH events in the LIGO Livingston O2 data, with the periodsRead More →

Cosmic rays across the star-forming galaxy sequence. I: Cosmic ray pressures and calorimetry. (arXiv:2006.15819v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Crocker_R/0/1/0/all/0/1">Roland M. Crocker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Krumholz_M/0/1/0/all/0/1">Mark R. Krumholz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Thompson_T/0/1/0/all/0/1">Todd A. Thompson</a> In the Milky Way, cosmic rays (CRs) are dynamically important in the interstellar medium, contribute to hydrostatic balance, and may help regulate star formation. However, we know far less about the importance of CRs in galaxies whose gas content or star formation rate differ significantly from those of the Milky Way. Here we construct self-consistent models for hadronic CR transport, losses, and contribution to pressure balance as a function of galaxy properties, covering a broad range ofRead More →

2020 Global reassessment of the neutrino oscillation picture. (arXiv:2006.11237v2 [hep-ph] UPDATED) <a href="http://arxiv.org/find/hep-ph/1/au:+Salas_P/0/1/0/all/0/1">P. F. de Salas</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Forero_D/0/1/0/all/0/1">D. V. Forero</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Gariazzo_S/0/1/0/all/0/1">S. Gariazzo</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Martinez_Mirave_P/0/1/0/all/0/1">P. Mart&#xed;nez-Mirav&#xe9;</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Mena_O/0/1/0/all/0/1">O. Mena</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Ternes_C/0/1/0/all/0/1">C. A. Ternes</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Tortola_M/0/1/0/all/0/1">M. T&#xf3;rtola</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Valle_J/0/1/0/all/0/1">J. W. F. Valle</a> We present an updated global fit of neutrino oscillation data in the simplest three-neutrino framework. In the present study we include up-to-date analyses from a number of experiments. Concerning the atmospheric and solar sectors, we give updated analyses of DeepCore and SNO data, respectively. We have also included the latest electron antineutrino data collected by the Daya Bay and RENO reactor experiments, and theRead More →

Testing one-loop galaxy bias: Power spectrum. (arXiv:2006.09729v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Eggemeier_A/0/1/0/all/0/1">Alexander Eggemeier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Scoccimarro_R/0/1/0/all/0/1">Rom&#xe1;n Scoccimarro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Crocce_M/0/1/0/all/0/1">Martin Crocce</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pezzotta_A/0/1/0/all/0/1">Andrea Pezzotta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sanchez_A/0/1/0/all/0/1">Ariel G. S&#xe1;nchez</a> We test the regime of validity of one-loop galaxy bias for a wide variety of biased tracers. Our most stringent test asks the bias model to simultaneously match the galaxy-galaxy and galaxy-mass spectrum, using the measured nonlinear matter spectrum from the simulations to test one-loop effects from the bias expansion alone. In addition, we investigate the relevance of short-range nonlocality and halo exclusion through higher-derivative and scale-dependent noise terms, as well as the impact of using co-evolution relations to reduceRead More →

Unravelling stellar populations in the Andromeda Galaxy. (arXiv:2005.04052v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Gajda_G/0/1/0/all/0/1">Grzegorz Gajda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gerhard_O/0/1/0/all/0/1">Ortwin Gerhard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blana_M/0/1/0/all/0/1">Mat&#xed;as Bla&#xf1;a</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhu_L/0/1/0/all/0/1">Ling Zhu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shen_J/0/1/0/all/0/1">Juntai Shen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Saglia_R/0/1/0/all/0/1">Roberto P. Saglia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bender_R/0/1/0/all/0/1">Ralf Bender</a> To understand the history and formation mechanisms of galaxies it is crucial to determine their current multidimensional structure. Here we focus on stellar population properties, such as metallicity and [$alpha$/Fe] enhancement. We devise a new technique to recover the distribution of these parameters using spatially resolved, line-of-sight averaged data. Our chemodynamical method is based on the made-to-measure (M2M) framework and results in an $N$-body model for the abundance distribution. We test our methodRead More →

A Microwave SQUID Multiplexer Optimized for Bolometric Applications. (arXiv:2010.07998v2 [astro-ph.IM] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Dober_B/0/1/0/all/0/1">B. Dober</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ahmed_Z/0/1/0/all/0/1">Z. Ahmed</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arnold_K/0/1/0/all/0/1">K. Arnold</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Becker_D/0/1/0/all/0/1">D.T. Becker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bennett_D/0/1/0/all/0/1">D.A. Bennett</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Connors_J/0/1/0/all/0/1">J.A. Connors</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cukierman_A/0/1/0/all/0/1">A. Cukierman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DEwart_J/0/1/0/all/0/1">J.M. D&#x27;Ewart</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Duff_S/0/1/0/all/0/1">S.M. Duff</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dusatko_J/0/1/0/all/0/1">J.E. Dusatko</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Frisch_J/0/1/0/all/0/1">J.C. Frisch</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gard_J/0/1/0/all/0/1">J.D. Gard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Henderson_S/0/1/0/all/0/1">S.W. Henderson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Herbst_R/0/1/0/all/0/1">R. Herbst</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hilton_G/0/1/0/all/0/1">G.C. Hilton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hubmayr_J/0/1/0/all/0/1">J. Hubmayr</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_Y/0/1/0/all/0/1">Y. Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mates_J/0/1/0/all/0/1">J.A.B. Mates</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McCarrick_H/0/1/0/all/0/1">H. McCarrick</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reintsema_C/0/1/0/all/0/1">C.D Reintsema</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Silva_Feaver_M/0/1/0/all/0/1">M. Silva-Feaver</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ruckman_L/0/1/0/all/0/1">L. Ruckman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ullom_J/0/1/0/all/0/1">J.N. Ullom</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vale_L/0/1/0/all/0/1">L.R. Vale</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Winkle_D/0/1/0/all/0/1">D.D. Van Winkle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vasquez_J/0/1/0/all/0/1">J. Vasquez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_Y/0/1/0/all/0/1">Y. Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Young_E/0/1/0/all/0/1">E. Young</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yu_C/0/1/0/all/0/1">C. Yu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zheng_K/0/1/0/all/0/1">K. Zheng</a> A microwave SQUIDRead More →

A two-moment radiation hydrodynamics scheme applicable to simulations of planet formation in circumstellar disks. (arXiv:2005.01785v2 [astro-ph.EP] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Fuksman_J/0/1/0/all/0/1">Julio David Melon Fuksman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Klahr_H/0/1/0/all/0/1">Hubert Klahr</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Flock_M/0/1/0/all/0/1">Mario Flock</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mignone_A/0/1/0/all/0/1">Andrea Mignone</a> We present a numerical code for radiation hydrodynamics designed as a module for the freely available PLUTO code. We adopt a gray approximation and include radiative transfer following a two-moment approach by imposing the M1 closure to the radiation fields. This closure allows for a description of radiative transport in both the diffusion and free-streaming limits, and is able to describe highly anisotropic radiation transport as can be expected in the vicinity of anRead More →

The possibility of twin star solutions in a model based on lattice QCD thermodynamics. (arXiv:2004.07026v2 [nucl-th] UPDATED) <a href="http://arxiv.org/find/nucl-th/1/au:+Jakobus_P/0/1/0/all/0/1">P. Jakobus</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Motornenko_A/0/1/0/all/0/1">A. Motornenko</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Gomes_R/0/1/0/all/0/1">R. O. Gomes</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Steinheimer_J/0/1/0/all/0/1">J. Steinheimer</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Stoecker_H/0/1/0/all/0/1">H. Stoecker</a> The properties of compact stars and in particular the existence of twin star solutions are investigated within an effective model that is constrained by lattice QCD thermodynamics. The model is modified at large baryon densities to incorporate a large variety of scenarios of first order phase transitions to a phase of deconfined quarks. This is achieved by matching two different variants of the bag model equation of state, in order to estimateRead More →

The Impact of Light Polarization Effects on Weak Lensing Systematics. (arXiv:1910.05063v2 [astro-ph.IM] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Lin_C/0/1/0/all/0/1">Chien-Hao Lin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tan_B/0/1/0/all/0/1">Brent Tan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mandelbaum_R/0/1/0/all/0/1">Rachel Mandelbaum</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hirata_C/0/1/0/all/0/1">Christopher M. Hirata</a> A fraction of the light observed from edge-on disk galaxies is polarized due to two physical effects: selective extinction by dust grains aligned with the magnetic field, and scattering of the anisotropic starlight field. Since the reflection and transmission coefficients of the reflecting and refracting surfaces in an optical system depend on the polarization of incoming rays, this optical polarization produces both (a) a selection bias in favor of galaxies with specific orientations and (b) a polarization-dependent PSF. InRead More →

On the Shapes of Interstellar Grains: Modeling Extinction and Polarization by Spheroids and Continuous Distributions of Ellipsoids. (arXiv:1710.08968v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Draine_B/0/1/0/all/0/1">B. T. Draine</a> (Princeton), <a href="http://arxiv.org/find/astro-ph/1/au:+Hensley_B/0/1/0/all/0/1">Brandon S. Hensley</a> (Princeton) Although interstellar grains are known to be aspherical, their actual shapes remain poorly constrained. We assess whether three continuous distributions of ellipsoidal shapes from the literature are suitable for describing the shapes of interstellar grains. Randomly-selected shapes from each distribution are shown as illustrations. The often-used Bohren-Huffman CDE includes a very large fraction of extreme shapes: fully 10% of random draws have axial ratio $a_3/a_1 > 19.7$, and 5% have $a_3/a_1 > 33$. The CDE2Read More →

Energy conditions and entropy density of the universe. (arXiv:1009.4513v3 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_W/0/1/0/all/0/1">Wen-Fei Liu</a> (1 and 2), <a href="http://arxiv.org/find/astro-ph/1/au:+Niu_J/0/1/0/all/0/1">Jing Niu</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Li_J/0/1/0/all/0/1">Juan Li</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_T/0/1/0/all/0/1">Tong-Jie Zhang</a> (2 and 1) ((1) College of Physics and Electronic Engineering, Qilu Normal University,(2) Department of Astronomy, Beijing Normal University) In the standard Friedmann-Lemaitre-Robertson-Walker (FLRW) cosmological model, the energy conditions provides model-independent bounds on the behavior of the distance modulus. However, this method can not provide us the detailed information about the violation between the energy conditions and the observation. In this paper, we present an extended analysis of the energy conditions based upon the entropy density ofRead More →

Agile Scrum Development in an ad hoc Software Collaboration. (arXiv:2101.07779v1 [cs.SE]) <a href="http://arxiv.org/find/cs/1/au:+Baxter_A/0/1/0/all/0/1">A. L. Baxter</a>, <a href="http://arxiv.org/find/cs/1/au:+BenZvi_S/0/1/0/all/0/1">S. Y. BenZvi</a>, <a href="http://arxiv.org/find/cs/1/au:+Bonivento_W/0/1/0/all/0/1">W. Bonivento</a>, <a href="http://arxiv.org/find/cs/1/au:+Brazier_A/0/1/0/all/0/1">A. Brazier</a>, <a href="http://arxiv.org/find/cs/1/au:+Clark_M/0/1/0/all/0/1">M. Clark</a>, <a href="http://arxiv.org/find/cs/1/au:+Coleiro_A/0/1/0/all/0/1">A. Coleiro</a>, <a href="http://arxiv.org/find/cs/1/au:+Collom_D/0/1/0/all/0/1">D. Collom</a>, <a href="http://arxiv.org/find/cs/1/au:+Colomer_Molla_M/0/1/0/all/0/1">M. Colomer-Molla</a>, <a href="http://arxiv.org/find/cs/1/au:+Cousins_B/0/1/0/all/0/1">B. Cousins</a>, <a href="http://arxiv.org/find/cs/1/au:+Orellana_A/0/1/0/all/0/1">A. Delgado Orellana</a>, <a href="http://arxiv.org/find/cs/1/au:+Dornic_D/0/1/0/all/0/1">D. Dornic</a>, <a href="http://arxiv.org/find/cs/1/au:+Ekimtcov_V/0/1/0/all/0/1">V. Ekimtcov</a>, <a href="http://arxiv.org/find/cs/1/au:+ElSayed_S/0/1/0/all/0/1">S. ElSayed</a>, <a href="http://arxiv.org/find/cs/1/au:+Rosso_A/0/1/0/all/0/1">A. Gallo Rosso</a>, <a href="http://arxiv.org/find/cs/1/au:+Godwin_P/0/1/0/all/0/1">P. Godwin</a>, <a href="http://arxiv.org/find/cs/1/au:+Griswold_S/0/1/0/all/0/1">S. Griswold</a>, <a href="http://arxiv.org/find/cs/1/au:+Habig_A/0/1/0/all/0/1">A. Habig</a>, <a href="http://arxiv.org/find/cs/1/au:+Horiuchi_S/0/1/0/all/0/1">S. Horiuchi</a>, <a href="http://arxiv.org/find/cs/1/au:+Howell_D/0/1/0/all/0/1">D. A. Howell</a>, <a href="http://arxiv.org/find/cs/1/au:+Johnson_M/0/1/0/all/0/1">M. W. G. Johnson</a>, <a href="http://arxiv.org/find/cs/1/au:+Juric_M/0/1/0/all/0/1">M. Juric</a>, <a href="http://arxiv.org/find/cs/1/au:+Kneller_J/0/1/0/all/0/1">J. P. Kneller</a>, <a href="http://arxiv.org/find/cs/1/au:+Kopec_A/0/1/0/all/0/1">A. Kopec</a>, <a href="http://arxiv.org/find/cs/1/au:+Kopper_C/0/1/0/all/0/1">C. Kopper</a>, <a href="http://arxiv.org/find/cs/1/au:+Kulikovskiy_V/0/1/0/all/0/1">V. Kulikovskiy</a>, <a href="http://arxiv.org/find/cs/1/au:+Lamoureux_M/0/1/0/all/0/1">M. Lamoureux</a>, <a href="http://arxiv.org/find/cs/1/au:+Lang_R/0/1/0/all/0/1">R. F. Lang</a>, <a href="http://arxiv.org/find/cs/1/au:+Li_S/0/1/0/all/0/1">S. Li</a>, <aRead More →

Multiwavelength constraints on the unidentified Galactic TeV sources HESS J1427$-$608, HESS J1458$-$608, and new VHE $gamma$-ray source candidates. (arXiv:2101.07775v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Devin_J/0/1/0/all/0/1">Justine Devin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Renaud_M/0/1/0/all/0/1">Matthieu Renaud</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lemoine_Goumard_M/0/1/0/all/0/1">Marianne Lemoine-Goumard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vasileiadis_G/0/1/0/all/0/1">Georges Vasileiadis</a> The H.E.S.S. Galactic Plane Survey (HGPS) revealed 78 TeV sources among which 47 are not clearly associated with a known object. We present a multiwavelength approach to constrain the origin of the emission from unidentified HGPS sources. We present a generic pipeline that explores a large database of multiwavelength archival data toward any region in the Galactic plane. Along with a visual inspection of the retrieved multiwavelength observations to search for faint andRead More →