RAS_WEB (Page 4,568)

Understanding the galactic cosmic ray dipole anisotropy with a nearby single source under the spatially-dependent propagation scenario. (arXiv:1901.00249v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Qu_X/0/1/0/all/0/1">Xiaobo Qu</a> Recently studies of the dipole anisotropy in the arrival directions of Galactic cosmic rays indicate that the TeV-PeV dipole anisotropy amplitude is not described by a simple power law, moreover a rapid phase change exists at an energy of $0.1sim0.3$ PeV. In this work we argue that the dipole anisotropy amplitude and phase evolution with energies can be reproduced under the spatially-dependent propagation scenario with a nearby single source added. Our results indicate a nearby single source have significant influence to the cosmicRead More →

The Milky Way Imaging Scroll Painting (MWISP): Project Details and Initial Results from the Galactic Longitude of 25.8deg to 49.7deg. (arXiv:1901.00285v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Su_Y/0/1/0/all/0/1">Yang Su</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yang_J/0/1/0/all/0/1">Ji Yang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_S/0/1/0/all/0/1">Shaobo Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gong_Y/0/1/0/all/0/1">Yan Gong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_H/0/1/0/all/0/1">Hongchi Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhou_X/0/1/0/all/0/1">Xin Zhou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_M/0/1/0/all/0/1">Min Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_Z/0/1/0/all/0/1">Zhiwei Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sun_Y/0/1/0/all/0/1">Yan Sun</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_X/0/1/0/all/0/1">Xuepeng Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xu_Y/0/1/0/all/0/1">Ye Xu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jiang_Z/0/1/0/all/0/1">Zhibo Jiang</a> The Milky Way Imaging Scroll Painting (MWISP) project is an unbiased Galactic plane CO survey for mapping regions of l=-10deg to +250deg and |b|Read More →

Analysis of layering-related linear features on comet 67P/Churyumov-Gerasimenko. (arXiv:1901.00290v1 [astro-ph.EP]) <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:+Penasa_L/0/1/0/all/0/1">Luca Penasa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boehnhardt_H/0/1/0/all/0/1">Hermann Boehnhardt</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:+Dolives_B/0/1/0/all/0/1">Benoit Dolives</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Souvannavong_F/0/1/0/all/0/1">Fabrice Souvannavong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Remetean_E/0/1/0/all/0/1">Emile Remetean</a> We analysed layering-related linear features on the surface of comet 67P/Churyumov-Gerasimenko (67P) to determine the internal configuration of the layerings within the nucleus. We used high-resolution images from the OSIRIS Narrow Angle Camera onboard the Rosetta spacecraft, projected onto the SHAP7 shape model of the nucleus, to map 171 layering-related linear features which we believe to represent terrace margins and strata heads. From these curved lineaments, extending laterally to up to 1925 m, weRead More →

Graph Database Solution for Higher Order Spatial Statistics in the Era of Big Data. (arXiv:1901.00296v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Sabiu_C/0/1/0/all/0/1">Cristiano G. Sabiu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hoyle_B/0/1/0/all/0/1">Ben Hoyle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_J/0/1/0/all/0/1">Juhan Kim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_X/0/1/0/all/0/1">Xiao-Dong Li</a> We present an algorithm for the fast computation of the general $N$-point spatial correlation functions of any discrete point set embedded within an Euclidean space of $mathbb{R}^n$. Utilizing the concepts of kd-trees and graph databases, we describe how to count all possible $N$-tuples in binned configurations within a given length scale, e.g. all pairs of points or all triplets of points with side lengths $Read More →

Rotational Evolution of The Slowest Radio Pulsar PSR J0250+5854. (arXiv:1901.00300v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Kou_F/0/1/0/all/0/1">F.F. Kou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tong_H/0/1/0/all/0/1">H.Tong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xu_R/0/1/0/all/0/1">R. X. Xu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhou_X/0/1/0/all/0/1">X. Zhou</a> We apply theoretical spin-down models of magentospheric evolution and magentic field decay to simulate the possible evolution of PSR J0250+5854, which is the slowest-spinning radio pulsar by now. It is possible that PSR J0250+5854 has a small inclination angle but a relatively high magnetic field by considering the alignment of inclination angle in a 3-D magnetosphere. Our calculations show that PSR J0250+5854 may be an old high magnetic field pulsar or magnetar. In this case, the clustering of similarly long-period pulsars wouldRead More →

Radial Acceleration Relation from Ultra-light Scalar Dark matter. (arXiv:1901.00305v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_J/0/1/0/all/0/1">Jae-Weon Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_H/0/1/0/all/0/1">Hyeong-Chan Kim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_J/0/1/0/all/0/1">Jungjai Lee</a> We show that ultra-light scalar dark matter (fuzzy dark matter) has a quantum mechanical universal acceleration scale about $10^{-10}ms^{-2}$, which naturally leads to the baryonic Tully-Fisher relation dynamically established. Baryon matter at central parts of galaxies acts as a boundary condition for dark matter wave equation and influences stellar rotation velocities in halos. This model also explains the radial acceleration relation and MOND-like behavior of gravitational acceleration found in various type of galaxies without any modification of gravity or mechanics. This analysis can be extended toRead More →

He-accreting WD: Nucleosynthesis in the extreme binary system (1.02+0.30) M$_odot$. (arXiv:1901.00340v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Piersanti_L/0/1/0/all/0/1">L. Piersanti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yungelson_L/0/1/0/all/0/1">L.R. Yungelson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cristallo_S/0/1/0/all/0/1">S. Cristallo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tornambe_A/0/1/0/all/0/1">A. Tornamb&#xe9;</a> We investigate the evolutionary properties of AM~CVn stars with massive white dwarf donors and accretors. As a representative of them we consider a binary initially composed by a 0.30 M$_odot$, He WD and a 1.02 M$_odot$, CO WD. We evaluate the time-dependent mass transfer rate from the donor and compute the evolution of the accretor, accounting for the effects of mass exchange on the evolution of orbital parameters. We model the thermal response of the accreting CO WD with the FUNRead More →

Contribution of Cosmic Rays from Sources with a Monoenergetic Proton Spectrum to the Extragalactic Diffuse Gamma-Ray Emission. (arXiv:1901.00376v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Uryson_A/0/1/0/all/0/1">Anna Uryson</a> The extragalactic sources of ultra-high-energy (E > 4×10^19 eV) cosmic rays that make a small contribution to the flux of particles recorded by ground-based arrays are discussed. We show that cosmic rays from such sources can produce a noticeable diffuse gamma-ray flux in intergalactic space compared to the the data obtained with Fermi LAT (onboard the Fermi space observatory). A possible type of active galactic nuclei (AGNs) in which cosmic-ray protons can be accelerated to energies 1021 eV is considered as an illustrationRead More →

Optical spectroscopic and polarization properties of 2011 outburst of the recurrent nova T Pyxidis. (arXiv:1901.00404v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Pavana_M/0/1/0/all/0/1">M. Pavana</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anche_R/0/1/0/all/0/1">Ramya M Anche</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anupama_G/0/1/0/all/0/1">G. C. Anupama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ramaprakash_A/0/1/0/all/0/1">A. N. Ramaprakash</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Selvakumar_G/0/1/0/all/0/1">G. Selvakumar</a> We study the spectroscopic and ionized structural evolution of T Pyx during its 2011 outburst, and also study the variation in degree of polarization during its early phase. Optical spectroscopic data of this system obtained from day 1.28–2415.62 since discovery, and optical, broadband imaging polarimetric observations obtained from day 1.36–29.33 during the early phases of the outburst are used in the study. The physical conditions and the geometry of the ionizedRead More →

HIDES spectroscopy of bright detached eclipsing binaries from the $Kepler$ field – III. Spectral analysis, updated parameters, and new systems. (arXiv:1901.00407v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Helminiak_K/0/1/0/all/0/1">K. G. He&#x142;miniak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Konacki_M/0/1/0/all/0/1">M. Konacki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maehara_H/0/1/0/all/0/1">H. Maehara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kambe_E/0/1/0/all/0/1">E. Kambe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ukita_N/0/1/0/all/0/1">N. Ukita</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ratajczak_M/0/1/0/all/0/1">M. Ratajczak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pigulski_A/0/1/0/all/0/1">A. Pigulski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kozlowski_S/0/1/0/all/0/1">S. K. Koz&#x142;owski</a> We present the latest results of our spectroscopic observations and refined modelling of a sample of detached eclipsing binaries (DEBs), selected from the $Kepler$} Eclipsing Binary Catalog, that are also double-lined spectroscopic binaries (SB2). New high resolution spectra obtained with the HIDES spectrograph, attached to the 1.88-m telescope of the Okayama Astrophysical Observatory supplemented the previous observations,Read More →

A Cloud-based architecture for the Cherenkov Telescope Array observation simulations. Optimisation, design, and results. (arXiv:1901.00410v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Landoni_M/0/1/0/all/0/1">M. Landoni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Romano_P/0/1/0/all/0/1">P. Romano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vercellone_S/0/1/0/all/0/1">S. Vercellone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Knodlseder_J/0/1/0/all/0/1">J. Knodlseder</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bianco_A/0/1/0/all/0/1">A. Bianco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tavecchio_F/0/1/0/all/0/1">F. Tavecchio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Corina_A/0/1/0/all/0/1">A. Corina</a> Simulating and analysing detailed observations of astrophysical sources for very high energy (VHE) experiments, like the Cherenkov Telescope Array (CTA), can be a demanding task especially in terms of CPU consumption and required storage. In this context, we propose an innovative cloud computing architecture based on Amazon Web Services (AWS) aiming to decrease the amount of time required to simulate and analyse a given field by distributing theRead More →

A special giant impact and its influence on Earths core and mantle. (arXiv:1901.00420v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Zhou_Y/0/1/0/all/0/1">You Zhou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reinhardt_C/0/1/0/all/0/1">Christian Reinhardt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Deng_H/0/1/0/all/0/1">Hongping Deng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xiaobin_C/0/1/0/all/0/1">Cao Xiaobin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_Y/0/1/0/all/0/1">Yun Liu</a> It is believed that tens of giant impacts had happened during the accretion of Earth. How these giant impacts occur has significant influence on the chemistry and physics of Earths mantle and core. Although the core-merging giant impact (CMGI) has been proposed by previous researchers, its occurrence and consequence are not well understood yet. Here the occurrence conditions of a CMGI had been studied via 800 runs of smoothed particle hydrodynamics simulations. The results show thatRead More →

Laboratory spectroscopic study of the $^{15}$N isotopomers of cyanamide, H$_2$NCN, and a search for them toward IRAS 16293$-$2422 B. (arXiv:1901.00421v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Coutens_A/0/1/0/all/0/1">A. Coutens</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zakharenko_O/0/1/0/all/0/1">O. Zakharenko</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lewen_F/0/1/0/all/0/1">F. Lewen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jorgensen_J/0/1/0/all/0/1">J. K. J&#xf8;rgensen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schlemmer_S/0/1/0/all/0/1">S. Schlemmer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Muller_H/0/1/0/all/0/1">H. S. P. M&#xfc;ller</a> Cyanamide is one of the few interstellar molecules containing two chemically different N atoms. It was detected recently toward the solar-type protostar IRAS 16293-2422 B together with H$_2$N$^{13}$CN and HDNCN in the course of the Atacama Large Millemeter/submillimeter Array (ALMA) Protostellar Interferometric Line Survey (PILS). The detection of the 15N isotopomers or the determination of upper limits to their column densities was hamperedRead More →

Helicity hardens the gas. (arXiv:1901.00423v1 [physics.flu-dyn]) <a href="http://arxiv.org/find/physics/1/au:+Peng_J/0/1/0/all/0/1">Jun Peng</a>, <a href="http://arxiv.org/find/physics/1/au:+Xu_J/0/1/0/all/0/1">Jin-Xiu Xu</a>, <a href="http://arxiv.org/find/physics/1/au:+Yang_Y/0/1/0/all/0/1">Yan Yang</a>, <a href="http://arxiv.org/find/physics/1/au:+Zhu_J/0/1/0/all/0/1">Jian-Zhou Zhu</a> A screw generally works better than a nail, or a complicated rope knot better than a simple one, in fastening solid matter, but a gas is more tameless. However, a flow itself has a physical quantity, helicity, measuring the screwing strength of the velocity field and the degree of the knottedness of the vorticity ropes. It is shown that helicity favors the partition of energy to the vortical modes, compared to others such as the dilatation and pressure modes of turbulence; that is, helicity stiffens the flow,Read More →

Stellar Flares from the First Tess Data Release: Exploring a New Sample of M-dwarfs. (arXiv:1901.00443v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Gunther_M/0/1/0/all/0/1">Maximilian N. G&#xfc;nther</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhan_Z/0/1/0/all/0/1">Zhuchang Zhan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Seager_S/0/1/0/all/0/1">Sara Seager</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rimmer_P/0/1/0/all/0/1">Paul B. Rimmer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ranjan_S/0/1/0/all/0/1">Sukrit Ranjan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stassun_K/0/1/0/all/0/1">Keivan G. Stassun</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oelkers_R/0/1/0/all/0/1">Ryan J. Oelkers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Daylan_T/0/1/0/all/0/1">Tansu Daylan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Newton_E/0/1/0/all/0/1">Elisabeth Newton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gillen_E/0/1/0/all/0/1">Edward Gillen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rappaport_S/0/1/0/all/0/1">Saul Rappaport</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ricker_G/0/1/0/all/0/1">George R. Ricker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Latham_D/0/1/0/all/0/1">David W. Latham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Winn_J/0/1/0/all/0/1">Joshua N. Winn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jenkins_J/0/1/0/all/0/1">Jon M. Jenkins</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Glidden_A/0/1/0/all/0/1">Ana Glidden</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fausnaugh_M/0/1/0/all/0/1">Michael Fausnaugh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Levine_A/0/1/0/all/0/1">Alan M. Levine</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dittmann_J/0/1/0/all/0/1">Jason A. Dittmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Quinn_S/0/1/0/all/0/1">Samuel N. Quinn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Krishnamurthy_A/0/1/0/all/0/1">Akshata Krishnamurthy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ting_E/0/1/0/all/0/1">Eric B. Ting</a> We perform a study of stellar flares for the 24,809 starsRead More →

Spatial and temporal structure of EAS reflected Cherenkov light signal. (arXiv:1901.00452v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Antonov_R/0/1/0/all/0/1">R.A. Antonov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bonvech_E/0/1/0/all/0/1">E.A. Bonvech</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chernov_D/0/1/0/all/0/1">D.V. Chernov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dzhatdoev_T/0/1/0/all/0/1">T.A. Dzhatdoev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Galkin_V/0/1/0/all/0/1">V.I. Galkin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Podgrudkov_D/0/1/0/all/0/1">D.A. Podgrudkov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Roganova_T/0/1/0/all/0/1">T.M. Roganova</a> A compact device lifted over the ground surface might be used to observe optical radiation of extensive air showers (EAS). Here we consider spatial and temporal characteristics of Vavilov-Cherenkov radiation (“Cherenkov light”) reflected from the snow surface of Lake Baikal, as registered by the SPHERE-2 detector. We perform detailed full direct Monte Carlo simulations of EAS development and present a dedicated highly modular code intended for detector response simulations. Detector response propertiesRead More →

The High-energy emission of jetted AGN. (arXiv:1901.00462v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Schwartz_D/0/1/0/all/0/1">Daniel A. Schwartz</a> Quasars with flat radio spectra and one-sided, arc-second scale, ~100 mJy GHz radio jets are found to have similar scale X-ray jets in about 60% of such objects, even in short 5 to 10 ks Chandra observations. Jets emit in the GHz band via synchrotron radiation, as known from polarization measurements. The X-ray emission is explained most simply, i.e. with the fewest additional parameters, as inverse Compton (iC) scattering of cosmic microwave background (CMB) photons by the relativistic electrons in the jet. With physics based assumptions, one can estimate enthalpy fuxes upwards ofRead More →

On the Compton scattering redistribution function in plasma. (arXiv:1602.05088v4 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Madej_J/0/1/0/all/0/1">J. Madej</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rozanska_A/0/1/0/all/0/1">A. R&#xf3;&#x17c;a&#x144;ska</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Majczyna_A/0/1/0/all/0/1">A. Majczyna</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nalezyty_M/0/1/0/all/0/1">M. Nale&#x17c;yty</a> Compton scattering is the dominant opacity source in hot neutron stars, accretion disks around black holes and hot coronae. We collected here a set of numerical expressions of the Compton scattering redistribution functions for unpolarized radiation (RF), which are more exact than the widely used Kompaneets equation. The principal aim of this paper is presentation of the RF by Guilbert (1981) which is corrected for the computational errors in the original paper. This corrected RF was used in the series of papersRead More →

Galaxy Quenching from Cosmic Web Detachment. (arXiv:1607.07881v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Aragon_Calvo_M/0/1/0/all/0/1">Miguel A. Aragon-Calvo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Neyrinck_M/0/1/0/all/0/1">Mark C. Neyrinck</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Silk_J/0/1/0/all/0/1">Joseph Silk</a> We propose the Cosmic Web Detachment (CWD) model, a framework to interpret the star-formation history of galaxies in a cosmological context. The CWD model unifies several starvation mechanisms known to disrupt or stop star formation into one single physical framework. Galaxies begin accreting star-forming gas at early times via a network of primordial filaments, simply related to the pattern of density fluctuations in the initial conditions. But when streams cross on intergalactic scales, this pattern is disrupted, and the galaxy textit{detaches} from its primordial filaments,Read More →

Discovery of an Enormous Ly$alpha$ nebula in a massive galaxy overdensity at $z=2.3$. (arXiv:1609.04021v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Cai_Z/0/1/0/all/0/1">Zheng Cai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fan_X/0/1/0/all/0/1">Xiaohui Fan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yang_Y/0/1/0/all/0/1">Yujin Yang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bian_F/0/1/0/all/0/1">Fuyan Bian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prochaska_J/0/1/0/all/0/1">J. Xavier Prochaska</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zabludoff_A/0/1/0/all/0/1">Ann Zabludoff</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McGreer_I/0/1/0/all/0/1">Ian McGreer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zheng_Z/0/1/0/all/0/1">Zhenya Zheng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Green_R/0/1/0/all/0/1">Richard Green</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cantalupo_S/0/1/0/all/0/1">Sebastiano Cantalupo</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:+Hamden_E/0/1/0/all/0/1">Erika Hamden</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jiang_L/0/1/0/all/0/1">Linhua Jiang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kashikawa_N/0/1/0/all/0/1">Nobunari Kashikawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_R/0/1/0/all/0/1">Ran Wang</a> Enormous Ly$alpha$ Nebulae (ELANe), unique tracers of galaxy density peaks, are predicted to lie at the nodes and intersections of cosmic filamentary structures. Previous successful searches for ELANe have focused on wide-field narrowband surveys, or have targeted known sources such as ultraluminous quasi-stellar-objectsRead More →