An Orbital Study of Intense Ram-Pressure Stripping in Clusters
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Ram Pressure Stripping and Galaxy Orbits: the Case of the Virgo Cluster
Ram pressure stripping and galaxy orbits: The case of the Virgo cluster B. Vollmer Max-Planck-Institut f¨ur Radioastronomie, Bonn, Germany and Observatoire de Paris, Meudon, France. V. Cayatte, C. Balkowski Observatoire de Paris, DAEC, UMR 8631, CNRS et Universit´e Paris 7, F-92195 Meudon Cedex, France. and W.J. Duschl1 Institut f¨ur Theoretische Astrophysik der Universit¨at Heidelberg, Tiergartenstraße 15, D-69121 Heidelberg, Germany. ABSTRACT We investigate the role of ram pressure stripping in the Virgo cluster using N-body simulations. Radial orbits within the Virgo cluster’s gravitational potential are modeled and analyzed with respect to ram pressure stripping. The N-body model consists of 10 000 gas cloud complexes which can have inelastic collisions. Ram pressure is modeled as an additional acceleration on the clouds located at the surface of the gas distribution in the direction of the galaxy’s motion within the cluster. We made several simulations changing the orbital parameters in order to recover different stripping scenarios using realistic temporal ram pressure profiles. We investigate systematically the influence of the inclination angle between the disk and the orbital plane of the galaxy on the gas dynamics. We show that ram pressure can lead to a temporary increase of the central gas surface density. In some cases a considerable part of the total atomic gas mass (several 108 M ) can fall back onto the galactic disk after the stripping event. A quantitative relation between the orbit parameters and the resulting Hi deficiency is derived containing explicitly the inclination angle between the disk and the orbital plane. -
Self-Consistent Nebular Emission and Stellar Population Analysis of Jellyfish Galaxies
UNIVERSIDADE FEDERAL DO RIO GRANDE DO SUL INSTITUTO DE F´ISICA DEPARTAMENTO DE ASTRONOMIA Self-consistent nebular emission and stellar population analysis of jellyfish galaxies Gabriel Maciel Azevedo Trabalho de Conclus~ao de Curso ap- resentado `aComi¸c~aode Gradua¸c~aoem F´ısica do Instituto de F´ısica da Univer- sidade Federal do Rio Grande do Sul sob orienta¸c~aoda Prof. Dr. Ana Leonor Chies Santiago Santos e do Prof. Dr. Rog´erio Riffel, como parte dos requisitos para a obten¸c~aodo grau de Bacharel em F´ısica- ^enfaseem Astrof´ısica. Porto Alegre, RS, Brasil May, 2021 \As flores brotam e morrem, as estrelas brilham, mas um dia se apagar~ao.Tudo morre, a Terra, o Sol, a Via L´actea, e at´emesmo todo esse universo n~ao´e exce¸c~ao.. Comparado a isso, a vida do homem ´et~aobreve e fugidia quanto um piscar de olhos. Nesse curto instante, os homens nascem, riem, choram, lutam, sofrem, festejam, lamentam, odeiam pessoas e amam outras. Tudo ´etransit´orio,e em seguida todos caem no sono eterno chamado morte." Masami Kurumada (Shaka, Cavaleiros do Zod´ıaco,ep 124) Agradecimentos Agrade¸co`aminha fam´ıliapor todo apoio e carinho ao longo desses anos, e em especial aos meus pais por sempre terem me incentivado a me dedicar aos estudos e continuamente trabalhado para me prover educa¸c~aode qualidade. Agrade¸co`aminha namorada Caroline, por ter me acompanhado, me divertido e me ajudado durante esses ´ultimossemestres de gradua¸c~ao. Agrade¸coaos meus amigos antigos por alegrarem meus dias ao longo de tantos anos, e em especial ao Eduardo, que me incentivou a seguir com minha escolha de profiss˜ao. -
Interaction Between Radio Plasma and Hot Gas in Galaxy Clusters
Ph.D. Student: Alessandro Ignesti Ph.D. Cycle: XXXIII Supervisors: Prof.ssa M. Gitti (DIFA), Dr. G. Brunetti (IRA INAF) Interaction between radio plasma and hot gas in galaxy clusters The presence of diffuse radio emission at the center of relaxed galaxy clusters, in the form of the so-called radio mini-halos, reveals that the intra-cluster medium (ICM) is permeated by relativistic particles and magnetic field. However, it is still unclear how relativistic electrons are diffused in the ICM. Another open question is if the central AGN plays a role in the origin of mini halos. In the first two years, we focused on the study of the spatial correlation between radio and X-ray surface brightness for a sample of relaxed clusters. Studying how the radio emission, which traces the ICM non-thermal components, is distributed with respect to the X- ray emission, which is instead a proxy of the thermal ICM density, can give us important insights into the origin of these radio sources. We observed that the distribution of the radio emission is more peaked than the one of the thermal plasma, which suggests that the relativistic particles are generated at the center of the cluster. This is also different from what is observed for giant radio halos in disturbed clusters, thus suggesting that these diffuse radio sources may be intrinsically different. Based on our results, we explored a scenario where the relativistic, radio-emitting electrons are produced by collisions between thermal ICM protons and relativistic protons injected by the central AGN. We found that the AGN cosmic ray luminosity required to power the radio emission (1044-46 erg s-1) is in agreement with the observations and, contrary to the case of giant radio halos, the expected γ-ray emission produced by the particle collisions does not violate the upper limits provided by the Fermi-LAT observatory. -
Jellyfish Galaxies with the Illustristng Simulations: I
Jellyfish galaxies with the IllustrisTNG simulations: I. Gas-stripping phenomena in the full cosmological context The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation Yun, Kiyun et al. "Jellyfish galaxies with the IllustrisTNG simulations: I. Gas-stripping phenomena in the full cosmological context." Monthly Notices of the Royal Astronomical Society 483, 1 (February 2019): 1042-1066 © 2018 The Author(s) As Published http://dx.doi.org/10.1093/MNRAS/STY3156 Publisher Oxford University Press (OUP) Version Author's final manuscript Citable link https://hdl.handle.net/1721.1/121269 Terms of Use Creative Commons Attribution-Noncommercial-Share Alike Detailed Terms http://creativecommons.org/licenses/by-nc-sa/4.0/ MNRAS 000,1–22 (2018) Preprint 27 November 2018 Compiled using MNRAS LATEX style file v3.0 Jellyfish galaxies with the IllustrisTNG simulations: I. Gas-stripping phenomena in the full cosmological context Kiyun Yun,1? Annalisa Pillepich,1 Elad Zinger,1 Dylan Nelson,2 Martina Donnari,1 Gandhali Joshi,1 Vicente Rodriguez-Gomez,3 Shy Genel,4;5 Rainer Weinberger,6 Mark Vogelsberger7 and Lars Hernquist6 1Max-Planck-Institut fur¨ Astronomie, Konigstuhl¨ 17, D-69117 Heidelberg, Germany 2Max-Planck-Institut fur¨ Astrophysik, Karl-Schwarzschild-Str. 1, D-85741 Garching, Germany 3Department of Physics & Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218, USA 4Center for Computational Astrophysics, Flatiron Institute, 162 Fifth Avenue, New York, NY 10010, USA 5Columbia Astrophysics Laboratory, Columbia University, 550 West 120th Street, New York, NY 10027, USA 6Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA 7Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA Accepted XXX. -
Annual Report ESO Staff Papers 2018
ESO Staff Publications (2018) Peer-reviewed publications by ESO scientists The ESO Library maintains the ESO Telescope Bibliography (telbib) and is responsible for providing paper-based statistics. Publications in refereed journals based on ESO data (2018) can be retrieved through telbib: ESO data papers 2018. Access to the database for the years 1996 to present as well as an overview of publication statistics are available via http://telbib.eso.org and from the "Basic ESO Publication Statistics" document. Papers that use data from non-ESO telescopes or observations obtained with hosted telescopes are not included. The list below includes papers that are (co-)authored by ESO authors, with or without use of ESO data. It is ordered alphabetically by first ESO-affiliated author. Gravity Collaboration, Abuter, R., Amorim, A., Bauböck, M., Shajib, A.J., Treu, T. & Agnello, A., 2018, Improving time- Berger, J.P., Bonnet, H., Brandner, W., Clénet, Y., delay cosmography with spatially resolved kinematics, Coudé Du Foresto, V., de Zeeuw, P.T., et al. , 2018, MNRAS, 473, 210 [ADS] Detection of orbital motions near the last stable circular Treu, T., Agnello, A., Baumer, M.A., Birrer, S., Buckley-Geer, orbit of the massive black hole SgrA*, A&A, 618, L10 E.J., Courbin, F., Kim, Y.J., Lin, H., Marshall, P.J., Nord, [ADS] B., et al. , 2018, The STRong lensing Insights into the Gravity Collaboration, Abuter, R., Amorim, A., Anugu, N., Dark Energy Survey (STRIDES) 2016 follow-up Bauböck, M., Benisty, M., Berger, J.P., Blind, N., campaign - I. Overview and classification of candidates Bonnet, H., Brandner, W., et al. -
OMEGA–OSIRIS Mapping of Emission-Line Galaxies in A901/2–V. the Rich
MNRAS 484, 892–905 (2019) doi:10.1093/mnras/stz007 Advance Access publication 2019 January 5 OMEGA–OSIRIS mapping of emission-line galaxies in A901/2–V. The rich population of jellyfish galaxies in the multicluster system Abell 901/2 Downloaded from https://academic.oup.com/mnras/article-abstract/484/1/892/5274139 by Universidade Federal do Rio Grande Sul user on 22 May 2019 Fernanda V. Roman-Oliveira ,1‹ Ana L. Chies-Santos ,1 Bruno Rodr´ıguez del Pino,2 A. Aragon-Salamanca´ ,3 Meghan E. Gray3 and Steven P. Bamford3 1Departamento de Astronomia, Instituto de F´ısica, Universidade Federal do Rio Grande do Sul, Porto Alegre, RS 91509-900, Brazil 2Centro de Astrobiolog´ıa, CSIC-INTA, Torrejon´ de Ardoz, E-28850 Madrid, Spain 3School of Physics and Astronomy, The University of Nottingham, University Park, Nottingham NG7 2RD, UK Accepted 2018 December 10. Received 2018 November 23; in original form 2018 October 12 ABSTRACT We present the results of a systematic search and characterization of galaxies with morphologi- cal signatures of ram pressure stripping, known as jellyfish galaxies, in the multicluster system A901/2, at z ∼ 0.165, as part of the OMEGA survey. By visually inspecting Advanced Camera for Surveys/Hubble Space Telescope F606W images looking for morphological signatures of ram pressure stripping events in H α-emitting galaxies, we identify a total of 70 jellyfish candidates. Of these, 53 are clearly star-forming galaxies and five are highly probable active galactic nucleus (AGN) hosts, the classification of the remaining galaxies is more uncertain. They have late-type and irregular morphologies, and most of them are part of the blue cloud with only. -
Ram Pressure Stripping of the Multiphase ISM and Star Formation in the Virgo Spiral Galaxy NGC 4330
A&A 537, A143 (2012) Astronomy DOI: 10.1051/0004-6361/201117680 & c ESO 2012 Astrophysics Ram pressure stripping of the multiphase ISM and star formation in the Virgo spiral galaxy NGC 4330 B. Vollmer1,M.Soida2, J. Braine3,A.Abramson4, R. Beck5, A. Chung6,H.H.Crowl7, J. D. P. Kenney4, and J. H. van Gorkom7 1 CDS, Observatoire astronomique de Strasbourg, UMR 7550, 11 rue de l’université, 67000 Strasbourg, France e-mail: [email protected] 2 Astronomical Observatory, Jagiellonian University, Kraków, Poland 3 Laboratoire d’Astrophysique de Bordeaux, Université de Bordeaux, OASU, CNRS/INSU, 33271 Floirac, France 4 Yale University Astronomy Department, PO Box 208101, New Haven, CT 06520-8101, USA 5 Max-Planck-Insitut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany 6 Department of Astronomy and Space Science, Yonsei University, Republic of Korea 7 Department of Astronomy, Columbia University, 538 West 120th Street, New York, NY 10027, USA Received 11 July 2011 / Accepted 11 November 2011 ABSTRACT It has been shown that the Virgo spiral galaxy NGC 4330 shows signs of ongoing ram pressure stripping at multiple wavelengths. At the leading edge of the interaction, the Hα and dust extinction curve sharply out of the disk. On the trailing side, a long Hα/UV tail has been found which is located upwind of a long Hi tail. We complement the multiwavelength study with IRAM 30m HERA CO(2–1) and VLA 6 cm radio continuum observations of NGC 4330. The data are interpreted with the help of a dynamical model including ram pressure and, for the first time, star formation. -
Small Near-Earth Asteroids As a Source of Meteorites
Small Near-Earth Asteroids as a Source of Meteorites Jiří Borovička and Pavel Spurný Astronomical Institute of the Czech Academy of Sciences Peter Brown University of Western Ontario __________________________________________________________________________ Small asteroids intersecting Earth’s orbit can deliver extraterrestrial rocks to the Earth, called meteorites. This process is accompanied by a luminous phenomena in the atmosphere, called bolides or fireballs. Observations of bolides provide pre-atmospheric orbits of meteorites, physical and chemical properties of small asteroids, and the flux (i.e. frequency of impacts) of bodies at the Earth in the centimeter to decameter size range. In this chapter we explain the processes occurring during the penetration of cosmic bodies through the atmosphere and review the methods of bolide observations. We compile available data on the fireballs associated with 22 instrumentally observed meteorite falls. Among them are the heterogeneous falls Almahata Sitta (2008 TC3) and Benešov, which revolutionized our view on the structure and composition of small asteroids, the Příbram-Neuschwanstein orbital pair, carbonaceous chondrite meteorites with orbits on the asteroid-comet boundary, and the Chelyabinsk fall, which produced a damaging blast wave. While most meteoroids disrupt into fragments during atmospheric flight, the Carancas meteoroid remained nearly intact and caused a crater-forming explosion on the ground. 1. INTRODUCTION Well before the first asteroid was discovered, people unknowingly had asteroid samples in their hands. Could stones fall from the sky? For many centuries, the official answer was: NO. Only at the end of the 18th century and the beginning of the 19th century did the evidence that rocks did fall from the sky become so overwhelming that this fact was accepted by the scientific community. -
Dynamics of the Polonnaruwa Meteorite Fall
EPSC Abstracts Vol. 8, EPSC2013-803, 2013 European Planetary Science Congress 2013 EEuropeaPn PlanetarSy Science CCongress c Author(s) 2013 Dynamics of the Polonnaruwa meteorite fall S. G. Coulson (1), M. K. Wallis (1), N. Miyake (1), J. Wallis (2), N. C. Wickramasinghe (1) (1) Buckingham Centre for Astrobiology, The University of Buckingham, Buckingham MK18 1EG, UK (2) School of Mathematics, Cardiff University, Cardiff,UK ([email protected] ) Abstract 1. Introduction The Polonnaruwa meteorite fell over the north east of Disintegration of meteoroids descending through the Sri Lanka on 29 Dec. 2012, with the fireball observed atmosphere is usually described by a process of descending at 18.30 local time. Fragments were continual ablation where the energy absorbed in picked up the following day from paddy fields, sized heating the bolide is proportional to the cube of its 3 from 10-15cm down to few mm. Meteorite speed (u ) [1] or by catastrophic fragmentation when fragments were readily identifiable on top of the the ram pressure (µ u2) exceeds the tensile strength sandy soil and scattered over an area of 1 km scale. of the body [2]. Both these models predict that ~ 1m The meteorites are unusually fragile and porous, with radii, low density meteoroids such reach a minimum mean density less than water. A thin fusion crust is altitude of 30-20 km. From analysis of a Leonid found around some cm-sized pieces. From their meteoroid, Coulson [3] suggested that ~90% of the spatial distribution, we infer the meteoroid survived initial mass of cometary fragments are a composite of to an unusually low altitude ~10km. -
Modelling of Bingham and Herschel-Bulkley Flows with Mixed
Journal of Non-Newtonian Fluid Mechanics 228 (2016) 1–16 Contents lists available at ScienceDirect Journal of Non-Newtonian Fluid Mechanics journal homepage: www.elsevier.com/locate/jnnfm Modelling of Bingham and Herschel–Bulkley flows with mixed P1/P1 finite elements stabilized with orthogonal subgrid scale Elvira Moreno a, Antonia Larese b,∗, Miguel Cervera b a Departamento de Ordenación de Cuencas, Ingeniería Forestal, Universidad de los Andes, ULA, Vía Chorros de Milla, 5101, Mérida Venezuela b International Center for Numerical Methods in Engineering (CIMNE), Technical University of Catalonia (UPC), Edificio C1, Campus Norte, Jordi Girona1-3, 08034, Barcelona Spain article info abstract Article history: This paper presents the application of a stabilized mixed pressure/velocity finite element formulation to Received 3 August 2015 the solution of viscoplastic non-Newtonian flows. Both Bingham and Herschel–Bulkley models are con- Revised 27 November 2015 sidered. Accepted 12 December 2015 Available online 19 December 2015 The detail of the discretization procedure is presented and the Orthogonal Subgrid Scale (OSS) stabiliza- tion technique is introduced to allow for the use of equal order interpolations in a consistent way. The Keywords: matrix form of the problem is given. Bingham flows Herschel–Bulkley flows A series of examples is presented to assess the accuracy of the method by comparison with the results Variational multiscale stabilization obtained by other authors. The extrusion in a Bingham fluid and the movement of a moving and rotating Orthogonal subscale stabilization cylinder are analyzed in detail. The evolution of the streamlines, the yielded and unyielded regions, the Moving cylinder drag and lift forces are presented. -
Dust Streamers in the Virgo Galaxy M86 from Ram Pressure Stripping
Astronomical Journal, August 2000, in press Dust Streamers in the Virgo Galaxy M86 from Ram Pressure Stripping of its Companion VCC 882 Debra Meloy Elmegreen1, Bruce G. Elmegreen2, Frederick R. Chromey1, Michael S. Fine1,3 ABSTRACT The giant elliptical galaxy M86 in Virgo has a ∼ 28 kpc long dust trail inside its optical halo that points toward the nucleated dwarf elliptical galaxy, VCC 882. The trail seems to be stripped material from the dwarf. Extinction measurements suggest that the ratio of the total gas mass in the trail to the blue luminosity of the dwarf is about unity, which is comparable to such ratios in dwarf irregular galaxies. The ram pressure experienced by the dwarf galaxy in the hot gaseous halo of M86 was comparable to the internal gravitational binding energy density of the presumed former gas disk in VCC 882. Published numerical models of this case are consistent with the overall trail-like morphology observed here. Three concentrations in the trail may be evidence for the predicted periodicity of the mass loss. The evaporation time of the trail is comparable to the trail age obtained from the relative speed of the galaxies and the trail length. Thus the trail could be continuously formed from stripped replenished gas if the VCC 882 orbit is bound. However, the high gas mass and the low expected replenishment rate suggest that this is only the first stripping event. Implications for the origin of nucleated dwarf ellipticals arXiv:astro-ph/0005243v1 11 May 2000 are briefly discussed. Subject headings: galaxies: interactions — galaxies: individual (M86) — galaxies: kinematics and dynamics — galaxies: clusters 1Department of Physics and Astronomy, Vassar College, Poughkeepsie, NY 12604; e–mail: [email protected], [email protected] 2IBM Research Division, T.J. -
Commencement Program
Graduate School of Arts and Sciences Commencement Ceremony Yale University Sunday, May 23, 2021 Order of Exercises commencement ceremony Graduate School of Arts and Sciences Sunday, May 23, 2021 Academic Procession Peter Salovey Michelle Nearon University President Senior Associate Dean for Graduate Student Chris Argyris Professor of Psychology Development and Diversity Lynn Cooley Allegra di Bonaventura Dean, Graduate School of Arts and Sciences Associate Dean for Graduate Student Academic Vice Provost for Postdoctoral Afairs Support C.N.H Long Professor of Genetics, Professor of Cell Ann Gaylin Biology and Molecular, Cellular and Developmental Associate Dean for Graduate Education Biology Lisa Brandes Akiko Iwasaki Assistant Dean for Student Life Waldemar Von Zedtwitz Professor of Immunobiology and Molecular, Cellular and Developmental Biology, Danica Tisdale Fisher and Professor of Epidemiology Assistant Dean of Diversity Gary Brudvig Lucylle Armentano ’21 PhD in Psychology Benjamin Silliman Professor of Chemistry Student Marshal Kelly Shue Stephen Gaughran ’21 PhD in Ecology and Professor of Finance Evolutionary Biology Student Marshal Sharon Kugler University Chaplain Pamela Schirmeister Deputy Dean and Dean of Strategic Initiatives commencement ceremony Graduate School of Arts and Sciences Sunday, May 23, 2021 Greetings Lynn Cooley Dean, Graduate School of Arts and Sciences Vice Provost for Postdoctoral Afairs C.N.H Long Professor of Genetics, Professor of Cell Biology and Molecular, Cellular and Developmental Biology President’s