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The Structure and Dynamics of Clusters and the Hi Content of Spiral Galaxies

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The Structure and Dynamics of Clusters and the Hi Content of Spiral Galaxies UNIVERSITAT DE BARCELONA U UNIVERSITAT DE BARCELONA Departament d’Astronomia i Meteorologia B The structure and dynamics of clusters and the H i content of spiral galaxies Mem`oria presentada per Maria Teresa Sanchis Estruch per optar al grau de Doctora en F´ısica Barcelona, octubre de 2003 Programa de Doctorat d’Astronomia i Meteorologia Bienni 1998–2000 Mem`oria presentada per Maria Teresa Sanchis Estruch per optar al grau de Doctora en F´ısica Directors de tesi Dr. Eduard Salvador Sol´e Dr. Josep Maria Solanes Maj´ua Contents Resumdelatesi v 1 Introduction 1 1.1Motivationofthisthesis......................... 3 1.2Thisworkandrelatedpublications................... 5 2 Historical overview 9 2.1 H i observations in clusters of galaxies . 9 2.1.1 Earlywork............................. 9 2.1.2 TheVirgocluster......................... 11 2.1.3 Recent results . 13 2.2Dynamicalmodelsofclusters...................... 15 2.2.1 Infallmodels........................... 15 2.2.2 Structuralmodels......................... 19 3 The 3D structure of the Virgo cluster region from Tully-Fisher and H i data 23 3.1Introduction................................ 23 5 6CONTENTS 3.2Observationaldata............................ 24 3.2.1 Galaxyselection.......................... 24 3.2.2 Homogenization of the distances to individual galaxies . 26 3.2.3 The21-cmsample........................ 27 3.3 The diagnosis of H i deficiency...................... 30 3.3.1 Possible bias of H i deficiencyinthedistance.......... 31 3.4 The H i deficiencyinVirgo........................ 34 3.4.1 Radialpattern........................... 34 3.4.2 Correlation with recessional velocities . 38 3.5ThestructureoftheVirgoregion.................... 40 3.5.1 Spherical coordinates . 41 3.5.2 Cartesiancoordinates....................... 43 3.6Summaryandconclusions........................ 46 4 Dynamical model of the Virgo region 51 4.1Introduction................................ 51 4.2 The main H i deficiency enhancements of the Virgo cluster . 53 4.3TheTolman-Bondimodel........................ 55 4.4Infallmodelwithrebound........................ 57 4.5Modelpredictionsvs.observations.................... 59 4.6Summaryandconclusions........................ 63 5 Numerical approach to halos: implications for the Virgo cluster 67 CONTENTS 7 5.1Introduction................................ 67 5.2 N-bodysimulations............................ 68 5.3Halostructureinradialphasespace................... 68 5.4Maximumreboundradius........................ 70 5.5 Virial radius, mass and velocity of the Virgo cluster . 74 5.6 Point mass model versus N-bodysimulations.............. 76 5.7Summaryandconclusions........................ 77 6 The velocity field drawn by the Virgo cluster 79 6.1Introduction................................ 79 6.2 The inclusion of ellipticals into the Virgo galaxy sample . 80 6.3Pickingisolatedhalos........................... 81 6.4 Rescaling the simulations to the scales of the Virgo cluster . 84 6.5Velocity-distancerelation......................... 86 6.6 Tolman-Bondi estimates of the Virgo cluster mass and distance . 90 6.7Summaryandconclusions........................ 92 7 On the origin of H i deficiency in galaxies on the outskirts of the Virgo cluster 93 7.1Introduction................................ 93 7.2 H i-deficient galaxies in the outskirts of the Virgo cluster . 94 7.3Inaccuratedistances........................... 95 7.4Interactionswithinsmallgroups..................... 97 8CONTENTS 7.5Interactionsfromcompanionsormergers................100 7.6 Errors in H i deficiency..........................101 7.7Casebycaseanalysis...........................105 7.8Summaryandconclusions........................107 8 Inferring the kinematical properties of bound systems: the effects of non-sphericity, substructure and streaming motions 111 8.1Introduction................................111 8.2Thesimulateddarkmatterhalos....................113 8.3Velocitymomentsofdarkmatterparticles...............117 8.4Modelingofthevelocitymoments....................124 8.5Summaryandconclusions........................132 9 Summary and future perspectives 137 A Additional tables 143 B Radius, time and density of turnaround in a flat ΛCDM cosmology161 C Velocity moments of dark matter particles 165 Bibliography 171 Resum de la tesi: Estructura i din`amica dels c´umuls i el contingut d’H i de les gal`axies espirals 1. Introducci´o L’origen i evoluci´o de les gal`axies ha estat una q¨uesti´o a resoldre des de l’establiment de la seq¨u`encia de Hubble (Hubble 1926, 1927) i el posterior descobriment que les gal`axies de diferents tipus no estan homog`eniament distribu¨ıdes a l’espai, sin´oque es presenten segregades segons la seua morfologia (Hubble & Humason 1931; Abell 1958; Morgan 1961). A l’univers proper, les gal`axies de tipus primerenc (el·l´ıptiques i lenticulars) es troben fonamentalment en regions d’elevada densitat com ara els centres dels c´umuls, mentre que les gal`axies de tipus tardiu (espirals i irregulars) s´on caracter´ıstiques d’entorns poc densos. Nombrosos autors han estudiat aquesta segregaci´o morfol`ogica per tal d’esbrinar els par`ametres f´ısics que caracteritzen la distribuci´o inhomog`enia de les gal`axies de diferents tipus (Oemler 1974; Dressler 1980; Salvador-Sol´e, Sanrom`a, & Rdz. Jordana 1989; Whitmore & Gilmore 1991, entre d’altres). Aquests par`ametres f´ısics donen evid`encies sobre els processos invo- lucrats en la formaci´o i possible evoluci´o de les gal`axies, contribuint al debat entre els defensors de la idea que les gal`axies presenten morfologies diferents segons l’en- torn on es van formar (Sandage, Freeman, & Stokes 1970; Silk 1978; Bardeen et al. 1986; Dekel & Rees 1987; Evrard, Silk, & Szalay 1990) i aquells que proposen que les gal`axies evolucionen al llarg de la seq¨u`encia de Hubble. El paradigma evolutiu va rebre import`ancia pel descobriment de l’anomenat efecte Butcher-Oemler (Butc- 9 10 Resum de la tesi her & Oemler 1978, 1984): els c´umuls a gran despla¸cament cap al roig tenen una fracci´o de gal`axies blaves major que els c´umuls propers. M´es recentment, gr`acies a la nova generaci´o de telescopis d’alta resoluci´o, capa¸cos de distingir la morfologia de les gal`axies en c´umuls llunyans, hem obtingut una visi´om´es acurada d’aquest efecte: Conforme s’observa enrera en el temps, la fracci´o d’espirals en c´umuls aug- menta amb z en detriment de la de lenticulars, mentre que la fracci´od’el·l´ıptiques roman constant (Couch et al. 1994; Dressler et al. 1994; Wirth, Koo, & Kron 1994; Dressler et al. 1997; Oemler, Dressler, & Butcher 1997; Smail et al. 1997; Fasano et al. 2000). La formaci´o estelar tamb´e evoluciona, augmentant amb z (Poggianti et al. 1999; Balogh et al. 1999). Segons el paradigma actualment acceptat, les gal`axies el·l´ıptiques (i potser les lenticulars m´es brillants) es van formar abans de la virialit- zaci´odelsc´umuls rics i evolucionen passivament des d’aleshores (Ellis et al. 1997), mentre que una fracci´o important de lenticulars (aproximadament el 50%) ´es gene- rada a partir de la transformaci´o morfol`ogica de les espirals (Dressler et al. 1997). Diferents mecanismes han estat proposats per tal d’explicar aquesta evoluci´odeles gal`axies: escombrat del gas causat per interaccions directes gal`axia-gal`axia (Spitzer & Baade 1951), per la pressi´ocin`etica del medi intracumular (Gunn & Gott 1972), per viscositat o per conducci´ot`ermica (Cowie & Songaila 1977; Nulsen 1982), in- teraccions de marea o fins i tot fusions (Toomre 1972), interacci´o gravitat`oria (Byrd & Valtonen 1990; Valluri 1993) o assetjament gal`actic (Moore, Katz, & Lake 1996). En qualsevol cas, per tal d’entendre les propietats de les gal`axies ´es necessari estudiar la f´ısica de les interaccions gal`actiques amb el medi dins del context del paradigma jer`arquic de formaci´o gal`actica (White & Rees 1978) on les gal`axies es desenvolupen a dins d’halos de mat`eria fosca que creixen jer`arquicament des de petites a grans escales. Cole (1991), Lacey & Silk (1991) i White & Frenk (1991) van ser els primers en abordar models de formaci´o gal`actica dins d’aquest context general. Aquests treballs van donar pas als anomenats Models Semi-anal´ıtics, els quals segueixen el creixement dels halos de mat`eria fosca i utilitzen, al si d’aquests halos, receptes anal´ıtiques per descriure la complicada f´ısica dels barions (veure per ex. Kauffmann, White, & Guiderdoni 1993; Lacey et al. 1993; Somerville & Primack 1999; Hatton et al. 2003, per citar alguns treballs). Seguint l’esperit d’aquests models semi-anal´ıtics, el nostre grup de recerca, liderat pel Dr. Eduard Salvador- Sol´e, est`a desenvolupant un nou model de formaci´ojer`arquica i evoluci´o de gal`axies totalment anal´ıtic que incorpora aspectes fins ara nom´es parcialment inclosos als models semi-anal´ıtics existents, com ara una descripci´o consistent de l’estructura interna de gal`axies de diferents tipus, la inclusi´o de forats negres massius centrals i Resumdelatesi 11 de les principals interaccions entre gal`axies: truncament per marea, fricci´odin`amica, fusions i escombrat per pressi´ocin`etica del medi intracumular. Per tal de discernir entre les abundants teories d’evoluci´o gal`actica en c´umuls i contrastar les prediccions dels models de formaci´ojer`arquica de gal`axies ´es necessari realitzar observacions en diferents entorns dels par`ametres f´ısics que caracteritzen les gal`axies al llarg de la seq¨u`encia de Hubble (Roberts & Haynes 1994). Aquestes observacions en c´umuls propers han mostrat que
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