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Environmental Effects on Galaxy Evolution in Nearby Clusters

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Environmental Effects on Galaxy Evolution in Nearby Clusters UNIVERSITA' DEGLI STUDI DI MILANO-BICOCCA Scuola di Dottorato di Scienze Corso di Dottorato di Ricerca in Fisica e Astronomia XVIII ciclo UNIVERSITE´ DE PROVENCE AIX-MARSEILLE I Ecole Doctorale "Physique et Sciences de la Mati`ere" Doctorat en Rayonnement et Plasmas A.A.2004-2005 ENVIRONMENTAL EFFECTS ON GALAXY EVOLUTION IN NEARBY CLUSTERS Coordinatore del Dottorato: Prof. Claudio Destri Directeur de l'Ecole´ Doctorale: Prof. Jean-Jacques Aubert Tutore: Prof. Giuseppe Gavazzi Directeur de th`ese: Dott. Alessandro Boselli Commissione-Jury: Dott. A. Boselli (Laboratoire d'Astrophysique de Marseille) Prof. V. Buat (Universit´e de Provence) Prof. G. Gavazzi (Universit`a di Milano - Bicocca) Prof. F. Haardt (Universit`a dell'Insubria) Rapporteurs: Prof. C. Balkowski (Observatoire Astronomique Paris-Meudon) Dott. B. Poggianti (Osservatorio Astronomico di Padova) Tesi di Dottorato di: Luca Cortese Matricola R00280 "Objectivity cannot be equated with mental blankness; rather, objectivity resides in recognizing your preferences and then subjecting them to especially harsh scrutiny ...and also in a willingness to revise or abandon your theories when the tests fail (as they usually do)." Stephen Jay Gould Acknowledgments This work represents the end point of my student career. After approximately twenty one years from my first entrance in a class room (it was September 1984 in Phoenix, AZ), I'm finally going to attend my last "school" examination. Therefore I want to seize this opportunity in order to briefly remember and to thank some of the friends met during this journey. First of all I must thank my advisor Peppo Gavazzi, my scientific father, for his precious guidance and his teachings especially at the beginning of my research carrier. Special thanks to Alessandro Boselli, my co-advisor, first of all for the the last year spent in Marseille: a splendid experience. Thanks also for all his helpful advices, comments and supports on this and other works during the last three years. Many people contributed, directly or indirectly, to this work, and I am grateful to all of them. Merci beaucoup to Samuel Boissier for all the interesting discussions and, above all, for his precious lessons of French. Thanks to Veronique Buat for his help during the year spent in Marseille and for having initiated me in the obscure secrets of dust. Thanks to Barry Madore for his hospitality at the Carnegie Observatories, for his kindness, support and, especially, for his help in improving my written English. Muchas gracias to Armando Gil de Paz for his precious help on making the GALEX data available to me: without his contribution a great part of this work would not have been possible. Many thanks to Bianca Poggianti for a careful reading of my thesis and for her useful comments and suggestions. I would like also to thank Monica Colpi for her scientific and, especially, financial support during these three years. Arigato to Tsutomu Takeuchi and Akio Inoue for useful discussions about dust and galaxy evolution, for their kindness and help during my stay in Marseille and for having introduced me to Japanese cuisine. Many friends made the last three years unique. At Milano University life wouldn't have been as much fun without all Peppo's students. In particular thanks to Ilaria, Lea and Paolo for their unique support and thanks also to Chri for having installed Linux on my laptop, making me able to write this work. In Marseille thanks a lot to all the "Caf´e du Coin": Helene, Claude, Kassem, Peter, Fabrice and the others. Thanks for all the coffees and cakes, and for having received me with open arms even if I wasn't able to speak French. Thanks to Alexie, Jean- v vi Baptiste, Hector who shared the office with me, and a special thanks to Celine for having borne my never ending phone calls with my advisors, for her kindness and for her precious help in understanding french bureaucracy. Life in Marseille would have been completely different without the volley matches with Raph, Patrick, Seb, Mika, Fabrice and all the others. Finally, nothing of this would have been possible without the constant support of my parents and my brother Claudio, who have always encouraged me to continue this beautiful adventure. This research was partly supported the Universit`a Italo-Francese through the Vinci Programme and by the CNES through GALEX-Marseille. Abstract The environmental effects on galaxy evolution in nearby clusters are investigated using a multiwavelength dataset. The present analysis is focused on the properties of three (Abell 1367, Virgo and Coma) among the best studied clusters in the local Universe. Due to the variety of their environmental conditions (e.g. spiral fraction, X-ray luminosity, evolutionary stage) they represent the most suitable "laboratory" for comparative studies. By combining for the first time GALEX UV observations with optical, near and far infrared data, the evolutionary history of cluster galaxies is studied. The main goals of this thesis are: (a) The study of the dependence of the UV emission of galaxies from their morphological type, mass and the environment they inhabit, through the study of UV luminosity functions and color magnitude relations. (b) The study of UV dust extinction properties of local cluster galaxies and investigation of possible empirical relations useful to estimate the amount of UV attenuation in local and high redshift galaxies. (c) Investigation of the effect of large scale structures assembling on galaxy evolution through the dynamical analysis of Abell 1367, one of the best examples of a dynamically young local cluster of galaxies. (d) The characterization of the effects of different environmental mechanisms (i.e. gravitation interactions, ram pressure, preprocessing) on the evolutionary history of cluster galaxies in order to gain more insight on the origin of the morphology-density and star-formation-density relations. The observational evidences presented in this work suggest that: (I) Giant ellipticals are an old, homogeneous population showing no or little evolution at least in the past 8 Gyr; unlike dwarf ellipticals which still contain young stellar populations. (II) The importance of different environmental mechanisms has changed during the age of the Universe. Tidal interactions and preprocessing probably dominated the past Universe and shaped part of the morphology-density relation during the phase of cluster accretion of small groups. Ram pressure dominates in today clusters and is surely affecting the star formation history of galaxies but with less influence on their morphology. (III) The heterogeneous class of S0s galaxies, from bulge dominated to the disky S0s, is not the result of a single transformation mechanism: if ram pressure is able to produce disk dominated S0s, tidal interactions (and thus preprocessing) are required to account for bulge dominated S0s. (VI) Different observational evidences vii viii confirm the presence of a correlation between the mean age of stellar populations and galaxy mass (downsizing effect). In the framework of the hierarchical model of galaxy formation, the origin of the downsizing effect remains unsolved. This clear observational evidences represents one of today's main challenge for models of galaxy evolution. Riassunto In questo lavoro vengono analizzati gli effetti dell'ambiente sull'evoluzione delle galassie, utilizzando una base di dati multi-lunghezza d'onda. In particolare tutta quest'analisi ´e focalizzata sullo studio di tre differenti ammassi di galassie dell'Universo Locale: Abell1367, Virgo, Coma. Questi tre ammassi sono tra i piu´ studiati nell'Universo locale e, date le loro differenti propriet´a (e.g. frazione di galassie a spirale, luminosit´a X, stadio evolutivo), rappresentano dei laboratori ideali per quantificare l’influenza dell'ambiente sull'evoluzione delle galassie. Combinando per la prima volta osser- vazioni ultraviolette del satellite GALEX a dati ottici, in vicino e lontano infrarosso viene ricostruita l'evoluzione delle galassie d'ammasso. I principali obiettivi di questa tesi sono: (a) Studiare il legame tra le propriet´a dell'emissione UV delle galassie, il loro tipo morfologico, la loro massa e l'ambiente in cui esse si trovano, attraverso l'analisi delle funzioni di luminosit´a UV e delle relazioni colore-magnitudine. (b) Comprendere le propriet´a delle polveri interstellari respon- sabili dell'assorbimento della radiazione ultravioletta e ricavare relazioni empiriche utili per poter quantificare l'assorbimento della radiazione ultravioletta in assenza di osservazioni in lontano infrarosso. (c) Analizzare se e come lo stato dinamico di un ammasso ´e in grado di influenzare la storia evolutiva delle galassie, attraverso lo studio dell'ammasso di Abell1367: uno dei migliori esempi di ammasso locale, dinami- camente ancora giovane. (d) Quantificare l’influenza di diversi effetti d'ambiente (i.e. interazioni gravitazionali, ram-pressure, galaxy preprocessing) sull'evoluzione delle galassie d'ammasso, in modo da comprendere le origini del fenomeno di segregazione morfologica. Tutte le evidenze osservative presentate e analizzate in questo lavoro suggeriscono che: (I) Le ellittiche giganti rappresentano una popolazione vecchia, omogenea che non ha subito una significativa evoluzione negli ultimi 8 Gyr; al contrario dell'ellittiche nane che sono ancora oggi dominate da popolazioni stellari giovani. (II) L’influenza dell'ambiente sull'evoluzione delle galassie cambia sensibilmente con l’et´a dell'Universo. Le interazioni gravitazionali ed il galaxy preprocessing sono stati gli effetti dominanti nell'Universo passato e sembrano essere i responsabili, almeno in parte, del fenomeno di segregazione morfologica. La ram pressure sembra essere dominante negli ammassi di oggi. Questo meccanismo ´e sicuramente in grado di influenzare la storia di for- ix x mazione stellare delle galassie, ma ha pochi effetti sulla loro morfologia. (III) Le galassie lenticolari (S0) risultano essere cos´ı il prodotto di processi completamente differenti: se oggi la ram pressure ´e in grado di trasformare una galassia a spirale in una lenticolare con piccolo bulge, sono necessarie interazioni gravitazionali per pro- durre i grandi bulge osservati in molte lenticolari nell'Universo locale.
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