Morphological evolution of galaxies over the last 8 billion years [Elektronische Ressource] / vorgelegt von Maurilio Pannella

Pannella Maurilio

Sujets

• Astronomie

Informations

• Publié par: ludwig-maximilians-universitat_munchen
• Publié le: 01 janvier 2007
• Nombre de lectures: 31
• Langue: English
• Poids de l'ouvrage: 9 Mo

Extrait

Morphological evolution of
galaxies over the last 8 billion years
Maurilio Pannella
Mu¨nchen 2007Morphological evolution of
galaxies over the last 8 billion years
Maurilio Pannella
Dissertation
¨ ¨an der Fakultat fur Physik
der
Ludwig-Maximilians-Universita¨t Munc¨ hen
vorgelegt von Maurilio Pannella
aus Turin (Italien)
Munc¨ hen, den 1 August 2007Erstgutachter: Prof. Dr. Ralf Bender
Zweitgutachter: Prof. Dr. Hans Bohr¨ inger
Tag der mundl¨ ichen Pruf¨ ung: 18. September 2007Morphological evolution of
galaxies over the last 8 billion years
Maurilio Pannella“... benvenuto raggio di sole, avrai matite per giocare
e un bicchiere per bere forte, e un bicchiere per bere piano
un sorriso per difenderti
e un passaporto per andare via lontano ...
... benvenuto figlio di nessuno, benvenuto in questo paese.”
.Contents
Zusammenfassung (Summary in German) 5
Summary 9
1 Galaxy formation and evolution in the cosmological framework 13
1.1 The hierarchical Universe . . . . . . . . . . . . . . . . . . . . . . . . . . . 13
1.2 The formation and evolution of galaxies . . . . . . . . . . . . . . . . . . . 15
1.2.1 Morphological properties . . . . . . . . . . . . . . . . . . . . . . . 17
1.2.2 Star formation and colors . . . . . . . . . . . . . . . . . . . . . . . 21
1.2.3 The Cosmic Star Formation History and Mass assembly . . . . . . 21
1.2.4 The Environmental dependence of galaxy evolution . . . . . . . . . 24
1.3 This Thesis . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 26
2 Observing the coloured Universe: the large deep surveys 29
2.1 The FORS Deep Field . . . . . . . . . . . . . . . . . . . . . . . . . . . . 30
2.1.1 Source detection and multi–band photometry . . . . . . . . . . . . 30
2.1.2 Photometric redshifts in the FORS Deep Field . . . . . . . . . . . 32
2.2 The Great Observatories Origins Deep Survey South Field . . . . . . . . . 34
2.2.1 A Ks-band selected galaxy sample in GOODS-S . . . . . . . . . . 35
2.2.1.1 Source detection and multi-band photometry . . . . . . . 35
2.2.1.2 Photometric redshift . . . . . . . . . . . . . . . . . . . . 38
2.2.1.3 Source catalogue . . . . . . . . . . . . . . . . . . . . . . 44
2.2.1.4 Redshift distribution . . . . . . . . . . . . . . . . . . . . 47
2.3 The Cosmic Evolution Survey . . . . . . . . . . . . . . . . . . . . . . . . 49
2.3.1 A deep galaxy catalogue in the COSMOS field . . . . . . . . . . . 49
2.3.1.1 NIR imaging data: acquisition . . . . . . . . . . . . . . . 50
2.3.1.2 NIR imaging data: reduction, photometry and cataloging 51
2.3.1.3 The i-selected catalogues . . . . . . . . . . . . . . . . . 54
2.3.1.4 Spectroscopic redshifts . . . . . . . . . . . . . . . . . . 58
2.3.1.5 Photometric redshifts . . . . . . . . . . . . . . . . . . . 60
3 Morphological characterization of high redshift galaxies 65
1Contents
3.1 The Advanced Camera for Surveys on board the HST . . . . . . . . . . . . 65
3.2 The morphological analysis . . . . . . . . . . . . . . . . . . . . . . . . . . 68
3.2.1 GIM2D . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 68
3.2.2 PSF influence on the morphological parameters . . . . . . . . . . . 69
3.2.3 Results on the overlapping COSMOS ACS tiles . . . . . . . . . . . 69
3.2.4 Results on simulated objects . . . . . . . . . . . . . . . . . . . . . 70
3.2.5 GIM2D vs. GALFIT . . . . . . . . . . . . . . . . . . . . . . . . . 71
3.2.6 Parametric profile fitting versus visual classification . . . . . . . . . 73
4 Morphological evolution in FDF and GOODS-S 77
4.1 Introduction . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 78
4.2 Ground-based data, photo–z and M /L ratios . . . . . . . . . . . . . . . . . 79∗
4.3 HST imaging and the morphological analysis . . . . . . . . . . . . . . . . 80
4.4 Evolution of the morphological mass function, total mass density and SSFR 81
4.5 Conclusions . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 85
5 Bulges and disks in the last 8 Gyrs of the COSMOS 87
5.1 Ground-based data and photometric redshifts . . . . . . . . . . . . . . . . 90
5.2 Computing mass–to–light ratios . . . . . . . . . . . . . . . . . . . . . . . 91
5.3 HST Advanced Camera for Surveys imaging . . . . . . . . . . . . . . . . . 94
5.3.1 Sources extraction, star-galaxy classification and cataloging . . . . 95
5.4 The morphological analysis . . . . . . . . . . . . . . . . . . . . . . . . . . 95
5.5 The evolution of the morphological mass function and mass density . . . . 97
5.6 A hole in the sky at z∼0.5 . . . . . . . . . . . . . . . . . . . . . . . . . . . 100
5.7 The environmental effect on morphological evolution . . . . . . . . . . . . 101
5.7.1 8 Giga years of morphology density relation . . . . . . . . . . . . . 104
5.8 Red sequence and blue cloud up to redshift 1.15 . . . . . . . . . . . . . . . 104
5.9 The specific star formation rate in the last 8 Gyrs . . . . . . . . . . . . . . 106
5.10 The ages of early-type objects in different environments . . . . . . . . . . . 110
5.11 Discussion and conclusions . . . . . . . . . . . . . . . . . . . . . . . . . . 111
6 Further work 115
6.1 The dark side of star formation: chasing the dusty Universe . . . . . . . . . 116
6.1.1 The GOODS-S test . . . . . . . . . . . . . . . . . . . . . . . . . . 116
6.2 Field to Clusters variation . . . . . . . . . . . . . . . . . . . . . . . . . . . 118
6.2.1 Virial masses of cluster galaxies through scaling relations . . . . . 118
6.3 The UV morphology of high redshift star forming galaxies . . . . . . . . . 122
6.3.0.1 Analysis of the UV morphology of high redshift galaxies 123
6.3.0.2 Morphological properties and extinction curve . . . . . . 124
6.4 The star formation rate history . . . . . . . . . . . . . . . . . . . . . . . . 126
6.4.1 The Star Formation Rate . . . . . . . . . . . . . . . . . . . . . . . 127
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