• No results found

The build-up of massive galaxies Damen, M.C.

N/A
N/A
Protected

Academic year: 2021

Share "The build-up of massive galaxies Damen, M.C."

Copied!
9
0
0

Bezig met laden.... (Bekijk nu de volledige tekst)

Hele tekst

(1)

Citation

Damen, M. C. (2010, June 22). The build-up of massive galaxies. Retrieved from https://hdl.handle.net/1887/15720

Version: Corrected Publisher’s Version

License: Licence agreement concerning inclusion of doctoral thesis in the Institutional Repository of the University of Leiden

Downloaded from: https://hdl.handle.net/1887/15720

Note: To cite this publication please use the final published version (if

applicable).

(2)

The build-up

of

massive galaxies

(3)
(4)

The build-up

of

massive galaxies

Proefschrift

ter verkrijging van

de graad van Doctor aan de Universiteit Leiden, op gezag van de Rector Magnificus prof. mr. P. F. van der

Heijden,

volgens besluit van het College voor Promoties te verdedigen op dinsdag 22 juni 2010

klokke 15.00 uur

door

Maria Catharina Damen geboren te Delft

in 1980

(5)
(6)

Voor Bas.

(7)
(8)

vii

Table of contents

Chapter 1. Introduction 1

1.1 Extragalactic Astronomy . . . 1

1.2 The Distant Universe . . . 2

1.3 Galaxy Design . . . 6

1.3.1 A Standard Model . . . 6

1.3.2 Semi-Analytic Models . . . 7

1.4 Outlook . . . 7

1.5 Thesis Summary . . . 8

Chapter 2. The SIMPLE survey 11 2.1 Introduction . . . 12

2.2 Observations . . . 14

2.3 Data Reduction . . . 16

2.3.1 Post-Processing of the BCD Frames . . . 17

2.3.2 Image Combination and Mosaicking . . . 21

2.3.3 Flux Calibration . . . 23

2.3.4 Additional Data Products . . . 23

2.3.5 Final Images . . . 24

2.4 Additional Data . . . 25

2.4.1 TheU − K Data . . . . 25

2.4.2 The MIPS 24μm Data . . . . 25

2.5 Source Detection and Photometry . . . 27

2.5.1 Detection . . . 27

2.5.2 Photometry . . . 27

2.5.3 Background and Limiting Depths . . . 30

2.5.4 Stars . . . 32

2.6 Derived Parameters . . . 32

2.6.1 Spectroscopic and Photometric Redshifts . . . 32

2.6.2 Star Formation Rates, Rest-frame Photometry and Stel- lar Masses . . . 35

2.7 Catalog Contents . . . 36

2.8 Comparison to Other Catalogs . . . 37

2.8.1 SIMPLE versus MUSYC . . . 37

2.8.2 SIMPLE versus FIREWORKS . . . 38

2.9 Summary . . . 41

(9)

3.6 Summary and Discussion . . . 60

Chapter 4. SIMPLE star formation in the E-CDFS 67 4.1 Introduction . . . 68

4.2 Data . . . 68

4.2.1 Observations and Sample Selection . . . 68

4.2.2 Spectroscopic and Photometric Redshifts . . . 70

4.2.3 Low-Redshift Sample . . . 70

4.3 Star Formation Rates, Mass and Completeness . . . 70

4.3.1 Inferring the SFRs from the 24μm Flux and UV Lumi- nosity . . . 70

4.3.2 Stellar Mass and Rest-Frame Colors . . . 71

4.3.3 Mass Completeness . . . 72

4.4 Star Formation Rates as a Function of Redshift . . . 72

4.5 Conclusions . . . 76

Chapter 5. Observations versus Simulations 83 5.1 Introduction . . . 84

5.2 Data . . . 85

5.2.1 Observations and Sample Selection . . . 85

5.2.2 Redshifts, masses and star formation rates . . . 85

5.2.3 Mass completeness . . . 87

5.3 The Evolution of the Specific Star Formation Rate . . . 87

5.4 Comparison with Model Predictions . . . 89

5.5 Discussion . . . 92

Nederlandse samenvatting 99

Curriculum Vitae 105

Nawoord 107

Referenties

GERELATEERDE DOCUMENTEN

Percentage of the mass growth as a function of time as expected by the abundance matching technique (black stars); as measured considering the combined contribution of SFR, mergers

The cyan cross marks the location of the UCHII (Walsh et al. b) Extinction map based on the JHK s colors of individual stars (see text). The SOFI point sources are color-coded

In summary, for each sample of galaxies, we create mock 3D-HST stacks based on three stellar population models ( BC03, FSPS10, FSPS-C3K ) with solar metallicity, Chabrier IMF, and

Evolution of the galactic interstellar medium for the fiducial simulation run that includes dissociating, ionizing, and supernova feedback (Run LW+EUV +SN), as viewed projected along

The ratio of hydrogen ionizing photons over the total ionizing photons versus the total amount of photons with E > 1 Ry, of models with SFR = 0.001 M  yr −1 and solar

When applying a rest-frame B-band limit (dark gray line), the sSFR-mass relation is recovered at high masses. At the low-mass end, the passive galaxies are not selected and the

Om te ontdekken hoe sterrenstelsels zijn gevormd en te weten te komen hoe ze zich daarna hebben ontwikkeld moeten we het verre heelal bestuderen.. Dankzij de eindigheid van

Pap, bedankt voor je nuchterheid, Martijn voor je intensieve en onvoorwaardelijke hulp met de omslag, Peter-Paul, voor het overnemen van het stokje. Jij bent nu de wetenschapper van