• No results found

Interstellar medium conditions in starburst galaxies Beirão, M.P.L.

N/A
N/A
Protected

Academic year: 2021

Share "Interstellar medium conditions in starburst galaxies Beirão, M.P.L."

Copied!
9
0
0

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

Hele tekst

(1)

Interstellar medium conditions in starburst galaxies

Beirão, M.P.L.

Citation

Beirão, M. P. L. (2010, January 13). Interstellar medium conditions in starburst galaxies.

Retrieved from https://hdl.handle.net/1887/14559

Version: Not Applicable (or Unknown)

License: Leiden University Non-exclusive license Downloaded from: https://hdl.handle.net/1887/14559

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

(2)

Interstellar Medium Conditions in

Starburst Galaxies

(3)
(4)

Interstellar Medium Conditions in Starburst 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 woensdag 13 januari 2010

klokke 13.45 uur

door

Pedro Maria Lopes Beir˜ao

geboren te Lisboa in 1977

(5)

Promotiecommissie

Promotor: Prof. dr. F. P. Israel Co-promotor: Dr. B. R. Brandl

Overige leden: Prof. dr. E. van Dishoeck Prof. dr. V. Icke

Prof. dr. M. Spaans (Rijksuniversiteit Groningen) Dr. P. van der Werf

Dr. N. M. F ¨orster Schreiber (Max-Plack-Institut f ¨ur Extraterrestrische Physik) Dr. B. Groves

(6)

A Mem´oria do Meu Pai. `

(7)

Cover: The region surrounding the Super Star Cluster 30 Doradus in the Large Magel- lanic Cloud. A composite of infrared light captured by Spitzer Space Telescope, with wave- lengths of 3.6 (blue) and 8 (green) microns captured by the telescope’s infrared array camera, and 24-micron light (red) detected by the multiband imaging photometer. Credit: NASA/JPL- Caltech/M. Meixner (STScI) & the SAGE Legacy Team.

(8)

Table of contents vii

Table of contents

Page

Chapter 1. Introduction 1

1.1 Starburst Galaxies . . . 1

1.2 The ISM of starburst galaxies at infrared wavelengths . . . 2

1.2.1 Gas and Dust . . . 3

1.2.2 The phases of the ISM . . . 4

1.3 This thesis . . . 6

1.4 Outlook . . . 10

Chapter 2. Spatially Resolved Spitzer Spectroscopy of the Starburst Nucleus in NGC 5253 13 2.1 Introduction . . . 14

2.2 Observations and data reduction . . . 15

2.3 Discussion . . . 16

2.3.1 Spectral properties . . . 16

2.3.2 PAH ratio maps . . . 18

2.3.3 Gradients in the radiation field . . . 20

2.3.4 Dependence of PAH strength on the radiation field . . . 21

2.3.5 [OIV] line emission . . . 23

2.3.6 Conclusions . . . 23

Chapter 3. Spatially Resolved Spitzer-IRS Spectroscopy of the Central Region of M82 25 3.1 Introduction . . . 26

3.2 Observations and data reduction . . . 27

3.3 Analysis . . . 29

3.4 Results and discussion . . . 30

3.4.1 The morphology of the starburst region . . . 32

3.4.2 Origins of the variation of the radiation field . . . 34

3.4.3 Extinction . . . 37

3.4.4 Variations of PAH emission features . . . 39

3.4.5 Excitation of the warm H2 . . . 46

3.5 Conclusion . . . 46

Chapter 4. Powerful H2Emission and Star Formation on the Interacting Galaxy System Arp 143: Observations withSpitzer and GALEX 51 4.1 Introduction . . . 51

4.2 Observations and data reduction . . . 53

4.2.1 Spectra . . . 53

4.2.2 Images . . . 55

4.3 Analysis . . . 57

4.3.1 H2 lines . . . 58

(9)

viii Table of contents

4.3.2 PAH features . . . 60

4.3.3 Ionic lines . . . 60

4.3.4 High resolution spectrum of the nucleus . . . 61

4.3.5 Photometry . . . 62

4.4 Results . . . 62

4.4.1 Morphology . . . 62

4.4.2 The shock front . . . 64

4.4.3 The properties of gas and PAHs in the knots . . . 66

4.4.4 The ages of the knots . . . 67

4.4.5 Star rormation rates . . . 69

4.5 The role of shocks in the propagation of star formation . . . 71

4.5.1 The evolution of PAH emission with cluster age . . . 71

4.5.2 The H2emission front and the simultaneity of knot formation . . . 72

4.6 Conclusions . . . 73

Chapter 5. Simple models for the SEDs of Star Forming Galaxies 79 5.1 Introduction . . . 79

5.2 Galaxy Sample and SEDs . . . 80

5.3 Analysis . . . 82

5.3.1 Colors . . . 82

5.3.2 Dust SED Model Fits . . . 86

5.3.3 Single dust-component fits . . . 87

5.3.4 Two dust components with free β . . . 89

5.3.5 Two dust components with fixed β . . . 92

5.3.6 The DBP90 model . . . 99

5.3.7 The variation of dust properties with the ISRF . . . 103

5.4 Discussion . . . 105

5.4.1 Correlations . . . 105

5.4.2 Very cold dust . . . 107

5.5 Summary and conclusions . . . 109

Chapter Appendices 111

Bibliography 117

Color figures 129

Nederlandse samenvatting 135

Curriculum vitae 141

Nawoord 143

Referenties

GERELATEERDE DOCUMENTEN

It will also be possible to resolve Giant Molecular Clouds (GMC) and study their size and turbulence in galaxies out to distances of 100 Mpc, which allow us to study in the

We studied spatially resolved mid-infrared spectra of the dwarf galaxy NGC 5253, a galaxy with its infrared luminosity dominated by a single very young and massive stel- lar

The noise is negligible and the spectra exhibit the classical features of star- burst galaxies (Brandl et al. 2006), such as strong emission features of the PAHs, fine- structure

The overwhelming majority of the PAH emission comes from the nucleus, which is also the region with the most emission at 8µm (Fig. From the star forming ring, Knots A, C, E, and F

Previous observations from NVSS found a radio source with a flux-density of ∼ 5 mJy. Three possible explanations could account for this; i) there is a radio-loud AGN within the

Figuur 7.2 — Links: a) Een moleculaire wolk met daarin gebieden van grotere dichtheid (in zwart), de zogenaamde hete kernen. Het middelste plaatje b) laat zien hoe één van die

Een jaar voor het behalen van mijn VWO diploma aan het Gymnasium Felisum in Velsen-Zuid, heb ik in 1996 deelgenomen aan de zomerschool Astrofysica georgani- seerd door de

In order to develop a complete understanding of star-forming regions in star- burst galaxies, observations obtained with space telescopes as well as data from large scale,