Observational Constraints on The Evolution of Dust in ...

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112 Spitzer Survey of Protoplanetary Disk Dust in Serpens Figure A.1 – IRS spectra of the background stars toward Serpens with the characteristic 10 µm silicate absorption feature and falling SED. In gray are the original spectra, while in black a binned version is overplotted. The object number is indicated at the top right of each panel. Besides these 18 objects, another 8 objects in this sample with falling mid-IR spectra show the 10 µm silicate feature in absorption (objects 19, 25, 37, 78, 95, 126 were not observed by Oliveira et al. 2009), leading to their classification as background stars. Alternatively, those eight objects could be highly extincted YSOs, with silicate features in absorption arising from such extinction. However, using the dense cloud dust properties, as in Section 4.3.3.5, an extinction of 10 mag would produce a τ 9.7 of only 0.14 (see also Chiar et al. 2007). Since these objects do have silicate features in absorption, it is understood that they have high extinction (considerably higher than what is found for the cloud at their location). Thus, it is unlikely that they are actually highly extincted cloud members. Our working assumption is that these are background objects. These 26 spectra are shown in Figure A.1.
A. Background Sources 113 Figure A.2 – IRS spectra of the background galaxies toward Serpens, shown in rest-frame wavelength. The dashed lines indicate the rest-frame PAH features at 6.2, 7.7, 8.6, 11.2, 12.8, and 16.4 µm. The object number and z are indicated in each panel. A.2 Background Galaxies Five of the sources with clear PAH features show wavelength shifts in their line positions compared with galactic sources. These features thus allow us to identify them as background galaxies in this sample. PAHs are common features in most nearby galaxies with ongoing or recent star formation (Smith et al. 2007), and some contamination by background galaxies is expected (Papovich et al. 2004). By identifying PAH features from their shape and pattern (Tielens 2008 and references therein), the observed wavelength (λ obs ) can be related to the rest-frame wavelength (λ rest ) of each feature through a redshift (z = λ obs λ rest − 1.0). Between 3 (#12) and 5 (#11 and 68) PAH features are identified in each spectrum, and the redshift of each line is calculated. For a given object, the z values derived from the various lines agree within 2% and the mean of these values is taken as the redshift for that source. These five redshifted galaxies can be seen, in rest-frame wavelength, in Figure A.2. Star-forming galaxies show strong correlations between the extinction-corrected Paschen α luminosity coming from H ii regions and the luminosity at 24 µm due to the emission of dust heated by hot, young stars. Rieke et al. (2009) obtained powerlaw fits to the relation between the star formation rate (SFR) and the observed 24 µm flux densities (f 24,obs ), parameterized with respect to z to take into account the fact that the rest-frame wavelengths sampled change with redshift (Equation 14 in their paper). In order to estimate the infrared luminosity (L(TIR)), we use their best-fit relations between the (rest) 24 µm luminosity, L(TIR) and SFR (Eqs. 11 and 25).
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Observational <str
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Promotiecommissie Promotor: Co-Prom
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Cover Artwork: Roderik Overzier
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viii Chapter 3. YSOs in the Lupus M
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x Publications 217 Acknowledgments
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2 Introduction planets may eventual
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4 Introduction Figure 1.1 - Illustr
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6 Introduction 1.3.1.1 Disk Observa
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8 Introduction 1.3.1.3 Processes Af
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10 Introduction of them (e.g., β P
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12 Introduction responsible for dis
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14 Introduction Figure 1.4 - Eviden
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16 Introduction stars (due to spect
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18 Introduction the potential to ch
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20 Introduction Gorti, U., Dullemon
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2 Optical Characterization of a New
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Evolution of Dust in Protoplanetary
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162 From Protoplanetary Disks to Pl
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164 From Protoplanetary Disks to Pl
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193 Figuur 1 - Het ontstaan van een
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195 kunnen worden om de verschillen
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197 Figuur 3 - Het planeetvormingsp
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199 parameter is. Na 6 tot 8 miljoe
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Resumo em Português Restrições O
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209 interagem gravitacionalmente, a
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216 Curriculum Vitæ omy Center (ES
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220 Thesis Acknowledgments Liesbeth
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