Observational Constraints on The Evolution of Dust in ...

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96 Spitzer Survey of Protoplanetary Disk Dust in Serpens Figure 4.12 – Clusters and groups in Serpens as defined according to the criteria in Jørgensen et al. (2008). The volume density contours are overlaid on the Serpens extinction map (Evans et al. 2007). The red dots are the YSOs in Serpens from Harvey et al. (2007b). Black contours indicate volume densities of 0.125, 0.25, 0.5, 2.0 and 4.0 M ⊙ pc −3 , gray contour corresponds to volume density of 1 M ⊙ pc −3 and white contours to a volume density of 25 M ⊙ pc −3 . (A color version of this figure is available in the online journal)
Evolution of Dust in Protoplanetary Disks 97 Figure 4.13 – Comparison between the clustered (dot-dashed black line) and field populations (solid dark gray line) of Serpens, with data from the c2d IRS program (dashed light gray line, Olofsson et al. 2009). In the left panel, the flux ratio between 30 and 13 µm (F 30 /F 13 ) is an indication of the disk geometry. The middle and right panels show the strength of the silicate features at 10 and 20 µm, respectively. (A color version of this figure is available in the online journal) IRS spectra. In the left panel, the flux ratio between 30 and 13 µm (F 30 /F 13 ) is an indication of disk geometry. The middle and right panels show the peak intensity of the silicate features at 10 and 20 µm, respectively. For all three quantities, the two populations (cluster and field) are statistically indistinguishable. A two sample Kolmogorov–Smirnov test (KS test) was performed for each quantity and the results show that the null hypothesis that the two distributions come from the same parent population cannot be rejected to any significance (18%, 13%, and 79% for F 30 /F 13 , S 10µm peak , and S20µm peak , respectively). Differences between the cluster versus field populations will be further investigated with ancillary data (e.g., relative stellar ages and masses) and modeling (e.g., disk sizes). However, the IRS spectra allow the conclusion that no significant differences are found for disk geometry or the grain size distribution in the upper layers of circumstellar disks in clustered compared with field stars. The latter result only applies to the inner disk, as traced by silicate features. The outer disk may still be different between cluster and field populations. 4.4.2 Comparison with Other Samples The young stars with disks observed by the c2d team with IRS spectroscopy (c2d IRS sample) are scattered across the sky in the five molecular clouds studied (Olofsson et al. 2009). The other four clouds studied by the c2d are Chamaeleon II, Lupus, Perseus and Ophiuchus. All clouds are nearby (within 300 pc), span a range of star-formation activity, have typical median ages of a few Myr and have a spread between more (Perseus and Ophiuchus) and less (Cha II and Lupus) clustered YSO populations (Evans et al. 2009). The results from this sample are also compared to the results in Serpens in Figures 4.9 and 4.13. A conspicuous similarity is seen between the samples. Note that Olofsson et al. (2009) do not analyze the 20 µm silicate feature in this same manner and, therefore, S 20µm peak for the c2d IRS sample is missing from the right panel in Figure 4.13.
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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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193 Figuur 1 - Het ontstaan van een
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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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209 interagem gravitacionalmente, a
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216 Curriculum Vitæ omy Center (ES
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218 Publications 8. c2d Spitzer-IRS
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220 Thesis Acknowledgments Liesbeth
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