Observational Constraints on The Evolution of Dust in ...

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114 Spitzer Survey of Protoplanetary Disk Dust in Serpens We have calculated SFRs 2 and L(TIR) for the five background galaxies contaminating this sample. These results can be found in Table A.1. L(TIR) ranges from a few times 10 11 to a few times 10 12 L ⊙ , indicating that these galaxies are typical so-called luminous infrared galaxies (LIRGs, L(TIR) > 10 11 L ⊙ ), while two are ultraluminous (ULIRGs, L(TIR) > 10 12 L ⊙ ). The latter are a class of heavily obscured galaxies having enormous instantaneous SFRs that are often associated with merging galaxies (Sanders & Mirabel 1996). These galaxies are very rare locally and become more common at high redshift. Their space density rises by about a factor of 10 from z = 0 to z ∼ 0.5 (Magnelli et al. 2009), consistent with the relatively high redshifts found (z ∼ 0.3 −0.5). Furthermore, due to its high SFR and the empirical correlation between the infrared and radio emission from starburst galaxies (Condon 1992), the ULIRG #12 at z = 0.46 can be identified with a previously unidentified radio source in the NRAO VLA Sky Survey (NVSS J182817+001604, Condon et al. 1998). The inferred SFRs range between 11 and 731 M ⊙ yr −1 , compared to a Milky Way SFR of about 3–5 M ⊙ yr −1 (Prantzos & Aubert 1995, and references therein). For further reference, the SFR of Serpens is 5.7×10 −5 M ⊙ yr −1 (Evans et al. 2009). Even though the star formation observed in those galaxies is due to high mass star-forming regions such as Orion, the high SFRs in the LIRGs and ULIRGs found are equivalent to 10 5 − 10 7 molecular clouds such as Serpens! A.3 High Ionization Object One of the objects, #17 (SSTc2dJ18282720+0044450), in this sample presents very strong emission lines that do not seem compatible with YSOs. Figure A.3 shows a blow-up of the spectrum, identifying the high ionization lines at z = 0. The source itself is highly reddened, being barely detected in IRAC1 (3.5 µm) but very prominent in MIPS1 (24 µm), with a 3–24 µm slope of 1.82. Two types of galactic objects show such high excitation lines: dusty planetary nebulae and supernova remnants. The IRS spectrum of this object (#17) resembles those of shocked ejecta of supernova remnants, as in Sandstrom et al. (2009) and Ghavamian et al. (2009) and that of planetary nebulae such as LMC 78, shown in Bernard-Salas et al. (2009). The spectrum also shows PAH emission at 6.2, 7.7, 11.2, and 12.8 µm. Optical and near-IR spectra are necessary to confirm the nature of this object. 2 The SFRs correspond to an IMF according to Chabrier (2003).
A. Background Sources 115 Figure A.3 – IRS spectra of the planetary nebula candidate (#17) found among this sample, presenting high ionization lines. Table A.1 – Characteristics of the Background Galaxies No. z 24µm (Jy) SFR (M ⊙ yr −1 ) L(TIR) (L ⊙ ) Type 11 0.1051 0.01800 16 1.5×10 11 LIRG 12 a 0.4637 0.00893 731 4.8×10 12 ULIRG 33 0.2742 0.01490 217 1.6×10 12 ULIRG 68 0.2032 0.00909 47 4.0×10 11 LIRG 128 0.1164 0.01010 11 1.1×10 11 LIRG a NVSS J182817+001604.
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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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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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199 parameter is. Na 6 tot 8 miljoe
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209 interagem gravitacionalmente, a
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220 Thesis Acknowledgments Liesbeth
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