Observational Constraints on The Evolution of Dust in ...

More documents

Recommendations

Info

56 YSOs in the Lupus Molecular Clouds Figure 3.1 – Example of the classification method of SST-Lup3-1 with high resolution standards. The black curves represent the high resolution standard models and the gray curves the science spectrum. At the left of each standard its spectral type is indicated. The range of plausible spectral types is determined to be M4 - M8.5 the best match for the TiO bands. The method for the low resolution standards is somewhat different because that library is not normalized. First, the resolution of the science spectra is lowered to that of the standard (3.59Å). This is done by convolving the spectrum with a Gaussian profile. The comparison of the spectra with the low resolution standards then happens in two ways. One way consists of scaling the spectra to the standards by anchoring their fluxes at certain wavelengths (6500, 7020 and 7050 Å). An example is shown in Figure 3.2 (top left, top right and bottom left). In the alternative method a scale factor is determined by first dividing both spectra and then taking the mean of those values, ignoring extreme features (like Hα emission lines) in the process. This factor is then used to scale the original spectra to the standards (see bottom right panel of Figure 3.2). Both methods agree very well, producing four different plots for each spectral type within the determined range. The correct spectral type is again visually determined by the best match at the TiO bands. The typical uncertainty in the spectral classification is one sub-class. 3.4.2 Special Spectra Some spectra present special features besides the temperature sensitive ones used for spectral classification. These objects were inspected more closely and are differentiated in three special types of spectra: • Ten spectra show [He i] emission lines at 6677.6 and 7064.6 Å (objects # 7, 52, 76, 82, 83, 84, 85, 87, 91, 93 - see examples in Figure 3.3). All of these objects also show strong Hα in emission. Strongly accreting objects produce emission lines other than Hα, such as this line. It is concluded that these lines are a sign
Evolution of Dust in Protoplanetary Disks 57 Figure 3.2 – Example of the classification methods of SST-Lup3-1 with the low resolution standard of a M6 main sequence star. The first three panels show the first method where the spectra are anchored at different wavelengths (wavelength explicitly mentioned in each plot, and marked to guide the eye). The last panel shows the second method. In all plots, the model is shown in black and the science spectrum in gray. Figure 3.3 – Sample of spectra (#82 on left panel and #7 on right panel) with strong Hα (6562.8 Å), and He i (6677.6 and 7064.6 Å) emission lines. of accretion, as is Hα (see Section 3.7 for more information on this subject). • Four spectra (objects #50, 59, 78 and 88) show the [Nii] doublet at 6548.4 and 6583.4 Å and the [Sii] doublet at 6715.8 and 6729.8 Å (see examples in Figure 3.4). These lines are indicative of ionised gas. Par-Lup3-4 (#50) and Sz102 (#78) are related to Herbig-Haro (HH) objects HH600 and HH228 respectively (Wang & Henning 2009). They classified these objects to be HHs with the [Sii] doublet line at 6717/6731 Å. The two other objects that show similar spectra, SSTc2dJ160708.6-391407 (#59) and Sz133 (#88), are not yet classified
Page 1:
Observational <str
Page 4 and 5:
Promotiecommissie Promotor: Co-Prom
Page 6 and 7:
Cover Artwork: Roderik Overzier
Page 8 and 9:
viii Chapter 3. YSOs in the Lupus M
Page 10 and 11:
x Publications 217 Acknowledgments
Page 12 and 13:
2 Introduction planets may eventual
Page 14 and 15:
4 Introduction Figure 1.1 - Illustr
Page 16 and 17: 6 Introduction 1.3.1.1 Disk Observa
Page 18 and 19: 8 Introduction 1.3.1.3 Processes Af
Page 20 and 21: 10 Introduction of them (e.g., β P
Page 22 and 23: 12 Introduction responsible for dis
Page 24 and 25: 14 Introduction Figure 1.4 - Eviden
Page 26 and 27: 16 Introduction stars (due to spect
Page 28 and 29: 18 Introduction the potential to ch
Page 30 and 31: 20 Introduction Gorti, U., Dullemon
Page 33 and 34: 2 Optical Characterization of a New
Page 35 and 36: Evolution of Dust in Protoplanetary
Page 59: Evolution of Dust in Protoplanetary
Page 62 and 63: 52 YSOs in the Lupus Molecular Clou
Page 87 and 88: 4 A Spitzer Survey of Protoplanetar
Page 117 and 118:
Evolution of Dust in Protoplanetary
Page 119 and 120:
Evolution of Dust in Protoplanetary
Page 121 and 122:
A. Background Sources 111 Table 4.3
Page 123 and 124:
A. Background Sources 113 Figure A.
Page 125:
A. Background Sources 115 Figure A.
Page 128 and 129:
118 Discovery of a Dusty Planetary
Page 130 and 131:
Page 132 and 133:
Page 134 and 135:
Page 136 and 137:
Page 138 and 139:
128 From Protoplanetary Disks to Pl
Page 140 and 141:
Page 142 and 143:
Page 144 and 145:
Page 146 and 147:
Page 148 and 149:
Page 150 and 151:
Page 152 and 153:
Page 154 and 155:
Page 156 and 157:
Page 158 and 159:
Page 160 and 161:
Page 162 and 163:
Page 164 and 165:
Page 166 and 167:
Page 168 and 169:
Page 170 and 171:
Page 172 and 173:
Page 174 and 175:
Page 176 and 177:
166 Spectral Energy Distributions o
Page 178 and 179:
Page 180 and 181:
Page 182 and 183:
Page 184 and 185:
Page 186 and 187:
Page 188 and 189:
Page 190 and 191:
Page 192 and 193:
Page 194 and 195:
Page 196 and 197:
Page 198 and 199:
Page 201 and 202:
Nederlandse Samenvatting Inleiding
Page 203 and 204:
193 Figuur 1 - Het ontstaan van een
Page 205 and 206:
195 kunnen worden om de verschillen
Page 207 and 208:
197 Figuur 3 - Het planeetvormingsp
Page 209 and 210:
199 parameter is. Na 6 tot 8 miljoe
Page 211 and 212:
201 van de X-shooter in het ultravi
Page 213 and 214:
Resumo em Português Restrições O
Page 215 and 216:
205 Figura 1 - Ilustração do cen
Page 217 and 218:
207 Figura 2 - O Telescópio Espaci
Page 219 and 220:
209 interagem gravitacionalmente, a
Page 221 and 222:
211 e discos são conectados, é ba
Page 223:
213 uma correta separação entre a
Page 226 and 227:
216 Curriculum Vitæ omy Center (ES
Page 228 and 229:
218 Publications 8. c2d Spitzer-IRS
Page 230 and 231:
220 Thesis Acknowledgments Liesbeth
show all

Observational Constraints on The Evolution of Dust in ...

You also want an ePaper? Increase the reach of your titles

Delete template?

Save as template?