Extragalactic abstracts - IRSA - California Institute of Technology

More documents

Recommendations

Info

Spitzer_Approved_Extragalactic Mar 25, 10 16:24 Page 251/742 Spitzer Space Telescope − Guaranteed Time Observer Proposal #214 IRAC and MIPS imaging of the HDF_S Principal Investigator: Giovanni Fazio Institution: Harvard−Smithsonian Astrophysical Observatory Technical Contact: Jiasheng Huang, CfA Co−Investigators: Pauline Barmby, SAO Myungshin Im, SSC Steve Willner, SAO Mike Pahre, SAO Zhong Wang, SAO Marijn Franx, Leiden Obs. Huub Rottgering, Leiden Obs. Paul van der Werf, Leiden Obs. Science Category: high−z galaxies (z>0.5) Observing Modes: IracMap MipsPhot Hours Approved: 14.0 Abstract: We will image the WFPC2 field of the Hubble Deep Field South with IRAC, in four bands (3.5−8 micron). Combined with the ultra−deep VLT near−infrared imaging, we will determine the spectral energy distributions of the high redshift galaxies to the restframe K band. These SED’s will be modeled using stellar population synthesis models. Spitzer_Approved_Extragalactic Printed_by_SSC Mar 25, 10 16:24 Page 252/742 Spitzer Space Telescope − Guaranteed Time Observer Proposal #30327 IR Spectroscopy of Massive Galaxies at z>2 Principal Investigator: Giovanni Fazio Institution: Harvard−Smithsonian Astrophysical Observatory Technical Contact: Jiasheng Huang, CfA Co−Investigators: Jiasheng Huang, SAO Steve Willner, SAO Dimitra Rigopoulou, Oxford Gillian Wilson, SSC Tracy Webb, Univeristy of McGill Rob Ivison, Edinburgh Sukanya Chakrabarti, Harvard Univ Chris Conselice, University of Norttingham Science Category: high−z galaxies (z>0.5) Observing Modes: IrsMap Hours Approved: 22.1 Abstract: More and more galaxies at z>2 are detected at 24 micron. Energy sources which power the emission at 24micron remain unknown for most of those galaxies. Previous IRS studies of objects at high red shifts focused on extreme red and 24 micron luminous objects, and found that most of them are AGN. We propose IRS observations on a sample of massive galaxies at 2.50.5 mJy, and f(20cm)>0.02mJy. That most massive galaxies are detected at 24micron implies a rapid star formation occuring on these galaxies. The high star formation rate helps to explain the formation of massive galaxies at high redshifts. Nevertheless AGN contribution to the 24micron flux cannot be ruled out. The IRS spectroscopy is essential in understanding various energy sources contributing to the 24micron flux of massive galaxies. Combining both the PAH emission flux at 7.7 microns and the 20cm flux density, we will be able to obtain a better star formation rate for these massive galaxies. Thursday March 25, 2010 xgal_covers.txt 126/371
Spitzer_Approved_Extragalactic Mar 25, 10 16:24 Page 253/742 Spitzer Space Telescope − Guaranteed Time Observer Proposal #40537 IRS Observation of IR luminous LBGs Principal Investigator: Giovanni Fazio Institution: Smithsonian Astrophysical Observatory Technical Contact: Jiasheng Huang, Smithsonian Astrophysical Observatory Co−Investigators: Dimitra Rigopoulou, Oxford Lin Yan, SSC Tracy Webb, McGill University Matt Ashby, SAO Steve Willner, SAO Casey Papovich, U Arizona Delphine Marcillac, U Arizona Science Category: high−z galaxies (z>0.5) Observing Modes: IrsMap IrsPeakupImage Hours Approved: 47.3 Abstract: Lyman−Break Galaxies (LBGs) and Submillimeter Galaxies (SMGs) are star−forming galaxies at high−redshifts, selected in very different ways. A large amount of spectroscopic data are now available for LBGs, and consequently we have an increasingly meaninful understanding of their physical properties. By contrast SMGs (i.e., high−redshift ULIRGs) are notoriously faint and difficult to identify at visible wavelengths, making it extremely hard even to measure their redshifts. However, we have recently discovered (Huang etal 2005) a population that links LBGs and SMGs: Infrared−Luminous Lyman Break Galaxies (ILLBGs). ILLBGs strongly resemble SMGs in the infrared, yet are surprisingly bright at visible wavelengths. This permits 1.) high S/N study of their rest−frame UV spectra, 2.) measurement of differences in physical properties between normal blue LBGs and ILLBGs, and 3.) comparison of ILLBGs to their local ULIRG/LIRG couterparts. We have recently completed a new, large photometric survey for LBGs in the Extended Groth Strip (EGS) field, in which we detected 6500 LBG candidates. Amoung these, 220 have clear detections in the MIPS 24 micron band −− in other words, they are ILLBGs. This is the largest ULIRG/LIRG sample at z=3 in existence. We ask for four nights of GMOS time to carry out a spectroscopic study of this important population that links LBGs and SMGs. Spitzer_Approved_Extragalactic Printed_by_SSC Mar 25, 10 16:24 Page 254/742 Spitzer Space Telescope − Guaranteed Time Observer Proposal #40689 Study AGN and Galaxy Environment and Evolution Since z=1: IRAC imaging of the DEEP2 fields Principal Investigator: Giovanni Fazio Institution: Smithsonian Astrophysical Observatory Technical Contact: Jiasheng Huang, Smithsonian Astrophysical Observatory Co−Investigators: Steve Willner, SAO Mat Ashby, SAO Pauline Barmby, SAO William Foreman, SAO Christine Jones−Foreman, SAO Ryan Hickox, SAO Science Category: high−z galaxies (z>0.5) Observing Modes: IracMap Hours Approved: 14.3 Abstract: We propose to carry out an IRAC imaging of the field 2 in the Deep Extragalactic Exploration Prober−2 (DEEP2) survey, as a part of a joint Spitzer and Chandra program. We perform multi−wavelength studies of galaxies and AGNs in a substantially large redshift sample with high resolution spectra observed with DEIMOS in DEEP2 . Our science goal is to study AGN enviroment and evolution since z=1. The IRAC colors and X−ray luminosities are essentail in selecting AGNs up to z=1. The IRAC bands also probe the rest−frame NIR bands (H and K) for galaxies at z=1, permitting to derive the rest−frame K−band luminosity function at z=1. Thursday March 25, 2010 xgal_covers.txt 127/371
Page 1 and 2:
Spitzer_Approved_Extragalactic Mar
Page 3 and 4:
Page 5 and 6:
Page 7 and 8:
Page 9 and 10:
Page 11 and 12:
Page 13 and 14:
Page 15 and 16:
Page 17 and 18:
Page 19 and 20:
Page 21 and 22:
Page 23 and 24:
Page 25 and 26:
Page 27 and 28:
Page 29 and 30:
Page 31 and 32:
Page 33 and 34:
Page 35 and 36:
Page 37 and 38:
Page 39 and 40:
Page 41 and 42:
Page 43 and 44:
Page 45 and 46:
Page 47 and 48:
Page 49 and 50:
Page 51 and 52:
Page 53 and 54:
Page 55 and 56:
Page 57 and 58:
Page 59 and 60:
Page 61 and 62:
Page 63 and 64:
Page 65 and 66:
Page 67 and 68:
Page 69 and 70:
Page 71 and 72:
Page 73 and 74:
Page 75 and 76: Spitzer_Approved_Extragalactic Mar
Page 121 and 122: Mar 25, 10 16:24 Spitzer_Approved_E
Page 125: Spitzer_Approved_Extragalactic Mar
Page 165 and 166: Mar 25, 10 16:24 Spitzer_Approved_E
Page 177 and 178:
Page 179 and 180:
Page 181 and 182:
Page 183 and 184:
Page 185 and 186:
Page 187 and 188:
Page 189 and 190:
Page 191 and 192:
Page 193 and 194:
Page 195 and 196:
Page 197 and 198:
Page 199 and 200:
Page 201 and 202:
Page 203 and 204:
Page 205 and 206:
Page 207 and 208:
Page 209 and 210:
Page 211 and 212:
Page 213 and 214:
Page 215 and 216:
Page 217 and 218:
Page 219 and 220:
Page 221 and 222:
Page 223 and 224:
Page 225 and 226:
Page 227 and 228:
Page 229 and 230:
Page 231 and 232:
Page 233 and 234:
Page 235 and 236:
Page 237 and 238:
Page 239 and 240:
Page 241 and 242:
Page 243 and 244:
Page 245 and 246:
Page 247 and 248:
Page 249 and 250:
Page 251 and 252:
Page 253 and 254:
Page 255 and 256:
Page 257 and 258:
Page 259 and 260:
Page 261 and 262:
Page 263 and 264:
Page 265 and 266:
Page 267 and 268:
Page 269 and 270:
Page 271 and 272:
Page 273 and 274:
Page 275 and 276:
Page 277 and 278:
Page 279 and 280:
Page 281 and 282:
Page 283 and 284:
Page 285 and 286:
Page 287 and 288:
Page 289 and 290:
Page 291 and 292:
Page 293 and 294:
Page 295 and 296:
Page 297 and 298:
Page 299 and 300:
Page 301 and 302:
Page 303 and 304:
Page 305 and 306:
Page 307 and 308:
Page 309 and 310:
Page 311 and 312:
Page 313 and 314:
Page 315 and 316:
Page 317 and 318:
Page 319 and 320:
Page 321 and 322:
Page 323 and 324:
Page 325 and 326:
Page 327 and 328:
Page 329 and 330:
Page 331 and 332:
Page 333 and 334:
Page 335 and 336:
Page 337 and 338:
Page 339 and 340:
Page 341 and 342:
Page 343 and 344:
Page 345 and 346:
Page 347 and 348:
Page 349 and 350:
Page 351 and 352:
Page 353 and 354:
Page 355 and 356:
Page 357 and 358:
Page 359 and 360:
Page 361 and 362:
Page 363 and 364:
Page 365 and 366:
Page 367 and 368:
Page 369 and 370:
Page 371:
show all

Extragalactic abstracts - IRSA - California Institute of Technology

Create successful ePaper yourself

Delete template?

Save as template?