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24 April 2024 |
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Spitzer IRS Spectra of Optically Faint Infrared Sources with Weak Spectral Features | | D. W. Weedman
; B. T. Soifer
; Lei Hao
; J. L. Higdon
; S. J. U. Higdon
; J. R. Houck
; E. LeFloc’h
; M. J. I. Brown
; A. Dey
; B. T. Jannuzi
; M. Rieke
; V. Desai
; C. Bian
; D. Thompson
; L. Armus
; H. Teplitz
; P. Eisenhardt
; S.P. Willner
; | | Date: |
29 Jun 2006 | | Abstract: | Spectra have been obtained with the low-resolution modules of the Infrared Spectrograph (IRS) on the Spitzer Space Telescope (Spitzer) for 58 sources having f$_{
u}$(24 micron) > 0.75 mJy. Sources were chosen from a survey of 8.2 deg$^{2}$ within the NOAO Deep Wide-Field Survey region in Bootes (NDWFS) using the Multiband Imaging Photometer (MIPS) on the Spitzer Space Telescope. Most sources are optically very faint (I > 24mag). Redshifts have previously been determined for 34 sources, based primarily on the presence of a deep 9.7 micron silicate absorption feature, with a median z of 2.2. Spectra are presented for the remaining 24 sources for which we were previously unable to determine a confident redshift because the IRS spectra show no strong features. Optical photometry from the NDWFS and infrared photometry with MIPS and the Infrared Array Camera on the Spitzer Space Telescope (IRAC) are given, with K photometry from the Keck I telescope for some objects. The sources without strong spectral features have overall spectral energy distributions (SEDs) and distributions among optical and infrared fluxes which are similar to those for the sources with strong absorption features. Nine of the 24 sources are found to have feasible redshift determinations based on fits of a weak silicate absorption feature. Results confirm that the "1 mJy" population of 24 micron Spitzer sources which are optically faint is dominated by dusty sources with spectroscopic indicators of an obscured AGN rather than a starburst. There remain 14 of the 58 sources observed in Bootes for which no redshift could be estimated, and 5 of these sources are invisible at all optical wavelengths. | | Source: | arXiv, astro-ph/0606740 | | Services: | Forum | Review | PDF | Favorites | |
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