Imaging of High Redshift Submillimeter Galaxies at 16 and 22microns with the Spitzer/IRS: Revealing a population at z>2.5

V. Charmandaris; K. I. Uchida; D. Weedman; T. Herter; J. R. Houck; H. I. Teplitz; L. Armus; B. R. Brandl; S. J. U. Higdon; B. T. Soifer; P. N. Appleton; J. van Cleve; J. L. Higdon

doi:10.1086/422359

arXiv · astro-ph/0406149

Imaging of High Redshift Submillimeter Galaxies at 16 and 22microns with the Spitzer/IRS: Revealing a population at z>2.5

V. Charmandaris·K. I. Uchida·D. Weedman·T. Herter·J. R. Houck·H. I. Teplitz·L. Armus·B. R. Brandl·S. J. U. Higdon·B. T. Soifer·P. N. Appleton·J. van Cleve·J. L. Higdon

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Abstract

We present broad band imaging observations obtained with the ``peak up'' imagers of the Spitzer Space Telescope Infrared Spectrograph (IRS) at wavelengths of 16micron and 22micron for a number of sources detected primarily at submillimeter wavelengths, which are believed to be at high, though undetermined, redshift. We targeted 11 sources originally detected by SCUBA and 5 submillimeter sources detected at 1.2mm by MAMBO. Two optically discovered quasars with z>6 were also observed to determine if there is detectable dust emission at such high redshifts. Seven of the submillimeter sources and both high-redshift quasars were detected, and upper limits of about ~50microJy apply to the remainder. Using their mid-/far-IR colors, we demonstrate that all of the submillimeter sources are at z>1.4. The mid-IR colors for two of our detections and three of our strong upper limits suggest that these galaxies must be at z>2.5. We also introduce a technique for estimating redshifts and source characteristics based only on the ratio of fluxes in the 16micron and 22micron images.

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V. Charmandaris, K. I. Uchida, D. Weedman, T. Herter, J. R. Houck, H. I. Teplitz, L. Armus, B. R. Brandl, S. J. U. Higdon, B. T. Soifer, P. N. Appleton, J. van Cleve, J. L. Higdon. 2004-06-07. Imaging of High Redshift Submillimeter Galaxies at 16 and 22microns with the Spitzer/IRS: Revealing a population at z>2.5. https://doi.org/10.1086/422359

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