Kozlowski, Szymon and Stern, Daniel and Bock, J. J. and Borys, C. and Eisenhardt, P. R. and Gorjian, V. and Griffith, R. and Jacob, J. and Mainzer, A. and Moustakas, L. and Stauffer, J. R. (2010) Mid-infrared Variability from the Spitzer Deep Wide-field Survey. Astrophysical Journal, 716 (1). pp. 530-543. ISSN 0004-637X http://resolver.caltech.edu/CaltechAUTHORS:20100621-142204054
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We use the multi-epoch, mid-infrared Spitzer Deep Wide-Field Survey to investigate the variability of objects in 8.1 deg^2 of the NOAO Deep Wide Field Survey Boötes field. We perform a Difference Image Analysis of the four available epochs between 2004 and 2008, focusing on the deeper 3.6 and 4.5 μm bands. Out of 474, 179 analyzed sources, 1.1% meet our standard variability selection criteria that the two light curves are strongly correlated (r > 0.8) and that their joint variance (σ_(12)) exceeds that for all sources with the same magnitude by 2σ. We then examine the mid-IR colors of the variable sources and match them with X-ray sources from the XBoötes survey, radio catalogs, 24 μm selected active galactic nucleus (AGN) candidates, and spectroscopically identified AGNs from the AGN and Galaxy Evolution Survey (AGES). Based on their mid-IR colors, most of the variable sources are AGNs (76%), with smaller contributions from stars (11%), galaxies (6%), and unclassified objects, although most of the stellar, galaxy, and unclassified sources are false positives. For our standard selection criteria, 11%-12% of the mid-IR counterparts to X-ray sources, 24 μm AGN candidates, and spectroscopically identified AGNs show variability. The exact fractions depend on both the search depth and the selection criteria. For example, 12% of the 1131 known z>1 AGNs in the field and 14%-17% of the known AGNs with well-measured fluxes in all four Infrared Array Camera bands meet our standard selection criteria. The mid-IR AGN variability can be well described by a single power-law structure function with an index of γ ≈ 0.5 at both 3.6 and 4.5 μm, and an amplitude of S _0 ≃ 0.1 mag on rest-frame timescales of 2 yr. The variability amplitude is higher for shorter rest-frame wavelengths and lower luminosities.
|Additional Information:||© 2010 The American Astronomical Society. Received 2010 February 5; accepted 2010 April 8; published 2010 May 20. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of the Technology under contract with the National Aeronautics and Space Administration (NASA). Support for this work was provided by NASA through award numbers 1310744 (C.S.K. and S.K.), 1314516 (M.L.N.A.), and 1317692 (H.A.S.) issued by JPL/CalTech. C.S.K. and S.K. are also supported by NSF grant AST-0708082. The NDWFS and the research of A.D. and B.T.J. are supported by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation. Support for M.B. was provided by the W. M. Keck Foundation.|
|Subject Keywords:||cosmology: observations; galaxies: active; infrared: galaxies; quasars: general|
|Classification Code:||PACS: 95.80.+p; 98.54.Cm; 98.62.Py; 98.62.Qz; 98.54.Aj|
|Official Citation:||Szymon Kozłowski et al 2010 ApJ 716 530 doi: 10.1088/0004-637X/716/1/530|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Ruth Sustaita|
|Deposited On:||22 Jun 2010 22:58|
|Last Modified:||26 Dec 2012 12:09|
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