YOUNG STELLAR OBJECT VARIABILITY (YSOVAR): LONG TIMESCALE VARIATIONS IN THE MID-INFRARED

The YSOVAR (Young Stellar Object VARiability) Spitzer Space Telescope observing program obtained the first extensive mid-infrared time series photometry of the Orion Nebula Cluster plus smaller footprints in 11 other star-forming cores. We present the data collection and reduction for the Spitzer an...

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Bibliographic Details
Published in:The Astronomical journal 2014-11, Vol.148 (5), p.1-46
Main Authors: REBULL, L M, Cody, A M, Covey, K R, Gunther, H M, Hillenbrand, L A, PLAVCHAN, P, POPPENHAEGER, K, Stauffer, J R, Wolk, S J, Gutermuth, R
Format: Article
Language:English
Subjects:
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
COMPARATIVE EVALUATIONS
ENERGY SPECTRA
Light curve
NEBULAE
Orion nebula
PERIODICITY
PHOTOMETRY
PROTOSTARS
REDUCTION
Samples
SPACE
Spectral energy distribution
STARS
Statistical analysis
Statistical methods
Statistics
TELESCOPES
TRANSIENTS
VISIBLE RADIATION
X RADIATION
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Summary:The YSOVAR (Young Stellar Object VARiability) Spitzer Space Telescope observing program obtained the first extensive mid-infrared time series photometry of the Orion Nebula Cluster plus smaller footprints in 11 other star-forming cores. We present the data collection and reduction for the Spitzer and ancillary data, and define the "standard sample" on which we calculate statistics, consisting of fast cadence data, with epochs roughly twice per day for ~40 days. We also define a "standard sample of members" consisting of all the IR-selected members and X-ray-selected members. We characterize the standard sample in terms of other properties, such as spectral energy distribution shape. We use three mechanisms to identify variables in the fast cadence data - the Stetson index, a x[sup 2] fit to a flat light curve, and significant periodicity. We do not find any evidence for variability that causes excesses to appear or vanish within our data set; out of members and field objects combined, at most 0.02% may have transient IR excesses.
ISSN:1538-3881
0004-6256
1538-3881
DOI:10.1088/0004-6256/148/5/92