/ftp/cats/aliases/M/./MSR2009



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J/ApJ/702/1507      Mid-IR photometry in IC 1396A      (Morales-Calderon+, 2009)
The following files can be converted to FITS (extension .fit or fit.gz)
	table1.dat table2.dat table3.dat table6.dat
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Query from: http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/ApJ/702/1507
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Beginning of ReadMe : J/ApJ/702/1507 Mid-IR photometry in IC 1396A (Morales-Calderon+, 2009) ================================================================================ Mid-infrared variability of protostars in IC 1396A. Morales-Calderon M., Stauffer J.R., Rebull L., Whitney B.A., Barrado y Navascues D., Ardila D.R., Song I., Brooke T.Y., Hartmann L., Calvet N. <Astrophys. J., 702, 1507-1529 (2009)> =2009ApJ...702.1507M ================================================================================ ADC_Keywords: Photometry, infrared ; YSOs ; Molecular clouds Keywords: infrared: stars - stars: pre-main sequence - stars: variables: other Abstract: We have used Spitzer/Infrared Array Camera (IRAC) to conduct a photometric monitoring program of the IC1396A dark globule in order to study the mid-IR (3.6-8um) variability of the heavily embedded young stellar objects (YSOs) present in that area. We obtained light curves covering a 14 day timespan with a twice daily cadence for 69 YSOs, and continuous light curves with approximately 12s cadence over 7hr for 38 YSOs. Typical accuracies for our relative photometry were 1%-2% for the long timespan data and a few millimagnitude, corresponding to less than 0.5%, for the 7hr continuous "staring-mode" data. More than half of the YSOs showed detectable variability, with amplitudes from  0.05mag to  0.2mag. One star, IC1396A-47, shows a 3.5hr periodic light curve; this object may be a PMS Delta Scuti star. Description: Thus, we have used a recent DDT program (PI: Soifer, PID:470) to study mid-IR variability of protostars in the very young star-forming globule IC1396A. The data were collected from 2008 January 24 to February 6 and observations were performed with two distinctly different observing modes (mapping and staring). We have used previous observations from the Spitzer archive to derive the fluxes of our new targets at 24um (PID:58, PI: Rieke).