HK photometry in an UCHII region near Sh2-217 (Brand+, 2011)

Details HK photometry in an UCHII region near Sh2-217 (Brand+, 2011) HK photometry in an UCHII region near Sh2-217 (Brand+, 2011)

Nov 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010ycat..35279062b&link_type=abstract

VizieR On-line Data Catalog: J/A+A/527/A62. Originally published in: 2011A&A...527A..62B

Astronomy and Astrophysics

Astronomy

H Ii Regions, Stars: Normal, Photometry: Ccd, Photometry: Infrared

Scientific paper

Coordinates and photometric parameters (magnitudes and colours) are presented of the stars located in a molecular condensation on the SW-border of the Galactic HII region Sh2-217. The data were obtained on January 4, 2004 with the 3.58-m Telescopio Nazionale Galileo (TNG; La Palma, Canary Islands, Spain). Near-infrared observations were carried out through H and K' broad-band filters with the camera NICS. The image scale is 0.25arcsec/pixel, yielding a field of view of about 4.2'x4.2'. Observing strategy and exposure times are described in Deharveng et al. (2006A&A...458..191D), the only difference being that the dithering sequence for the H-band images was the same as adopted for K'. The data reduction steps adopted are outlined in Deharveng et al. (2006A&A...458..191D). Aperture photometry was done using the DAOPHOT package in IRAF. We followed the same procedure described in Deharveng et al. (2006A&A...458..191D) to obtain aperture photometry, after which PSF-fitting photometry was performed.
Although the seeing was good (<1"), the night was barely photometric, so we calibrated our H, K' photometry with that performed on the same field by Deharveng et al. (2003, Cat. J/A+A/399/1135). We calculated the difference in magnitudes for each coinciding source and plotted it against our derived instrumental H-K'. A colour term was present in K' because of the difference between the K and K' filters. After a best-fit calibration, a residual r.m.s. of about 0.2mag. was present in the difference between our photometry and that of Deharveng et al. (2003, J/A+A/399/1135), probably because of the different seeing and possibly also due to the intrinsic variability of young stars. Our photometry is thus on the same HK standard system as Deharveng et al. (2003, J/A+A/399/1135). Sources with K, H < 11-12 are in the non-linear regime or saturated, but such bright objects are few in number and lie outside the cluster, and are probably foreground stars. The approximate limiting magnitudes are K=18.48 and H=19.52, much deeper than achieved by Deharveng et al. (2003, J/A+A/399/1135). We estimate completeness limits of approximately K=16.5 and H=17.5 from the peak in histograms of the number of detected sources as a function of magnitude, after binning in 1mag. intervals.
The astrometric calibration of the frames was obtained by measuring the position on the image of a sample of stars and fitting those positions to the equatorial coordinates given by Deharveng et al. (2006A&A...458..191D), using tasks of STSDAS/IRAF. The typical accuracy of this procedure is of the order of 1".
(1 data file).

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