H-band observations of the Chandra Deep Field South

Abstract

Abstract. We report results of our H-band survey of the Chandra Deep Field South (CDFS). The observations, made with SofI on the NTT, cover 0.027 square degrees to H < 20.5 and 0.17 square degrees to H < 19.8 (50% completeness limits). In total, 4819 objects were detected, of which 80% are galaxies based on the SExtractor parameter "stellarity index" having a value less than 0.5. Our astrometric solutions are in good agreement with those of the Las Campanas Infrared Survey (LCIRS), the COMBO-17, and the ESO-EIS surveys. Our photometry compares satisfactorily with the LCIRS results as well as with GOODS data. Galaxy number counts are ∼50 000 galaxies per square degree at H < 20.75, in good agreement with those of LCIRS. The object catalog is published electronically at the CDS .

The Great Observatories Origins Deep Survey

“…In the H-band the results of two imaging surveys which have been conducted in the CDF-S region previously, by Moy et al (2003) and Cimatti et al (2002), are fully compatible with our findings. Also the number counts resulting from the completely independent study by Metcalfe et al (2006) based on imaging of the 7 × 7 William Herschel Deep Field using the Omega Prime camera on the 3.5-m Calar Alto telescope, Spain, are perfectly in agreement with our data.…”

“…The apparent scatter is larger than what the individual flux error estimates suggest -a finding that applies to this and the following comparisons as well. The magnitude differences with respect to the H-band observations of the CDF-S by Moy et al (2003) are noticeably more dispersed while not exhibiting any systematic offset. The comparison with the Las Campanas Infrared survey (LCIRS, Chen et al 2002) features a slight trend with magnitude in such a way that bright sources (H < ∼ 18) appear brighter in GOODS/ISAAC while faint sources appear to be unbiased or even slightly fainter than in the LCIRS.…”

“…The J and K s observations that were used belong to the infrared part of the ESO Imaging Survey (e.g. Olsen et al 2006), the H band data were originally obtained within a program led by Rigopoulou (see Moy et al 2003) 3 . The layout of the JHK s SOFI observations in the CDF-S generally includes some overlap of adjacent images, and, additionally, a series of lowexposure "calibration images" arranged in a pattern being offset to the deep integrations had been acquired in J and K s , so that accurate photometric scalings could be measured not only between ISAAC and SOFI but also between adjacent SOFI images.…”

“…The comparison with the Las Campanas Infrared survey (LCIRS, Chen et al 2002) features a slight trend with magnitude in such a way that bright sources (H < ∼ 18) appear brighter in GOODS/ISAAC while faint sources appear to be unbiased or even slightly fainter than in the LCIRS. The (Olsen et al 2006), g) H-band observations of the CDF-S by Moy et al (2003), h) Las Campanas Infrared survey (Chen et al 2002), and, i) K20 survey (Cimatti et al 2002). The differences of magnitudes of sources as measured on the GOODS/ISAAC images and as given in the respective reference catalogs are displayed as a function of the measured GOODS/ISAAC magnitude in the AB system.…”

Tracing the Mass‐Dependent Star Formation History of Late‐Type Galaxies Using X‐Ray Emission: Results from the Chandra Deep Fields

“…For the E-CDF-S, we used (1) the 17-bandpass photometry available through COMBO-17, (2) J and K s imaging from the ESO Imaging Survey (Olsen et al 2006), (3) J, H, and K from the MUSYC collaboration ( E. N. Taylor et al, in preparation; see also Moy et al 2003;Gawiser et al 2006), and (4) Spitzer IRAC data from the GOODS and SIMPLE teams (M. Dickinson et al, in preparation; P. G. van Dokkum et al, in preparation). Using these data, we constructed a rest-frame near-UVYtoYnear-IR SED for each galaxy.…”