TY - JOUR
T1 - Observations of the Hubble Deep Field with the Infrared Space Observatory - II. Source detection and photometry
AU - Goldschmidt, Pippa
AU - Oliver, Sebastian
AU - Serjeant, Steve
AU - Baker, Amanda
AU - Eaton, N
AU - Efstathiou, Andreas
AU - Gruppioni, C.
AU - Mann, Robert
AU - Mobasher, Bahram
AU - Rowan-Robinson, M.
AU - Sumner, Tim
AU - Danese, L.
AU - Elbaz, David
AU - Franceschini, Alberto
AU - Egami, Eiichi
AU - Kontizas, M.
AU - Lawrence, Andrew
AU - McMahon, Richard
AU - Norgaard-Nielsen, H. U.
AU - Perez-Fournon, Ismael
AU - Gonzalez-Serrano, J. I.
PY - 1997/8/1
Y1 - 1997/8/1
N2 - We present positions and fluxes of point sources found in the Infrared
Space Observatory (ISO) images of the Hubble Deep Field (HDF) at 6.7 and
15 mu. We have constructed algorithmically selected `complete'
flux-limited samples of 19 sources in the 15-mu image, and seven sources
in the 6.7-mu image. The typical flux limit at 15 mu is ~0.2 mJy and at
6.7 mu is ~0.04 mJy. We have selected `supplementary' samples of three
sources at 15 mu and 20 sources at 6.7 mu by eye. We discuss the
completeness and reliability of the connected pixel source detection
algorithm used, by comparing the intrinsic and estimated properties of
simulated data, and also by estimating the noise properties of the real
data. The most pessimistic estimate of the number of spurious sources in
the `complete' samples is one at 15 mu and two at 6.7 mu, and in the
`supplementary' lists is one at 15 mu and five at 6.7 mu.
AB - We present positions and fluxes of point sources found in the Infrared
Space Observatory (ISO) images of the Hubble Deep Field (HDF) at 6.7 and
15 mu. We have constructed algorithmically selected `complete'
flux-limited samples of 19 sources in the 15-mu image, and seven sources
in the 6.7-mu image. The typical flux limit at 15 mu is ~0.2 mJy and at
6.7 mu is ~0.04 mJy. We have selected `supplementary' samples of three
sources at 15 mu and 20 sources at 6.7 mu by eye. We discuss the
completeness and reliability of the connected pixel source detection
algorithm used, by comparing the intrinsic and estimated properties of
simulated data, and also by estimating the noise properties of the real
data. The most pessimistic estimate of the number of spurious sources in
the `complete' samples is one at 15 mu and two at 6.7 mu, and in the
`supplementary' lists is one at 15 mu and five at 6.7 mu.
KW - SURVEYS
KW - INFRARED: GALAXIES
U2 - 10.1093/mnras/289.2.465
DO - 10.1093/mnras/289.2.465
M3 - Article
SN - 0035-8711
VL - 289
SP - 465
EP - 470
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 2
ER -