Catalogue of Young Stellar Objects
Attila Moór, Peter Ábrahám,
Ágnes Kóspál, Attila Juhász, Csaba Kiss
Konkoly Observatory, Budapest, Hungary
20 December 2006
The authors present 288 ISOPHOT observations of 183|
young stellar objects.
The data set consists on:
The final photometric values are presented in the
form of a catalogue that can be queried from the ISO Data Archive.
AAP data structure files as produced by PIA 10.0
and the same in FITS format.
A detailed report is available
List of corrected caveats related to the observing
modes involved in the present work::
GENERAL CAVEATS FOR ISOPHOT
Signal Transients (ISOPHOT HB
chapter 4.2.3 and
OLP caveat 10.7)
As described in the
data processing report a flux dependent transient
correction on all C100 data using an IDL routine is applied. For details of the
algorithm see del Burgo et al. (ESA SP-511, 2002). The correction noticeably
improved the results at intermediate fluxes (~ 2-16 Jy). In the case of the C200 detector
signal transients are small and negligible compared to other error sources
(P. Héraudeau, private communication).
Incomplete error propagation (ISOPHOT HB
OLP caveat 10.3)
- Mini-map observations:
Individual error bars for each measurement are obtained as the standard deviation
of flux values obtained by different detector pixels. In parallel the empirical
total uncertainty for the whole ensemble of 555 normal star measurements are
also assessed by computing the standard deviation of the [measured - predicted]
flux differences. The two kinds of errors were in reasonable agreement. The results
confirmed that the main components of the total uncertainty are instrumental noise
and sky confusion noise. In the case of C200 measurements the dominant factor is
the sky confusion noise.
Scan and sparse map observations:
Formal flux uncertainty values were provided by the IDL procedure which fitted
the measured fluxes of the different pixels as a function of the footprint
data processing report).
CAVEATs for DETECTORS C100 and C200
Restricted signal non-linearity correction (ISOPHOT HB
OLP caveat 10.10)
- Mini-map and scan observations:
As a last step of the processing scheme an empirical flux-dependent correction is
performed which - signals and fluxes are approximately proportional - corrects
to a large extent for the possible artifacts related to the restricted range
of signal non-linearity correction.
- Sparse map observations:
Tests on normal star observations performed in sparse map mode show no obvious
systematic photometric discrepancies as a function of stellar flux, indicating
that the restrictions in the signal non-linearity correction do not lead to
noticable quality decrease in the present sparse map data set.
Responsivity Drifts (ISOPHOT HB
chapter 4.2.4 and
OLP caveat 10.8):
In those cases when enough data points were available the long term drift
evolution was fitted with a 2nd order polynomial and subtracted from the
observation. This correction improved the photometric results significantly.
Mini-map, scan and sparse map observations:
The flux extraction method adopted in our data reduction scheme is based on
a simultaneous fitting of the background level and the source flux
using the point-spread function.
- FCS calibration quality restricted
All C100 and C200 observations of the present data set were observed after
- Aperture photometry from surface brightness maps
In our processing the flux was reconstructed with the help of the
detector footprint shape.
- CAVEATs for DETECTORS P1 & P2 & P3