The authors present a full catalogue of 269 ISOPHOT observations (291 measurements) of 181 compact objects. They were observed in staring mode with the P1 detector at 3.6 micrometer. The catalogue is split into two separated catalogues. Second one contains observations at two or more different wavelengths. The measurement at 3.6 micrometer has been re-processed for 237 observations of 179 compact objects.

The data set consists on:

• AAP data structure files as produced by PIA 10.0 and the same in FITS format.

A detailed report is available here.
 

List of caveats related to P1 staring observing mode corrected in this work:

• CAVEATs for DETECTORS P1 & P2:
  • Non-standard apertures (ISOPHOT HB Section 5.4)

    If observations are performed in non-standard apertures, deviations from the exact flux calibration can occur. One effect is related to the aperture dependent responsivity calibration with the internal Fine Calibration Source (FCS).
    However in our data processing scheme we adopted default responsivities and the FCS calibration was not used. Therefore the photometric fluxes presented in this catalogue are not affected by this caveat. It is also known that the scaling of the signal in different apertures is non-linear with the geometric aperture size (PHT Handbook Section 10.6). Since this catalogue contains observations of compact sources located at the centre of the aperture this caveat is irrelevant in this case.

  • Restricted signal non-linearity correction (ISOPHOT HB OLP caveat 10.10)

    The ISOPHOT-P detectors show a non-linear response with flux.
    As part of the analysis this non-linear response has been characterized and then each observation was corrected for this effect (see "empirical correction" in the data processing report).

  • Aperture correction factor for point source applied!

    The fluxes have been corrected for the loss of flux outside the aperture under the assumption that the source is a point source (PHT Handbook Section 10.12 and Table 2.3). Since the background has not been subtracted before, this correction factor has to be applied to the background value before subtraction.
    In most cases, the background is negligible, compared to source flux at 3.6um. Thus this effect has no influence on our photometric results.

  • Responsivity Drifts

    The detector response, i.e. the amount of photo current per amount of illuminated radiation, can vary, in particular due to cosmic ray hits (PHT Handbook Section 4.2.4 and 10.8)). This affects mainly long lasting map observations.
    Since this catalogue contains typically short ON/OFF observations this caveat is irrelevant.

  • Background Subtraction

    Staring mode observations of point sources are not background subtracted.
    In the preparation of this catalogue the corresponding background measurements (if any) have been identified and subtracted from the source observation. When no dedicated background observation was available an average "empty sky" signal was subtracted (see data processing report).

  • Color Correction

    The flux density values in this catalogue are not color corrected.

  • Signal Transients

    Gradual (transient) adjustment of the detector output signal in response to an instantaneous flux change. Time constants can be several minutes. PHT Handbook Section 4.2.3 and 10.7
    No transient correction algorithm is available for the P1 detector yet. In cases of unstable signals only the last part of the measurement was used (selected interactively).

  • Incomplete Error Propagation

    The PHT OLP data product does only contain an uncertainty from the statistical signal evaluation. It does not give any estimates of the systematic uncertainties of all applied calibration steps. Therefore, the provided uncertainties must be considered as minimal errors (PHT Handbook Section 10.3).
    As described in the data processing report a typical ensemble flux uncertainty was derived for a subset of the sample. This uncertainty was found to depend on the flux of the source. The formal uncertainties in the catalogue were computed as the maximum of the PIA error bars and the ensemble uncertainty.