IC348CXO2 - IC 348 Chandra X-Ray Point Source Catalog 2
X-ray fluxes are presented for all (185) known optical/infrared IC348 members which were observed and detected by Chandra. The basic source parameters for all X-ray sources, i.e., including an additional 105 sources not associated with known IC 348 members, are given. The X-ray flux upper limits for 129 IC 348 members which were observed but not detected by Chandra (present in the as published version of Table 3 from the reference paper) are not included in this HEASARC representation of the data given in Tables 3 and 7 from the reference paper. Thus, this table contains 290 (185 + 105) rows, one for each X-ray source (IC 348 member or not) detected by Chandra in the direction of IC 348.
X-ray view of IC348 in the light of an updated cluster census. Stelzer B., Preibisch T., Alexander F., Mucciarelli P., Flaccomio E., Micela G., Sciortino S. <Astron. Astrophys. 537, A135 (2012)> =2012A&A...537A.135S (SIMBAD/NED BibCode)
A unique identification number for each X-ray source in the catalog, in order of increasing J2000.0 Right Ascension.
The Chandra X-ray source designation, in the form recommended by the Dictionary of Nomenclature of Celestial Objects for unregistered Chandra sources based on their truncated J2000.0 equatorial coordinates, viz., 'CXOU JHHMMSS.s+DDMMSS'. In the reference paper, the authors used names with higher precision, i.e., 'CXOU JHHMMSS.ss+DDMMSS.s' which the HEASARC shortened accordingly after verifying that no duplicate names resulted.
The Right Ascension of the Chandra source in the selected equinox. This was given in J2000.0 equatorial coordinates in decimal degrees to a precision of 10-6 degrees in the original table.
The Declination of the Chandra source in the selected equinox. This was given in J2000.0 equatorial coordinates in decimal degrees to a precision of 10-6 degrees in the original table.
The Galactic Longitude of the Chandra source.
The Galactic Latitude of the Chandra source.
The estimated standard deviation of the random component of the position error, sqrt (sigma(x)2 + sigma(y)2) of the Chandra source, in arcseconds. The single-axis position errors, sigma(x) and sigma(y), are estimated from the single-axis standard deviations of the PSF inside the extraction region and the number of counts extracted.
The off-axis angle of the Chandra source from the nominal pointing direction, in arcminutes.
The net counts extracted for the Chandra source in the total energy band (0.5 - 8.0 keV).
The 1-sigma uncertainty (the average of the upper and lower errors) for the net source counts extracted in the total energy band.
The background counts expected in the Chandra source extraction region in the total energy band.
The net counts extracted for the Chandra source in the hard energy band (2.0 - 8.0 keV).
The fraction of the PSF which is enclosed within the extraction region (at 1.497 keV). Note that a reduced PSF fraction (significantly below 90%) may indicate that the source is in a crowded region or on the edge of the field.
The photometric significance of the Chandra source computed as the net counts divided by the upper error in the net counts.
This flag is set to '<' if the corresponding parameter value is an upper limit.
The logarithm of the probability Pb that the observed counts (in the total band) are solely from a background fluctuation rather than from a real source. Some sources have Pb values above the 0.1% threshold that defines the catalog because local background estimates can rise during the final extraction iteration after sources are removed from the catalog.
This parameter contains a source anomalies flag which is set to 'g' if the fractional time that the source was on a detector (the FRACEXPO value from mkarf) is < 0.9.
This parameter contains flag values which can be set to to the following values indicative of the presence or absence of source variability based on the Kolmogorov-Smirnov (K-S) statistic (no value is reported for sources with fewer than four counts or for sources in chip gaps or on field edges):
a = no evidence for variability (0.05 < PKS) b = possibly variable (0.005 < PKS < 0.05) c = definitely variable (PKS < 0.005)
The effective exposure time for the Chandra source, in seconds. This is the approximate time that the source would have to have been observed at the aimpoint of the Chandra ACIS-I detector to obtain the same number of counts that were actually obtained at its position in the focal plane.
The background-corrected median photon energy for the Chandra source over the total 0.5 - 8 keV energy band, in keV.
The source identifier for members of the IC 348 cluster. If the object is not a known cluster member, this parameter is left blank. To construct a name for the cluster members which is recognized by the Simbad name resolver, the user should add the prefix of 'Cl* IC 348 LRL ' (for Luhman, Rieke, Lada+ 1998 ApJ, 508, 347 who began numbering members of IC 348) to the cluster number value, e.g., Cl* IC 348 LRL 2' for the source with cluster number = 2.
The X-ray flux of the Chandra source, in erg s-1 cm-2, presumably in the total 0.5-8.0 keV energy band. This is either (1) the intrinsic, i.e., extinction-corrected, X-ray flux of the Chandra source obtained using the XPHOT software (for those sources for which the flux_flag parameter is blank) or (2) the observed, i.e., not the intrinsic, X-ray flux of the Chandra source (called FLUX2 by the authors) which is computed by the AE software from the product of the photon flux and the median photon energy (for those sources which are too faint to perform the XPHOT analysis on and for which the flux_flag parameter is set to to 'f2').
The logarithm of the X-ray luminosity of the Chandra source, in erg s-1. This is given only for those 187 sources which are known to be associated with cluster members, else it is left blank. The HEASARC created this parameter using the X-ray flux values which were provided and assuming a distance of 310 pc to the cluster. If flux_flag is blank, the luminosity is the intrinsic, extinction-corrected, luminosity, whereas if flux_flag is 'f2', it is the observed luminosity and may be significantly less than the intrinsic luminosity if there is significant extinction towards the source.
This prameter flag indicates the type of flux quoted for the Chandra source: a blank value means that the flux is the intrinsic, i.e., extinction-corrected, X-ray flux of the Chandra source obtained using the XPHOT software, while a value of 'f2' means it is the observed, i.e., not the intrinsic, X-ray flux of the Chandra source (called FLUX2 by the authors) which is computed by the AE software from the product of the photon flux and the median photon energy.