IC348CXO - IC 348 Chandra X-Ray Point Source Catalog
Optical and infrared counterparts have been identified for most of the X-ray sources. Some 40 X-ray sources do not have optical or IR counterparts, and are most likely background (probably extragalactic) objects. This number is consistent with the expected number of extragalactic background X-ray sources based on the observed log N - log S statistics from the deep X-ray counts in the Chandra Deep Field South.
Deep Chandra X-ray observatory imaging study of the very young stellar cluster IC 348. Preibisch T., Zinnecker H. <Astron. J. 122, 866 (2001)> =2001AJ....122..866P X-ray properties of the young stellar and substellar objects in the IC 348 cluster: the Chandra view. Preibisch T., Zinnecker H. <Astron. J. 123, 1613 (2002)> =2002AJ....123.1613PP
A sequential identification number for each X-ray source in this study, in order of increasing J2000 Right Ascension.
An alternative designation for the X-ray source, using the CXOPZ prefix (Chandra X-ray Observatory, Preibisch & Zinnecker) registered by the authors and its source_number value.
The Right Ascension of the X-ray source in the selected equinox. This parameter was given in J2000 coordinates and to a precision of 0.01 seconds of time in the originating table.
The Declination of the X-ray source in the selected equinox. This parameter was given in J2000 coordinates and to a precision of 0.1 arcseconds in the originating table. A small offset of 0.51" +/ 0.14" between the declinations in the X-ray and optical coordinate frames has been applied to the X-ray declinations listed in this table.
The Galactic Longitude of the X-ray source.
The Galactic Latitude of the X-ray source.
The X-ray source positional uncertainty in the Right Ascension direction, in arcseconds.
The X-ray source positional uncertainty in the Declination direction, in arcseconds.
The exposure-time-corrected X-ray source count rate in the 0.2 - 8.0 keV ACIS energy band, in counts per second.
The unceratinty in the X-ray source count rate, in counts per second.
The preferred designation for the X-ray source, using the CXOPZ prefix (Chandra X-ray Observatory, Preibisch & Zinnecker) registered by the authors, followed by the 'J' and the usual numeric string format based on the J2000 position truncated to 0.1 seconds of time and 1 arcsecond of declination, e.g., 'CXOPZ J034346.9+321320'.
The identifications of the X-ray source with an optical and/or infrared counterpart from the catalogs of (i) Herbig (1998, ApJ, 497, 736) if the name begins with an 'H-' prefix, (ii) Luhman et al. (1998, ApJ, 508, 347) or Luhman (1999, ApJ, 525, 466) if the name begins with an 'L-' prefix, or (iii) Najita et al. (2000, ApJ, 541, 977) if the name begins with an 'N-' prefix. Stars known to be foreground or background objects are marked with 'FG' and 'BG', respectively. If no catalogued counterpart is known, the entry '2MASS' means that the X-ray source has a counterpart in the 2MASS point source catalog, while 'noCP' means that no optical or infrared counterpart could be found. Source CXOPZ-J034424.6+321349 is identified with a faint infrared source not included in the 2MASS catalog.
The spectral type of the counterpart to the X-ray source.
The visual extinction of the counterpart to the X-ray source, in magnitudes.
This flag parameter for the visual extinction has the following values:
'i' means that the value has been estimated from the near-infrared colors ':' means that, due to a lack of further information, an extinction of 3.5 magnitudes has been assumed
The equivalent width of the H-alpha emission line, in Angstroms. Negative values denote H-alpha absorption.
The best-fit temperature found in a single-component model to the X-ray spectrum, or, if such a model did not yield an acceptable fit, the emission-weighted mean of the best-fit temperature values that were found in a 2-component model of the X-ray spectrum of the source, in keV.
The uncertainty in the derived characteristic plasma temperature inferred from X-ray spectral modeling, in keV.
The extinction-corrected, 0.2 - 10 keV band X-ray luminosity of the source, in erg/s, calculated based on the analysis of the X-ray spectra as described in Section 5 of Preibisch & Zinnecker (2002) and assuming a distance of 310 pc.
The uncertainty in the X-ray luminosity of the source, in erg/s.
The HEASARC Browse object classification, based on the spectral type of the counterpart when available.