RASSNORSAM - ROSAT All-Sky Survey Completely Identified Northern Sample
Identification of a complete sample of northern ROSAT All-Sky Survey X-ray sources. III. The catalog. Appenzeller I., Thiering I., Zickgraf F.-J., Krautter J., Voges W., Chavarria C., Kneer R., Mujica R., Pakull M., Rosso C., Ruzicka F., Serrano A., Ziegler B. <Astrophys. J. Suppl. Ser. 117, 319 (1998)> =1998ApJS..117..319A
This is an internal designation for the X-Ray sources in the six study areas using the recommended 'ATZ98 ' prefix, a letter code, and a sequence number in order of increasing J2000 RA. The letter codes A through F refer to study areas I, II, III, IV, V, and VI. One of the study areas (V) was chosen to be close to the North Ecliptic Pole, another (IV) is close to the North Galactic Pole, while the other four areas are in regions of medium to high X-ray sensitivity levels.
The ROSAT "RX J" X-ray source designation.
The Right Ascension of the X-ray source in the selected equinox. This was given in J2000 coordinates and to a precision of 0.1 seconds of time in the original catalog.
The Declination of the X-ray source in the selected equinox. This was given in J2000 coordinates and to a precision of 1 arcsecond in the original catalog.
The Galactic Longitude of the X-ray source.
The Galactic Latitude of the X-ray source.
The net X-Ray source count rate, in counts/s, as derived after superposition of all ROSAT scan stripes and correction for vignetting and dead time.
The RMS uncertainty in the X-ray source count rate, in counts/s, as given by the maximum likelihood algorithm of the ROSAT Standard Analysis Software System (SASS) of MPE, Garching.
The hardness ratio HR1 = (B-A)/(B+A), where A is the integrated counts in the energy range 0.11-0.41 keV, and B is the integrated counts in the energy range 0.52-2.01 keV.
The statistical mean error in the hardness ratio HR1.
The hardness ratio HR2 = (D-C)/(D+C), where C is the integrated counts in the energy range 0.52-0.90 keV, and D is the integrated counts in the energy range 0.91-2.01 keV.
The statistical mean error in the hardness ratio HR2.
The X-Ray flux, in units of erg/s/cm^2 derived from the count rate (as described by Zickgraf 1997, A&AS, 123, 103).
The Right Ascension of the X-ray source minus the RA of the optical counterpart, in arcsec, for the J2000.0 equinox. For extended objects, double stars, and other cases where no accurate position could be determined, this is left blank.
The Declination of the X-ray source minus the Declination of the optical counterpart, in arcsec, for the J2000.0 equinox. For extended objects, double stars, and other cases where no accurate position could be determined, this is left blank.
An identification quality index which can have the following possible values:
1: reliable identifications based on authors' own observations 2: reliable informations with a known object based on literature data 3: likely but uncertain identifications 4: case in which no plausible optical counterpart could be found
The classification of the optical counterpart to the X-ray source. For multiple (maximum 3) counterparts, the entries are listed in order of likelihood or assumed relative contribution to the total X-ray flux and are separated by a colon. The abbreviations have the following meanings:
st: normal star (i.e., an unresolved objects showing a stellar absorption spectrum, including late-type stars showing chromospheric emission lines, such as dMe stars). ES: (hot) emission-line star (unresolved objects showing a blue continuum, with or without absorption lines, and unshifted emission lines. Most objects classified ES show typical CV spectra). WD: white dwarf (star showing absorption lines with FWHM>1500km/s). WDA: white dwarf with Balmer lines only. S1: Seyfert 1 galaxy (galaxy with an unresolved nucleus showing a Seyfert-type spectrum with broad (>2000km/s) permitted lines and with M_B_>-23.5). S15..S19: Seyfert galaxy of type 1.5-1.9 NL1: Narrow-line Seyfert 1 galaxy (spectrum showing line ratios typical of Seyfert 1 but with lower FWHM of permitted lines). S2: Seyfert 2 galaxy LI: LINER QSO: quasi-stellar object (unresolved or resolved object with M_B_<-23.5 showing a Seyfert 1 spectrum). BLL: BL Lac object G: (single) galaxy Gin: interacting galaxy pair Gr: radio galaxy GSB: starburst galaxy C: cluster or group of galaxies
The spectral type for stellar sources.
The redshift for extragalactic sources, as determined from the authors' spectra (if not mentioned otherwise in the notes to the published Table 2 and/or in the file ftp://cdsarc.u-strasbg.fr/pub/cats/J/ApJS/117/319/notes.dat.gz).
The Johnson V magnitude of the optical counterpart. With the exception of bright stars for which photometry was available from SIMBAD, V was calculated from the E and O magnitudes of the APM sky survey scans as described by Zickgraf et al. (1997). As the APM scans are known to contain errors, the individual magnitudes should be used with caution. In some cases, only an O or a B magnitude either from the COSMOS UKST database (only field III) or NED existed: in such cases, the B-V color was assumed according to the object type, 0.5 for AGN, 1.0 for galaxies, and, for stars, the color appropriate for the corresponding spectral type.
The B-V color index of the optical counterpart calculated from the E and O magnitudes of the APM sky survey scans. As the APM scans are known to contain errors, the individual colors should be used with caution. In some cases, only an O or a B magnitude either from the COSMOS UKST database (only field III) or NED existed: in such cases, the B-V color was assumed according to the object type, 0.5 for AGN, 1.0 for galaxies, and, for stars, the color appropriate for the corresponding spectral type. In such cases, this field has not been populated.
The XV-Index log f_x/f_V, i.e., the decadic logarithm of the ratio of the X-ray flux and the visual flux, the latter being calculated from the V magnitude according to the relation given by Stocke et al. (1996, ApJS, 76, 813).
The radio flux at 4.85 GHz (6 cm) in mJy, for sources within the declination range 0 < Dec < +75 degrees, from Gregory & Condon (1991, ApJS, 75, 1011).
The alternative designation of the (main) optical counterpart, if known. For stars, the entry numbers in the most common star catalogs are listed. For other objects, the corresponding designations and abbreviations listed in the NED and SIMBAD databases are given. In a few cases of very long designations, the names have been shortened or truncated. Since in all these cases coordinate information is given in the table, this should not result in ambiguities. The full designations can be obtained from the NED. Although in the Remarks NRAO VLA Sky Survey (NVSS) (Condon et al., 1998, CDS Cat. <J/AJ/115/1693>) data are quoted for some sources, no NVSS designations are used since the final version of the NVSS catalog is still listed as "in preparation."
A flag parameter which is set to "R" to indicate that there is a detailed remark in the documentation file at ftp://cdsarc.u-strasbg.fr/pub/cats/J/ApJS/117/319/notes.dat.gz
A flag parameter which is set to "Y" to indicate that the source is in the complete X-ray subsample, i.e., is listed in Table 1 of the published paper, or is set to "N" to indicate that the source is one of the additional sources not part of the complete sample which are listed in Table 2 of the published paper. This parameter was added by the HEASARC when it combined these two tables to make one HEASARC table.
The HEASARC Browse object classification based on the classification and/or spect_type parameter values.