Collinder 261 Chandra X-Ray Source Optical Counterparts Catalog

Collinder 261 Chandra X-Ray Source Optical Counterparts Catalog CR261OID ivo://nasa.heasarc/cr261oid NASA/GSFC HEASARC Vats et al. 2026-10-09 NASA/GSFC HEASARC help desk heasarc-vo at athena.gsfc.nasa.gov Survey Source This table contains some of the results from the first X-ray study of Collinder 261 (Cr 261), which at an age of 7 Gyr is one of the oldest open clusters known in the Galaxy. This observation with the Chandra X-Ray Observatory was aimed at uncovering the close interacting binaries in Cr 261, and reached a limiting X-ray luminosity of LX ~ 4 x 1029 erg s-1 (0.3-7 keV) for stars in the cluster. The authors detected 107 sources within the cluster half-mass radius rh, and they estimate that among the sources with LX >~ 1030 erg s-1, about 26 are associated with the cluster. They identify a mix of active binaries and candidate active binaries, candidate cataclysmic variables, and stars that have "straggled" from the main locus of CR 261 in the color-magnitude diagram. Based on a deep optical source catalog of the field, the authors estimate that Cr 261 has an approximate mass of 6500 Msun, roughly the same as the old open cluster NGC 6791. The X-ray emissivity of Cr 261 is similar to that of other old open clusters, supporting the trend that they are more luminous in X-rays per unit mass than old populations of higher (globular clusters) and lower (the local neighborhood) stellar density. This implies that the dynamical destruction of binaries in the densest environments is not solely responsible for the observed differences in X-ray emissivity. Cr 261 was observed with the Advanced CCD Imaging Spectrometer (ACIS) on board Chandra starting 2009 November 9 14:50 UTC, for a total exposure time of 53.8 ks (ObsID 11308). The observation was made in Very Faint, Timed exposure mode, with a single frame exposure time of 3.2 s. Kharchenko et al. (2013, A&A, 558, A53) estimate that the radius of Cr 261 is ~ 14.1 arcminutes. This is considerably larger than a single ACIS chip (8 4 x 8 4 arcminute2) and therefore the authors placed the center of the cluster (J2000.0 RA = 12h 38m 06.0s, Dec = -68o 22' 01" according to Kharchenko et al. 2013) close to the I3 aimpoint so that a larger contiguous part of the cluster could be imaged (see Figure 1 in the reference paper). The CCDs used were I0, I1, I2, and I3 from the ACIS-I array, and S2 and S3 from the ACIS-S array. The authors limited the X-ray analysis to the data from chips I0, I1, I2, and I3. The S2 and S3 chips lie far from the I3 aimpoint, giving rise to large positional errors on any sources detected on them. Such large errors make it hard to identify optical counterparts, and thus to classify the sources. The authors retrieved optical images of Cr 261 in the B and V bands from the ESO public archive. These data were taken as part of the ESO Imaging Survey (EIS; program ID 164.O-0561). The observations of Cr 261 were made using the Wide Field Imager (WFI), mounted on the 2.2 m MPG/ESO telescope at La Silla, Chile. After correcting the X-ray source positions for the (almost negligible) boresight correction (0.06 =/- 0.07 arcseconds in RA and 0.09 +/- 0.08 arcseconds in Dec), the authors matched their X-ray source list with the entire optical source list, using 95% match radii. For 89 unique X-ray sources, they found 124 optical matches; of the latter, 104 are present in both the V and B images, while for 20 there is only a V or B detection. The authors also inspected the area around each X-ray source in the WFI images by eye, and discovered that five more X-ray sources have candidate optical counterparts that are saturated and therefore missing from their optical catalog. Finally, they added to the list of candidate counterparts six optical sources that lay just outside the 95% match radius, but inside the 3-sigma radius. In total, 98 of the 151 unique X-ray sources were thus matched to one or more optical sources. This HEASARC table contains the list of the 135 optical counterparts to 98 of the 151 X-ray sources from Table 2 of the reference paper. Information about the 151 X-ray sources is available in the HEASARC table CR261CXO (based on Table 1 of the reference paper) to which this current table has links. This table was created by the HEASARC in June 2017 primarily based upon the machine-readable version of Table 2 from the reference paper, the catalog of optical counterparts to Chandra sources in Cr 261, that was obtained from the ApJ web site. The information on the X-ray source positions was taken from the machine-readable version of Table 1 from the reference paper that was also obtained from the ApJ web site. This is a service provided by NASA HEASARC . 2017ApJ...837..130V https://heasarc.gsfc.nasa.gov/W3Browse/all/cr261oid.html Catalog Research served-by HEASARC TAP https://heasarc.gsfc.nasa.gov/xamin/vo/cone?showoffsets&table=cr261oid& GET text/xml 180 99999 true 189.646754 -68.5129 0.0166666666666667 https://heasarc.gsfc.nasa.gov/xamin/vo/tap https://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=cr261oid GET text/xml https://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_cr261oid&Action=More+Options&Action=Parameter+Search&ConeAdd=1 CHANDRA 0.0166666666666667 X-ray public cr261oid Collinder 261 Chandra X-Ray Source Optical Counterparts Catalog name Chandra Source Designation meta.id;meta.main char nullable source_number Sequential Identification Number for Each Source in the Catalog meta.id;src short nullable ra Chandra Right Ascension degree pos.eq.ra;meta.main double nullable dec Chandra Declination degree pos.eq.dec;meta.main double nullable optical_id Optical Identifier meta.id.cross char nullable off_set Distance Between X-Ray and its Optical Counterpart arcsec pos.angDistance;em.X-ray;em.opt double nullable vmag V Band Magnitude mag phot.mag;em.opt.V double nullable bv_color The (B-V) Color mag phot.color;em.opt.B;em.opt.V double nullable lx Unabsorbed 0.3-7 keV X-Ray Luminosity erg/s phys.luminosity;em.X-ray double nullable log_fx_over_fv Logarithm of the Ratio of X-Ray to V Band Fluxes phot.flux;em.X-ray;em.opt.V;arith.ratio double nullable broad_type Broad Classification src.class char nullable "__x_ra_dec" System unit vector column double nullable "__y_ra_dec" System unit vector column double nullable "__z_ra_dec" System unit vector column double nullable "__row" System index column char nullable optical_id_flag Flag [ac] Indicates Note Concerning Optical Counterpart meta.code;em.opt char nullable var_type Mazur et al. 1995 Variable Type src.class char nullable mazur_source_number Mazur et al. 1995 Short-Period Binary Identifier meta.id.cross char nullable bii chandra Galactic Latitude degree pos.galactic.lat double nullable lii Chandra Galactic Longitude degree pos.galactic.lon double nullable orbital_period Period of Short-Period Binary d time.period double nullable class Browse Object Classification src.class short nullable vmag_flag Flag [bd] Indicates Note Concerning Magnitude meta.code;phot.mag;em.opt.V char nullable bv_color_flag Flag [de] Indicates Note Concerning B-V Color meta.code;phot.color;em.opt.B;em.opt.V char nullable orbital_period_flag Flag [?] Indicates Uncertainty in Period meta.code;time.period char nullable