RASSASASEB - RASS/All-Sky Automated Survey Eclipsing Binaries Catalog
The authors expect that only 1.4% (i.e., 12 out of 836) of the matches between the ASAS eclipsing binary and RASS sources will be false given their maximum angular separation criterion of 50 arcseconds. This Browse table excludes 29 contact binaries for which the separate distance estimates made by the authors using the source V-band and I-band magnitudes differed by more than 20%, and hence contains 807 (836 - 29) eclipsing and X-ray emitting binary systems.
Complete information on ASAS and its freely accessible data are available at the ASAS web site: http://www.astrouw.edu.pl/asas/.
Coronal activity from the ASAS eclipsing binaries. Szczygiel D.M., Socrates A., Paczynski B., Pojmanski G., Pilecki B. <Acta Astron., 58, 405-418 (2008)> =2008AcA....58..405S (SIMBAD/NED BibCode)
The ASAS source identification in the recommended format using the truncated J2000.0 equatorial coordinates , e.g., 'ASAS JHHMMSS+DDMM.m'.
The RASS source identification in the recommended format using the truncated J2000.0 equatorial coordinates , e.g., '1RXS JHHMMSS.s+DDMMSS'.
The Right Ascension of the RASS Source in the selected equinox. This was created by the HEASARC from the RASS name and hence has a precision of 0.1 seconds of time.
The Declination of the RASS Source in the selected equinox. This was created by the HEASARC from the RASS name and hence has a precision of 1 arcsecond.
The Galactic Longitude of the RASS Source.
The Galactic Latitude of the RASS Source.
The angular separation between the ASAS and RASS source positions, in arcseconds.
The orbital period P of the binary, in days.
The heliocentric date/time of the epoch of minimum light of the eclipsing binary. This was given as a 'modified' Julian Date (HJD - 2450000), where HJD is the heliocentric Julian Date, to a precision of 0.001 days, i.e., of about 1.4 minutes. Given this level of precision, and remembering that HJD and the Barycentric Julian Date (BJD) differ by no more than +/- 4 seconds, this date/time is thus essentially barycentric also.
The V-Band brightness at maximum light, expressed as an apparent magnitude.
The I-Band brightness at maximum light, expressed as an apparent magnitude.
The distance D to the eclipsing binary, in parsecs. This was calculated as discussed in Section 4 of the reference paper using a main-sequence fit for the detached and semi-detached systems (treating them as single stars) from Hawley et al. (1999, AJ, 117, 1341) assuming solar metallicity, and a fit from Rucinski and Duerbeck (1997, PASP, 109, 1340) for the contact binaries.
The logarithm of the bolometric luminosity of the binary system, in erg/s, based on the observed magnitude, the calculated distance and an adopted bolometric correction, as discussed in Section 4.1 of the reference paper.
The hardness ratio HR = (H-S)/(H+S) of the RASS X-ray source, where H is the counts in the 0.5-2.0 keV energy range and S is the counts in the 0.1-0.4 keV energy range.
The uncertainty in the hardness ratio.
The ROSAT All-Sky Survey X-ray source count rate, CR, in counts per second (ct/s).
The uncertainty in the RASS X-ray source count rate, in counts per second (ct/s).
The logarithm of the X-ray luminosity of the RASS source. in erg/s, based on the observed count rate, CR, and hardness ratio HR of the X-ray source, and the estimated distance D in the usual manner for RASS sources:
fX = CR * (5.30*HR + 8.7) * 1.0E-12 LX = 1.20E38 * D2 * fX
The logarithm of the Rossby Number for the eclipsing binary log R0 = log (Prot/tauC), where the rotational period Prot is assumed to be equal to the orbital period P, i.e., the system is assumed to be tidally locked, for those binaries with orbital periods less than 10 days, and tauC is the convective turnover time of the primary star and is calculated as discussed in Section 6 of the reference paper.
Another identification for the binary from the literature, mainly from the GCVS.
The ASAS classification of the variability type of the binary, where EC = contact (W UMa type), ESD = semi-detached (Algol), and ED = detached binary.
The HEASARC Browse object classification, based on the binary_type, where we have called detached (ED) systems "RS CVn systems". While it is true that most RS CVn binaries are detached, a few are semi-detached, so that there is not a precise one-to-one match between these classes.