RASSASASPV - All-Sky Automatic Survey (ASAS) Photometry of ROSAT All-Sky Survey Sources
The catalog includes 1,936 stars (1,233 new) considered to be variable due to presence of spots (rotationally variable), 127 detached eclipsing binary stars (33 new), 124 contact binaries (11 new), 96 eclipsing stars with deformed components (19 new), 13 ellipsoidal variables (4 new), 5 miscellaneous variables and one pulsating RR Lyr type star (blended with an eclipsing binary). More than 70% of the new variable stars have amplitudes smaller than 0.1 magnitudes, but for the star ASAS 063656-0521.0 the authors have found the largest known amplitude of brightness variations due to the presence of spots (up to Delta V = 0.8 magnitudes).
ASAS photometry of ROSAT sources. I. Periodic variable stars coincident with bright sources from the ROSAT All Sky Survey. Kiraga M. <Acta Astron., 62, 67-95 (2012)> =2012AcA....62...67K
The ASAS source designation, viz., 'ASAS Jhhmmss+ddmm.m'.
The Right Ascension of the ASAS star in the specified equinox. This was not explicitly given in the original table, but was constructed by the HEASARC from the positional part of the ASAS name. The precision is thus 1 second of time.
The Declination of the ASAS star in the specified equinox. This was not explicitly given in the original table, but was constructed by the HEASARC from the positional part of the ASAS name. The precision is thus 0.1 arcminutes.
The Galactic Longitude of the ASAS star.
The Galactic Latitude of the ASAS star.
The angular distance Between the formal ASAS position and the related object from the Simbad database, in arcseconds. Note that 1 pixel of the ASAS detector = 14 arcseconds.
The Simbad designation of the star.
The Simbad object type of the star. See http://simbad.u-strasbg.fr/simbad/sim-display?data=otypes for details on the Simbad classification.
The Simbad proper motion of the star in the Right Ascension direction, in milliarcseconds per year (mas/year).
The Simbad proper motion of the star in the Declination direction, in milliarcseconds per year (mas/year).
The Simbad heliocentric parallax of the star, in milliarcseconds.
The Simbad radial velocity of the star, in km/s.
This parameter is set to '<' if the corresponding parameter value is an upper limit rather than a measured value.
The equivalent width of the Lithium line at 6707 Angstrom, in Angstroms.
This parameter is set to '?' if the corresponding parameter value is considered to be uncertain.
This parameter is set to '<' if the corresponding parameter value is an upper limit rather than a measured value, or set to '>' if the corresponding parameter value is a lower limit rather than a measured value.
The Simbad projected rotational velocity (v sin i) of the star, in km/s.
This parameter can contain a caveat about the Simbad projected rotational velocity, with the following possible non-blank values:
a = there are substantial differences in v sin i values found in literature b = data about v sin i are probably related to a companion star ? = considered uncertain
This parameter can contain a caveat about the presence of visual companions to the ASAS star, with the following possible non-blank values:
- = no known visual companion b = blended with much fainter star or stars (information based on visual inspection of DSS frames - usually DSS-2-red) B = blended with a star or stars of comparable brightness (information based on visual inspection of DSS frames - usually DSS-2-red) c = close visual companion (visual binary) much fainter than the primary star (information based on SIMBAD database or literature) C = close visual companion of comparable brightness (information based on SIMBAD database or literature)
This parameter can contain a caveat about the presence of close or spectroscopic companions to the ASAS star, with the following possible non-blank values:
p = photometry may indicate a close companion P = definitely eclipsing binary (based on photometric data) SB1 = spectroscopic binary (single lined) SB2 = spectroscopic binary (double lined) SB3 = triple spectroscopic systems SB4 = quadruple spectroscopic systems ? = there is no data about spectroscopic variability (no radial velocity measurement or single radial velocity measurement, no spectroscopic lines of secondary star) and there is no photometric indication of close companion no = radial velocity measurements indicate constant radial velocity (no close companion star detected) C = composite spectrum of two or more stars, but without noticeable changes in the radial velocity
The Simbad B magnitude of the ASAS star.
The Simbad V magnitude of the ASAS star.
The Simbad MK spectral type of the ASAS star.
The number of ASAS observations of the star in the I-band.
The ASAS mean magnitude of the star in the I-band.
The dispersion of the ASAS I-band measurements, in magnitudes.
The number of ASAS observations of the star in the V-band.
The ASAS mean magnitude of the star in the V-band.
The dispersion of the ASAS V-band measurements, in magnitudes.
The adopted bolometric correction for the I-band magnitude of the star. This is based on the (V-I) color (calculated from the mean I- and V-band magnitudes) using a fit to atmospheric models presented by Bessel et al. (1998, A&38;A, 333, 231) of the form BCI = -0.08 + 1.86(V-I)- 1.33(V-I)2 + 0.251(V-I)3 for values of (V-I) in the range of 0 to 1.), and a slightly changed formula given by Reid and Gilmore (1984, MNRAS, 206, 19) for values of (V-I) in the range of 1.5 to 4.6: BCI =-0.31(V-I) + 1.03. The value of the free parameter is changed from 1.05 to 1.03 to obtain continuity with the formula for smaller values of (V-I). There are 5 stars without V-band measurements and 6 stars without I-band measurements.
The ROSAT Bright Source Catalog count rate of the associated X-ray source in the 0.1-2.0 keV band, in counts per second (ct/s).
The uncertainty in the ROSAT Bright Source Catalog count rate of the associated X-ray source in the 0.1-2.0 keV band, in counts per second (ct/s).
The ROSAT Bright Source Catalog hardness ratio 1 (HR1), where HR1 = (H-S)/(H+S), and H and S are the counts in the 0.5-2 keV and 0.1-0.4 keV bands, respectively.
The uncertainty in the ROSAT Bright Source Catalog hardness ratio 1 (HR1).
The logarithm of the ratio of the X-ray to bolometric luminosity of the source, Rx. A conversion from the count ratio and HR1 index to the flux in the 0.1-2.4 keV photon energy range is given by Schmitt et al. (1995, ApJ, 450, 392): Fx = (5.31HR1 + 8.31) * 10-12 * CR. Here Fx is expressed in ergs/cm2/s and CR is the count rate in counts per second listed in the ROSAT catalog. This formula was derived for X-ray coronal emission, but the authors adopted it for all of the stars in this catalog. The value of Rx is calculated as Fx/Fbol where Fbol was obtained from the mean I magnitude, the bolometric correction BCI , and the assumption that the solar absolute bolometric magnitude is equal to 4.75.
The uncertainty in the logarithm of the ratio of the X-ray to bolometric luminosity of the source, Rx.
The adopted period for the variability of the ASAS source, in days.
The lower limit for the maximum amplitude of the I-band variability of the ASAS source, in magnitudes.
The lower limit for the maximum amplitude of the V-band variability of the ASAS source, in magnitudes. The amplitudes of some variable stars (especially eclipsing variables) may be underestimated due to the rejection of extreme data points.
Information about the photometric variability type of the ASAS source, as follows:
ED = detached eclipsing binary (127 stars) EB = close eclipsing binary with deformed component, and unequal depths of eclipses (96 stars) EC = contact eclipsing binary (124 stars) Ell = variability due to the deformation of a star in a close binary system (13 stars) rot = rotational variability due to the presence of spots (1936 stars) puls = variability due to stellar pulsations (1 star) msc = the variability is difficult to interpret (5 stars)
This field can contain the authors' remarks and data from the literature about particular objects. Information from different sources is separated by semicolons and may include:
PACVS = period from ASAS Catalog of Variable Stars Pphot = photometric period found in the literature (i.e., from other sources then ACVS) n(vrad) = number of radial velocity measurements in cited paper sig(vrad) = dispersion of radial velocity measurements given in cited paper Porb = spectroscopic orbital period (with K1 and K2 radial velocity semiamplitudes when available) RS = RS CVn type variable star, i.e., a coronally active evolved star in a close binary system RS? = probably an RS CVn type star (based on photometric behavior and X-ray data), but its binarity should be confirmed EW Li line = equivalent width of Li line at 6707 Angstrom vis bin = visual binary star with a given separation and luminosity contrast given by the difference in magnitudes at given band, or measured flux ratio at given band F03 = star is listed in the catalog of Fuhrmeister and Schmitt (2003, A&A, 403, 247) and has variable X-ray emissionThe full version of the references that are mentioned in this field is available at http://cdsarc.u-strasbg.fr/ftp/cats/J_AcA/62/67/refs.dat.
The HEASARC Browse object classification of the star based on its spectral type.