Table description

Column No.Description
1 Sequential number.
2 Master ASAS identification (in the format of hhmmss+ddmm.m) coming from the equatorial coordinates of the object (epoch 2000.0) in the abbreviated form.
3 Right ascension of the object (for epoch 2000.0) [in degrees].
4 Declination of the object (for epoch 2000.0) [in degrees]. Right ascension and declination are given with the accuracy of 0.00001 deg for objects identified with 2MASS sources and with the accuracy of 0.0001 deg for the remaining stars. The latter means that a star is a blend and we are not sure which star of two (or more) objects is variable.
5 Mean V magnitude from ASAS (if V data were available).
6 Mean I magnitude from ASAS (if available).
7 V-I colour index from ASAS (if both V and I were available).
8 J magnitude from 2MASS All-Sky Catalog of Point Sources (Cutri et al. 2003).
9 J-H colour index from the 2MASS catalog.
10 H-K colour index from the 2MASS catalog. The entries in columns 8-10 are given only if a star was identified with a 2MASS source and the photometric quality flag was equal to A, B, C or D.
11 Type of variability. The following types of variability were assigned:
PER       stricly periodic variable with sinusoidal light curve. This category may include Delta Scuti, Beta Cephei, Slowly Pulsating B, Gamma Doradus and other types of variability. However, we did not assign the type of variability as this can be assigned in most cases only with additional information like spectral type.
HADS high-amplitude Delta Scuti star.
RRAB RR Lyrae-type variable of Bailey type ab.
RRC RR Lyrae-type variable of Bailey type c.
CEP Cepheids, including also some RV Tauri-type variable candidates.
EW Eclipsing binary with W UMa-type light curve.
EB Eclipsing binary with Beta Lyrae-type light curve.
EA Eclipsing binary with Algol-type light curve.
MIRA Mira-type variable.
QPER Star with a dominating periodicity, but showing also amplitude and/or phase changes or periodic changes superimposed on the variability on a longer time scale. Stars of this type are commonly designated also as semi-regular (SR) or long-period variables (LPV).
APER star with no well-defined periodicity in light variations.
12 The (quasi)period of variability [in days]. It is given for all periodic and quasiperiodic (QPER) stars.
13 Range of variability in V [in mag].
14 Range of variability in I [in mag].
Note, please, that the range of variability for periodic stars was derived from phase diagrams in which the shape of the light curve was approximated by a truncated Fourier series and the outliers from such a fit were rejected. Unfortunately, this procedure usually removed points in the very deep and narrow minima of eclipsing binaries (mainly of EA type) thus leading to underestimation of derived range. On the other hand, the ranges of variability for stars identified as APER, QPER and MIRA were derived from the original light curves. In this case, the presence of outliers might lead to overestimation of the range of variability.
15 Remarks, notes and cross-identifications. The column contains link 'see' if there is an entry for a given star in this column. The stars were cross-identified with the following sources of variability in this area of the sky:
(1) General Catalogue of Variable Stars (GCVS), e.g. HO Lyr.
(2) New Catalogue of Suspected Variable Stars, including the Supplement (Kazarovets et al., 1998, IBVS 4655). Star numbers from this catalog are preceded by 'NSV'.
(3) ROTSE1 catalog (Akerlof et al., 2000, AJ 119,1901).
(4) Northern Sky Variability Survey (NSVS, Wozniak et al., 2004, AJ 127,2436) red variables (Wozniak et al., 2004, AJ 128,2965) and RR Lyrae stars (Wils et al., 2006, MNRAS 368,1757).
(5) Hungarian-made Automated Telescope Network (HATnet) catalog (Hartman et al., 2004, AJ 128,1761) in field #199. The names from this catalog are preceded by 'HAT199'.