******************************************************** * * * DESCRIPTION OF TABLE HEADINGS AND OF ABBREVIATIONS * * * * (ONLINE VERSION) * * * ******************************************************** Object Name: Wherever possible, the designation of the object given in the General Catalogue of Variable Stars is used here. Altern.Name: is a frequently used alternative name. Further alternative designations are given in the "Who's Who ?" section. Coordinates: First row right ascension (J2000) in hrs min sec Second row declination (J2000) in deg ' " The coordinates are given in the following format: right ascension: HH MM SS.S declination : DDD MM SS A In the declination field, "A" is the accuracy of the coordinates in seconds of arc. If "A" > 9" or if the accuracy of the coordinates is not known, the "A"-field is left blank. If "A" = P, the star has a high proper motion and the coordinates refer to the epoch 2000.0. Type: (first and second row), the object type is coarsely characterised using the following abbreviations: AC = AM CVn star, spectrum devoid of hydrogen lines, subtype of NL AM = polar = AM Her system, subtype of NL, contains a synchronously or nearly synchronously rotating, magnetized white dwarf AS = subtype of AM, with a slowly asynchronously rotating, magnetized white dwarf AS = atoll source, subtype of the LMXBs BD = secondary star is a brown dwarf BH = black hole candidate, subtype of the LMXBs BO = LMXB, X-ray burster with coherent burst oscillations at the neutron star spin period CP = coherent pulsator, contains a coherently pulsating white dwarf or subdwarf CV = cataclysmic variable of unspecified subtype DA = non-magnetic direct accretor DC = source with an accretion disc corona, subtype of the LMXBs DD = DS system consisting of two degenerate components DN = dwarf nova DQ = DQ Her star, contains a non-synchronously rotating, magnetized white dwarf; usually not seen in X-rays DS = detached system EC = contains a pulsating sdB star of the V361 Hya type (EC 14026-2647 type) with short-period pulsations EG = extragalactic source EL = EL CVn star = detached, eclipsing, possibly post-common envelope/pre-CV binary consisting of a low-mass (pre-)He-WD and an A-type companion ER = ER UMa star = SU UMa star with an extremely short supercycle GC = source in a globular cluster GP = contains a sdB-star of V1093 Her type with long-period g-mode pulsations GW = contains a pulsating white dwarf of the GW Vir = PG 1159-035 type IP = intermediate polar, shows coherent X-ray period from a non-synchronously spinning, magnetized white dwarf; usually a strong X-ray source LA = low accretion rate polar (LARP), i.e. a somewhat detached magnetic CV/pre-CV LI = low-accretion rate intermediate polar (LARIP), i.e. a somewhat detached magnetic CV/pre-CV MQ = microquasar, source of relativistic jets N = classical nova Na = fast nova (decline from max. by 3 mag. in less than about 100 days) Nb = slow nova (decline from max. by 3 mag. in more than about 100 days) Nc = extremely slow nova (typical time scale of the decline from maximum: decades) NL = nova-like variable Nr = recurrent nova NS = system showing negative (nodal) superhumps PN = central star of a planetary nebula PW = precessing white dwarf QN = quiescent neutron star LMXB RP = primary is also seen as a radio pulsar RS = system shows RS CVn-like chromospheric activity SC = sub-stellar companion SH = non-SU UMa star showing either permanent or transient positive (apsidal) superhumps SS = supersoft X-ray source; in CVs with stationary hydrogen burning on the white dwarf SU = SU UMa star, subtype of DN SW = SW Sex star, subtype of NL UG = dwarf nova of either U Gem or SS Cyg subtype UL = ultra-luminous X-ray source UX = UX UMa star, subtype of NL VY = VY Scl star (anti dwarf nova), subtype of NL WZ = WZ Sge star = SU UMa star with an extremely long supercycle XB = X-ray burst source XP = X-ray pulsar XT = transient X-ray source ZC = Z Cam star, subtype of DN ZS = Z-source, subtype of the LMXBs ZZ = white dwarf shows ZZ Ceti-type pulsations Mag1, Mag3 Mag2, Mag4: apparent V magnitude (B, b, g, I, J, K, p, R, U, w = "white light" magnitude) if followed respectively by B, b, g, I, J, K, p, R, U, w) with the following meaning: Mag1 = maximum brightness of novae (N, Na, Nb, Nc, Nr) in minimum DN (UG, ZC, SU) in minimum NL (UX, AC) in normal state NL (DQ, IP, AM, VY) in high state SS in high state XT in quiescence DS outside eclipse Mag2 = minimum brightness, in case of eclipses magn. at mideclipse, of novae (N, Na, Nb, Nc, Nr) in minimum DN (UG, ZC, SU) in minimum NL (UX, AC) in normal state NL (DQ, IP, AM, VY) in high state SS in high state XT in quiescence DS Mag3 = maximum brightness of novae (N, Na, Nb, Nc, Nr) in outburst DN (UG, ZC) in outburst DN (SU) in normal outburst DN (WZ) in echo outburst NL (AM, VY) in low state SS in low state XL (XB, XT) in outburst = brightness of NL (DQ, IP) in low state Mag4 = brightness of novae (N, Na, Nb, Nc, Nr) in DN outbursts ZC in standstill SU in superoutburst WZ in superoutburst NL (DQ, IP) in flaring state = minimum brightness of NL (AM, VY) in low state SS in low state T1: for DN (UG,ZC), the typical time interval (in days) between two subsequent outbursts for DN (SU), the typical time interval (in days) between two subsequent normal outbursts for XT, the typical time interval (in days) between two subsequent X-ray active states T2: for DN (SU), the typical time interval (in days) between two subsequent superoutbursts Lx/Lo: for LMXBs, the ratio of X-ray to optical luminosity Orb.Per.: orbital period (in days), in case of object type SU or SH: if followed by *, the orbital period has been estimated from the known superhump period using the empirical relation given by Stolz & Schoembs (1984, A&A 132, 187). 2. Per.: second period, in case of object type N, Na, Nb, Nc, Nr: photometric period (in days), if it is different from the spectroscopic one. DQ or IP: photometric period (in days), if it is different from the spectroscopic one. AM: polarization period (in days) = spin period of the white dwarf, if it is different from the presumed orbital period (subtype AS). SU: superhump period (in days), wherever possible, at the beginning of a superoutburst. SH: photometric period (in days), superhump period of either permanent or transient superhumps if 2. Per > Orb.Per. NS: photometric period (in days), period of either permanent or transient negative superhumps if 2. Per. < Orb.Per. DS: spin period (in seconds) of the white dwarf (or neutron star). 3. Per. 4. Per.: additional periods in the system (in seconds), in case of object type CP: 3. Per. = period of coherent pulsation, (transient if followed by T). 4. Per. = second period of coherent pulsation, (transient if followed by T). DQ: 3. Per. = spin period of the white dwarf. 4. Per. = additional period, presumably due to reprocessed X-Rays. IP: 3. Per. = spin period of the white dwarf, usually detected in X-Rays. 4. Per. = additional period, usually seen in the optical and presumably due to reprocessed X-Rays. RP: 3. Per. = spin period of the radio pulsar. SW: 3. Per. = probably the spin period of the white dwarf. XP: 3. Per. = pulse period of the pulsar. 4. Per. = optical period, presumably due to reprocessed X-Rays. ZZ: 3. Per. = period of ZZ Ceti-type non-radial pulsation of the WD. 4. Per. = period of ZZ Ceti-type non-radial pulsation of the WD. EB: indicates the occurrence of eclipses if blank no eclipses observed if 1 1 eclipse per orbital revolution observed (Note that in cataclysmic binaries and LMXBs the eclipsed "object" is either the accretion disc and/or the hot spot or, in case of AM Her stars, the white dwarf or the matter stream.) if 2 2 eclipses per orbital revolution observed (Note that in cataclysmic binaries the two eclipsed "objects" are the white dwarf and the hot spot or, in case of AM Her stars, the white dwarf and the matter stream.) if D periodic eclipse-like dips are observed (typically in the X-ray light curves of LMXBs) SB: type of spectroscopic binary if 1 single-line spectroscopic binary if 2 double-line spectroscopic binary Spectr2: spectral type of the secondary Spectr1: spectral type of the primary the number to the right of the slash indicates the luminosity class , i.e. I = 1 II = 2 III = 3 IV = 4 V = 5 VI = 6 e: first row eccentricity of the orbit second row the corresponding error M1/M2: first row mass ratio M1/M2 second row the corresponding error Incl: first row orbital inclination (in degrees) second row the corresponding error M1: first row mass of the primary (in solar masses) second row the corresponding error R1: first row radius of the primary (in solar radii) second row the corresponding error M2: first row mass of the secondary (in solar masses) second row the corresponding error R2: first row radius of the secondary (in solar radii) second row the corresponding error Uncertain values are followed by a colon.