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Date: Wed, 10 Nov 1993 13:31:35 +0000 (WET) From: Fred Ringwald <far@astro.keele.ac.uk> Subject: Cataclysmic Variables from the Palomar-Green survey Dear Mr. Kato: The FSPACE CV Circular 1993.4 (FSPACE NO.5), edited by N.Makiguchi, says that Japanese observers watch these cataclysmic variable stars: SY Cnc (UGZ) DO Dra (UGSS) AH Her (UGZ) T Leo (UGSU) BZ UMa (UG) CH UMa (UGSS) SS UMi (UGSU) PG0943+521 (CV) The last, PG0943+521, especially interests me. The name of this cataclysmic variable (CV) begins with "PG". This means it was found by the Palomar-Green survey (Green, R. F., Schmidt, M., & Liebert, J. 1986, the Astrophysical Journal Supplement, volume 61, page 305). My recent Ph.D. thesis was on these same stars, the CVs found by the Palomar-Green survey. I call them "the PG CVs". Since they were selected by color, and not by any outburst properties, they form a statistically complete sample of CVs, which is useful for studying their physical properties and evolution. What I would like to know is, do you know anyone who observes any of the other PG CVs? The Palomar-Green survey rediscovered many CVs that were already known, including all the stars on the above list, other than PG0943+521. PG0943+521 was discovered for the first time by the Palomar-Green survey, as were several other other CVs. Even with many of the stars that were already known, though they have not been observed often, by professional or by amateur astronomers. These include especially: PG0834+488 = EI UMa PG0859+415 PG0917+342 PG0943+521 PG1000+667 PG1341-079 = HS Vir PG1510+234 PG1524+622 PG1633+115 PG1711+336 = V795 Her PG1717+413 = V825 Her PG2133+115, and PG2337+123 = HX Peg. Little is know of any of these stars' outburst properties, because so few observations of them exist. Al(hr) Type 0027+260 PX And 00 30 05.86 +26 17 25.9 1 15.41 3.51 ecl SW VY 0134+070 AY Psc 01 36 55.52 +07 16 29.2 1 15.41 5.22 ecl NL 0244+104 WX Ari 02521.20 -04 26 06.5 1 15.39 4.38 UG AAVSO 1316+678 13 17 51.88 +67 31 58.5 1 16.02 ? New - CV: 1341-079 HS Vir 13 43 38.51 -08 14 03.9 1 15.76 2.01: DN: 1510? Orbital period unknown (Column 7) Type: ecl = eclipsing PSH = photometric period exceeds spectroscopic period; may have permanent superhumps (Patterson, J., & Richman, H. 1991, PASP, 103, 735) XR = HEAO-1 MC-LASS X-ray source (Silbe=============================================== NON-CVs, from the Palomar-Green Catalog (Green, Schmidt, & Liebert 1986) Most may be hot/cool binaries (see Ferguson, Green sdB 1315-123 13 17 39.5 -12 32 52 5 15.25 sdB 1443+337 CBS 200 14 46 00.4 +33 28 54 5 16.01 COMP DA2 1445+584 14 46 57.20 +58 09 (1986), but reclassified by me, and with new comments: NO HA = sdB with H alpha weak or "missing" (Downes, R. A. 1987, ApJ, 316, 763) VAR HA = variable H alpha line profile ====.2 +15 27 14 2 15.75 5.63 ecl NL 1101+453 AN UMa 11 01 35.2 +45 19 27 2 16.08 1.91 AM AAVSO 1114+187 11 14 26.0 +18 42 24 5 15.22 ? New - CV: 1119+147 SA79-B1 11 19 3 a colon () (Column 4) Position references follow DEC(1950): B Bruch, A. Fischer, F.-J., & Wilmsen, U. 1987, A&AS, 70, 481 M McNaught, R. H. 1986, IBVS, No. 2926 L Lieber Thorstensen et al. 1991, A, 102 272) VY = anti-dwarf nova; NL with unpredictable low states, excluding AM Hers DQ = DQ Her star, with magnetized white dwarf AM = AM Her star, with strongly magnetizBE UMa 11 55 09.8 +49 13 01 5 15.15 Bin 1156-037 11 56 48.3 -03 44 40 5 13.79 sdB 1157+004 11 57 18.1 +00 24 40 5 15.88 DA 1217-067 12 17 23.0 -d Class, with designations of ree, Schmit, & Liebert (1986), but reclassified by me, and with new comments: NO HA= sdB with H alpha weak or "mising" (Downes, R. A. 1
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