Objects found by Mike Collins on UK Nova Patrol Photographs in 1990 Designation Q no. Mag range Date reported Announced on 1950 Position Notes Con Area(s) V386 Cep 1990/4 9.5-11.0 18 Jan 1990 TA EC-382 TAV 2251+61 Object appeared faint in December 1988 and January 1990. Cep 7(17) Identified as bright IR source IRAS 22512+6100 = IRC +60374 = AFGL 2982 = Dearborn 42141. Noguchi et al. (1991b) present JHKL photometry and suggest an S-type classification rather than M3. Details given in The Astronomer, vol.27, no.319, p.149 (1990). Omont et al. (1993) record failure to detect OH maser and CO emissions. Designated V386 Cep on IBVS 4140 (72nd Name-List). GSC-based chart with new designation re-issued and details given on TA EC-951. TASV 0008+47 1990/12 9.3-10.1 16 Feb 1990 TA EC-390 And 32 Object appeared faint in February 1990 and bright in July 1989. Identified as IRAS 00089+4720. Details given in The Astronomer, vol.27, no.323, p.240 (1991). Marsakova et al. (1994) report a periodogram analysis of 134 plates in the Odessa collection which reveals aperiodic variations superimposed on a slow decline in brightness. TASV 0739+15 1990/15 10.3-11.0 24 Feb 1990 TA EC-392 Gem 81 Object appeared bright in mid-February 1990. Identified as IRAS 07392+1527 = Dearborn 13246. Details given in The Astronomer, vol.27, no. 323, p.240 (1991). Marsakova et al. (1994) report a periodogram analysis of 66 plates in the Odessa collection which argues for variations on time scales of a few days. EQ Dra 1990/20 10.0-11.6 3 Mch 1990 TA EC-393 TASV 1924+57 Faint in June 1989 and bright in March 1990. Dra 14 Identified as IRAS 19243+5707. Details given in The Astronomer, vol.27, no.323, p.240 (1991). Analysis by Dietmar Boehme in The Astronomer, vol.29, no.337, p.15 (1992) suggest a SRb-type star with an ephemeris given by JDmax = 2445530 + 380E. Designated as EQ Dra on IBVS 3840 (71st Name-List). Marsakova et al. (1994) report a periodogram analysis of 50 plates in the Odessa collection. NSV 2557 1990/26 8.3-10.8 17 Mch 1990 TA EC-399 0538+12 Faint in March 1990. Ori 78 Identified as NSV 2557 = IRC +10094 = Dearborn 1241 = IRAS 05383+1216, C star found in Two Micron Survey. Epchtein et al., Astron. Astrophys., 227, 82-104 (1990) give IJHKLM photometry but no variability data. Chan and Kwok, Astron. Astrophys., 237, 354-68 (1990) determine optical depth at 11.3 microns and mass loss rate. Details given in The Astronomer, vol.27, no.323, p.240 (1991). Photograph on back cover of TA vol. 28, no. 27 (July 1991) by Azema shows object embedded in lambda Ori nebulosity. Marsakova et al. (1994) report a periodogram analysis of 60 plates in the Odessa collection which suggests a semiregular variation with a period of 317 days. Rudolf (1997) analyses red-sensitive plates of the Sonneberg Sky Patrol. TASV 1913+25 1990/44 10.3-11.3 20 May 1990 TA EC-422 Vul 59 Bright in March 1989. Another carbon star. Identified as IRAS 19131+2507 = Dearborn 17564 = CCS 2714 = Case 449 = BD +25 3762 = Dearborn C star D208. Details given in The Astronomer, vol.27, no.323, p.240 (1991). Rudolf (1994) reports an analysis of 369 red Sonneberg plates showing the star to be semiregular with cycle length increase from 360 days (1963) to 400 days (1993). V336 Vul 1990/45 7.1-10.9? 20 May 1990 TA EC-422 NSV 12178 Bright in March 1989. Identified as NSV 12178 = BV 142 = DHK 6 BD +23 3694 = IRAS 19325+2346 = RAFGL 5398S = IRC +20415 = 1932+23 Dearborn 17894. Discovered by Strohmeier et al. (1956) Vul 59 Rediscovered by Kaiser and described in IBVS 3443. Also studied photographically by Wakuda and Huruhata in Variable Star Bull., No. 7, p. 26 (1988). Lewis et al. (1990) failed to detect this suspect at 1612 MHz. Details given in The Astronomer, vol.27, no.323, p.240 (1991). Designated V336 Vul on IBVS 3840 (71st Name-List) on basis of Japanese study. Omont et al. (1993) record failure to detect OH maser and CO emissions. Lewis and Engels (1995) again fail to detect either water or OH maser line maser emission. NSV 13514 1990/55A 9.8-11.4? 7 Jly 1990 TA EC-428,430 2102+27 Bright in June-July 1989. Identified as NSV 13514 discovered Vul 62 by Lange in September 1925. Object also IRAS 21028+2711 = RAFGL 2700 = IRC+30469. Dearborn 19933 is 10' west of object. Vogt in Astron. J., 78, 389-94 and 443 (1973) classifies the suspect as Sp. M7. Lewis et al. (1990) failed to detect to detect OH maser emission at 1612 MHz and Lewis (1992) reports inability to detect water maser emission at 22 GHz. Dedoch (1995) presents an analysis of 1991-2 visual observations suggesting either a W UMa or delta Sct type variable with a period of 0.148737 day. His finding chart does not clearly identify the variable which is immediately above the gap between the N and S of the label "NSV". V335 Vul 1990/60 10.1-12? 21 Jly 1990 TA EC-440 TAV 1921+24 Bright in August 1989 and August 1990. Identified as C star LD 120 IRAS 19211+2421 = MHalpha 215-33 = CCS 2728 = Case 452 = AS 356. Vul 59 Observations in 1991 suggest JDmax = 2447767 + 336E. Details given in The Astronomer, vol.28, no.332, p.182 (1991). Designated V335 Vul on IBVS 3840 (71st Name-List). Independently discovered by Dahlmark (1993) and designated as LD 120. Dahlmark (1994) provides further details and light curve. Munari et al. (1999a) suggest spectral evidence for a possible carbon symbiotic star and give the identification GSC 2128.0676. Munari et al. (1999b) report a bright outburst in early December 1999 together with spectroscopy showing emission lines. TAV 0042+53 1990/67 9.6-12.5 2 Sep 1990 TA EC-444 Cas 19 Bright in late 1989 and early 1990. Identified as IRAS 00422+5310, a C-rich star. Sivagnanam et al. (1990) fail to detect OH maser lines. Noguchi et al. (1991a) present JHKL and 3.1 micron (SiC) photometry on 1989 October 8. Rudolf (1993) analyses 300 Sonneberg plates to reveal semiregular variation with cycle lengths of 420 days (1971-86) and 456 days (from 1988). V451 Cep 1990/69 9.8-10.8 14 Sep 1990 TA EC-453 TAV 2230+58 Faint in September 1990 and October 1989. Cep 17 Identified as IRAS 22305+5821 = CCS 253 = Case 253 = MSB 72 = IRC +60358. Carbon star (Sp. N) close to W Cep field. Independently found to be variable by Hipparcos with designation HIP 111250, range 10.27-11.12 and type LB. Named V451 Cep in 74th Name-List. EO Dra 1990/77 10.8-13? 5 Oct 1990 TA EC-468 NSV 10701 Bright in early September 1989 and late September 1990. 1819+50 Identified as NSV 10701 = IRC +50278 = IRAS 18196+5030. Dra (25) IRAS LRS class suggests an O-rich star. Vogt (1973) assigns a spectral type of M9 as opposed to the G0 given in the IRC. Stephenson (1986) assigns Sp M7. Finding chart by Wyckoff and Wehinger (1974) confirms the identity but does not provide a sequence. Guide Star Catalog records a possible maximum suggesting an ephemeris JDmax = 2447777 + 386E. First well-recorded max reported by Swedish observers in early October 1991. Details published in The Astronomer, vol.28, no.332, p.182 (1991). Designated EO Dra on IBVS 3840 (71st Name-List). Rudolf (1994) reports an analysis of 422 blue Sonneberg Schmidt plates from the years 1982-91 confirming the Mira type with a period of 390 days. TASV 0234+38 1990/79 9.6-10.3 7 Oct 1990 TA EC-473 And 49(35) Faint in late September 1990. Identified as IRAS 02341+3845 = IRC +40046 in UY And field. The suspect appears on AAVSO (d) and (e) charts and is given a preliminary magnitude of 9.8. TAV 1933+53 1990/80 10.3-11.4 8 Oct 1990 TA EC-482 Cyg 14 Bright in March 1990 fading by June, still faint in September. Identified as IRAS 19331+5346 = Dearborn 37467 TAV 0033+59 1990/87 10.3-11.9 6 Nov 1990 TA EC-459 Cas 19(9) Faint in October 1990. Identification with B-star LS I +59 48 = DP 24 in Dolidze and Ponomareva, Astron. Zh., 42, 205-7 (1965). DP finder agrees with position of suspect. Rapid fade in December 1990 reported on TA EC-469 and 471. Spectral evidence for shell episode reported on TA EC-609. Studied by Marquez-Limon et al. (1992) as candidate young Orion population member. Star appears in NSV Supplement 1.0 as NSV 15133. TAV 0346+38 1990/88 10.3-11.4 7 Nov 1990 TA EC-487 Per 51 Faint in October 1990. Identified as IRAS 03467+3838 = Dearborn 10109 = CCS 158 in XY Per field. TASV 0534+10 1990/92 8.0-8.8 8 Dec 1990 TA EC-523 Ori 78 Bright in late November 1990. Identified as IRAS 05342+1025 = IRC +10092. V503 Ori is 6' north of suspect. TASV 0358+57 1990/95 10.0-10.6 14 Dec 1990 TA EC-528 Cam 22 Bright in early December 1990. Identified as IRAS 03582+5718 = Dearborn 27830. No variability pattern obvious. REFERENCES Dahlmark, L. 1993, Inf. Bull. Variable Stars, 3855 Dahlmark, L. 1994, J. Am. Assoc. Variable Star Obs., 23, 34-63 Dedoch, A. 1995, Contrib. N. Copernicus Obs. Planet. Brno, 31, 90-2 Lewis, B.M. et al. 1990, Astrophys. J., 362, 634-51 Lewis, B.M. 1992, Astrophys. J., 396, 251-66 Lewis, B.M., Engels, D. 1995, Mon. Not. R. Astron. Soc., 274, 439-46 Marquez-Limon, A. et al. 1992, Astron. Astrophys. Suppl., 95, 391-6 Marsakova, V.I. et al. 1994, Odessa Astron. Publ., 7, 70-5 Munari, U. et al. 1999a, Inf. Bull. Variable Stars, 4668 Munari, U. et al. 1999b, Int. Astron. Union Circ., 7329 Noguchi, N. et al. 1991a, Publ. Astron. Soc. Japan, 43, 275-310 Noguchi, N. et al. 1991b, Publ. Astron. Soc. Japan, 43, 311-43 Omont, A. et al. 1993, Astron. Astrophys., 267, 515-48 Rudolf, E. 1993, Mitt. Veranderliche Sterne, 12, 165 (German) Rudolf, E. 1994, Mitt. Veranderliche Sterne, 12, 186-7 (German) Rudolf, E. 1997, BAV Rundbrief, 46, 62 (German) Sivagnanam, P. et al. 1990, Astron. Astrophys., 233, 112-20 Stephenson, C.B. 1986, Astrophys. J., 301, 927-37 Vogt, S.S. 1973, Astron. J., 78, 389- Wyckoff, S., Wehinger, P. 1974, Publ. Astron. Soc. Pacific, 86, 464-9 VSTAT90.TXT December 1999