Objects found by Mike Collins on UK Nova Patrol Photographs in 1995 Designation Q no. Mag range Date reported Announced on 1950 Position or Notes J2000 Position Con Area(s) 1910+47 1995/004 11.0-11.7 4 Jan 1995 Cyg/Lyr 26 Object appeared bright in August and September 1991. Identified as IRAS 19103+4740. 2118+48 1995/007 10.9-11.5 13 Jan 1995 Cyg 29 Object appeared bright in December 1988 and possibly again in November 1990. Identified as IRAS 21181+4855 = IRC +50373. NSV 438 1995/008 11.3-(12.3 17 Jan 1995 0110+62 Object faded in early 1991 and late 1994. Identified as Cas 10 NSV 438 = IRC +60041 = IRAS 01105+6241. Bachiller et al. (1997) study CN line emission from envelope. 0618+13 1995/009 9.4-10.3 23 Jan 1995 Ori 79 Object faint in 1993 October and December 1994. Identified as IRAS 06182+1355 and BD +13 1212 with spectral type M3. Bowers (1975 and 1981) and Sivagnanam et al. (1990) failed to detect OH maser lines. TASV J0752+133 1995/015 10.8-11.6 31 Jan 1995 TA EC-1092 0750+13 Object faint at the end of December 1994. Identified as Gem 81 IRAS 07500+1330. Faint again in April 1996 and found to be GSC 0791.1215 at V magnitude 11.59. Independently discovered by Kesao Takamizawa and designated TmzV 382. Takamizawa records a photographic magnitude range 11.2-12.2 and SR: type variation. 0408+58 1995/021 11.7-(12.3 17 Feb 1995 Cam 23 Object appeared bright in early February 1995. Four previous maxima suggest a period of approx. 350 days. Identified as IRAS 04081+5832. 0704+24 1995/047 10.8-(12.1 27 Apr 1995 Gem 67 Object appeared bright in late February 1995 but was not detected until April 1995. A previous brightening occurred in late 1991. Identified as IRAS 07045+2418. NSV 674 1995/052 10.4-11.3 12 May 1995 0154+63 Object appeared bright in September 1992 and again in early Cas 10 May 1995. Identified as IRAS 01546+6349 = Dearborn 25054 = GSC 4040.0216 (V=10.96). The suspect may also be NSV 674, found by Romano in 1960 and designated GR 74, but this object was recorded as white- yellowish with fainter range (13.2-14.3). Romano's chart requires some imagination but the identification seems likely. NSV 9817 1995/070 11.1-12.1 13 Jul 1995 1750+35 Object appeared bright in early July 1995. Identified as Her 41 NSV 9817 discovered by Otto Morgenroth in 1934. Also found to be IRAS 17509+3539. 1931+16 1995/071 10.7-12.3 17 Jul 1995 Sge/Aql 75 Object appeared bright in late June 1995. Archived film reveals only modest variation, no other obvious brightenings. Identified as IRAS 19314+1619. 1930+59 1995/072 10.9-(11.8 19 Jul 1995 Dra 14 Object appeared bright at end of June 1995. Also bright in October 1989, May 1991, and March 1992. Identified as IRAS 19300+5913 = GSC 3933.0464. Subsequently discovered by Lennart Dahlmark and designated LD 284. NSV 362 1995/106 9.9-10.6 12 Nov 1995 0056+51 Object appeared faint in September 1995. Identified as BV 2 = BD +51 206 = CSV 5883 = NSV 362 = IRAS 00568+5137 = Dearborn 23949 = GSC 3275.0009 found by Strohmeier and first reported in 1955. 0227+48 1995/107 9.4-10.3 19 Nov 1995 And 35(21) Object bright in October 1994 and again in October 1995. Identified as IRAS 02276+4836 = Dearborn 25816 = GSC 3303.1082. TASV J2352+665 1996/002 10.9-(14.6 31 Dec 1995 TA EC-1032 Cas 8 Object bright in mid-November 1995 and at three other epochs suggesting a period of 334 days. Identified as IRAS 23496+6618 = RAFGL 3170. Glyn Marsh reports on TA EC-1038 that the object had already faded to magnitude 13 by the end of November 1995. An analysis of this star appears in The Astronomer, vol.33, no.387, p.67 (1996 July) refining the light ephemeris to be JDmax = 2447697.03 + 332.05 E and providing a chart and sequence. The best sinusoidal fit to the light curve suggests a photovisual magnitude range of 11.3 to 18.1 with rises to 10.9. Lennart Dahlmark reports (3 November 1996) that an inspection of his film archive indicates that the period is slowly increasing. He reports that between 1970 and 1979 (10 cycles) the period was 327 or 328 days, between 1979 and 1995 it was 331 days, and averaged over the period 1988 to 1995 it agrees with the 332 days recorded above. Dahlmark also reports that he has recorded the star obviously close to minimum at 14.6 and suggests that the range may be 11.3 to 15. References Bachiller, R. et al. 1997, Astron. Astrophys., 319, 235-43 Bowers, P.F. 1975, Astron. J., 80, 512- Bowers, P.F. 1981, Astron. J., 86, 1930- Dahlmark, L. 1998, IBVS (to be published) Sivagnanam, P. et al. 1990, Astron. Astrophys., 233, 112-20 VSTAT95.TXT July 1999