Objects found by Mike Collins on UK Nova Patrol Photographs in 1998
 
Designation    Q no.     Mag range     Date reported   Announced on
      1950 Position or              Notes
     J2000 Position  
  Con   Area(s)
 
     J0712+296 1998/007  11.2-(12.3    20 Jan 1998     TA-EC 1267
  Gem 67 (56)  Object appeared bright in early 1995 and again in late
               1997. Identified as GSC 1908.0192. The faint IR source
               IRAS 07088+2942 is nearby and may be the same star.

TASV J1803+441 1998/044  10.1-11.1     16 Jun 1998     TA-EC 1587
  Her   25     Object bright in February 1993, May 1997 and May 1998.
               identified as IRAS 18018+4409 = Dearborn 36035 =
               GSC 3114.0985.  Taichi Kato (2000) provides the 
               additional identifications: Dearborn 36035 = 
               USNO 1275.09853983 = ROTSE1 J180322.10+440948.1 and 
               reports that the star appears in the 2MASS.
 
 TAV J0218+507 1998/073  10.5-(14?     12 Oct 1998     TA-EC 1369
  And 21 (35)  Object appeared bright in mid-September 1998. Identified
               as IRAS 02150+5032.  Does not appear on GSC.
               Film archive reveals maxima satisfied by Mira-type 
               variation with JDmax=2447553+350.7E.
               CCD images obtained by Tom Boles in late 1998 confirm
               the variation and show variable to be the SE component of
               a close pair.

  NSV 14687    1998/090  11.7-(13.3?   21 Oct 1998
     J2343+717 Object appeared bright in mid-October 1998. Identified as
  Cep  2  (8)  NSV 14687 discovered in 1934 by Otto Morgenroth (1935) who
               reported it as slowly varying. Subsequently designated
               Prager 5784 and CSV 5785.  Also found to be
               IRAS 23413+7130 and GSC 4487.0490.

     J0145+713 1998/089  10.6-(12.8    31 Oct 1998
  Cas  4  (10) Object appeared bright in late October 1998. Identified as
               IRAS 01411+7104 and GSC 4318.2025. Film archive reveals a
               faint (11.5) maximum in late March 1989 followed by nearly
               two years below the film limit.  Possibly SRb type.


References

Kato, T. 2000, vsnet-newvar 670 (*)
Morgenroth, O. 1935, Astron. Nach., 254, 369-74

* URI http://www.kuastro.kyoto-u.ac.jp/vsnet-newvar/msg00670.html

VSTAT98.TXT   11 December 2000