By Roberts F.S.
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1972. Adventures in Experimental Physics 1972~ p. 7. , 1984a. Astrophys. J. Suppl. 55~ 657. , 1984b. Astrophys. ~ 285~ 195. , 1985. Mon. Not. R. astr. ~ 212~ 709. , Willmer, C. , 1984. Astron. ~ 89~ 1310. , 1972. Mon. Not. R. astr. ~ 160~ 213. L. , 1978. Astron. ~ 83~ 980. P. , 1972. Astrophys. J. ~ 175~ L 79. D. , 1981. Publ. Astr. Soc. Pacific~ 93~ 388. , 1969. Mon. Not. R. astr. ~ 145~ 163. , 1975. Astrophys. J. ~ 29~ 431. , 1949. Science~ 109~ 166. E. , 1985. Publ. Astr. Soc. Pacific~ 97~ 465.
A. 5 /""---.... 0 ~ --r ------......... PHASE Figure 4. 2. Light curves of RR Lyrae stars in the NGC 6522 Baade window. The star density of even relatively bright stars in this region is extremely high making any sort of photometry extraordinarily difficult. For the CCD work to be a significant advance in accuracy over other methods requires good seeing when observing and the use of a multi star fitting algorithm when reducing the data. Even so, the light curve quality is poorer than that achieved for stars of similar brightness in less crowded fields.
1979) for stars with periods over 10 days . ~ A. 5 /""---.... 0 ~ --r ------......... PHASE Figure 4. 2. Light curves of RR Lyrae stars in the NGC 6522 Baade window. The star density of even relatively bright stars in this region is extremely high making any sort of photometry extraordinarily difficult. For the CCD work to be a significant advance in accuracy over other methods requires good seeing when observing and the use of a multi star fitting algorithm when reducing the data. Even so, the light curve quality is poorer than that achieved for stars of similar brightness in less crowded fields.