Palomar 3 / C1003+003 (Updated August 2, 2011) RA: 10:05:31.9 DEC: +00:04:18 (J2000) ============================================================ Bytes Format Explanation 1-8 A8 Star ID 10-32 A11,1x,A11 Position 34-35 A2 Units for position R0 denotes RA, DEC in the J2000 coordinates R5 denotes RA, DEC in the 1950 coordinates XA denotes X, Y in arcseconds XP denotes X, Y in pixels 37-44 F8.4 Period (days) 46-51 F6.3 Mean magnitude (or maximum magnitude if "max" is indicated in the remarks column) 53-57 F5.3 Light amplitude (range of variability) 59 A1 Colour for mean magnitude and amplitude e.g. B, V, R, I, J, K or P (for photographic). 61-65 A5 Type of variable (draft 2006 GCVS classifications) CST denotes non variable stars previously designated as variables 67-80 A19 Notes and Remarks (f denotes field star) "--" or "----" indicates no data available ========================================================================= ID Position Period ampl C Type Notes/ RA/X Dec/Y Units Remarks ========================================================================= 1 10:05:35.94 +00:05:08.9 R0 ---- 20.52 -- V RR0 2 10:05:31.53 +00:04:21.5 R0 ---- 20.62 -- V RR0 3 10:05:28.23 +00:03:33.9 R0 ---- 20.51 -- V RR0 4 10:05:32.87 +00:04:36.0 R0 3.4 19.28 0.43 V CW Note 5 10:05:29.63 +00:04:11.9 R0 ---- 20.4 -- V RR0 6 10:05:31.34 +00:04:14.2 R0 ---- 20.6 -- V RR0 7 10:05:32.63 +00:04:21.1 R0 ---- 20.5 -- V RR0 8 10:05:27.74 +00:04:35.4 R0 ---- 20.4 -- V CST? 9 10:05:33.21 +00:04:37.9 R0 ---- 20.5 -- V CST? 10 10:05:27.55 +00:04:59.7 R0 ---- 20.5 -- V CST? 11 10:05:31.07 +00:04:17.4 R0 ---- 18.7 -- V L? blend;red 12 10:05:28.81 +00:04:10.2 R0 ---- 20.4 -- V CST? Note 13 10:05:29.65 +00:03:38.0 R0 ---- 20.4 -- V RR0 14 10:05:27.39 +00:05:09.7 R0 ---- 20.5 -- V RR0 ===================================================================== Supplementary Notes The RA and dec for V1-12 are from Samus et al. (2009). The remaining data for V1-3 are from Gratton & Ortolani (1984). The data for V5-12 are from Borissova et al. (1998) where the adopted mean V magnitudes are the means of the magnitudes that they listed for each star. In their paper, V5-12 were listed as BS58, V1-5 and V9-10 respectively. All of the data for V13-14 are from Stetson et al. (1999) where the mean V magnitudes were estimated from their light curves. ==================================================================== Notes on individual stars V4: Period, magnitude, amplitude and variability type from Borissova et al. (2000) V11: Samus et al. (2009) pointed out that the image of V11 was blended. V12: This star was classified as a probable RR0 variable by Borrisova et al. (1998). However, it should have been in the field of Stetson et al. (1999) and they did not identify it as an RR Lyrae variable. Therefore its variability is questioned. ===================================================================== Discovery of the variable stars in Pal 3: V1-4 = star # 34, 155, 283, 102 respectively Gratton & Ortolani (1984) with x,y pixel positions and an ID chart. The numbers V1-4 were assigned in our electronic update to the Sawyer Hogg catalogs (Clement et al. 2001). Their star #34 was outside the field of view of subsequent invesigations. V5 = star 188 of Gratton & Ortolani (1984), formerly V1 This variable was first detected by Burbidge & Sandage (1958) who published an ID chart (Figure 6 of their paper). It was subsequently designated as V1 by Sawyer Hogg in her 3rd catalog, but was removed from the electronic edition after Gratton & Ortolani (1984) detected no variability. Since then, two independent investigations (Borissova et al. 1998; Stetson et al. 1999) have confirmed that it varies so it is included again and numbered as V5. V6-12 = Borissova's V1-5 and V9-10 Borissova et al. (1998) with x,y arcsec positions. These authors also derived x,y arcsec positions for V2, V4 and V5 which they listed as No. 155, Pop II Cep. and BS58 respectively. Three of their candidates, V8-10 in the above table, did not satisfy all of the variability criteria and are therefore classified as "CST?". Furthermore V8 and V10 should have been in the field studied by Stetson et al. (1999), but were not recognized as variables. Thus it appears to be unlikely that they are variable. V13-14 = Stetson's 2-368 and 3-269 Stetson et al. (1999). Their RA and Dec were provided by Stetson (2011, private communication). Stetson et al. (1999) announced five other RR Lyrae variables in Pal 3. They noted that three of them (1-233, 2-614 and 2-198) are the same as Gratton & Ortolani's (1984) #155, 283 and 188 which are V2, V3 and V5 in the above table. The RA and dec for the others, 1-299 and 1-404 (Stetson 2011, private communication) indicate that they are V1 and V2 of Borissova et al. (1998) which are V6 and V7 in the above table. ====================================================================== References Borissova, J., Ivanov, V. D., Catelan, M. 2000, IBVS, 4919 Borissova, J., Spassova, N., Catelan, M., Ivanov, V. D. 1998, ASP Conf 135, 188 Burbidge, E. M. & Sandage A. 1958, ApJ, 127, 527 Clement, C. M., Muzzin, A., Dufton, Q., Ponnampalam, T., Wang, J., Burford, J., Richardson, A., Rosebery, T. 2001, AJ, 122, 2587 Gratton, R. G. & Ortolani, S. A&A Supp. 1984, 57, 177 Samus, N. N., Kazarovets, E. V., Pastukhova, E. N., Tsvetkova, T. M., Durlevich, O. V. 2009, PASP, 121, 1378 Stetson, P., Bolte, M., Harris, W. E., Hesser, J., van den Bergh, S., Vandenberg, D. A., Bell, R. A. et al. 1999, AJ, 117, 247 ===============================================================