NGC 5024 / C1310+184 / Messier 53 (Updated May 2012) RA: 13:12:55.25 DEC: 18:10:05.4 (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 13:12:56.32 +18:07:13.9 R0 0.6098 16.927 1.062 V RR0 2 13:12:50.28 +18:07:00.9 R0 0.3862 16.887 0.474 V RR1 3 13:12:51.38 +18:07:45.4 R0 0.6306 16.953 0.853 V RR0 4 13:12:43.88 +18:07:26.4 R0 0.3856 16.903 0.432 V RR1 5 13:12:39.08 +18:05:42.7 R0 0.6394 16.788 0.989 V RR0 6 13:13:03.90 +18:10:19.9 R0 0.6640 16.862 1.011 V RR0 7 13:13:00.86 +18:11:30.0 R0 0.5448 16.975 1.116 V RR0 8 13:13:00.41 +18:11:05.1 R0 0.6155 16.969 1.078 V RR0 9 13:13:00.07 +18:09:25.1 R0 0.6003 16.949 1.122 V RR0 10 13:12:45.72 +18:10:55.5 R0 0.6083 16.861 1.108 V RR0 11 13:12:45.38 +18:09:02.0 R0 0.6299 16.905 1.142 V RR0 12 13:13:23.84 +18:13:16.6 R0 0.6126 16.93 1.550 B RR0 Gor 13 13:13:28.24 +18:05:13.1 R0 0.6274 16.87 1.570 B RR0 Gor 14 13:13:20.55 +18:06:42.7 R0 0.5453 16.98 1.450 B RR0 Gor 15 13:13:12.38 +18:13:55.3 R0 0.3087 16.920 0.391 V RR1 16 13:12:46.19 +18:06:39.3 R0 0.3032 16.936 0.585 V RR1 17 13:12:40.34 +18:11:54.1 R0 0.3811 16.903 0.432 V RR1 18 13:12:48.6 +18:10:13.2 R0 0.3361 16.925 0.444 V RR1 19 13:13:07.01 +18:09:26.4 R0 0.3910 16.924 0.457 V RR1 20 13:13:09.08 +18:04:16.3 R0 0.3842 17.18 0.65 B RR1 Gor 21 13:13:26.07 +18:09:43.3 R0 0.3385 17.16 0.64 B RR1 Gor 22 13:12:51.97 +18:05:16.5 R0 ---- -- -- CST Note 23 13:13:02.34 +18:08:36.0 R0 0.3658 16.897 0.497 V RR1 24 13:12:47.28 +18:09:32.4 R0 0.7632 16.824 0.598 V RR0 25 13:13:04.41 +18:10:37.3 R0 0.7051 16.894 0.829 V RR0 26 13:12:35.76 +18:05:20.1 R0 0.3911 17.02 0.57 B RR1 Gor 27 13:12:41.43 +18:07:23.8 R0 0.6711 16.870 0.898 V RR0 28 13:12:42.12 +18:16:37.7 R0 0.6328 16.93 1.44 B RR0 Gor;Note 29 13:13:04.26 +18:08:47.0 R0 0.8233 16.812 0.395 V RR0 30 13:13:00.17 +18:02:04.0 R0 0.5355 16.93 1.35 B RR0 Gor 31 13:12:59.57 +18:10:04.9 R0 0.7057 16.798 0.998 V RR0 32 13:12:47.73 +18:08:35.9 R0 0.3904 16.897 0.502 V RR1 33 13:12:43.86 +18:10:13.1 R0 0.6246 16.904 1.051 V RR0 34 13:12:45.70 +18:06:26.2 R0 0.2896 16.928 0.198 V RR1 Note 35 13:13:02.42 +18:12:37.9 R0 0.3727 16.919 0.534 V RR1 36 13:13:03.29 +18:15:10.4 R0 0.3732 16.891 0.454 V RR1 37 13:12:52.28 +18:11:05.4 R0 0.7176 16.873 0.810 V RR0 38 13:12:57.14 +18:07:40.6 R0 0.7058 16.903 0.847 V RR0 39 13:12:38.75 +18:13:31.2 R0 ---- -- -- CST Note 40 13:12:55.86 +18:11:54.7 R0 0.3147 16.947 0.458 V RR1 41 13:12:56.75 +18:11:08.5 R0 0.6144 16.952 0.965 V RR0 42 13:12:50.54 +18:10:20.1 R0 0.7137 16.865 0.873 V RR0 43 13:12:53.08 +18:10:55.5 R0 0.7120 16.761 0.727 V RR0 44 13:12:51.66 +18:10:00.6 R0 0.3749 16.892 0.462 V RR1 Note 45 13:12:55.16 +18:09:27.4 R0 0.6550 16.840 0.993 V RR0 46 13:12:54.53 +18:10:37.0 R0 0.7036 16.874 0.894 V R0 47 13:12:50.42 +18:12:24.7 R0 0.3354 16.828 0.341 V RR1 48 13:13:14.31 +18:22:04.9 R0 0.3328 17.12 0.54 V RR1 Cuf;Note 49 13:12:59.16 +18:14:35.6 R0 111.6 14.08 0.23 V SR Cuf;Note 50 13:12:45.52 +18:11:29.0 R0 55.4 13.77 0.20 V SR Cuf;Note 51 13:12:57.59 +18:10:49.7 R0 0.3552 16.762 0.346 V RR1 52 13:12:55.92 +18:10:37.1 R0 0.3741 16.994 0.596 V RR1 53 13:12:55.83 +18:10:31.6 R0 0.3891 16.362 0.349 V RR1 54 13:12:54.31 +18:10:31.5 R0 0.3151 16.803 0.438 V RR1 55 13:12:53.46 +18:10:36.6 R0 0.4433 16.694 0.465 V RR1 56 13:12:53.69 +18:09:26.0 R0 0.3289 16.894 0.445 V RR1 57 13:12:55.56 +18:09:58.2 R0 0.5683 16.917 1.239 V RR0 Note 58 13:12:55.60 +18:09:31.0 R0 0.3550 16.864 0.521 V RR1 59 13:12:56.66 +18:09:20.8 R0 0.3039 16.870 0.248 V RR1 60 13:12:56.98 +18:09:36.5 R0 0.6448 16.378 0.673 V RR0 blend 61 13:12:55.12 +18:10:12.5 R0 0.3795 -- -- RR1 blend;Note 62 13:12:54.00 +18:10:29.8 R0 0.3599 15.581 0.140 V RR1 blend 63 13:12:56.29 +18:10:00.7 R0 0.3105 16.715 0.363 V RR1 64 13:12:52.52 +18:10:12.5 R0 0.3197 16.074 0.261 V RR1 blend 65 13:13:04.68 +18:10:59.5 R0 ---- -- -- SR? Kop 66 13:13:01.58 +18:10:03.9 R0 ---- -- -- SR? Kop 67 13:13:01.01 +18:10:09.6 R0 29.4 14.221 -- SR? 68 13:12:56.57 +18:08:23.1 R0 ---- -- -- SR? Kop 69 13:12:56.17 +18:10:19.5 R0 ---- -- -- SR? Kop 70 13:12:55.32 +18:09:42.0 R0 ---- -- -- SR? Kop 71 13:12:54.38 +18:09:54.0 R0 0.3045 16.652 0.393 V RR1 blend 72 13:12:55.94 +18:09:52.3 R0 0.3407 16.726 0.2 V RR1 73 13:13:03.35 +18:09:25.1 R0 0.0701 18.974 0.240 V SXPHE 74 13:12:49.7 +18:07:26.0 R0 0.0454 19.031 0.247 V SXPHE 75 13:13:09.4 +18:09:39.8 R0 0.0443 19.477 0.201 V SXPHE 76 13:13:04.97 +18:08:35.8 R0 0.0415 19.522 0.194 V SXPHE 77 13:13:20.8 +18:15:34.9 R0 0.0769 18.478 0.35 V SXPHE DK 78 13:12:49.91 +18:08:56.6 R0 0.0449 18.210 0.144 V SXPHE 79 13:12:46.60 +18:11:37.0 R0 0.0463 -- -- SXPHE 80 13:12:57.37 +18:10:15.2 R0 0.0674 -- -- SXPHE 81 13:13:02.69 +18:06:29.7 R0 ---- -- -- CST 82 13:12:56.46 +18:13:09.9 R0 ---- -- -- CST 83 13:12:50.11 +18:07:43.0 R0 ---- -- -- CST? 84 13:12:36.17 +18:07:32.2 R0 22.4 14.720 -- V Lb? Note 85 13:12:50.69 +18:10:39.6 R0 19.8 14.024 -- V Lb? Note 86 13:12:52.71 +18:10:28.1 R0 22.2 14.154 -- V Lb? Note 87 13:13:01.92 +18:10:13.2 R0 0.0463 19.367 0.218 V SXPHE 88 13:13:19.09 +18:06:40.7 R0 0.0500 19.171 0.138 V SXPHE Jeon 89 13:13:08.16 +18:07:38.5 R0 0.0434 19.539 0.084 V SXPHE 90 13:12:52.77 +18:04:58.4 R0 0.0385 18.959 0.060 V SXPHE Jeon 91 13:12:53.62 +18:10:13.6 R0 0.3024 16.928 0.117 V RR1 92 13:12:54.91 +18:10:50.3 R0 0.2772 16.966 0.105 V RR1 93 13:12:40.00 +18:08:39.0 R0 0.0401 18.840 0.028 V SXPHE 94 13:12:42.11 +18:07:39.8 R0 0.0380 19.750 0.044 V SXPHE 95 13:12:47.94 +18:09:55.2 R0 0.0411 19.564 0.058 V SXPHE 96 13:12:48.29 +18:13:18.9 R0 0.0393 19.589 0.126 V SXPHE 97 13:12:48.27 +18:14:34.6 R0 0.0602 18.762 0.066 V SXPHE 98 13:12:48.67 +18:09:35.9 R0 0.0384 19.642 0.080 V SXPHE 99 13:12:52.91 +18:10:35.8 R0 0.0564 18.456 0.128 V SXPHE blend 100 13:12:53.42 +18:14:46.2 R0 0.0482 19.264 0.090 V SXPHE 101 13:12:53.65 +18:08:57.9 R0 0.0525 19.211 0.192 V SXPHE 102 13:12:54.76 +18:09:37.7 R0 0.0724 18.576 0.306 V SXPHE blend 103 13:12:58.32 +18:08:41.2 R0 0.0443 19.484 0.136 V SXPHE 104 13:12:59.00 +18:10:22.0 R0 0.1476 19.342 0.230 V SXPHE 105 13:13:01.92 +18:12:30.4 R0 0.0453 19.609 0.134 V SXPHE 106 13:12:48.69 +18:10:10.3 R0 0.0500 19.487 0.212 V SXPHE 107 13:12:56.38 +18:11:05.3 R0 0.0496 18.101 0.050 V SXPHE blend 108 13:12:59.52 +18:11:17.4 R0 0.0379 19.645 0.121 V SXPHE 109 13:12:53.55 +18:09:55.4 R0 21.93 15.208 0.05 V SR ========================================================================== Supplementary Notes V1-105: The data for all except 20 of these stars are from Arellano Ferro et al. (2011). These authors also published ID charts for all of the variables they studied. Some of the mean magnitudes and amplitudes were published in their 2011 MNRAS paper and the rest were supplied by Arellano Ferro (2011, private communication). The amplitudes listed for the SX Phe variables in the above table are double the values that were published by Arellano Ferro et al. (2011). In a separate paper (Arellano Ferro et al. 2012), they discussed the properties of the M53 Blazkko variables. The 20 variables not included in the study of Arellano Ferro et al. (2011) are V12, 13, 14, 20, 21, 22, 26, 28, 30, 48, 77, 88, 90 which were not in their field of view and V49, 50, 65, 66, 68, 69, 70 which were saturated in their images. The RA and dec listed above for these 20 stars are from Samus et al. (2009). The sources for their periods, magnitudes, amplitudes and variability types are indicated in the remarks column where Gor refers to Goranskij (1976), Cuf refers to Cuffey (1965, 1966), Kop refers to Kopacki (2000), DK refers to Dekany & Kovacs (2009) and Jeon refers to Jeon (2003). The Goranskij study was based on photographic observations and the mean B magnitude is the mean of their B_max and B_min. Kopacki (2000) reduced his data using the image subtraction method and therefore did not derive magnitudes for many of the variables in his investigation, including the SR variables he discovered. Kopacki's paper gave a good summary of previous investigations of the variables in M53. He also published an ID chart covering an area of about 6 by 4 arcmin and labelled all of the variables (up to V70) in the field of view. V106-109: All the data are from Bramich et al. (2012). ====================================== Notes on individual stars V22, V34, V39: van den Hoven van Genderen (1947) stated that the variability of V22, V34 and V39 seemed very doubtful and Cuffey's (1965) analysis confirmed this. However, Dekany & Kovacs (2009) found that V34 was an RR Lyrae with low ampltude and derived a period. Arellano Ferro et al. (2011) verified the RR Lyrae period for V34 and confirmed that V39 is not variable; V22 was outside of their field of view. V28: Evstigneeva et al. (1997) noted that the y value (+459.0") listed in all Sawyer Hogg's catalogs (1939, 1955, 1973) and in our electronic versions was incorrect. Baade's (1931) discovery paper listed y=+399.0". V43: typo in the dec listed by Arellano Ferro et al. (2011) V44: Evstigneeva et al. (1997) noted that the sign of the x coordinate was incorrect (+53" should be -53") in the discovery paper by van den Hoven van Genderen (1947) and the incorrect value was listed in Sawyer Hogg's (1955, 1973) 2nd and 3rd catalogs and again in our 2001 on-line version. V48, V49, V50: Periods and amplitudes for V48-50 are from Cuffey (1966) and the mean magnitudes are from Cuffey (1965). Kopacki (2000) confirmed the variability of V50 and derived a tentative period of approximately 49 days. Kopacki also pointed out that the x,y coordinates listed for these three stars in Helen Hogg's 3rd catalog were incorrect. These errors were repeated in our original electronic catalogs and the RA and dec derived by Evstigneeva et al. (1997) were based on the erroneous coordinates. Samus et al. (2009) published the correct RA and dec for these three stars. They all correspond to 2MASS positions. V57, V61: According to Arellano Ferro et al. (2011), these two variables were misidentified by Kopacki (2000). V84, V85, V86: The magnitudes are from Arellano Ferro et al. (2011) and the periods are from Dekany & Kovacs (2009). Safanova & Stalin (2011) pointed out that V84 and V85 are S1 and S17 in Stetson's (2000) standard field for NGC 5024. =============================================================================== Discovery of the variable stars in M53: V1-23 Shapley (1920) with x,y coordinates and an ID chart V24-40 Baade (1931) with x,y coordinates V41-42 Grosse (1932) with an ID chart. Variables 1-40 were also identified on the chart. In a later paper, Grosse (1933) discovered 7 additional variables in the field around M53 and published their 1900 RA and dec. V43-46 van den Hoven van Genderen (1947) with x,y coordinates and an ID chart. She also published x,y coordinates for V41 and V42 and included them on the ID chart. V47 Margoni (1964) with x,y coordinates and an ID chart V48-50 = Cuffey's V47-V49 = stars 4-7-8, 4-4-16 and K Cuffey (1965) wth an ID chart. The numbers V48-V50 were assigned by Sawyer Hogg (1973) in her 3rd catalog because data for a new V47 had been published previously by Margoni (1964). Sawyer Hogg derived x,y coordinates for Cuffey's new variables, but Kopacki (2000) discovered that they were incorrect and that the RA and dec computed by Evstigneeva et al. (1997) were based on these incorrect values. Samus et al. (2009) computed the correct RA and dec for these three stars. They all correspond to 2MASS positions. V51-60 = Kravtsov's V1-5,7-11 Kravtsov (1990) with x,y coordinates and an ID chart. The numbers V51-60 were assigned by Kopacki (2000) Kopacki did not assign a new number for Kravtsov's V6 because it was the same star as V44. V61-70 Kopacki (2000) with x,y coordinates and an ID chart. V71-72 Dekany & Kovacs (2009) with RA & dec Arellano Ferro et al. (2011) found small errors in the coordinates for both of these stars and provided ID charts and revised coordinates. V73-76 = SXP1, SXP2, SXP6, SXP7 Jeon et al. (2002, 2003) with RA, dec and an ID chart in the 2003 paper. The numbers V73-76 were assigned by Dekany & Kovacs (2009). V77-86 Dekany & Kovacs (2009) with RA & dec Arellano Ferro et al. (2011) found a small errors in the coordinates of V80 and provided an ID chart and revised coordinates. Also, the variability of V81, V82 and V83 was not confirmed in the Arellano Ferro et al. study. V87-90 = SXP3, SXP4, SXP5, SXP8 Jeon et al. (2002, 2003) with RA, dec and an ID chart in the 2003 paper. The numbers V87-90 were assigned in the September 2009 update to the CVSGC electronic catalog. These stars were not studied by Dekany & Kovacs (2009) because V87 was not resolved on their frames and the amplitudes of V88-90 were too low to be identified in their data. V91-105 Arellano Ferro et al. (2011) with RA, dec and ID charts They also listed 5 suspected variables, S1-5, that were blue stragglers. V106-108 = SX4, SX16, SX21 Safanova & Stalin (2011) with RA, dec and ID chart The numbers V106-108 were assigned by Bramich et al. (2012) who confirmed their variability. Some of the other SXPHE candidates announced by Safanova & Stalin were independently discovered by Arellano Ferro et al. (2011) or were known from previous studies. V109 Bramich et al. (2012) with RA, dec and an ID chart V109 was announced as VC10, a candidate variable, with variations on a time scale of a few hours, by Safanova & Stalin (2011). Bramich et al. (2012) did not confirm the short term variability of VC10, but in the course of their analysis discovered that it was a semi-regular variable near the red giant tip. ---------------------------------------------------------------------- The 2011 paper by Safanova & Stalin (2011) was based on R band observations of M53 made over an interval of 7.2 hours on March 24, 2010. They recovered most of the known variables and announced many new candidates. However, their data were not extensive enough to confirm the variability of most of the new candidates. An independent analysis of these stars was carried out by Bramich et al. (2012) who found most to be non-variable, with the exception of V106-V109 listed above. Also, Bramich et al. tentatively confirmed the variability of S&S candidates W11 and SX12, but commented that follow-up observations of better precision would be required to establish their variable nature. =========================================================================== References Arellano Ferro, A., Figuera, J. R., Giridhar, S., Bramich, D. M., Hernandez Santisteban, J. V., Kuppuswamy, K. 2011, MNRAS, 416, 2265 Arellano Ferro, A., Bramich, D. N., Figuera, J. R., Giridhar, S., Kuppuswamy, K. 2012, MNRAS, 420, 1333 Baade, W. 1931, Mitt Hamburg, 6, 67 Bramich, D. M., Arellano Ferro, A., Figuera Jaimes, R., Giridhar, S. 2012, MNRAS (accepted) Cuffey, J. 1965, AJ, 70, 732 Cuffey, J. 1966, AJ, 71, 514 Dekany, I. & Kovacs, G. 2009, A&A, 507, 803 Evstigneeva, N. M., Samus, N. N., Alcaino, G. 1997, Ast Let, 23, 395 Goranskij, V. P. 1976, Per. Zvez. Pril., 3, 1 Grosse, E. 1932, AN, 246, 377 = Ast Abh Hamburg, 4, 39 Grosse, E. 1933, AN, 249, 389 Jeon, Y.-B., Kim, S.-L., Lee, H., Lee, M. G. 2002. ASP Conf, 259, 140 Jeon, Y.-B., Lee, M. G., Kim, S.-L., Lee, H. 2003, AJ, 125, 3165 Kopacki, G. 2000, A&A, 358, 547 Kravtsov, V. V. 1990, Ast Tsirk, 1544, 21 Margoni, R. 1964, Mem. S. A. I., 35, 107 = Asiago-Padova Cont 150 Safanova, M. & Stalin, C. S. 2011, AJ, 142, 179 Shapley, H. 1920, ApJ, 52, 73 Stetson, P.B. 2000, PASP, 112, 925 van den Hoven van Genderen, E. 1947, BAN, 10, 241 =================================================================