2015AJ....149...91P

Query : 2015AJ....149...91P

2015AJ....149...91P - Astron. J., 149, 91 (2015/March-0)

The Hubble Space Telescope UV legacy survey of galactic globular clusters. I. Overview of the project and detection of multiple stellar populations.

PIOTTO G., MILONE A.P., BEDIN L.R., ANDERSON J., KING I.R., MARINO A.F., NARDIELLO D., APARICIO A., BARBUY B., BELLINI A., BROWN T.M., CASSISI S., COOL A.M., CUNIAL A., DALESSANDRO E., D'ANTONA F., FERRARO F.R., HIDALGO S., LANZONI B., MONELLI M., ORTOLANI S., RENZINI A., SALARIS M., SARAJEDINI A., VAN DER MAREL R.P., VESPERINI E. and ZOCCALI M.

Abstract (from CDS):

In this paper we describe a new UV-initiative Hubble Space Telescope project (GO-13297) that will complement the existing F606W and F814W database of the Advanced Camera for Surveys Globular Cluster (GC) Treasury by imaging most of its clusters through UV/blue WFC3/UVIS filters F275W, F336W, and F438W. This "magic trio" of filters has shown an uncanny ability to disentangle and characterize multiple population (MP) patterns in GCs in a way that is exquisitely sensitive to C, N, and O abundance variations. Combination of these passbands with those in the optical also gives the best leverage for measuring helium enrichment. The dozen clusters that had previously been observed in these bands exhibit a bewildering variety of MP patterns, and the new survey will map the full variance of the phenomenon. The ubiquity of multiple stellar generations in GCs has made the formation of these cornerstone objects more intriguing than ever; GC formation and the origin of their MPs have now become one and the same problem. In this paper we will describe the database and our data reduction strategy, as well as the uses we intend to make of the final photometry, astrometry, and PMs. We will also present preliminary color-magnitude diagrams from the data so far collected. These diagrams also draw on data from GO-12605 and GO-12311, which served as a pilot project for the present GO-13297.

Abstract Copyright: ∼

Journal keyword(s): globular clusters: general - Hertzsprung-Russell and C-M diagrams - proper motions - stars: Population II

Simbad objects: 65

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Number of rows : 65
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024 		#notes
1 NGC 104 GlC 00 24 05.359 -72 04 53.20     4.09     ~ 3922 0
2 NGC 288 GlC 00 52 45.24 -26 34 57.4   10 8.13     ~ 1046 0
3 NGC 362 GlC 01 03 14.26 -70 50 55.6     6.58     ~ 1089 0
4 NGC 1261 GlC 03 12 16.21 -55 12 58.4     8.63     ~ 521 0
5 NGC 1851 GlC 05 14 06.76 -40 02 47.6           ~ 1433 0
6 NGC 2298 GlC 06 48 59.41 -36 00 19.1     8.89     ~ 499 0
7 NGC 2808 GlC 09 12 03.10 -64 51 48.6           ~ 1424 0
8 NGC 3201 GlC 10 17 36.82 -46 24 44.9           ~ 888 0
9 NGC 4147 GlC 12 10 06.149 +18 32 31.78   11.45 10.74     ~ 575 0
10 M 87 AGN 12 30 49.42338414 +12 23 28.0436859 10.16 9.59 8.63   7.49 ~ 7221 3
11 C 1235-509 GlC 12 38 40.20 -51 09 01.0           ~ 379 0
12 M 68 GlC 12 39 27.98 -26 44 38.6     7.96     ~ 999 0
13 NGC 4833 GlC 12 59 33.92 -70 52 35.4           ~ 426 0
14 M 53 GlC 13 12 55.25 +18 10 05.4     7.79     ~ 839 0
15 NGC 5053 GlC 13 16 27.09 +17 42 00.9     9.96     ~ 623 0
16 NGC 5139 GlC 13 26 47.28 -47 28 46.1           ~ 3433 0
17 M 3 GlC 13 42 11.62 +28 22 38.2     6.39     ~ 2481 0
18 NGC 5286 GlC 13 46 26.81 -51 22 27.3           ~ 444 0
19 NGC 5466 GlC 14 05 27.29 +28 32 04.0     9.70     ~ 830 0
20 IC 4499 GlC 15 00 18.57 -82 12 49.6     8.56     ~ 352 0
21 NGC 5824 GlC 15 03 58.612 -33 04 06.70   10.28 9.56     ~ 409 0
22 NGC 5897 GlC 15 17 24.40 -21 00 36.4   10.16 8.52     ~ 390 0
23 M 5 GlC 15 18 33.22 +02 04 51.7     5.95     ~ 1982 0
24 NGC 5927 GlC 15 28 00.69 -50 40 22.9           ~ 463 0
25 NGC 5986 GlC 15 46 03.00 -37 47 11.1     6.92     ~ 375 0
26 M 80 GlC 16 17 02.41 -22 58 33.9           ~ 719 0
27 M 4 GlC 16 23 35.22 -26 31 32.7           ~ 1856 0
28 NGC 6101 GlC 16 25 48.12 -72 12 07.9           ~ 295 0
29 NGC 6144 GlC 16 27 13.86 -26 01 24.6           ~ 246 0
30 M 107 GlC 16 32 31.86 -13 03 13.6           ~ 788 0
31 M 13 GlC 16 41 41.634 +36 27 40.75     5.8     ~ 2196 0
32 M 12 GlC 16 47 14.18 -01 56 54.7     6.07     ~ 681 0
33 M 10 GlC 16 57 09.05 -04 06 01.1     4.98     ~ 791 0
34 NGC 6304 GlC 17 14 32.25 -29 27 43.3           ~ 362 0
35 M 92 GlC 17 17 07.39 +43 08 09.4     6.52     ~ 2119 0
36 NGC 6352 GlC 17 25 29.11 -48 25 19.8           ~ 397 0
37 NGC 6366 GlC 17 27 44.24 -05 04 47.5           ~ 313 0
38 NGC 6362 GlC 17 31 54.99 -67 02 54.0           ~ 587 0
39 NGC 6388 GlC 17 36 17.461 -44 44 08.34           ~ 917 1
40 NGC 6397 GlC 17 40 42.09 -53 40 27.6     5.17     ~ 1979 0
41 Cl Terzan 5 Cl* 17 48 05.00 -24 46 48.0           ~ 851 1
42 NGC 6441 GlC 17 50 13.06 -37 03 05.2           ~ 887 0
43 NGC 6496 GlC 17 59 03.68 -44 15 57.4   9.96       ~ 226 0
44 NGC 6535 GlC 18 03 50.51 -00 17 51.5     9.85     ~ 295 0
45 NGC 6541 GlC 18 08 02.36 -43 42 53.6           ~ 379 0
46 NGC 6584 GlC 18 18 37.60 -52 12 56.8     8.17     ~ 289 0
47 NGC 6624 GlC 18 23 40.51 -30 21 39.7           ~ 888 1
48 M 69 GlC 18 31 23.10 -32 20 53.1           ~ 464 0
49 NGC 6652 GlC 18 35 45.63 -32 59 26.6           ~ 441 0
50 M 22 GlC 18 36 23.94 -23 54 17.1           ~ 1381 0
51 M 70 GlC 18 43 12.76 -32 17 31.6           ~ 387 0
52 M 54 GlC 18 55 03.33 -30 28 47.5           ~ 1071 0
53 NGC 6717 GlC 18 55 06.04 -22 42 05.3           ~ 247 0
54 NGC 6723 GlC 18 59 33.15 -36 37 56.1           ~ 504 0
55 NGC 6752 GlC 19 10 52.11 -59 59 04.4           ~ 2004 0
56 M 56 GlC 19 16 35.57 +30 11 00.5           ~ 423 0
57 NGC 6791 OpC 19 20 53.0 +37 46 41   10.52 9.5     ~ 1040 0
58 M 55 GlC 19 39 59.71 -30 57 53.1     6.49     ~ 857 0
59 M 71 GlC 19 53 46.49 +18 46 45.1           ~ 1130 0
60 NGC 6934 GlC 20 34 11.37 +07 24 16.1           ~ 423 0
61 M 72 GlC 20 53 27.70 -12 32 14.3     8.96     ~ 431 0
62 M 15 GlC 21 29 58.33 +12 10 01.2           ~ 3143 0
63 M 2 GlC 21 33 27.02 -00 49 23.7     6.25     ~ 1032 1
64 M 30 GlC 21 40 22.12 -23 10 47.5     7.10     ~ 1050 0
65 NAME Local Group GrG ~ ~           ~ 8415 0

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