2015A&A...581A..72F


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.13CEST07:23:31

2015A&A...581A..72F - Astronomy and Astrophysics, volume 581A, 72-72 (2015/9-1)

Stroemgren uvby photometry of the peculiar globular cluster NGC 2419.

FRANK M.J., KOCH A., FELTZING S., KACHAROV N., WILKINSON M.I. and IRWIN M.

Abstract (from CDS):

NGC 2419 is a peculiar Galactic globular cluster offset from the others in the size-luminosity diagram, and showing several chemical abundance anomalies. Here, we present Stroemgren uvby photometry of the cluster. Using the gravity- and metallicity-sensitive c1 and m1 indices, we identify a sample of likely cluster members extending well beyond the formal tidal radius. The estimated contamination by cluster non-members is only one per cent, making our catalogue ideally suited for spectroscopic follow-up. We derive photometric [Fe/H] of red giants, and depending on which metallicity calibration from the literature we use, we find reasonable to excellent agreement with spectroscopic [Fe/H], both for the cluster mean metallicity and for individual stars. We demonstrate explicitly that the photometric uncertainties are not Gaussian and this must be accounted for in any analysis of the metallicity distribution function. Using a realistic, non-Gaussian model for the photometric uncertainties, we find a formal internal [Fe/H] spread of σ=0.11+0.02–0.01 dex. This is an upper limit to the cluster's true [Fe/H] spread and may partially, and possibly entirely, reflect the limited precision of the photometric metallicity estimation and systematic effects. The lack of correlation between spectroscopic and photometric [Fe/H] of individual stars is further evidence against a [Fe/H] spread on the 0.1 dex level. Finally, the CN-sensitive δ4, among other colour indices, anti-correlates strongly with magnesium abundance, indicating that the second-generation stars are nitrogen enriched. The absence of similar correlations in some other CN-sensitive indices supports the second generation being enriched in He, which in these indices approximately compensates the shift due to CN. Compared to a single continuous distribution with finite dispersion, the observed δ4 distribution of red giants is slightly better fit by two distinct populations with no internal spread, with the nitrogen-enhanced second generation accounting for 53±5 per cent of stars. Despite its known peculiarities, NGC 2419 appears to be very similar to other metal-poor Galactic globular clusters with a similarly nitrogen-enhanced second generation and little or no variation in [Fe/H], which sets it apart from other suspected accreted nuclei such as ωCen.

Abstract Copyright:

Journal keyword(s): globular clusters: individual: NGC 2419 - stars: abundances - techniques: photometric

VizieR on-line data: <Available at CDS (J/A+A/581/A72): catalog.dat>

Status at CDS:   All or part of tables of objects could be ingested in SIMBAD with priority 2.

Simbad objects: 34

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Number of rows : 34

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 HD 51754 PM* 06 58 38.5387307770 -00 28 49.697886299 9.60 9.567 9.009 8.663 8.334 G2V 110 0
2 NGC 2419 GlC 07 38 08.51 +38 52 54.9     10.05     ~ 815 0
3 HD 64090 PM* 07 53 33.1186555870 +30 36 18.263360879 8.75 8.86 8.25 7.70 7.30 K0:V_Fe-3 340 0
4 NAME UMa II Galaxy G 08 51 30.0 +63 07 48     13.3     ~ 311 0
5 IRAS 09110-6439 GlC 09 12 03.10 -64 51 48.6   7.77 5.69     ~ 1245 0
6 NAME Leo I dSph G 10 08 28.12 +12 18 23.4   11.3 10.0     ~ 1045 1
7 HD 88371 PM* 10 11 48.0685636384 +23 45 18.705316029   9.06   8.0   G2V 83 0
8 NAME Dwarf Elliptical Galaxy in Sex G 10 13 02.9 -01 36 53   12 10.4     ~ 706 0
9 BD-05 3063 PM* 10 26 41.2767372063 -06 31 34.906414344   9.97 9.72     K3 51 0
10 BD-01 2457 PM* 10 52 36.2761243259 -02 06 39.790862380   10.83 9.82     K4 47 0
11 V* SU Crt dS* 11 32 51.5731761732 -12 02 06.465171801   8.89 8.65     F8V 60 0
12 BD+51 1696 PM* 11 46 35.1557706721 +50 52 54.682692534 10.32 10.47   9.5   sdG0 129 0
13 BD-04 3208 PM* 12 07 15.0719832426 -05 44 01.609304815   10.40 9.99     A7 133 0
14 HD 107853 * 12 23 29.8329217149 +26 33 56.662133206   9.56 9.12     G0 26 0
15 HD 108754 SB* 12 29 42.7346214444 -03 19 58.687651080 9.92 9.74 9.03     G6V 120 0
16 G 14-39 PM* 13 14 26.8899272365 -04 05 43.474243462   13.713 12.807 12.263 11.738 K3 38 0
17 NGC 5139 GlC 13 26 47.28 -47 28 46.1   6.12 5.33     ~ 2997 0
18 HD 118659 PM* 13 38 00.4712954269 +19 08 53.098367002 9.58 9.47   8.4   G4V 80 0
19 BD-05 3763 PM* 13 47 23.4437896994 -06 08 12.729254432   11.30 10.28     K3.5V 43 0
20 HD 123265 PM* 14 06 41.2799215970 -05 31 06.008549865   9.19 8.36     K1V 61 0
21 BD-13 3834 PM* 14 10 27.0759078866 -13 56 04.287709497   11.261 10.681 10.305 9.908 G0: 75 0
22 BD+26 2606 SB* 14 49 02.3550036151 +25 42 09.136461939 9.92 10.16 9.73 9.27 8.95 A5 351 0
23 HD 134088 PM* 15 08 12.5670991059 -07 54 47.535631396   9.266 9.018     G2/3(V) 91 0
24 NAME Her Dwarf Galaxy G 16 31 02.0 +12 47 30     14.0     ~ 275 1
25 M 92 GlC 17 17 07.39 +43 08 09.4     6.52     ~ 1905 0
26 NAME Dra dSph G 17 20 14.335 +57 55 16.39   12.40 10.6     ~ 1165 1
27 NGC 6397 GlC 17 40 42.09 -53 40 27.6   7.39 5.17     ~ 1799 1
28 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11542 0
29 M 22 GlC 18 36 23.94 -23 54 17.1   7.16 6.17     ~ 1217 0
30 M 54 GlC 18 55 03.33 -30 28 47.5           ~ 898 0
31 NGC 6752 GlC 19 10 52.11 -59 59 04.4   6.96 6.28     ~ 1807 0
32 V* RR Lyr RR* 19 25 27.9123232234 +42 47 03.690634101   7.36   7.6   A8-F7 880 0
33 M 55 GlC 19 39 59.71 -30 57 53.1     6.49     ~ 758 0
34 M 15 GlC 21 29 58.33 +12 10 01.2   3       ~ 2907 0

    Equat.    Gal    SGal    Ecl

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2020.07.13-07:23:31

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