2023A&A...671A.106M


Query : 2023A&A...671A.106M

2023A&A...671A.106M - Astronomy and Astrophysics, volume 671A, 106 (2023/3-1)

Kinematic differences between multiple populations in Galactic globular clusters.

MARTENS S., KAMANN S., DREIZLER S., GOTTGENS F., HUSSER T.-O., LATOUR M., BALAKINA E., KRAJNOVIC D., PECHETTI R. and WEILBACHER P.M.

Abstract (from CDS):

Aims. The formation process of multiple populations in globular clusters is still up for debate. These populations are characterized by different light-element abundances. Kinematic differences between the populations are particularly interesting in this respect because they allow us to distinguish between single-epoch formation scenarios and multi-epoch formation scenarios. We derive rotation and dispersion profiles for 25 globular clusters and aimed to find kinematic differences between multiple populations to constrain their formation process.
Methods. We split red-giant-branch (RGB) stars in each cluster into three populations (P1, P2, and P3) for the type-II clusters and two populations (P1 and P2) otherwise using Hubble photometry. We derived the global rotation and dispersion profiles for each cluster by using all stars with radial velocity measurements obtained from MUSE spectroscopy. We also derived these profiles for the individual populations of each cluster. Based on the rotation and dispersion profiles, we calculated the rotation strength in terms of ordered-over-random motion, (v/σ)HL, evaluated at the half-light radius of the cluster. We then consistently analyzed all clusters for differences in the rotation strength of their populations.
Results. We detect rotation in all but four clusters. For NGC 104, NGC 1851, NGC 2808, NGC 5286, NGC 5904, NGC 6093, NGC 6388, NGC 6541, NGC 7078, and NGC 7089, we also detect rotation for P1 and/or P2 stars. For NGC 2808, NGC 6093, and NGC 7078 we find differences in (v/σ)HL between P1 and P2 that are larger than 1σ. Whereas we find that P2 rotates faster than P1 for NGC 6093 and NGC 7078, the opposite is true for NGC 2808. However, even for these three clusters the differences are still of low significance. We find that the rotation strength of a cluster generally scales with its median relaxation time. For P1 and P2 the corresponding relation is very weak at best. We observe no correlation between the difference in rotation strength between P1 and P2 and the cluster relaxation time. The stellar radial velocities derived from MUSE data that this analysis is based on are made publicly available.

Abstract Copyright: © The Authors 2023

Journal keyword(s): globular clusters: general - stars: kinematics and dynamics - techniques: imaging spectroscopy

VizieR on-line data: <Available at CDS (J/A+A/671/A106): table2.dat>

Simbad objects: 32

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Number of rows : 32
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 362 GlC 01 03 14.26 -70 50 55.6     6.58     ~ 1089 0
3 NGC 1783 GlC 04 59 08.590 -65 59 15.84   10.9 10.93     ~ 253 0
4 NGC 1851 GlC 05 14 06.76 -40 02 47.6           ~ 1433 0
5 M 79 GlC 05 24 10.59 -24 31 27.3     8.16     ~ 819 0
6 NGC 2808 GlC 09 12 03.10 -64 51 48.6           ~ 1424 0
7 NGC 3201 GlC 10 17 36.82 -46 24 44.9           ~ 888 0
8 M 3 GlC 13 42 11.62 +28 22 38.2     6.39     ~ 2481 0
9 NGC 5286 GlC 13 46 26.81 -51 22 27.3           ~ 444 0
10 M 5 GlC 15 18 33.22 +02 04 51.7     5.95     ~ 1982 0
11 M 80 GlC 16 17 02.41 -22 58 33.9           ~ 719 0
12 M 4 GlC 16 23 35.22 -26 31 32.7           ~ 1856 0
13 M 13 GlC 16 41 41.634 +36 27 40.75     5.8     ~ 2196 0
14 M 12 GlC 16 47 14.18 -01 56 54.7     6.07     ~ 681 0
15 M 10 GlC 16 57 09.05 -04 06 01.1     4.98     ~ 791 0
16 M 62 GlC 17 01 12.60 -30 06 44.5           ~ 623 0
17 NGC 6293 GlC 17 10 10.42 -26 34 54.2           ~ 284 0
18 NGC 6352 GlC 17 25 29.11 -48 25 19.8           ~ 397 0
19 NGC 6362 GlC 17 31 54.99 -67 02 54.0           ~ 587 0
20 NGC 6388 GlC 17 36 17.461 -44 44 08.34           ~ 917 1
21 NGC 6397 GlC 17 40 42.09 -53 40 27.6     5.17     ~ 1979 0
22 NGC 6441 GlC 17 50 13.06 -37 03 05.2           ~ 887 0
23 NGC 6522 GlC 18 03 34.08 -30 02 02.3           ~ 529 0
24 NGC 6541 GlC 18 08 02.36 -43 42 53.6           ~ 379 0
25 NGC 6624 GlC 18 23 40.51 -30 21 39.7           ~ 888 1
26 M 22 GlC 18 36 23.94 -23 54 17.1           ~ 1381 0
27 M 70 GlC 18 43 12.76 -32 17 31.6           ~ 387 0
28 NGC 6752 GlC 19 10 52.11 -59 59 04.4           ~ 2004 0
29 M 71 GlC 19 53 46.49 +18 46 45.1           ~ 1130 0
30 M 15 GlC 21 29 58.33 +12 10 01.2           ~ 3143 0
31 M 2 GlC 21 33 27.02 -00 49 23.7     6.25     ~ 1032 1
32 M 30 GlC 21 40 22.12 -23 10 47.5     7.10     ~ 1050 0

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