2011A&A...532A.147L


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.04CEST13:39:02

2011A&A...532A.147L - Astronomy and Astrophysics, volume 532A, 147-147 (2011/8-1)

Resolved photometry of extragalactic young massive star clusters.

LARSEN S.S., DE MINK S.E., ELDRIDGE J.J., LANGER N., BASTIAN N., SETH A., SMITH L.J., BRODIE J. and EFREMOV Yu.N.

Abstract (from CDS):

We present colour-magnitude diagrams (CMDs) of young massive star clusters in several galaxies located well beyond the Local Group. The richness of these clusters allows us to obtain large samples of post-main sequence stars and test how well the observed CMDs are reproduced by canonical stellar isochrones. We use imaging of seven clusters in the galaxies NGC 1313, NGC 1569, NGC 1705, NGC 5236 and NGC 7793 obtained with the Advanced Camera for Surveys on board the Hubble Space Telescope and carry out PSF-fitting photometry of individual stars in the clusters. The clusters have ages in the range ~(5-50)x106 years and masses of ∼105M-106M. Although crowding prevents us from obtaining photometry in the inner regions of the clusters, we are still able to measure up to 30-100 supergiant stars in each of the richest clusters. The resulting CMDs and luminosity functions are compared with photometry of artificially generated clusters, designed to reproduce the photometric errors and completeness as realistically as possible. In agreement with previous studies, our CMDs show no clear gap between the H-burning main sequence and the He-burning supergiant stars, contrary to predictions by common stellar isochrones. In general, the isochrones also fail to match the observed number ratios of red-to-blue supergiant stars, although the difficulty of separating blue supergiants from the main sequence complicates this comparison. In several cases we observe a large spread (1-2mag) in the luminosities of the supergiant stars that cannot be accounted for by observational errors. We find that this spread can be reproduced by including an age spread of ~(10-30)x106 years in the models. However, age spreads cannot fully account for the observed morphology of the CMDs and other processes, such as the evolution of interacting binary stars, may also play a role. Colour-magnitude diagrams can be successfully obtained for massive star clusters out to distances of at least 4-5 Mpc. Comparing such CMDs with models based on canonical isochrones we find several areas of disagreement. One interesting possibility is that an age spread of up to ∼30Myr may be present in some clusters. The data presented here may provide useful constraints on models for single and/or binary stellar evolution.

Abstract Copyright:

Journal keyword(s): open clusters and associations: general - galaxies: star clusters: general - galaxies: spiral - Hertzsprung-Russell, diagrams C-M

VizieR on-line data: <Available at CDS (J/A+A/532/A147): table1.dat table4.dat-table10.dat>

Nomenclature: Table 4: [LDE2011] NGC1569-A NNNNN N=365 among (Nos 3736-10559). Table 5: [LDE2011] NGC1569-B NNNN N=449 among (Nos 1095-9253). Table 6: [LDE2011] NGC1705-1 NNNN N=489 among (Nos 3355-3402). Table 7: [LDE2011] NGC1313-F3-1 NNNN N=201 among (Nos 3312-7779). Table 8: [LDE2011] NGC5236-F1-1 NNNN N=122 among (Nos 2350-7579). Table 9: [LDE2011] NGC5236-F1-3 NNNN N=98 among (Nos 3579-9991). Table 10: [LDE2011] NGC7793-F1-1 NNNNN N=100 among (Nos 3655-10371).

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

Simbad objects: 27

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Number of rows : 27

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 NGC 45 LSB 00 14 03.989 -23 10 55.53 11.92 11.21 10.73 10.58 10.4 ~ 227 1
2 M 31 G 00 42 44.330 +41 16 07.50 4.86 4.36 3.44     ~ 10902 1
3 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9440 1
4 NGC 346 Cl* 00 59 05.090 -72 10 33.24           ~ 449 0
5 M 33 GiG 01 33 50.904 +30 39 35.79 6.17 6.27 5.72     ~ 5134 1
6 NGC 604 HII 01 34 32.1 +30 47 01           ~ 544 0
7 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5665 1
8 [SL2011] NGC 1313 3 7 Cl* 03 17 47.7631398321 -66 30 18.640980566 17.75 18.26 18.13   17.53 ~ 6 0
9 NGC 1313 G 03 18 16.046 -66 29 53.74   10.06 10.0 9.40 10.4 ~ 605 2
10 NAME NGC 1569 CL* A Cl* 04 30 48.2 +64 50 59   15.45 15.22     ~ 97 1
11 NAME NGC 1569 CL* B Cl* 04 30 49.0 +64 50 53           ~ 70 0
12 NGC 1569 IG 04 30 49.186 +64 50 52.52 11.72 11.86 11.03     ~ 1147 3
13 NAME NGC 1705 CL* A Cl* 04 54 13.24 -53 21 36.1           ~ 40 0
14 NGC 1705 SBG 04 54 13.500 -53 21 39.82 12.32 12.96 12.56 12.58 12.9 ~ 593 1
15 NGC 1850 Cl* 05 08 50.190 -68 45 35.65   8.84 8.96     ~ 231 1
16 NGC 1866 GlC 05 13 38.920 -65 27 52.75   9.98 9.73     ~ 388 0
17 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14826 1
18 SN 1987A SN* 05 35 28.020 -69 16 11.07           SNIIpec 4484 2
19 NGC 2403 AGN 07 36 51.396 +65 36 09.17 9.31 8.84 8.38 8.19   ~ 1606 1
20 SN 1993J SN* 09 55 24.77476 +69 01 13.7026   10.8 12.0     SNIIb 1253 1
21 NGC 4395 Sy2 12 25 48.8639154223 +33 32 48.694684028 10.84 10.54 10.11 9.98   ~ 993 1
22 M 83 SBG 13 37 00.919 -29 51 56.74 8.85 8.11 7.52 7.21   ~ 2228 2
23 [L99] n5236-1182 Cl* 13 37 01.28 -29 50 49.8   16.77 16.73     ~ 4 0
24 [L99] n5236-1234 Cl* 13 37 04.58 -29 50 35.9   17.63 17.67     ~ 4 0
25 [L99] n7793-298 Cl* 23 57 35.880 -32 35 40.92 16.59 17.24 17.22   16.75 ~ 4 0
26 NGC 7793 GiG 23 57 49.7533807411 -32 35 27.708304655 10.26 9.74 9.28 9.06 9.7 ~ 921 2
27 NAME Local Group GrG ~ ~           ~ 6970 0

    Equat.    Gal    SGal    Ecl

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2020.07.04-13:39:02

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