2017A&A...608A..85L


C.D.S. - SIMBAD4 rel 1.7 - 2020.12.02CET11:49:57

2017A&A...608A..85L - Astronomy and Astrophysics, volume 608A, 85-85 (2017/12-1)

Detailed chemical composition of classical Cepheids in the LMC cluster NGC 1866 and in the field of the SMC.

LEMASLE B., GROENEWEGEN M.A.T., GREBEL E.K., BONO G., FIORENTINO G., FRANCOIS P., INNO L., KOVTYUKH V.V., MATSUNAGA N., PEDICELLI S., PRIMAS F., PRITCHARD J., ROMANIELLO M. and DA SILVA R.

Abstract (from CDS):

Context. Cepheids are excellent tracers of young stellar populations. They play a crucial role in astrophysics as standard candles. The chemistry of classical Cepheids in the Milky Way is now quite well-known, however despite a much larger sample, the chemical composition of Magellanic Cepheids has been only scarcely investigated.
Aims. For the first time, we study the chemical composition of several Cepheids located in the same populous cluster: NGC 1866, in the Large Magellanic Cloud (LMC). To also investigate the chemical composition of Cepheids at lower metallicity, we look at four targets located in the Small Magellanic Cloud (SMC). Our sample allows us to increase the number of Cepheids with known metallicities in the LMC/SMC by 20%/25% and the number of Cepheids with detailed chemical composition in the LMC/SMC by 46%/50%.
Methods. We use canonical spectroscopic analysis to determine the chemical composition of Cepheids and provide abundances for a good number of α, iron-peak, and neutron-capture elements.
Results. We find that six Cepheids in the LMC cluster NGC 1866 have a very homogeneous chemical composition, also consistent with red giant branch (RGB) stars in the cluster. Period-age relations that include no or average rotation indicate that all the Cepheids in NGC 1866 have a similar age and therefore belong to the same stellar population. Our results are in good agreement with theoretical models accounting for luminosity and radial velocity variations. Using distances based on period-luminosity relations in the near- or mid-infrared, we investigate for the first time the metallicity distribution of the young population in the SMC in the depth direction. Preliminary results show no metallicity gradient along the SMC main body, but our sample is small and does not contain Cepheids in the inner few degrees of the SMC.

Abstract Copyright: © ESO, 2017

Journal keyword(s): stars: variables: Cepheids - Magellanic Clouds - galaxies: star clusters: individual: NGC 1866 - galaxies: star clusters: individual: NGC 1866

Simbad objects: 46

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Number of rows : 46

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 SV* HV 1328 cC* 00 32 54.9174261947 -73 49 19.086114742   14.17 14.116   13.431 ~ 30 0
2 SV* HV 1333 cC* 00 36 03.4614162922 -73 55 58.866210528   15.87 14.702   13.820 ~ 23 0
3 SV* HV 1335 cC* 00 36 55.6923398590 -73 56 28.055695177   15.399 14.746   13.983 ~ 31 0
4 SV* HV 817 cC* 00 39 16.5692812473 -72 01 58.302902914   14.44 13.847   13.088 ~ 35 0
5 SV* HV 1365 cC* 00 41 49.0804221683 -73 43 42.179739346   15.672 15.080   14.221 ~ 41 0
6 SV* HV 822 cC* 00 41 55.4775921384 -73 32 23.609186717   14.39 14.524   13.618 ~ 27 0
7 SV* HV 823 cC* 00 43 48.4444591659 -73 36 48.759833880   13.99 13.864   12.790 ~ 40 0
8 OGLE SMC-CEP-921 s*y 00 46 53.1110749320 -72 42 51.737002042   12.67 12.04   11.421 G0Iab 58 0
9 SV* HV 829 cC* 00 50 28.7967644603 -72 45 09.212650923 12.97 12.26 11.63   11.017 G0Ib 78 0
10 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9610 1
11 SV* HV 834 cC* 00 53 42.6455452168 -72 17 13.635274374   12.48 11.89   11.268 F2Ib 61 0
12 SV* HV 837 cC* 00 55 56.0569263828 -71 59 02.692782547   14.16 13.233   12.297 ~ 61 0
13 SV* HV 847 cC* 01 01 02.6889668865 -72 11 54.229938936   14.96 13.907   13.035 ~ 35 0
14 SV* HV 1954 cC* 01 04 00.3154946448 -72 13 59.864395541   13.94 14.003   13.254 ~ 34 0
15 SV* HV 2064 cC* 01 08 11.5815339725 -72 31 18.348679068   13.89 13.732   12.768 ~ 34 0
16 SV* HV 2195 cC* 01 14 28.0645476624 -72 39 53.532454980   14.02 13.115   12.144 F5Ib 45 0
17 V* BF Tuc cC* 01 17 52.9975933947 -73 37 25.153275568 14.94 14.51 13.72   12.89 F0 33 0
18 V* ST Hyi cC* 01 40 32.2014332345 -74 30 25.593040870   13.49 13.289   12.289 ~ 28 0
19 SV* HV 11211 cC* 02 20 49.4876820936 -73 05 08.320955074   14.88 13.836   13.125 ~ 25 0
20 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5794 1
21 SV* HV 12197 Ce* 05 13 13 -65 30.8   16.741 16.102     ~ 28 0
22 SV* HV 12199 Ce* 05 13 19 -65 29.5   16.916 16.289     ~ 30 0
23 OGLE LMC-CEP-3721 cC* 05 13 20.7914110141 -65 24 57.730298437   16.20 15.70 15.97 15.30 ~ 5 0
24 SV* HV 12198 cC* 05 13 26.6694544251 -65 27 04.933284395   16.627 15.970   15.230 ~ 40 0
25 Cl* NGC 1866 SAB V1 * 05 13 30.8 -65 25 37           ~ 4 0
26 SV* HV 12200 Ce* 05 13 36 -65 28.1   16.913 16.247     ~ 15 0
27 Cl* NGC 1866 SAB V4 Ce* 05 13 37.8 -65 26 55   16.715 16.068     ~ 15 1
28 NGC 1866 GlC 05 13 38.920 -65 27 52.75   9.98 9.73     ~ 389 0
29 SV* HV 12202 Ce* 05 13 39 -65 29.0   16.756 16.080     ~ 28 0
30 Cl* NGC 1866 SAB V5 * 05 13 40.0 -65 30 33   16.13 15.67     ~ 4 0
31 SV* HV 12203 Ce* 05 13 40 -65 29.6   16.811 16.140     ~ 29 0
32 MACHO 59.5436.172 Ce* 05 13 41.911 -65 27 59.98   16.696 16.54 16.02   ~ 13 0
33 Cl* NGC 1866 WE 1 Ce* 05 13 42.4 -65 27 10   16.622 15.973     ~ 12 0
34 Cl* NGC 1866 ROB B430 Ce* 05 13 42.9 -65 27 00   16.773 16.159     ~ 13 0
35 SV* HV 12204 cC* 05 13 57.8739395146 -65 28 39.329976067   16.18 15.715   15.076 ~ 32 0
36 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 15063 1
37 Cl* NGC 1866 W 4212 Ce* ~ ~   17.871 16.658     ~ 8 0
38 Cl* NGC 1866 WE 6 Ce* ~ ~           ~ 7 0
39 Cl* NGC 1866 WE 7 Ce* ~ ~           ~ 6 0
40 Cl* NGC 1866 WS 9 Ce* ~ ~           ~ 4 0
41 Cl* NGC 1866 WE 8 Ce* ~ ~   16.76 16.15     ~ 9 0
42 Cl* NGC 1866 W 3575 Ce* ~ ~   16.733 15.950     ~ 6 0
43 Cl* NGC 1866 WE 2 Ce* ~ ~           ~ 11 0
44 Cl* NGC 1866 W 3671 Ce* ~ ~   16.73 16.06     ~ 10 0
45 Cl* NGC 1866 WS 5 Ce* ~ ~           ~ 5 0
46 Cl* NGC 1866 WS 11 Ce* ~ ~           ~ 5 0

    Equat.    Gal    SGal    Ecl

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2020.12.02-11:49:57

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