2012A&A...544A..64A


Query : 2012A&A...544A..64A

2012A&A...544A..64A - Astronomy and Astrophysics, volume 544A, 64-64 (2012/8-1)

Open clusters. I. Fundamental parameters of B stars in NGC 3766 and NGC 4755.

AIDELMAN Y., CIDALE L.S., ZOREC J. and ARIAS M.L.

Abstract (from CDS):

Spectroscopic investigations of galactic open clusters are scarce and limited to a reduced sample of cluster members. We intend to perform a complete study of the physical parameters of two galactic clusters as well as of their individual members. To carry out this study, we used the BCD (Barbier-Chalonge-Divan) spectrophotometric system, which is based on the study of the Balmer discontinuity and is independent of interstellar and circumstellar extinction. Additional physical properties were derived from the line profiles (FWHM) and stellar evolution models. We analyzed low-resolution spectra around the Balmer discontinuity for normal B-type and Be stars in two open clusters: NGC 3766 and NGC 4755. We determined the stellar fundamental parameters, such as effective temperatures, surface gravities, spectral types, luminosity classes, absolute and bolometric magnitudes, and color gradient excesses. The stellar rotation velocity was also determined. Complementary information, mainly stellar mass, age, and radius of the star population were calculated using stellar evolution models. In some cases, the stellar fundamental parameters were derived for the first time. The obtained results allowed us also to determine the reddening, age, and distance to the clusters. The cluster parameters obtained through the BCD method agree very well with those derived from classical methods based on photometric data. The BCD system also provides physical properties of the star members. This study enables us to test the good behavior of Mbol1,D)-calibrations and detect systematic discrepancies between logg estimates from model atmospheres and those derived from stellar evolution models. To improve our knowledge on the formation and evolution of the clusters, more statistical studies on the initial mass luminosity and angular momentum distributions should be addressed. Therefore, the BCD spectrophotometric system could be a powerful tool for studying far galactic and extragalactic clusters with the generation of large telescopes and the multi-object technique.

Abstract Copyright:

Journal keyword(s): open clusters and associations: individual: NGC 3766 - stars: emission-line, Be - stars: fundamental parameters - open clusters and associations: individual: NGC 4755 - stars: early-type

Simbad objects: 59

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Number of rows : 59
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 HD 60848 Be* 07 37 05.7325392528 +16 54 15.300327852 5.55 6.67 6.87     O8:V:pe 134 0
2 * eta Hya bC* 08 43 13.4749927 +03 23 55.186711 3.380 4.100 4.300 4.37 4.56 B3V 391 1
3 NAME Car Arm PoG 10 00 -60.0           ~ 414 1
4 HD 306644 EB* 11 34 50.8899727368 -61 27 56.598565788   10.24 10.19     B8 6 0
5 HD 306657 Be* 11 35 15.1705815168 -61 41 59.551771488   10.383 10.299 10.36   B2Ve 28 0
6 HD 306793 Be* 11 35 22.0708509960 -61 32 10.949862480   10.606 10.532 10.84   B3Vn 23 0
7 V* V910 Cen LP* 11 35 44.9538524256 -61 34 41.020805424 11.60 9.106 6.859     M0Ib 51 0
8 HD 100840 * 11 35 47.1108851352 -61 33 37.891146528 7.39 8.051 8.022 8.98   B1/2(Ib) 32 0
9 HD 306785 * 11 35 48.5749575648 -61 29 19.187001744   9.671 9.663     B3 19 0
10 HD 308740 * 11 35 48.8866201704 -61 45 03.999884472   11.002 10.893     B5 10 0
11 CPD-60 3098 * 11 35 52.2496358448 -61 38 07.538625996 9.02 9.596 9.591 9.96   B2V 20 0
12 HD 306784 * 11 35 54.2075403720 -61 24 51.472178172   9.853 9.870     B5 5 0
13 HD 100856 Be* 11 35 55.4594969064 -61 36 13.744109088 7.29 8.52 8.57 9.41   B2IVp(e) 44 0
14 HD 306794 * 11 36 04.5016985184 -61 35 22.744617072 8.03 8.03 8.11 9.03   OB 25 0
15 HD 308743 * 11 36 04.8350714136 -61 50 34.584031896   10.87 10.74     B8 3 0
16 HD 306797 Be* 11 36 05.4841182288 -61 42 06.058771524 9.19 9.93 9.78 10.06   B5II 41 0
17 HD 306798 Be* 11 36 09.3687546672 -61 41 41.574344856 8.84 9.74 9.64 9.83   Be 36 0
18 CPD-60 3125 Be* 11 36 09.5641183512 -61 35 38.145238836 8.58 9.15 9.13 9.72   B2IVne 34 0
19 CPD-60 3128 Be* 11 36 11.865192 -61 35 50.27604 7.78     9.27   B2IV-V 30 0
20 CPD-60 3131 * 11 36 12.0290610408 -61 35 10.635848736   11.3 11.3     B 8 0
21 CD-60 3626A Be* 11 36 12.3647329632 -61 32 44.968102584       10.24   B3V 8 0
22 CD-60 3626B * 11 36 12.5246565264 -61 32 40.225579368   9.5 9.4 10.50   B3Vn 17 0
23 NGC 3766 OpC 11 36 15 -61 37.0   5.66 5.3     ~ 197 0
24 CPD-60 3135 * 11 36 15.7738371888 -61 36 08.150540688   11.138 11.070     B 8 0
25 V* BF Cen EB* 11 36 17.0350090608 -61 28 01.402061376   8.508 8.484   8.619 B8 46 0
26 Cl* NGC 3766 MG 116 * 11 36 18.7483286184 -61 37 10.236370080   12.500 12.164     ~ 4 0
27 CPD-60 3138 * 11 36 18.8562650640 -61 37 03.877192128   11.219 11.126     ~ 7 0
28 HD 100943 Em* 11 36 28.3717504776 -61 39 54.514770300 6.66 6.804 6.655 8.00   B1Iab/b 63 0
29 HD 306791 Be* 11 36 31.5551060424 -61 34 25.733980380 8.03 8.507 8.429 9.35   B2III 43 0
30 * tet Crt PM* 11 36 40.9133537 -09 48 08.091238   4.604 4.673     B9.5V 205 0
31 HD 100969 * 11 36 41.8917551472 -61 31 37.393274460 8.47 9.074 9.055     B2/5 23 0
32 HD 306787 * 11 36 48.3049261656 -61 26 41.916972336   10.805 10.825 10.888   B9 2 0
33 Cl* NGC 3766 MG 177 * 11 36 50.3311305360 -61 40 07.713089364           ~ 2 0
34 HD 306800 * 11 37 10.9345626672 -61 39 22.662040824   10.817 10.909     B9 10 0
35 HD 306778 * 11 37 21.4372199592 -61 26 04.910768376   9.53 9.50     B8 7 0
36 HD 308852 * 11 37 41.9543696208 -61 45 42.774079032   11.0 10.6     B5 6 0
37 HD 306788 * 11 37 45.7815575448 -61 29 30.065167392   10.3 10.0     B9 5 0
38 CPD-60 3087 * 11 37 48.8540520624 -61 45 05.195786436   11.23 10.99     ~ 9 0
39 HD 312079 * 12 53 10.2301911048 -60 25 59.480339268 9.66 10.24 10.08 10.22   B5 20 0
40 HD 312080 * 12 53 14.2580848896 -60 27 38.129667876   10.23 10.10 10.23   B9 19 0
41 CD-59 4454 Pu* 12 53 20.6734801416 -60 23 16.843450812 9.26 9.90 9.74 10.03   B1V 51 0
42 HD 111904 V* 12 53 21.8944330272 -60 19 42.561114312 5.75 6.05 5.77 7.09   B9Iab 104 0
43 CPD-59 4530 * 12 53 22.5904404528 -60 23 47.624386920 11.31 11.66 11.45 11.48   B3V 20 0
44 CPD-59 4531 * 12 53 24.2615260128 -60 21 30.846183588 10.44 11.01 10.89     B2.5Vn 19 0
45 CPD-59 4532 bC* 12 53 25.6733913792 -60 22 00.097867236 9.72 10.288 10.142     B1V 27 0
46 CPD-59 4540 ** 12 53 33.1564978536 -60 24 33.251907427 9.21 10.185 10.035 10.446   B1.5V 20 0
47 CPD-59 4542 * 12 53 35.4991773048 -60 23 46.681317816 9.2 9.91 9.73 9.99   B1.5V 35 1
48 V* BU Cru EB* 12 53 37.6193092848 -60 21 25.425832356 6.49 7.04 6.84 7.55   B2Ib 108 0
49 NGC 4755 OpC 12 53 40 -60 22.3           ~ 275 0
50 CPD-59 4552 * 12 53 46.4935086912 -60 24 12.419407044 7.79 8.337 8.24 9.13   B1III 49 0
51 V* CC Cru El* 12 53 47.2742360136 -60 19 55.349178564 7.44 8.00 7.83 7.68   B2III 32 0
52 * kap Cru SB* 12 53 48.9198156672 -60 22 34.469837436 5.62 6.12 5.94 7.12   B5I 124 0
53 V* CN Cru EB* 12 53 49.4982338184 -60 23 02.952242196 7.87 8.69 8.58     B1V 34 0
54 CPD-59 4559 Be* 12 53 51.5776218216 -60 23 16.874046276 9.76 10.254 9.983     B2IVne 30 0
55 NGC 4755 202 bC* 12 53 51.7420242144 -60 21 58.595523264 9.56 10.162 10.024     B2IV 25 0
56 LS 2814 bC* 12 53 52.0067925720 -60 22 15.879036216 8.92 9.54 9.38 9.81   B1V 31 0
57 CPD-59 4564 bC* 12 53 57.5386794336 -60 24 58.092625152 8.45 9.12 9.06 9.64   B2III 59 0
58 * 108 Vir * 14 45 30.2044637184 +00 43 02.180202816   5.656 5.665     B9.5V 149 0
59 * 58 Aql * 19 54 44.7948526968 +00 16 25.050363384   5.703 5.631     B9IV 204 0

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2022.08.15-14:46:11

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