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


C.D.S. - SIMBAD4 rel 1.7 - 2020.03.28CET22:35:25

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

Status at CDS:  

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 - 2020
#notes
1 HD 60848 Be* 07 37 05.7328585099 +16 54 15.303398878 5.55 6.67 6.87     O8:V:pe 129 0
2 * eta Hya bC* 08 43 13.4749927 +03 23 55.186711 3.380 4.100 4.300 4.37 4.56 B3V 383 1
3 NAME Car Arm PoG 10 00 -60.0           ~ 373 1
4 HD 306644 EB* 11 34 50.8897586687 -61 27 56.597063830   10.24 10.19     B8 3 0
5 HD 306657 Be* 11 35 15.1700191813 -61 41 59.550147246   10.383 10.299 10.36   B2Ve 24 0
6 HD 306793 Be* 11 35 22.0704661040 -61 32 10.945621376   10.606 10.532 10.84   B3Vn 21 0
7 V* V910 Cen LP* 11 35 44.9537674232 -61 34 41.019250573 11.60 9.106 6.859     M0Ib 40 0
8 HD 100840 * 11 35 47.1107760528 -61 33 37.887981820 7.39 8.051 8.022 8.98   B1/2(Ib) 28 0
9 HD 306785 * 11 35 48.5749352792 -61 29 19.182846944   9.671 9.663     B3 14 0
10 HD 308740 * 11 35 48.8864920793 -61 45 03.998043905   11.002 10.893     B5 6 0
11 CPD-60 3098 * 11 35 52.2498941995 -61 38 07.537377922 9.02 9.596 9.591 9.96   B2V 16 0
12 HD 306784 * 11 35 54.2074502310 -61 24 51.473338422   9.853 9.870     B5 3 0
13 HD 100856 Be* 11 35 55.4592323756 -61 36 13.744784516 7.29 8.52 8.57 9.41   B2IVp(e) 39 0
14 HD 306794 * 11 36 04.5015350877 -61 35 22.743418424 8.03 8.03 8.11 9.03   OB 23 0
15 HD 308743 * 11 36 04.8352503096 -61 50 34.584251239   10.87 10.74     B8 2 0
16 HD 306797 Be* 11 36 05.4838549502 -61 42 06.058548774 9.19 9.93 9.78 10.06   B5II 35 0
17 HD 306798 Be* 11 36 09.3688317648 -61 41 41.572799484 8.84 9.74 9.64 9.83   Be 32 0
18 CPD-60 3125 Be* 11 36 09.5642583289 -61 35 38.141324847 8.58 9.15 9.13 9.72   B2IVne 31 0
19 CPD-60 3128 Be* 11 36 11.865192 -61 35 50.27604 7.78     9.27   B2IV-V 29 0
20 CPD-60 3131 * 11 36 12.0295331254 -61 35 10.632869627   11.3 11.3     B 8 0
21 CD-60 3626A Be* 11 36 12.3648796968 -61 32 44.968547524       10.24   B3V 5 0
22 CD-60 3626B * 11 36 12.5247103224 -61 32 40.221308003   9.5 9.4 10.50   B3Vn 16 0
23 CPD-60 3135 * 11 36 15.7816954252 -61 36 08.111208617   11.138 11.070     B 8 0
24 V* BF Cen Al* 11 36 17.0350065550 -61 28 01.401506065   8.508 8.484   8.619 B8 37 0
25 NGC 3766 OpC 11 36 18 -61 36.9   5.66 5.3     ~ 180 0
26 Cl* NGC 3766 MG 116 * 11 36 18.7478273891 -61 37 10.233868615   12.500 12.164     ~ 3 0
27 CPD-60 3138 * 11 36 18.8562236464 -61 37 03.875254707   11.219 11.126     ~ 5 0
28 HD 100943 Em* 11 36 28.3715544548 -61 39 54.514836385 6.66 6.804 6.655 8.00   B1Iab/b 59 0
29 HD 306791 Be* 11 36 31.5552738719 -61 34 25.731117578 8.03 8.507 8.429 9.35   B2III 38 0
30 * tet Crt PM* 11 36 40.9133537 -09 48 08.091238   4.604 4.673     B9.5V 198 0
31 HD 100969 * 11 36 41.8927055911 -61 31 37.387646126 8.47 9.074 9.055     B2/5 20 0
32 HD 306787 * 11 36 48.37 -61 26 41.7   9.6       B9 2 0
33 Cl* NGC 3766 MG 177 * 11 36 50.3309046550 -61 40 07.710103234           ~ 2 0
34 HD 306800 * 11 37 10.9343388378 -61 39 22.661424653   10.817 10.909     B9 7 0
35 HD 306778 * 11 37 21.4369826912 -61 26 04.911031250   9.53 9.50     B8 4 0
36 HD 308852 * 11 37 41.9528876219 -61 45 42.769883222   11.0 10.6     B5 4 0
37 HD 306788 * 11 37 45.7815373137 -61 29 30.064416280   10.3 10.0     B9 3 0
38 CPD-60 3087 * 11 37 48.8540595018 -61 45 05.194214696   11.23 10.99     ~ 9 0
39 HD 312079 * 12 53 10.2301906295 -60 25 59.478727528 9.66 10.24 10.08 10.22   B5 19 0
40 HD 312080 * 12 53 14.2583882474 -60 27 38.129491800   10.23 10.10 10.23   B9 17 0
41 CD-59 4454 Pu* 12 53 20.6733731480 -60 23 16.842018998 9.26 9.90 9.74 10.03   B1V 48 0
42 HD 111904 V* 12 53 21.8939526500 -60 19 42.561485784 5.75 6.05 5.77 7.09   B9Iab 99 0
43 CPD-59 4530 * 12 53 22.5902428843 -60 23 47.622691352 11.31 11.66 11.45 11.48   B3V 18 0
44 CPD-59 4531 * 12 53 24.2615264881 -60 21 30.846100118 10.44 11.01 10.89     B2.5Vn 17 0
45 CPD-59 4532 bC* 12 53 25.6731338797 -60 22 00.097922271 9.72 10.288 10.142     B1V 26 0
46 CPD-59 4540 * 12 53 33.1564450551 -60 24 33.249556079 9.21 9.471 9.33     B1.5V 20 0
47 LS 2806 * 12 53 35.4991995489 -60 23 46.679526612 9.2 9.91 9.73 9.99   B1.5V 31 1
48 V* BU Cru EB* 12 53 37.6191876667 -60 21 25.424160921 6.49 7.04 6.84 7.55   B2Ib 99 0
49 NGC 4755 OpC 12 53 39 -60 21.7           ~ 267 0
50 CPD-59 4552 * 12 53 46.4933523228 -60 24 12.416336476 7.79 8.337 8.24 9.13   B1III 45 0
51 V* CC Cru El* 12 53 47.2743079060 -60 19 55.346496966 7.44 8.00 7.83 7.68   B2III 28 0
52 * kap Cru SB* 12 53 48.9195114429 -60 22 34.468234629 5.62 6.12 5.94 7.12   B2/3Ia 119 0
53 V* CN Cru bL* 12 53 49.4981104128 -60 23 02.955358116 7.87 8.69 8.58     B1V 33 0
54 CPD-59 4559 Be* 12 53 51.5776201662 -60 23 16.870573247 9.76 10.254 9.983     B2IVne 27 0
55 NGC 4755 202 bC* 12 53 51.7419348165 -60 21 58.594441515 9.56 10.162 10.024     B2IV 22 0
56 LS 2814 bC* 12 53 52.0073735911 -60 22 15.880025394 8.92 9.54 9.38 9.81   B1V 30 0
57 CPD-59 4564 bC* 12 53 57.5384969135 -60 24 58.089466050 8.45 9.12 9.06 9.64   B2III 53 0
58 * 108 Vir * 14 45 30.2060174766 +00 43 02.178514704   5.656 5.665     B9.5V 143 0
59 * 58 Aql * 19 54 44.7954348711 +00 16 25.053387202   5.703 5.631     B9IV 193 0

    Equat.    Gal    SGal    Ecl

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2020.03.28-22:35:25

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