2013A&A...558A..17O


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.16CEST22:56:00

2013A&A...558A..17O - Astronomy and Astrophysics, volume 558A, 17-17 (2013/10-1)

Probing the ejecta of evolved massive stars in transition. A VLT/SINFONI K-band survey.

OKSALA M.E., KRAUS M., CIDALE L.S., MURATORE M.F. and BORGES FERNANDES M.

Abstract (from CDS):

Massive evolved stars in transition phases, such as luminous blue variables (LBVs), B[e] supergiants (B[e]SGs), and yellow hypergiants (YHGs), are not well understood, and yet crucial steps in determining accurate stellar and galactic evolution models. The circumstellar environments of these stars reveal their mass-loss history, identifying clues to both their individual evolutionary status and the connection between objects of different phases. Here we present a survey of 25 such evolved massive stars (16 B[e]SGs, 6 LBVs, 2 YHGs, and 1 Peculiar Oe star), observed in the K-band with the Spectrograph for INtegral Field Observation in the Near-Infrared (SINFONI; R=4500) on the ESO VLT UT4 8m telescope. The sample can be split into two categories based on spectral morphology: one group includes all of the B[e]SGs, the Peculiar Oe star, and two of the LBVs, while the other includes the YHGs and the rest of the LBVs. The difference in LBV spectral appearance is due to some objects being in a quiescent phase and some objects being in an active or outburst phase. CO emission features are found in 13 of our targets, with first time detections for MWC 137, LHA 120-S 35, and LHA 115-S 65. From model fits to the CO band heads, the emitting regions appear to be detached from the stellar surface. Each star with 12CO features also shows 13CO emission, signaling an evolved nature. Based on the level of 13C enrichment, we conclude that many of the B[e]SGs are likely in a pre-Red Supergiant phase of their evolution. There appears to be a lower luminosity limit of log L/L=5.0 below which CO is not detected. The lack of CO features in several high luminosity B[e]SGs and variability in others suggests that they may in fact be LBV candidates, strengthening the connection between these two very similar transition phases.

Abstract Copyright:

Journal keyword(s): infrared: stars - techniques: spectroscopic - stars: massive - circumstellar matter - stars: evolution

Simbad objects: 39

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Number of rows : 39

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 HD 269 * 00 07 20.2809425443 -32 03 08.544239756   9.66 8.61     K1/2III 6 0
2 M 31 G 00 42 44.330 +41 16 07.50 4.86 4.36 3.44     ~ 10561 1
3 LHA 115-S 6 s*b 00 46 55.0295095056 -73 08 34.139503944 12.14 13.02 12.91   12.52 B0/0.5[e] 76 1
4 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9088 1
5 LHA 115-S 18 Em* 00 54 09.5415603586 -72 41 43.291670748 12.94 13.48 13.82   12.55 B[e] 72 0
6 LHA 115-S 23 Em* 00 55 53.8117943063 -72 08 59.510230206 12.82 13.29 13.25   13.04 B8Ib[e] 31 1
7 HD 5980 WR* 00 59 26.5847969465 -72 09 53.927725716   11.13 11.31   11.029 WN4+O7I: 355 1
8 HD 6884 s*b 01 07 18.2183812921 -72 28 03.658768522   10.32 10.2     B9Ia0ek 111 0
9 M 33 GiG 01 33 50.904 +30 39 35.79 6.17 6.27 5.72     ~ 5019 1
10 CPD-75 116 s*b 01 44 03.8712992159 -74 40 49.801190680   11.54 11.43 11.69   B5Ia[e] 75 0
11 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5373 1
12 HD 268835 s*b 04 56 47.0796207119 -69 50 24.767090336 10.21 10.77 10.63 10.72 10.16 B8[e] 96 0
13 LHA 120-S 12 s*b 04 57 36.7804325423 -67 47 37.378243521 11.833 12.66 12.547 12.56 12.151 B0.5Ie 35 0
14 HD 269006 s*b 05 02 07.3944119328 -71 20 13.118657760 9.93 10.60 10.55 10.43 10.38 LBV 230 0
15 HD 269217 s*b 05 13 38.9188358563 -69 21 08.085451831 11.325 12.084 11.754 12.16 11.54 B5/6Ia[e] 67 0
16 HD 34664 s*b 05 13 52.9943883589 -67 26 54.822130587 11.509 11.88 11.774 11.63 10.991 B0/0.5I[e] 93 0
17 LHA 120-S 93 Em* 05 16 31.7927458109 -68 22 09.269710456 12.537 12.81 12.69 12.79 12.501 A0:I: 29 0
18 V* S Dor sg* 05 18 14.3572490675 -69 15 01.148131817 9.08 10.39 10.25 9.74 9.14 A5Iaeq 337 0
19 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14323 1
20 LHA 120-S 35 Em* 05 27 17.8395729210 -66 22 05.631785570 12.458 11.5 13.056 13.14 12.484 ~ 26 1
21 HD 269599 ** 05 28 22.71 -69 08 31.9   10.741       ~ 60 3
22 HD 269662 sg* 05 30 51.4755593461 -69 02 58.591230109 10.23 10.52 10.28 10.40 10.390 A0Ia 89 0
23 HD 269723 s*y 05 32 24.9647913138 -67 41 53.611350999   10.98 9.91     G4_0 50 0
24 HD 37836 Em* 05 35 16.6331678655 -69 40 38.439677992 9.87 10.736 10.599 10.73 10.164 B0e(q) 72 0
25 HD 37974 s*b 05 36 25.8537892343 -69 22 55.789283933 10.056 11.12 10.99 11.00 10.423 B0.5e 113 0
26 HD 269858 s*b 05 36 43.6942807271 -69 29 47.449383685   10.24 10.15 9.95 9.05 LBV 261 2
27 HD 269953 s*y 05 40 12.1670932520 -69 40 04.852901756   10.83 9.95     G0_0 71 0
28 HD 38489 s*b 05 40 13.3208554964 -69 22 46.485104413 11.236 12.295 11.93 11.79 10.891 B[e] 81 1
29 LHA 120-S 137 Em* 05 41 43.7414829134 -69 37 38.285364895 13.504 14.305 14.199 14.310 13.463 BIaePCyg 15 0
30 LHA 120-S 59 sr* 05 45 29.4734284871 -68 11 45.924367609 13.367 14.22 13.95 14.23 13.651 B0.5IIIe 17 0
31 EM* MWC 137 Ae* 06 18 45.5220562759 +15 16 52.242746933 12.89 13.30 13.759 11.67 10.31 sgB[e]d 220 1
32 WRAY 15-406 Em* 09 36 44.2096715780 -53 28 01.344715143     11.4     B:e 13 0
33 HD 90177 s*b 10 22 53.8426931454 -59 37 28.361118869 9.16 9.66 8 8.15   LBV 300 0
34 * eta Car Em* 10 45 03.5455050 -59 41 03.951060 6.37 7.034 6.21 4.90 4.41 OBepec 2148 0
35 HD 94878 bL* 10 55 58.9150038252 -60 23 33.434805592 8.67 9.37 8.70 8.07   B0/2eq 138 0
36 V* AG Car WR* 10 56 11.5779283438 -60 27 12.809532379 7.00 7.57 6.96 7.73   WN11h 580 0
37 MR 35 s*b 11 08 40.0633818066 -60 42 51.718989987   13.7       LBV 112 0
38 CPD-52 9243 Em* 16 07 02.0295845997 -53 03 45.416876395 12.36 11.84 10.22 9.87   B3Ieq 53 0
39 HD 327083 s*b 17 15 15.3714469957 -40 20 06.793634106 12.07 11.44 10.00 9.64   B6Ieq 52 0

    Equat.    Gal    SGal    Ecl

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2019.10.16-22:56:00

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