2019ApJ...878..155D

Query : 2019ApJ...878..155D

2019ApJ...878..155D - Astrophys. J., 878, 155-155 (2019/June-3)

Short-term variability of evolved massive stars with TESS.

DORN-WALLENSTEIN T.Z., LEVESQUE E.M. and DAVENPORT J.R.A.

Abstract (from CDS):

We present the first results from a study of Transiting Exoplanet Survey Satellite (TESS) Sector 1 and 2 light curves for eight evolved massive stars in the LMC: six yellow supergiants (YSGs) and two luminous blue variables (LBVs), including S Doradus. We use an iterative prewhitening procedure to characterize the short-timescale variability in all eight stars. The periodogram of one of the YSGs, HD 269953, displays multiple strong peaks at higher frequencies than its fellows. While the field surrounding HD 269953 is quite crowded, it is the brightest star in the region, and has infrared colors indicating it is dusty. We suggest HD 269953 may be in a post-red supergiant evolutionary phase. We find a signal with a period of ∼5 days for the LBV HD 269582. The periodogram of S Doradus shows a complicated structure, with peaks below frequencies of 1.5 cycles per day. We fit the shape of the background noise of all eight light curves, and find a red noise component in all of them. However, the power-law slope of the red noise and the timescale over which coherent structures arise changes from star to star. Our results highlight the potential for studying evolved massive stars with TESS.

Abstract Copyright: © 2019. The American Astronomical Society. All rights reserved.

Journal keyword(s): stars: evolution - stars: massive - stars: oscillations - stars: rotation - stars: variables: general

Simbad objects: 20

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Number of rows : 20
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 12317 1
2 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 7988 0
3 HD 268687 s*y 04 50 55.8562324872 -69 25 52.504903884 11.33 11.12 10.730 10.70 10.145 F6Ia 38 0
4 HD 269110 LP* 05 09 10.6083407328 -69 36 12.203504280 12.51 11.76 10.82     G0I: 38 0
5 HD 269331 s?y 05 18 01.8324453648 -69 33 37.767513132   10.56 10.31 9.72 9.869 A5Ia0 37 0
6 V* S Dor sg* 05 18 14.3570612088 -69 15 01.149576912 9.08 10.39 10.25 9.74 9.14 Be3 395 0
7 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 19090 0
8 HD 269582 WR* 05 27 52.6621673400 -68 59 08.488879836 12.206 10.818 11.093 12.70 11.234 WN10h 117 0
9 HD 269593 * 05 28 20.0256671112 -67 40 30.753215904   11.2 11.1     B6I 32 0
10 NGC 2085 Cl* 05 40 08.6 -69 40 20     12.06     ~ 21 0
11 HD 269953 s*y 05 40 12.1666201344 -69 40 04.853223012   10.83 9.95     G0_0 94 0
12 HD 270046 * 05 43 25.1858081160 -69 14 54.629414016 11.98 11.33 10.38 9.52 9.449 G5I 47 0
13 HD 270111 * 05 45 00.6221325504 -67 10 34.289904144 11.38 10.88 10.20     G5I 37 0
14 HD 46769 * 06 35 15.8285310432 +00 53 24.785166300 5.43 5.84 5.86 5.78 5.81 B7Ib-II 94 0
15 HD 268582 * 07 05 50.7141451992 +34 40 11.809028928   11.85 11.22     ~ 4 0
16 * eta Car s*b 10 45 03.545808 -59 41 03.95124 6.37 7.03 6.48 6.123 4.41 LBV 2543 0
17 HD 165688 WR* 18 07 56.9609461704 -19 23 56.863324824 10.46 10.31 9.87 9.85   WN5-6b 162 0
18 * P Cyg s*b 20 17 47.2019733389 +38 01 58.549132671 4.66 5.24 4.82 4.28 4.02 B1-2Ia-0ep 1200 1
19 * bet Cep bC* 21 28 39.5968513 +70 33 38.574681 2.05 3.01 3.23 3.33 3.55 B0.5IIIs 756 0
20 SN 2009ip s*b 22 23 08.26 -28 56 52.4           LBV 406 0

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