J/ApJS/271/28 β Cephei pulsating variables from TESS and Gaia (Shi+, 2024)
Observational properties of 155 β Cephei pulsating variable stars.
Shi X.-D., Qian S.-B., Zhu L.-Y., Li L.-J., Zhao E.-G., Lin W.-X.
<Astrophys. J. Suppl. Ser., 271, 28 (2024)>
=2024ApJS..271...28S 2024ApJS..271...28S
ADC_Keywords: Photometry, UBV; Parallaxes, trigonometric; Extinction;
Effective temperatures; Stars, variable
Keywords: Massive stars ; Pulsating variable stars
Abstract:
β Cephei pulsating variable (BCEP) stars are the most massive
pulsating variable stars in the main sequence, exhibiting both p- and
g-mode pulsations. In this study, we identified 155 BCEP stars or
candidates using data from TESS and Gaia, of which 83 were first
confirmed as BCEP stars. They have visual magnitudes ranging from 8 to
12mag and effective temperatures between approximately 20000 and
30000K, while the parallaxes of most targets are between 0.2 and
0.6mas. The study indicates that these BCEP stars have pulsation
periods ranging from 0.06 to 0.31 days, with amplitudes ranging from
0.1 to 55.8 mmag in the TESS band. Additionally, the number of BCEP
stars increases as the pulsation amplitude decreases. These targets
align with the distribution region of BCEP stars in the
luminosity-period (L-P) and temperature-period diagrams. We have
updated the L-P relation of BCEP stars. The Hertzsprung-Russell
diagram indicates that these targets are in the main-sequence
evolutionary phase, with masses ranging from 7 to 20M☉ and
luminosities between 2800 and 71000L☉. They are almost in the
theoretical instability region of BCEP stars but as previously
reported, this region at the low-mass end (red) is not filled. The
distribution of the pulsation constant indicates that the dominant
pulsation periods of BCEP stars consist mainly of low-order p-mode
pulsations with a high proportion of radial fundamental modes. These
BCEP stars are excellent objects for enhancing our understanding of
the structure and evolution of massive stars through asteroseismology.
Description:
We acquired the TESS photometric data with a 2 minute short cadence
for sectors 1-55 from the Mikulski Archive for Space Telescopes
database.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 105 155 Catalog of β Cephei pulsating variable (BCEP)
stars observed by TESS and Gaia
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See also:
B/gcvs : General Catalogue of Variable Stars (Samus+, 2007-2017)
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
I/350 : Gaia EDR3 (Gaia Collaboration, 2020)
IV/39 : TESS Input Catalog version 8.2 (TIC v8.2) (Paegert+, 2021)
I/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)
I/358 : Gaia DR3 Part 4. Variability (Gaia Collaboration, 2022)
J/ApJS/158/193 : Catalog of Galactic β Cephei stars (Stankov+, 2005)
J/A+A/477/917 : Beta Cephei stars in the ASAS-3 data. II. (Pigulski+, 2008)
J/AJ/156/102 : TESS Input Catalog & Candidate Target List (Stassun+, 2018)
J/MNRAS/493/5871 : TESS A and B stars and the Maia variables (Balona+, 2020)
J/AJ/160/32 : beta Cephei LCs from KELT project (Labadie-Bartz+, 2020)
J/MNRAS/495/2738 : Luminosities of slowly pulsating B stars (Pedersen+, 2020)
J/AJ/161/46 : (O-C) curve of the binary system KIC 06852488 (Shi+, 2021)
J/ApJS/259/50 : EA-type eclipsing binaries observed by TESS (Shi+, 2022)
J/ApJS/265/33 : OB pulsating stars with TESS, LAMOST & Gaia (Shi+, 2023)
J/ApJS/268/16 : Pulsating B stars from TESS, LAMOST & Gaia DR3 (Shi+, 2023)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 9 I9 --- TIC [2323229/469223889] TESS Identifier
11- 16 F6.2 mas plx [0.1/1.5]? Parallax (1)
18- 22 F5.2 mag Vmag [8/12] Apparent V band magnitude, TESS Input
Catalog or SIMBAD
24- 28 F5.2 mag BCmag [-3/-1.9] Bolometric correction
30- 33 F4.2 mag Avmag [0/4.2] V-band interstellar extinction, Gaia
A0-HS
35- 39 I5 K Teff [19719/29781] Effective temperature, Gaia
Extended Stellar Parametrizer for Hot Stars
(ESP-HS)
41- 44 I4 K e_Teff [109/4345] Uncertainty in Teff
46- 51 F6.2 [Lsun] logL [3/4.9]? Log luminosity
53- 63 F11.9 d Per [0.059/0.31] Period
65- 75 F11.9 d e_Per [1e-09/8e-09] Uncertainty in Per
77- 81 F5.2 mmag Amp [0.1/56] Amplitude, TESS-band light curve
83- 86 F4.2 mmag e_Amp [0.01/0.06] Uncertainty in Amp
88- 97 A10 --- Comm Comments (2)
99- 105 A7 --- Flag Flag (s) (3)
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Note (1): In general parallax is from Gaia DR3, but DR2 was used for outliers;
Note (2): The capital letter "C" in the parentheses represents targets
that may be contaminated by neighboring stars in the TESS
photometry apertures.
Note (3): Some targets that are also listed in other literature are
given as follows:
1 = listed as BCEP stars by Labadie-Bartz+ 2020, J/AJ/160/32
(1) = listed as candidates by Labadie-Bartz+ 2020, J/AJ/160/32
2 = listed as BCEP stars by Balona & Ozuyar 2020, J/MNRAS/493/5871
(2) = listed in the Catalog of Balona & Ozuyar 2020, J/MNRAS/493/5871
but not as BCEP stars
3 = listed as MS oscillators by Gaia DR3
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 29-Apr-2024