J/ApJS/265/33 OB-type pulsating stars with TESS, LAMOST & Gaia (Shi+, 2023)
Observational properties of 155 O- and B-type massive pulsating stars.
Shi X.-D., Qian S.-B., Zhu L.-Y., Liu L., Li L.-J., Zang L.
<Astrophys. J. Suppl. Ser., 265, 33 (2023)>
=2023ApJS..265...33S 2023ApJS..265...33S
ADC_Keywords: Stars, variable; Parallaxes, trigonometric; Photometry; Optical;
Effective temperatures; Stars, B-type
Keywords: Pulsating variable stars ; Massive stars
Abstract:
O- and B-type (OB-type) pulsating stars are important objects for
studying the structure and evolution of massive stars through
asteroseismology. A large amount of data from various sky surveys
provides an unprecedented opportunity to search for and study this
kind of variable star. We identify 155 OB-type pulsating stars or
candidates, including 38 Oe/Be stars or candidates, from the data
observed by TESS, LAMOST, and Gaia, which are almost new. Among the
155 objects, 87 samples are identified as slowly pulsating B (SPB)
stars including 37 objects with pure low-frequency and 50 objects with
both low- and high-frequency pulsation, and 14 samples are identified
as β Cephei pulsating variable (BCEP) stars with both low- and
high-frequency pulsation. An H-R diagram shows that these SPB and BCEP
stars are mainly located in their instability regions and in the
evolutionary stage of the main sequence with mass ranges of
2.5-20M☉ and 7-20M☉, respectively. Two special objects
show Fourier spectra similar to BCEP stars but with different
positions in H-R, period-temperature (P-T), and period-luminosity
(P-L) diagrams. Meanwhile, 52 other targets are identified as
candidates of OB-type pulsating stars. We also derive the preliminary
results of the P-L relation for SPB and BCEP stars, respectively. This
work also indicates that in addition to the H-R diagram, the P-T and
P-L diagrams are also very useful for the classification of SPB and
BCEP stars. Further detailed analysis of these objects can
dramatically increase our understanding of the theories of evolution
and structure for massive OB-type pulsating stars.
Description:
From the Mikulski Archive for Space Telescopes database, we downloaded
the light curves observed by TESS with a 2 minute short cadence.
See Section 2.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 90 103 The catalog of OB-type massive pulsating stars
observed by TESS, LAMOST, and Gaia
table2.dat 53 52 The candidates of OB-type pulsating stars observed
by TESS, LAMOST, and Gaia
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See also:
IV/38 : TESS Input Catalog - v8.0 (TIC-8) (Stassun+, 2019)
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
V/156 : LAMOST DR7 catalogs (Luo+, 2019)
IV/39 : TESS Input Catalog version 8.2 (TIC v8.2) (Paegert+, 2021)
I/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)
J/A+A/393/965 : Intrinsic frequencies of SPB stars (de Cat+, 2002)
J/ApJS/158/193 : Catalog of Galactic β Cephei stars (Stankov+, 2005)
J/A+A/463/243 : Variations of O-B stars in Mercator obs. (De Cat+, 2007)
J/A+A/506/471 : Frequency analysis of CoRoT B stars (Degroote+, 2009)
J/ApJS/208/9 : Intrinsic colors & temp. of PMS stars (Pecaut+, 2013)
J/A+A/580/A23 : Stroemgren-Crawford uvbyβ phot. cat. (Paunzen, 2015)
J/MNRAS/475/478 : delta Scuti pulsating stars LAMOST views (Qian+, 2018)
J/ApJS/235/5 : EA-type EBs observed by LAMOST (Qian+, 2018)
J/AJ/156/102 : TESS Input Cat. & Candidate Target List (Stassun+, 2018)
J/MNRAS/485/2380 : Gaia-derived luminosities of Kepler stars (Murphy+, 2019)
J/other/RAA/19.64 : LAMOST sp. binaries & variable stars (Qian+, 2019)
J/ApJS/244/43 : Binary stars param. from LAMOST & Kepler (Zhang+, 2019)
J/MNRAS/493/5871 : TESS A and B stars and the Maia variables (Balona+, 2020)
J/A+A/639/A81 : Variability of OB stars (Burssens+, 2020)
J/AJ/160/32 : beta Cephei LCs from KELT project (Labadie-Bartz+, 2020)
J/other/RAA/20.163 : Contact binaries in LAMOST DR7 (Qian+, 2020)
J/ApJS/257/54 : Early-type star param. from LAMOST LRS & MRS (Guo+, 2021)
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)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 I9 --- TIC [1827744/712312017] TESS identifier
11- 14 F4.2 mas plx [0.1/7.34] Gaia parallax
16- 20 F5.2 mag Vmag [5.36/13.5] Apparent V magnitude (G1)
22- 26 I5 K Teff [9549/32447] Effective temperature
28- 31 I4 K e_Teff [46/4422]? Teff uncertainty
33 I1 --- r_Teff [1/4] Reference on Teff (G2)
35- 37 A3 --- Be Be = Hα emission-line profile detected
from LAMOST
39- 42 F4.2 [Lsun] logL [1.6/4.63] Log of the luminosity
44- 48 A5 --- FS Fourier spectra
50- 57 A8 --- OT Object type (1)
59 A1 --- f_TIC C = may be contaminated by nearby stars
in the TESS photometry apertures
61- 69 F9.7 d Per [0.07/9.2] Period
71- 79 F9.7 d e_Per [2e-07/0.01] Per uncertainty
81- 85 F5.2 mmag Amp [0.13/28.8] Amplitude
87- 90 F4.2 mmag e_Amp [0.01/0.2] Amp uncertainty
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Note (1): Object type as follows:
SPB = Slowly pulsating B stars (87 occurrences)
BCEP = β Cephei pulsating variable stars (14 occurrences)
BCEP/SPB = 2 occurrences
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 I9 --- TIC [16700873/470472700] TESS identifier
11- 14 F4.2 mas plx [0.14/6.7] Gaia parallax
16- 20 F5.2 mag Vmag [4.4/13] Apparent V magnitude (G1)
22- 26 I5 K Teff [9760/36131] Effective temperature
28- 31 I4 K e_Teff [10/1856]? Teff uncertainty
33 I1 --- r_Teff [1/4] Reference on Teff (G2)
35- 37 A3 --- Be Be or Oe = Hα emission-line profile
detected from LAMOST
39- 42 F4.2 [Lsun] logL [1.45/5] Log of the luminosity
44- 51 A8 --- OT Object type
53 A1 --- f_TIC C = may be contaminated by nearby stars
in the TESS photometry apertures
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Global notes:
Note (G1): The visual magnitude is from the TESS Input Catalog (TIC; see IV/38)
or SIMBAD.
Note (G2): Source for effective temperature as follows:
1 = Gaia Extended Stellar Parameterizer for Hot Stars (ESP-HS)
2 = LAMOST derived by Guo+ 2021, J/ApJS/257/54 (LAMOST_Guo)
3 = Gaia General Stellar Parameterizer from Photometry (GSP-Phot)
4 = temperature estimation from the spectral type given by LAMOST
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History:
From electronic version of the journal
References:
Shi et al. Paper II. 2023ApJS..268...16S 2023ApJS..268...16S Cat. J/ApJS/268/16
(End) Emmanuelle Perret [CDS] 21-Nov-2023