J/AJ/163/226 Classifying Be Star Variability with TESS I. (Labadie-Bartz+, 2022)
Classifying Be Star Variability With TESS.
I. The Southern Ecliptic.
Labadie-Bartz J., Carciofi A.C., Henrique de Amorim T., Rubio A.,
Luiz Figueiredo A., Ticiani dos Santos P., Thomson-Paressant K.
<Astron. J., 163, 226 (2022)>
=2022AJ....163..226L 2022AJ....163..226L
ADC_Keywords: Stars, Be; Stars, variable; Photometry, RI
Keywords: Be stars ; Pulsating variable stars ; Stellar mass loss ;
Photometry ; Light curves ; Early-type emission stars ;
Circumstellar disks ; Multi-periodic variable stars
Abstract:
TESS photometry is analyzed for 430 classical Be stars observed in the
first year of the mission. The often complex and diverse variability
of each object in this sample is classified to obtain an understanding
of the behavior of this class as a population. Ninety-seven percent of
the systems are variable above the noise level, with timescales
spanning nearly the entire range of what is accessible with TESS, from
tens of minutes to tens of days. The variability seen with TESS is
summarized as follows. Nearly every system contains multiple periodic
signals in the frequency regime between about 0.5 and 4/day. One or
more groups of closely spaced frequencies is the most common feature,
present in 87% of the sample. Among the Be stars with brightening
events that are characteristic of mass ejection episodes (18% of the
full sample, or 31% of early-type stars), all have at least one
frequency group, and the majority of these (83%) show a concurrent
temporary amplitude enhancement in one or more frequency groups. About
one-third (34%) of the sample is dominated by longer-term trends
(timescales >2day). Low-frequency stochastic signals are prominent in
about 25% of the sample, with varying degrees of intensity.
Higher-frequency signals (6<f<15/day) are sometimes seen (in 15% of
the sample) and in most cases likely reflect p-mode pulsation. In rare
cases (∼3%), even higher frequencies beyond the traditional p-mode
regime (f>15/day) are observed.
Description:
NASA Transiting Exoplanet Survey Satellite (TESS) is a photometric
mission performing wide-field photometry over nearly the entire sky.
The four identical cameras of TESS cover a combined field of view of
24x96deg. During the first year of TESS operations, nearly the entire
southern ecliptic sky was observed in 13 sectors, with each sector
being observed for 27.4days. TESS records red optical light with a
wide bandpass spanning roughly 600-1000nm, centered on the traditional
Cousins I band.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 188 543 Table of full sample (including the non-Be stars)
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See also:
B/gcvs : General Catalogue of Variable Stars (Samus+, 2007-2017)
III/17 : Early-Type Emission-Line Stars (Wackerling 1970)
III/67 : Catalogue of Be stars (Jaschek+, 1982)
III/135 : Henry Draper Catalogue and Extension (Cannon+ 1918-1924; ADC 1989)
IX/10 : ROSAT All-Sky Bright Source Catalogue (1RXS) (Voges+ 1999)
I/276 : Tycho Double Star Catalogue (TDSC) (Fabricius+ 2002)
III/260 : General Catalogue of Ap and Am stars (Renson+ 2009)
IV/38 : TESS Input Catalog - v8.0 (TIC-8) (Stassun+, 2019)
J/AJ/107/1556 : Late B-type stars classification (Garrison+, 1994)
J/A+AS/104/315 : Member of Herbig Ae/Be stellar group (The+ 1994)
J/ApJS/99/135 : Rotation and Spectral Peculiarities (Abt+ 1995)
J/A+A/304/235 : UBV Photometry of phi Per (Bozic+, 1995)
J/A+A/378/861 : Spectroscopy of Be stars (Chauville+, 2001)
J/A+A/368/912 : Polarization & rotational veloc. of Be stars (Yudin, 2001)
J/AJ/124/2039 : LMC Blue variable stars from MACHO (Keller+, 2002)
J/A+A/409/275 : Rotation and magnetic field in omega Ori (Neiner+, 2003)
J/AcA/54/207 : Ephemerids of eclipsing binaries (Kreiner, 2004)
J/AJ/127/2659 : CHANDRA observations of NGC 2264 (Ramirez+, 2004)
J/A+A/440/305 : Fundamental param. of fast-rotating B stars (Fremat+, 2005)
J/ApJS/158/193 : Catalog of Galactic β Cephei stars (Stankov+, 2005)
J/other/NewA/10.325 : 2MASS observations of Be stars (Zhang+, 2005)
J/A+A/451/1053 : Fundamental parameters of Be stars (Fremat+, 2006)
J/ApJ/647/1375 : BV light curves of γ Cas (Smith+, 2006)
J/ApJ/652/458 : BVRHα photom. candidates Be stars (Wisniewski+, 2006)
J/ApJ/686/1280 : Discovery hot subdwarf companion to FY CMa (Peters+, 2008)
J/A+A/477/917 : Beta Cephei stars in the ASAS-3 data. II. (Pigulski+, 2008)
J/A+A/506/95 : Fourier analysis of HD 49330 CoRoT light curve (Huat+, 2009)
J/AJ/137/3358 : Speckle interferometry of massive stars (Mason+, 2009)
J/A+A/506/1055 : Hot stars emitting in X-ray. I. (Naze, 2009)
J/AJ/140/328 : LMC High-amplitude delta Scuti stars (Garg+, 2010)
J/A+A/542/A116 : Rotation in A-F stars (Ammler-von Eiff+, 2012)
J/MNRAS/424/1925 : Spectrocopic Binarity of O and B type stars (Chini+, 2012)
J/ApJ/760/10 : BV light curves of γ Cas (1997-2011) (Henry+, 2012)
J/A+A/545/A121 : ο Puppis spectra (Koubsky+, 2012)
J/MNRAS/426/2738 : Magnetic properties of ω Ori (Neiner+, 2012)
J/A+A/555/A83 : X-ray properties of HM1 and IC2944/2948 (Naze+, 2013)
J/AJ/149/7 : SDSS-III/APOGEE. I. Be stars (Chojnowski+, 2015)
J/MNRAS/458/3479 : SVM selection of WISE YSO Candidates (Marton+, 2016)
J/ApJ/828/47 : Radial velocities of the Be star HR 2142 (Peters+, 2016)
J/AJ/152/207 : Spectroscopic Indicators in SeisMic Archive (Rainer+, 2016)
J/A+A/595/A132 : Be star rotational velocities distribution (Zorec+, 2016)
J/MNRAS/465/2432 : MiMeS magnetic analysis of O-type stars (Grunhut+, 2017)
J/AJ/153/252 : Photom. variability BeSS-KELT stars (Labadie-Bartz+, 2017)
J/MNRAS/466/546 : Parameters for the 172 λ Boo stars (Murphy+, 2017)
J/MNRAS/474/5287 : BeSOS Be stars stellar parameters (Arcos+, 2018)
J/A+A/610/A70 : 28 Cygni BRITE and SMEI satellite photometry (Baade+, 2018)
J/MNRAS/479/2909 : Variability Galactic Be stars using ASAS-3 (Bernhard+, 2018)
J/A+A/618/A110 : IR nebulae around bright massive stars (Bodensteiner+, 2018)
J/MNRAS/480/2953 : Catalogue of CP stars (HgMn, ApBp, AmFm) (Ghazaryan+, 2018)
J/AJ/155/53 : Outbursts & disk variability Be stars (Labadie-Bartz+, 2018)
J/A+A/619/A148 : Hot stars observed by XMM-Newton. II. (Naze+, 2018)
J/A+A/613/A70 : Be stars in the exofield of CoRoT. II. (Semaan+, 2018)
J/A+A/609/A108 : Stellar parameters Be stars with X-shooter (Shokry+, 2018)
J/AJ/156/102 : TESS Input Catalog & Candidate Target List (Stassun+, 2018)
J/A+A/641/A42 : Main-sequence comp to massive Be stars (Bodensteiner+, 2020)
J/A+A/640/A36 : OB stars TESS phot. & HR spectroscopy (Bowman+, 2020)
J/A+A/639/A81 : Variability of OB stars (Burssens+, 2020)
J/AJ/160/32 : beta Cephei light curves KELT project (Labadie-Bartz+, 2020)
J/AJ/159/119 : HST emission line survey of Andromeda. I.(Peters+, 2020)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 10 I10 --- TIC Input Catalog identifier
12- 30 A19 --- OName Common name
32- 41 A10 --- SpT Spectral type, BeSS database
43- 43 I1 --- q [0/1] Data quality (1)
45- 45 A1 --- Be Be type (2)
47- 59 A13 --- signals Signals (3)
61- 61 I1 --- Ns [0/8]? Number of group identified in light curve
63- 63 A1 --- tgs Typical groups (4)
65- 68 F4.2 /d fg1 [0/3.28]? Central frequency of g1
70- 73 F4.2 /d fg2 [0.8/6.53]? Central frequency of g2
75- 78 A4 --- gratio Stronger group?
80- 84 F5.2 mag Tmag [4.05/12.73] TESS Magnitude
86- 92 F7.4 --- contratio [0.0001/14.7] Contamination ratio (5)
94-109 F16.12 deg RAdeg [0.93/360] Right Ascension (J2000)
111-125 F15.11 deg DEdeg [-80.2/18.6] Declination (J2000)
127-155 A29 --- SectorsC1 TESS Sectors, C1
157-188 A32 --- SectorsC3 TESS Sectors, C3
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Note (1): Quality as follows:
0 = the system was either not observed by TESS in Cycle 1, or there were
significant problems with the data (including severe blending where
it cannot be determined from which source(s) the detected signals
originate; 64 occurrences).
Note (2): Be type as follows:
Y = classical Be star (410 occurrences)
S = classical Be designation may be suspect, but there is insufficient
evidence to reject it (20 occurrences)
U = rejected as a classical Be star but the nature of the system is not
necessarily known (14 occurrences)
N = Systems known to be something other than a classical Be star
(35 occurrences)
""= Star with insufficient data or that is rejected from the
sample, subsequent fields are also set to nulls (64 occurrences)
Note (3): signals values as follows:
S = indicate the presence of stochastic variability;
I = when isolated signals exist (and ?I+? when there are harmonics);
L = low-frequency signals dominate;
H = high frequency signals exist;
V = very high frequency signals exist;
F = systems with flickers (and ?F+? when an enhancement in frequency
groups accompanies one or more flickers);
G = there are frequency groups.
Note (4): Typical groups as follows:
Y = the system has groups in the typical configuration (313 occurrences)
? = this is unclear (7 occurrences)
N = there are not groups in the typical configuration (110 occurrences)
Note (5): the ratio of flux from neighboring stars in a typical aperture
divided by the flux of the target star.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Coralie Fix [CDS], 14-Sep-2022