J/ApJ/844/66 The Sco-Cen Rotation Catalogue - SCRC (Mellon+ 2017)
Angular momentum evolution of young stars in the nearby Scorpius-Centaurus OB
association.
Mellon S.N., Mamajek E.E., Oberst T.E., Pecaut M.J.
<Astrophys. J., 844, 66-66 (2017)>
=2017ApJ...844...66M 2017ApJ...844...66M (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, open ; Binaries, eclipsing ; Photometry
Keywords: binaries: eclipsing -
open clusters and associations: individual: Sco-Cen -
starspots - stars: pre-main sequence - stars: rotation
Abstract:
We report the results of a study of archival SuperWASP light curves
for stars in Scorpius-Centaurus (Sco-Cen), the nearest OB association.
We use SuperWASP time-series photometry to extract rotation periods
for 189 candidate members of the Sco-Cen complex and verify that 162
of those are members of the classic Sco-Cen subgroups of Upper
Scorpius (US), Upper Centaurus-Lupus (UCL), and Lower Centaurus-Crux
(LCC). This study provides the first measurements of rotation periods
explicitly for large samples of pre-main-sequence (pre-MS) stars
spanning the UCL and LCC subgroups. Our final sample of 157
well-characterized pre-MS stars spans ages of ∼10-20Myr, spectral
types of ∼F3-M0, and masses of M~=0.3-1.5 M☉N. For this
sample, we find a distribution of stellar rotation periods with a
median of Prot~=2.4-days, an overall range of 0.2<Prot<8-days, and
a fairly well-defined mass-dependent upper envelope of rotation
periods. This distribution of periods is consistent with recently
developed stellar angular momentum evolution models. These data are
significant because they represent an undersampled age range and the
number of measurable rotation periods is large compared to recent
studies of other regions. We also search for new examples of eclipsing
disk or ring systems analogous to 1SWASP J140747.93-394542.6 (J1407),
but find none. Our survey yielded five eclipsing binaries, but only
one appears to be physically associated with the Sco-Cen complex.
V2394 Oph is a heavily reddened (AV~=5mag) massive contact binary in
the LDN 1689 cloud whose Gaia astrometry is clearly consistent with
kinematic membership with the Ophiuchus star-forming region.
Description:
We report the results of a study of archival SuperWASP light curves
for stars in Scorpius-Centaurus (Sco-Cen), the nearest OB
association. We use SuperWASP time-series photometry to extract
rotation periods for candidate members of the Sco-Cen complex. Our
final sample contains 157 well-characterized pre-MS stars.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 101 162 Data for Sco-Cen main group members
table3.dat 82 28 Data for other stars
table4.dat 89 157 Adopted photometry for stellar parameters
table1.dat 58 567 Periodogram analysis results
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 18 A18 --- SWASPJ SWASP identifier (HHMMSS.ss+DDMMSS.s)
20- 35 A16 --- 2MASSJ 2MASS identifier (HHMMSSss+DDMMSSs)
37- 39 A3 --- Sub Sco-Cen Subgroup (LCC, UCL or US)
41- 45 F5.3 d Per Reported Period
47- 51 F5.3 d e_Per Error on Period
53- 54 A2 --- Flag [abcde ] Flags (1)
56- 64 A9 --- SpType Spectral Type
66- 67 I2 --- r_SpType ? Spectral Type Reference (2)
69- 73 F5.2 mag Vmag SuperWASP V magnitude
75- 79 F5.2 mag Kmag 2MASS K magnitude
81- 85 F5.3 mag Av Reddening coefficient
87- 91 F5.3 mag V-K0 Reddening corrected V-K
93- 96 I4 K Teff ? Effective temperature
98-101 F4.2 Msun Mass ? Mass
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Note (1): Flags as follows:
a = Stars that have statistically similar periods to the nearest spatial
entry in the Variable Star Index (Watson, 2006, Cat. B/vsx)
b = Stars that have statistically different periods to the nearest spatial
entry in the Variable Star Index (Watson, 2006, Cat. B/vsx)
c = Stars without spectral types use the Sco-Cen subgroup-averaged
reddening coefficients for color estimation only
d = The only star in our sample found in David et al. (2014JAD....20....5D 2014JAD....20....5D).
We find the same period.
e = Stars for which the APASS V band was unavailable; SPM4 photometry was
adopted in its place.
Note (2): References as follows:
1 = Riaz et al. (2006, Cat. J/AJ/132/866)
2 = Pecaut & Mamajek (2016, Cat. J/MNRAS/461/794)
3 = Houk (1978, Cat. III/51)
4 = Mamajek et al. (2002, Cat. J/AJ/124/1670)
5 = Spencer Jones & Jackson (1936, Cat. I/5)
6 = Torres et al. (2006, Cat. J/A+A/460/695)
7 = Houk (1982, Cat III/80)
8 = Wichmann et al. (1997, Cat. J/A+A/326/211)
9 = Krautter et al. (1997, Cat. J/A+AS/123/329)
10 = Kohler et al. (2000, Cat. J/A+A/356/541)
11 = Preibisch et al. (1998, Cat. J/A+A/333/619)
12 = Houk & Smith-Moore (1988, Cat. III/133)
13 = Rizzuto et al. (2015, Cat. J/MNRAS/448/2737)
14 = Luhman & Mamajek (2012, Cat. J/ApJ/758/31)
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 15 A15 --- Name Star name
16- 23 A8 --- Group Star's group
(CrA, Oph, TWA, Lup I, Lup II or Lup III)
25- 42 A18 --- SWASPJ SWASP identifier (HHMMSS.ss+DDMMSS.s)
44- 59 A16 --- 2MASSJ 2MASS identifier (HHMMSSss+DDMMSSs)
61- 66 F6.3 d Per Reported period
68- 72 F5.3 d e_Per Error on Per
74 A1 --- Flag [ab] Flag (1)
76- 80 A5 --- SpType Spectral type
82 I1 --- r_SpType Spectral type reference (2)
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Note (1): Flags as follows:
a = Stars that have statistically similar periods to the nearest spatial entry
in the Variable Star Index (Watson, 2006, Cat. B/vsx)
b = Stars that have statistically different periods to the nearest spatial
entry in the Variable Star Index (Watson, 2006, Cat. B/vsx)
Note (2): References as follows:
1 = Torres et al. (2006, Cat. J/A+A/460/695)
2 = Krautter et al. (1997, Cat. J/A+AS/123/329)
3 = Houk (1982, Cat III/80)
4 = Hughes et al. (1994AJ....108.1071H 1994AJ....108.1071H)
5 = Pecaut & Mamajek (2016, Cat. J/MNRAS/461/794)
6 = Antoniucci et al. (2014, estimates Teff=5000K, which would be roughly
consistent with a K0 pre-MS star on the spectral type versus Teff scale
of Pecaut & Mamajek, 2013, Cat. J/ApJS/208/9)
7 = Preibisch et al. (1998, Cat. J/A+A/333/619)
8 = Meyer & Wilking (2009PASP..121..350M 2009PASP..121..350M)
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- 2MASSJ The 2MASS identifier ((HHMMSSss+DDMMSSs) (1)
18- 23 F6.3 mag Bmag Apparent B band magnitude
25- 29 F5.3 mag e_Bmag Uncertainty in Bmag
31- 33 A3 --- r_Bmag Reference on Bmag (2)
35- 40 F6.3 mag Vmag Apparent V band magnitude
42- 46 F5.3 mag e_Vmag Uncertainty in Vmag
48- 50 A3 --- r_Vmag Reference on Vmag (2)
52- 57 F6.3 mag Jmag 2MASS J band magnitude
59- 63 F5.3 mag e_Jmag Uncertainty in Jmag
65- 70 F6.3 mag Hmag 2MASS H band magnitude
72- 76 F5.3 mag e_Hmag Uncertainty in Hmag
78- 83 F6.3 mag KSmag 2MASS KS band magnitude
85- 89 F5.3 mag e_KSmag Uncertainty in KSmag
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Note (1): Where the identifier is the J2000 coordinates.
Note (2): Reference as follows:
DR6 = APASS DR6
DR7 = APASS DR7
DR9 = APASS DR9
P97 = Hipparcos, Perryman et al. (1997A&A...323L..49P 1997A&A...323L..49P, Cat. I/239)
H00 = Converted from Tycho-2 BT, VT,
Hog et al. (2000A&A...355L..27H 2000A&A...355L..27H, Cat I/259)
T06 = Torres et al. (2006A&A...460..695T 2006A&A...460..695T, Cat. J/A+A/460/695)
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 18 A18 --- SWASPJ The SWASP identifier (HHMMSS.ss+DDMMSS.s) (1)
20- 31 F12.4 d Start Heliocentric Julian Date of season start
33- 44 F12.4 d End Heliocentric Julian Date of season end
46- 51 F6.3 d Period Period
53- 58 F6.4 mag Amp Amplitude
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Note (1): Where the identifier is the J2000 coordinates.
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Acknowledgements:
Samuel Mellon, smellon(at)ur.rochester.edu
(End) Patricia Vannier [CDS] 19-Sep-2017