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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 (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 MN. 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:
FileName Lrecl Records Explanations
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
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
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
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). 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)
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
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)
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) 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)
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
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
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, Cat. I/239) H00 = Converted from Tycho-2 BT, VT, Hog et al. (2000A&A...355L..27H, Cat I/259) T06 = Torres et al. (2006A&A...460..695T, Cat. J/A+A/460/695)
Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
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
Note (1): Where the identifier is the J2000 coordinates.
Acknowledgements: Samuel Mellon, smellon(at)ur.rochester.edu
(End) Patricia Vannier [CDS] 19-Sep-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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