J/ApJ/691/342 griBVI photometry in M37 (Hartman+, 2009)
Deep MMT transit survey of the open cluster M37. III. Stellar rotation at 550 Myr. Hartman J.D., Gaudi B.S., Pinsonneault M.H., Stanek K.Z., Holman M.J., McLeod B.A., Meibom S., Barranco J.A., Kalirai J.S. <Astrophys. J., 691, 342-364 (2009)> =2009ApJ...691..342H
ADC_Keywords: Clusters, open ; Stars, dwarfs ; Photometry Keywords: open clusters and associations: individual (M37) - stars: low-mass, brown dwarfs - stars: rotation - stars: spots - stars: variables: other Abstract: In the course of conducting a deep (14.5≲r≲23), 20 night survey for transiting planets in the rich ∼550Myr old open cluster M37, we have measured the rotation periods of 575 stars, which lie near the cluster main sequence, with masses 0.2M☉≲M≲1.3M☉. This is the largest sample of rotation periods for a cluster older than 500Myr. Using this rich sample we investigate a number of relations between rotation period, color, and the amplitude of photometric variability. Description: The observations and data reduction procedure were described in detail in Papers I (J/ApJ/675/1233) and II (J/ApJ/675/1254). The primary time-series photometric observations were done using the r filter and consist of ∼4000 high-quality images obtained over 24 nights (including eight half-nights) between 2005 December 21 and 2006 January 21. The spectra were obtained on four separate nights between 2007 February 23 and 2007 March 12. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 126 575 Candidate cluster members with measured rotation periods: coordinates and periods table2.dat 98 575 Candidate cluster members with measured rotation periods: magnitudes
See also: J/ApJ/675/1233 : gri photometry in M37 (NGC 2099) (Hartman+, 2008) J/ApJ/675/1254 : M37 variable stars (Hartman+, 2008) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 4 I4 --- ID Member identification number, <Cl* NGC 2099 HGH VNNNN> in Simbad 6- 7 I2 h RAh Hour of Right Ascension (J2000) 9- 10 I2 min RAm Minute of Right Ascension (J2000) 12- 16 F5.2 s RAs Second of Right Ascension (J2000) 18 A1 --- DE- Sign of the Declination (J2000) 19- 20 I2 deg DEd Degree of Declination (J2000) 22- 23 I2 arcmin DEm Arcminute of Declination (J2000) 25- 28 F4.1 arcsec DEs Arcsecond of Declination (J2000) 30- 31 I2 --- Chip Chip identification 33- 43 F11.8 d Per Period from Paper II (J/ApJ/675/1254) 45- 54 F10.8 d e_Per The 1σ error in Per 56- 66 F11.8 d Per1 Multi-harmonic AoV algorithm N=1 period 68- 77 F10.8 d e_Per1 The 1σ error in Per1 79- 89 F11.8 d Per2 Multi-harmonic AoV algorithm N=2 period 91-100 F10.8 d e_Per2 The 1σ error in Per2 102-112 F11.8 d Per3 Multi-harmonic AoV algorithm N=3 period 114-124 F11.8 d e_Per3 The 1σ error in Per3 126 I1 --- C [0/1] Clean flag (1)
Note (1): Set to either 1 or 0. Stars with a value of 1 were included in the clean sample of stars in Section 5.
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 4 I4 --- ID Member identification number, Cl* NGC 2099 HGH VNNNN in Simbad 6- 11 F6.3 mag <rmag> Flux averaged r band magnitude 13- 17 F5.3 mag e_<rmag> Root-mean-square of rmag 19- 24 F6.3 mag gmag Paper I (J/ApJ/675/1233) catalog g band magnitude 26- 31 F6.3 mag rmag Paper I (J/ApJ/675/1233) catalog r band magnitude 33- 38 F6.3 mag imag Paper I (J/ApJ/675/1233) catalog i band magnitude 40- 45 F6.3 mag Bmag Kalirai et al. (2001AJ....122.3239K) B band magnitude 47- 52 F6.3 mag Vmag Kalirai et al. (2001AJ....122.3239K) V band magnitude 54- 59 F6.3 mag Imag I band magnitude transformed from r and i bands 61- 65 F5.3 mag rAmp1 Multi-harmonic AoV N=1, peak-to-peak, r band amplitude 67- 72 F6.3 mag rAmp1m Minimum multi-harmonic AoV N=1, peak-to-peak, r band amplitude (1) 74- 78 F5.3 mag rAmp2 Multi-harmonic AoV N=2, peak-to-peak, r band amplitude 80- 85 F6.3 mag rAmp2m Minimum multi-harmonic AoV N=2, peak-to-peak, r band amplitude (1) 87- 91 F5.3 mag rAmp3 Multi-harmonic AoV N=3, peak-to-peak, r band amplitude 93- 98 F6.3 mag rAmp3m Minimum multi-harmonic AoV N=3, peak-to-peak, r band amplitude (1)
Note (1): That the light curve could have had and still have been detected as a variable. Entries with no value correspond to light curves that would be selected as variable even when Ar,N=0.0. The model does not adequately describe the light curve in these cases.
History: From electronic version of the journal References: Hartman et al., Paper I 2008ApJ...675.1233H, Cat. J/ApJ/675/1233 Hartman et al., Paper II 2008ApJ...675.1254H, Cat. J/ApJ/675/1254 Hartman et al., Paper IV 2009ApJ...695..336H
(End) Greg Schwarz [AAS], Patricia Vannier [CDS] 21-Jul-2010
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