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J/AJ/134/1890       Secondary standard stars in u'g'r'i'z'    (Clem+, 2007)

Secondary standard stars for the u'g'r'i'z' photometric system. Clem J.L., Vandenberg D.A., Stetson P.B. <Astron. J., 134, 1890-1900 (2007)> =2007AJ....134.1890C
ADC_Keywords: Clusters, globular ; Photometry, SDSS ; Photometry, standards Keywords: globular clusters: individual (M92, M13, M3, M71) - Hertzsprung-Russell diagram - open clusters and associations: individual (M67, NGC 6791) - standards - stars: fundamental parameters Abstract: We present a new set of secondary standard stars for the u'g'r'i'z' photometric system that has been established in selected open and globular star clusters. These standards are calibrated to the original standard system defined by Smith et al. with an accuracy of 1% or better, extend as faint as r'∼20, and are concentrated in small regions of the sky. As a result, they can serve as viable calibrators of photometry obtained on some of the large-aperture, high-demand telescopes that employ the u'g'r'i'z' filter set. Description: This project was allocated a total of 135 nights spanning a 15 month period beginning in 2003 July and ending in 2004 September on the 1.8m Plaskett Telescope at the Dominion Astrophysical Observatory (DAO). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table5.dat 150 12225 Secondary standards in star clusters NGC 2682, NGC 5272, NGC 6205, NGC 6341, NGC 6791, NGC 6838
Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
1- 8 A8 --- Cluster Globular cluster name (1) 10- 14 I5 --- Star Sequential identification number, Cl* NGC NNNN CVS NNNNN in Simbad 16- 22 F7.1 pix Xpos X pixel coordinate (2) 24- 30 F7.1 pix Ypos Y pixel coordinate (3) 32- 37 F6.3 mag u'mag ?=99.999 The u' band magnitude (4) 39- 44 F6.4 mag e_u'mag ?=9.9999 Uncertainty in u'mag (4) 46 I1 --- o_u'mag Number of measurements in u'mag 48- 53 F6.3 mag g'mag ?=99.999 The g' band magnitude (4) 55- 60 F6.4 mag e_g'mag ?=9.9999 Uncertainty in g'mag (4) 62- 63 I2 --- o_g'mag Number of measurements in g'mag 65- 70 F6.3 mag r'mag ?=99.999 The r' band magnitude (4) 72- 77 F6.4 mag e_r'mag ?=9.9999 Uncertainty in r'mag (4) 79- 80 I2 --- o_r'mag Number of measurements in r'mag 82- 87 F6.3 mag i'mag ?=99.999 The i' band magnitude (4) 89- 94 F6.4 mag e_i'mag ?=9.9999 Uncertainty in i'mag (4) 96- 97 I2 --- o_i'mag Number of measurements in i'mag 99-104 F6.3 mag z'mag ?=99.999 The z' band magnitude (4) 106-111 F6.4 mag e_z'mag ?=9.9999 Uncertainty in z'mag (4) 113 I1 --- o_z'mag Number of measurements in z'mag 115-119 F5.3 --- chi Mean value of chi image-quality index (5) 121-126 F6.3 --- sharp Mean value of sharp image-quality index (5) 128-129 I2 h RAh Hour of Right Ascension (J2000) 131-132 I2 min RAm Minute of Right Ascension (J2000) 134-138 F5.2 s RAs Second of Right Ascension (J2000) 140 A1 --- DE- Sign of the Declination (J2000) 141-142 I2 deg DEd Degree of Declination (J2000) 144-145 I2 arcmin DEm Arcminute of Declination (J2000) 147-150 F4.1 arcsec DEs Arcsecond of Declination (J2000)
Note (1): Where the cluster centers are: NGC 2682 = 08:51:18.00 +11:48:00.0 (J2000) NGC 5272 = 13:42:11.23 +28:22:31.6 (J2000) NGC 6205 = 16:41:41.44 +36:27:36.9 (J2000) NGC 6341 = 17:17:07.27 +43:08:11.5 (J2000) NGC 6791 = 19:20:53.00 +37:46:18.0 (J2000) NGC 6838 = 19:53:46.11 +18:46:42.3 (J2000) Note (2): Increases West at 0.25arcsec/pixel. Note (3): Increases North at 0.25arcsec/pixel. Note (4): Values of 99.999 and 9.9999 indicate unknown magnitudes and uncertainties, respectively. Note (5): DAOPHOT parameters: * "chi" measures the PSF match; large values should be disregarded. * "sharp" is close to zero for isolated stars; significantly negative for bad pixels and cosmic rays; significantly positive for blended or non-stellar objects.
History: Prepared via OCR at CDS.
(End) Greg Schwarz [AAS], Patricia Vannier [CDS] 08-Jan-2010
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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