CDROM/AJ/V112/P2408 Light Curves of 29 SNe (Hamuy+ 1996) ================================================================================ BVRI Light Curves for 29 Type Ia Supernovae Mario Hamuy et al. <1996, AJ, 112, 2408> =1996AJ....112.2408H ================================================================================ Abstract: BV(RI)_(KC) light curves are presented for 27 type Ia supernovae discovered during the course of the Calan/Tololo Survey and for two other SNe Ia observed during the same period. Estimates of the maximum light magnitudes in the B, V, and I bands and the initial decline rate parameter Delta m_(15)(B) are also given. (Copyright) 1996 American Astronomical Society. File Summary: -------------------------------------------------------------------------------- File Name Lrecl Records Explanations -------------------------------------------------------------------------------- table4.dat 66 568 BV(RI)_KC photometry for the 29 SNe Ia -------------------------------------------------------------------------------- Byte-by-byte Description of file: table4.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 6 A6 --- SN Supernova designation 7-14 F8.2 JD JD Julian Date of Observation (-2440000) 15-21 F7.3 mag B []? B magnitude 22-27 F6.3 mag e_B *[]? Error in B 28-34 F7.3 mag V []? V magnitude 35-40 F6.3 mag e_V *[]? Error in V 41-47 F7.3 mag R []? R magnitude 48-53 F6.3 mag e_R *[]? Error in R 54-60 F7.3 mag I []? I magnitude 61-66 F6.3 mag e_I *[]? Error in I -------------------------------------------------------------------------------- Notes for file: table4.dat -------------------------------------------------------------------------------- e_B, e_V, e_R, e_I: The uncertainties quoted for each magnitude correspond to the sum in quadrature of the errors due to photon Poisson statistics and an _assumed_ additional error of 0.03 mag in each individual observation. The latter uncertainty was included in order to account for errors involved in the transformation from the authors' instrumental system to the standard system, and also due to the subtraction of the underlying host galaxy. -------------------------------------------------------------------------------- ================================================================================ (End) Lee Brotzman [ADS] 30-Mar-1997