J/MNRAS/429/1102    UBV(RI)c photometry of 6 open clusters   (Glushkova+, 2013)

Photometric study of open clusters Berkeley 96, Berkeley 97, King 12, NGC 7261, NGC 7296 and NGC 7788. Glushkova E.V., Zabolotskikh M.V., Koposov S.E., Spiridonova O.I., Leonova S.I., Vlasyuk V.V., Rastorguev A.S. <Mon. Not. R. Astron. Soc., 429, 1102-1112 (2013)> =2013MNRAS.429.1102G 2013MNRAS.429.1102G
ADC_Keywords: Clusters, open ; Photometry, UBVRI Keywords: open clusters and associations: individual: Berkeley 96 - open clusters and associations: individual: Berkeley 97 - open clusters and associations: individual: King 12 - open clusters and associations: individual: NGC 7261 - open clusters and associations: individual: NGC 7296 - open clusters and associations: individual: NGC 7788 Abstract: We present BVRcIc CCD photometry in the fields of six Galactic open clusters toward the Perseus spiral arm. These data, complemented with J, H and Ks magnitudes from 2MASS, have been used to determine the following ages, distances and colour excesses E(B-V) for these clusters: 40Myr, 3180-380+440pc, 0.54±0.03mag (Berkeley 96); 250Myr, 2410-200+220pc, 0.77±0.06mag (Berkeley 97); 70Myr, 2490-170+180pc, 0.51±0.05mag (King 12); 160Myr, 2830-150+160pc, 0.88±0.09mag (NGC 7261); 280Myr, 2450-170+190pc, 0.24±0.03mag (NGC 7296); 160Myr, 2750-210+220pc, 0.49±0.02mag (NGC 7788). We found gaps in the mass function of clusters Be 97, King 12 and NGC 7788 in the mass intervals [1.3-1.5], [1.4-1.6] and [1.5-1.7] solar masses, respectively. Description: We observed six open clusters in the Johnson/Kron-Cousins broad band BVRcIc using the Zeiss-1000 telescope at the Special Astrophysical Observatory of the Russian Academy of Sciences equipped with a photometer based on an EEV 42-40 2Kx2K CCD. Objects: --------------------------------------------------------------------- RA (ICRS) DE Designation(s) (file) --------------------------------------------------------------------- 22 29 49.0 +55 23 47 Berkeley 96 = C 2227+551 (table4.dat) 22 39 28.0 +58 59 51 Berkeley 97 = C 2237+587 (table5.dat) 23 53 01.0 +61 56 45 King 12 = C 2350+616 (table6.dat) 22 20 07.0 +58 07 41 NGC 7261 = C 2218+578 (table7.dat) 22 28 01.0 +52 19 22 NGC 7296 = C 2226+520 (table8.dat) 23 56 38.0 +61 24 02 NGC 7788 = C 2354+611 (table9.dat) --------------------------------------------------------------------- File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file table4.dat 76 1235 Photometric data for Berkeley 96 table5.dat 76 888 Photometric data for Berkeley 97 table6.dat 76 706 Photometric data for King 12 table7.dat 76 782 Photometric data for NGC 7261 table8.dat 76 808 Photometric data for NGC 7296 table9.dat 76 777 Photometric data for NGC 7788 -------------------------------------------------------------------------------- Byte-by-byte Description of file: table[456789].dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 10 F10.6 deg RAdeg Right ascension (J2000) 12- 20 F9.6 deg DEdeg Declination (J2000) 22- 27 F6.3 mag Vmag Johnson V magnitude 30- 34 F5.3 mag e_Vmag rms uncertainty on Vmag 36- 41 F6.3 mag B-V ?=99.999 Johnson B-V colour index 43- 48 F6.3 mag e_B-V ?=99.999 rms uncertainty on B-V 50- 55 F6.3 mag V-Rc ?=99.999 Johnson-Cousins V-Rc colour index 57- 62 F6.3 mag e_V-Rc ?=99.999 rms uncertainty on V-Rc 64- 69 F6.3 mag V-Ic ?=99.999 Johnson-Cousins V-Ic colour index 71- 76 F6.3 mag e_V-Ic ?=99.999 rms uncertainty on V-Ic -------------------------------------------------------------------------------- History: From electronic version of the journal
(End) Patricia Vannier [CDS] 14-Mar-2014
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