J/other/JAD/17.1 1961-1999 UBV photometry of 14 variables (Oja, 2011) ================================================================================ Photoelectric UBV photometry of variable stars observed during the years 1961-1999. Oja T. =2011JAD....17....1O ================================================================================ ADC_Keywords: Stars, variable ; Photometry, UBV Keywords: technique: photometric - stars: variable Abstract: Photoelectric UBV photometry of the variable stars V636 Cas, alpha UMi, V440 Per, zeta Gem, UU Cnc, TYC2-880-515-1, V473 Lyr, chi Cyg, V1794 Cyg, DT Cyg, V1334 Cyg, V532 Cyg, pi Aqr, and DY Peg is reported. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file table1.dat 61 14 The variable stars table3.dat 61 448 UBV measurements of V636 Cas = HD 620274 table4.dat 61 233 UBV measurements of alpha UMi = HR 424 table5.dat 61 719 UBV measurements of V440 Per = HR 690 table6.dat 61 955 UBV measurements of zeta Gem = HR 2650 table7.dat 61 214 UBV measurements of UU Cnc = BD+15 1733 table8.dat 61 28 UBV measurements of TYC2-880-515-1 = Anon table9.dat 61 1141 UBV measurements of V473 Lyr = HR 7308 table10.dat 61 71 UBV measurements of chi Cyg = HR 7564 table11.dat 61 457 UBV measurements of V1794 Cyg = BD+43 3759 table12.dat 61 44 UBV measurements of DT Cyg = BD+30 4318 table13.dat 61 716 UBV measurements of V1334 Cyg = HR 8157 table14.dat 61 31 UBV measurements of V532 Cyg = BD 443779 table15.dat 61 60 UBV measurements of pi Aqr = HR 8539 table16.dat 61 93 UBV measurements of DY Peg = BD+16 3877 -------------------------------------------------------------------------------- Byte-by-byte Description of file: table1.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 14 A14 --- Name Star name 17- 21 A5 --- VType Variable type 23- 24 I2 h RAh Right ascension (J2000) 26- 29 F4.1 min RAm Right ascension (J2000) 31 A1 --- DE- Declination sign (J2000) 32- 33 I2 deg DEd Declination (J2000) 35- 36 I2 arcmin DEm Declination (J2000) 38- 43 A6 --- ID Identification number of the star 45- 55 A11 --- Tab Name of the table with UBV photometry 57- 61 I5 d DT ? Time interval between first and last observation -------------------------------------------------------------------------------- Byte-by-byte Description of file: table[3456789].dat table1?.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 6 A6 --- ID Identification number of the star (1) 8- 17 A10 "YYYY/MM/DD" Date Observation date 19- 23 F5.2 h theta ? Local sideral time in hours and decimals of hour of mid-observation 25- 30 F6.3 mag Vmag ? V magnitude 33- 37 F5.3 mag B-V B-V colour index 38- 43 F6.3 mag U-B ? U-B colour index 46- 55 F10.4 d JD HJD-2400000 at mid-observation 57 A1 --- Inst [EKLNSU] Instrument used (2) 59- 61 A3 --- R Remark (3) -------------------------------------------------------------------------------- Note (1): Some tables contains also photometry of comparison stars Note (2): Instruments code as follows: E = Observations made with single-channel UBV photometers at the 50-cm Danish Cassegrain telescope or the ESO 50-cm Cassegrain telescope at the European Southern Observatory. The magnitudes and colour indices were reduced to the UBV system by means of the best values of the southern E-region standard stars available at the time. One observation of z Gem with each instrument is included here. K = A single-channel UBV photometer attached to the 40-cm Cassegrain telescope at the Kvistaberg Observatory, the northern observing station of the Uppsala Observatory. The observations were reduced to the UBV system by means of the standard stars published by Oja (1996BaltA...5..103O). L = Measurementsmade with the Swedish Academy of Sciences 60-cm Cassegrain telescope located at El Observatorio del Roque de los Muchachos on La Palma, belonging to El Instituto de Astrofisica de Canarias. During the 1988 observations a UBV photometer, constructed at the Stockholm Observatory, using a rotating filter-wheel was utilized. The wheel stopped at every pre-selected filter position during an interval of time approximately inversely proportional to the count rate in that position. In 1991-1995 the telescope was equipped with another single-channel UBV photometer, also built at the Stockholm Observatory. All measurements have been reduced to the UBV system by means of the standard stars published by Oja (1996BaltA...5..103O). N = Measurements made with the Turku Observatory simultaneous five-colour photo-polarimeter at the 2.5-m Nordic Optical telescope located at El Observatorio del Roque de los Muchachos on La Palma. Only one measurement of UU Cnc (together with its standards) is included here. S = A simultaneous UBV three-colour photometer used with the 1-m Schmidt-Cassegrain telescope at the Kvistaberg Observatory. All observations were reduced to the UBV system by means of the standard stars listed by Oja (1996BaltA...5..103O). U = A single-channel BV photometer attached to the 33-cm photographic tube of the Uppsala double refractor. The observations, originally reduced by the standard values given by Haggkvist and Oja (1969ArA.....5..303H), were reduced to the BV system by correcting the original results by DV=-0.003, D(B-V)=+0.005, the corrections having been derived from a comparison of the list mentioned above and that published by Oja (1996BaltA...5..103O). Only a UMi and z Gem were measured with the Uppsala refractor. Note (3): Remarks as follows: R = differential measurement, referred to the local standard(s) only RV = the magnitude V has been referred to the local standard(s) only U = the whole measurement is more uncertain than normal measurements, generally due to weather problems, sometimes aurora borealis UV = the magnitude V is more uncertain than usual (weather problems) UU = the U-B colour index is more uncertain than usual, generally because of faint U and/or bright sky -------------------------------------------------------------------------------- History: From electronic version of the journal ================================================================================ (End) Patricia Vannier [CDS] 13-Dec-2011