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J/other/RAA/17.20   V977 Cep and V982 Cep long-term photometry (Ibryamov+, 2017)

Long-term photometric behavior of the PMS stars V977 Cep and V982 Cep in the vicinity of NGC 7129. Ibryamov S.I., Semkov E.H., Milanov T.R., Peneva S.P. <Res. Astron. Astrophys., 17, 20 (2017)> =2017RAA....17...20I (SIMBAD/NED BibCode)
ADC_Keywords: Stars, variable ; Stars, pre-main sequence ; Photometry, UBVRI Keywords: stars: pre-main sequence - star: variable: T Tauri - stars: individual (V977 Cep, V982 Cep) Abstract: Long-term BVRI photometric light curves of the pre-main sequence stars V977 Cep and V982 Cep during the period from 2000 October to 2016 August are presented. The stars are located in the vicinity of the reflection nebula NGC 7129. Our photometric data show that both stars exhibit strong photometric variability in all optical passbands, which is typical for Classical T Tauri stars. Using our observational data we analyze the reasons for the observed brightness variations. In the case of V977 Cep we identify previously unknown periodicity in its light curve. Description: BVRI photometric data of V977 Cep and V982 Cep during the period from 2000 October to 2016 August are presented. The CCD observations were carried out with the 50/70-cm Schmidt and the 60-cm Cassegrain telescopes administered by Rozhen National Astronomical Observatory in Bulgaria. The observations were performed with four different types of CCD cameras: SBIG ST-8, SBIG STL-11000M and FLI PL16803 on the 50/70-cm Schmidt telescope, and FLI PL09000 on the 60-cm Cassegrain telescope. All frames were taken through a standard Johnson-Cousins set of filters. All obtained frames are dark frame subtracted and flat field corrected. The photometric data were reduced using subroutine DAOPHOT in the IDL software package. All data were analyzed using the same aperture, which was chosen to have a 6-arcsec radius and background annulus from 10-arcsec to 15-arcsec. As a reference sequence we used the BVRI comparisons reported in Semkov (2002IBVS.5214....1S; 2003IBVS.5373....1S). The average value of the errors in the reported magnitudes are 0.01-0.02mag for the I- and R-band data, and 0.02-0.03mag for the V- and B-band data. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file stars.dat 39 2 List of studied stars table1.dat 61 156 V977 Cep photometric CCD observations during the period 2000 Oct. - 2016 Aug. table2.dat 61 180 V982 Cep photometric CCD observations during the period 2002 Oct. - 2016 Aug.
See also: J/other/RAA/14.1264 : V350 Cep UBVRI long-term photometry (Ibryamov+, 2014) Byte-by-byte Description of file: stars.dat
Bytes Format Units Label Explanations
1- 9 A9 --- Star Star name 11- 12 I2 h RAh Righ ascension (J2000) 14- 15 I2 min RAm Righ ascension (J2000) 17- 20 F4.1 s RAs Righ ascension (J2000) 22 A1 --- DE- Declination sign (J2000) 23- 24 I2 deg DEd Declination (J2000) 26- 27 I2 arcmin DEm Declination (J2000) 29- 32 F4.1 arcsec DEs Declination (J2000) 34- 39 A6 --- FileName Name of the file with photometry
Byte-by-byte Description of file: table1.dat table2.dat
Bytes Format Units Label Explanations
1- 10 A10 "date" Date Date of observation ('YYYYMMDD' format) 12- 22 A11 d JD Julian Date 24- 28 F5.2 mag Imag ? Cousins I magnitude 30- 34 F5.2 mag Rmag ? Cousins R magnitude 36- 40 F5.2 mag Vmag ? Johnson V magnitude 42- 46 F5.2 mag Bmag ? Johnson B magnitude 48- 54 A7 --- Tel Telescope used (1) 56- 61 A6 --- CCD CCD used (2)
Note (1): Telescopes as follows: Schmidt = 50/70-cm Schmidt telescope of the Rozhen NAO 60-cm = 60-cm Cassegrain telescope of the Rozhen NAO Note (2): CCD cameras as follows: ST-8 = SBIG ST-8 STL-11 = SBIG STL-11000M FLI = FLI PL16803 (50/70-cm Shmidt telescope) FLI PL09000 (60-cm Cassegrain telescope)
Acknowledgements: Dr. Sunay I. Ibryamov, sibryamov(at)shu.bg, Department of Physics, University of Shumen, Bulgaria
(End) Patricia Vannier [CDS] 27-Feb-2017
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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