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J/A+A/515/A16       UBVI light curves of NGC 884 variables       (Saesen+, 2010)

Photometric multi-site campaign on the open cluster NGC 884. I. Detection of the variable stars. Saesen S., Carrier F., Pigulski A., Aerts C., Handler G., Narwid A., Fu J.N., Zhang C., Jiang X.J., Vanautgaerden J., Kopacki G., Steslicki M., Acke B., Poretti E., Uytterhoeven K., Gielen C., Ostensen R., De Meester W., Reed M.D., Kolaczkowski Z., Michalska G., Schmidt E., Yakut K., Leitner A., Kalomeni B., Cherix M., Spano M., Prins S., Van Helshoecht V., Zima W., Huygen R., Vandenbussche B., Lenz P., Ladjal D., Puga Antolin E., Verhoelst T., De Ridder J., Niarchos P., Liakos A., Lorenz D., Dehaes S., Reyniers M., Davignon G., Kim S.-L., Kim D.H., Lee Y.-J., Lee C.-U., Kwon J.-H., Broeders E., Van Winckel H., Vanhollebeke E., Waelkens C., Raskin G., Blom Y., Eggen J.R., Degroote P., Beck P., Puschnig J., Schmitzberger L., Gelven G.A., Steininger B., Blommaert J., Drummond R., Briquet M., Debosscher J. <Astron. Astrophys. 515, A16 (2010)> =2010A&A...515A..16S
ADC_Keywords: Clusters, open ; Stars, variable ; Photometry, CCD ; Photometry, Geneva Keywords: Galaxy: open cluster and associations: individual: NGC 884 - techniques: photometric - stars: variables: general - stars: oscillations - binaries: eclipsing Abstract: Recent progress in the seismic interpretation of field beta Cep stars has resulted in improvements of the physics in the stellar structure and evolution models of massive stars. Further asteroseismic constraints can be obtained from studying ensembles of stars in a young open cluster, which all have similar age, distance and chemical composition. To improve our comprehension of the beta Cep stars, we studied the young open cluster NGC 884 to discover new B-type pulsators, besides the two known beta Cep stars, and other variable stars. An extensive multi-site campaign was set up to gather accurate CCD photometry time series in four filters (U, B, V, I) of a field of NGC 884. The images were calibrated and reduced to transform the CCD frames into interpretable light curves. Various variability indicators and frequency analyses were applied to detect variable stars in the field. Description: We present here the light curves in the four filters of the 184 detected variable stars in NGC 884. These variable stars are listed in tables 3 and A.1 of the paper. The CCD images were calibrated and reduced as described in sections 4 and 5 of the paper. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file sources.dat 111 184 Overview of the variable stars phot/* 31 684 Individual UBVI light curves
Byte-by-byte Description of file: sources.dat
Bytes Format Units Label Explanations
1- 5 I05 --- Seq Star sequential number 7- 10 I4 --- WEBDA ? WEBDA number 11 A1 --- --- [/] 12- 15 I4 --- WEBDA2 ? Second WEBDA number 17- 18 I2 h RAh Right ascension (J2000) 20- 21 I2 min RAm Right ascension (J2000) 23- 27 F5.2 s RAs Right ascension (J2000) 29 A1 --- DE- Declination sign (J2000) 30- 31 I2 deg DEd Declination (J2000) 33- 34 I2 arcmin DEm Declination (J2000) 36- 37 I2 arcsec DEs Declination (J2000) 39- 47 A9 --- SpType MK spectral type 49- 53 F5.2 mag Vmag ? Geneva V magnitude 55- 59 F5.2 mag B2-V1 ? Geneva B2-V1 colour index 61- 65 F5.2 mag B2-U ? Geneva B2-U colour index 67- 72 F6.3 d-1 Freq ? Main frequency in day-1 74- 79 F6.2 uHz Freq2 ? Main frequency in µHz 81- 85 F5.1 mmag Amp ? Amplitude 87 A1 --- n_Seq [kn] known or new for eclipsing binary 89- 93 F5.2 d Per1 ? Period for eclipsing binary, if exist 95-111 A17 --- Per2 Other possible periods for Seq 02217
Byte-by-byte Description of file: phot/*
Bytes Format Units Label Explanations
1- 13 F13.5 d HJD Heliocentric Julian Date 15- 21 F7.4 mag mag Differential magnitude 23- 28 F6.4 mag e_mag Error on magnitude 30- 31 I2 --- Site [1,16] Observing site (1)
Note (1): For more information on the observing sites and their equipment, we refer to table 1 of the paper. Sites numbered as follows: 1 = Bialkow, Poland 2 = ORM, La Palma, Spain (season 1) 3 = ORM, La Palma, Spain (season 2+3, field a) 4 = ORM, La Palma, Spain (season 2+3, field b) 5 = Michelbach, Austria 6 = Vienna, Austria (season 1) 7 = Vienna, Austria (season 2) 8 = Baker, Missouri, USA (CCD Roper Sci. 1340 B) 9 = Xinglong, China 10 = SOAO, South Korea 11 = EUO, Turkey 12 = TUG, Turkey (40-cm telescope) 13 = OFXB, Switzerland 14 = Athens, Greece (binned images) 15 = Athens, Greece (non-binned images) 16 = TUG, Turkey (150-cm telescope)
Acknowledgements: Sophie Saesen, sophie(at), Instituut voor Sterrenkunde, Leuven, Belgium
(End) Sophie Saesen [Leuven, Belgium], Patricia Vannier [CDS] 03-Jun-2010
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