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 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:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
sources.dat 111 184 Overview of the variable stars
phot/* . 684 Individual UBVI light curves
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Byte-by-byte Description of file: sources.dat
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Bytes Format Units Label Explanations
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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
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Byte-by-byte Description of file: phot/*
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Bytes Format Units Label Explanations
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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)
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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)
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Acknowledgements:
Sophie Saesen, sophie(at)ster.kuleuven.be,
Instituut voor Sterrenkunde, Leuven, Belgium
(End) Sophie Saesen [Leuven, Belgium], Patricia Vannier [CDS] 03-Jun-2010