J/AZh/91/382 New variable stars in field SA9 (Sokolovsky+, 2014)
New variable stars on digitized plates of the Moscow collection. Field SA9.
Sokolovsky K.V., Antipin S.V., Zubareva A.M., Kolesnikova D.M.,
Lebedev A.A., Samus N.N., Sat L.A.
<Astron. Zh. 91, 382 (2014)>
=2014AZh....91..382S 2014AZh....91..382S
=2014ARep...58..319S 2014ARep...58..319S
ADC_Keywords: Stars, variable ; Photometry
Abstract:
The new stage of work on digitizing the astronomical plates of the
Sternberg Astronomical Institute's collection and searching for new
variable stars using the digitized photographic plates includes a
considerable improvement of the automated search techniques for
objects with variable brightnesses. In particular, the technique for
taking into account the non-linear response of the photographic light
detector has been improved. Applying the improved techniques to 182
digitized images of a 10°x10° field centered at SA9, obtained
from scanning photographic plates taken with the Sternberg
Astronomical Institute 40-cm astrograph, has enabled the discover and
study of 77 new variable stars (MDV 519-595). These include 3
Cepheids, 2 probableBY Draconis stars, 65 eclipsing binaries, 3RR
Lyrae stars, 1 high-amplitude δ Scuti star (HADS), and 3
irregular variables. Special CCD observations have confirmed the
presence of brightness variations in 7 of the 77 variables that were
initially considered uncertain.
Description:
This new paper presents the results of a search for and study of new
variables using scans of plates from the 40-cm astrograph in a field
centred on Kapteyn's area SA9. According to Kapteyn's scheme, this
area is located around the star BD +60 636 = HIP 14833 (03:11:31.7,
+60 38 06, J2000.0). This star is close to, but not always coincident
with, the centers of the studied plates. The exposure time of this
area was most often 45-min, so that the limiting magnitude of
good-quality plates is about 17.5mB.
Individual light curves are available at
http://www.sai.msu.su/groups/cluster/gcvs/digit/mdv/data/mdvNNN.dat
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 82 77 New variable stars
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See also:
J/AZh/87/1087 : New variable stars in 66 Oph field (Kolesnikova+, 2010)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- --- [MDV]
5- 7 I3 --- MDV [519/595] MDV number
9- 10 I2 h RAh Right ascension (J2000)
12- 13 I2 min RAm Right ascension (J2000)
15- 19 F5.2 s RAs Right ascension (J2000)
21 A1 --- DE- Declination sign (J2000)
22- 23 I2 deg DEd Declination (J2000)
25- 26 I2 arcmin DEm Declination (J2000)
28- 31 F4.1 arcsec DEs Declination (J2000)
33- 36 A4 --- Type Variable type
38- 42 F5.2 mag mMax Magnitude at maximum brightness
44- 48 F5.2 mag mMin Magnitude at minimum brightness
49 A1 --- u_mMin Uncertainty flag on mMin
51- 55 F5.2 mag mMin2 ? Magnitude at second minimum brightness
56 A1 --- u_mMin2 Uncertainty flag on mMin2
58- 67 F10.4 d Epoch ? Epoch of extremum brightness (JD-2400000)
69- 76 F8.6 d Per ? Period
79- 82 A4 --- Notes ? Notes (1)
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Note (1): Notes as follows:
1 = Type EW with double the period is possible
2 = A double star. The eastern star of the pair varies, as confirmed with
CCD observations. The tabulated coordinates are from the 2MASS catalog
3 = Brightness variability and type were confirmed with CCD observations
4 = Varies in the NSVS data, which indicate P=9.23d
5 = Type RRC with half the period is possible
6 = Eccentric orbit; the secondary minimum is at phase 0.465
7 = A period of about 8000 days is possible; J-K=0.635 (from 2MASS)
8 = Double the period is possible
9 = The periods 0.337844d or 0.252442d are possible (type EW in both cases)
10 = The period varies. Variable in the NSVS data, which indicate P=1.07213d
11 = Probably can be identified with the X-ray source 1RXS J033501.6+623655
12 = IRAS 03417+6002. Varies in the NSVS data, which indicate that it may be
a semi-regular variable (type SR:) with P∼92d
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 22-Jul-2014