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Peremennye Zvezdy (Variable Stars) 34, No. 1, 2014 Received 7 March; accepted 13 March.
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Article in PDF |
USNO-B1.0 1329-0132547, a New Double-Mode
High-Amplitude 
Scuti Variable
A. V. Khruslov1, A.V. Kusakin2
- Institute of Astronomy, Russian Academy of Sciences,
Moscow, Russia; e-mail: khruslov@bk.ru
- Fesenkov Astrophysical Institute, Almaty, Kazakhstan; e-mail: un7gbd@gmail.com
We present our discovery of a new double-mode
high-amplitude Scuti variable, HADS(B) type, USNO-B1.0
1329-0132547. We found the frequencies  and  . The period
ratio
 is typical of radially pulsating HADS(B)
stars.
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1. Introduction
In this paper, we present our discovery of the new variable star USNO-B1.0 1329-0132547. Its coordinates in the 2MASS catalog (Skrutskie et al. 2006) are 04
44
37
78, +42
54
34
4 (J2000.0). According to our CCD observations, this star
is a double-mode high-amplitude Scuti variable, HADS(B)
type. The variable was discovered in the region of the double-mode
variable GSC 2901-00089; our study of the latter star will be
submitted to "Peremennye Zvezdy" later.
2. Observations
Our CCD observations in the Johnson
bands were performed at
the Tien Shan Astronomical Observatory of the V.G. Fesenkov
Astrophysical Institute, at the altitude of 2750 m above the sea
level, using a Zeiss 1000-mm reflector with an Apogee U9000 D9 CCD
photometer. Reductions were performed using the MaxIM DL aperture
photometry package. The finding chart (Fig. 1) identifies the
variable star, comparison star, and check star. The comparison
star was USNO-B1.0 1329-0132636, at the coordinates
04444488 +42 55 08
7 (J2000.0), and the
check star, USNO-B1.0 1329-0132524, at 04443582 +42
54 19
1 (J2000.0). The magnitudes of the comparison star
in the AAVSO Photometric All-Sky Survey (APASS,
http://www.aavso.org/download-apass-data) catalog are
and
(Johnson's system) . We express our
-band measurements as magnitude differences with respect to the
comparison star.
Our observations are available online in the html version of this paper.
3. Results
We analyzed the time series using Deeming's method implemented in the WinEfk code written by V.P. Goranskij. Using our observations of USNO-B1.0 1329-0132547, we found the frequencies
and
(see the power spectrum in Fig. 2). The results are
presented in the Table.
Table. Detected frequencies
| Mode | Frequency, c/d | Semi-amplitude | Period, d | Epoch, HJD | ||
 , mag |
 , mag |
, mag |
||||
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6.1770 | 0.051 | 0.046 | 0.034 | 0.16189 | 2456585.582 |
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8.0561 | 0.053 | 0.049 | 0.040 | 0.12413 | 2456585.598 |
The light curves of USNO-B1.0 1329-0132547 in the , and
bands are displayed in Figs. 3, 4, 5. The power spectra of
USNO-B1.0 1329-0132547 (Fig. 2) are plotted both for the raw data
and with the fundamental-mode oscillations subtracted.
The -band range of USNO-B1.0 1329-0132547 is from 17
28 to
1758; the -band range is 183-187. The delta
magnitude -band range is 2.18-2.40. The period ratio
is typical of high-amplitude double-mode Scuti
stars radially pulsating in the fundamental and first overtone
modes (Petersen & Christensen-Dalsgaard 1996). The infrared color
index 
(2MASS) does not contradict the suggested type
if we take into account possible reddening for the galactic
latitude
.
Acknowledgments: The authors are grateful to Dr. V.P.
Goranskij for providing software for the light-curve analysis. We
wish to thank M.A. Krugov for technical assistance during the
observations. This study was supported by the Russian Foundation
for Basic Research (grant 13-02-00664), the Programme
"Non-stationary Phenomena of Objects in the Universe" of the
Presidium of Russian Academy of Sciences, and the program
"Studies of Physical Phenomena in Star-forming Regions and
Nuclear Zones of Active Galaxies" of the Ministry of Education of
Science (Republic of Kazakhstan).
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Fig. 3.
The light curves of USNO-B1.0 1329-0132547,
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References:
Skrutskie, M.F., Cutri, R.M., Stiening, R., et al., 2006, Astron. J., 131, 1163
Petersen, J.O., Christensen-Dalsgaard, J., 1996, Astron. and Astrophys., 312, 463