Peremennye Zvezdy (Variable Stars) 39, No. 4, 2019
Received 11 December; accepted 18 December.
|Article in PDF|
Sternberg Astronomical Institute, Moscow State University, Universitetsky pr. 13, 119992, Moscow, Russia; e-mail: email@example.com
Institute of Astronomy, Russian Academy of Sciences, Pyatnitskaya Str. 48, 119017, Moscow, Russia
Fesenkov Astrophysical Institute, Observatory 23, 050020, Almaty, Kazakhstan; e-mail: firstname.lastname@example.org
|ISSN 2221–0474||DOI: 10.24411/2221-0474-2019-10006|
|We present a photometric study of two new double-mode Cepheids, pulsating in the first and second overtones modes: V470 Cas and GSC 02901-00089. For the search for double-mode variability, we used all available observations from the ROTSE-I/NSVS and 1SWASP online public archives. Our multicolour CCD observations in the , and bands in Johnson's system and ASAS-SN data in the filter (that became available later) confirm the double-mode periodicity of these variables. We study period variations of the two stars; variations of the first-overtone periods were reliably detected.|
Classical Cepheid are radially pulsating periodic variable stars. Pulsations of single-period Cepheids occur in the fundamental mode (F) or in the first overtone mode (1O). In addition, several examples of possible second-overtone (2O) Cepheids are known. The double-mode Cepheids (or beat Cepheids) pulsate simultaneously in two radial pulsation modes: in the fundamental mode and in the first overtone mode (F/1O) or in the first and second overtone modes (1O/2O). There are known cases of triple-mode pulsations, F/1O/2O or 1O/2O/3O (3O being a possible third overtone mode).
The period ratio is a good indicator of the excited modes. Characteristic period ratios are and . The mass of the Cepheid can be derived using the two pulsation periods only. The first results based on the linear theory of stellar pulsations were obtained by Petersen (1973). For recent results of non-linear modelling of double-mode Cepheids, see Smolec & Moskalik (2010).
The group of the double-mode Cepheids is known for more than half a century. Florya (1937) discovered double periodicity of AC And (later proved to be a triple-mode star). Oosterhoff (1957) was the first to detect a group of Cephei variable stars with a large scatter in their photoelectric phased light curves, because of superposition of two oscillations. Later, double periodicity oscillations in the fundamental mode and first overtone were confirmed for most of these stars. The first Cepheid pulsating in the first and second overtones, CO Aur, was discovered by Mantegazza (1983). To date, according to AAVSO-VSX database1, there are 58 F/1O (type DCEP(B)) and 97 1O/2O (type DCEPS(B)) beat Cepheids known in the Galaxy. Also, several galactic triple-mode stars with periods in the Cepheid range have been detected.
Double-mode Cepheids are well represented in the Large (LMC) and Small (SMC) Magellanic Clouds. According to the OGLE-IV survey (Soszynski et al., 2015), in the LMC, there are 95 F/1O and 322 1O/2O Cepheids; in the SMC, there are 68 F/1O and 239 1O/2O Cepheids. Also, several triple-mode 1O/2O/3O stars are known (7 in LMC and one in SMC), and stars of F/1O/2O, 1O/3O and 2O/3O types in LMC (one case each).
In this paper, we present a photometric study of two new double-mode Cepheids, pulsating in the first and second overtone modes: V470 Cas and GSC 02901-00089. Our results were preliminarily announced by Khruslov & Kusakin (2016).
In this paper, we analyze the data of available photometric archives and our CCD observations. The light curves, power spectra, photometric data from the archives and from our CCD observations, light curves are available online in the html version of this paper as a zip file. The results of our CCD observations are presented in the figures in the main text of this paper. The tables include the results of all our data analysis.
We analyzed the time series using Deeming's method (Deeming, 1975), implemented in the WinEfk code written by V.P. Goranskij.
To search for double-mode variability, we used all available observations from the Northern Sky Variability Survey (ROTSE-I/NSVS2, Wozniak et al. 2004) and the Wide Angle Search for Planets (1SWASP3, Butters et al. 2010) online public archives. The 1SWASP observations are available as FITS tables, which were converted into ASCII tables using the OMC2ASCII program as described by Sokolovsky (2007); we also used the SuperWASP FITS to ASCII lightcurve conversion service4.
Based on these data, we reliably classified GSC 02901-00089 as a 1O/2O Cepheid, and suspected double periodicity of V470 Cas.
To confirm the double-mode variability and photometric study of these stars, we started multicolor CCD observations in 2013. Our CCD observations in the Johnson , and 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. The observatory has two Zeiss 1000-mm telescopes. Most of our observations were performed with the eastern Zeiss 1000-mm reflector (the focal length of the system was mm before JD 2456500 and 6650 mm after this date; the detector was an Apogee U9000 D9 CCD camera; the chip was cooled to C). The time interval of the observations for GSC 02901-00089 is JD 2456364-2456963 (March 12, 2013 - November 1, 2014); for V470 Cas, it is JD 2456575-2456964 (October 9, 2013 - November 2, 2014). Additionally, for observations of V470 Cas during two nights (JD 2456899 and 2456959), we used the newly introduced western Zeiss 1000-mm reflector (the focal length of the system was mm, the detector being an Apogee F16M CCD camera); during one night, JD 2456584, we used the 360-mm Ritchey-Chretien telescope designed by V.B. Sekirov (the focal length of the system is 1440 mm; the detector was an ST-402 SBIG CCD camera; the chip was cooled to C).
Reductions were performed using the MaxIm DL aperture photometry package. For GSC 02901-00089, we obtained a homogeneous observation set. For V470 Cas, exposures of different lengths were used, and we obtained a non-homogeneous observations set. In addition, the small amplitude of the second oscillation, 2O, requires minimal observation errors. Therefore, we averaged individual values over time intervals of nearly the same duration, each point being an average of 3-6 individual observations.
Information on the comparison stars and check stars used in our CCD photometry for the two Cepheids is presented in Table 1. Magnitudes of the comparison stars (in Johnson's and bands) were taken from the AAVSO Photometric All-Sky Survey (APASS, http://www.aavso.org/download-apass-data) catalog. The -band observations could be presented only as magnitude differences with respect to the comparison star. For GSC 02901-00089, the magnitude differences in the band are ; for V470 Cas, .
The finding charts of the two Cepheids are displayed in Fig. 1.
|Variable||V470 Cas||GSC 02901-00089|
|Compar.||Name||GSC 03678-00722||GSC 02901-00493|
|star||Coord., J2000||01321275 +563040 0||04450634 +425750 9|
|Check||Name||GSC 03678-01408||USNO-B1.0 1329-0132855|
|star||Coord., J2000||01315171 +562753 6||04445964 +425725 5|
Later, we have improved and supplemented our results using data of the All-Sky Automated Survey for Supernovae (ASAS-SN5, Shappee et al., 2014 and Kochanek et al., 2017). We used the photometric band of this survey.
The variability of V470 Cas = S8459 ( , J2000) was discovered by Hoffmeister (1964). The variable was classified as a short-periodic variable (possibly eclipsing), the variability range was 125 - 130. The first study of the variability of V470 Cas was published by Meinunger (1968) who classified the star as an eclipsing variable with the light elements:
The variability range is 130 - 135.
Gessner & Meinunger (1973) confirmed these light elements but remarked on their being not quite certain. Eight times of light minima were reported. The variable was included in the General Catalog of Variable Stars (Samus et al., 2017) based on this publication.
Agerer et al. (1996) performed CCD observations of V470 Cas and studied plates of the Sonneberg Sky Patrol. It was found that the star was not an eclipsing variable. V470 Cas is a possible RR Lyrae variable star with a long period and small amplitude. The amplitude of variability in the instrumental system (without filters) is 035. Asymmetry of the light curve is more typical of classical Cepheids ( ). During the interval of observations (photographic observations: JD 2436200-2448862, CCD observations: JD 2449170-2450013), the period of variability changed. Therefore, Agerer et al. (1996) gave two systems of the light elements:
for JD 2436200-2445000: HJD ;
for JD 2445000-2450013: HJD .
We suspected double-mode variability of V470 Cas from NSVS and 1SWASP data. The second frequency was detected sufficiently reliably in the NSVS data (for this analysis, we excluded data with the errors ); its detection in the 1SWASP data is much less certain. In the ASAS-SN -band observations, we excluded data with the errors .
Our classification of V470 Cas is confirmed with its low galactic latitude ( ) and color indices (2MASS), (Tycho2), and (APASS), typical of Cepheids.
Our CCD observations completely confirmed the double-mode nature of V470 Cas: this star is a double-mode Cepheid, pulsating in the first and second overtone modes. The period ratio is typical of the double-mode 1O/2O variables.
The light elements of the two pulsations for all data sets are presented in Table 2. Semi-amplitudes of the individual oscillations and variability ranges in individual bands are collected in Table 3. Besides the first and second overtone frequencies, we detected one interaction frequency, , of V470 Cas in our CCD data.
CCD light curves of V470 Cas in the , , and bands are displayed in Figs. 2 and 3. The power spectra according to CCD observations are displayed in Fig. 4. The structure of the power spectra leaves no doubt that is a real frequency.
|Data||, days||Epoch, HJD||, days||Epoch, HJD||, days|
Fig. 3. CCD observations: light curves in , , and bands for V470 Cas; the folded light curves for the 2O period with the other oscillation pre-whitened.
|NSVS (R)||0.137||0.026||-||11.95 - 12.40|
|1SWASP||0.189||0.015||-||11.92 - 12.42|
|0.3327||0.0364||0.0176||12.82 - 13.54|
|0.2447||0.0252||0.0116||12.03 - 12.58|
|ASAS-SN,||0.207||0.040||0.019||11.93 - 12.53|
Period variations of the first overtone oscillation () can be represented by an diagram, see Fig. 5. The parabolic shape of this diagram is typical of secular period variations of classical Cepheids, the period is increasing systematically. Figure 5 is based on linear light elements for the middle of the time interval:
Before JD 2449000, all points are times of high brightness according to photographic photometry; after JD 2449000, all points are CCD maxima. We used the data from Agerer et al. (1996), Agerer & Huebscher (2002), Huebscher (2005), Huebscher et al. (2005), Huebscher et al. (2006), Huebscher et al. (2009), Huebscher et al. (2010), Huebscher & Lehmann (2012), and data from our study.
Period of second overtone also varies (decreases), see Table 2.
Fig. 4. Power spectra of V470 Cas for the frequencies and according to CCD observations in the band. Upper panel: raw data; lower panel: the first overtone oscillation pre-whitened.
The variability of GSC 02901-00089 ( , J2000) was reported by Hoffman et al. (2009) from ROTSE-I/NSVS data (NSVS 4346946). The variable was classified as an RR Lyrae star with the period of 0.53391 days.
Later, we classified GSC 02901-00089 as a 1O/2O double-mode Cepheid (Khruslov 2013) using all available observations from the ROTSE-I/NSVS and SuperWASP online public archives. In the cited paper, we presented the preliminary results. The paper contained only the two periods and the new classification, CEP(B) variability type in the GCVS classifications system (Samus et al., 2017). Now we have re-analysed NSVS, 1SWASP and ASAS-SN data and our CCD observations, confirmed the 1O/2O double periodicity of GSC 02901-00089, and improved its light elements.
We detected double-mode variability of GSC 02901-00089 from NSVS and 1SWASP data. For this analysis, we excluded data with the errors in the NSVS data, and the errors in the 1SWASP data. In the ASAS-SN -band observations, we excluded data with the errors .
Our classification is confirmed with the low galactic latitude and with the color indices (2MASS), (APASS).
Our CCD observations completely confirmed the double-mode nature of GSC 02901-00089: this star is a 1O/2O double-mode Cepheid. The period ratio is typical of variables of this type. Besides the first and second overtone frequencies, we detected two interaction frequencies of GSC 02901-00089, and , in our CCD data.
The light elements of the two pulsations for all data sets are presented in Table 4: the first-overtone period and epoch, the second-overtone period and epoch, periods for the frequencies and . The periods and epochs are given for all individual data sets. Semi-amplitudes of the individual oscillations and the variability ranges in different bands are collected in Table 5. For the band, we give the full variability amplitude (peak to peak).
The CCD light curves in the , , and bands for GSC 02901-00089 are displayed in Figs. 6 and 7. The power spectra according to CCD observations are shown in Fig. 8. The structure of the power spectra leaves no doubt that is a real frequency.
The periods of the first and second overtone oscillations vary significantly, see Table 4. We can claim it beyond doubt for (progressive decrease). The diagram of the period variations of GSC 02901-00089 is displayed in Fig. 9.
|Data||, days||Epoch, HJD||, days||Epoch, HJD||, days||, days|
Fig. 6. CCD observations: light curves in , , and bands for GSC 02901-00089; raw data for the 1O period.
|NSVS||0.119||0.029||-||-||12.9 - 13.35|
|1SWASP||0.179||0.044||0.017||-||12.74 - 13.37|
|0.2349||0.0418||0.0154||0.0115||13.98 - 14.63|
|0.1626||0.0289||0.0114||0.0094||13.11 - 13.54|
|ASAS-SN,||0.133||0.028||0.012||0.009||13.02 - 13.46|
Fig. 7. CCD observations: light curves in , , and bands for GSC 02901-00089; the folded light curves for the 2O period with the other oscillation pre-whitened.
Fig. 8. Power spectra of GSC 02901-00089 for the frequencies and according to CCD observations in the band. Upper panels: raw data; lower panels: the first overtone oscillation pre-whitened.
Acknowledgments: The authors are grateful to Dr. V. P. Goranskij for providing light-curve analysis software. Thanks are due to Drs. S.V. Antipin and N.N. Samus for helpful discussions and to Dr. K.V. Sokolovsky for his advice concerning data retrieving. We wish to thank M.A. Krugov, N.V. Lichkanovsky, I.V. Rudakov, R.I. Kokumbaeva, and W. Mundrzyjewski for their assistance during the observations.
This study was supported in part by the Programme No. 12 "Origin and Evolution of the Universe from Ground-based Observations and Space Studies" of the Presidium of Russian Academy of Sciences. It was carried out within the framework of Project No. BR05236322 "Studies of physical processes in extragalactic and galactic objects and their subsystems", financed by the Ministry of Education and Science of the Republic of Kazakhstan.
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