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18Peremennye Zvezdy ( Variable ¡Stars) 39, No. 4, 2019 Received 11 December; accepted 18 December.
V470 Cas and GSC 02901-00089, Two New Double-mode Cepheids
DOI 10.24411/2221-0474-2019-00006
A. V. Khruslov1'2, A. V. Kusakin3, I. V. Reva3
1 Sternberg Astronomical Institute, Moscow State University, Universitetsky pr. 13, 119992, Moscow, Russia; e-mail: khruslov@bk.ru
2 Institute of Astronomy, Russian Academy of Sciences, Pyatnitskaya Str. 48, 119017, Moscow, Russia
3 Fesenkov Astrophysical Institute, Observatory 23, 050020, Almaty, Kazakhstan; e-mail: un7gbd@gmail.com
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 B, V and R bands in Johnson's system and ASAS-SN data in the V 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.
1 Introduction
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 0.69 < P1/P0 < 0.73 and P2/P1 = 0.80. 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 8 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.
1 http://www.aavso.org/vsx/
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).
2 Observations and data reduction
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.
2.1 NSVS and 1SWASP data
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 Super-WASP 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.
2.2 Our CCD observations
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 B, V and R 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 f = 13380 mm before JD 2456500 and 6650 mm after this date; the detector was an Apogee U9000 D9 CCD camera; the chip was cooled to —40° C). The time interval of the observations for GSC 0290100089 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 f = 13250 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
2 http://skydot.lanl.gov/nsvs/nsvs.php
3 http://wasp.cerit-sc.cz/form
4 http://scan.sai.msu.ru/swasp_converter/
Table 1. Comparison and check stars.
Variable V470 Cas GSC 02901-00089
Compar. Name GSC 03678-00722 GSC 02901-00493
star Coord., J2000 01h32m12S75 +56°30/40/./0 04h45m06S34 +42°57/50/./9
V mag 13.937 12.827
B mag 14.755 13.326
Check Name GSC 03678-01408 USN0-B1.0 1329-0132855
star Coord., J2000 01h31m51S71 +56°27/53/./6 04h44m59S64 +42°57/25/./5
system is 1440 mm; the detector was an ST-402 SBIG CCD camera; the chip was cooled to —20° 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 B and V bands) were taken from the AAVSO Photometric All-Sky Survey (APASS, http://www.aavso.org/download-apass-data) catalog. The R-band observations could be presented only as magnitude differences with respect to the comparison star. For GSC 02901-00089, the magnitude differences AR in the R band are AR for V470 Cas, AR = mvar — mcomp + 1m916.
The finding charts of the two Cepheids are displayed in Fig. 1.
m,
— m.
comp)
V470 Cas
GSC 2901-00089
POSS II red Figure 1. The finding charts.
• • T ■•
#
• • • • comp ■ ■ • ** » *
, ■ r * * • . 1 '
• • 1 . . ■ check .
var ■ X.
• * ■ ' * • \ • • • * » , * N J •
POSS II red 7'x7'
2.3 ASAS-SN data
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 V photometric band of this survey.
3 V470 Cas
3.1 Earlier studies
The variability of V470 Cas = S8459 (a = 01h32m18!16, 5 = +56°29/58"0, J2000) was discovered by Hoffmeister (1964). The variable was classified as a short-periodic variable (possibly eclipsing), the variability range was 12m5 - 13m0. 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:
Mini (JD) = 2429231.369 + 0d444692 x E. The variability range is 13m0 - 13m5.
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 0m35. Asymmetry of the light curve is more typical of classical Cepheids (M — m = 0?35). 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(max) = 2436200.588 + 0d874356 x E; for JD 2445000-2450013: HJD(max) = 2449170.518 + 0d8744654 x E.
3.2 Analysis of survey photometric data
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 err > 0m05); its detection in the 1SWASP data is much less certain. In the ASAS-SN V-band observations, we excluded data with the errors err > 0m015.
Our classification of V470 Cas is confirmed with its low galactic latitude (b = —5°9) and color indices J — K = 0.48 (2MASS), B — V = 0.94 (Tycho2), and B — V = 0.84 (APASS), typical of Cepheids.
3.3 CCD observations
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 P2/P1 = 0.8029 is typical of the double-mode 1O/2O variables.
5 https://asas-sn.osu.edu/
Table 2. Light elements of V470 Cas.
Data P1, days Epoch1, HJD P2, days Epoch2, HJD P2+i, days
NSVS 1SWASP CCD ASAS-SN 0.8744 0.8745 0.87454 0.87454 2451510.732 2454390.438 2456789.160 2457777.400 0.7028 0.7025 0.70217 0.70214 2451510.920 2454390.425 2456789.670 2457777.575 0.389467 0.389460
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, f2 + f1, of V470 Cas in our CCD data.
CCD light curves of V470 Cas in the B, V, and R 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 f2 is a real frequency.
A R
-0.1 0.0 0.1 0.2 0.3 0.4
B
12.7
12.8 12.9
13.0
13.1
13.2
13.3
13.4
13.5
13.6
0.0 0.5 1.0 1.5
Phase
Figure 2. CCD observations: light curves in B, V and R bands for V470 Cas; raw data for the 1O period.
Table 3. Semi-amplitudes and variability ranges of V470 Cas.
Band Ai A2+1 mag
NSVS (R) 0.137 0.026 - 11.95 - 12.40
1SWASP 0.189 0.015 - 11.92 - 12.42
B 0.3327 0.0364 0.0176 12.82 - 13.54
V 0.2447 0.0252 0.0116 12.03 - 12.58
R 0.1910 0.0185 0.0092 0.42
ASAS-SN, V 0.207 0.040 0.019 11.93 - 12.53
Figure 3. CCD observations: light curves in B, V, and R bands for V470 Cas; the folded light curves for the 2O period with the other oscillation pre-whitened.
3.4 Period variations
Period variations of the first overtone oscillation (Pi) can be represented by an O — C 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:
HJD(max)= 2446000.633 + 0d874434 x E.
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 P2 also varies (decreases), see Table 2.
Figure 4. Power spectra of V470 Cas for the frequencies fi and f2 according to CCD observations in the V band. Upper panel: raw data; lower panel: the first overtone oscillation pre-whitened.
Figure 5. O — C diagram for the period of the first overtone oscillation of V470 Cas.
4 GSC 02901-00089
4.1 Earlier studies
The variability of GSC 02901-00089 (a = 04h45m23s89, 8 = +42°55'20"0, 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.
4.2 Analysis of survey photometric data
We detected double-mode variability of GSC 02901-00089 from NSVS and 1SWASP data. For this analysis, we excluded data with the errors err > 0m 1 in the NSVS data, and the errors err > 0m.05 in the 1SWASP data. In the ASAS-SN V-band observations, we excluded data with the errors err > 0m02.
Our classification is confirmed with the low galactic latitude b = — 1°7 and with the color indices J — K = 0.54 (2MASS), B — V =1.05 (APASS).
4.3 CCD observations
Our CCD observations completely confirmed the double-mode nature of GSC 0290100089: this star is a 1O/2O double-mode Cepheid. The period ratio P2/Pi = 0.8036 is typical of variables of this type. Besides the first and second overtone frequencies, we detected two interaction frequencies of GSC 02901-00089, f2 + fi and f2 — fi, in our CCD data.
The light elements of the two pulsations for all data sets are presented in Table 4: the first-overtone period Pi and epoch, the second-overtone period P2 and epoch, periods for the frequencies f2 + fi and f2 — fi. 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 R band, we give the full variability amplitude (peak to peak).
The CCD light curves in the B, V, and R 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 f2 is a real frequency.
4.4 Period variations
The periods of the first and second overtone oscillations vary significantly, see Table 4. We can claim it beyond doubt for Pi (progressive decrease). The diagram of the period variations of GSC 02901-00089 is displayed in Fig. 9.
A.V. Khruslov et al.: V470 Cas and GSC 02901-00089, Two New Double-mode Cepheids Table 4. Light elements of GSC 02901-00089.
Data P1, days Epochi, HJD P2, days Epoch2, HJD P2+1, days P2-1, days
NSVS 1SWASP CCD ASAS-SN 0.53394 0.53389 0.533824 0.533818 2451450.393 2453700.227 2456650.325 2457777.770 0.42905 0.42905 0.428983 0.428976 2451450.387 2453700.333 2456650.288 2457777.630 0.23796 0.237848 0.237845 2.1843 2.1844
Figure 6. CCD observations: light curves in B, V, and R bands for GSC 02901-00089; raw data for the 1O period.
10 A.V. Khruslov et al.: V470 Cas and GSC 02901-00089, Two New Double-mode Cepheids Table 5. Semi-amplitudes and variability ranges of GSC 02901-00089.
Band A A2+1 A2-1 mag
NSVS 0.119 0.029 - - 12.9 - 13.35
1SWASP 0.179 0.044 0.017 - 12.74 - 13.37
B 0.2349 0.0418 0.0154 0.0115 13.98 - 14.63
V 0.1626 0.0289 0.0114 0.0094 13.11 - 13.54
R 0.1278 0.0209 0.0091 0.0075 0.34
ASAS-SN, V 0.133 0.028 0.012 0.009 13.02 - 13.46
Figure 7. CCD observations: light curves in B, V, and R bands for GSC 02901-00089; the folded light curves for the 2O period with the other oscillation pre-whitened.
Figure 8. Power spectra of GSC 02901-00089 for the frequencies f and f2 according to CCD observations in the B band. Upper panels: raw data; lower panels: the first overtone oscillation pre-whitened.
Figure 9. The period variations of GSC 02901-00089.
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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