A&A 407, 1059-1065 (2003)
E. Rodríguez1 - A. Arellano Ferro2 - V. Costa1 - M. J. López-González1 - J. P. Sareyan3
1 - Instituto de Astrofísica de Andalucía, CSIC, PO Box 3004, 18080 Granada, Spain
2 - Instituto de Astronomía, UNAM, PO Box 70-264, 4510 Mexico DF, Mexico
3 - Observatoire de la Côte d'Azur, BP 4229, 0634 Nice Cedex 4, France
Received 12 February 2003 / Accepted 12 June 2003
We present the results of simultaneous photometry carried out from 1999 to 2001 of the variable V2109 Cyg together with a spectroscopic analysis based on one high resolution spectrum obtained in 2000. From this study, the star is definitively classified as an evolved Sct-type variable with solar metal abundances. This conclusion is also supported by the detected multiperiodic pulsational behaviour and the observed variation of the m1 index over the pulsation cycle. This variation is slightly reversed relative to the V light curve, in very good agreement with the m1 variation expected from the photometric calibrations. Besides the main frequency f1=5.3745 cd-1 and its first harmonic 2f1, a secondary peak is found at f2=5.8332 cd-1 ( f1/f2=0.92) with f1 identified as a radial mode and f2 as non-radial. Whereas no significant variations are found in the amplitude of f1 from season to season, the amplitude of f2 changes strongly. Moreover, the main period has remained constant since 1990, within the observational uncertainties. Additional secondary frequencies may also be excited in this variable.
Key words: stars: variables: Sct - stars: individual: V2109 Cyg - stars: oscillations - techniques: photometric, spectroscopic
V2109 Cyg ( , F0) is a pulsating star discovered by the Hipparcos satellite (ESA 1997). It has a period of and full amplitude . However, the type of variability has been subject of controversy during the last few years: in the Hipparcos catalogue it is identified as an RRc-type variable, but Kazarovets et al. (1999) proposed a Sct-type classification whereas Kiss et al. (1999) claimed again this star as an RRc pulsator. Finally, Rodríguez et al. (2000) re-classified this star as a Sct variable on the basis of its period and its Strömgren photometric indices. The importance of this topic arises from the fact that if this star is an RR Lyr-type pulsator, it would be the RR Lyr-type variable with the shortest period known up to date. In order to clarify this point new photometric and spectroscopic observations have been carried out.
The photometric observations were collected through the years 1999 to 2001 at Sierra Nevada Observatory (SNO), Spain ( measurements using the 0.9 m telescope) and in 2000 at San Pedro Mártir Observatory (SPMO), Mexico (uvby photometry using the 1.5 m telescope). Both telescopes are equipped with identical six-channel spectrophotometers for simultaneous measurements in uvby or in the narrow and wide H channels (Nielsen 1983).
HD 189013 ( , A2) was used as main comparison star with HD 191022 ( , G0) as check star. The latter was used as comparison star by Kiss et al. (1999). Additionally, a few data of HD 193701 ( , F5IV) were also collected at SNO for calibration purposes. Table 1 lists the journal of the photometric observations. In the present work no variations, within our observational errors, were found for any of the comparison stars. No noticeable nightly zero-point shifts nor short-period periodicities are present. The mean values obtained for the C2-C1 differences on each of the nights were always the same within 0 002, as standard deviation, for any of the vby filters and 0 004 in the u band. Moreover, when Fourier analyses are perfomed, no significant peaks are detected in the spectra. No periodicities with amplitudes larger than about 1.5 mmag are present.
In order to transform our instrumental magnitude differences into the standard system, we have used the procedure described in Rodríguez et al. (1997). The agreement found between the derived standard differences from the two observatories was very good among each other and with those found in the different catalogues available in the bibliography (Olsen 1983, 1996; Hauck & Mermilliod 1998). However, large discrepancies are found for the derived values of V2109 Cyg with respect to the values published in Kiss et al. (1999), especially in the m1 and c1 indices. This seems to be very probably due to calibration problems by these authors as will be seen in Sect. 4. Our determined standard magnitude differences of V-C1 versus Heliocentric Julian Day have been deposited in the Commission 27 IAU Archives of Unpublished Observations, file 350E, and can also be requested from the authors.
In addition, one high resolution (42 000) spectrum of V2109 Cyg was
obtained on October 6, 2000 with the 1.93 m telescope of the Haute-Provence
Observatory (France). This telescope
is equipped with the echelle spectrograph ELODIE. Details of the
instrument are described by Baranne et al. (1996).
The spectrum was reduced
using the spectroscopic data reduction tasks of the IRAF package.
Period analysis, using the classical O-C method, was performed with the new times of maximum derived in the present work together with those determined by Kiss et al. (1999). The new times of maximum were calculated as an average over the three vby bands following the method described in Rodríguez et al. (1990). If we use a linear ephemeris, with a period of 0 186049 (from Kiss et al. 1999), to phase our data (time span of 1.43 years), we can see that this period does not work well, suggesting that the true period needs to be longer. In fact, a new linear ephemeris with origin in ) and period ) was derived in our O-C analysis with the residuals randomly distributed around zero, as listed in Table 2. This new value is in very good agreement with that of 0 1860656 given by the Hipparcos catalogue (ESA 1997) using the data collected by this satellite between the years 1990 to 1993. Thus, it suggests that the main period of V2109 Cyg has remained constant since 1990 and no sudden period decrease has occurred between 1991 and 1998, as mentioned by Kiss et al. (1999). In fact, when a Fourier analysis is performed to the V+y data of these authors, a main peak at f=5.3746 cd-1 (that is, period of 0 186060) is found in good agreement with our results.
On the other hand, from Table 2 we see that the residuals are too large (standard deviation of the fit is 0 0040) as compared with the estimated times of maximum error bars (0 0007). This means that a secondary period is probably present in the light curves. This agrees well with the differences found between the light curves obtained in different nights, as shown in Fig. 1 for the individual light curves obtained at &O.
|Figure 1: Nightly light curves of V2109 Cyg collected at San Pedro Mártir Observatory during seven nights in September, 2000. Different symbols correspond to different nights.|
|Figure 2: Power spectra in the v band before and after removing the frequencies detected in the Fourier analysis.|
|Figure 3: Light curves phased for each frequency after removing the other. Top panel: for f1. Bottom panel: for f2.|
This was confirmed when a Fourier analysis was made of our data collected in the year 2000 (our largest data set), following the method described in Rodríguez et al. (1998). When the v filter was analysed, a main peak was found at f1=5.3745 cd-1. A secondary peak was also detected at f2=5.8332 cd-1 after f1 and its first harmonic (2f1) were removed from the spectra. The corresponding power spectra are shown in Fig. 2. When these peaks are extracted, no new significant periodicities are present in our data. Similar results were obtained in the other filters.
Table 3 lists the amplitude signal/noise (S/N) ratios obtained for each of the frequencies and filters, following Handler et al. (1996). As shown, the three peaks are intrinsic of the variable (Breger et al. 1993, 1996). Figure 3 shows the 2000 data set phased for each frequency after prewhitening of the other one. The results of the Fourier analysis are listed in Table 4. The amplitude ratios and phase shifts determined for different colours indicate that the secondary peak is also due to pulsation.
From Table 4 it can also be seen that the residuals in vby are smaller when the wavelength is larger. This suggests that more frequencies are remaining. This is also supported by the fact that these residuals are much larger than the white noise found for the C2-C1 spectra (e.g., in the filter v we have 8.7 mmag for V-C1, but only 3.1 mmag for C2-C1) taking into account that C2 and the variable are of similar brightness.
The existence of f2 is also confirmed when the 2000 data sets collected at SPMO and SNO are independently analysed. However, this cannot be found with our 1999 or 2001 data sets, because both the number of points and hours of observation are insufficient.
In order to investigate the existence of f2 in other data sets, the measurements collected in 1998 by Kiss et al. (1999), in both Strömgren and Johnson photometry, were analysed. The V and y data were merged and then investigated by means of Fourier analysis. The main peak was found at 5.3746 cd-1 in good agreement with our results. When this frequency and its first harmonic were removed from the spectra, no new peaks were present with amplitudes larger than 6.0 mmag. Similar results are found when the vby and BV data are analysed separately. Table 5 shows the results of the Fourier fitting when f1=5.3745 cd-1 and 2f1 are simultaneously extracted. Hence, f2 is not significant in these data sets, but the vby residuals decrease from filters v to b and y suggesting that some periodicities are still remaining in the light curves. In the case of the BV data, the noise level in the V filter is too high dominating over the eventually remaining signals.
The Hp data collected by the Hipparcos satellite (ESA 1997) were also investigated. The main peak is detected at 5.3745 cd-1 together with its first harmonic. When f1 and 2f1 are removed from the amplitude spectra, a flat spectrum remains with a level of about 6.0 mmag and no new peaks are detectable. The results of the fitting are listed in Table 5. The amplitude of f1 in Hp magnitudes is of ) mmag which means an amplitude in the Johnson V filter of ) mmag (Rodríguez 1999).
In summary, the secondary frequency f2=5.8332 cd-1 seems to be well established in the measurements obtained during the year 2000 with an amplitude of 10 mmag in the y=V filter. However, its existence has not been proven in the data collected during 1998 by Kiss et al. (1999) nor during the interval 1990-1993 by the Hipparcos satellite (ESA 1997). If this frequency is present in these data sets, it should be with an amplitude smaller than about 6 mmag. On the other hand, no significant variations are found in the amplitude of the main frequency f1=5.3745 cd-1.
Moreover, the corresponding period ratio P2/P1=0.92 indicates that at least one of the two frequencies corresponds to a nonradial mode. From Table 4, we can also see that the phase differences between the light curves in v and y or b and y are positive for f1 and negative for f2, suggesting that the main frequency corresponds to a radial mode while f2 is nonradial (Garrido et al. 1990). This is also supported by the observed phase shifts between b-y and y. Despite the error bars being too large in the Fourier fitting of the 1998 data sets (Table 5), the observed phase shifts seem to confirm that f1 corresponds to a radial mode.
This resembles the high amplitude Sct star RY Lep, where besides the main radial mode of constant amplitude, a secondary non-radial mode with variable amplitude within a time scale of years has been recently detected (Laney et al. 2003). Indeed, the secondary frequency is not detectable in some observing runs. Secondary frequencies with variable amplitudes are also detected in the medium amplitude Sct-type star AN Lyn (Zhou 2002) and strong amplitude variations of the main frequency are also found in the low amplitude Sct variable 28 And (Rodríguez et al. 1998) where the secondary frequency is commonly below the limit of photometric detectability.
|C1 = HD 189013||6.890||0.089||0.171||1.011||2.846|
|C2 = HD 191022||7.438||0.413||0.192||0.391||2.603|
|C3 = HD 193701||6.981||0.301||0.167||0.503||2.659|
|C1 = HD 189013||6.885||0.089||0.176||1.015||2.843|
|C2 = HD 191022||7.444||0.410||0.190||0.382||2.602|
|C3 = HD 193701||6.978||0.307||0.162||0.512||2.663|
With the aim of deriving the uvby indices for each of the stars observed in the present work, we followed the method described in Rodríguez et al. (2003). Thus, we use the uvby indices listed in earlier catalogues for each of the three comparison stars as zero-points and then, derive the indices for the remaining objects. In the case of C1 and C3, the more homogeneous catalogue of Olsen (1996) was used, but that of Hauck & Mermilliod (1998) was chosen for C2 (this star was not available in the former catalogue). The corresponding values are listed in the lower part of Table 6. The new derived indices for each of the comparison stars are presented in the upper part of the same table together with the number of points collected and the errors, as the standard deviations of the magnitude differences relative to C1. Good agreement is found between our derived indices and those found in earlier catalogues. This is also true when we compare with the values of C1 and C3 given in the other available lists of Olsen (1983) and Hauck & Mermilliod (1998).
In the case of V2109 Cyg, we list the mean values over the pulsation cycle based on the normal points of Table 7 (the large sigma values are due to the intrinsic variation of the star). These normal points were calculated according to the standard magnitude differences of V-C1 and the indices derived for C1. As it can be seen, some discrepancies seem to be present for the V and c1 values of V2109 Cyg as compared with the indices in the literature (Olsen 1996). However, these indices are based in a few points obtained by Olsen (1983) during only one night and the corresponding phase is unknown, but very probably near the light maximum. In fact, if we compare with our normal points at phase 0.15 (Table 7), the agreement is very good.
The indices listed in Table 6 for each of the comparison stars are also in good agreement with the spectral types published in the literature (Simbad 2002). They indicate that C1 is placed inside the Sct instability region whereas C2 and C3 are too cool to be both Dor or Sct-type pulsators.
|Eb-y||0 037||0 001||-|
|(b-y)0||0 189||0 015||0 168-0 208|
|m0||0 184||0 001||0 183-0 185|
|c0||0 831||0 036||0 883-0 785|
|m1||-0 001||0 004||0 005-|
|c1||0 177||0 011||0 150-0 190|
|Mv||1 14||0 3||-|
|1 15||0 3||-|
|D.M.||6 19||0 3||-|
|Age (Gyr)||1.0-1.4||0 1||-|
The V light and colour index variations over the main pulsational cycle were phased in Fig. 4 according to the linear ephemeris derived in Sect. 3. Normal points every 0.05 units of phase were calculated and listed in Table 7. Their standard errors are typically of 0 002, 0 001, 0 001, 0 003 and 0 004 in V, b-y, m1, c1 and , respectively. The method described in Rodríguez et al. (2001) was used to estimate the physical parameters of V2109 Cyg and their variation along the pulsation cycle. Thus, using the Crawford's (1979) calibrations, the reddening can be derived by comparing the intrinsic and observed b-y values at normal points along the cycle. In this way, a mean colour excess of ) is obtained. The results are summarized in Table 8 indicating that this star is a normal Population I Sct-type variable with approximately solar metal abundances and slightly evolved. The location of V2109 Cyg in the H-R diagram is shown in Fig. 5, together with the sample of known Sct-type variables.
In deriving its luminosity,
the obtained photometric value (Mv(ph) = 1
39( 0.3)) and
the one determined from
its Hipparcos parallax (Mv() = 0
88( 0.27), ESA 1997)
The metal content [Me/H]
was calculated from the m1 parameter
at minimum light (phases between 0.5 and 0.7) where the metal lines are
strongest and m1 is most sensitive to abundance differences. In this
and a value of
obtained using the Smalley's (1993)
calibration for metal abundances.
Figure 6 presents the changes in effective temperature
and surface gravity in a (c1, b-y) versus (,
(Smalley & Kupka 1997). If the evolutionary tracks
for Z=0.02 from Claret (1995) are used, the position of the star is
close to the overall contraction phase. Assuming the star is still in the main
sequence stage, a mass of
and an age of
) Gyr are estimated. If the star had already evolved off the main
sequence, values of 2.00
and 1.4 Gyr are found.
|Figure 5: Location of V2109 Cyg (star) in the H-R diagram together with the sample of Sct-type pulsators from Rodríguez & Breger (2001). The edges of the observational Dor region (dashed lines), from Handler & Shobbrook (2002), are also shown.|
The above conclusion on the Sct nature of V2109 Cyg is also supported by the behaviour of the m1 index along the pulsational cycle.
The metallicity of this variable can also be derived using the observed variation of the m1 index over the pulsation cycle (Rodríguez et al. 1991). This variation is slightly reversed with respect to the V light curve, as shown in Fig. 4, suggesting solar metal abundances for a star in a similar evolutionary stage as V2109 Cyg (<> =7080 K, <> =3.67). The same behaviour is shown in Fig. 1 of Kiss et al. (1999).
From our data, we find a total variation of (see Table 7) along the pulsational cycle (the negative sign means that m1 is higher when the luminosity or temperature are lower and viceversa). Then, a variation of 0 012 (in the same sense of the light curve) is found for the metallicity m1 parameter over the pulsation cycle. This means (the total observed variation in the index is = 0 038) a m1 variation of 0 032 per 0 1 variation in the index as shown in Table 9. This variation is similar to that found for other high amplitude Sct stars, in particular RY Lep which presents , <> = 7010 K and <> = 3.43 (Rodríguez et al. 1995).
In the case of V2109 Cyg, <> = 2
<> = 3.67. Hence, taking into account the observed variation
m1 = -0
002, we find
a metal content of
grids of Rodríguez et al. (1991).
This is in perfect agreement with the value previously obtained
in Table 8.
However, if the value of
= -0.9 (Kiss et al.
1999) is assumed, a
variation of m1 = +0
012 should be expected over the pulsation
cycle of V2109 Cyg in bad agreement with the observations. Thus, it is
followed that V2109 Cyg is a Population I Sct-type variable rather
than a RR Lyr star.
|Figure 6: Observed loop in the (c1, b-y) diagram. and lines are from Smalley & Kupka (1997) for .|
The same conclusion on the nature of V2109 Cyg is also supported by the analysis of abundances carried out on the high resolution spectrum obtained with the echelle spectrograph ELODIE.
Before performing a line synthesis analysis of the spectrum, we estimated its effective temperature by comparing the width of H at residual intensities between 0.7 and 0.9, with those of the theoretical profiles calculated by Kurucz (1993) for all gravities. We found between 6500 and 6800 K as initial values for the synthesis analysis.
We have used ATLAS9 (Kurucz 1993) model atmospheres as an input to the 1997 version of LTE line synthesis program MOOG first described in Sneden (1973). The procedure assumes plane-parallel atmospheres, hydrostatic equilibrium and LTE.
We have worked without prejudice of the RR Lyr or Sct nature
of the star in assigning initial values to log g. We used excitation
equilibrium of Fe I lines to get a preliminary estimate of ,
that the derived abundances be independent of the lower excitation potential
of the lines, followed by ionisation equilibrium of Fe I/Fe II, Ti I/Ti II
and Cr I/Cr II to arrive at a satisfactory estimate of
The microturbulence velocity
was estimated by requiring that weak,
medium and strong lines give a consistent value of abundance. The
atmospheric parameters found were
) dex and
) km s-1 in good agreement with those values
obtained from photometric calibrations (Table 8).
The derived elemental abundances are listed in Table 10. The discussion on the uncertainties in the elemental abundances obtained by the above procedure can be found in Arellano Ferro et al. (2001). The errors in [X/H] elemental abundances can be found by dividing the standard deviations by the square root of the number of lines used given in Table 10.
Recently, Kiss et al. (1999) concluded that the star is a RR Lyr based upon their Strömgren photometry and a number of empirical calibrations. These authors estimated ) K, ) and ). Our detailed atmospheric analysis does not support their conclusions. Based on 122 Fe I and 16 Fe II lines cleanly seen in our high resolution spectrum, we find that V2109 Cyg has solar iron and calcium abundance, precluding the classification of this object as an RR Lyr star. Moreover, a mean value of ) dex is obtained from Table 10 (calculated as an average with weighting according to the corresponding error bars) in very good agreement with that of ) dex derived from photometry.
Therefore our abundances analysis of the atmosphere of V2109 Cyg does not support its classification as an RR Lyr star but confirms the Sct classification obtained independently on pulsational arguments.
As s-process elements can only be formed in the hot bottom burning convection region of stars ascending the AGB (e.g. Arellano Ferro et al. 2001), small overabundances of Y, Zr, Ba and Ce in this mildly evolved star are probably explained as an inheritance of the star from the original star-forming cloud.
This research was supported by the Junta de Andalucía and the Dirección General de Investigación (DGI) under project AYA2000-1559 and by DGAPA-UNAM (Mexico) under project number IN110102-3. This research has made use of the Simbad database, operated at CDS, Strasbourg, France. Acknowledgements are made to L. L. Kiss for making available his 1998 data sets on V2109 Cyg.