1 INTRODUCTION
OB associations host the gravitationally unbound youngest and massive stars in the galaxy; therefore, stellar parameters of the members of OB associations help understanding their structure and evolution. The most powerful technique to obtain age, chemical properties, and a reliable distance is doubtlessly the use of eclipsing binaries, which are the members of the association. Luckily, the relative number of eclipsing binary and multiple (EBM) systems in OB associations is high (e.g. Mason et al. Reference Mason, Gies, Hartkopf, Bagnuolo, ten Brummelaar and McAlister1998). Within the scope of investigating EBM systems in OB associations with modern analysis techniques (i.e. Bakış et al. Reference Bakış, Hensberge, Demircan, Zejda, Bilir and Nitschelm2015), an early-type massive binary DN Cas in the direction of Cas OB6 complex is selected for a more detailed study than available in the literature today.
Located in the front edge of the Perseus spiral arm, the Cas OB6 association is one of the most outstanding associations in the Cas OB complex (see Figure 1). Its distance and mean radial velocity were determined by Mel’nik & Dambis (Reference Meln’ik and Dambis2009) as 1.8 (kpc) and –42.7 ± 8.2 km s−1, respectively. The association hosts a number of H ii regions (IC 1805, IC 1848, S196, and S201) and several radio sources W5 (IC 1848), W4 (surrounding IC 1805), and the W3 region (IC 1795). These regions are known with massive stellar content and active stellar formation which goes back in time to 3–5 Myr for IC 1795 (Bik et al. Reference Bik2012), 1–3 Myr for IC 1805 (Straižys et al. Reference Straižys, Boyle, Janusz, Laugalys and Kazlauskas2013), and 3–5 Myr for IC 1848 (Lim et al. Reference Lim, Sung, Kim, Bessell and Karimov2014).
Figure 1. The distribution of the Cas OB associations towards galactic coordinates l = 120.3° and b = −0.9°, created with the Aladin Sky Atlas (Bonnarel et al. Reference Bonnarel2000). The borders of individual associations were determined using the catalogue data of Meln’ik and Dambis (Reference Meln’ik and Dambis2009) and Tetzlaff et al. (Reference Tetzlaff, Neuhäuser, Hohle and Maciejewski2010).
DN Cas is located within the borders of Cas OB6. Its photometric variation was discovered by Hoffmeister (Reference Hoffmeister1947) and has been observed photometrically by Frazier & Hall (Reference Frazier and Hall1974) for the first time. Due to variability of the selected comparison star, Frazier & Hall (Reference Frazier and Hall1974) was not able to solve the multi-band light curves. Davidge (Reference Davidge1980) performed UBV photometry of the system without the light curve solution. Zakirov (Reference Zakirov2001) who investigated the relationship of DN Cas with Cas OB6 made estimations on the absolute parameters of the companions using his own photometric data in UBVRI-bands . However, due to absence of the spectral information, the estimated parameters were not consistent with the spectral types of the components.
The most recent study on DN Cas is the radial velocity survey of the 14 association members of Cas OB6 (Hillwig et al. Reference Hillwig, Gies, Bagnuolo, Huang, McSwain and Wingert2006). They reported a binarity of 50% in their sample and obtained the spectroscopic orbit of DN Cas for the first time. Using the orbital parameters from the analysis of incomplete monochromatic light curve of DN Cas, stellar parameters of the components of DN Cas were estimated. However, necessity of multi-band photometric observations of the system was announced probably due to the need to clarify the inconsistency of the mass and spectral type of the components they derived.
2 OBSERVATIONS
2.1. Photometry
There are three sources of photometric data of DN Cas used in this research: The first set of photometric data comes from the observations of Zakirov (Reference Zakirov2001) which is not available in the literature. The observations of Zakirov (Reference Zakirov2001) were used in this paper for only orbital period study (Section 3). The second set of photometric data was collected from the observations which were performed in Çanakkale Onsekiz Mart University Ulupınar Observatory in 2009 with 30- and 40-cm Cassegrain–Schmidt type telescopes equipped with 1k × 1k CCDs and Bessell UBVRcIc filters. A total of 4 956 images have been collected in seven nights. The data obtained in this campaign was not evenly distributed in phase; therefore, they were used for only orbital period analysis with a new time of minimum (HJD 2455128.3279 ± 0.0005) (see Section 3).
The third set of photometric data was collected during the observing campaign in Akdeniz University Campus Telescope (AUCT) in 2012 using a 25-cm Ritchey–Chretien type telescope equipped with a back-illuminated 1k × 1k CCD camera and Bessell UBVRcIc filters. A total of 3 840 images has been collected in nine nights. The number of data and its distribution are enough to analyse the multi-band light curves of DN Cas. The mean standard deviation of the observations are 0.033, 0.011, 0.009, 0.007, and 0.010 in UBVRc and Ic filters, respectively. The comparison star HD 14558 was selected for differential photometry and the check star was SAO 12245. The reduction of the photometric data is standard for CCD photometry; bias and dark subtraction and flat field correction. The photometry of the reduced data were performed by means of aperture photometry where the star aperture was selected to be three times the FWHM of the stellar profile. A new time of primary minimum has been extracted from the AUCT observations (HJD 2456287.2716 ± 0.0003).
2.2. Spectroscopy
The spectroscopic observations has been obtained in 2013 with the intermediate resolution (R ~ 5 100) TUG Faint Object Spectrograph and Camera (TFOSC) attached to 1.5-m RTT150 telescope of TÜBİTAK National ObservatoryFootnote 1 , Turkey. TFOSC provides a wavelength coverage from λ = 330 to 1 200 nm in 11 spectral orders. A total of 20 spectra have been obtained with TFOSC. The reduction of TFOSC spectra has been made in Image Reduction and Analysis Facility (iraf Footnote 2 ) software . The journal of spectroscopic observations is given in Table 1 and two spectral orders obtained at three different epochs are shown in Figure 2. The spectral data obtained in this study were used as complementary to the existing radial velocity data of Hillwig et al. (Reference Hillwig, Gies, Bagnuolo, Huang, McSwain and Wingert2006).
Figure 2. Two spectral orders obtained at three different orbital phases.
Table 1. Journal of spectroscopic observations and radial velocities (RV) of the components.
The spectral lines of the components of DN Cas are well separated (see Figure 2) which allowed us to measure the spectral lines of the individual components reliably. The radial velocities of DN Cas were measured by means of fitting Gaussian to the line centres using the splot task in iraf. The uncertainties of the radial velocity measurements have been determined as the standard deviation of three consecutive measurements which is on the order of 2–3 km s−1. However, we estimate overall radial velocity uncertainty in the range 5–9 km s−1 due to the low resolution of the spectrograph. The measured radial velocities are given in Table 1.
3 ORBITAL PERIOD VARIATION
The best tool to analyse the orbital period variation is the O–C analysis. The available times of minima data of DN Cas were collected from the literature and listed in Table 2 together with those determined in this study. The O–C residuals in Table 2 were calculated with the following light elements (Kreiner, Kim, & Nha Reference Kreiner, Kim and Nha2001):
$$\begin{equation}
\text{HJD}_{\text{min}}= 2441388.5662 + 2^d.31095111 \times E,
\end{equation}$$
where
$\text{HJD}_{\text{min}}$
and E are the heliocentric time of conjunction for the primary minimum and the epoch number, respectively.
Table 2. Times of minima of DN Cas.
As listed in Table 2, the complete data set consists of 1 visual (vis), 21 photographic (pg), 7 photoelectric (pe), and 16 ccd times of minima. The visual and photographic observations are relatively less accurate; therefore, the weighting scheme was chosen as follows: vis and pg = 1, pe and ccd = 10.
The O–C residuals are plotted in Figure 3. The relative accuracy of the pe and ccd data except in a few case is noteworthy. The residuals after the epoch number 2 000 clearly shows a cyclic change which can be modelled by the light time effect (LTE) caused by gravitational disturbance of a distant companion to DN Cas. Irwin (Reference Irwin1959) derived the following equation [Equation (2] to represent the O–C variations in the case of an existence of a distant companion:
$$\begin{equation}
\Delta t=\frac{a^{\prime }_{12}\sin i^{\prime }}{c}\left\lbrace \frac{1-e^{\prime 2}}{1+e^{\prime }\cos \nu ^{\prime }}\sin (\nu ^{\prime }+\omega ^{\prime })+e^{\prime }\cos \omega ^{\prime }\right\rbrace ,
\end{equation}$$
where a′12, i′, e′, and ω′ are the semi-major axis, orbital inclination, eccentricity, and the argument of periastron of the long orbit (AB), respectively. Analysing the times of minima data with Equation (2) yielded the orbital period of the wide orbit as P 12 = 42(9) yr with an eccentricity of 0.37(0.2). Other orbital parameters of the distant companion are listed in Table 3. The best fitting LTE model is shown in Figure 3.
Table 3. Parameters of the wide orbit from the O–C analysis.
Figure 3. O–C residuals and the best fitting LTE orbit.
4 ANALYSIS OF THE PHOTOMETRIC AND RADIAL VELOCITY DATA
The photometric data in the UBVRc and Ic bands have been analysed together with the radial velocity data of DN Cas using the 2007 version of the Wilson–Devinney (wd) code (Wilson & Devinney Reference Wilson and Devinney1971). The initial values of the input parameters such as the orbital inclination, mass-ratio, and relative radii of the components were adopted from the work of Hillwig et al. (Reference Hillwig, Gies, Bagnuolo, Huang, McSwain and Wingert2006). The orbital period and the conjunction time were adopted from the orbital period analysis (Section 3) and fixed during the solution. The albedo and gravity darkening coefficients were set to 1.0 as suggested for early type stars. An infrared light source near DN Cas with an angular distance of 5.3 arcsec has been noted by Hillwig et al. (Reference Hillwig, Gies, Bagnuolo, Huang, McSwain and Wingert2006), which is in the area covered by our photometric aperture. Hence, the third light source has been considered and the third light contribution (l 3) has been converged during the solution. The orbital eccentricity was also taken into account and it was set as a free parameter during the first iterations.
The wd code converged and found the best fitting model parameters after a few iterations. Initial system parameters were altered and the data were re-analysed to check if the solution is stable and hence, final parameter set is reliable. Only a small value found for the eccentricity (e = 0.001) was doubtful. However, its relatively big uncertainty Δe = 0.003 decreased its reliability and allowed us to adopt a circular orbit although the system DN Cas did not still complete its circularisation time scale yet (see Section 5.3). Nevertheless, it should be noted that the effect of such a small eccentricity on the determination of the physical parameters of the components is negligible.
In order to check the synchronicity of the components with the orbit, we modelled the spectral lines of the components and it is found that they rotate synchronously with the orbit (see Table 5). In the wd code, this synchronous rotation is stated by fixing the F parameter to 1.0 for each parameter to express the rotation rate of the component star.
The shapes of the components of close binary systems departs from sphere due to tidal effects causing a shift of the light centres from the mass centre of the components. Due to the difference between the light centres and the mass centres of the component stars, the spectroscopic orbital model does not represent the true orbit (see the study by Özkardeş, Erdem, & Bakış (Reference Özkardeş, Erdem and Bakış2009) on the highly distorted star CN Hyi). In the case of DN Cas, both stars are well inside their roche lobes (see Table 4) and therefore nearly spherical. The final set of light curve and spectroscopic orbital parameters are listed in Table 4 and the model light curves together with the spectroscopic orbit are shown in Figure 4. The system is detached and both components were found to be well inside their roche lobes.
Figure 4. Light curve (top) and spectroscopic orbit (bottom) models. The radial velocities shown by filled and empty circles are from Hillwig et al. (Reference Hillwig, Gies, Bagnuolo, Huang, McSwain and Wingert2006) and the filled and empty squares are obtained in this study. Radial velocities shown with crosses were not included in the analysis.
Table 4. Results from the simultaneous solution of light curves of DN Cas. Adjusted and fixed parameters are presented in the separate panels of the table. Uncertainties of the adjusted parameters, as suggested by wd code, are given in brackets.
The third light contribution was found to be negligible in all bands. As calculated by Hillwig et al. (Reference Hillwig, Gies, Bagnuolo, Huang, McSwain and Wingert2006), the light contribution of the third star is 14% at H & K infrared bands. This means that the light contribution of the third light source is not detectable at the I-band. The nature of the third light source is discussed in Section 5.2.
5 DISCUSSION
5.1. Astrophysical parameters and the distance of the system
The simultaneous solution of the light curve and the radial velocity data allowed us to obtain the physical parameters of the components of DN Cas, which are presented in Table 5. The masses and radii of the components are derived with an uncertainty of ~ 0.5% . The masses of the components derived in this study is ~ 1% smaller than the masses derived by Hillwig et al. (Reference Hillwig, Gies, Bagnuolo, Huang, McSwain and Wingert2006), which is in the uncertainty box given for their mass determinations. Following the tables of stellar parameters given by Straižys & Kurilene (Reference Straižys and Kuriliene1981), the physical parameters of the components imply that the spectral types of the primary and secondary components are B0V and B1V.
Table 5. Close binary stellar parameters of DN Cas. Errors of parameters are given in brackets.
The distance of the system is calculated by deriving the unreddened colour indices of the components with the Q-method of Johnson & Morgan (Reference Johnson and Morgan1953). The unreddened colour indices allowed us to derive the interstellar extinction of Av = 3 m .1(0.03). The absolute visual magnitude of the components has been derived by using the bolometric magnitude and the bolometric correction. Visual magnitude of the system, interstellar extinction, and the absolute visual magnitude of the components has been used in the distance modulus to derive the distance of 1740 ± 220 pc for the system.
The rotational velocities of the components were also measured by means of fitting synthetic spectra to the spectral lines of the components. The model atmosphere parameters were adopted from Table 5 and the suitable model atmospheres were selected from the Kurucz/Grids of model atmospheresFootnote
3
. Modelling the spectral lines showed that both components rotate (
$V_{\text{rot}1}=160\,\text{km} \text{s}^{-1}$
,
$V_{\text{rot}2}=130\,\text{km} \text{s}^{-1}$
) in accordance with their synchronisation rotational velocities given in Table 5.
5.2. The unseen third companion
The orbital period analysis of the system (Section 3) yielded a cyclic period change, which was modelled with LTE orbit of P
12 = 42(9) yr. The mass function for this triple system is
$f(m_3)=a^{\prime }_{12}{\mathrm{\sin }}i^{\prime }/P_{12}=0.0006\pm 0.0002\,\text{M}_\odot$
. Assuming the inclination of the third component’s orbit is 90°, the mass of the third star is found to be
$0.88\,\text{M}_\odot$
. In case, the orbit of the third star is co-planar (i = i′ = 77.2°) with the close binary system, the mass of the third star is
$0.90\,\text{M}_\odot$
. If we assume a main-sequence star for the third companion, it should be a K0 type star and its light ratio in a system with B0 and B1 stars is much less than 1% . Low light contribution of the third star can explain its invisibility in the visible region of the light curve and spectra.
5.3. Evolutionary status of DN Cas
The evolutionary status of the components of DN Cas have been investigated by locating the components in the HR-diagram together with the evolutionary tracks and isochrones of Bertelli et al. (Reference Bertelli, Nasi, Girardi and Marigo2009) (see Figure 5). The chemical composition of DN Cas is not known, therefore, the isochrones in Figure 5 have been calculated for two metallicity values (Z = 0.02 and 0.04) in order to set the lower and upper limits of the age. Moreover, we have plotted the members of IC 1805 and IC 1848 open clusters in the same plane in Figure 5 to see if there is an age difference. The best fitting isochrones yielded an age of τ = 3 Myr for Z = 0.04 and τ = 5 Myr for Z = 0.019 with and uncertainty of ± 1 Myr. Isochrones in Figure 5 imply that the members of the two open clusters are 1–2 Myr younger than DN Cas.
Figure 5. Location of DN Cas components in the
$\log T_{\text{eff}}$
– log L plane together with the members of two nearby open clusters (IC 1805 and IC 1848).
According to Zahn (Reference Zahn1977), close binary systems tend to circularise their orbit due to tidal effects. Following his mathematical formulation, the circularisation time scale for DN Cas is ~ 22 ± 0.2 Myr. This circularisation time scale is apparently bigger than the age of the system (τ = 3–5 Myr) but the difference is small compared to stellar evolution. This may imply a possible eccentricity for the orbit. However, the light curve and spectroscopic orbit analysis yielded a very small eccentricity (e = 0.001) with a relatively big uncertainty box (Δe = 0.003). Moreover, we do not know the effect of the third star on the orbit circularisation. Therefore, higher quality observational data especially radial velocity measurements are needed to uncover the orbital eccentricity issue. One should note that a light curve alone does not provide a unique solution for e and ω but ecosω for eclipsing binary systems (Kallrath & Milone, Reference Kallrath and Milone2009).
5.4. Kinematical analysis and possible origin of DN Cas
To analyse the kinematical and dynamical properties of DN Cas, we have used the system’s proper motion, the distance, and the velocity of the centre-of-mass, which are given in Table 5. The proper motions were taken from the PPMXL Catalog of Positions and Proper Motions (Roeser, Demleitner, & Schilbach Reference Roeser, Demleitner and Schilbach2010), whereas the centre-of-mass velocity and the distance are evaluated in this study. The system’s space velocity with respect to Sun was calculated using Johnson & Soderblom’s (Reference Johnson and Soderblom1987) algorithm where the space velocity components and their errors were found as (U, V, W)=(43.0 ± 9.6, –21.8 ± 9.2, –18.1 ± 13.4) km s−1 and given in Table 5. The first-order galactic differential rotation corrections were taken into account for precise space velocities, i.e. –34.1 and –2.9 km s−1 for U and V space velocity components, respectively (Mihalas & Binney Reference Mihalas and Binney1981). The W component is not affected from this first-order approximation. The velocity components are also corrected for the peculiar velocity of the Sun, which is 8.5 ± 0.29, 13.38 ± 0.43, 7 ± 0.26 km s−1 given by Coşkunoğlu et al. (Reference Coşkunoǧlu2011). Thus, the final LSR space velocity components (U, V, W)
$_{\text{LSR}}$
of DN Cas are 17.4 ± 9.6, –5.5 ± 9.2, –11.6 ± 13.4 km s−1. So that the total space velocity of DN Cas is S = 21.6 ± 18.9 km s−1. This value is in agreement with the space velocities of young thin-disc stars (Leggett Reference Leggett1992).
We also have performed test-particle integration in a Milky Way potentials of disc, halo, and bulge components. The galactic orbital parameters of the system were calculated within the integration time of 3 Gyr using the galpy code of Bovy (Reference Bovy2015). This integration time corresponds to about 15 revolutions around the Galactic centre, so that the orbital parameters could be determined reliably. The perigalactic (
$R_{\text{min}}$
) and apogalactic (
$R_{\text{max}}$
) distances of the system were found as 8.07 and 9.83 kpc, respectively. It turned out that the maximum distance of the system from the Galactic plane and the planer ellipticity of the system are
$Z_{\text{max}}=203$
pc and about ep
= 0.10, respectively. These values show that DN Cas system is orbiting the Galaxy almost in a circular orbit and that the system belongs to the galactic thin-disc population.
We have also compared the kinematic data of OB associations and open clusters in the vicinity of the binary system in order to investigate the possible birthplace of DN Cas. There are two sources of kinematical data of associations, Mel’nik & Dambis (Reference Meln’ik and Dambis2009) and Tetzlaff et al. (Reference Tetzlaff, Neuhäuser, Hohle and Maciejewski2010). The space velocity components given in these studies are almost the same. According to the galactic velocities, the DN Cas is in agreement with Cas OB1 and Cas OB6 within the uncertainty box. However, the distance of Cas OB6 is given as 1.8 kpc by Meln’ik & Dambis (Reference Meln’ik and Dambis2009) and as 2.4 kpc by Tetzlaff et al. (Reference Tetzlaff, Neuhäuser, Hohle and Maciejewski2010), whilst the distance of Cas OB1 is given as 2 kpc by Meln’ik & Dambis (2010) and as 2 kpc by Tetzlaff et al. (Reference Tetzlaff, Neuhäuser, Hohle and Maciejewski2010). Nevertheless, there are distance determinations of the embedded clusters (see Section 1) in Cas OB6 which is in between 1.9–2.0 kpc. Moreover, according to the partition of Meln’ik & Dambis (Reference Meln’ik and Dambis2009) (see Figure 1), the direction of the binary goes through the Cas OB6 borders and ~ 10° far from the Cas OB1 association. Consequently, the possibility of Cas OB1 membership of DN Cas is weaker than its OB6 membership. Considering a similar radial extension of the Cas OB6 association with its tangential extension (234 pc) given by Tetzlaff et al. (Reference Tetzlaff, Neuhäuser, Hohle and Maciejewski2010), the photometric distance of DN Cas (d = 1.7 ± 0.2 kpc) implies that DN Cas is within the borders of Cas OB6. Moreover, the age of DN Cas (τ = 3–5 Myr) which is 1–2 Myr older than the embedded open clusters in Cas OB6 is another supporting evidence for the Cas OB6 membership. Further evidence which would rely on accurately determined chemical composition is needed for a secure membership.
6 CONCLUDING REMARKS
The present study of DN Cas, which is one of the massive members of Cas OB6 association, could be concluded with the following remarks:
-
• The physical parameters of DN Cas are obtained with high precision. These parameters allowed us to derive reliable distance and age for the system.
-
• Higher accuracy radial velocity measurements are necessary to investigate further if the very small eccentricity found in this study for the close orbit is true or spurious.
-
• The radial velocities given by Hillwig et al. (2010) perfectly matches the spectroscopic orbit without non-Keplerian effects. However, the model constructed for the system in the present study requires departures from pure-Keplerian motion in the radial velocities during the eclipses. More reliable radial velocities are necessary to clarify this discrepancy.
-
• It has been shown that DN Cas has at least one physically bound distant companion with a minimum mass of 0.86 M⊙ in a P 12 = 42(9) yr orbit.
-
• DN Cas is ~ 1–2 Myr older than some known clusters (IC 1805 and IC 1848) in Cas OB6 implying an age dispersion in stellar formation history of Cas OB6.
ACKNOWLEDGMENTS
The spectroscopic observations with TFOSC are granted by the TÜBİTAK National Observatory with the project code 12ARTT150-255. This research has made use of ‘Aladin sky atlas’developed at CDS, Strasbourg Observatory, France.
