The orbits of subdwarf-B + main-sequence binaries

The orbits of subdwarf-B + main-sequence binaries

II. Three eccentric systems; BD 293070, BD 341543 and Feige 87
J. Vos Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, B-3001 Leuven, Belgium
   R.H. Østensen Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, B-3001 Leuven, Belgium
   P. Németh Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, B-3001 Leuven, Belgium
   E.M. Green Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA    U. Heber Dr. Remeis-Sternwarte Astronomisches Institut, Universität Erlangen-Nürnberg, D-96049 Bamberg, Germany    H. Van Winckel Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, B-3001 Leuven, Belgium
Received July 16, 2019; accepted ???
Key Words.:
stars: evolution – stars: fundamental parameters – stars: subdwarfs – stars: binaries: spectroscopic

Context:The predicted orbital-period distribution of the subdwarf-B (sdB) population is bi-modal with a peak at short ( 10 days) and long ( 250 days) periods. Observationally, many short-period sdB systems are known, but the predicted long period peak is missing as orbits have only been determined for a few long-period systems. As these predictions are based on poorly understood binary-interaction processes, it is of prime importance to confront the predictions with reliable observational data. We therefore initiated a monitoring program to find and characterize long-period sdB stars.

Aims:In this paper we aim to determine the orbital parameters of the three long-period sdB+MS binaries BD+293070, BD+341543 and Feige 87, to constrain their absolute dimensions and the physical parameters of the components.

Methods:High-resolution spectroscopic time series were obtained with HERMES at the Mercator telescope on La Palma, and analyzed to determine the radial velocities of both the sdB and MS components. Photometry from the literature was used to construct the spectral-energy distribution (SED) of the binaries. Atmosphere models were used to fit these SEDs and to determine the surface gravities and temperatures of both components of all systems. Spectral analysis was used to check the results of the SEDs.

Results:An orbital period of 1283 63 d, a mass ratio of = 0.39 0.04 and a significant non-zero eccentricity of = 0.15 0.01 were found for BD+293070. For BD+341543 we determined = 972 2 d, = 0.57 0.01 and again a clear non-zero eccentricity of = 0.16 0.01. Last, for Feige 87 we found = 936 2 d, = 0.55 0.01 and = 0.11 0.01.

Conclusions:BD+293070, BD+341543 and Feige 87 are long period sdB + MS binaries on clearly eccentric orbits. These results are in conflict with the predictions of stable Roche-lobe overflow models.

1 Introduction

Hot subdwarf-B (sdB) stars are core helium burning stars with a very thin hydrogen envelope (M 0.02 ), and a mass close to the core helium flash mass 0.47 (Saffer et al. 1994; Brassard et al. 2001). These hot subdwarfs are found in all galactic populations, and they are the main source for the UV-upturn in early-type galaxies (Green et al. 1986; Greggio & Renzini 1990; Brown et al. 1997). Furthermore, their photospheric chemical composition is governed by diffusion processes causing strong He-depletion and other chemical peculiarities (Heber 1998). The formation of these extreme horizontal branch objects is still puzzling. To form an sdB star, its progenitor needs to lose its hydrogen envelope almost completely before reaching the tip of the red giant branch (RGB), so that the core ignites while the remaining hydrogen envelope is not massive enough to sustain hydrogen shell burning. A variety of possible formation channels have been proposed. The earlier suggestions were based on single star evolution, e.g. stellar wind mass loss near the tip of the RGB (D’Cruz et al. 1996) or enhanced mass loss due to rotationally driven helium mixing (Sweigart 1997). It was found, however, that many sdB stars reside in binary systems (Maxted et al. 2001), indicating that binary interaction plays an important role (Mengel et al. 1976). Currently, there is a consensus that sdB stars are formed by binary evolution only, and several evolutionary channels have been proposed, where binary-interaction physics plays a major role. Close binary systems can be formed in a common envelope (CE) ejection channel (Paczynski 1976), while stable Roche-lobe overflow (RLOF) can produce wide sdB binaries (Han et al. 2000, 2002). An alternative formation channel forming a single sdB star is the double white dwarf (WD) merger, where a pair of white dwarfs spiral in to form a single sdB star (Webbink 1984).

Han et al. (2002, 2003) addressed these three binary formation mechanisms, and performed binary population synthesis (BPS) studies for two kinds of CE ejection channels, two possible stable RLOF channels and the WD merger channel. The CE ejection channels produce close binaries with periods of = 0.1 – 10 d, and main-sequence (MS) or white-dwarf (WD) companions. The sdB binaries formed through stable RLOF have orbital periods ranging from 10 to 500 days, and MS companions. An alternative stable RLOF channel based on the -formalism is described by Nelemans et al. (2000, 2001); Nelemans (2010) and can produce sdB binaries with periods on the order of years. Finally, The WD merger channel can lead to sdB stars with a higher mass, up to 0.65 . A detailed review of hot subdwarf stars is given by Heber (2009).

Many observational studies have focused on short-period sdB binaries (Koen et al. 1998; Maxted et al. 2000, 2001; Heber et al. 2002; Morales-Rueda et al. 2003; Napiwotzki et al. 2004; Copperwheat et al. 2011), and over 100 of these systems are currently known (Geier et al. 2011, Appendix A). These observed short-period sdB binaries correspond very well with the results of BPS studies. However, only a few long period sdB binaries are known (Green et al. 2001; Østensen & Van Winckel 2011, 2012; Deca et al. 2012; Barlow et al. 2012; Vos et al. 2012), and the current studies show that there are still large discrepancies between theory and observations (Geier 2013). In a recent response to these discoveries Chen et al. (2013) have revisited the RLOF models of Han et al. (2003) with more sophisticated treatment of angular momentum loss. Their revised models show mass – orbital period relations that increase substantially as a function of composition, with solar metallicity models reaching periods up to 1100 d. They also note that by allowing the transfer of material extending beyond the classic Roche lobe (atmospheric RLOF) they can reach periods as long as 1600 d.

In this paper we present the orbital and atmospheric parameters of the three long-period sdB + MS binaries BD+293070, BD+341543 and Feige 87, using the methods described in Vos et al. (2012), hereafter Paper I. In Sect. 2 the radial velocities are determined for both components after which the orbital parameters are derived. Using the obtained mass ratio, the atmospheric parameters are derived from the spectral-energy distribution (Sect. 3), and spectral analysis (Sect. 4). Furthermore, the surface gravity of the sdB component is estimated based on the gravitational redshift in Sect. 5. Finally in Sect. 6 and 8 all results are summarized. BD+293070, BD+341543 and Feige 87 are part of a long-term spectroscopic monitoring program, and preliminary results of these and five more systems in this program were presented in Østensen & Van Winckel (2011, 2012).

2 Spectroscopy

High resolution spectroscopic observations of BD+293070, BD+341543 and Feige 87 were obtained with the HERMES spectrograph (High Efficiency and Resolution Mercator Echelle Spectrograph, R = 85 000, 55 orders, 3770-9000 Å, Raskin et al. 2011) attached to the 1.2-m Mercator telescope at the Roque de los Muchachos Observatory, La Palma. HERMES is connected to the Mercator telescope by an optical fiber, and is located in a temperature controlled enclosure to ensure optimal wavelength stability. In [Sect. 2]Vos12 the wavelength stability was checked, using 38 radial velocity standard stars of the IAU observed over a time span of 1481 days, and a standard deviation of 80 m s with a non-significant shift to the IAU radial velocity standard scale was found. In total there were 31 spectra of BD+293070, 30 of BD+341543 and 33 of Feige 87 taken between June 2009 and January 2013. The observations are summarized in Table 1. HERMES was used in high-resolution mode, and Th-Ar-Ne exposures were made at the beginning and end of the night. The exposure time of the science observations was adapted to reach a signal-to-noise ratio (S/N) of 25 in the –band, whenever observing conditions permitted. The HERMES pipeline v5.0 was used for the basic reduction of the spectra, including barycentric correction.

For BD+341543 there was one more high resolution spectrum available, taken with the FOCES spectrograph (Fiber-Optics Cassegrain Echelle Spectograph, R = 30 000, 3600-6900 Å) attached to the 2.2-m telescope at Calar Alto observatory, Spain. This spectrum was obtained in February 2000 (HJD = 2451576.5166). The spectrum was reduced as described in Pfeiffer et al. (1998) using the IDL macros developed by the Munich Group.

Flux-calibrated spectra of BD+293070, BD+341543, and Feige 87 were taken with the Boller and Chivens (B&C) spectrograph attached to the University of Arizona’s 2.3 m Bok telescope located on Kitt Peak. All three stars were observed using a 2.5” slit and 1st order 400/mm grating blazed at 4889 A, with a UV-36 filter to block 2 order light. These parameters provided a 9 Å resolution over the wavelength range 3600-6900 Å. BD+293070 was observed on 25-06-2000 with an exposure time of 30 s, resulting in an overall S/N of 235 per resolution element (134 per pixel, and slightly higher in the range 3600-5000 Å). BD+341543 was observed once on 17-09-1998 and five additional times between 2005 and 2007, for a total exposure time of 260 s and a (formal) S/N 750 (435 per pixel). Feige 87 was observed twice, on 10-03-1999 and 06-06-1999, for a total exposure time of 210 s and S/N of 345 (195 per pixel). The spectra were bias-subtracted, flat-fielded, optimally extracted, and wavelength calibrated using standard IRAF111IRAF is distributed by the National Optical Astronomy Observatory; see tasks. They were flux calibrated using either BD+284211 or Feige 34 as flux standards. The individual spectra for BD+341543 and Feige 87 were combined by determining the cross-correlation velocities using only the Balmer and helium lines, and shifting each spectrum to the mean sdB velocity before combining (although the velocity shifts were always small, less than 1/3 of a pixel, compared to the spectral resolution 3.15 pixels). While these spectra have a too low resolution to obtain radial velocities, they are used to determine spectroscopic parameters of both components in Section 4.3.

BD+293070 BD+341543 Feige 87
BJD Exp. BJD Exp. BJD Exp.
–2450000 s –2450000 s –2450000 s
5029.4643 1800 5166.5252 700 5028.4488 1800
5040.4568 1800 5218.5730 600 5028.4703 1800
5055.4675 1200 5238.5505 900 5028.4917 1800
5060.3980 1210 5238.5664 900 5251.7145 890
5321.6137 1500 5238.5775 900 5251.7247 390
5351.4739 1500 5240.5316 1800 5341.5722 1603
5425.4024 1600 5475.6918 900 5351.4184 2700
5619.7185 1500 5502.7281 900 5371.4175 2700
5638.6611 1700 5507.6955 900 5566.7810 2700
5648.6732 1500 5553.5767 900 5616.6402 2100
5658.6816 1600 5614.5668 900 5622.7074 720
5670.5225 1500 5621.5560 800 5622.7317 2000
5678.5495 1940 5658.3476 594 5656.6032 911
5686.5327 1800 5807.7326 600 5658.5870 1210
5701.5513 1750 5844.6708 900 5660.6107 704
5718.4729 2000 5861.7131 900 5663.5411 1200
5745.4261 1950 5887.6807 900 5666.5345 1800
5761.5685 1800 5932.5869 900 5937.7967 1800
5772.5841 1950 5942.6039 1200 5964.6900 3400
5778.4452 1700 5949.5190 900 5965.5843 2400
5795.3894 1500 5954.4967 1000 5968.6517 1800
5808.3721 1500 5965.4262 1100 5990.7225 1800
5829.3696 1500 5968.6346 900 6017.6145 1500
5999.7619 900 5978.5722 1050 6042.4773 1800
6027.6990 1500 6007.5012 820 6060.4147 1800
6049.5559 1500 6043.4301 900 6064.5674 1800
6082.5484 1150 6058.3969 1500 6066.4652 1800
6135.4325 800 6066.3756 1800 6068.4574 1800
6135.4423 800 6068.3894 1250 6082.4504 1800
6139.4292 1400 6069.3668 900 6138.4374 1800
6145.4352 1000 6141.4016 1800
6196.3415 1800
6301.7679 1800
Table 1: The observing dates (mid-time of exposure) and exposure times of the spectra of BD+293070, BD+341543 and Feige 87

2.1 Radial Velocities

Østensen & Van Winckel (2011) determined preliminary orbital periods of both BD+293070, BD+341543 and Feige 87 based on the radial velocities of the cool companion and assuming circular orbits, resulting in respectively 1160 67 days, 818 21 days and 915 16 days. These long periods allow us to sum spectra that are taken within a five-day interval to increase the signal to noise (S/N), without significantly smearing or broadening the spectral lines. This five-day interval corresponds to about 0.5 % of the orbital period, and a maximum radial velocity shift of 0.06 km s. After this merging, 28 spectra of BD+293070, 22 spectra of BD+341543 and 19 spectra of Feige 87 remain, with a S/N varying from 25 to 50. These spectra with the averaged BJD in case of the merged spectra are displayed in Table 2, 3 and 4.

The radial velocities of the MS components are determined with the cross-correlation method of the HERMES pipeline, based on a discrete number of line positions. This is possible because the sdB component has only a few H and He lines, which are avoided in the cross correlation. To determine the radial velocities of the MS components of the three systems, a G2-type mask was used on orders 55-74 (4780 - 6530 Å) as these orders give the best compromise between maximum S/N for G-K type stars and absence of telluric influence. The final errors on the radial velocities (see Table 2, 3 and 4) are calculated taking into account the formal errors on the Gaussian fit to the normalized cross-correlation function and the error due to the stability of the wavelength calibration.

To determine the radial velocities of the sdB components a different technique is necessary as these stars have only few spectral lines visible in the composite spectra. The only spectral line that is not contaminated by the MS components is the He I blend at 5875.61 Å. To derive the radial velocity based on only one line, a more specific method is necessary to avoid unacceptably high errors. The region around the He I line is first cleaned by hand of all remaining cosmic rays after which it is normalized by fitting low order polynomials to the spectrum. The cleaned and normalized spectra are then cross correlated with a high-resolution synthetic sdB spectrum from the LTE grids of Heber et al. (2000). For all three systems a synthetic spectrum of = 30000 K, = 5.50 dex, and a resolution matching that of HERMES was used. Spectra with different and were tried, but did not result in a significant change. The cross correlation (CC) is carried out in wavelength space, and the resulting radial velocity is calculated by fitting a Gaussian to the cross-correlation function. The error is determined by performing a Monte-Carlo (MC) simulation in which Gaussian noise is added to the observed spectra after which the CC is repeated. The final error is based on the standard deviation of the radial-velocity results of 1000 MC iterations, the wavelength stability of HERMES and the dependence on the used sdB template. For a more elaborate explanation on the derivation of radial velocities from the HERMES spectra see [Sect. 2.1]Vos12. The final radial velocities of both the MS and sdB component of BD+293070 together with their errors are given in Table 2, while those of BD+341543 and Feige 87 can be found in Table 3 and 4 respectively.

The FOCES spectrum of BD+341543 is analyzed in exactly the same way as the HERMES spectra to determine the radial velocities of both components. The results are given in Table 3 together with the HERMES results.

MS component sdB component
BJD RV Error RV Error
-2450000 km s km s km s km s
5029.4643 -52.88 0.26 -68.81 0.66
5040.4568 -52.93 0.29 -67.11 0.54
5057.9327 -53.60 0.31 -67.54 0.63
5321.6137 -62.78 0.24 -42.40 0.63
5351.4739 -63.33 0.28 -41.13 0.70
5425.4024 -64.21 0.32 -38.11 0.92
5619.7185 -61.96 0.26 -47.31 0.40
5638.6611 -61.48 0.26 -46.01 0.60
5648.6732 -61.46 0.28 -49.33 0.42
5658.6816 -61.23 0.28 -49.87 0.46
5670.5225 -60.54 0.31 -49.68 0.65
5678.5495 -60.54 0.29 -49.87 0.57
5686.5327 -60.53 0.28 -50.48 1.51
5701.5513 -60.16 0.26 -50.08 0.45
5718.4729 -59.57 0.31 -51.23 0.62
5745.4260 -58.64 0.27 -53.05 0.56
5761.5685 -57.96 0.27 -54.34 0.47
5772.5840 -57.41 0.42 -55.12 1.16
5778.4452 -57.97 0.27 -56.52 0.53
5795.3894 -57.04 0.26 -56.18 0.52
5808.3721 -57.29 0.26 -57.48 0.81
5829.3696 -56.31 0.27 -60.02 0.49
5999.7619 -53.06 0.30 -68.54 0.60
6027.6990 -52.27 0.24 -69.76 0.54
6049.5559 -52.56 0.28 -70.69 0.59
6082.5484 -51.93 0.26 -71.97 0.52
6136.7680 -51.29 0.30 -71.20 0.97
6145.4352 -51.17 0.27 -73.82 0.56
Table 2: The radial velocities of both components of BD+293070.
MS component sdB component
BJD RV Error RV Error
-2450000 km s km s km s km s
1576.5166FOCES spectrum 29.23 0.25 38.66 1.02
5166.5252 37.78 0.28 22.99 1.06
5218.5730 38.22 0.16 23.70 0.64
5239.0565 37.89 0.18 22.93 0.85
5475.6918 28.84 0.15 40.31 0.72
5505.2118 27.43 0.18 39.93 0.59
5553.5767 26.53 0.14 42.56 0.41
5614.5668 26.06 0.18 43.16 0.86
5621.5560 26.32 0.15 43.37 0.55
5658.3476 26.49 0.18 42.43 1.07
5807.7326 29.81 0.16 37.27 0.66
5844.6708 30.83 0.16 36.26 0.54
5861.7131 31.03 0.14 35.21 0.48
5887.6807 32.11 0.16 33.09 0.44
5932.5869 33.17 0.14 30.80 0.47
5942.6039 33.67 0.14 31.00 0.43
5952.0079 33.85 0.14 31.00 0.47
5967.0304 34.00 0.16 30.38 0.45
5978.5721 34.43 0.17 28.29 0.69
6007.5012 35.16 0.14 26.71 0.47
6043.4301 36.11 0.15 25.59 0.61
6058.3969 36.20 0.22 25.36 1.45
6068.0440 36.10 0.18 24.30 0.77
Table 3: The radial velocities of both components of BD+341543.
MS component sdB component
BJD RV Error RV Error
-2450000 km s km s km s km s
5028.4488 28.02 0.12 42.74 0.48
5341.5722 31.03 0.13 39.20 0.71
5351.4184 31.74 0.31 37.43 0.93
5371.4175 32.33 0.25 35.43 0.47
5566.7810 40.20 0.35 22.72 0.59
5616.6402 40.42 0.31 22.35 0.69
5622.7074 39.77 0.35 20.36 0.47
5656.6032 39.63 0.36 21.10 0.86
5663.5411 39.78 0.38 20.40 0.49
5937.7967 29.72 0.16 41.10 0.58
5964.6900 28.30 0.32 42.98 0.50
5990.7225 26.68 0.17 46.81 0.75
6017.6145 24.14 0.81 46.12 0.95
6042.4773 24.42 0.37 49.18 0.80
6060.4147 24.30 0.37 51.28 1.11
6066.4651 24.04 0.25 50.75 0.63
6082.4504 23.80 0.28 50.80 0.62
6196.3415 26.92 0.29 45.67 0.72
6301.7679 32.12 0.30 36.19 0.48
Table 4: The radial velocities of both components of Feige 87.

2.2 Orbital parameters

Figure 1: The radial velocity curves for BD+293070 (left), BD+341543 (center) and Feige 87 (right). Top: spectroscopic orbital solution (solid line: MS, dashed line: sdB), and the observed radial velocities (HERMES: blue circles, FOCES: green squares, filled symbols: MS component, open symbols: sdB component). The measured system velocities of both components are shown by a dotted line. Middle: residuals of the MS component. Bottom: residuals of the sdB component.
BD+293070 BD+341543 Feige 87
Parameter MS sdB MS sdB MS sdB
(d) 1283 63 972 2 936 2
2453877 41 2451519 11 2453259 21
0.15 0.01 0.16 0.01 0.11 0.01
1.60 0.22 1.58 0.07 2.92 0.15
0.39 0.01 0.57 0.01 0.55 0.01
(km s) 57.58 0.36 56.8 0.9 32.10 0.06 33.12 0.15 32.98 0.08 34.32 0.16
(km s) 6.53 0.31 16.6 0.6 5.91 0.07 10.31 0.22 8.19 0.11 15.01 0.21
() 164 15 416 35 112 2 196 4 150 2 276 3
() 1.15 0.19 0.45 0.08 0.27 0.01 0.15 0.01 0.77 0.03 0.42 0.01
333 denotes the semi-major-axis of the orbit. The quoted errors are the standard deviation from the results of 5000 iterations in a Monte Carlo simulation.
Table 5: Spectroscopic orbital solutions for both the main-sequence (MS) and subdwarf-B (sdB) component of BD+293070 , BD+341543 and Feige 87.

The orbital parameters of the sdB and MS components are calculated by fitting a Keplerian orbit to the radial velocity measurements, while adjusting the period (), time of periastron (), eccentricity (), angle of periastron (), two amplitudes ( and ) and two systemic velocities ( and ). As a first guess for these parameters, the results of Østensen & Van Winckel (2011) were used. The radial velocity measurements were weighted according to their errors as . For each system, the Lucy & Sweeney (1971) test was used to check if the orbit is significantly eccentric. In the fitting process, the system velocities of both components are allowed to vary independently of each other, to allow for gravitational redshift effects in the sdB component (see [Sect. 4]Vos12, and Sect. 5 in this paper). The uncertainties on the final parameters are obtained using 5000 iterations in a Monte-Carlo simulation where the radial velocities were perturbed based on their errors. The spectroscopic parameters of BD+293070 and BD+341543 are shown in Table 5. The radial-velocity curves and the best fits are plotted in Fig. 1.

Feige 87 (= PG 1338+611) has been studied by Barlow et al. (2012) as part of a long term observing program with the Hobby-Eberly telescope lasting from January 2005 till March 2008. They published radial velocities for both the MS and sdB component. However, Barlow et al. (2012) find a difference in systemic velocity for the MS and sdB component of km s (compared to km s for the HERMES spectra), which they attribute to gravitational redshift. If this was caused by gravitational redshift, this shift would mean that the MS component has a higher surface gravity than the sdB component, a highly unlikely situation (see also Sect. 5). A more plausible cause can be found in the lines used to derive the radial velocities of the sdB component. Barlow et al. (2012) used both the He i 4472 and He i 5876 lines, but when comparing the He i 4472 line with a synthetic G2 spectrum, it is clear that this line is significantly contaminated by spectral features of the cool companion. In the analysis of the radial-velocity curves of Feige 87, we used their results of Barlow et al. (2012) of the MS component, but discarded the results of the sdB component. The phase-folded radial velocity curve of the HERMES data is shown in Fig. 1, while the radial velocity curve of both HERMES and Barlow et al. (2012) is shown in Fig. 2. The spectroscopic parameters of Feige 87 are given in Table 5.

Figure 2: The radial velocity curve of Feige 87, showing the spectroscopic orbital solution (solid line: MS, dashed line: sdB), and the observed radial velocities (HERMES: blue circles, Barlow et al.: green squares, filled symbols: MS component, open symbols: sdB component). The measured system velocities of both components based on the HERMES data and the MS radial velocities of Barlow et al. are shown by a dotted red line, while the system velocity of the sdB component based on the data of Barlow et al. is plotted in a green dotted line.

3 Spectral Energy Distribution

The spectral-energy distribution (SED) of the systems can be used to determine the spectral type of the MS and sdB component. We used photometric SEDs which were fitted with model SEDs to determine both the effective temperature and surface gravity of both components.

3.1 Photometry

To collect the photometry of both systems the subdwarf database444 (Østensen 2006), which contains a compilation of data on hot subdwarf stars collected from the literature, is used. These photometric measurements are supplemented with photometry obtained from several other catalogs as listed in Table 6. In total we obtained 17 photometric measurements for BD+293070, 14 for BD+341543 and 11 for Feige 87. Both accurate photometric measurements at short and long wavelengths are used to establish the contribution of the hot sdB component and the cool MS component.

Band Wavelength Width Magnitude Error
Å Å mag mag
Johnson Mermilliod et al. (1997) 3640 550 10.030 0.020
Johnson Mermilliod et al. (1997) 4450 940 10.600 0.020
Johnson Mermilliod et al. (1997) 5500 880 10.420 0.020
Johnson Kharchenko (2001) 4450 940 10.590 0.013
Johnson Kharchenko (2001) 5500 880 10.416 0.013
Johnson Richmond (2007) 5500 880 10.376 0.052
Cousins Richmond (2007) 7880 1490 10.026 0.053
Geneva Mermilliod et al. (1997) 3460 170 10.264 0.010
Geneva Mermilliod et al. (1997) 4250 283 9.638 0.010
Geneva Mermilliod et al. (1997) 5500 298 10.359 0.010
Geneva Mermilliod et al. (1997) 4020 171 10.523 0.011
Geneva Mermilliod et al. (1997) 4480 164 11.103 0.011
Geneva Mermilliod et al. (1997) 5400 202 11.075 0.011
Geneva Mermilliod et al. (1997) 5810 206 11.476 0.011
2MASS Cutri et al. (2003) 12410 1500 9.773 0.020
2MASS Cutri et al. (2003) 16500 2400 9.621 0.023
2MASS Cutri et al. (2003) 21910 2500 9.546 0.022
Johnson Kharchenko (2001) 4450 940 10.293 0.014
Johnson Kharchenko (2001) 5500 880 10.145 0.013
Johnson Richmond (2007) 5500 880 10.156 0.048
Cousins Richmond (2007) 7880 1490 9.758 0.077
Geneva Mermilliod et al. (1997) 3460 170 9.759 0.008
Geneva Mermilliod et al. (1997) 4250 283 9.362 0.009
Geneva Mermilliod et al. (1997) 5500 298 10.140 0.007
Geneva Mermilliod et al. (1997) 4020 171 10.215 0.010
Geneva Mermilliod et al. (1997) 4480 164 10.865 0.010
Geneva Mermilliod et al. (1997) 5400 202 10.854 0.010
Geneva Mermilliod et al. (1997) 5810 206 11.260 0.010
2MASS Cutri et al. (2003) 12410 1500 9.485 0.023
2MASS Cutri et al. (2003) 16500 2400 9.326 0.033
2MASS Cutri et al. (2003) 21910 2500 9.207 0.018
Feige 87
Johnson Allard et al. (1994) 4450 940 11.598 0.050
Johnson Allard et al. (1994) 5500 880 11.693 0.050
Cousins Allard et al. (1994) 6470 1515 11.671 0.050
Cousins Allard et al. (1994) 7880 1490 11.623 0.050
Stromgren Bergeron et al. (1984) 3500 300 11.800 0.045
Stromgren Bergeron et al. (1984) 4110 190 11.747 0.045
Stromgren Bergeron et al. (1984) 4670 180 11.698 0.045
Stromgren Bergeron et al. (1984) 5470 230 11.730 0.090
2MASS Cutri et al. (2003) 12410 1500 11.484 0.022
2MASS Cutri et al. (2003) 16500 2400 11.359 0.026
2MASS Cutri et al. (2003) 21910 2500 11.312 0.022
Table 6: Photometry of BD+293070, BD+341543 and Feige 87 collected from the literature.

3.2 SED fitting

The SED fitting method is similar to the one described in Paper I. The observed photometry is fitted with a synthetic SED integrated from model atmospheres. For the MS component Kurucz atmosphere models (Kurucz 1979) ranging in effective temperature from 4000 to 9000 K, and in surface gravity from =3.0 dex (cgs) to 5.0 dex (cgs) are used. For the hot sdB component TMAP (Tübingen NLTE Model-Atmosphere Package, Werner et al. 2003) atmosphere models with a temperature range from 20000 K to 50000 K, and from 4.5 dex (cgs) to 6.5 dex (cgs) are used.

The SEDs are fitted in two steps. First the grid based approach described in Degroote et al. (2011) extended for binarity is used to scan the entire parameter space. For each point the is calculated as


where is the observed photometry and is the calculated model photometry. The grid point with the lowest is used as starting point for a least-squares minimizer which will then determine the final result. In a binary system, there are eight parameters to consider: the effective temperatures ( and ), surface gravities ( and ) and radii ( and ) of both components, the interstellar reddening and the distance () to the system. The interstellar reddening is presumed equal for both the MS and the sdB component. To increase the accuracy, the models are first corrected for interstellar reddening and then integrated over the photometric pass-bands using the reddening law of Fitzpatrick (2004) with = 3.1. The distance to the system is used as a scale factor and is calculated analytically, by shifting the synthetic models to the photometric observations.

As shown in Paper I, the mass ratio obtained from the radial velocity curves can be used to couple the radii of both components to their surface gravity, and thus reducing the number of free parameters from eight to six. The total flux of a binary system is then calculated using:


The uncertainties on the final parameters are determined by calculating two-dimensional confidence intervals (CI) for all parameter pairs. This is done by creating a 2D-grid for each parameter pair. For each point in this grid, the two parameters for which the CI is calculated are kept fixed on the grid-point value, while the least-squares minimizer is used to find the best-fitting values for all other parameters. The resulting for each point in this grid is stored. All these s are then rescaled so that the of the best fit has the expected value , with N the number of observations and N the number of free parameters in the fit. The cumulative density function (CDF) is used to calculate the probability of a model to obtain a certain value as:


Where P is the regularized -function. Based on the obtained probability distribution, the uncertainties on the parameters can be derived.

3.3 Results

Figure 3: The spectral energy distribution and (O-C) of BD+293070 (left), BD+341543 (center) and Feige 87 (right). The measurements are given in blue, the integrated synthetic models are shown in black, where a horizontal error bar indicates the width of the pass-band. The best fitting model is plotted in red. In the bottom panels the residuals are plotted for each system.
BD+293070 BD+341543 Feige 87
Parameter Best fit 95% Best fit 95% Best fit 95%
T (K) 6570 5800 – 7100 6210 6000 – 6440 5840 5300 – 6400
(dex) 4.40 4.00 – 4.80 4.19 4.05 – 4.35 4.40 4.15 – 4.60
T (K) 28500 24000 – 36000 36700 30000 – / 27400 21000 – 33000
(dex) 5.76 5.20 – 6.20 5.92 5.75 – 6.05 5.54 5.20 – 5.80
E() 0.007 0 – 0.052 0.007 0 – 0.068 0.012 0 – 0.057
555For some parameters the confidence intervals could not be calculated due to the limited range of the model atmospheres.
Table 7: The results of the SED fit for BD+293070, BD+341543 and Feige 87, together with the 95% probability intervals derived from the confidence intervals plotted in Fig. 4.
Figure 4: The confidence intervals of the SED fits of BD+293070, BD+341543 and Feige 87. The different colors show the cumulative density probability connected to the statistics given by equation 3. The best fitting values and there errors are plotted in black.

To fit the SEDs of the three systems, first a grid of composite binary spectra is calculated for  1 000 000 points randomly distributed over the , and E() intervals for both components. Then the 50 best-fitting grid points are used as starting values for the least-squares minimizer. For this best fit the CIs are estimated, and used to limit the original ranges on the parameters, after which the fitting process (grid search and least-squares minimizer) is repeated. To determine the CIs of the parameters, for each two parameters a grid with a resolution of 45 45 points was used, with the limits adjusted based on the resulting confidence intervals. When the model atmospheres allowed, the limits of the grid are set to include the 95 % CI, when this was not possible, the limits of the model atmosphere grid were used. The final uncertainties on the parameters are an average of the 95 % CIs for that parameter in all two-dimensional CIs that contain that parameter.

The photometry of BD+293070 has a rather large spread, which will result in large uncertainties on the derived parameters. The best fitting effective temperatures are = 6570 550 K and = 28500 5000 K, with surface gravities of = 4.4 0.5 dex and = 5.76 0.5 dex. The reddening is E() = 0.009 mag. This value is consistent with the maximum reddening E() = 0.052 derived from the dust maps of Schlegel et al. (1998). The of the best fit is 45.6 which is more than three times as high as the expected value (N - N = 12), indicating that the stated errors on the photometry are too small. When calculating the confidence intervals, a scaling factor of 3.8 is used when converting the values to probabilities. As can be seen on the plots of the CIs in Fig. 4, there is no strong constraint possible on the surface gravity of the components. Increasing the surface gravity of one component can be countered by increasing the of the other component as well, and thus effectively shrinking the radii of both components. For the sdB component there is a strong correlation between and visible. The effect on the atmosphere models of an increase in can be diminished by increasing , and thus decreasing the radius. However, it is possible to provide an upper limit on the effective temperature as the He ii lines are not visible in the HERMES spectra, indicating that the effective temperature is below 35000 K (Heber 2009).

For BD+341543 fourteen photometric measurements are available, with a smaller spread than for BD+293070. The effective temperatures of the components derived from the SED fit are = 6210 250 K and = 36700 5000 K, while a surface gravity of = 4.19 0.20 dex and = 5.92 0.40 dex are found. The reddening is determined to be E() = 0.007 which is consistent with the maximum reddening found on the dust maps of Schlegel et al. (1998), and supported by the absence of sharp interstellar absorption lines in the spectrum. As can be seen in Fig. 4 the probability distributions of the MS components parameters form a Gaussian-like pattern, and the and of the MS component have stronger constraints than for BD+293070, independently of the parameters for the sdB components. The uncertainty on the effective temperature and surface gravity of the sdB component is larger as both parameters are correlated in the same way as for BD+293070. However, the presence of clearly visible He i and He ii lines in the HERMES spectra of BD+341543 indicates that the effective temperature should be between 35000 and 50000 K.

In the case of BD+341543 the parallax was measured by Hipparcos (van Leeuwen 2007) to be 4.22 1.72 mas. This parallax could be used to fix the distance to the system in the SED fitting process. Since the parallax is of the same order as the projected size of the orbit for this system, one may presume that the Hipparcos parallax is unreliable, but as both components of BD+341543 have a very similar flux in the Hipparcos pass band, the center of light does not change during the orbit. However, the uncertainty on the parallax is large ( 40 %). Using this parallax to fix the distance to the system, without propagating the uncertainty on it, results in effective temperatures of = 6230 100 K and = 37900 3500 K, and surface gravities of = 4.04 0.05 dex and = 5.81 0.15 dex. The reddening is determined to be E() = 0.011. The uncertainties are much smaller as when the distance is included as a free parameter, especially on the surface gravity. However, due to the large uncertainty on the parallax, only the atmospheric parameters derived with the distance as a free parameter are used.

For Feige 87 there are only eleven photometric measurements found in the literature, but there is a very good agreement between all the measurements in the different bands. When checking the residuals of the fit, Feige 87 has the smallest spread of all three systems, with a total of 2.9. The SED results in an effective temperature of = 5840 500 K and = 27400 5000 K for the MS and sdB component, together with a surface gravity of = 4.40 0.30 dex and = 5.50 0.50 dex. The reddening of the system is found to be E() = 0.012, consistent with the results from the dust maps of Schlegel et al. (1998). On Fig. 4 the probability distributions show a similar pattern as for BD+293070. Although the distribution in and have a clearer Gaussian pattern, indicating that they are determined more accurate as for BD+293070.

The advantage of having an estimate of the distance to the target is clear when considering the uncertainties of the atmospheric parameters. Because the radii of the components are derived from their surface gravity, limiting the distance will also limit the radii. If the distance is accurately known, the accuracy of the surface gravity can be increased by a factor ten compared to when the distance is treated as a free parameter. Determining atmospheric parameters from photometry will greatly benefit from the Gaia mission that will derive accurate distances of about a billion stars.

4 Spectral analysis

The atmospheric parameters determined from the SEDs can be checked using the spectra. The HERMES echelle spectra are not easy to flux calibrate accurately, and therefore not well suited to fit model atmospheres, but it is possible to subtract the continuum contribution of the sdB component as explained in the following subsection. The resulting spectra of the MS components can be used to derive atmospheric parameters based on the Fe i and Fe ii lines. Apart from the HERMES spectra, we have obtained flux calibrated long-slit spectra with the Bok telescope (see Sect. 4.3). The resolution of these spectra is too low to determine radial velocities, but they can be used to fit model atmospheres and provide an independent set of atmospheric parameters.

4.1 Disentangling

When the spectroscopic parameters of both components in a system are known, it is possible to extract the spectrum of the MS component from the combined spectrum. This is done by subtracting a synthetic sdB spectrum with a surface gravity and effective temperature determined from the SED fit. As the sdB component only has a few lines and only wavelength regions that don’t contain balmer or He lines are used, this is equivalent to subtracting the continuum contribution of the sdB component.

Each HERMES spectrum is treated separately. First the HERMES response curve is removed from the spectrum after which its continuum is determined by fitting a low degree polynomial to the spectrum. Then the continuum contribution of the sdB component is subtracted following:


Where is the total flux in the HERMES spectrum, and are the normalized fluxes of the MS and sdB components, is the continuum of the HERMES spectrum, and is the ratio of the sdB flux to the MS flux. As only the regions where the sdB component does not have significant lines are used, = 1 for every . The normalized MS spectrum is then given by:


The obtained MS spectra are shifted to zero velocity, and averaged weighted by their S/N. An example region of the final extracted spectra for both systems is plotted in Fig. 5.

Figure 5: The disentangled HERMES spectra of the MS components obtained by subtracting the sdB continuum and averaging all spectra (black full line), together with Kurucz model atmospheres based on the atmospheric parameters determined from the iron lines (red dotted line). Top: BD+293070, center: BD+341543, bottom: Feige 87.

This way of disentangling the spectra is dependent on the atmospheric parameters of both components, which means that the disentangling process needs to be repeated when a new set of atmospheric parameters for the MS component is derived from the iron lines. This is done until convergence, which happened for all systems after two iterations. The parameters of the sdB component cannot be derived from the resulting spectra, but tests were performed to check their influence. As it turns out, changing the or of the sdB component within the errors determined in the SED fitting process, does not have a significant effect on the parameters of the MS component derived from the iron lines.

4.2 Atmospheric parameters and abundances

The Versatile Wavelength Analysis666 (VWA) tool developed by Bruntt et al. (2002) is used to determine the effective temperature, surface gravity, microturbulent velocity and abundances of the MS components. VWA generates synthetic spectra using the SYNTH software of Valenti & Piskunov (1996). Atomic line data is taken from the VALD database (Kupka et al. 1999), but the values are adjusted so that every line measured by Wallace et al. (1998) reproduces the atmospheric abundances by Grevesse et al. (2007). The atmosphere models are interpolated from MARCS model atmospheres (Gustafsson et al. 2008) using the solar composition of Grevesse et al. (2007). The VWA package fits abundances in a semi-automatic way. It first selects the least blended lines in the spectra, and determines the abundances of these lines by calculating synthetic spectra for each line while iteratively changing the input abundance until the equivalent widths of the observed and synthetic spectrum match. The main advantage of VWA is that the synthetic spectrum includes the contribution of neighboring lines, thus making it possible to analyze stars with a high rotational velocity. A detailed description of the VWA software can be found in Bruntt et al. (2004, 2008); Bruntt (2009); Bruntt et al. (2010a, b).

Before the spectra are analyzed, they are carefully normalized with the RAINBOW tool of the VWA package. Then the spectra are compared to synthetic spectra, and projected rotational velocities of 52 5 km s, 17 4 km s and 8 3 km s are found for the G-star components of respectively BD+293070, BD+341543 and Feige 87. Especially BD+293070 has a high rotational velocity, resulting in severe line blending, which makes it difficult to derive the atmospheric parameters. These parameters are determined using only the iron lines. The effective temperature is determined by requiring the abundance of the Fe i lines to be independent of the excitation potential. The surface gravity is derived by requiring the same abundance for Fe i and Fe ii lines, and checked by fitting synthetic spectra to several calcium and magnesium lines that are sensitive to changes in (Gray 2005). Furthermore the independence of abundance on equivalent width gives the microturbulence velocity. When the atmospheric parameters are determined the final abundances of all measured lines are calculated, and the overall metallicity is obtained by averaging all abundances over the measured elements weighted by the number of lines found for each element.

The disentangled spectrum of BD+293070 has the highest signal-to-noise ratio of the three systems (S/N 130), making it possible to derive robust parameters regardless of the high rotational blending. In total, 401 suitable lines were selected after comparing the data with a synthetic spectrum. In the abundance determination process 56 lines (of which 34 Fe i and 3 Fe ii lines) were used and had an equivalent width between 10 and 90 mÅ. The three Fe ii lines have too large scatter to constrain the surface gravity and are ignored for this purpose. To obtain an estimate of the surface gravity three calcium lines (Ca 6122, Ca 6162, Ca 6439) and the magnesium triplet (Mg-1b 5172) are fitted with synthetic spectra. This resulted in a surface gravity of = 4.3 0.5 dex. Using the surface gravity determined from the Ca and Mg lines, the atmospheric parameters determined based on the Fe i lines are: = 6100 200 K and = 1.50 0.35 km s. The overall metallicity calculated using all 56 lines is [M/H] = 0.09 0.21. The abundances of all lines are given in Table 8.

Having a lower rotational velocity and a still a high signal to noise (S/N 90), more useful lines (578) were found in BD+341543. After the fitting process 99 lines (including 50 Fe i and 6 Fe ii lines) were fitted and had an equivalent width between 10 and 90 mÅ. In this case the scatter on the abundances of the Fe ii lines was low, we used it together with the Fe i lines to constrain the surface gravity, resulting in = 4.2 0.3 dex. This value is supported by fitting synthetic spectra to the same Ca and Mg lines as for BD+293070. Based on the Fe i lines an effective temperature of = 6150 150 K and a microturbulence of = 1.45 0.25 km s were found. The averaged metallicity is found to be slightly sub solar at [M/H] = 0.24 0.12. The abundances of all elements are shown in Table 8.

Feige 87 has the lowest rotational velocity, but this advantage is partly countered by the low signal-to-noise ratio of the disentangled spectrum (S/N 35). From the 428 selected lines 93 were used (including 51 Fe i lines and 3 Fe ii lines). The scatter of the Fe ii lines is high compared to the previous system, thus they are not very reliable in constraining the surface gravity. Based on fitting synthetic spectra to Ca and Mg lines, and on the ionization balance between Fe i and Fe ii, we find a surface gravity of = 4.5 0.6 dex. Based on the Fe i lines, the effective temperature is constrained to = 6175 150 K and the microturbulence results in = 1.15 0.25 km s. The average metallicity based on 96 lines in total is clearly sub solar at [M/H] = 0.48 0.26. The abundances of all elements are shown in Table 8.

BD+293070 BD+341543 Feige 87
Ion [El/H] NNumber of lines used per ion, the stated error is the rms error computed if two or more lines are available. [El/H] NNumber of lines used per ion, the stated error is the rms error computed if two or more lines are available. [El/H] NNumber of lines used per ion, the stated error is the rms error computed if two or more lines are available.
Al i 0.26 0.1 2
Si i 0.24 0.19 8 0.12 0.08 11 0.38 0.13 9
Si ii 0.25 1 0.21 0.06 2
Ca i 0.03 1 0.14 0.04 7 0.27 0.06 7
Sc ii 0.09 1 0.70 0.13 3
Ti i 0.05 0.06 3 0.09 0.25 2
Ti ii 0.07 0.12 2 0.77 1
Cr i 0.27 0.13 4 0.04 2
Cr ii 0.08 1 0.25 1
Mn i 0.07 1 0.82 1
Mg i 0.12 1
Fe i 0.04 0.16 34 0.26 0.07 50 0.49 0.17 51
Fe ii 0.1 0.18 3 0.26 0.12 6 0.60 0.4 3
Ni i 0.08 0.16 6 0.34 0.10 11 0.40 0.25 12
Na i 0.44 1
Table 8: The abundances ([El/H]) for the MS components of BD+293070, BD+341543 and Feige 87 obtained from the disentangled HERMES spectra.

4.3 Spectral fitting

F and G type MS companions of sdB stars can be easily resolved in the optical as they have similar brightnesses and distinct spectra. This allows one to disentangle such composite spectra from a single observation without knowing the radii or fluxes of the components. Such a binary decomposition was implemented in the XTgrid (Németh et al. 2012) spectral fitting algorithm and was used to estimate the atmospheric parameters of the components in 29 composite spectra binaries. XTgrid employs the NLTE model atmosphere code TLUSTY (Hubeny & Lanz 1995) for the subdwarf component and interpolated MILES (Cenarro et al. 2007) template spectra for the MS companion. The binary spectrum is fitted with a linear combination of the two components. This method is independent from the SED and VWA analysis and was applied for low-resolution flux calibrated spectra obtained with the B&C spectrograph, therefore it can be used to check the consistency of the different approaches.

Without preliminary assumptions on the spectral types XTgrid confirmed the results of the SED and VWA analysis on BD293070 and BD341543 within error bars, but predicted a lower surface gravity of the components in Feige 87. Then, with the help of the radial velocity measurements, we could constrain the surface gravities of the companions which helped achieving a better consistency of the decomposition in all three cases. Our results are listed in Table 9 and the disentangled binary spectra are plotted in Fig. 6. We note that the lower contribution of the MS star in Feige 87 raises the uncertainties of our parameter determination.

Parameter BD+293070 BD+341543 Feige 87
E() (mag) 0.013 0.002 0.000
Flux ratioFlux ratio F / F in wavelength range 6720 - 6800 Å 1.353 1.337 2.252
MS component
T (K) 6026 300 5715 300 5675 250
(dex) 4.26 0.30 4.11 0.30 4.23 0.35
Fe/H 0.08 0.25 -0.37 0.25 -0.39 0.25
sdB component
T (K) 25380 990 36640 810 27270 500
(dex) 5.54 0.18 6.13 0.16 5.47 0.15
HeAbundance given as -2.63 -1.49 0.13 -2.56
CAbundance given as -3.27 -4.64 -3.77
NAbundance given as -2.79 -3.28 -3.69
OAbundance given as -1.93 -3.72 -2.89
Table 9: The atmospheric parameters obtained from the flux calibrated spectra of BD+293070, BD+341543 and Feige 87.
Figure 6: The flux calibrated B&C spectra observed with the Bok telescope (black line) of BD+293070, BD+341543 and Feige 87 together with the best fitting binary atmosphere models from the XTgrid code (red line). The decomposition of the model in the MS and sdB component is plotted in respectively blue and green.

5 Gravitational redshift

If the difference between the surface gravity of both components in a binary system is substantial, this can give rise to a frequency shift in the emitted radiation. This effect is caused by a difference in gravitational redshift for the two stars. From general relativity one can derive that the gravitational redshift as function of the mass and surface gravity of the star (Einstein 1916):


Where is the gravitational redshift, the speed of light, the gravitational constant, the mass, and the surface gravity. This will effectively change the apparent systemic velocity for the star. In a binary system the difference in surface gravity for both components will be visible as a difference in systemic velocity between the components. As is proportional to the square root of the surface gravity, this effect is only substantial when there is a large difference in between the components, as is the case for compact subdwarfs and main-sequence stars.

The difference in systemic velocity between the MS and sdB component measured in the radial velocity curves can be used to estimate the surface gravity of the sdB component (see also Paper I). Using a canonical value of 0.47 for the sdB component and the mass ratio, the mass of the MS component can be calculated. Together with the surface gravity of the MS component derived from the SED fit and spectral analysis, the of the MS component can be calculated. The of the sdB component can then be derived by combining with the measured difference in systemic velocity, and can be converted to an estimated surface gravity for the sdB component. A caveat here is that the wavelength of the He I 5875 multiplet is only known with a presision of 0.01 Å, corresponding to a systematic radial velocity uncertainty of up to 0.5 . The measured shift in systemic velocity could be partly due to this uncertainty, but since the observations are consistent with the predicted gravitational redshift we believe this to be the main contributor.

For BD+293070, the system velocity of the sdB component is weakly constrained and does not yield a very constrained surface gravity for the sdB component. However, the system velocities of the other two systems are better constrained. The measured differences in system velocity for the three systems are:


Using the averaged values for the surface gravity of the MS components as given in Table 10, the estimated surface gravities of the sdB components of these systems are:

The asymmetrical error on the surface gravity is calculated using a Monte Carlo simulation taking into account the error on the difference in system velocity and the errors on the parameters of the MS component. The resulting surface gravities correspond with the results from the other methods presented in this paper.

6 Absolute parameters

BD+293070 BD+341543 Feige 87
Parameter MS sdB MS sdB MS sdB
(d) 1283 63 972 2 936 2
2453877 41 2451519 11 2453259 21
0.15 0.01 0.16 0.01 0.11 0.01
1.60 0.22 1.58 0.07 2.92 0.15
(km s) 57.58 0.36 32.10 0.06 32.98 0.08
0.39 0.01 0.57 0.01 0.55 0.01
() 586 12 447 4 442 3
81 5 43 1 75 2
0.010 0.030 0.005 0.030 0.006 0.030
(pc) 238 25 207 30 383 40
Fe/H 0.05 0.16 0.26 0.08 -0.50 0.18
(km s 6.53 0.30 16.6 0.6 5.91 0.07 10.31 0.15 8.19 0.11 15.01 0.21
( 1.19 0.09 0.47 0.05 0.82 0.07 0.47 0.05 0.86 0.07 0.47 0.05
(cgs) 4.32 0.50 5.56 0.44 4.18 0.40 5.84 0.35 4.36 0.42 5.54 0.34
( 1.25 0.97 0.19 0.10 1.21 0.48 0.14 0.06 1.02 0.50 0.19 0.07
(K) 6180 420 25900 3000 6100 300 36600 3000 5980 325 27300 2700
() 2.06 0.25 14.3 3.0 1.83 0.25 30.13 4.0 1.19 0.20 18.04 3.0
(mag) 10.91 0.10 11.47 0.15 10.72 0.10 11.11 0.15 12.54 0.10 12.36 0.15
(mag) 4.02 0.10 4.58 0.15 4.14 0.10 4.54 0.15 4.62 0.10 4.44 0.15
999The sdB mass is the canonical value.
Table 10: Fundamental properties for both the main-sequence (MS) and subdwarf (sdB) component of BD+293070, BD+341543 and Feige 87.

Combining the results of the SED fit, the spectral analysis, gravitational redshift and the orbital parameters derived from the radial velocity curves, the absolute dimensions of BD+293070, BD+341543 and Feige 87 can be determined. With the assumed canonical sdB mass of = 0.47 , the inclination of the systems can be derived from the reduced mass determined in Sect. 2.2. This inclination can be used to calculate the semi-major axis of the systems. The atmospheric parameters (, ) determined with the four different methods (SED fitting, derived from the iron lines, spectral fitting and from the gravitational-redshift) correspond well within their errors. The final values for these parameters are the averages of the three methods weighted by their errors. The radii of the components is calculated from the mass and surface gravity. The system velocity is set to the system velocity of the MS component as the sdB component is subjected to significant gravitational redshift as discussed in Section 5.

The luminosity of both components can be calculated using . The apparent V magnitudes are obtained directly from the SED fitting procedure, while the absolute magnitude can be obtained by integrating the best fit model SEDs over the Johnson V band, and scaling the resulting flux to a distance of 10 pc. The distance to the system is then calculated from . For BD+341543 the distance obtained in this way corresponds within errors with the distance obtained from the Hipparcos parallax 236 80 pc. The absolute dimensions of all three systems are summarized in Table 10.

The proper motions of BD+293070, BD+341543 and Feige 87 as measured by van Leeuwen (2007) are:


Using the method of Johnson & Soderblom (1987), these numbers together with the measured value of , can be used to compute the galactic space velocity vector with respect to the local standard of rest from Dehnen & Binney (1998). Resulting in


for respectively BD+293070, BD+341543 and Feige 87. U is defined as positive towards the galactic center. Following the selection criteria of Reddy et al. (2006), all systems are bound to the galaxy, and belong to the thin or thick disk population.

7 Eccentric orbits

The three systems presented here are part of a sample consisting of six sdB + MS binaries, of which four systems have been analysed up till now. The first system PG 1104243 was described in Paper I, and is the only one from our sample with a circular orbit ( = 753 d, 0.002). The two remaining systems (Balloon 82800003 and BD75977) have longer periods that have not yet been covered completely at all phases, but preliminary results were presented in Vos et al. (2013) demonstrating that both systems are significantly eccentric. Furthermore (Barlow et al. 2013) analysed PG 1449653 ( = 909 d, = 0.11) and PG 1701+359 ( = 734 d, circular), and (Deca et al. 2012) published results of PG 1018243 which has a possible eccentric orbit ( = 759 d, 0.2). At the time of this publication, there are nine long period sdB + MS systems know of which six have a significant eccentric orbit, one might have an eccentric orbit and two have a circular orbit.

Current theory predicts only circular orbits for these long period sdB binaries formed through the stable RLOF channel. During the red giant phase of the sdB progenitor the tidal forces between the sdB progenitor and its companion should circularize the orbit very efficiently (Zahn 1977), and the further evolution provides very few possibilities to re-introduce eccentricity to the orbit. Deca et al. (2012) proposed the hierarchial triple merger scenario of Clausen & Wade (2011) for the possibly eccentric sdB + K system PG 1018-047, where the K-type companion would not have been involved in the evolution of the sdB component. However, such a scenario seems too unlikely to be observed frequently.

Another possible explanation for these eccentric systems would be that tidal circularization during the RGB and the RLOF phase is not as efficient as currently assumed. In highly eccentric systems the mass transfer through RLOF and mass loss due to stellar winds will not be constant over the orbit. Bonačić Marinović et al. (2008) studied this effect in binary systems with an AGB star, and found that enhanced mass loss from the AGB star at orbital phases closer to periastron can work efficiently against the tidal circularization of the orbit. Further theoretical studies could investigate if this eccentricity enhancement mechanism can work in in the progenitors of sdB + MS binaries as well.

A last interesting observation of this small sample is that the two circular systems and PG 1018243 with a possible circular orbit, have the shortest orbital periods. Although the sample is too small to state strong conclusions, this might support the above claim that the circularization process is not as efficient as expected and doesn’t fully circularize the longer period systems.

8 Conclusions

Using both literature photometry and observed spectra, detailed astrophysical parameters of BD+293070, BD+341543 and Feige 87 have been established. The long time-base spectroscopic observations made it possible to determine accurate periods, and to solve the orbit of both the MS and sdB component in all three systems. The atmospheric parameters were determined with three different techniques: based on the spectral energy distribution, using iron lines in the disentangled MS spectra, and from low-resolution flux calibrated spectra. Furthermore, the measured gravitational-redshift could be used to derive the surface gravity of the sdB components. The results obtained with these different methods agree within their errors.

The sdB components of all three systems are consistent with a canonical post-core-helium-flash model with a mass around 0.47 . However, the orbits of these systems are clearly eccentric, as opposed to what the current theory predicts. The periods found here correspond with the updated version of the BPS studies of Chen et al. (2013), although a significant degree of atmospheric RLOF must be included in order to reach the 1300 d period of BD+293070. Furthermore, Chen et al. (2013) finds a metallicity – orbital period relation, where the orbital period will decrease with decreasing metallicity. The observed periods of BD+293070, BD+341543 and Feige 87 (1283 d, 972 d, 936 d) for metallicities (solar, about half solar, about 1/3 solar) follow the metallicity relation, but significantly exceed the predictions of Chen et al. (2013). The same conclusion can be reached for PG 1104243 (P = 753 d, 1/3 solar, Paper I). We assume that the metallicity measured for the companion is comparable to the initial Z for the system, which ignores any contamination during RLOF, and can therefore be considered as an upper limit to the initial Z. All four systems call for the inclusion of atmospheric RLOF, also at lower metallicities. While the sample is too limited yet to make conclusions with respect to the period distribution, the long periods found in this paper indicates that an additional mechanism such as atmospheric RLOF is required for all the systems, not just those with periods 1100 d, as suggested by Chen et al. (2013).

BD+293070, BD+341543 and Feige 87 are part of an ongoing long-term observing program of sdB + MS binaries with HERMES at Mercator. Currently most of the systems accessible with the 1.2m Mercator + HERMES telescope-spectrograph combination have been analysed, but orbital solutions of more systems are needed in order to test the predicted orbital distributions. Our results call for the study of eccentricity pumping mechanisms (e.g. Bonačić Marinović et al. 2008) also in the framework of sdB binaries.

Based on observations made with the Mercator Telescope, operated on the island of La Palma by the Flemish Community, at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias. Based on observations obtained with the HERMES spectrograph, which is supported by the Fund for Scientific Research of Flanders (FWO), Belgium , the Research Council of K.U.Leuven, Belgium, the Fonds National Recherches Scientific (FNRS), Belgium, the Royal Observatory of Belgium, the Observatoire de Genève, Switzerland and the Thüringer Landessternwarte Tautenburg, Germany. The research leading to these results has received funding from the European Research Council under the European Community’s Seventh Framework Programme (FP7/2007–2013)/ERC grant agreement N 227224 (prosperity), as well as from the Research Council of K.U.Leuven grant agreements GOA/2008/04 and GOA/2013/012, the German Aerospace Center (DLR) under grant agreement 05OR0806 and the Deutsche Forschungsgemeinschaft under grant agreement WE1312/41-1. The following Internet-based resources were used in research for this paper: the NASA Astrophysics Data System; the SIMBAD database and the VizieR service operated by CDS, Strasbourg, France; the arive scientific paper preprint service operated by Cornell University. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.


  • Allard et al. (1994) Allard, F., Wesemael, F., Fontaine, G., Bergeron, P., & Lamontagne, R. 1994, AJ, 107, 1565
  • Barlow et al. (2013) Barlow, B. N., Liss, S. E., Wade, R. A., & Green, E. M. 2013, ApJ, 771, 23
  • Barlow et al. (2012) Barlow, B. N., Wade, R. A., Liss, S. E., Østensen, R. H., & Van Winckel, H. 2012, ApJ, 758, 58
  • Bergeron et al. (1984) Bergeron, P., Fontaine, G., Lacombe, P., et al. 1984, AJ, 89, 374
  • Bonačić Marinović et al. (2008) Bonačić Marinović, A. A., Glebbeek, E., & Pols, O. R. 2008, A&A, 480, 797
  • Brassard et al. (2001) Brassard, P., Fontaine, G., Billères, M., et al. 2001, ApJ, 563, 1013
  • Brown et al. (1997) Brown, T. M., Ferguson, H. C., Davidsen, A. F., & Dorman, B. 1997, ApJ, 482, 685
  • Bruntt (2009) Bruntt, H. 2009, A&A, 506, 235
  • Bruntt et al. (2010a) Bruntt, H., Bedding, T. R., Quirion, P.-O., et al. 2010a, MNRAS, 405, 1907
  • Bruntt et al. (2004) Bruntt, H., Bikmaev, I. F., Catala, C., et al. 2004, A&A, 425, 683
  • Bruntt et al. (2002) Bruntt, H., Catala, C., Garrido, R., et al. 2002, A&A, 389, 345
  • Bruntt et al. (2008) Bruntt, H., De Cat, P., & Aerts, C. 2008, A&A, 478, 487
  • Bruntt et al. (2010b) Bruntt, H., Deleuil, M., Fridlund, M., et al. 2010b, A&A, 519, A51
  • Cenarro et al. (2007) Cenarro, A. J., Peletier, R. F., Sánchez-Blázquez, P., et al. 2007, MNRAS, 374, 664
  • Chen et al. (2013) Chen, X., Han, Z., Deca, J., & Podsiadlowski, P. 2013, MNRAS, 434, 186
  • Clausen & Wade (2011) Clausen, D. & Wade, R. A. 2011, ApJ, 733, L42
  • Copperwheat et al. (2011) Copperwheat, C. M., Morales-Rueda, L., Marsh, T. R., Maxted, P. F. L., & Heber, U. 2011, MNRAS, 415, 1381
  • Cutri et al. (2003) Cutri, R. M., Skrutskie, M. F., van Dyk, S., et al. 2003, VizieR Online Data Catalog, 2246, 0
  • D’Cruz et al. (1996) D’Cruz, N. L., Dorman, B., Rood, R. T., & O’Connell, R. W. 1996, ApJ, 466, 359
  • Deca et al. (2012) Deca, J., Marsh, T. R., Østensen, R. H., et al. 2012, MNRAS, 421, 2798
  • Degroote et al. (2011) Degroote, P., Acke, B., Samadi, R., et al. 2011, A&A, 536, A82
  • Dehnen & Binney (1998) Dehnen, W. & Binney, J. J. 1998, MNRAS, 298, 387
  • Einstein (1916) Einstein, A. 1916, Relativity: the special and general theory (Methuen & Co Publishing Ltd)
  • Fitzpatrick (2004) Fitzpatrick, E. L. 2004, in ASPCS, Vol. 309, Astrophysics of Dust, ed. A. N. Witt, G. C. Clayton, & B. T. Draine, 33
  • Geier (2013) Geier, S. 2013, in European Physical Journal Web of Conferences, Vol. 43, European Physical Journal Web of Conferences, 4001
  • Geier et al. (2011) Geier, S., Hirsch, H., Tillich, A., et al. 2011, A&A, 530, A28
  • Gray (2005) Gray, D. F. 2005, The Observation and Analysis of Stellar Photospheres
  • Green et al. (2001) Green, E. M., Liebert, J., & Saffer, R. A. 2001, in ASPCS, Vol. 226, 12th European Workshop on White Dwarfs, ed. J. L. Provencal, H. L. Shipman, J. MacDonald, & S. Goodchild , 192
  • Green et al. (1986) Green, R. F., Schmidt, M., & Liebert, J. 1986, ApJS, 61, 305
  • Greggio & Renzini (1990) Greggio, L. & Renzini, A. 1990, ApJ, 364, 35
  • Grevesse et al. (2007) Grevesse, N., Asplund, M., & Sauval, A. J. 2007, Space Sci. Rev., 130, 105
  • Gustafsson et al. (2008) Gustafsson, B., Edvardsson, B., Eriksson, K., et al. 2008, A&A, 486, 951
  • Han et al. (2003) Han, Z., Podsiadlowski, P., Maxted, P. F. L., & Marsh, T. R. 2003, MNRAS, 341, 669
  • Han et al. (2002) Han, Z., Podsiadlowski, P., Maxted, P. F. L., Marsh, T. R., & Ivanova, N. 2002, MNRAS, 336, 449
  • Han et al. (2000) Han, Z., Tout, C. A., & Eggleton, P. P. 2000, MNRAS, 319, 215
  • Heber (1998) Heber, U. 1998, in ESA Special Publication, Vol. 413, Ultraviolet Astrophysics Beyond the IUE Final Archive, ed. W. Wamsteker, R. Gonzalez Riestra, & B. Harris, 195
  • Heber (2009) Heber, U. 2009, ARA&A, 47, 211
  • Heber et al. (2002) Heber, U., Moehler, S., Napiwotzki, R., Thejll, P., & Green, E. M. 2002, A&A, 383, 938
  • Heber et al. (2000) Heber, U., Reid, I. N., & Werner, K. 2000, A&A, 363, 198
  • Hubeny & Lanz (1995) Hubeny, I. & Lanz, T. 1995, ApJ, 439, 875
  • Johnson & Soderblom (1987) Johnson, D. R. H. & Soderblom, D. R. 1987, AJ, 93, 864
  • Kharchenko (2001) Kharchenko, N. V. 2001, Kinematika i Fizika Nebesnykh Tel, 17, 409
  • Koen et al. (1998) Koen, C., Orosz, J. A., & Wade, R. A. 1998, MNRAS, 300, 695
  • Kupka et al. (1999) Kupka, F., Piskunov, N., Ryabchikova, T. A., Stempels, H. C., & Weiss, W. W. 1999, A&AS, 138, 119
  • Kurucz (1979) Kurucz, R. L. 1979, ApJS, 40, 1
  • Lucy & Sweeney (1971) Lucy, L. B. & Sweeney, M. A. 1971, AJ, 76, 544
  • Maxted et al. (2001) Maxted, P. f. L., Heber, U., Marsh, T. R., & North, R. C. 2001, MNRAS, 326, 1391
  • Maxted et al. (2000) Maxted, P. F. L., Moran, C. K. J., Marsh, T. R., & Gatti, A. A. 2000, MNRAS, 311, 877
  • Mengel et al. (1976) Mengel, J. G., Norris, J., & Gross, P. G. 1976, ApJ, 204, 488
  • Mermilliod et al. (1997) Mermilliod, J.-C., Mermilliod, M., & Hauck, B. 1997, A&AS, 124, 349
  • Morales-Rueda et al. (2003) Morales-Rueda, L., Maxted, P. F. L., Marsh, T. R., North, R. C., & Heber, U. 2003, MNRAS, 338, 752
  • Napiwotzki et al. (2004) Napiwotzki, R., Karl, C. A., Lisker, T., et al. 2004, Ap&SS, 291, 321
  • Nelemans (2010) Nelemans, G. 2010, Ap&SS, 329, 25
  • Nelemans et al. (2000) Nelemans, G., Verbunt, F., Yungelson, L. R., & Portegies Zwart, S. F. 2000, A&A, 360, 1011
  • Nelemans et al. (2001) Nelemans, G., Yungelson, L. R., Portegies Zwart, S. F., & Verbunt, F. 2001, A&A, 365, 491
  • Németh et al. (2012) Németh, P., Kawka, A., & Vennes, S. 2012, MNRAS, 427, 2180
  • Østensen (2006) Østensen, R. H. 2006, Baltic Astronomy, 15, 85
  • Østensen & Van Winckel (2011) Østensen, R. H. & Van Winckel, H. 2011, in ASPCS, Vol. 447, Evolution of Compact Binaries, ed. L. Schmidtobreick, M. R. Schreiber, & C. Tappert, 171
  • Østensen & Van Winckel (2012) Østensen, R. H. & Van Winckel, H. 2012, in ASPCS, Vol. 452, Fifth Meeting on Hot Subdwarf Stars and Related Objects, ed. D. Kilkenny, C. S. Jeffery, & C. Koen, 163
  • Paczynski (1976) Paczynski, B. 1976, in IAU Symposium, Vol. 73, Structure and Evolution of Close Binary Systems, ed. P. Eggleton, S. Mitton, & J. Whelan, 75
  • Pfeiffer et al. (1998) Pfeiffer, M. J., Frank, C., Baumueller, D., Fuhrmann, K., & Gehren, T. 1998, A&AS, 130, 381
  • Raskin et al. (2011) Raskin, G., van Winckel, H., Hensberge, H., et al. 2011, A&A, 526, A69
  • Reddy et al. (2006) Reddy, B. E., Lambert, D. L., & Allende Prieto, C. 2006, MNRAS, 367, 1329
  • Richmond (2007) Richmond, M. W. 2007, PASP, 119, 1083
  • Saffer et al. (1994) Saffer, R. A., Bergeron, P., Koester, D., & Liebert, J. 1994, ApJ, 432, 351
  • Schlegel et al. (1998) Schlegel, D. J., Finkbeiner, D. P., & Davis, M. 1998, ApJ, 500, 525
  • Sweigart (1997) Sweigart, A. V. 1997, ApJ, 474, L23
  • Valenti & Piskunov (1996) Valenti, J. A. & Piskunov, N. 1996, A&AS, 118, 595
  • van Leeuwen (2007) van Leeuwen, F. 2007, A&A, 474, 653
  • Vos et al. (2012) Vos, J., Østensen, R. H., Degroote, P., et al. 2012, A&A, 548, A6
  • Vos et al. (2013) Vos, J., Østensen, R. H., & Van Winckel, H. 2013, in 6th Meeting on Hot Subdwarf Stars and Related Objects, ed. E. Green & G. Fontaine, PASPC, in press
  • Wallace et al. (1998) Wallace, L., Hinkle, K., & Livingston, W. 1998, An atlas of the spectrum of the solar photosphere from 13,500 to 28,000 cm (3570 to 7405 Å), ed. Wallace, L., Hinkle, K., & Livingston, W.
  • Webbink (1984) Webbink, R. F. 1984, ApJ, 277, 355
  • Werner et al. (2003) Werner, K., Deetjen, J. L., Dreizler, S., et al. 2003, in ASPCS, Vol. 288, Stellar Atmosphere Modeling, ed. I. Hubeny, D. Mihalas, & K. Werner, 31
  • Zahn (1977) Zahn, J.-P. 1977, A&A, 57, 383
Comments 0
Request Comment
You are adding the first comment!
How to quickly get a good reply:
  • Give credit where it’s due by listing out the positive aspects of a paper before getting into which changes should be made.
  • Be specific in your critique, and provide supporting evidence with appropriate references to substantiate general statements.
  • Your comment should inspire ideas to flow and help the author improves the paper.

The better we are at sharing our knowledge with each other, the faster we move forward.
The feedback must be of minimum 40 characters and the title a minimum of 5 characters
Add comment
Loading ...
This is a comment super asjknd jkasnjk adsnkj
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters

You are asking your first question!
How to quickly get a good answer:
  • Keep your question short and to the point
  • Check for grammar or spelling errors.
  • Phrase it like a question
Test description