EDP Sciences logo
Subscriber Authentication Point
Search
Menu
Home All issues Volume 561 (January 2014) A&A, 561 (2014) L3 Full HTML
Free Access
Issue
A&A
Volume 561, January 2014
Article Number L3
Number of page(s) 5
Section Letters
DOI https://doi.org/10.1051/0004-6361/201322883
Published online 23 December 2013

© ESO, 2013

1. Introduction

Cepheids are powerful astrophysical laboratories that provide fundamental clues for studying the pulsation and evolution of intermediate-mass stars. However, the discrepancy between masses predicted by stellar evolutionary and pulsation models is still not understood well. The most cited scenarios to explain this discrepancy are a mass-loss process during the Cepheid’s evolution and/or convective a core overshooting during the main-sequence stage (Neilson et al. 2011; Keller 2008; Bono et al. 2006). Therefore, accurate masses of a few percent are needed to help constrain the two models.

So far, the mass of only one Cepheid, Polaris, has been measured (Evans et al. 2008); otherwise, they are derived through the mass of the companion inferred from a mass-temperature relation. When in binary systems, Cepheids offer the unique opportunity to make progress in resolving the Cepheid mass problem. The dynamical masses can be estimated (Pietrzyński et al. 2011, 2010; Evans et al. 2008), and provide new constraints on evolution and pulsation theory (e.g. Prada Moroni et al. 2012). This gives new insight on the Cepheid mass, and can settle the discrepancy between pulsation and evolution models. Binary systems are also valuable tools to obtain independent distance measurements of Cepheids, needed to calibrate the Leavitt Law.

Table 1

Parameters of the Cepheid and its close companion.

However, most of the companions are hot main-sequence stars, and are located too close to the Cepheid (~1−40 mas) to be observed with a 10-m class telescope at optical wavelengths. The already existing orbit measurements were estimated only from IUE spectrum or from the radial velocity variations. The only way to spatially resolve such systems is to use long-baseline interferometry or aperture masking. We started a long-term interferometric observing program that aims at studying a sample of northern and southern binary Cepheids. The first goal is to determine the angular separation and the apparent brightness ratio from the interferometric visibility and closure phase measurements. Our long-term objective is to determine the full set of orbital elements, absolute masses and geometric distances. Our program started in 2012 and has already provided new informations on the V1334 Cyg Cepheid system (Gallenne et al. 2013, hereafter Paper I).

In this second paper, we report the detection of the orbiting companion around the Cepheid AX Cir (HD 130701, HR 5527). This pulsating star has a spectroscopic companion, first suspected from composite spectra by Jaschek & Jaschek (1960), and later confirmed by Lloyd Evans (1982). A preliminary orbital period of about 4600 days was then estimated by Szabados (1989). Bohm-Vitense & Proffitt (1985) and Evans (1994) also detected the companion from International Ultraviolet Exporer (IUE) low-resolution spectra, and set its spectral type to be a B6V star. The first orbital solution was provided by Petterson et al. (2004) from precise and homogeneous high-resolution spectroscopic measurements; however, it does not include the semi-major axis, the inclination angle, and the longitude of the ascending node, which can only be provided from astrometry. We list some parameters of the AX Cir system in Table 1.

We present here the first spatially resolved detection of this companion from VLTI/PIONIER observations. We first describe in Sect. 2 the beam combiner, the observations, and the raw data calibration. In Sect. 3 we explain the data analysis and present our results. We then discuss our measured flux ratio and projected separation, and conclude in Sect. 5.

2. Observations and data reduction

We used the Very Large Telescope Interferometer (VLTI; Haguenauer et al. 2010) with the four-telescope combiner PIONIER (Le Bouquin et al. 2011) to measure squared visibilities and closure phases of the AX Cir binary system. PIONIER combines the light coming from four telescopes in the H band, either in a broad band mode or with a low spectral resolution, where the light is dispersed into three or seven spectral channels. The recombination provides simultaneously six visibilities and four closure phase signals per spectral channel.

Our observations were carried out on UT 2013 July 11 and 14, with dispersed fringes in three spectral channels. All observations made use of the 1.8 m Auxiliary Telescopes with the configuration K0-A1-G1-J3 and D0-G1-H0-I1, providing six projected baselines ranging from 40 to 140 m. To monitor the instrumental and atmospheric contributions, the standard procedure, which consists of interleaving the science target by reference stars, was used. The calibrators, HD 133869 and HD 129462, were selected using the SearchCal1 software (Bonneau et al. 2006, 2011) provided by the JMMC. The journal of the observations is presented in Table 2 and the (u,v) plane covered by the observations is shown in Fig. 1. We have collected a total of 435 squared visibility and 300 closure phase measurements.

The data have been reduced with the pndrs package described in Le Bouquin et al. (2011). The main procedure is to compute squared visibilities and triple products for each baseline and spectral channel, and to correct for photon and readout noises. The final calibrated closure phases of July 14 are presented in Fig. 3. The variations in the signal suggest the presence of the companion, and this is strengthened by a higher signal-to-noise ratio when combining all the data.

thumbnail Fig. 1

(u,v) plane coverage for all our observations of AX Cir.

3. Model fitting

The squared visibilities and closure phase signals were modeled assuming a uniform disk (UD) angular diameter for the Cepheid (the primary) plus a point source companion. The fitted parameters are the angular diameter of the Cepheid θUD, the relative position of the component (Δα, Δδ), and the flux ratio f = fcom/fcep. The coherence loss effect due to spectral smearing on the companion was also modeled using the function | sincx |, where x = π(uΔα + vΔδ)/(λR) at spectral resolution R = 18 and spatial frequencies (u,v).

The choice of a UD diameter for the Cepheid instead of a limb-darkened (LD) disk for the fitting procedure is justified because the angular diameter is small compared to the angular resolution of the interferometer, and the limb darkening effects are therefore undetectable. The conversion from UD to LD angular diameter was done afterwards by using a linear-law parametrization Iλ(μ) = 1 − uλ(1 − μ), with the LD coefficient uλ = 0.2887 (Claret & Bloemen 2011) for both epochs, and using the stellar parameters Teff = 5400 K, log   g = 2.0, [Fe/H] = 0.0, and vt = 5 km s-1 (Usenko et al. 2011; Acharova et al. 2012). The conversion is then given by the approximate formula of Hanbury Brown et al. (1974): θLD(λ)=θUD(λ)1−uλ/31−7uλ/15·\begin{eqnarray*} \theta_\mathrm{LD}(\lambda) = \theta_\mathrm{UD}(\lambda) \sqrt{\frac{1-u_\lambda/3}{1-7u_\lambda/15}}\cdot \end{eqnarray*}Changing Teff by ± 400 k changes the diameter by less than 0.2%, well below our measured uncertainties.

thumbnail Fig. 2

Probability map for the companion position of July 14.

thumbnail Fig. 3

Closure phase signal of AX Cir for July 14, with respect to the modified Julian date. The spectral channels were averaged for clarity. The solid black line represents our best fit model.

thumbnail Fig. 4

Squared visibility measurements of AX Cir. The data are in blue for July 14 and in green for July 11, while the red dots are the fitted binary model for both epochs.

For each epoch, the fitting procedure was done in two steps. We first proceeded to a 80    ×    80 mas grid search in the χ2 space, with spacing of 0.2 mas, which aims at determining the approximate position of the companion and avoid local minima. Then a finer search of 5    ×    5 mas with a 0.05 mas spacing around the most likely position was carried out to obtain the final parameters. We chose θUD = 0.76 mas (Gallenne et al. 2011) and f = 1.5% (Evans 1994) as first guesses.

Our model did not take a possible circumstellar envelope (CSE) emission into account, which could lead to an overestimate of the angular diameter. From the spectral energy distribution AX Cir given by Gallenne et al. (2011), the infrared excess caused by the CSE appears around 10   μm, while it is negligible at 1.6   μm (i.e., <2%, which would lead to visibility loss of the same amount at first order, and below our visibility accuracy).

The probability map for the observations of July 14 is shown in Fig. 2, and the fitted parameters for both epochs are reported in Table 3. The companion is clearly detected at the two epochs at coordinates ρ = 29.2 ± 0.2 mas and PA = 167.6    ±    0.3°. The model for the observations of July 14 is represented graphically in Fig. 3. We estimated limb-darkened angular diameters θLD = 0.742    ±    0.020 mas and 0.839    ±    0.023 mas, for July 11 and 14, respectively (at pulsation phases φ = 0..48 and 0.24, respectively), in agreement with the angular diameter, 0.76    ±    0.03 estimated by Gallenne et al. (2011) at phase φ = 0.27. It is also consistent with the average value of 0.84 mas estimated from the surface brightness relation of Kervella et al. (2004, using magnitudes from Table 1. However, no IR photometric measurements were available at the time of our interferometric observations, and we cannot compare our measured diameters to those derived from surface brightness relationships. Uncertainties were estimated using the subsample bootstrap technique with replacement and 10 000 subsamples. The medians of the probability distribution of the parameters match the best-fit values very well, and we used the maximum value between the 16% and 84% percentiles as uncertainty estimates (although the distributions were roughly symmetrical about the median values).

Table 3

Final best-fit parameters.

4. Discussion

The measured flux ratios are slightly different between the two epochs, although within the uncertainties. This is because the Cepheid is slightly brighter at phase φ = 0.48 (July 11) than in φ = 0.24, which makes the contrast a bit lower. Since we do not have H-band light curves to extract the Cepheid magnitude at a given phase, we took an average to estimate a mean contrast f = 0.83 ± 0.14%. This gives a difference in apparent magnitude of ΔmH = 5.20 ± 0.18 mag. This converts to apparent magnitudes for each component by using the 2MASS magnitude as a measure of the combined flux and the following equations: m1=m12+2.5log(1+f)m2=m12+2.5log(1+1/f)\begin{eqnarray} m_1 &=& m_{12} + 2.5\log(1 + f)\\ m_2 &=& m_{12} + 2.5\log(1 + 1/f) \end{eqnarray}where m12 is the 2MASS measurements, and m1 and m2 the apparent magnitude of the Cepheid and the component, respectively. We obtain Hcomp = 9.06    ±    0.24 mag and Hcep = 3.86    ±    0.24 mag. The quoted errors are due to the uncertainties in 2MASS. We determined the dereddened magnitude, H0comp=8.94 ± 0.24\hbox{$H_{0}^\mathrm{comp} = 8.94 \,\pm\, 0.24$} mag and H0cep=3.72 ± 0.24\hbox{$H_{0}^\mathrm{cep} = 3.72 \,\pm\, 0.24$} mag, by adopting the reddening law from Fouqué et al. (2007) with a total-to-selective absorption in the V band of RV = 3.23 (Sandage et al. 2004) and a color excess E(B − V) = 0.262 from Tammann et al. (2003). From the distance d = 500    ±    10 pc given by the K-band period-luminosity relation (Storm et al. 2011, the quoted error is statistical), we obtain an absolute magnitude for the companion MH = 0.45    ±    0.24 mag. Combining the known spectral type B6V with a color-spectral type relation (Ducati et al. 2001), we obtain MV = −0.12    ±    0.24 mag.

From Kepler’s law and assuming our measured projected separation ρ as a lower limit for the angular semi-major axis, that is a ≥ ρ, a minimal total mass for the system can be derived: MT=M1+M2≥ρ3d3P2,\begin{eqnarray*} M_\mathrm{T} = M_\mathrm{1} + M_\mathrm{2} \geq \frac{\rho^3 d^3}{P^2}, \end{eqnarray*}with ρ in arcsecond, d in parsec, and P in year. We therefore derived MT ≥ 9.7 ± 0.6   M⊙. This is compatible with the 5.1   M⊙ for the Cepheid, predicted from the pulsation mass (Caputo et al. 2005), and with the 5   M⊙ for the companion, inferred from its spectral type.

5. Conclusion

We used the high angular resolution provided by the four-telescope combiner PIONIER to detect the orbiting companion of the short-period cepheid AX Cir. We employed a binary model with a primary represented by a uniform disk and the secondary as an unresolved source. We derived a limb-darkened angular diameter for the Cepheid at two pulsation phases, θLD = 0.839    ±    0.023 mas (at φ = 0.24) and θLD = 0.742    ±    0.020 mas (at φ = 0.48). We also measured an averaged H-band flux ratio between the companion and the Cepheid, f = 0.83    ±    0.14%, and the astrometric position of the secondary relative to the primary, ρ = 29.2    ±    0.2 mas and PA = 167.8    ±    0.3°. We also set a lower limit on the total mass of the system based on our measured projected separation. Finally, we pointed out the need of accurate infrared light curves to enable a more precise flux estimate of the companion from the contrast measured from interferometry.

This second detection (after that of V1334 Cyg, Paper I) demonstrates the capabilities of long-baseline interferometers for studying the close-orbit companions of Cepheids. Further interferometric observations will be obtained in the future to

cover the orbit, and then combined with radial velocity measurements to derive all orbital elements. For now, only single-line spectroscopic measurements are available, we are also involved in a long-term spectroscopic program to detect the radial velocity of the companion. This will provide an orbital parallax and model-free masses.

Online material

Table 2

Journal of the observations.

Acknowledgments

The authors thank all the people involved in the VLTI project. A.G. acknowledges support from FONDECYT grant 3130361. J.D.M. acknowledges funding from the NSF grants AST-1108963 and AST-0807577. W.G. and G.P. gratefully acknowledge financial support for this work from the BASAL Centro de Astrofísica y Tecnologías Afines (CATA) PFB-06/2007. Support from the Polish National Science Center grant MAESTRO and the Polish Ministry of Science grant Ideas Plus (awarded to G.P.) is also acknowledged. We acknowledge financial support from the Programme National de Physique Stellaire (PNPS) of CNRS/INSU, France. PIONIER was originally funded by the Poles TUNES and SMING of Université Joseph Fourier (Grenoble) and subsequently supported by INSU-PNP and INSU-PNPS. The integrated optics beam combiner is the result of collaboration between IPAG and CEA-LETI based on CNES R&T funding. This research received the support of PHASE, the high angular resolution partnership between ONERA, the Observatoire de Paris, CNRS, and University Denis Diderot Paris 7. This work made use of the SIMBAD and VIZIER astrophysical database from the CDS, Strasbourg, France, and the bibliographic informations from the NASA Astrophysics Data System. This research has made use of the Jean-Marie Mariotti Center SearchCal service, co-developed by FIZEAU and LAOG/IPAG. The research leading to these results received funding from the European Research Council under the European Community’s Seventh Framework Program (FP7/2007–2013)/ERC grant agreement N° 227224 (PROSPERITY).

References

  1. Acharova, I. A., Mishurov, Y. N., & Kovtyukh, V. V. 2012, MNRAS, 420, 1590 [NASA ADS] [CrossRef] [Google Scholar]
  2. Bohm-Vitense, E., & Proffitt, C. 1985, ApJ, 296, 175 [NASA ADS] [CrossRef] [Google Scholar]
  3. Bonneau, D., Clausse, J.-M., Delfosse, X., et al. 2006, A&A, 456, 789 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  4. Bonneau, D., Delfosse, X., Mourard, D., et al. 2011, A&A, 535, A53 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  5. Bono, G., Caputo, F., & Castellani, V. 2006, Mem. Soc. Astron. Italiana, 77, 207 [Google Scholar]
  6. Caputo, F., Bono, G., Fiorentino, G., Marconi, M., & Musella, I. 2005, ApJ, 629, 1021 [NASA ADS] [CrossRef] [Google Scholar]
  7. Claret, A., & Bloemen, S. 2011, A&A, 529, A75 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  8. Cutri, R. M., Skrutskie, M. F., van Dyk, S., et al. 2003, VizieR Online Data Catalog: II/246 [Google Scholar]
  9. Ducati, J. R., Bevilacqua, C. M., Rembold, S. B., & Ribeiro, D. 2001, ApJ, 558, 309 [NASA ADS] [CrossRef] [Google Scholar]
  10. Evans, N. R. 1994, ApJ, 436, 273 [NASA ADS] [CrossRef] [Google Scholar]
  11. Evans, N. R. 2000, AJ, 119, 3050 [NASA ADS] [CrossRef] [Google Scholar]
  12. Evans, N. R., Schaefer, G. H., Bond, H. E., et al. 2008, AJ, 136, 1137 [NASA ADS] [CrossRef] [Google Scholar]
  13. Fouqué, P., Arriagada, P., Storm, J., et al. 2007, A&A, 476, 73 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  14. Gallenne, A., Kervella, P., & Mérand, A. 2011, A&A, 538, A24 [Google Scholar]
  15. Gallenne, A., Monnier, J. D., Mérand, A., et al. 2013, A&A, 552, A21 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  16. Haguenauer, P., Alonso, J., Bourget, P., et al. 2010, in SPIE Conf. Ser., 7734 [Google Scholar]
  17. Hanbury Brown, R., Davis, J., Lake, R. J. W., & Thompson, R. J. 1974, MNRAS, 167, 475 [NASA ADS] [CrossRef] [Google Scholar]
  18. Jaschek, M., & Jaschek, C. 1960, PASP, 72, 500 [Google Scholar]
  19. Keller, S. C. 2008, ApJ, 483 [Google Scholar]
  20. Kervella, P., Bersier, D., Mourard, D., et al. 2004, A&A, 428, 587 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  21. Klagyivik, P., & Szabados, L. 2009, A&A, 504, 959 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  22. LeBouquin, J.-B., Berger, J.-P., Lazareff, B., et al. 2011, A&A, 535, A67 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  23. Lloyd Evans, T. 1982, MNRAS, 199, 925 [NASA ADS] [Google Scholar]
  24. Neilson, H. R., Cantiello, M., & Langer, N. 2011, A&A, 529, L9 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  25. Petterson, O. K. L., Cottrell, P. L., & Albrow, M. D. 2004, MNRAS, 350, 95 [NASA ADS] [CrossRef] [Google Scholar]
  26. Pietrzyński, G., Thompson, I. B., Gieren, W., et al. 2010, Nature, 468, 542 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
  27. Pietrzyński, G., Thompson, I. B., Graczyk, D., et al. 2011, ApJ, 742, L20 [Google Scholar]
  28. Prada Moroni, P. G., Gennaro, M., Bono, G., et al. 2012, ApJ, 749, 108 [NASA ADS] [CrossRef] [Google Scholar]
  29. Samus, N. N., Durlevich, O. V., et al. 2009, VizieR Online Data Catalog: B/gcvs [Google Scholar]
  30. Sandage, A., Tammann, G. A., & Reindl, B. 2004, A&A, 424, 43 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  31. Storm, J., Gieren, W., Fouqué, P., et al. 2011, A&A, 534, A94 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  32. Szabados, L. 1989, Commun. Konkoly Obs. Hungary, 94, 1 [NASA ADS] [Google Scholar]
  33. Tammann, G. A., Sandage, A., & Reindl, B. 2003, A&A, 404, 423 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  34. Usenko, I. A., Kniazev, A. Y., Berdnikov, L. N., & Kravtsov, V. V. 2011, Astron. Lett., 37, 499 [NASA ADS] [CrossRef] [Google Scholar]

All Tables

Table 1

Parameters of the Cepheid and its close companion.

In the text
Table 3

Final best-fit parameters.

In the text
Table 2

Journal of the observations.

In the text

All Figures

thumbnail Fig. 1

(u,v) plane coverage for all our observations of AX Cir.
In the text
thumbnail Fig. 2

Probability map for the companion position of July 14.
In the text
thumbnail Fig. 3

Closure phase signal of AX Cir for July 14, with respect to the modified Julian date. The spectral channels were averaged for clarity. The solid black line represents our best fit model.
In the text
thumbnail Fig. 4

Squared visibility measurements of AX Cir. The data are in blue for July 14 and in green for July 11, while the red dots are the fitted binary model for both epochs.
In the text

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.