EDP Sciences logo
Subscriber Authentication Point
Search
Menu
Home All issues Volume 545 (September 2012) A&A, 545 (2012) L10 Full HTML
Highlight
Free Access
Issue
A&A
Volume 545, September 2012
Article Number L10
Number of page(s) 4
Section Letters
DOI https://doi.org/10.1051/0004-6361/201219800
Published online 20 September 2012

© ESO, 2012

1. Introduction

MWC 300 is an enigmatic early-type emission-line star whose nature and evolutionary state are not well known. Herbig (1960) classified MWC 300 as a pre-main-sequence star since nebulosity exists around the star. It is included in several catalogs of pre-main-sequence stars (e.g., Thé et al. 1994). However, MWC 300 was also listed as a probable B[e] supergiant (e.g., Allen & Swings 1976; Appenzeller 1977; Lamers et al. 1998). Miroshnichenko et al. (2004, hereafter M04) carried out extensive spectroscopic and photometric studies on MWC 300, and strengthened the arguments in favor of the supergiant classification. M04 suggest that MWC 300 has an effective temperature of 19 000 K, a distance of 1.8 ± 0.2 kpc, and a luminosity of log L/L⊙ = 5.1 ± 0.1.

Two-dimensional radiative transfer modeling shows that MWC 300 has a flared dusty disk rather than a spherical dusty envelope (M04). The modeled disk has an inner radius of  ~11 mas and is viewed almost edge-on. Domiciano de Souza et al. (2008) observed MWC 300 at 11.25 μm using the BURST mode of VLT/VISIR. The obtained diffraction-limited (~0.3′′) image shows that MWC 300 is partially resolved with an FWHM diameter of 69 ± 10 mas. Monnier et al. (2009) observed MWC 300 with the Keck telescope and measured a Gaussian FWHM diameter of 49 ± 3 mas at 10.7 μm.

MWC 300 exhibits radial velocity (RV) variations that suggest a binary (Corporon & Lagrange 1999). Takami et al. (2003) carried out spectro-astrometric observations and studied the absorption feature of Hα. They detected a positional displacement of the line-emitting region of 17 ± 4 mas with respect to the position of the continuum. Photospheric line RV variations detected by M04 also suggest a companion.

Table 1

Observation log of our VLTI/AMBER observation of MWC 300.

thumbnail Fig. 1

Observations and temperature-gradient model (i = 80°) of MWC 300. The upper-left panel shows the observed visibilities and the visibilities of the best-fitting model; lower-left the model-predicted and observed closure phases, upper-right the different lines refer to the SED contributions from different components of our model. Black dots are the observed data. The lower-right panel shows the logarithm of brightness distribution of the model disk. North is up and east to the left. The white point represents the location of the primary star. Our observations were performed along the PA of 66.2° (red line). The green line refers to the possible locations of the secondary companion.

Thanks to the development of near-infrared interferometry, we can now achieve a high spatial resolution of a few mas. It allows us to directly resolve the MWC 300 system and study the circumstellar disk structure, as well as the central binary. In this paper, we present the first near-infrared interferometric AMBER/VLTI observations of MWC 300. The observations are described in Sect. 2. In Sect. 3, we present a model consisting of a binary and a temperature-gradient disk that can reproduce the visibilities, closure phases, and SED. The results are discussed in Sect. 4, and conclusions are summarized in Sect. 5.

2. Observation and data reduction

We observed MWC 300 with the ESO Very Large Telescope Interferometer (VLTI) and the AMBER instrument (Petrov et al. 2007) in the low spectral resolution mode (R = 35) on 18 April 2009 (ID 083.D-0224; PI G. Weigelt). The observation log is presented in Table 1.

For data reduction, we used the AMBER data reduction package amdlib1 (Tatulli et al. 2007; Chelli et al. 2009). To improve the calibration, we used 20% of the frames with the best fringe signal-to-noise ratio of both the target and calibrator data (Tatulli et al. 2007) and applied a method for equalizing of the target and calibrator histograms of the optical path differences (Kreplin et al. 2012). The obtained visibilities and closure phases are shown in Fig. 1 (left two panels). We were not able to derive visibilities at all H-band wavelengths (see Fig. 1) because MWC 300 is quite faint in the H band (H = 8.2). The data were calibrated using the calibrator HD 142669 (diameter = 0.27 ± 0.027 mas; Pasinetti Fracassini et al. 2001).

3. Temperature-gradient disk model and binary

The observational data of MWC 300 shows strong closure phases up to 180°, which suggest that MWC 300 is a binary. Therefore, we have used a model consisting of a temperature-gradient disk and a binary to interpret the data.

Table 2

Scan ranges of the model parameters and their values for the best-fitting models with different inclination angles.

3.1. Model description

Our model consists of a primary star located at the center of the system, a companion, and a ring-shaped disk with a power-law temperature distribution. M04 find that the stellar SED of MWC 300 can be fitted by a single Kurucz O/B-type model (Kurucz 1994), and they suggest that the companion of MWC 300 may be either faint (3–4 mag fainter than the primary) or an O/B-type companion of a similar (but not identical) brightness. We adopt the latter case here, since it is consistent with the detected strong closure phase. We assume that the secondary companion has approximately the same effective temperature as the primary star and that the total flux from the two stars is approximately equivalent to a single star fitted by a Kurucz model with Teff = 19   000 K and R∗ = 29   R⊙ (M04). The brightness ratio, κ, between the two stars is a free fitting parameter. Owing to the linear array configuration we used, we can only derive the projected binary separations rs along the baseline position angle (PA) of 66.2°.

The measured low visibilities suggest that MWC 300 has a well resolved extended disk. We assume the disk is geometrically thin and optically thick and that it is emitting as a blackbody. The disk has an inner radius of rin, outer radius of rout, and a power-law temperature distribution of T = Tin(r/rin) − α, where Tin is the disk temperature at rin (Hillenbrand et al. 1992). Since our interferometric data are measured at only one hour angle with a linear array configuration, we are not able to directly derive the disk elongation and inclination. M04 suggest that the disk of MWC 300 is viewed almost edge-on, based on their two-dimensional radiative transfer modeling. We adopt their inclination angle of i = 80° as a fixed value in our modeling.

Our model has seven free parameters (see Table 2): the inner disk radius rin, the outer disk radius rout, the disk temperature Tin at the inner radius, the temperature power-law index α, the projected separation rs of the binary, the flux ratio κ between the two stars, and the PA θdisk of the major axis of the inclined disk. The mass center of the binary is expected to be at the center of the disk. However, since we do not know the mass ratio and in order to keep the number of parameters small, we assume that the primary star is located at the center of the disk (for more discussion, see Sect. 3.2).

The total complex visibility of our model is given by Vtotal = fprimaryVprimary + fsecondaryVsecondary + fdiskVdisk, where f is the flux contribution of each component to the total system flux and V the complex visibility contributed by each component. We calculated the model-predicted visibilities and closure phases for each model (Table 2; Sect. 3.2) and compared them with the observations in order to study if our model can simultaneously reproduce all interferometric observations, as well as the spectral energy distribution (SED). The dereddened SED data (shown in the upper right panel in Fig. 1) is taken from M04 and Domiciano de Souza et al. (2008), including UBV data from Wolf & Stahl (1985), JHK data from Skrutskie et al. (2006), LM data from Bouchet & Swings (1982), NQs data from M04, and MSX B1B2ACDE data from Egan et al. (2003).

3.2. Results of the temperature-gradient modeling

We searched for the best-fitting model in a large parameter space (see two-step search in Table 2). During each step, we divided the search range for each of the model parameters into 10 − 20 intervals and calculated the visibilities, closure phases, and SEDs of all models that correspond to all combinations of all free model parameter values (~2    ×    8    ×    107 models; see Table 2). Then the derived visibilities, closure phases, and SEDs of all 1.6    ×    108 models were compared with the observations in order to find the best-fitting model with the minimum overall reduced χ2.

Figure 1 and Table 2 show our best-fitting MWC 300 models, which are able to approximately reproduce the observed wavelength dependence of the visibilities and the closure phase, along with the SED. In our first model (Fig. 1 and first three lines in Table 2), we adopted the inclination angle of i = 80° (M04) as a fixed value, as discussed above. The flux contributions from the binary and the disk at different wavelengths (e.g. 1.6 μm, 1.9 μm, 2.1 μm, and 2.4 μm) are listed in Table 3. This modeling provided the following parameters. The secondary companion is times fainter than the primary star and has a projected separation of 4.4 ± 0.2 mas or 7.9 ± 0.4 AU along the PA of 66.2°. The temperature-gradient disk has an inner radius of  ~ 17 mas or  ~ 30 AU and an outer radius rout of  ~ 200 mas or  ~ 360 AU, while rout cannot be well constrained since the outer (colder) parts of the disk are faint in the infrared. The disk major axis has a PA of  ~ 4°. The temperature at the inner disk radius is  ~ 890 K, and the temperature power-law index is  ~ 0.57 (see Table 2). All uncertainties correspond to the 5σ confidence level.

We also calculated models assuming that the geometric center of the binary instead of the primary star is at the center of the disk. However, these models cannot provide a better fit. Therefore, in the following, we only discuss the models with the primary star located at the center of disk.

4. Discussion

4.1. Disk inclination angle

The emission line profile of MWC 300 and strong extinction along the line of sight suggest an almost edge-on disk (M04). The value of 80° (i.e., almost edge-on) derived by radiative transfer modeling (M04) is only a rough estimate, so we also investigated models with other inclination angles. The values of parameters for the best-fitting models with i = 60° and 70° are listed in Tabel 2 (lines 4 − 9). These models can fit the observations with similar χ2 values. Our results in Table 2 show that some of our model parameters (e.g., Tin, α, rs, and κ) are independent of the disk inclination angle. However, rin and θdisk strongly depend on the disk inclination angle and cannot be constrained well. Our interferometric data do not yet allow us to constrain the inclination angle since our three visibilities were measured at the same PA. Therefore, more observations at different PAs are required in the future to improve the accuracy of the disk parameters.

4.2. Disk size

M04 modeled MWC 300 with a two-dimensional flared dusty-disk model and suggest that the inner boundary of the disk has a radius of  ~20 AU and a temperature of  ~1120 K. With the same assumed disk inclination angle of 80°, our best-fitting model suggests a slightly larger and cooler disk, with an inner radius of  ~30 AU and a temperature at the inner radius of  ~890 K. This radius is consistent with the dust sublimation radius of  ~35 AU for 890 K and gray dust opacities, but is about 2.5 times larger than the 1500 K dust sublimation radius of  ~12 AU (Monnier & Millan-Gabet 2002). This large inner disk radius and cool inner disk temperature may be explained by the existence of the secondary companion. Considering the minimum binary separation of 4.4 mas (7.9 AU), MWC 300 may have a circumbinary disk, and the secondary companion may be close enough to the disk inner radius to interact strongly with the disk (Shi et al. 2012).

Table 3

Flux contribution from different components at different wavelengths.

4.3. Binarity and B[e] phenomenon

Our interferometric data shows strong closure phases that suggest asymmetries. The asymmetries can be attributed to a binary or an extremely inhomogeneous disk. However, the observed closure phase signature is too strong to be caused by the asymmetry of the disk since the disk is only partially resolved (Monnier et al. 2006). The observed closure phase is therefore the result of a secondary companion.

Adopting the distance of 1.8 kpc, we obtain a small projected binary separation of  ~7.9 AU. However, due to our one-dimensional uv coverage, we can only derive the projected separation of the binary along PA of 66.2° and not its exact separation. The lower-right hand panel of Fig. 1 indicates the possible locations of the secondary companion. All companion positions on the green line correspond to a projected binary separation of 7.9 AU. The figure shows that MWC 300 may have a circumbinary disk if the binary separation is small enough (as, for example, in HD 62623; Plets et al. 1995; Millour et al. 2009). However, considering the AMBER AT’s field of view, the binary separation can be large enough (with a maximum value of 150 mas) for the disk to be a circumprimary disk (as, for example, in HD 87643; Millour et al. 2009). More interferometric observations are required in order to constrain the exact separation and PA of the binary.

Several other B[e] stars were also found to be binaries: η Car, MWC 349A, HD 87643, V921 Sco, and HD 327083. In HD 87643 (Millour et al. 2009) and V921 Sco (Kraus et al. 2012a), circumprimary disks were resolved, whereas in HD 327083 (Wheelwright et al. 2012) a circumbinary disk was detected. The η Car binary was found by photometric observations (Damineli et al. 1997). The binarity of MWC 349A has not been directly confirmed, but was suggested by Hofmann et al. (2002). Although the exact role of binarity in the B[e] phenomenon is still an open question, it is possible that the disks are the result of mass exchange episodes between the stellar components of the B[e] stars (Sheikina et al. 2000; Miroshnichenko 2007; Miroshnichenko et al. 2007, 2009; Kraus et al. 2010, 2012b). The slowing down of the radiative wind by the companion gravitational effect or wind shock may also be an explanation (Plets et al. 1995). Future interferometric observations will allow us to improve our understanding, since these observations will be able to determine the orbits of the B[e] binaries and to investigate the interaction of the binary companion with the disk or the wind.

5. Summary

We have presented the first VLTI/AMBER observations of the enigmatic B[e] star MWC 300. The low visibility values, the wavelength dependence of the visibilities, and the wavelength dependence of the closure phase directly suggest that MWC 300 consists of a resolved disk and a binary. To interpret our observations, we used a temperature-gradient model consisting of a binary and a ring-shaped disk. The best-fitting model is able to simultaneously reproduce the wavelength dependence of the visibilities and the closure phase, as well as the SED. Because of our one-dimensional uv coverage, we can only derive a projected binary separation of  ~4.4 mas (~7.9 AU) along PA of 66.2°, with a binary flux ratio of  ~2.2 (see Table 2). The increasing number of detected binaries in B[e] stars suggests that the binarity may play an important role in the B[e] phenomenon.

1

The AMBER – reduction package amdlib is available at: http://www.jmmc.fr/data_processing_amber.htm

Acknowledgments

We thank the ESO VLTI team on Paranal for the excellent collaboration. The data presented here were reduced using the publicly available data-reduction software package amdlib kindly provided by the Jean-Marie Mariotti Center.

References

  1. Allen, D. A., & Swings, J. P. 1976, A&A, 47, 293 [NASA ADS] [Google Scholar]
  2. Appenzeller, I. 1977, A&A, 61, 21 [NASA ADS] [Google Scholar]
  3. Bouchet, P., & Swings, J. P. 1982, in Be Stars, eds. M. Jaschek, & H.-G. Groth, IAU Symp., 98, 241 [Google Scholar]
  4. Chelli, A., Utrera, O. H., & Duvert, G. 2009, A&A, 502, 705 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  5. Corporon, P., & Lagrange, A.-M. 1999, A&AS, 136, 429 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  6. Damineli, A., Conti, P. S., & Lopes, D. F. 1997, NewA, 2, 107 [Google Scholar]
  7. Domiciano de Souza, A., Kervella, P., Bendjoya, P., & Niccolini, G. 2008, A&A, 480, L29 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  8. Egan, M. P., Price, S. D., & Kraemer, K. E. 2003, in BAAS, 35, AAS Meeting Abstracts, 1301 [Google Scholar]
  9. Herbig, G. H. 1960, ApJS, 4, 337 [NASA ADS] [CrossRef] [Google Scholar]
  10. Hillenbrand, L. A., Strom, S. E., Vrba, F. J., & Keene, J. 1992, ApJ, 397, 613 [NASA ADS] [CrossRef] [Google Scholar]
  11. Hofmann, K.-H., Balega, Y., Ikhsanov, N. R., Miroshnichenko, A. S., & Weigelt, G. 2002, A&A, 395, 891 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  12. Kraus, S., Hofmann, K.-H., Menten, K. M., et al. 2010, Nature, 466, 339 [NASA ADS] [CrossRef] [MathSciNet] [PubMed] [Google Scholar]
  13. Kraus, S., Calvet, N., Hartmann, L., et al. 2012a, ApJ, 746, L2 [NASA ADS] [CrossRef] [Google Scholar]
  14. Kraus, S., Calvet, N., Hartmann, L., et al. 2012b, ApJ, 752, 11 [NASA ADS] [CrossRef] [Google Scholar]
  15. Kreplin, A., Kraus, S., Hofmann, K.-H., et al. 2012, A&A, 537, A103 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  16. Kurucz, R. 1994, Solar abundance model atmospheres for 0, 1, 2, 4, 8 km s-1, Kurucz CD-ROM No. 19, Cambridge, Mass.: Smithsonian Astrophysical Observatory, 19 [Google Scholar]
  17. Lamers, H. J. G. L. M., Zickgraf, F.-J., de Winter, D., Houziaux, L., & Zorec, J. 1998, A&A, 340, 117 [NASA ADS] [Google Scholar]
  18. Millour, F., Chesneau, O., Borges Fernandes, M., et al. 2009, A&A, 507, 317 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  19. Miroshnichenko, A. S. 2007, ApJ, 667, 497 [NASA ADS] [CrossRef] [Google Scholar]
  20. Miroshnichenko, A. S., Levato, H., Bjorkman, K. S., et al. 2004, A&A, 417, 731 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  21. Miroshnichenko, A. S., Manset, N., Kusakin, A. V., et al. 2007, ApJ, 671, 828 [NASA ADS] [CrossRef] [Google Scholar]
  22. Miroshnichenko, A. S., Chentsov, E. L., Klochkova, V. G., et al. 2009, ApJ, 700, 209 [NASA ADS] [CrossRef] [Google Scholar]
  23. Monnier, J. D., & Millan-Gabet, R. 2002, ApJ, 579, 694 [NASA ADS] [CrossRef] [Google Scholar]
  24. Monnier, J. D., Berger, J.-P., Millan-Gabet, R., et al. 2006, ApJ, 647, 444 [NASA ADS] [CrossRef] [Google Scholar]
  25. Monnier, J. D., Tuthill, P. G., Ireland, M., et al. 2009, ApJ, 700, 491 [NASA ADS] [CrossRef] [Google Scholar]
  26. Pasinetti Fracassini, L. E., Pastori, L., Covino, S., & Pozzi, A. 2001, A&A, 367, 521 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  27. Petrov, R. G., Malbet, F., Weigelt, G., et al. 2007, A&A, 464, 1 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  28. Plets, H., Waelkens, C., & Trams, N. R. 1995, A&A, 293, 363 [NASA ADS] [Google Scholar]
  29. Sheikina, T. A., Miroshnichenko, A. S., & Corporon, P. 2000, in The Be Phenomenon in Early-Type Stars, eds. M. A. Smith, H. F. Henrichs, & J. Fabregat, ASP Conf. Ser., 214, IAU Colloq., 175, 494 [Google Scholar]
  30. Shi, J.-M., Krolik, J. H., Lubow, S. H., & Hawley, J. F. 2012, ApJ, 749, 118 [NASA ADS] [CrossRef] [Google Scholar]
  31. Skrutskie, M. F., Cutri, R. M., Stiening, R., et al. 2006, AJ, 131, 1163 [NASA ADS] [CrossRef] [Google Scholar]
  32. Takami, M., Bailey, J., & Chrysostomou, A. 2003, A&A, 397, 675 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  33. Tatulli, E., Millour, F., Chelli, A., et al. 2007, A&A, 464, 29 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  34. Thé, P. S., de Winter, D., & Perez, M. R. 1994, A&AS, 104, 315 [NASA ADS] [Google Scholar]
  35. Wheelwright, H. E., de Wit, W. J., Oudmaijer, R. D., & Vink, J. S. 2012, A&A, 538, A6 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  36. Wolf, B., & Stahl, O. 1985, A&A, 148, 412 [NASA ADS] [Google Scholar]

All Tables

Table 1

Observation log of our VLTI/AMBER observation of MWC 300.

In the text
Table 2

Scan ranges of the model parameters and their values for the best-fitting models with different inclination angles.

In the text
Table 3

Flux contribution from different components at different wavelengths.

In the text

All Figures

thumbnail Fig. 1

Observations and temperature-gradient model (i = 80°) of MWC 300. The upper-left panel shows the observed visibilities and the visibilities of the best-fitting model; lower-left the model-predicted and observed closure phases, upper-right the different lines refer to the SED contributions from different components of our model. Black dots are the observed data. The lower-right panel shows the logarithm of brightness distribution of the model disk. North is up and east to the left. The white point represents the location of the primary star. Our observations were performed along the PA of 66.2° (red line). The green line refers to the possible locations of the secondary companion.
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.