Orbital Solution for the Spectroscopic Binary in the GW Ori Hierarchical Triple
We present the first double-lined orbital solution for the close binary in the GW Ori triple system. Using 12 epochs of infrared spectroscopy, we detected the lines of both stars in the inner pair, previously known as single-lined only. Our preliminary infrared orbital solution has an eccentricity of , a period of days, and a mass ratio of . We find a larger semi-amplitude for the primary star, km s, with an infrared-only solution compared to km s with optical data from the literature, likely the result of line blending and veiling in the optical. The component spectral types correspond to G3 and K0 stars, with values of 43 km s and 50 km s, respectively. We obtained a flux ratio of 0.58 0.14 in the H-band, allowing us to estimate individual masses of 3.2 and 2.7 M for the primary and secondary, respectively, using evolutionary tracks. The tracks also yield a coeval age of 1 Myr for both components to within 1. GW Ori is surrounded by a circumbinary/circumtriple disk. A tertiary component has been detected in previous studies; however, we did not detect this component in our near-infrared spectra, probably the result of its relative faintness and blending in the absorption lines of these rapidly rotating stars. With these results, GW Ori joins the small number of classical T Tauri, double-lined spectroscopic binaries.
Measurements of stellar masses are fundamental to our understanding of the formation and evolution of pre-main sequence (PMS) stars because mass determines the manner of a star’s birth and early development, and likely plays a role in the planet formation properties of a system. Short-period binaries provide an ideal means to precise dynamical mass determination because observations sampling repeated orbits are achievable in months to years time scales. Mass ratio distributions also yield insight into binary formation mechanisms, which are important to explore as most low-mass young stars are located in binary and multiple systems (e.g., Simon et al., 1995). To measure absolute masses and to determine the young binary mass ratio distribution with high statistical significance, it is necessary to determine precise properties for a larger sample of low mass spectroscopic binaries (SBs) than is presently available, i.e. for hundreds of systems rather than dozens. This work represents part of that effort.
GW Ori was originally described as a single-line SB classical T Tauri system with a nearly circular orbit and an orbital period of 242 days (Mathieu et al., 1991). Mathieu et al. (1991) found a primary component with a value of 40 km s and effective temperature () of 6000 K from cross-correlating with a synthetic spectrum. They estimated masses of 2.5 M and 0.5 M for the primary and secondary components, respectively. Analysis of RV residuals identified evidence for a third companion. All three stars were angularly resolved interferometrically in the H-band by Berger et al. (2011), who obtained an image of GW Ori as a triple system with an inner binary separation of 1.4 AU and a third component with a projected separation of 8 AU. Using a primary component temperature of 5700 K at an age of 10 Myrs, Berger et al. (2011) calculated a primary mass of 3.6 M. The presence of near- and far-infrared (IR) excesses was inferred from the GW Ori spectra and explained by modeling circumprimary and circumbinary disks (Mathieu et al., 1991).
GW Ori is one of the few PMS SBs to host both circumbinary and circumstellar material (Basri et al., 1997; Jensen & Mathieu, 1997; Prato et al., 2002b; Kellogg et al., 2017). These systems are important because they potentially support circumstellar and circumbinary planet formation; some research indicates a paucity of planet formation in the closest binary systems (e.g., Kraus et al., 2016). Also, classical T Tauri SBs challenge our understanding of mass transfer from circumbinary to circumstellar disks and may represent a transitory evolutionary phase. Finally, SBs with circumbinary material potentially provide precise component stellar mass measurements (e.g., Simon et al., 2017), as well as disk mass estimates (Andrews & Williams, 2005), which would greatly inform our understanding of the star-disk interaction.
The use of infrared spectroscopy in observations of SBs permits the detection of photospheric lines in the fainter, redder secondary star, given the much more favorable secondary/primary flux ratio at longer wavelengths, compared to the optical, in which the stars’ spectral energy distributions (SEDs) are in the Raleigh-Jeans regime (e.g., Prato et al., 2002a). We successfully obtained the double-lined orbital parameters for the GW Ori SB. We briefly describe our observations (§2), analysis and results (§3), and discuss the properties of this complex T Tauri triple (§4).
2 Observations and Data Reduction
We used the facility near-IR spectrograph, NIRSPEC, at the Keck II telescope on Mauna Kea (McLean et al., 1998, 2000). With a 0288 (2 pixel) slit width, the spectral resolution is 30,000 (8 km s). Our observations were centered in the -band on order 49 (1.545–1.565 m), a region almost entirely free of telluric absorption (Rousselot et al., 2000). Multiple epochs of IR spectra were obtained for GW Ori from 2002–2010; specific dates appear in Table 1. The observations were taken in ABBA nod sequences to allow for subtraction of the sky background and bad pixels. The spectra were extracted with REDSPEC
3 Analysis and Results
To measure the RVs for the stellar components of the GW Ori SB, we cross-correlated our observed spectra against a grid of template spectra rotationally broadened to different values of (Mace et al., 2012). Unfortunately, as illustrated in Figure 1, the spectral lines are very broad, making the process of measuring the RVs more challenging (Ruíz-Rodríguez et al., 2013). Absorption line veiling as the result of accretion and photometric variability, for example from cool star spots, can also impact the cross-correlation. We follow the approach of Zucker & Mazeh (1994) with a similar algorithm. Given the variability and veiling, we measured the average of the flux ratios, , calculated only for the phases with the largest radial velocity semi-amplitudes. We then repeated the cross-correlations, holding this value fixed for all phases.
The best fit between our observed spectra and the grid of template spectra was found using a G3V (HD 1835), with km s, for the primary star and a K0V (BS 7368), with km s, for the secondary. The flux ratio, 0.58 0.14, was held constant for all final cross-correlations. Remarkably, this ratio is almost equal to the weighted average H-band flux ratio determined by Berger et al. (2011), 0.57 0.05, on the basis of their visibility and closure phase modeling analysis. We did not detect the tertiary component, likely because of veiling and the blending of the spectral lines in the rapidly rotating primary and secondary stars. In Table 1, we provide the GW Ori IR RV measurements and the barycentric Julian dates of the observations. Uncertainties in the IR RVs, determined following the procedure outlined in Mace et al. (2012) and Ruíz-Rodríguez et al. (2013), were 1.8 km s for the primary and 2.0 km s for the secondary.
We used the Levenberg-Marquardt approach (Press et al., 1992) to derive the orbital elements for the inner binary on the basis of the IR RVs (Table 2). The RVs show a large scatter of 1–3 from the orbital fit, likely resulting from contamination by the tertiary spectrum, as well as line-blending, veiling, and strong and variable IR excess in the system. Our orbital solution is shown in Figure 2. We followed the same approach to fit a single-lined solution to the optical RVs (Mathieu et al., 1991); these optical data and our corresponding orbital fit are also shown in Figure 2. For the optical data we found km s, compared to km s for the IR-only solution; the smaller amplitude of the optical-only orbital solution is likely the outcome of bias from blending of the broad lines, given the large , and veiling in the optical. The blended lines of the tertiary component could in principle impact the IR RVs and orbital solution in particular; however, even with the more favorable flux ratio in the IR, the tertiary is much fainter than the SB components and its small mass is unlikely to cause perceptible effects, particularly over the three years during which almost all of the IR data were taken.
4 Discussion and Conclusions
The IR orbit presented here is likely to be relatively accurate but lacks precision. A dozen observations is close to the lower limit for the derivation of an SB orbit. Hence, the parameters presented in Table 2 have large associated uncertainties. However, there is value in the publication of such a preliminary orbit because knowledge of the component mass and flux ratios, only possible with the IR detection of the secondary, are of value for other investigations (e.g., Czekala et al. 2017). Furthermore, a system such as the GW Ori SB, with a period of 241 days, requires a long term investment of at least several years and flexible scheduling with a high-resolution IR spectrograph to obtain the desirable phase coverage required for a more precise orbital solution. Because the tertiary component in this young star triple system is significantly fainter and likely much less massive than the SB components, its impact on the solution presented here is likely minimal. Additional observations should be taken in order to improve the phase coverage and precision, but publication of this preliminary orbit will serve to optimize future efforts.
GW Ori is one of a handful of pre-main sequence SBs with a circumbinary disk and active accretion, implying the presence of circumstellar material as well. Other objects in this category include V4046 Sgr (Stempels & Gaum 2004), AK Sco (Andersen et al. 1989), DQ Tau (Mathieu et al. 1997), UZ Tau E (Prato et al. 2002b), TWA 3 (Kellogg et al., 2017), and AS 205 (Eisner et al. 2005). Apart from DQ Tau, all of these systems have companions at separations of tens to thousands of AU and ages of 1 to 12 Myr. The periods of the spectroscopic orbits cover a range from 2 days to 12 years and the eccentricities from 0 to 0.6. The mass ratios of these systems span 0.3 to 1.0 and they are located in a variety of star forming regions. Thus, there seem to be no unifying properties to this accreting sample of young SBs.
The discovery of planets in orbit around main sequence SBs (e.g., Doyle et al., 2011) underscores the potential importance of studying circumbinary disks. Photometric and spectroscopic monitoring programs of the binary orbits and pulsed accretion in DQ Tau (Basri et al. 1997), UZ Tau E (Jensen et al. 2007), and TWA 3 (Tofflemire et al., 2017) demonstrate the direct link between the circumbinary disk, properties of the binary stars, and stimulation of the accretion process. It may also be possible to connect the disk and accretion characteristics to the binary’s angular momentum; with observed component values of 4050 km s, the stars in the inner GW Ori binary are relatively rapid rotators.
Rosero et al. (2011) discussed the possibility of Kozai perturbations in the 3 day orbital period binary RX J1622.7Ð2325Nw as the source of the system’s unusually large eccentricity, 0.3. For orbital period of less than a few days, normally the eccentricity would be zero (e.g., Melo et al. 2001). In the GW Ori SB, with of only 0.21, some circularization may have already taken place even at an age of only 1 Myr. Both SBs have companions at similar projected separations, 100 AU, although RX J1622.7Ð2325Nw hosts no disk material. Also, the RX J1622.7Ð2325Nw companion is itself a close binary and roughly equal in total mass to the SB. The GW Ori SB is probably at least a factor of 5 greater in mass than the tertiary (Berger et al. 2011); it is unlikely that this companion has an impact of the same magnitude on the SB as the companion in the RX J1622.7Ð2325Nw system. It is possible that the complex circumbinary and circumstellar disk material in concert with the dynamical action of the tertiary in the GW Ori system may be responsible for some degree of rapid damping of the binary eccentricity. With only 12 epochs of IR data, the may be smaller than determined here and more in line with the value determined in our fit to the optical-only data.
We used the H-band flux ratios for the component pairs given in Table 2 of Berger et al. (2011) to calculate the flux ratio of the inner, spectroscopic binary to the tertiary component, 6.58 2.96. Combined with the total H-band magnitude of the system, 7.103 0.029 mag, we then determined the apparent H magnitude of the spectroscopic binary to be 7.26 0.07 mag. Using our flux ratio for the spectroscopic binary components, 0.58 0.14, determined from the cross-correlation of multiple epochs and in agreement with that of Berger et al. (2011) (§3), we then derived the individual apparent H-band magnitudes for each star in the inner binary, 7.76 0.12 mag for the primary and 8.35 0.18 mag for the secondary. Applying a distance modulus corresponding to the 414 7 pc distance to Orion (Menten et al., 2007), we found absolute H magnitudes of and for the primary and secondary, respectively. The final uncertainties represent the error propagation of the uncertainties in the 2MASS H-magnitude, the flux ratios, and the distance.
Values for the SB components’ were estimated using the spectral types determined from the cross-correlation and adopting the temperature scale illustrated in Figure 5 of Luhman et al. (2003). We found 5780 100 K for the primary and 5250 100 K for the secondary; the uncertainties of 100 K correspond to 1 spectral subclasses. To estimate the individual masses and age of the system, we plotted the GW Ori SB components on the Hertzsprung-Russell (HR) diagram and compared them to the evolutionary models of Dotter et al. (2008) (Figure 3). For the primary and secondary masses we found 3.2 M and 2.7 M, respectively. Uncertainties are approximately 0.2 and the mass ratio is 0.84 0.08. From our cross-correlation of the spectra we found a value for the mass ratio of , less than that calculated from the tracks, although within 1 of that value given the uncertainties of 10% or more in both mass ratios. This discrepancy may be the result of excess flux from the secondary star in the SB. Given that the components are of unequal mass, and the system is embedded in a complex circumbinary/circumtriple disk structure, yet shows evidence for active accretion, the lower mass secondary in a larger radius orbit may be preferentially accreting, increasing its H-band flux and hence the mass derived from the HR Diagram (Figure 3). We find a total mass of 5.9 M for the inner binary, well within 1 of that calculated by Berger et al. (2011), 5.6 M. Both component fall within 1 of the 1 Myr isochrone.
We used the track-derived masses and and from Table 2 to estimate the SB’s inclination and found values of and , respectively, consistent with the results of Berger et al. (2011) for a lower inclination than previously identified (Shevchenko et al., 1998). Given this low inclination, it is unlikely that the stellar components in the GW Ori SB are eclipsing. A potential origin for the intermittent dimming observed in the system (e.g., Shevchenko et al., 1998) could arise from clumpy accretion (e.g., Graham, 1992) onto the secondary star in a stream from the circumbinary/circumtriple disk structure with a geometry such that eclipses of one of the stars by the accretion stream, with the period of the SB, is observable. Torques on the system could alter the geometry of the accretion stream and/or disks, compounding the aperiodic accretion action and leading to the intermittent nature of the dimming. A misalignment between the SB and the disk material could support this hypothesis.
Using high-resolution, IR spectroscopy, we have determined the first double-lined solution for the inner SB in the GW Ori system. Our results are consistent with a 1 Myr system of relatively massive stars, 3.2 d 2.7 M, with at least one component undergoing active accretion. The orbital solution presented here indicates that the system is relatively close to face-on and that the periodic dimming observed between 1987 and 1992 was unlikely the result of eclipsing stellar components; however, periodic occultations of one of the stars by circumstellar or streaming circumbinary material could explain this phenomenon. GW Ori provides an important opportunity for detailed study of multiple star and disk evolution, and for the interaction of circumbinary/circumtriple and circumstellar disk material.
|(km s)||(km s)||(km s)||(km s)|
|2001 Jan 05||2451914.84608||30.20||27.26||0.2017|
|2001 Oct 10||2452192.70857||29.75||17.82||0.3539|
|2001 Dec 29||2452272.86298||25.76||32.96||0.6863|
|2002 Feb 05||2452310.84005||19.27||34.99||0.8438|
|2002 Oct 30||2452578.09003||21.29||34.46||0.9520|
|2002 Dec 14||2452622.94721||25.61||34.53||0.1381|
|2002 Dec 22||2452631.01035||26.30||30.49||0.1715|
|2003 Feb 08||2452678.87603||34.32||19.03||0.3700|
|2003 Nov 04||2452948.16698||34.33||18.63||0.4867|
|2004 Jan 26||2453030.93007||22.92||36.75||0.8299|
|2004 Dec 26||2453365.96450||27.53||31.83||0.2193|
|2010 Dec 12||2455543.08232||29.52||24.04||0.2475|
|P (days)||241.15 0.72|
|sin (10 km)|
|sin (10 km)|
- affiliation: Lowell Observatory, 1400 West Mars Hill Road Flagstaff, AZ 86001 USA; firstname.lastname@example.org
- affiliation: Center for Imaging Science, School of Physics & Astronomy, and Laboratory for Multiwavelength Astrophysics, Rochester Institute of Technology, 54 Lomb Memorial Drive, Rochester, NY 14623, USA
- affiliation: Lowell Observatory, 1400 West Mars Hill Road Flagstaff, AZ 86001 USA; email@example.com
- Primary star RV uncertainty is 1.8 km s.
- Secondary star RV uncertainty is 2.0 km s.
- Andrews, S. M., & Williams, J. P. 2005, ApJ, 631, 1134
- Basri, G., Johns-Krull, C. M., & Mathieu, R. D. 1997, AJ, 114, 781
- Berger, J.-P., Monnier, J. D., Millan-Gabet, R., et al. 2011, A&A, 529, L1
- Czekala, I., Andrews, S. M., Torres, G., et al. 2017, arXiv:1710.03153
- Dotter, A., Chaboyer, B., Jevremović, D., et al. 2008, ApJS, 178, 89
- Doyle, L. R., Carter, J. A., Fabrycky, D. C., et al. 2011, Science, 333, 1602
- Graham, J. A. 1992, PASP, 104, 479
- Jensen, E. L. N., & Mathieu, R. D. 1997, AJ, 114, 301
- Kellogg, K., Prato, L., Torres, G., et al. 2017, ApJ, 844, 168
- Kim, S., Prato, L., & McLean, I. 2015, REDSPEC: NIRSPEC data reduction, Astrophysics Source Code Library, ascl:1507.017
- Kraus, A. L., Ireland, M. J., Huber, D., Mann, A. W., & Dupuy, T. J. 2016, AJ, 152, 8
- Luhman, K. L., Briceño, C., Stauffer, J. R., et al. 2003, ApJ, 590, 348
- Mace, G. N., Prato, L., Torres, G., et al. 2012, ArXiv e-prints, arXiv:1206.3329
- Mathieu, R. D., Adams, F. C., & Latham, D. W. 1991, AJ, 101, 2184
- McLean, I. S., Graham, J. R., Becklin, E. E., et al. 2000, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 4008, Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, ed. M. Iye & A. F. Moorwood, 1048–1055
- McLean, I. S., Becklin, E. E., Bendiksen, O., et al. 1998, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 3354, Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, ed. A. M. Fowler, 566–578
- Menten, K. M., Reid, M. J., Forbrich, J., & Brunthaler, A. 2007, A&A, 474, 515
- Prato, L., Simon, M., Mazeh, T., et al. 2002a, ApJ, 569, 863
- Prato, L., Simon, M., Mazeh, T., Zucker, S., & McLean, I. S. 2002b, ApJL, 579, L99
- Press, W. H., Teukolsky, S. A., Vetterling, W. T., & Flannery, B. P. 1992, Numerical recipes in FORTRAN. The art of scientific computing, ed. Press, W. H., Teukolsky, S. A., Vetterling, W. T., & Flannery, B. P.
- Rousselot, P., Lidman, C., Cuby, J.-G., Moreels, G., & Monnet, G. 2000, AA, 354, 1134
- Ruíz-Rodríguez, D., Prato, L., Torres, G., Wasserman, L. H., & Neuhäuser, R. 2013, AJ, 145, 162
- Shevchenko, V. S., Grankin, K. N., Mel’Nikov, S. Y., & Lamzin, S. A. 1998, Astronomy Letters, 24, 528
- Simon, M., Ghez, A. M., Leinert, C., et al. 1995, ApJ, 443, 625
- Simon, M., Guilloteau, S., Di Folco, E., et al. 2017, ApJ, 844, 158
- Tofflemire, B. M., Mathieu, R. D., Herczeg, G. J., Akeson, R. L., & Ciardi, D. R. 2017, ApJ, 842, L12
- Torres, G. 2001, AJ, 121, 2227
- Zucker, S., & Mazeh, T. 1994, ApJ, 420, 806