GCIRS 16SW: A Massive Eclipsing Binary in the Galactic Center

Martins, F.; Trippe, Sascha; Paumard, T.; Ott, T.; Genzel, R.; Rauw, Grégor; Eisenhauer, F.; Gillessen, S.; Maness, H.; Abuter, R.

doi:10.1086/508328

Cited by 67 publications

(92 citation statements)

References 16 publications

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“…Thus far, photometric variations have been the primary search method. Several binaries have been revealed (Ott et al 1999;Martins et al 2006;Rafelski et al 2007;Pfuhl et al 2014), although none among the S-stars. However, eclipsing binaries are expected to be only a small fraction of the true binary population.…”

Section: Introductionmentioning

confidence: 99%

Investigating the Binarity of S0-2: Implications for Its Origins and Robustness as a Probe of the Laws of Gravity around a Supermassive Black Hole

Chu

Hees

et al. 2018

ApJ

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The star S0-2, which orbits the supermassive black hole (SMBH) in our Galaxy with a period of 16 years, provides the strongest constraint on both the mass of the SMBH and the distance to the Galactic center. S0-2 will soon provide the first measurement of relativistic effects near a SMBH. We report the first limits on the binarity of S0-2 from radial velocity (RV) monitoring, which has implications for both understanding its origin and robustness as a probe of the central gravitational field. With 87 RV measurements, which include 12 new observations that we present, we have the requisite data set to look for RV variations from S0-2′s orbital model. Using a Lomb-Scargle analysis and orbit-fitting for potential binaries, we detect no RV variation beyond S0-2′s orbital motion and do not find any significant periodic signal. The lack of a binary companion does not currently distinguish different formation scenarios for S0-2. The upper limit on the mass of a companion star (M comp ) still allowed by our results has a median upper limit of M comp sini1.6 M e for periods between 1 and 150 days, the longest period to avoid tidal break-up of the binary. We also investigate the impact of the remaining allowed binary system on the measurement of the relativistic redshift at S0-2′s closest approach in 2018. While binary star systems are important to consider for this experiment, we find that plausible binaries for S0-2 will not alter a 5σ detection of the relativistic redshift.

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Section: Introductionmentioning

confidence: 99%

Investigating the Binarity of S0-2: Implications for Its Origins and Robustness as a Probe of the Laws of Gravity around a Supermassive Black Hole

Chu

Hees

et al. 2018

ApJ

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“…of two cooler extreme B supergiants/LBV candidates (P orb = 19.45 days; Martins et al 2006), with stellar mass loss resulting in an eventual lengthening of the orbital period of B17. Indeed, assuming the system avoids merger during the LBV phase and, remaining bound, receives a favourable SNe kick to reduce the orbital separation it might briefly form a high mass X-ray binary with a WR mass donor prior to the second SN.…”

Section: Discussionmentioning

confidence: 99%

The eclipsing, double-lined, Of supergiant binary Cygnus OB2-B17

Stroud

Clark

Negueruela

et al. 2010

A&A

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Context. Massive, eclipsing, double-lined, spectroscopic binaries are not common but are necessary to understand the evolution of massive stars as they are the only direct way to determine stellar masses. They are also the progenitors of energetic phenomena such as X-ray binaries and γ-ray bursts.Aims. We present a photometric and spectroscopic analysis of the candidate binary system Cyg OB2-B17 to show that it is indeed a massive evolved binary. Methods. We utilise V band and white-light photometry to obtain a light curve and period of the system, and spectra at different resolutions to calculate preliminary orbital parameters and spectral classes for the components. Results. Our results suggest that B17 is an eclipsing, double-lined, spectroscopic binary with a period of 4.0217 ± 0.0004 days, with two massive evolved components with preliminary classifications of O7 and O9 supergiants. The radial velocity and light curves are consistent with a massive binary containing components with similar luminosities, and in turn with the preliminary spectral types and age of the association.

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“…-Both H and K bands are scaled to have the same amplitude and mean magnitude as the Ott et al (1999) K-band data presented by Martins et al (2006). All errors are set to 0.04 mag, corresponding to the typical variation seen for a constant star of similar magnitude (M. Peeples et al 2007, in preparation).…”

Section: Observationsmentioning

confidence: 99%

“…Assuming the orbital separation as calculated by Martins et al (2006) is correct (if it is smaller, then will be even L/L Edd larger), this calculation implies that the temperature of Najarro et al (1997) is an overestimate. A change in the assumed affects the WD model parameters; specifically, a decrease T eff in by a few thousand kelvins will decrease the inclination T eff angle i, and thus increase the masses of the stars, by more than the formal 1 j uncertainties given by WD.…”

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confidence: 96%

“…It remains a puzzle as to why IRS 16SW does not appear to be a double-line spectroscopic binary. It is readily apparent from the depths of the eclipses that the two stars have near-equal fluxes, and from the depth ratio that they have near-equal surface brightnesses, yet Martins et al (2006) see only one set of spectroscopic lines. However, since the spectral features used by Martins et al (2006) are wind lines, with strong characteristic P Cygni profiles (Najarro et al 1997), differences in wind strength or small differences in the effective temperatures of the stars could easily conspire to make detection of the second set of lines difficult.…”

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confidence: 99%

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The Nature of the Variable Galactic Center Source GCIRS 16SW Revisited: A Massive Eclipsing Binary

Peeples

Bonanos

DePoy

et al. 2006

ApJ

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We present a reanalysis of our H-and K-band photometry and light curves for GCIRS 16SW, a regular periodic source near the Galactic center. These data include those presented by DePoy et al.; we correct a sign error in their reduction, finding GCIRS 16SW to be an eclipsing binary with no color variations. We find the system to be an equal-mass overcontact binary (both stars overfilling their Roche lobes) in a circular orbit with a period days and an inclination angle . This confirms and strengthens the findings of Martins et P p 19.4513 i p 71Њ al. that GCIRS 16SW is an eclipsing binary composed of two ∼50 M , stars, further supporting evidence of recent star formation very close to the Galactic center. Finally, the calculated luminosity of each component is close to the Eddington luminosity, implying that the temperature of 24,400 K given by Najarro et al. might be overestimated for these evolved stars.

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GCIRS 16SW: A Massive Eclipsing Binary in the Galactic Center

Cited by 67 publications

References 16 publications

Investigating the Binarity of S0-2: Implications for Its Origins and Robustness as a Probe of the Laws of Gravity around a Supermassive Black Hole

Investigating the Binarity of S0-2: Implications for Its Origins and Robustness as a Probe of the Laws of Gravity around a Supermassive Black Hole

The eclipsing, double-lined, Of supergiant binary Cygnus OB2-B17

The Nature of the Variable Galactic Center Source GCIRS 16SW Revisited: A Massive Eclipsing Binary

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