A noninteracting low-mass black hole–giant star binary system

See allHide authors and affiliations

Science  01 Nov 2019:
Vol. 366, Issue 6465, pp. 637-640
DOI: 10.1126/science.aau4005

A black hole hiding in a binary star

As material falls toward a black hole, it heats up and emits x-rays. Almost all black holes are discovered by this x-ray emission. Thompson et al. observed light from a giant star that is Doppler shifted, indicating an orbit around a binary companion. The companion object must weigh more than 2.6 solar masses, but it emits no light, including x-rays. This indicates the presence of a black hole that is not currently consuming any material. There may be a population of similarly hidden black holes that have been missed by x-ray observations.

Science, this issue p. 637


Black hole binary systems with companion stars are typically found via their x-ray emission, generated by interaction and accretion. Noninteracting binaries are expected to be plentiful in the Galaxy but must be observed using other methods. We combine radial velocity and photometric variability data to show that the bright, rapidly rotating giant star 2MASS J05215658+4359220 is in a binary system with a massive unseen companion. The system has an orbital period of ~83 days and near-zero eccentricity. The photometric variability period of the giant is consistent with the orbital period, indicating star spots and tidal synchronization. Constraints on the giant’s mass and radius imply that the unseen companion is 3.30.7+2.8 solar masses, indicating that it is a noninteracting low-mass black hole or an unexpectedly massive neutron star.

The observed distributions of neutron star and stellar black hole masses are connected to the mechanism of core-collapse supernovae, its rate as the Universe evolves, and the physics of binary stars (1, 2). An unbiased census of neutron star and black hole masses is required to understand these interconnected areas. However, our knowledge of neutron star and black hole demography is limited because mass measurements are obtained almost exclusively for pulsar and accreting binary systems selected from radio, x-ray, and gamma-ray surveys (35). While gravitational microlensing has the potential to reveal compact object mass distributions (6), individual systems are difficult to characterize. The detections of merging black hole and neutron star binaries by gravitational wave experiments (7, 8) provide compact object masses, but these merging systems are an intrinsically biased subset of the parent population.

Studies of compact object populations are complemented by those of massive star binary systems (9), whose more massive “primary” components ultimately produce neutron stars and black holes [for stars >10M (solar masses)]. These studies reveal a broad distribution of secondary masses and orbital periods, implying that many massive stars have low-mass, long-lived companions. Quiescent noninteracting black hole stellar binaries have not been found in radial velocity searches, although the existence of such systems has been discussed for decades (10, 11). The only known candidate formed by dynamical scattering processes in a dense globular cluster (12), so it did not form as an isolated binary in the more typical Galactic field environment. Although subject to their own selection biases, a sample of Galactic binary star systems with black hole or neutron star companions would inform binary evolution models, which are currently limited by comparison to pulsar binaries and interacting or merging systems.

We searched for stellar binaries with massive unseen companions in data from the Apache Point Observatory Galactic Evolution Experiment (APOGEE) (13). APOGEE provides multi-epoch near-infrared spectroscopy for >105 stars in the Milky Way. These observations provide stellar elemental abundances and can also reveal radial velocity variations indicative of binary orbital motion (14). We searched for systems with large apparent accelerations—the difference in radial velocity divided by the difference in time between two epochs. Systems were ranked by an estimate of the binary mass function given the irregular timing of the APOGEE observation epochs.

Although the radial velocity measurements from APOGEE can immediately indicate the presence of a binary, the mass of the companion is not determined, because the orbital period, inclination, and eccentricity are unknown. To constrain the orbital periods of the ~200 APOGEE sources with the highest accelerations, we searched for periodic variations in photometric data from the All-Sky Automated Survey for Supernovae (ASAS-SN) (15, 16) for evidence of transits, ellipsoidal variations, or star spots. This process identified the giant star 2MASS J05215658+4359220 (hereafter J05215658), which exhibits an acceleration of ≃2.9 km s−1 day−1 and periodic photometric variability with a period of ~82.2 ± 2.5 days (Fig. 1 and table S2). This system lies in the constellation Auriga, near the outer Galactic plane, with Galactic coordinates (l, b) = (164.774°, 4.184°).

Fig. 1 Multi-epoch ASAS-SN light curves.

V-band ASAS-SN light curves for J05215658 over four observing seasons (A to D), phased to the orbital period of 83.2 days and duplicated over two periods. Blue points are the observed data with 1σ error bars. Red points are the running median of 20 data points. The same data before phasing are shown in fig. S1.

Previous analysis of J05215658 determined an effective stellar temperature Teff ≃ 4480 ± 62 K, a surface gravitational acceleration log[g/(cm s−2)] ≃ 2.59 ± 0.06, and a near-Solar value for the carbon-to-nitrogen abundance ratio (17). Our analysis of the APOGEE spectrum yields a projected rotational velocity of v·sin irot ≃ 14.1 ± 0.6 km s−1 (18), where irot is the inclination angle of the rotation axis projected onto the plane of the sky. We obtained additional optical spectra with the Tillinghast Reflector Echelle Spectrograph (TRES), which indicate a consistent effective temperature but lower log g ≃ 2.35 ± 0.14, and higher v·sin irot ≃ 16.8 ± 0.6 km s−1. We adopt the TRES log g and the APOGEE v·sin irot in our analysis (18).

We further constrained the system using radial velocity and multiband photometric follow-up (Fig. 2). The photometric variability amplitude increases from the redder to bluer bands. The shape, character, and phasing of the light curve are inconsistent with stellar pulsations or ellipsoidal variations but are typical of the class of spotted K-type giants such as HD 1833, V1192 Orionis, and KU Pegasi (19, 20). Binary systems with periods less than ~150 days often have low eccentricities, implying rapid tidal circularization (21, 22). The change in the shape of the light curve over time (Fig. 1) is likely due to star spot evolution.

Fig. 2 Multicolor light curves and TRES radial velocities.

(A) The B-band (lowest, triangles), V-band (pentagons), r-band (circles), and i-band (highest, squares) light curves with arbitrary zero-point offsets applied for display. (B) The TRES radial velocity (RV) measurements as a function of heliocentric Julian date (HJD). Maximum blueshift (negative RV) occurs near the photometric maximum in all bands, and maximum redshift occurs after photometric minimum, near the shoulder or plateau in the light curve at HJD − 2,450,000 ≃ 8080. Figure 1 shows the evolution of the phased multi-epoch V-band ASAS-SN light curve for comparison.

Figure 2B shows the TRES radial velocity measurements. The APOGEE and TRES spectra exhibit only a single set of absorption lines, i.e., a single-lined spectroscopic binary. The system has a nearly circular orbit with orbital period Porb ≃ 83.2 ± 0.06 days, radial velocity semi-amplitude K ≃ 44.6 ± 0.1 km s−1, and eccentricity e ≃ 0.0048 ± 0.0026. The mass function isf(M)MCO3sin3iorb(Mgiant+MCO)2=K3Porb2πG(1e2)3/20.766±0.006M(1)where G is the gravitational constant, MCO is the compact object companion mass, iorb is the orbital inclination, and M is the mass of the Sun. Figure 3 shows allowed values of MCO as a function of the mass of the giant star Mgiant for several values of sin iorb. For Mgiant1Mand sin iorb = 1.0, the minimum possible companion mass is MCO1.8 M. The observed spectral energy distribution (SED) is inconsistent with a stellar companion of such high mass (18) (fig. S8). We conclude that the unseen companion is either a massive neutron star or a black hole. Follow-up x-ray observations yield a tight upper limit on emission from the system (18).

Fig. 3 Compact object mass constraints.

Solutions to the mass function (solid black lines) for the compact object’s mass MCO as a function of the giant’s mass Mgiant at five values of the orbital inclination from sin i = 1.0 to 0.6. The vertical band labeled L,Teff denotes the best-fitting range of Mgiant when the giant’s measured L,Teff, and log g are matched to theoretical single-star evolutionary models. The regions enclosed by the thick and thin dashed lines show the resulting 1σ and 2σ mass ranges, respectively. The best-fitting value is denoted with the empty circle. The vertical band labeled [C/N] denotes the range of Mgiant implied by the observed carbon to nitrogen ratio and the mean locus of the observed [C/N] − Mgiant correlation for giant stars (18), although we regard this solution as unlikely (see text). The horizontal bands denote the largest observed neutron star mass (lowest), a theoretical maximum neutron star mass (middle), and a theoretical minimum black hole mass (top).

To determine the nature of the compact object companion we must constrain the mass of the giant and the orbital inclination. We can estimate minimum values of the giant radius and bolometric luminosity using the star’s projected rotation velocity. The low orbital eccentricity and the correspondence between the orbital and photometric periods imply that the system is tidally circularized and synchronized. We therefore adopt the hypothesis that the giant’s rotational period is equal to the binary orbital period and that they have the same inclination (irot = iorb = i). This yields a minimum radius of R23±1R/sini, a minimum luminosity L=4πR2σSBTeff4210±20L/sin2i for Teff ≃ 4500 K, and a minimum distance D[L/(4πF)]1/22.45±0.1 kpc/sini, where R is the radius of the Sun, L is the luminosity of the Sun, σSB is the Stefan-Boltzmann constant, and F is the bolometric (all-wavelength) flux measured from the SED (18). Combining the minimum giant radius with the TRES log g ≃ 2.35 ± 0.14 gives an estimate for the giant mass of Mgiantlogg=gR2/G4.41.5+2.2M/sin2i, implying a minimum companion mass of MCO2.9 M.

Alternatively, R and L can be determined directly from the measured distance and flux. The parallax of this system measured by the Gaia satellite is 0.272 ± 0.049 milliarcseconds (mas) (23), corresponding to a nominal distance of 3.7 kpc, but there are systematic offsets in the Gaia parallaxes that are a function of both sky position and brightness (23). Additionally, the companion will induce astrometric binary motion of the giant that is not accounted for in Gaia’s parallax measurement (23). Given f(M) and P, the ratio of the binary angular motion to the parallax is 0.34/sin i, which could bias the measured parallax. Applying a zero-point offset and an additional systematic uncertainty, and accounting for the phased binary motion with the geometry and timing of the observations by Gaia for J05215658 using Monte Carlo simulations for an arbitrary orbital sky projection (18), we find a parallax of π0.3220.074+0.086 mas (1σ confidence interval) for all sin i > 0, corresponding to a distance D3.110.66+0.93 kpc. The observed flux then gives L331127+231 L and R306+9 R, consistent with the estimates from v·sin i. Combining the Gaia lower bound of R24 R with the TRES log g gives Mgiantlogg4.8M and a value of MCO in the black hole regime (Fig. 3). Direct comparison between R306+9 derived from the parallax and R23±1R/sini derived from v·sin i suggests that sin i ≃ 0.8 ± 0.2. The 2σ upper limit on the Gaia parallax of 0.486 mas for sin i > 0.6, gives lower limits of L150 L and R20 R (18). The TRES log g = 2.35 ± 0.14 then gives Mgiantlogg3.20.9+1.2 M, implying a lower limit on the companion mass of MCO2.5 M.

The giant mass can also be estimated by comparing its properties to single-star evolutionary models, with the caveats that (i) strong binary interaction likely occurred in the history of the system, and (ii) rapidly rotating, spotted giants like J05215658 are observed to be redder than expected for a given luminosity, underestimating the true dynamical mass (24). Nevertheless, we searched for the best-fitting model over a range of stellar metallicity and with the constraint log g = 2.35 ± 0.14, and the other parameters (L, R, and Teff) inferred from the parallax and SED. We found it difficult to simultaneously match the temperature and surface gravity, which is a known systematic problem for models of giant stars (25). The best matches were for solar metallicity models. Combining all models, the joint best-fitting mass is Mgiant3.21.0+1.0 M (2σ), shown in Fig. 3. The model fitting is driven to a giant mass of 2 to 4 M primarily by the L and R inferred from the parallax and SED. Given the APOGEE measurement of v·sin i, the best-fitting mass implies sini0.970.12+0.03. Solving the mass function f(M) for this range of Mgiant and sin i yields MCO3.30.7+2.8 M (2σ; also shown in Fig. 3). While a lower assumed value of v·sin i allows for a lower mass giant, it also leads to a smaller sin i that drives MCO upwards. Similarly, if we assume a lower log g, or impose no constraint on log g, we obtain best-fitting giant masses at the low end of the range denoted in Fig. 3 (Mgiant2.22.5 M), but with compact object companion masses of 2.9 to 4.0 M.

All of our determinations consistently require Mgiant2 to 4 M. Stars in this mass range are rare in APOGEE (18). However, J05215658 would be unusual even among APOGEE’s massive giants because it has a near-solar carbon-to-nitrogen abundance ratio. Giants exhibit a strong correlation between this abundance ratio and mass that would imply a low value of Mgiant1.0 M for J05215658. We also show this “low-mass giant” possibility in Fig. 3 but consider it highly unlikely, because it is inconsistent with the mass determination from all other methods, and because some higher-mass giants with solar carbon-to-nitrogen abundance ratios do exist in the APOGEE sample (18).

We conclude that J05215658 likely consists of a 3.21.0+1.0 M giant star and a noninteracting low-mass black hole companion with MCO3.30.7+2.8 M (the 2σ range in Fig. 3). This range of compact object mass falls in the so-called mass gap between neutron stars and black holes (5). It is above the highest neutron star masses thus far observed [2.01±0.04 M (26) and 2.140.09+0.10 M (27)], and the uncertainty range nearly spans from the predicted theoretical maximum neutron star mass [2.5 M (28)] to the lowest well-measured black hole masses [5 to 6 M (4, 5)]. Whereas some models of black hole formation indicate a lower mass limit of 4 M (1, 29), others predict a wide range of masses throughout the mass gap (30, 31). J05215658 joins a handful of other known binaries that may host compact objects in this mass range, including the x-ray binaries GX 339-4 [2.3 to 9.5 M(32)] and 4U 1543-47 [2.7 to 7.5 M (33)].

Supplementary Materials

Materials and Methods

Figs. S1 to S9

Tables S1 to S8

References (3489)

References and Notes

  1. Additional data, materials, and methods are provided as supplementary materials.
Acknowledgments: We thank J. Choi for making MIST models available and C. Jordi and C. Fabricius for discussions. We thank the Ohio State University College of Arts and Sciences Technology Services for setting up the ASAS-SN Sky Patrol light curve server, which was critically useful during this work. T.A.T. thanks J. Zinn, T. Sukhbold, S. Gaudi, O. Pejcha, K. Stassun, M. Pinsonneault, A. Brown, C. Gammie, E. Rossi, J. Fuller, S. Phinney, A.-C. Eilers, D. Hogg, K. Cunha, and R. Poleski for discussions, and K. A. Byram for encouragement and support. Full facility acknowledgments are provided in the supplementary materials. Funding: T.A.T. acknowledges support from Scialog Scholar grant 24216 from the Research Corporation; a Simons Foundation Fellowship; and an IBM Einstein Fellowship from the Institute for Advanced Study, Princeton. C.B. acknowledges support from PHY 14-30152: Physics Frontier Center/JINA Center for the Evolution of the Elements (JINA-CEE), awarded by the National Science Foundation. C.S.K. and K.Z.S. are supported in part by NSF grants AST-1515927 and AST-1515876. J.T. acknowledges support from NASA Hubble Fellowship grant 51424 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. Author contributions: T.A.T. led the project, conceived of the search strategy, led the analysis, and led the writing of the text. C.S.K. analyzed the SED and the ASAS-SN photometry and fitted the observational data with evolutionary models. K.Z.S. analyzed the Post and ASAS-SN photometry and interpreted the system. R.S.P. provided the Post photometry. C.B. provided APOGEE RV analysis and interpretation of the system. T.J. carried out the time-series analysis of the ASAS-SN photometry. D.W.L., A.B., G.A.E., P.B., and M.L.C. obtained the TRES data and carried out the RV analysis. J.T. provided the rotation measurement from the APOGEE spectrum. L.L. provided the Gaia parallax bias analysis. J.A.J. consulted on the APOGEE spectra. T.W.-S.H. and K.A. obtained and analyzed the Swift data. K.C. participated in preparing the text and discussions of the APOGEE RV data. Competing interests: There are no competing interests to declare. Data and materials availability: The ASAS-SN light curve data are available at The APOGEE observations, including all individual spectra, the combined spectrum, and analysis results are available at Photometry for J05215658 is listed in table S8. X-ray and ultraviolet observations from the Neil Gehrels Swift Observatory (18) are available at under target id 10442. The code used to calculate the parallax bias in the Gaia observations is available at
View Abstract

Stay Connected to Science

Navigate This Article