Weighing the Darkness: Astrometric Mass Measurement of Hidden Stellar Companions Using Gaia

Andrews, Jeff J.; Breivik, Katelyn; Chatterjee, Sourav

doi:10.3847/1538-4357/ab441f

Cited by 68 publications

(65 citation statements)

References 113 publications

(141 reference statements)

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“…Some of these binaries may be observable by Gaia. Andrews et al (2019) postulate that Gaia can detect and measure the properties of hidden wide binaries with WD and NS components using astrometric observations. The comparison of NS-WD observations to final orbital parameters from our calculations might help in understanding which binaries have undergone a super-Eddington mass-transfer phase in the past and could have been observed as ULXs, as well as constrain binary evolution physics such as the accretion efficiency.…”

Section: Likelihoodmentioning

confidence: 99%

The origin of pulsating ultra-luminous X-ray sources: Low- and intermediate-mass X-ray binaries containing neutron star accretors

Misra

Fragos

Tauris

et al. 2020

A&A

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Context. Ultra-luminous X-ray sources (ULXs) are those X-ray sources located away from the centre of their host galaxy with luminosities exceeding the Eddington limit of a stellar-mass black hole (LX > 1039 erg s−1). Observed X-ray variability suggests that ULXs are X-ray binary systems. The discovery of X-ray pulsations in some of these objects (e.g. M82 X-2) suggests that a certain fraction of the ULX population may have a neutron star as the accretor. Aims. We present systematic modelling of low- and intermediate-mass X-ray binaries (LMXBs and IMXBs; donor-star mass range 0.92–8.0 M⊙ and neutron-star accretors) to explain the formation of this sub-population of ULXs. Methods. Using MESA, we explored the allowed initial parameter space of binary systems consisting of a neutron star and a low- or intermediate-mass donor star that could explain the observed properties of ULXs. These donors are transferring mass at super-Eddington rates while the accretion is limited locally in the accretion disc by the Eddington limit. Thus, our simulations take into account beaming effects and also include stellar rotation, tides, general angular momentum losses, and a detailed and self-consistent calculation of the mass-transfer rate. Results. Exploring the initial parameters that lead to the formation of neutron-star ULXs, we study the conditions that lead to dynamical stability of these systems, which depends strongly on the response of the donor star to mass loss. Using two values for the initial neutron star mass (1.3 M⊙ and 2.0 M⊙), we present two sets of mass-transfer calculation grids for comparison with observations of NS ULXs. We find that LMXBs/IMXBs can produce NS-ULXs with typical time-averaged isotropic-equivalent X-ray luminosities of between 1039 and 1041 erg s−1 on a timescale of up to ∼1.0 Myr for the lower luminosities. Finally, we estimate their likelihood of detection, the types of white-dwarf remnants left behind by the donors, and the total amount of mass accreted by the neutron stars. Conclusions. We show that observed super-Eddington luminosities can be achieved in LMXBs/IMXBs undergoing non-conservative mass transfer while assuming geometrical beaming. We also compare our results to the observed pulsating ULXs and infer their initial parameters. Our results suggest that a large subset of the observed pulsating ULX population can be explained by LMXBs/IMXBs in a super-Eddington mass-transfer phase.

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Section: Likelihoodmentioning

confidence: 99%

The origin of pulsating ultra-luminous X-ray sources: Low- and intermediate-mass X-ray binaries containing neutron star accretors

Misra

Fragos

Tauris

et al. 2020

A&A

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“…In addition, Gaia can characterize orbits with periods ranging from 10 days to thousands of days. Using 0.1 mas as the size of the primary star's orbit resolvable by Gaia (Andrews, Breivik & Chatterjee 2019) and a distance of 37 pc, Gaia should be able to easily resolve the astrometric orbit for WD 1418−088 within the next several years. Figure 9 shows the radial velocity measurements and the Lomb-Scargle periodogram for the single-lined binary WD 1447−190.…”

Section: Wd 1418−088mentioning

confidence: 99%

Two new double-lined spectroscopic binary white dwarfs

Kilic

Bédard

Bergeron

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present radial velocity observations of four binary white dwarf candidates identified through their over-luminosity. We identify two new double-lined spectroscopic binary systems, WD 0311−649 and WD 1606+422, and constrain their orbital parameters. WD 0311−649 is a 17.7 h period system with a mass ratio of 1.44 ± 0.06 and WD 1606+422 is a 20.1 h period system with a mass ratio of 1.33 ± 0.03. An additional object, WD 1447−190, is a 43 h period single-lined white dwarf binary, whereas WD 1418−088 does not show any significant velocity variations over timescales ranging from minutes to decades. We present an overview of the 14 over-luminous white dwarfs that were identified by Bédard et al., and find the fraction of double-and single-lined systems to be both 31%. However, an additional 31% of these overluminous white dwarfs do not show any significant radial velocity variations. We demonstrate that these must be in long-period binaries that may be resolved by Gaia astrometry. We also discuss the over-abundance of single low-mass white dwarfs identified in the SPY survey, and suggest that some of those systems are also likely long period binary systems of more massive white dwarfs.

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“…many tens of thousands of [brown dwarf] desert occupants might be expected'. The prediction of several tens of BDs mentioned in Andrews et al (2019) was mainly related to their goal of tightly constraining the mass function, which requires more signal than that for a detection or even an orbital fit. They also examined predictions of unseen companions using simulated Gaia radial velocities.…”

Section: Introductionmentioning

confidence: 99%

Gaia predicted brown dwarf detection rates around FGK stars in astrometry, radial velocity, and photometric transits

Holl,

Perryman,

Lindegren

et al. 2021

Preprint

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Context. After more than two decades of relevant radial velocity surveys, the current sample of known brown dwarfs (BDs) around FGK-stars is only of the order of a hundred, limiting our understanding of their occurrence rate, properties, and formation. The ongoing ESA mission Gaia has already collected more than its nominal 5 years of mission data, and is expected to operate for up to 10 years in total. Its exquisite astrometric precision allows for the detection of (unseen) companions down to the Jupiter-mass level, hence allowing for the efficient detection of large numbers of brown dwarfs. Additionally, its low-accuracy multi-epoch radial velocity measurements for G RVS < 12 can provide additional detections or constraints for the more massive BDs, while a further small sample will have detectable transits in the Gaia photometry. Aims. Using detailed simulations, we provide an assessment of the number of brown dwarfs that could be discovered by Gaia astrometry, radial velocity, and photometric transits around main sequence (V) and subgiants (IV) FGK host stars for the nominal 5-yr and extended 10-yr mission. Methods. Using a robust ∆χ 2 statistic we analyse the BD companion detectability from the Besançon Galaxy population synthesis model for G = 10.5 − 17.5 mag, complemented by Gaia DR2 data for G < 10.5, using the latest Gaia performance and scanning law, and literature-based BD-parameter distributions. Results. We report here only reliable detection numbers with ∆χ 2 > 50 for a 5-year mission and between square brackets for a 10-year mission. For astrometry alone we expect 28 000-42 000 [45 000-55 000] detections out to several hundred pc [up to more than a kiloparsec]. The majority of these have G ∼ 14 − 15 [14 − 16] and periods above 200 d, extending up to the longest simulated periods of 5 year. Gaia radial velocity time series for G RVS < 12 (G 12.7), should allow the detection of 830-1100 [1500-1900] BDs, most having orbital periods <10 days, and being amongst the most massive BDs (55 − 80M J ), though several tens will extend down to the 'desert' and lowest BD masses. Systems with at least three photometric transits having S/N>3 are expected for 720-1100 [1400-2300] BDs, averaging at 4-5 [5-6] transits per source. The combination of astrometric and radial velocity detections should yield some 370-410 [870-950] detections. BDs have both transit and radial velocity detections, while both transits and astrometric detection will lead to a meagre 1-3 [4-6] detection(s). Conclusions. Though above numbers have ±50% uncertainty due to the uncertain occurrence rate and period distribution of BDs around FGK host stars, detections of BDs with Gaia will number in the tens-of-thousands, enlarging the current BD sample by at least two orders of magnitude and thus allowing to investigate the BD fraction and orbital architectures as a function of host stellar parameters in greater detail than every before.

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Weighing the Darkness: Astrometric Mass Measurement of Hidden Stellar Companions Using Gaia

Cited by 68 publications

References 113 publications

The origin of pulsating ultra-luminous X-ray sources: Low- and intermediate-mass X-ray binaries containing neutron star accretors

The origin of pulsating ultra-luminous X-ray sources: Low- and intermediate-mass X-ray binaries containing neutron star accretors

Two new double-lined spectroscopic binary white dwarfs

Gaia predicted brown dwarf detection rates around FGK stars in astrometry, radial velocity, and photometric transits

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