<i>Gaia</i>Data Release 1

Leeuwen, F. van; Evans, D. W.; Angeli, F. De; Jordi, C.; Busso, G.; Cacciari, C.; Riello, M.; Pancino, E.; Altavilla, G.; Brown, A. G. A.; Burgess, P.; Carrasco, J. M.; Cocozza, G.; Cowell, S.; Davidson, M.; Luise, F. De; Fabricius, C.; Galleti, S.; Gilmore, G.; Giuffrida, G.; Hambly, N. C.; Harrison, D. L.; Hodgkin, S. T.; Holland, G.; MacDonald, Ian G.; Marinoni, S.; Montegrffo, P.; Osborne, P.; Ragaini, S.; Richards, P. J.; Rowell, N.; Voss, H.; Walton, N. A.; Weiler, Michael; Castellani, M.; Delgado, A.; Høg, E.; Leeuwen, M. van; Millar, N. R.; Pagani, C.; Piersimoni, A. M.; Pulone, L.; Rixon, G.; Suess, F. F.; Wyrzykowski, Ł.; Yoldaş, A.; Alecu, A.; Allan, P. M.; Balaguer-Núñez, L.; Barstow, M. A.; Bellazzini, M.; Belokurov, V.; Blagorodnova, N.; Bonfigli, M.; Bragaglia, A.; Brown, S.; Bunclark, P.; Buonanno, R.; Burgon, Ross; Campbell, H.; Collins, R. S.; Cross, N. J. G.; Ducourant, C.; Elteren, A. van; Evans, N. W.; Federici, L.; Fernández-Hernández, J.; Figueras, F.; Fraser, M.; Fyfe, D.; Gebran, M.; Heyrovsky, A.; Holl, B.; Holland, Andrew D.; Iannicola, G.; Irwin, M. J.; Koposov, S. E.; Krone-Martins, A.; Mann, R. G.; Marrese, P. M.; Masana, E.; Munari, U.; Ortiz, P.; Ouzounis, A.; Peltzer, C.; Portell, J.; Read, A. M.; Terrett, D. L.; Torra, J.; Trager, S. C.; Troisi, L.; Valentini, G.; Vallenari, A.; Wevers, T.

doi:10.1051/0004-6361/201630064

Cited by 50 publications

(20 citation statements)

References 12 publications

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“…Depending on both the neutron star mass and the inclination angle of the binary orbit, we expect a semi-major axis a * in the range 70-430 microarcseconds. This range is well within the final capabilities of Gaia given that LS 2883 has G-magnitude 9.5 (Gaia Collaboration et al 2016b;Carrasco et al 2016;Evans et al 2017;van Leeuwen et al 2017). More importantly, the combination of the VLBI-measured orbit of the pulsar with the Gaia-measured orbit of the companion could eventually enable us to solve for the individual component masses, providing an accurate neutron star mass measurement from the combination of pulsar timing with high-precision optical and radio astrometry.…”

Section: Component Massessupporting

confidence: 71%

“…With the caveat that the spin-down luminosity is inherently somewhat uncertain due to the unknown moment of inertia of the pulsar , our results would therefore appear to favour gamma-ray production mechanisms involving Doppler boosting (e.g. Dubus et al 2010;Tam et al 2011;Kong et al 2012). Finally, our new distance estimate can be used to update the inferred optical luminosity for the stellar companion, LS 2883 (Negueruela et al 2011), to L * = 2.9 +1.0 −0.6 × 10 38 erg s −1 .…”

Section: Discussionmentioning

confidence: 82%

“…Such inverse Compton emission depends on the scattering angle between the electrons and the stellar photons, and would thus be subject to relativistic aberration and boosting (Dubus, Cerutti & Henri 2010). Alternatively, it has been proposed that the GeV flares could be attributed to Doppler-boosted synchrotron emission in the bow-shock tail formed as the shocked pulsar wind is collimated by the stellar wind (Dubus, Cerutti & Henri 2010;Kong, Cheng & Huang 2012). Regardless of the exact mechanism, the observed emission will depend on the orbital parameters of the system, in particular the inclination to the line of sight.…”

mentioning

confidence: 99%

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The geometric distance and binary orbit of PSR B1259–63

Miller-Jones

Deller

Shannon

et al. 2018

Monthly Notices of the Royal Astronomical Society

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The pulsar/massive star binary system PSR B1259−63/LS 2883 is one of the beststudied gamma-ray binaries, a class of systems whose bright gamma-ray flaring can provide important insights into high-energy physics. Using the Australian Long Baseline Array we have conducted very long baseline interferometric observations of PSR B1259−63 over 4.4 years, fully sampling the 3.4-year orbital period. From our measured parallax of 0.38 ± 0.05 mas we use a Bayesian approach to infer a distance of 2.6 +0.4 −0.3 kpc. We find that the binary orbit is viewed at an angle of 154 ± 3 • to the line of sight, implying that the pulsar moves clockwise around its orbit as viewed on the sky. Taking our findings together with previous results from pulsar timing observations, all seven orbital elements for the system are now fully determined. We use our measurement of the inclination angle to constrain the mass of the stellar companion to lie in the range 15-31M . Our measured distance and proper motion are consistent with the system having originated in the Cen OB1 association and receiving a modest natal kick, causing it to have moved ∼ 8 pc from its birthplace over the past ∼ 3 × 10 5 years. The orientation of the orbit on the plane of the sky matches the direction of motion of the X-ray synchrotron-emitting knot observed by the Chandra X-ray Observatory to be moving away from the system.

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Section: Component Massessupporting

confidence: 71%

Section: Discussionmentioning

confidence: 82%

mentioning

confidence: 99%

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The geometric distance and binary orbit of PSR B1259–63

Miller-Jones

Deller

Shannon

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…We used the Gaia DR1 source catalog (Gaia Collaboration et al 2016a,b) as both an astrometric (Lindegren et al 2016) and photometric (van Leeuwen et al 2017) reference catalog. DR1 was used instead of DR2 because our analysis began prior to DR2's release.…”

Section: K2 Image Subtraction Reduction and Variable Searchmentioning

confidence: 99%

Ultralow-amplitude RR Lyrae Stars in M4

Wallace

Hartman

Bakos

et al. 2019

ApJL

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We report evidence for a new class of variable star, which we dub millimagnitude RR Lyrae (mmRR). From K2 observations of the globular cluster M4, we find that out of 24 horizontal branch stars not previously known to be RR Lyrae variables, two show photometric variability with periods and shapes consistent with those of first overtone RR Lyrae variables. The variability of these two stars, however, have amplitudes of only one part in a thousand, which is ∼200 times smaller than for any RR Lyrae variable in the cluster, and much smaller than any known RR Lyrae variable generally. The periods and amplitudes are: 0.33190704 d with 1.0 mmag amplitude and 0.31673414 d with 0.3 mmag amplitude. The stars lie just outside the instability strip, one blueward and one redward. The star redward of the instability strip also exhibits significant multi-periodic variability at lower frequencies. We examine potential blend scenarios and argue that they are all either physically implausible or highly improbable. Stars such as these are likely to shed valuable light on many aspects of stellar physics, including the mechanism(s) that set amplitudes of RR Lyrae variables.

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“…These cases are slightly more challenging to detect, but still well within the capabilities of modern facilities (e.g. GAIA; van Leeuwen et al 2017).…”

Section: "Normal" Binary Systemsmentioning

confidence: 99%

Physics of Eclipsing Binaries. IV. The Impact of Interstellar Extinction on the Light Curves of Eclipsing Binaries

Jones

Conroy

Horvat

et al. 2020

ApJS

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Traditionally, the effects of interstellar extinction on binary star light curves have been treated as a uniform reduction in the observed brightness of the system that is independent of orbital phase. However, unless the orbital plane of the system coincides with the plane of the sky, or if the two stars are completely identical and present with minimal mutual irradiation and tidal/rotational distortions, then this is unlikely to be an accurate representation of the effect of interstellar extinction. Here, we present an updated treatment of interstellar extinction as incorporated in the PHOEBE 2.2 release (publicly available from http://phoebe-project.org) and assess the importance of using such an approach in the modeling of different types of binary systems. We also present the incorporation of PHOENIX model atmospheres into the PHOEBE 2.2 release, providing increased fidelity on computed observables down to lower temperatures than previously available. The importance of these new code developments is then highlighted via an extincted toy model of the eclipsing white-dwarf-subdwarf binary SDSS J235524.29+044855.7 -demonstrating that, in the age of LSST as well as complementary space-based photometric missions, a proper accounting for extinction and as well as the use of realistic model atmospheres will be essential in deriving accurate binary parameters.

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GaiaData Release 1

Cited by 50 publications

References 12 publications

The geometric distance and binary orbit of PSR B1259–63

The geometric distance and binary orbit of PSR B1259–63

Ultralow-amplitude RR Lyrae Stars in M4

Physics of Eclipsing Binaries. IV. The Impact of Interstellar Extinction on the Light Curves of Eclipsing Binaries

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