Discovery of an OB runaway star inside SNR S147

Dinçel, B.; Neuhäuser, R.; Yerli, Sinan Kaan; Ankay, A.; Tetzlaff, N.; Torres, Guillermo; Mugrauer, M.

doi:10.1093/mnras/stv124

Cited by 48 publications

(89 citation statements)

References 66 publications

(72 reference statements)

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“…That the binary SN ejection mechanism for producing runaway stars works, can also be shown inside SN remnants: E.g., ∼ 30 kyr ago, both a pulsar and a runaway star were near the center of the SN remnant S147 (Dinçel et al 2015); the distance of SN and SNR was estimated from the spectrophotometric distance towards the runaway star HD 37424 (1.3 ± 0.1 kpc), confirmed by Gaia DR2 (1.47 ± 0.15 kpc). Most recently numerical simulations of the evolution of binary stars with one supernova progenitor were performed by Zapartas et al (2017b) and Renzo et al (2019), who could show that about one third of original binaries should produce at least one ejected runaway star.…”

Section: Introduction: 60 Fe On Earthmentioning

confidence: 86%

A nearby recent supernova that ejected the runaway star ζ Oph, the pulsar PSR B1706−16, and 60Fe found on Earth

Neuhäuser

Gießler

Hambaryan

2019

Monthly Notices of the Royal Astronomical Society

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The detection of ∼ 1.5−3.2 Myr old 60 Fe on Earth indicates recent nearby core-collapse supernovae. For supernovae in multiple stars, the primary stars may become neutron stars, while former companions may become unbound and become runaway stars. We wrote software for tracing back the space motion of runaway and neutron stars to young associations of massive stars. We apply it here to the nearby young Scorpius-Centaurus-Lupus groups, all known runaway stars possibly coming from there, and all 400 neutron stars with known transverse velocity. We find kinematic evidence that the runaway ζ Oph and the radio pulsar PSR B1706-16 were released by a supernova in a binary 1.78 ± 0.21 Myr ago at 107 ± 4 pc distance (for pulsar radial velocity 260 ± 43 km/s); association age and flight time determine the progenitor mass (16-18 M ), which can constrain supernova nucleosynthesis yields and 60 Fe uptake on Earth. In addition, we notice that the only high-mass X-ray binary in Scorpius-Centaurus-Lupus (1H11255-567 with µ 1 and µ 2 Cru) may include a neutron star formed in another SN, up to ∼ 1.8 Myr ago at 89 − 112 pc, i.e. also yielding 60 Fe detectable on Earth. Our scenario links 60 Fe found on Earth to one or two individual supernovae in multiple stars.

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Section: Introduction: 60 Fe On Earthmentioning

confidence: 86%

A nearby recent supernova that ejected the runaway star ζ Oph, the pulsar PSR B1706−16, and 60Fe found on Earth

Neuhäuser

Gießler

Hambaryan

2019

Monthly Notices of the Royal Astronomical Society

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“…None of these systems have been investigated in any quantitative detail. Dinçel et al (2015) identify a good candidate in the ∼ 3 × 10 4 year old SNR S147 containing PSR J0538+2817 and argue that it was also likely to have been an interacting binary. Considerably more effort has been devoted to searching for single degenerate companions to Type Ia SN (e.g., Schweizer & Middleditch 1980Ruiz-Lapuente et al 2004, Ihara et al 2007, González Hernández et al 2012, Schaefer & Pagnotta 2012.…”

Section: Introductionmentioning

confidence: 88%

Cas A and the Crab were not stellar binaries at death

Kochanek¹

2017

Monthly Notices of the Royal Astronomical Society

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The majority of massive stars are in binaries, which implies that many core collapse supernovae (ccSNe) should be binaries at the time of the explosion. Here we show that the three most recent, local (visual) SNe (the Crab, Cas A and SN 1987A) were not binaries, with limits on the initial mass ratios of q = M 2 /M 1 < ∼ 0.1. No quantitative limits have previously been set for Cas A and the Crab, while for SN 1987A we merely updated existing limits in view of new estimates of the dust content. The lack of stellar companions to these three ccSNe implies a 90% confidence upper limit on the q > ∼ 0.1 binary fraction at death of f b < 44%. In a passively evolving binary model (meaning no binary interactions), with a flat mass ratio distribution and a Salpeter IMF, the resulting 90% confidence upper limit on the initial binary fraction of F < 63% is in considerable tension with observed massive binary statistics. Allowing a significant fraction f M ≃ 25% of stellar binaries to merge reduces the tension, with−1 % ≃ 81%, but allowing for the significant fraction in higher order systems (triples, etc.) reintroduces the tension. That Cas A was not a stellar binary at death also shows that a massive binary companion is not necessary for producing a Type IIb SNe. Much larger surveys for binary companions to Galactic SNe will become feasible with the release of the full Gaia proper motion and parallax catalogs, providing a powerful probe of the statistics of such binaries and their role in massive star evolution, neutron star velocity distributions and runaway stars.

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“…This SNR has its geometrical center at (l, b) = (180.17, b = −1.81) with a diameter of about 180 arcmin (Green 2009). Its suggested distance ranges from 0.6 to 1.9 kpc (see Table 1 from Dinçel et al 2015). For its related pulsar PSRJ0538+2817 Ng et al (2007 estimated a distance of 1.47…”

Section: Three-dimensional Extinction Map In the Anticenter Directionmentioning

confidence: 98%

First detection of the field star overdensity in the Perseus arm

Monguió

Grosbøl

Figueras

2015

A&A

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Aims. The main goal of this study is to detect the stellar overdensity associated with the Perseus arm in the anticenter direction. Methods. We used the physical parameters derived from Strömgren photometric data to compute the surface density distribution as a function of galactocentric distance for different samples of intermediate young stars. The radial distribution of the interstellar absorption has also been derived. Results. We detected the Perseus arm stellar overdensity at 1.6 ± 0.2 kpc from the Sun with a significance of 4-5σ and a surface density amplitude of around 10%, slightly depending on the sample used. Values for the radial scale length of the Galactic disk have been simultaneously fitted obtaining values in the range [2.9,3.5] kpc for the population of the B4-A1 stars. Moreover, the interstellar visual absorption distribution is congruent with a dust layer in front of the Perseus arm. Conclusions. This is the first time that the presence of the Perseus arm stellar overdensity has been detected through individual star counts, and its location matches a variation in the dust distribution. The offset between the dust lane and the overdensity indicates that the Perseus arm is placed inside the co-rotation radius of the Milky Way spiral pattern.

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Discovery of an OB runaway star inside SNR S147

Cited by 48 publications

References 66 publications

A nearby recent supernova that ejected the runaway star ζ Oph, the pulsar PSR B1706−16, and 60Fe found on Earth

A nearby recent supernova that ejected the runaway star ζ Oph, the pulsar PSR B1706−16, and 60Fe found on Earth

Cas A and the Crab were not stellar binaries at death

First detection of the field star overdensity in the Perseus arm

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