The Distance of the γ-Ray Binary 1FGL J1018.6–5856

Napoli, Vanessa J.; McSwain, M. Virginia; Boyer, A. N. Marsh; Roettenbacher, Rachael M.

doi:10.1086/662692

Cited by 16 publications

(13 citation statements)

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“…The system is composed of an O6 V((f)) star and a compact object that orbits it every 16.544 ± 0.008 d (Napoli et al 2011;Fermi LAT Collaboration et al 2012;An et al 2015). Assuming a total mass for the system of ≈ 29 M (Williams et al 2015) we estimate a semi-major axis of the orbit of ∼ 0.4 au.…”

Section: The Gamma-ray Binary 1fgl J10186−5856mentioning

confidence: 89%

Refining the origins of the gamma-ray binary 1FGL J1018.6–5856

Marcote

Ribó

Paredes

et al. 2018

A&A

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Context. Gamma-ray binaries are systems composed of a massive star and a compact object that exhibit emission from radio to very high energy gamma rays. They are ideal laboratories to study particle acceleration and a variety of physical processes that vary as a function of the orbital phase. Aims. We aim to study the radio emission of the gamma-ray binary 1FGL J1018.6−5856 to constrain the emitting region and determine the peculiar motion of the system within the Galaxy to clarify its origin. Methods. We analyzed an observation of 1FGL J1018.6−5856 with the Australian Long Baseline Array (LBA) at 8.4 GHz to obtain an accurate astrometry of the system and study its emission on milliarcsecond scales. We combined these data with the optical Gaia DR2 and UCAC4 catalogs to consolidate the astrometry information therein. Results. The gamma-ray binary 1FGL J1018.6−5856 shows compact radio emission (< 3 mas or 20 au at ∼ 6.4 kpc distance), implying a brightness temperature of 5.6×10 6 K, and confirming its nonthermal origin. We report consistent results between the proper motion reported by Gaia data release 2 (DR2) and the positions obtained from the Gaia DR2, UCAC4, and LBA data (spanning 20 yr in total). We also determined the distance to 1FGL J1018.6−5856 to be 6.4 +1.7 −0.7 kpc. Together with the radial velocity of the source we computed its three-dimensional (3D) proper and peculiar motion within the Galaxy. We obtained a peculiar motion of 1FGL J1018.6−5856 on its regional standard of rest (RSR) frame of |u| = 45 +30 −9 km s −1 , with the system moving away from the Galactic plane. In the simplest scenario of a symmetric stellar core collapse we estimate a mass loss of 4 ∆M 9 M during the creation of the compact object.Conclusions. 1FGL J1018.6−5856 exhibits compact radio emission similar to that detected in other gamma-ray binaries. We provide the first accurate peculiar motion estimations of the system and place it within the Galaxy. The obtained motion and distance excludes the physical relation of the binary source with the supernova remnant (SNR) G284.3−1.8.

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Section: The Gamma-ray Binary 1fgl J10186−5856mentioning

confidence: 89%

Refining the origins of the gamma-ray binary 1FGL J1018.6–5856

Marcote

Ribó

Paredes

et al. 2018

A&A

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“…This primary mass would be allowed by the spectroscopic observations only if i 13 • -16 • (M 2 = 20-26.4 M ⊙ ). Due to the presence of (sin i) 3 in the mass function equation, this conclusion would be very similar even if the secondary were somewhat more massive (∼ 30M ⊙ ; Napoli et al 2011). However, these same inclinations are generally excluded by the measurement of the projected rotational velocity of the star ( §3.3).…”

Section: Mass Of the Compact Objectmentioning

confidence: 89%

OPTICAL SPECTROSCOPY OF THE HIGH-MASS γ -RAY BINARY 1FGL J1018.6−5856: A PROBABLE NEUTRON STAR PRIMARY

Strader

Chomiuk

Cheung

et al. 2015

ApJ

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We present medium-resolution optical spectroscopy with the SOAR telescope of the O star secondary of the high-mass γ-ray binary 1FGL J1018.6-5856 to help determine whether the primary is a neutron star or black hole. We find that the secondary has a low radial velocity semi-amplitude of 11-12 km s −1 , with consistent values obtained for H and He absorption lines. This low value strongly favors a neutron star primary: while a black hole cannot be excluded if the system is close to face on, such inclinations are disallowed by the observed rotation of the secondary. We also find the high-energy (Xray and γ-ray) flux maxima occur when the star is behind the compact object along our line of sight, inconsistent with a simple model of anisotropic inverse Compton scattering for the γ-ray photons.

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“…The spectral type of the companion star places tighter constraints on the exploded star than would otherwise be possible. Ground-based observations revealed a massive star of spectral type O6V((f)) (V ≈ 13.5; Napoli et al 2011) and mass of ∼ 30 M ⊙ , very similar to that of the γ-ray binary LS 5039. J1018 was observed with the H.E.S.S.…”

Section: Introductionmentioning

confidence: 85%

“…The fundamental problem is that SNe are plentiful but distant and point-like, while SNRs are local and resolvable but limited in number. SNR G284.3-1.8 (also known as MSH 10-53; hereafter G284) has been identified through radio (Milne et al 1989), optical (Ruiz & May 1986), and X-ray (HESS Collaboration et al 2012) observations, and is perhaps 10 4 years old (Ruiz & May 1986) with a distance of 5.4 2.1 4.6 -+ kpc (Napoli et al 2011). It is interacting with a molecular cloud in the north.…”

Section: Introductionmentioning

confidence: 99%

Magnesium-Rich Ejecta in the SNR G284.3–1.8 Around the High-Mass Gamma-Ray Binary 1fgl J1018.6–5856

Williams

Rangelov

Kargaltsev

et al. 2015

ApJ

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We present results from two Chandra observations of the 16.6 day X-ray/γ-ray high-mass binary 1FGL J1018.6-5856 located at the center of the supernova remnant (SNR) G284.3-1.8. The binary spectra, separated by 0.25 in binary phase, are fit with an absorbed power-law model with 1.7 1.8 G » -for both observations (the flux during the second observation is a factor of 1.7 smaller). In the high-resolution ACIS-I image we found a hint of extended emission 2 » -3″ southeast of the binary, significant at the 3s level. Binary evolution codes reproduce the system's observed properties with two massive stars with an initial 18 day period, undergoing mass transfer and leaving behind a heavy 2 » M  neutron star. The initial mass of the progenitor star in this scenario is 27 ± 4 M  . Chandra and XMM-Newton images of the remnant show it has a relatively low X-ray surface brightness. The two brightest regions of extended X-ray emission, with luminosities 10 33 erg s −1 for d = 5 kpc, lie in the northern and western portions and show significantly different spectra. The northern patch is consistent with shocked ISM, with a low temperature and long ionization timescale. However, the western patch is dominated by ejecta, and shows significantly enhanced Mg content relative to other ejecta products. The abundance ratios inferred resemble those from the Large Magellanic Cloud remnant N49B. To our knowledge, this is only the second case of such Mg-rich ejecta found in an SNR. Nucleosynthesis models for core-collapse supernovae predict Mg-rich ejecta from very massive progenitors of 25 > M  .

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The Distance of the γ-Ray Binary 1FGL J1018.6–5856

Cited by 16 publications

References 14 publications

Refining the origins of the gamma-ray binary 1FGL J1018.6–5856

Refining the origins of the gamma-ray binary 1FGL J1018.6–5856

OPTICAL SPECTROSCOPY OF THE HIGH-MASS γ -RAY BINARY 1FGL J1018.6−5856: A PROBABLE NEUTRON STAR PRIMARY

Magnesium-Rich Ejecta in the SNR G284.3–1.8 Around the High-Mass Gamma-Ray Binary 1fgl J1018.6–5856

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