Is HESS J1912+101 Associated with an Old Supernova Remnant?

Su, Yang; Zhou, Xin; Yang, Ji; Chen, Yang; Chen, Xue-Peng; Gong, Y.; Zhang, Shaobo

doi:10.3847/1538-4357/aa7f2a

Cited by 21 publications

(31 citation statements)

References 58 publications

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“…For HESS J1912+101, Su et al (2017) derived a distance of about 4.1 kpc based on HI self-absorption data, which is in rough agreement with the dispersion measure based distance of PSR J1913+1011 (Morris et al 2002) of about 4.5 kpc, located near to the centre of HESS J1912+101. The distance agreement suggests that PSR J19133+1011 and HESS J1912+101 are related.…”

Section: Discussionsupporting

confidence: 78%

“…Also the age estimate by Su et al (2017) for HESS J1912+101 of about 0.7-2.0 10 5 years and that of PSR J193+1011 of about 1.7 10 5 years (Morris et al 2002) agree within the errors and support a physical association. Su et al (2017) suggest a scenario, where the stellar winds of the massive progenitor created a bubble in the molecular material. This stellar wind also had an effect on the ambient magnetic field, which gets compressed.…”

Section: Discussionmentioning

confidence: 74%

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Polarised radio emission associated with HESS J1912+101

Reich

Sun

2019

Res. Astron. Astrophys.

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The shell-type TeV source HESS J1912+101 was tentatively identified as an old supernova remnant, but is missing counterparts at radio and other frequencies. We analysed the Sino-German Urumqi λ6 cm survey and the Effelsberg λ11 cm and λ21 cm surveys to identify radio emission from HESS J1912+101 to clarify the question of a supernova origin. We find a partial shell of excessive polarisation at λ6 cm at the periphery of HESS J1912+101. At λ11 cm, its polarised emission is faint and suffers from depolarisation, while at λ21 cm, no related polarisation is seen. We could not separate the shell's total intensity signal from the confusing intense diffuse emission from the inner Galactic plane. However, a high-percentage polarisation of the shell's synchrotron emission is indicated. Our results support earlier suggestions that HESS J1912+101 is an old supernova remnant. The synchrotron emission is highly polarised, which is typical for evolved supernova remnants of low surface-brightness.

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Section: Discussionsupporting

confidence: 78%

Section: Discussionmentioning

confidence: 74%

Polarised radio emission associated with HESS J1912+101

Reich

Sun

2019

Res. Astron. Astrophys.

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“…In the case that G21.8−3.0 is not young, the small physical size requires a low initial explosion energy and/or a high ambient density into which it expands (Sedov 1959). However, as we failed to identify any related H i structures, it is difficult to estimate the initial ambient number density and further the age of G21.8−3.0 as done by Su et al (2017) and Kothes et al (2017). For the shell-type SNRs, distance and diameter can also be estimated from the empirical radio surface brightness -diameter (Σ-D) relation.…”

Section: Size Age and Brightnessmentioning

confidence: 99%

Discovery of a new supernova remnant G21.8−3.0

Gao

Reich

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Sensitive radio continuum surveys of the Galactic plane are ideal for discovering new supernova remnants (SNRs). From the Sino-German λ6 cm polarisation survey of the Galactic plane, an extended shell-like structure has been found at ℓ = 21. • 8, b = −3. • 0, which has a size of about 1 • . New observations were made with the Effelsberg 100-m radio telescope at λ11 cm to estimate the source spectrum together with the Urumqi λ6 cm and the Effelsberg λ21 cm data. The spectral index of G21.8−3.0 was found to be α = −0.72 ± 0.16. Polarised emission was mostly detected in the eastern half of G21.8−3.0 at both λ6 cm and λ11 cm. These properties, together with the Hα filament along its northern periphery and the lack of infrared emission, indicate that the emission is non-thermal as is usual in shell-type SNRs.

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“…The observing strategy, the instrument, and the quality of the CO observations were described in our recent paper (see Su et al 2017b). Briefly, Each 30 ′ × 30 ′ map was covered with position-switch On-The-Fly mode at least twice in scanning direction along Galactic longitude and latitude to minimize the fluctuation of noise.…”

Section: Co Datamentioning

confidence: 99%

The Large-scale Interstellar Medium of SS 433/W50 Revisited

Zhou

Yang

et al. 2018

ApJ

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With new high-resolution CO and H i data, we revisited the large-scale interstellar medium (ISM) environment toward the SS 433/W50 system. We find that two interesting molecular cloud (MC) concentrations, G39.315−1.155 and G40.331−4.302, are well aligned along the precession cone of SS 433 within a smaller opening angle of ∼ ±7 • . The kinematic features of the two MCs at ∼73-84 km s −1 , as well as those of the corresponding atomic-gas counterparts, are consistent with the kinematic characteristics of SS 433. That is, the receding gas from SS 433 jet is probably responsible for the redshifted feature of G39.315−1.155 near the Galactic plane and the approaching one may power the blueshifted gas of G40.331−4.302 toward the observer. Moreover, the H i emission at V LSR ∼70-90 km s −1 displays the morphological resemblance with the radio nebula W50. We suggest that the V LSR =77±5 km s −1 gas is physically associated with SS 433/W50, leading to a near kinematic distance of 4.9±0.4 kpc for the system. The observed gas features, which are located outside the current radio boundaries of W50, are probably the fossil record of jet-ISM interactions at ∼ 10 5 years ago. The energetic jets of the unique microquasar have profound effects on its ISM environment, which may facilitate the formation of molecular gas on the timescale of < ∼ 0.1 Myr for the ram pressure of ∼ 2 × 10 6 K cm −3 .

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Is HESS J1912+101 Associated with an Old Supernova Remnant?

Cited by 21 publications

References 58 publications

Polarised radio emission associated with HESS J1912+101

Polarised radio emission associated with HESS J1912+101

Discovery of a new supernova remnant G21.8−3.0

The Large-scale Interstellar Medium of SS 433/W50 Revisited

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