H I distribution in the region of the supernova remnant G78.2+2.1

Gosachinskij, I. V.

doi:10.1134/1.1358380

Cited by 15 publications

(18 citation statements)

References 5 publications

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“…Given that no significant CO emission is detected in this area of the remnant, any target material must be atomic rather than molecular, with the necessary high density perhaps arising in the swept-up H i shell. Gosachinskij (2001) estimated a gas density of 2.5 cm −3 in the H i shell surrounding the remnant, consistent with the range of densities derived from the TeV data. Optical data also shed some light on densities in the vicinity of VER J2019+407.…”

Section: Discussionsupporting

confidence: 84%

“…The TeV gamma-ray emission and the features observed in the X-ray, optical, and radio continuum can be most simply related to the presence of shocks at the interaction of the supernova ejecta and the surrounding medium. SNR G78.2+2.1 has a relatively low interior density and, as previously noted, appears to be surrounded by a dense H i shell (Gosachinskij 2001). Lozinskaya et al (2000) suggest that this H i shell was created by the progenitor stellar wind as it swept up the ambient medium.…”

Section: Discussionmentioning

confidence: 55%

“…The TeV gammaray emission is coincident with the leading edge of a prominent arc-shaped radio continuum feature along the SNR rim ( Figure 1) and with a region of enhanced X-ray emission that we identify as thermal in origin (Figures 3-5). VER J2019+407 lies near the inner edge of a slowly expanding H i shell immediately surrounding the radio shell identified in 21 cm line observations (Gosachinskij 2001); it also lies near a region of bright [S ii] optical line emission within the SNR that is identified as shock-heated gas based on the [S ii]/Hα line ratio (Mavromatakis 2003). There are also two GeV sources associated with SNR G78.2+2.1.…”

Section: Discussionmentioning

confidence: 92%

“…It is considered young to middle-aged at ∼7000 yr (Higgs et al 1977;Landecker et al 1980;Lozinskaya et al 2000) and in an early phase of adiabatic expansion into a medium of fairly low density (Lozinskaya et al 2000). Gosachinskij (2001) also identifies a slowly expanding H i shell immediately surrounding the radio shell. Lozinskaya et al (2000) suggest this shell was created by the progenitor stellar wind.…”

Section: Introductionmentioning

confidence: 99%

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DISCOVERY OF TeV GAMMA-RAY EMISSION TOWARD SUPERNOVA REMNANT SNR G78.2+2.1

Aliu

Archambault

Arlen

et al. 2013

ApJ

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We report the discovery of an unidentified, extended source of very-high-energy gamma-ray emission, VER J2019+407, within the radio shell of the supernova remnant SNR G78.2+2.1, using 21.4 hr of data taken by the VERITAS gamma-ray observatory in 2009. These data confirm the preliminary indications of gamma-ray emission previously seen in a two-year (2007-2009) blind survey of the Cygnus region by VERITAS. VER J2019+407, which is detected at a post-trials significance of 7.5 standard deviations in the 2009 data, is localized to the northwestern rim of the remnant in a region of enhanced radio and X-ray emission. It has an intrinsic extent of 0. • 23±0. • 03 stat

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Section: Discussionsupporting

confidence: 84%

Section: Discussionmentioning

confidence: 55%

Section: Discussionmentioning

confidence: 92%

Section: Introductionmentioning

confidence: 99%

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DISCOVERY OF TeV GAMMA-RAY EMISSION TOWARD SUPERNOVA REMNANT SNR G78.2+2.1

Aliu

Archambault

Arlen

et al. 2013

ApJ

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“…It is absent in the northwest. The location of this shell is nearly coincident with a similar structure proposed by Gosachinskij (2001). Figure 22 shows that the bright radio continuum emission is indeed circumscribed by the H i feature.…”

Section: Neutral Hydrogen Morphologically Related To the Snrsupporting

confidence: 78%

New perspectives on the supernova remnant G78.2+2.1

Ladouceur¹,

Pineault²

2008

A&A

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Aims. The Galactic object G78.2+2.1 is a classical shell-type supernova remnant. Previous radio continuum studies have shown substantial variations in spectral index across the object. Existing studies of the neutral hydrogen are of relatively low resolution and sensitivity. Much higher sensitivity and resolution data from the Canadian Galactic Plane Survey justify a re-examination of the properties of this SNR. Methods. In order to improve the accuracy of spectral index determination and its spatial variation, we first remove the underlying thermal emission with the use of a correlation between the 60 μm infrared continuum and 1420 MHz radio continuum. We use the so-called TT-plot technique to obtain the continuum spectral index between 408 and 1420 MHz. We also apply a "tomography" technique to investigate the spectral index variations, while keeping the full resolution of the data. Complementary X-ray and infrared data are used to study associated structures in both continuum and in the 21 cm line of neutral hydrogen. Results. The spectral index α (S ν ∝ ν −α ) averaged over the SNR is 0.75 ± 0.03, significantly higher than previous studies. The TT-plots and tomography image show spatial variations ranging from as low as 0.40 to as high as 0.80. Two complementary neutral hydrogen structures at LSR velocities of 5.5 and −14 km s −1 , respectively, are shown to circumscribe the continuum emission. A number of scenarios are presented to account for the observed properties. A faint shell to the north-west of the SNR is visible in both radio and infrared continuum as well as in neutral hydrogen, and could be associated with a local blowout of the SNR blast wave into a medium of lower density. An isolated cloudlet probably accelerated by the SNR blast wave shows considerable structure in neutral hydrogen emission, suggesting the cloudlet is either beginning to dissolve within the SNR or is interacting with neighbouring gas. The previously proposed cloudlet at ∼−117 km s −1 is not isolated, but is part of a more extended structure, and is thus unlikely an accelerated cloudlet.

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Shell‐type supernova remnants and very high energy cosmic rays

Sinitsyna

2022

Astron Nachr

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The investigation of very high energy (VHE) γ‐ray sources by any methods, including mirror Cherenkov telescopes, touches on the problem of the cosmic‐ray origin and, accordingly, the role of the Galaxy in their generation. The SHALON observations have yielded the results on Galactic supernova remnants (SNR) of different ages. Among them are: the shell‐type SNRs Tycho's SNR, Cas A, IC 443, γCygni SNR, G166.0+4.3. For each of SNRs, the observation results are presented with spectral energy distribution by SHALON in comparison with other experiment data and images by SHALON in together with data from X‐ray by Chandra and radio‐data by CGPS. The experimental data presented here have confirmed the prediction of the theory about the hadronic generation mechanism of VHE 800 GeV–100 TeV γ‐rays in Tycho's SNR, Cas A and IC 443, and also the collected experimental data help to make clear the origin of TeV γ‐ray emission in the older SNRs like γCygni SNR and G166.0+4.3.

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H I distribution in the region of the supernova remnant G78.2+2.1

Cited by 15 publications

References 5 publications

DISCOVERY OF TeV GAMMA-RAY EMISSION TOWARD SUPERNOVA REMNANT SNR G78.2+2.1

DISCOVERY OF TeV GAMMA-RAY EMISSION TOWARD SUPERNOVA REMNANT SNR G78.2+2.1

New perspectives on the supernova remnant G78.2+2.1

Shell‐type supernova remnants and very high energy cosmic rays

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