Far-Ultraviolet Spectral Images of the Cygnus Loop

Seon, Kwang‐Il; Han, Wonyong; Nam, UW; Jh, Park; Edelstein, Jerry; Korpela, E. J.; Sankrit, Ravi; Kang, Min; Ryu, Kyoung‐Seok; Ij, Kim

doi:10.1086/505201

Cited by 23 publications

(41 citation statements)

References 36 publications

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“…Spectral resolution at the given line was employed as the width (FWHM) of the Gaussian function. The final image was constructed using the method of adaptive smoothing to increase the signal-to-noise ratio (S/N; Seon et al 2006). The Gaussian smoothing scale varied from 1.2Њ to 6Њ.…”

Section: Introductionmentioning

confidence: 99%

Far-Ultraviolet Observations of the Loop I/North Polar Spur Region

Park

Kang

Seon

et al. 2007

ApJ

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The results of diffuse far-ultraviolet observations of the Loop I/North Polar Spur (NPS) region are presented in this Letter. Several important ionic emission lines, including C iv, Si ii*, Si iv, and Al ii, were detected. Fluorescent emission lines from hydrogen molecules were also seen in the spectra. A spectral image made with C iv emission shows a shell-like feature colocated with the X-ray NPS. This feature is located just inside the Loop I radio ridges. Another interesting C iv feature is seen at the inner edge of the "interaction ring," where the cold interstellar medium is in direct contact with the X-ray-bright hot gas. The present observation is in good agreement with a model of recent supernova explosion in an inhomogeneous medium, possibly disturbed by previous multiple supernova explosions.

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Section: Introductionmentioning

confidence: 99%

Far-Ultraviolet Observations of the Loop I/North Polar Spur Region

Park

Kang

Seon

et al. 2007

ApJ

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“…Adopting a distance of 900 pc to the target (Reich et al 1979), the line luminosities were calculated and listed along with the values of the Cygnus Loop ) and the Vela (Nishikida et al 2006) in Table 1. The X-ray luminosities (Shelton et al 2004;Seon et al 2006;Lu & Aschenbach 2000) are also shown for comparison. Line luminosities with <2σ significance are indicated by 1σ upper limits.…”

Section: Data Analysis and Resultsmentioning

confidence: 99%

“…c The value is from Shelton et al (2004) and the corresponding energy band is 0.11-2.04 keV. d The value is from Seon et al (2006) and the corresponding energy band is 0.1-4.0 keV. e The value is from Lu & Aschenbach (2000) and the corresponding energy band is 0.1-2.5 keV.…”

Section: Discussionmentioning

confidence: 99%

Far-Ultraviolet Emission-Line Morphologies of the Supernova Remnant G65.3+5.7

Kim

Seon

Kang

et al. 2010

ApJ

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We present the first far-ultraviolet (FUV) emission-line morphologies of the whole region of the supernova remnant (SNR) G65.3+5.7 using the FIMS/SPEAR data. The morphologies of the C iv λλ1548, 1551, He ii λ1640, and O iii] λλ1661, 1666 lines appear to be closely related to the optical and/or soft X-ray images obtained in previous studies. Dramatic differences between the C iv morphology and the optical [O iii] λ5007 image provide clues to a large resonant-scattering region and a foreground dust cloud. The FUV morphologies also reveal the overall distribution of various shocks in different evolutionary phases and an evolutionary asymmetry between the east and the southwest sides in terms of Galactic coordinates, possibly due to a Galactic density gradient in the global scale. The relative X-ray luminosity of G65.3+5.7 to C iv luminosity is considerably lower than those of the Cygnus Loop and the Vela SNRs. This implies that G65.3+5.7 has almost evolved into the radiative stage in the global sense and supports the previous proposal that G65.3+5.7 has lost its bright X-ray shell and become a member of mixed-morphology SNRs as it has evolved beyond the adiabatic stage.

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“…644 (Nishikida et al 2006) and the Cygnus Loop SNR (Seon et al 2006). Both Nishikida et al and Seon et al find that the spatial distribution of FUV emission cannot be simply predicted using visible Ha or X-ray emission maps.…”

Section: Supernova Remnants and Superbubblesmentioning

confidence: 99%

The "Spectroscopy of Plasma Evolution from Astrophysical Radiation" Mission

Edelstein

Min

Han

et al. 2006

ApJ

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The "Spectroscopy of Plasma Evolution from Astrophysical Radiation" (SPEAR, also known as the "FarUltraviolet Imaging Spectrograph") instruments, flown aboard the STSAT-1 satellite mission, have provided the first large-area spectral mapping of the cosmic far-ultraviolet (FUV; 900-1750 ) background. We describe the A mission and its science motivation, the mission data and their processing, and the effects of mission performance on the science data. We present the first map of the cosmic FUV background (1360-1710 ) over most of the A sky as an example of the mission results. These SPEAR data reveal diffuse radiation from warm and hot (10 4 -10 6 K) plasma, molecular hydrogen fluorescence, and dust-scattered starlight. They allow for an unprecedented characterization of the spectral emission from a variety of environments, including the general interstellar medium (ISM), molecular clouds, supernova remnants, and superbubbles.

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Far-Ultraviolet Spectral Images of the Cygnus Loop

Cited by 23 publications

References 36 publications

Far-Ultraviolet Observations of the Loop I/North Polar Spur Region

Far-Ultraviolet Observations of the Loop I/North Polar Spur Region

Far-Ultraviolet Emission-Line Morphologies of the Supernova Remnant G65.3+5.7

The "Spectroscopy of Plasma Evolution from Astrophysical Radiation" Mission

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