Far-Ultraviolet Spectral Images of the Vela Supernova Remnant

Nishikida, Koichi; Edelstein, Jerry; Korpela, E. J.; Sankrit, Ravi; Feuerstein, W. M.; Kang, Min; Shinn, Jong-Ho; Dh, Lee; Yuk, I. S.; Jin, Ho; Seon, Kwang‐Il

doi:10.1086/505197

Cited by 24 publications

(58 citation statements)

References 25 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…It is widely believed to be a superbubble blown by strong stellar winds and supernovae of the Sco-Cen OB association ($170 pc away). X-ray, neutral hydrogen, and optical absorption measurements are consistent with a shell of radius $100 pc centered $130 pc away in the direction (l; b) ¼ (330 ; 15 ), with the receding shell P212 pc away (Nishikida 1999). Note, however, that Welsh & Lallement (2005) used HST-STIS UV absorption spectra toward the approximate center of Loop I, (l; b) ¼ (330 ; 18 ), and estimated that the approaching and receding walls of Loop I are about 90 and 150Y180 pc, respectively.…”

Section: Description Of Regionmentioning

confidence: 55%

“…Assuming the distance to the IZ is $70 pc (Egger & Aschenbach 1995), and the radius of the Loop I superbubble is $100 pc (Nishikida 1999), we can use the angular distance between the unshadowed sight line and the center of Loop I (Nishikida1999) to geometrically determine the distance to the center of Loop I and the path length of the unshadowed sight line through Loop I (under the poor assumption of spherical symmetry; see Fig. 2).…”

Section: à3mentioning

confidence: 99%

“…Dixon et al (2006) noted two sight lines in their survey that fit this category, each with O vi intensities exceeding 8000 LU. SPEAR detected the extremely high value of 180,000 LU toward the Vela SNR (Nishikida et al 2006), and nearly 7000 LU toward the edge of the Orion-Eridanus Superbubble (Kregenow et al 2006). …”

Section: Introductionmentioning

confidence: 97%

See 2 more Smart Citations

FUSEObservations of the Loop I/Local Bubble Interaction Region

Sallmen

Korpela

Yamashita

2008

ApJ

View full text Add to dashboard Cite

We used the FUSE (Far Ultraviolet Spectroscopic Explorer ) satellite to observe O vi emission along two sight lines toward the edge of the interaction zone (IZ ) between the Loop I superbubble and the Local Bubble. One sight line was chosen because material in the interaction zone blocks distant X-ray emission, and should thus do the same for nonlocal O vi emission. We measured an O vi intensity of I shad ¼ 2750 AE 550 photons cm À2 s À1 sr À1 along this ''shadowed'' sight line, and I unshad ¼ 10;800 AE 1200 photons cm À2 s À1 sr À1 along the other sight line. Given these results, very little (P 800 photons cm À2 s À1 sr À1

show abstract

Section: Description Of Regionmentioning

confidence: 55%

Section: à3mentioning

confidence: 99%

See 1 more Smart Citation

FUSEObservations of the Loop I/Local Bubble Interaction Region

Sallmen

Korpela

Yamashita

2008

ApJ

View full text Add to dashboard Cite

show abstract

“…Using E(B − V ) = 0.017 (from the relation N H = 5.8 × 10 21 E(B − V ) cm −2 mag −1 of Bohlin et al 1978) and the extinction curve of Cardelli et al (1989) with R V = 3.1, the reddening-corrected values were obtained. 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.…”

Section: Data Analysis and Resultsmentioning

confidence: 99%

“…a The values are from Seon et al (2006). b The values are from Nishikida et al (2006). c The value is from Shelton et al (2004) and the corresponding energy band is 0.11-2.04 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

Self Cite

View full text Add to dashboard Cite

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.

show abstract

Science with a Small Two-Band UV-Photometry Mission I: Mission Description and Follow-up Observations of Stellar Transients

Werner,

Řípa,

Thöne

et al. 2024

Space Sci Rev

View full text Add to dashboard Cite

This is the first in a collection of three papers introducing the science with an ultra-violet (UV) space telescope on an approximately 130 kg small satellite with a moderately fast re-pointing capability and a real-time alert communication system approved for a Czech national space mission. The mission, called Quick Ultra-Violet Kilonova surveyor—QUVIK, will provide key follow-up capabilities to increase the discovery potential of gravitational wave observatories and future wide-field multi-wavelength surveys. The primary objective of the mission is the measurement of the UV brightness evolution of kilonovae, resulting from mergers of neutron stars, to distinguish between different explosion scenarios. The mission, which is designed to be complementary to the Ultraviolet Transient Astronomy Satellite—ULTRASAT, will also provide unique follow-up capabilities for other transients both in the near- and far-UV bands. Between the observations of transients, the satellite will target other objects described in this collection of papers, which demonstrates that a small and relatively affordable dedicated UV-space telescope can be transformative for many fields of astrophysics.

show abstract

Far-Ultraviolet Spectral Images of the Vela Supernova Remnant

Cited by 24 publications

References 25 publications

FUSEObservations of the Loop I/Local Bubble Interaction Region

FUSEObservations of the Loop I/Local Bubble Interaction Region

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

Science with a Small Two-Band UV-Photometry Mission I: Mission Description and Follow-up Observations of Stellar Transients

Contact Info

Product

Resources

About