The "Spectroscopy of Plasma Evolution from Astrophysical Radiation" Mission

Edelstein, Jerry; Min, Kyoung Wook; Han, Wonyong; Korpela, E. J.; Nishikida, Koichi; Welsh, Barry Y.; Heiles, Carl; Adolfo, J.; Bowen, M. Shane; Feuerstein, W. M.; McKee, Ken; Lim, Jaechang; Ryu, Kwang‐Sun; Shinn, Jong-Ho; Nam, Uk-Won; Park, J.-H.; Yuk, In-Soo; Jin, Ho; Seon, Kwang‐Il; Lee, D.H.; Sim, Eun-Sup

doi:10.1086/505208

Cited by 62 publications

(34 citation statements)

References 52 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The instrument was launched in 2003 as the main payload of STSAT-1 and was operated for one and a half years (see Edelstein et al 2006aEdelstein et al , 2006b for more information on the FIMS/SPEAR mission). It consists of two spectral channels, a short-wavelength channel (S band, 900-1150 Å) and a longwavelength channel (L band, 1350-1750 Å).…”

Section: Observationsmentioning

confidence: 99%

“…However, we used only the L-band data in the present study, as these data are less affected by strong geocoronal lines. Details regarding the on-orbit performance and the data analysis procedures are described in Edelstein et al (2006aEdelstein et al ( , 2006b). …”

Section: Observationsmentioning

confidence: 99%

“…In the following discussions, we will use the FIMS/SPEAR data for spectral analyses, as FUV line emissions can be discriminated from stellar continuum emissions, and the GALEX data for photometric analyses as they give more reliable diffuse emission than the FIMS/SPEAR data. These FUV maps are compared with the observations made in other wavelength bands: the velocityintegrated CO emission map in Figure 1(c) (Dame et al 2001) and the Hα map in Figure 1(d) (Finkbeiner 2003). The velocityintegrated CO image was provided through private communications with the authors and the Hα map was obtained from the Virtual Sky View Observatory (http://skyview.gsfc.nasa.gov).…”

Section: Observationsmentioning

confidence: 99%

See 2 more Smart Citations

FAR-ULTRAVIOLET OBSERVATION OF THE AQUILA RIFT WITHFIMS/SPEAR

Park

Kang

Seon

et al. 2012

ApJ

Self Cite

View full text Add to dashboard Cite

We present the results of far ultraviolet (FUV) observations of the broad region around the Aquila Rift including the Galactic plane. As compared with various wavelength data sets, dust scattering is found to be the major origin of the diffuse FUV continuum in this region. The FUV intensity clearly correlates with the dust extinction level for E(B − V ) < 0.2, while this correlation disappears for E(B − V ) > 0.2 due to heavy dust extinction combined with the effect of nonuniform interstellar radiation fields. The FUV intensity also correlates well with Hα intensity, implying that at least some fraction of the observed Hα emission could be the dust-scattered light of Hα photons originating elsewhere in the Galaxy. Most of the Aquila Rift region is seen devoid of diffuse FUV continuum due to heavy extinction while strong emission is observed in the surrounding regions. Molecular hydrogen fluorescent emission lines are clearly seen in the spectrum of "Aquila-Serpens," while "Aquila-East" does not show any apparent line features. CO emission intensity is also found to be higher in the "Aquila-Serpens" region than in the "Aquila-East" region. In this regard, we note that regions of star formation have been found in "Aquila-Serpens" but not in "Aquila-East."

show abstract

Section: Observationsmentioning

confidence: 99%

Section: Observationsmentioning

confidence: 99%

Section: Observationsmentioning

confidence: 99%

See 1 more Smart Citation

FAR-ULTRAVIOLET OBSERVATION OF THE AQUILA RIFT WITHFIMS/SPEAR

Park

Kang

Seon

et al. 2012

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

“…3) and moderate spectral (λ/Δλ ∼ 550) and angular (∼5 ) resolutions, the instrument is optimized for the observation of diffuse emissions (Edelstein et al 2006a(Edelstein et al , 2006b. Though the OES region was observed in both the S and the L band, we analyzed only the L-band data for the present study since the S-band data were strongly contaminated by geocoronal emission lines.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Simulation Study of Dust-Scattered Far-Ultraviolet Emission in the Orion-Eridanus Superbubble

Jo¹,

Kang²,

Lim³

et al. 2012

ApJ

View full text Add to dashboard Cite

We present the results of dust scattering simulations carried out for the Orion-Eridanus Superbubble region by comparing them with observations made in the far-ultraviolet. The albedo and the phase function asymmetry factor (g-factor) of interstellar grains were estimated, as were the distance and thickness of the dust layers. The results are as follows: 0.43 +0.02 −0.04 for the albedo and 0.45 +0.2 −0.2 for the g-factor, in good agreement with previous determinations and theoretical predictions. The distance of the assumed single dust layer, modeled for the Orion Molecular Cloud Complex, was estimated to be ∼110 pc and the thickness ranged from ∼130 at the core to ∼50 pc at the boundary for the region of present interest, implying that the dust cloud is located in front of the superbubble. The simulation result also indicates that a thin (∼10 pc) dust shell surrounds the inner X-ray cavities of hot gas at a distance of ∼70-90 pc.

show abstract

“…3 field of view), with λ/Δλ ∼ 550 spectral resolution and 5 angular resolution. The instrument, its on-orbit performance, and the basic processing of the data are described in detail in Edelstein et al (2006aEdelstein et al ( , 2006b.…”

Section: Observations and Data Reductionmentioning

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

The "Spectroscopy of Plasma Evolution from Astrophysical Radiation" Mission

Cited by 62 publications

References 52 publications

FAR-ULTRAVIOLET OBSERVATION OF THE AQUILA RIFT WITHFIMS/SPEAR

FAR-ULTRAVIOLET OBSERVATION OF THE AQUILA RIFT WITHFIMS/SPEAR

Simulation Study of Dust-Scattered Far-Ultraviolet Emission in the Orion-Eridanus Superbubble

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

Contact Info

Product

Resources

About