FAR-ULTRAVIOLET OBSERVATION OF THE AQUILA RIFT WITH<i>FIMS</i>/<i>SPEAR</i>

Park, S.-J.; Kang, Min; Seon, Kwang‐Il; Han, Wonyong; Lee, D.-H.; Edelstein, Jerry

doi:10.1088/0004-637x/754/1/10

Cited by 7 publications

(10 citation statements)

References 43 publications

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“…On physical scales corresponding to molecular clouds, there can be significant deviations in the relationship between FUV and dust. Observations in Aquila with FIMS/SPEAR (Park et al 2012) found FUV intensity correlates well with dust column for low extinction sightlines, while there is no correlation in regions with higher dust column. Similarly, in the Draco Cloud, Sujatha et al (2010) found substantial variations in the relationship between diffuse FUV intensity and 100 µm intensity using GALEX data.…”

Section: Introductionmentioning

confidence: 87%

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The Diffuse Galactic Far-Ultraviolet Sky

Hamden

Schiminovich

Seibert

2013

ApJ

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We present an all sky map of the diffuse Galactic far ultraviolet (1344-1786Å) background using GALEX data, covering 65% of the sky with 11.79 arcmin 2 pixels. We investigate the dependence of the background on Galactic coordinates, finding that a standard cosecant model of intensity is not a valid fit. Furthermore, we compare our map to Galactic all sky maps of 100 µm emission, N HI column, and Hα intensity. We measure a consistent low level FUV intensity at zero-points for other Galactic quantities, indicating a 300 CU non-scattered isotropic component to the diffuse FUV. There is also a linear relationship between FUV and 100 µm emission below 100 µm values of 8 MJy/sr. We find a similar linear relationship between FUV and N HI below 10 21 cm −2 . The relationship between FUV and Hα intensity has no such constant cutoff. For all Galactic quantities, the slope of the linear portion of the relationship decreases with Galactic latitude. A modified cosecant model, taking into account dust scattering asymmetry and albedo, is able to accurately fit the diffuse FUV at latitudes above 20 • . The best fit model indicates an albedo, a, of 0.62 ± 0.04 and a scattering asymmetry function, g, of 0.78 ± 0.05. Deviations from the model fit may indicate regions of excess FUV emission from fluorescence or shock fronts, while low latitude regions with depressed FUV emission are likely the result of self-shielding dusty clouds.

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Section: Introductionmentioning

confidence: 87%

“…Ophiuchus, and brights stars, e.g. the spectroscopic binary Spica (at l=316, b=51., Park et al (2012)).…”

Section: Fuv Vs 100 µMmentioning

confidence: 99%

The Diffuse Galactic Far-Ultraviolet Sky

Hamden

Schiminovich

Seibert

2013

ApJ

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“…Furthermore, the diffuse FUV continuum background radiation probes the dust scattering of starlight (Bowyer 1991;Henry 2002;Seon et al 2011a,b). Hence, a variety of astrophysical targets have been analyzed based on FUV observations, such as supernova remnants (SNRs; Seon et al (2006); Kim et al (2010a,b)), superbubbles (Kim et al 2007;Jo et al 2011Jo et al , 2012, diffuse and molecular clouds, and interstellar dust (Lee et al 2006;Park et al 2009Park et al , 2012Lim et al 2013) .…”

Section: Introductionmentioning

confidence: 99%

Far-Ultraviolet Observations of the Spica Nebula and the Interaction Zone

Choi

Kang

Seon

et al. 2013

ApJ

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We report the analysis results of far ultraviolet (FUV) observations, made for a broad region around α Vir (Spica) including the interaction zone of Loop I and the Local Bubble. Whole region was optically thin and a general correlation was seen between the FUV continuum intensity and the dust extinction, except in the neighborhood of the bright central star, indicating the dust scattering nature of the FUV continuum. We performed Monte-Carlo radiative transfer simulations to obtain the optical parameters related to the dust scattering as well as the geometrical structure of the region. The albedo and asymmetry factor were found to be 0.38±0.06 and 0.46±0.06, respectively, in good agreement with the Milky Way dust grain models. The distance to and the thickness of the interaction zone were estimated to be 70 +4 −8 pc and 40 +8 −10 pc, respectively. The diffuse FUV continuum in the northern region above Spica was mostly the result of scattering of the starlight from Spica, while that in the southern region was mainly due to the background stars. The C IV λλ1548, 1551 emission was found throughout the whole region, in contrast to the Si II* λ1532 emission which was bright only within the H II region. This indicates that the C IV line arises mostly at the shell boundaries of the bubbles, with a larger portion likely from the Loop I than from the Local Bubble side, whereas the Si II* line is from the photoionized Spica nebula.

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“…These limits do not take into account the uncertainty in the dust distribution. Although the bright scattering nebula around HIP 88149 is hidden in the exclusion zone of GALEX, because of the safety restrictions on observing near bright stars, it is prominent in the SPEAR data of Park et al (2012) in the region they call "Ophiuchus". Note that there is no dependence of the modelled or the observed flux on the Galactic latitude.…”

Section: Modelling and Resultsmentioning

confidence: 99%

“…One of the few surveys at low Galactic latitudes was the spectral imaging survey of the SPEAR (Spectroscopy of Plasma Evolution from Astrophysical Radiation: Edelstein et al (2006)) satellite at wavelengths between 900 and 1750 Å. Park et al (2012) combined SPEAR and Galaxy Evolution Explorer (GALEX) data to study the diffuse UV radiation over a 30 square degree region in the vicinity of the Aquila Rift. They deduced that most of the continuum emission was due to dust-scattered light but with contributions from molecular hydrogen fluorescence over part of the field.…”

Section: Introductionmentioning

confidence: 99%

Diffuse Radiation from the Aquila Rift

Jyothy

Murthy

Karuppath

et al. 2015

Mon. Not. R. Astron. Soc.

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We present an analysis of the diffuse ultraviolet (UV) background in a low latitude region near the Aquila Rift based on observations made by the Galaxy Evolution Explorer (GALEX). The UV background is at a level of about 2000 ph cm −2 s −1 srA −1 with no correlation with either the Galactic latitude or the 100 micron infrared (IR) emission. Rather, the UV emission falls off with distance from the bright B2 star HIP 88149, which is in the centre of the field. We have used a Monte Carlo model to derive an albedo of 0.6 -0.7 in the UV with a phase function asymmetry factor (g) of 0.2 -0.4. The value for the albedo is dependent on the dust distribution while g is determined by the extent of the halo.

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FAR-ULTRAVIOLET OBSERVATION OF THE AQUILA RIFT WITHFIMS/SPEAR

Cited by 7 publications

References 43 publications

The Diffuse Galactic Far-Ultraviolet Sky

The Diffuse Galactic Far-Ultraviolet Sky

Far-Ultraviolet Observations of the Spica Nebula and the Interaction Zone

Diffuse Radiation from the Aquila Rift

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