Detection of [N [CSC]ii[/CSC]] λ5755 Emission from Low-Density Ionized Interstellar Gas

Reynolds, R. J.; Sterling, N. C.; Haffner, L. M.; Tufte, S. L.

doi:10.1086/319119

Cited by 30 publications

(27 citation statements)

References 20 publications

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“…Models of N + in the WIM at T K = 8000 K reproduce both the submm-wave absorption towards W 49N and W 31C reported here and the intensities of [N ii] 6583, 5755, and Hα 6563 Å reported by Reynolds et al (2001). The latter refer to emission lines over a one-degree region in the direction G130.0 − 7.5 in several broad velocity components with corresponding kinematical distances between 0.6 kpc and 9.7 kpc.…”

Section: Radex Modellingsupporting

confidence: 71%

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First detection of [N II] 205μm absorption in interstellar gas

Persson

Gérin

Mookerjea

et al. 2014

A&A

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We present high resolution [N ii] 205 μm ( 3 P 1 − 3 P 0 ) spectra obtained with Herschel-HIFI towards a small sample of far-infrared bright star forming regions in the Galactic plane: W 31C (G10.6−0.4), W 49N (G43.2−0.1), W 51 (G49.5−0.4), and G34.3+0.1. The detection of the 205 μm line in absorption emphasises the importance of a high spectral resolution, and also offers a new tool for investigation of the WIM.

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Section: Radex Modellingsupporting

confidence: 71%

“…The same conditions explain the diffuse optical emission lines of [N ii] and Hα (Reynolds et al 2001). The real interstellar medium is, however, more complex than our static, uniform models; in particular, the WIM represents an average over space and time of wildly varying conditions (Dong & Draine 2011).…”

Section: Radex Modellingmentioning

confidence: 54%

First detection of [N II] 205μm absorption in interstellar gas

Persson

Gérin

Mookerjea

et al. 2014

A&A

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“…The last six rows show the data obtained for sight lines that sample the much fainter diffuse ionized medium. One WIM sight line, (130 , À7N5), was reported previously by Reynolds et al (2001b). For some directions, [N ii] k5755 was not detected, and only upper limits to the line ratio of [N ii] k5755/[N ii] k6584 are given, as described in x 3.3.…”

Section: Observations Of [N Ii] K5755mentioning

confidence: 84%

“…In addition, the elevated [N ii]/ H and [S ii]/ H ratios in the WIM suggest that this low-density diffuse gas is significantly warmer than traditional H ii regions and may require spectral processing of the stellar radiation (e.g., Wood & Mathis 2004) and /or an additional heating source beyond photoionization ). Recent observations of [ N ii] k5755/ [N ii] k6583 have indeed confirmed that the WIM is about 2000 K warmer than H ii regions (Reynolds et al 2001b). …”

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confidence: 86%

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A Multiwavelength Optical Emission Line Survey of Warm Ionized Gas in the Galaxy

Madsen

Reynolds²,

Haffner³

2006

ApJ

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172

270

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We report on observations of several optical emission lines toward a variety of newly revealed faint, large-scale H -emitting regions in the Galaxy. The lines include [, and He i k5876 obtained with the Wisconsin H Mapper (WHAM ) toward sight lines that probe superbubbles, high-latitude filamentary features, and the more diffuse warm ionized medium ( WIM). Our observations include maps covering thousands of square degrees toward the well-known Orion-Eridanus bubble, a recently discovered 60; 20 bipolar superbubble centered in Perseus, plus several classical H ii regions surrounding OB stars and hot evolved stellar cores. We use the emission-line data to explore the temperature and ionization conditions within the emitting gas and their variations between the different emission regions. We find that in the diffuse WIM and in the faint high-latitude filamentary structures the line ratios of [ N ii]/H and [S ii]/H are generally high, while [O iii]/ H and He i/H are generally low compared to the bright classical H ii regions. This suggests that the gas producing this faint widespread emission is warmer, in a lower ionization state, and ionized by a softer spectrum than gas in classical H ii regions surrounding O stars, the presumed ionization source for the WIM. In addition, we find differences in physical conditions between the large bubble structures and the more diffuse WIM, suggesting that the ionization of superbubble walls by radiation from interior O associations does not account entirely for the range of conditions found within the WIM, particularly the highest values of [ N ii]/H and [S ii]/ H .

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The Wham Northern Sky Survey and the Nature of the Warm Ionized Medium in the Galaxy

Madsen

Astrophysics and Space Science Library

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The Wisconsin H-Alpha Mapper (WHAM) has completed a velocity-resolved map of diffuse Hα emission of the entire northern sky, providing the first comprehensive picture of both the distribution and kinematics of diffuse ionized gas in the Galaxy. WHAM continues to advance our understanding of the physical conditions of the warm ionized medium through observations of other optical emission lines throughout the Galactic disk and halo. We discuss some highlights from the survey, including an optical window into the inner Galaxy and the relationship between H I and H II in the diffuse ISM.

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Detection of [N [CSC]ii[/CSC]] λ5755 Emission from Low-Density Ionized Interstellar Gas

Cited by 30 publications

References 20 publications

First detection of [N II] 205μm absorption in interstellar gas

First detection of [N II] 205μm absorption in interstellar gas

A Multiwavelength Optical Emission Line Survey of Warm Ionized Gas in the Galaxy

The Wham Northern Sky Survey and the Nature of the Warm Ionized Medium in the Galaxy

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