Diffuse far-infrared [$\ion{C}{ii}$] line emission from high Galactic latitude

Makiuti, S.; Shibai, Hiroshi; Okuda, H.; Okumura, K.; Matsuhara, Hideo; Hiromoto, Norihisa; Doi, Yasuo

doi:10.1051/0004-6361:20011626

Cited by 12 publications

(25 citation statements)

References 43 publications

(36 reference statements)

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“…Makiuti et al (2002) conclude that the major source of the [C ii] line emission observed by IRTS/FILM at high Galactic latitudes is the WIM. However, the data and the interpretation for the high latitude diffuse [C ii] emission seen by COBE (cf.…”

Section: Introductionmentioning

confidence: 79%

“…to larger values of b than BICE (Makiuti et al 2002), but FILM only observed [C ii] in a narrow strip along a great circle crossing the plane at l = 50…”

Section: Z-distribution Of [C Ii] Emission Gas Componentsmentioning

confidence: 95%

“…Whereas, those components traced by H i and CO are well established from large scale Galactic surveys, the gas traced by Wright et al 1991;Bennett et al 1994), BIRT (Shibai et al 1991), FILM onboard IRTS (Shibai et al 1994;Makiuti et al 2002), and BICE (Nakagawa et al 1998) are spectrally unresolved. Consequently the z-distribution of the clouds traced by [C ii] still remains not well characterized.…”

Section: Z-distribution Of [C Ii] Emission Gas Componentsmentioning

confidence: 99%

“…In contrast the diffuse H i or WIM component has the largest extent (FWHM ∼ 330 pc), as expected for [C ii] emission from the WIM or diffuse H i and may be consistent with the weak emission observed by FILM at higher latitudes (cf. Makiuti et al 2002). The scale height ∼400 pc for the emission measure (EM) derived from the Wisconsin Hα Mapper (WHAM) data (cf.…”

Section: ) To Estimate the Z-scalesmentioning

confidence: 99%

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Origin andz-distribution of Galactic diffuse [C II] emission

Velusamy

Langer

2014

A&A

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Context. The [C ii] emission is an important probe of star formation in the Galaxy and in external galaxies. The GOT C+ survey and its follow up observations of spectrally resolved 1.9 THz [C ii] emission using Herschel HIFI provides the data needed to quantify the Galactic interstellar [C ii] gas components as tracers of star formation. Aims. We determine the source of the diffuse [C ii] emission by studying its spatial (radial and vertical)

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Section: Introductionmentioning

confidence: 79%

“…to larger values of b than BICE (Makiuti et al 2002), but FILM only observed [C ii] in a narrow strip along a great circle crossing the plane at l = 50…”

Section: Z-distribution Of [C Ii] Emission Gas Componentsmentioning

confidence: 95%

Section: Z-distribution Of [C Ii] Emission Gas Componentsmentioning

confidence: 99%

Section: ) To Estimate the Z-scalesmentioning

confidence: 99%

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Origin andz-distribution of Galactic diffuse [C II] emission

Velusamy

Langer

2014

A&A

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“…Nonetheless, BICE, with its 15 beam, was able to resolve peaks in intensity along several lines of sight. The FILM instrument on board IRTS (Shibai et al 1994;Makiuti et al 2002) had a beam size of 8 × 15 , and a velocity resolution comparable to FIRAS (∼750 km s −1 ), inadequate to resolve any velocity structure. It surveyed the Galaxy only along two 5 • wide bands forming a great circle on the sky.…”

Section: Introductionmentioning

confidence: 99%

AHerschel[C ii] Galactic plane survey

Langer

Velusamy

Pineda

et al. 2014

A&A

153

184

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Context. H i and CO large scale surveys of the Milky Way trace the diffuse atomic clouds and the dense shielded regions of molecular hydrogen clouds, respectively. However, until recently, we have not had spectrally resolved C + surveys in sufficient lines of sight to characterize the ionized and photon dominated components of the interstellar medium, in particular, the H 2 gas without CO, referred to as CO-dark H 2 , in a large sample of interstellar clouds.Aims. We use a sparse Galactic plane survey of the 1.9 THz (158 μm) [C ii] spectral line from the Herschel open time key programme, Galactic Observations of Terahertz C+ (GOT C+), to characterize the H 2 gas without CO in a statistically significant sample of interstellar clouds.Methods. We identify individual clouds in the inner Galaxy by fitting the [C ii] and CO isotopologue spectra along each line of sight. We then combine these spectra with those of H i and use them along with excitation models and cloud models of C + to determine the column densities and fractional mass of CO-dark H 2 clouds.Results. We identify1804 narrow velocity [C ii] components corresponding to interstellar clouds in different categories and evolutionary states. About 840 are diffuse molecular clouds with no CO, ∼510 are transition clouds containing [C ii] and 12 CO, but no 13 CO, and the remainder are dense molecular clouds containing 13 CO emission. The CO-dark H 2 clouds are concentrated between Galactic radii of ∼3.5 to 7.5 kpc and the column density of the CO-dark H 2 layer varies significantly from cloud to cloud with a global average of 9 × 10 20 cm −2 . These clouds contain a significant fraction by mass of CO-dark H 2 , that varies from ∼75% for diffuse molecular clouds to ∼20% for dense molecular clouds.Conclusions. We find a significant fraction of the warm molecular ISM gas is invisible in H i and CO, but is detected in [C ii]. The fraction of CO-dark H 2 is greatest in the diffuse clouds and decreases with increasing total column density, and is lowest in the massive clouds. The column densities and mass fraction of CO-dark H 2 are less than predicted by models of diffuse molecular clouds using solar metallicity, which is not surprising as most of our detections are in Galactic regions where the metallicity is larger and shielding more effective. There is an overall trend towards a higher fraction of CO-dark H 2 in clouds with increasing Galactic radius, consistent with lower metallicity there.

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Infrared Sky Surveys

Price

2009

Space Sci Rev

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A retrospective is given on infrared sky surveys from Thomas Edison's proposal in the late 1870s to IRAS, the first sensitive mid-to far-infrared all-sky survey, and the mid-1990s experiments that filled in the IRAS deficiencies. The emerging technology for space-based surveys is highlighted, as is the prominent role the US Defense Department, particularly the Air Force, played in developing and applying detector and cryogenic sensor advances to early mid-infrared probe-rocket and satellite-based surveys. This technology was transitioned to the infrared astronomical community in relatively short order and was essential to the success of IRAS, COBE and ISO. Mention is made of several of the little known early observational programs that were superseded by more successful efforts.

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Diffuse far-infrared [$\ion{C}{ii}$] line emission from high Galactic latitude

Cited by 12 publications

References 43 publications

Origin andz-distribution of Galactic diffuse [C II] emission

Origin andz-distribution of Galactic diffuse [C II] emission

AHerschel[C ii] Galactic plane survey

Infrared Sky Surveys

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