Far-infrared Detection of C[TINF]3[/TINF] in Sagittarius B2 and IRC +10216

Cernicharo, J.; Goicoechea, J. R.; Caux, E.

doi:10.1086/312668

Cited by 139 publications

(179 citation statements)

References 25 publications

Supporting

Mentioning

162

Contrasting

Order By: Relevance

“…Sternberg & Dalgarno 1995). The abundance patterns that we see in diffuse molecular gas are clearly different from those in Sgr B2, where NH 3 /NH 2 /NH ∼ 100/10/1 and the fractional abundance of NH is a few times ×10 −9 (Cernicharo et al 2000;Goicoechea et al 2004). …”

Section: Discussioncontrasting

confidence: 67%

“…Interstellar NH 2 was first observed by van Dishoeck et al (1993) in absorption towards Sgr B2 in three fine-structure components of the para-NH 2 1 1,0 −1 0,1 transition with partially resolved hyperfine structure at frequencies 461 to 469 GHz. Further absorption lines of both ortho and para forms of NH 2 and NH were observed through use of the long-wavelength spectrometer aboard ISO (Cernicharo et al 2000;Goicoechea et al 2004;Polehampton et al 2007). The ISO observations were unable to resolve the hyperfine structure of either molecule.…”

Section: By Optical Absorptionmentioning

confidence: 99%

See 1 more Smart Citation

Nitrogen hydrides in interstellar gas

Persson¹,

Black²,

Cernicharo

et al. 2010

A&A

View full text Add to dashboard Cite

The HIFI instrument on board the Herschel Space Observatory has been used to observe interstellar nitrogen hydrides along the sight-line towards G10.6−0.4 in order to improve our understanding of the interstellar chemistry of nitrogen. We report observations of absorption in NH N = 1 ← 0, J = 2 ← 1 and ortho-NH 2 1 1,1 ← 0 0,0 . We also observed ortho-NH 3 1 0 ← 0 0 , and 2 0 ← 1 0 , para-NH 3 2 1 ← 1 1 , and searched unsuccessfully for NH + . All detections show emission and absorption associated directly with the hot-core source itself as well as absorption by foreground material over a wide range of velocities. All spectra show similar, non-saturated, absorption features, which we attribute to diffuse molecular gas. Total column densities over the velocity range 11−54 km s −1 are estimated. The similar profiles suggest fairly uniform abundances relative to hydrogen, approximately 6 × 10 −9 , 3 × 10 −9 , and 3 × 10 −9 for NH, NH 2 , and NH 3 , respectively. These abundances are discussed with reference to models of gas-phase and surface chemistry.

show abstract

Section: Discussioncontrasting

confidence: 67%

Section: By Optical Absorptionmentioning

confidence: 99%

Nitrogen hydrides in interstellar gas

Persson¹,

Black²,

Cernicharo

et al. 2010

A&A

View full text Add to dashboard Cite

show abstract

“…Previous searches had been unsuccessful (Snow et al 1988;Clegg & Lambert 1982). The infrared spectrum of C 3 was measured in the circumstellar envelope of CW Leo (IRC +10216) by Hinkle et al (1988), and in interstellar absorption toward Sgr B2 by Cernicharo et al (2000). Giesen et al (2001) discussed new laboratory data on the vibrational spectrum of C 3 in its low-frequency bending mode and re-visited an earlier tentative identification of the ν 2 R(2) line in absorption toward Sgr B2 (Van Orden et al 1995).…”

Section: Introductionmentioning

confidence: 99%

Interstellar C$_\mathsf{3}$ toward HD 210121

Roueff¹,

Felenbok²,

Black³

et al. 2002

A&A

View full text Add to dashboard Cite

Abstract.We report the detection of the 405 nm band of interstellar C3 in absorption toward HD 210121. The abundance of triatomic carbon is approximately 1/17 of that of diatomic carbon in the same diffuse molecular cloud. Rotational levels of C3 up to J = 14 are seen in this cloud. The rotational excitation of C3 in the interstellar medium may reflect a competition between inelastic collisions, formation and destruction of the molecule, and radiative pumping in the far-infrared. The abundance of C3 is compared with chemical models. Attention is called to molecular properties that need to be better determined.

show abstract

“…Triatomic carbon, C 3 , was first tentatively identified in interstellar gas by Van Orden et al (1995) and Haffner & Meyer (1995). The mid-infrared spectrum of C 3 (ν 3 antisymmetric stretching mode) was measured in the circumstellar envelope of CW Leo (IRC +10216) by Hinkle et al (1988), and in lowresolution interstellar absorption in the far-IR (ν 2 bending mode) toward Sgr B2 by Cernicharo et al (2000). Giesen et al (2001) discussed new laboratory data on the vibrational spectrum of C 3 in its low-frequency bending mode and re-visited the first identification of the ν 2 R(2) line in absorption toward Sgr B2 (Van Orden et al 1995).…”

Section: Introductionmentioning

confidence: 99%

Excitation and abundance of C₃in star forming cores

Mookerjea¹,

Giesen

Stützki

et al. 2010

A&A

View full text Add to dashboard Cite

We present spectrally resolved observations of triatomic carbon (C 3 ) in several ro-vibrational transitions between the vibrational ground state and the low-energy ν 2 bending mode at frequencies between 1654−1897 GHz along the sight-lines to the submillimeter continuum sources W31C and W49N, using Herschel's HIFI instrument. We detect C 3 in absorption arising from the warm envelope surrounding the hot core, as indicated by the velocity peak position and shape of the line profile. The sensitivity does not allow to detect C 3 absorption due to diffuse foreground clouds. From the column densities of the rotational levels in the vibrational ground state probed by the absorption we derive a rotation temperature (T rot ) of ∼50−70 K, which is a good measure of the kinetic temperature of the absorbing gas, as radiative transitions within the vibrational ground state are forbidden. It is also in good agreement with the dust temperatures for W31C and W49N. Applying the partition function correction based on the derived T rot , we get column densities N(C 3 ) ∼ 7−9 × 10 14 cm −2 and abundance x(C 3 ) ∼ 10 −8 with respect to H 2 . For W31C, using a radiative transfer model including far-infrared pumping by the dust continuum and a temperature gradient within the source along the line of sight we find that a model with x(C 3 ) = 10 −8 , T kin = 30−50 K, N(C 3 ) = 1.5 × 10 15 cm −2 fits the observations reasonably well and provides parameters in very good agreement with the simple excitation analysis.

show abstract

Far-infrared Detection of C[TINF]3[/TINF] in Sagittarius B2 and IRC +10216

Cited by 139 publications

References 25 publications

Nitrogen hydrides in interstellar gas

Nitrogen hydrides in interstellar gas

Interstellar C$_\mathsf{3}$ toward HD 210121

Excitation and abundance of C₃in star forming cores

Contact Info

Product

Resources

About

Far-infrared Detection of C[TINF]3[/TINF] in Sagittarius B2 and IRC +10216

Cited by 139 publications

References 25 publications

Nitrogen hydrides in interstellar gas

Nitrogen hydrides in interstellar gas

Interstellar C$_\mathsf{3}$ toward HD 210121

Excitation and abundance of C3in star forming cores

Contact Info

Product

Resources

About

Excitation and abundance of C₃in star forming cores