Perspective from a Younger Generation — The Astro-spectroscopy of Gisbert Winnewisser

Menten, K. M.

doi:10.1007/978-3-642-18902-9_11

Cited by 7 publications

(5 citation statements)

References 99 publications

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“…This higher spatial resolution allows separation of different components in a complex source like Sgr B2; iv) the observed line intensity ratios are consistent with those predicted in the LTE approximation; v) it should also be noted that all lines of HOCN with an expected intensity over the noise level have either been detected or are blended in the covered frequency range towards the six selected sources; i.e., no expected lines are missing. HNCO is ubiquitous throughout the Central Molecular Zone (CMZ) of our Galaxy (Menten 2004), stretching from longitudes of −0.2 to 1.8 degrees over a ∼300 pc long band along the Galactic plane (Dahmen et al 1997). In Sgr B2 -the most prominent molecular emission region within the CMZ -the molecule exhibits large-scale abundance variations peaking not at the hot core positions -where most other molecules show strong emission -but rather has an extended ring-like structure, investigated in detail by Minh & Irvine (2006) and Jones et al (2008).…”

Section: Discussionmentioning

confidence: 99%

Interstellar HOCN in the Galactic center region

Brünken¹,

Беллоче

Martín

et al. 2010

A&A

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Aims. Our aim is to confirm the interstellar detection of cyanic acid, HOCN, in the Galactic center clouds. It has previously been tentatively detected only in Sgr B2(OH). Methods. We used a complete line survey of the hot cores Sgr B2(N) and (M) in the 3 mm range, complemented by additional observations carried out with the IRAM 30 m telescope at selected frequencies in the 2 mm band and towards four additional positions in the Sgr B2 cloud complex in the 2 and 3 mm bands. The spectral survey was analysed in the local thermodynamical equilibrium approximation (LTE) by modeling the emission of all identified molecules simultaneously. This allowed us to distinguish weak features of HOCN from the rich line spectrum observed in Sgr B2(N) and (M). Lines of the more stable (by 1.1 eV) isomer isocyanic acid, HNCO, in these sources, as well as those of HOCN and HNCO towards the other positions, were analysed in the LTE approximation as well. Results. Four transitions of HOCN were detected in a quiescent molecular cloud in the Galactic center at a position offset in (RA, Dec) by (20 , 100 ) from the hot core source Sgr B2(M), confirming its previous tentative interstellar detection. Up to four transitions were detected toward five other positions in the Sgr B2 complex, including the hot cores Sgr B2(M), (S), and (N). A fairly constant abundance ratio of ∼0.3−0.8% for HOCN relative to HNCO was derived for the extended gas components, suggesting a common formation process of these isomers.

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Section: Discussionmentioning

confidence: 99%

Interstellar HOCN in the Galactic center region

Brünken¹,

Беллоче

Martín

et al. 2010

A&A

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“…At submillimeter wavelengths, numerous molecules have been detected in absorption via their ground-state transitions (until recently mostly) toward Sgr B2 (for summaries see Menten 2004;Lis et al 2009). In particular, the 1 10 −1 01 transition of ortho-H 16 2 O and -H 18 2 O was detected with the Submillimeter Wave Astronomy Satellite (Neufeld et al 2000); this H 16 2 O line, near 557 GHz, is responsible for much of the Earth atmosphere's shorter-wavelength submillimeter opacity.…”

Section: (Sub)millimeter Spectroscopy Of Diffuse Interstellar Cloudsmentioning

confidence: 99%

Submillimeter absorption from SH⁺, a new widespread interstellar radical,¹³CH⁺and HCl

Menten

Wyrowski

Беллоче

et al. 2010

A&A

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We have used the Atacama Pathfinder Experiment 12 m telescope (APEX) to carry out an absorption study of submillimeter wavelength rotational ground-state lines of H 35 Cl, H 37 Cl, 13 CH + , and, for the first time, of the SH + radical (sulfoniumylidene or sulfanylium). We detected the quartet of ground-state hyperfine structure lines of SH + near 683 GHz with the CHAMP+ array receiver against the strong continuum source Sagittarius B2, which is located close to the center of our Galaxy. In addition to absorption from various kinematic components of Galactic center gas, we also see absorption at the radial velocities belonging to intervening spiral arms. This demonstrates that SH + is a ubiquitous component of the diffuse interstellar medium. We do not find clear evidence for other SH + lines we searched for, which is partially due to blending with lines from other molecules. In addition to SH + , we observed absorption from H 35 Cl, H 37 Cl, and 13 CH + . The observed submillimeter absorption is compared in detail with absorption in 3 mm transitions of H 13 CO + and c-C 3 H 2 and the CO J = 1−0 and 3−2 transitions.

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“…G1.6−0.025 IS AT THE OUTER REACHES OF THE GALACTIC CENTER ORGANIC MOLECULE REGION There actually is evidence for a giant repository of organic molecules coextensive with the CMZ, of which G1.6−0.025 demarcates the high-longitude border (Menten 2004).…”

Section: Shock Chemistry In G16−0025mentioning

confidence: 99%

Molecules in G1.6–0.025—“HOT” Chemistry in the Absence of Star Formation at the Periphery of the Galactic Center Region

Menten

Wilson

Leurini

et al. 2009

ApJ

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We present molecular line mapping of the Giant Molecular Cloud G1.6−0.025, which is located at the highlongitude end of the Central Molecular Zone (CMZ) of our Galaxy. We assess the degree of star formation activity in that region using several tracers, and find very little. We made a large-scale, medium (2 ) resolution map in the J = 2 − 1 transition of SiO for which we find clumpy emission over a ∼ 0.• 8 × 0.• 3 sized region stretching along the Galactic plane. Toward selected positions we also took spectra in the easy-to-excite J k = 2 k − 1 k quartet of CH 3 OH and the carbon monosulfide (CS) 2 − 1 line. Throughout the cloud these CH 3 OH lines are, remarkably, several times stronger than both the CS and the SiO lines. The large widths of all the observed lines, similar to values generally found in the Galactic center, indicate a high degree of turbulence. Several high LSR velocity clumps that have 50-80 km s −1 higher velocities than the bulk of the molecular cloud appear at the same projected position as "normal" velocity material; this may indicate cloud-cloud collisions. Statistical equilibrium modeling of the CH 3 OH lines observed by us and others yields relatively high densities and moderate temperatures for a representative dual velocity position. We find 8×10 4 cm −3 /30 K for material in the G1.6−0.025 cloud and a higher temperature (190 K), but a 50% lower density in a high-velocity clump projected on the same location. Several scenarios are discussed in which shock chemistry might enhance the CH 3 OH and SiO abundances in G1.6−0.025 and elsewhere in the CMZ.

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Perspective from a Younger Generation — The Astro-spectroscopy of Gisbert Winnewisser

Cited by 7 publications

References 99 publications

Interstellar HOCN in the Galactic center region

Interstellar HOCN in the Galactic center region

Submillimeter absorption from SH⁺, a new widespread interstellar radical,¹³CH⁺and HCl

Molecules in G1.6–0.025—“HOT” Chemistry in the Absence of Star Formation at the Periphery of the Galactic Center Region

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Perspective from a Younger Generation — The Astro-spectroscopy of Gisbert Winnewisser

Cited by 7 publications

References 99 publications

Interstellar HOCN in the Galactic center region

Interstellar HOCN in the Galactic center region

Submillimeter absorption from SH+, a new widespread interstellar radical,13CH+and HCl

Molecules in G1.6–0.025—“HOT” Chemistry in the Absence of Star Formation at the Periphery of the Galactic Center Region

Contact Info

Product

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Submillimeter absorption from SH⁺, a new widespread interstellar radical,¹³CH⁺and HCl