Pure Rotational Spectra of SO: Rare Isotopomers in the 80-GHz to 1.1-THz Region

Klaus, Th.; Saleck, A. H.; Белов, С. П.; Winnewisser, G.; Hirahara, Yasuhiro; Hayashi, Masato; Kagi, Eriko; Kawaguchi, K.

doi:10.1006/jmsp.1996.0243

Cited by 36 publications

(13 citation statements)

References 13 publications

(19 reference statements)

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“…Its rotational levels are characterized by the rotational angular momentum quantum number, N, and the total angular momentum 2 Spectroscopic parameters for SO (dipole moment μ = 1.535 D) have been obtained from Clark & DeLucia (1976), Tiemann (1982, Lovas et al (1992), Cazzoli et al (1994), Klaus et al (1996), Bogey et al (1997), Powell &Lide (1964), andMartin-Drumel (2012). For 34 SO and S 18 O (μ = 1.535 D) from Tiemann (1974), Tiemann (1982, Lovas et al (1992), Klaus et al (1996), Bogey et al (1982), and Powell & Lide (1964). And for 33 SO (μ = 1.535 D) from Klauss et al (1996), Lovas et al (1992), and Powell & Lide (1964).…”

Section: Resultsmentioning

confidence: 99%

A line confusion-limited millimeter survey of Orion KL

Esplugues

Tercero

Cernicharo

et al. 2013

A&A

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Context. We present a study of the sulfur-bearing species detected in a line confusion-limited survey towards Orion KL performed with the IRAM 30-m telescope in the frequency range 80−281 GHz. Aims. This study is part of an analysis of the line survey divided into families of molecules. Our aim is to derive accurate physical conditions, as well as molecular abundances, in the different components of Orion KL from observed SO and SO 2 lines. Methods. As a starting point, we assumed local thermodynamic equilibrium (LTE) conditions obtain rotational temperatures. We then used a radiative transfer model, assuming either LVG or LTE excitation to derive column densities of these molecules in the different components of Orion KL. = 1 and for several undetected sulfur-bearing species. In addition, we present 2 × 2 maps around Orion IRc2 of SO 2 transitions with energies from 19 to 131 K and also maps with four transitions of SO, 34 SO, and 34 SO 2 . We observe an elongation of the gas along the NE-SW direction. An unexpected emission peak appears at 20.5 km s −1 in most lines of SO and SO 2 . A study of the spatial distribution of this emission feature shows that it is a new component of a few arcseconds (∼5 ) in diameter, which lies ∼4 west of IRc2. We suggest the emission from this feature is related to shocks associated to the BN object. Conclusions. The highest column densities for SO and SO 2 are found in the high-velocity plateau (a region dominated by shocks) and in the hot core. These values are up to three orders of magnitude higher than the results for the ridge components. We also find high column densities for their isotopologues in both components. Therefore, we conclude that SO and SO 2 are good tracers, not only of regions affected by shocks, but also of regions with warm dense gas (hot cores).

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Section: Resultsmentioning

confidence: 99%

A line confusion-limited millimeter survey of Orion KL

Esplugues

Tercero

Cernicharo

et al. 2013

A&A

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“…(3) For each species, the spectroscopic references given here are the most recent cited in the CDMS and JPL databases. All of them should be read as reference and references therein: (aa) Winnewisser et al (1997); (ab) Cazzoli et al (2004); (ac) Klapper et al (2001); (ad) Klapper et al (2003); (ae) Bogey et al (1997); (a f ) Klaus et al (1996); (ag) Müller et al (2000d); (ah) Bocquet et al (1999); (ai) Müller et al (2000c); (a j) Lohilahti & Horneman (2004); (ak) Müller et al (2000b); (al) Müller et al (2000a); (am) Belov et al (1998); (an) Müller et al (2004); ( Kim & Yamamoto (2003); (aw) Thorwirth et al (2003); (ax) ; (ay) Brünken et al (2004); (az) ; (ba) Kleiner et al (1996); (bb) Müller et al (2009);(bc) Clouthier et al (1994); (bd) Brown et al (1987); (be) Minowa et al (1997); (b f ) Golubiatnikov et al (2005); (bg) Lovas & Suenram (1987); (bh) Maeda et al (2008); (bi) Cho & Saito (1998); (b j) Thorwirth et al (2000a); (bk) Brünken et al (2006); (bl) Thorwirth et al (2000b); (bm) Spahn et al (2008); (bn) Belov (1995); (bo) Camy-Peyret et al (1985); (bp) …”

Section: Line Parametersmentioning

confidence: 99%

TIMASSS: the IRAS 16293-2422 millimeter and submillimeter spectral survey

Caux

Kahane

Castets

et al. 2011

A&A

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Context. Unbiased spectral surveys are powerful tools to study the chemistry and the physics of star forming regions, because they can provide a complete census of the molecular content and the observed lines probe the physical structure of the source. Aims. While unbiased surveys at the millimeter and sub-millimeter wavelengths observable from ground-based telescopes have previously been performed towards several high mass protostars, very little exists on low mass protostars, which are believed to resemble our own Sun's progenitor. To help fill up this gap in our understanding, we carried out a complete spectral survey of the bands at 3, 2, 1, and 0.9 mm towards the solar type protostar IRAS 16293-2422. Methods. The observations covered a range of about 200 GHz and were obtained with the IRAM-30 m and JCMT-15 m telescopes during about 300 h of observations. Particular attention was devoted to the inter-calibration of the acquired spectra with previous observations. All the lines detected with more than 3σ confidence-interval certainty and free from obvious blending effects were fitted with Gaussians to estimate their basic kinematic properties. Results. More than 4000 lines were detected (with σ ≥ 3) and identified, yielding a line density of approximatively 20 lines per GHz, comparable to previous surveys in massive hot cores. The vast majority (about two-thirds) of the lines are weak and produced by complex organic molecules. The analysis of the profiles of more than 1000 lines belonging to 70 species firmly establishes the presence of two distinct velocity components associated with the two objects, A and B, forming the IRAS 16293-2422 binary system. In the source A, the line widths of several species increase with the upper level energy of the transition, a behavior compatible with gas infalling towards a ∼1 M object. The source B, which does not show this effect, might have a much lower central mass of ∼0.1 M . The difference in the rest velocities of both objects is consistent with the hypothesis that the source B rotates around the source A. Conclusions. This spectral survey, although obtained with single-dish telescopes at a low spatial resolution, allows us to separate the emission from two different components, thanks to the large number of lines detected. The data of the survey are public and can be retrieved on the TIMASSS web site .

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“…The K = 3−2 data in Belov et al (1994) is too low compared with the data reported in Behrend et al (1990) by about 300 kHz with rather small scatter. The absence of a reference signal in, e.g., Belov et al (1994) could be an explanation, see SO data in Klaus et al (1994) and Klaus et al (1996). Therefore, the K = 3−2 data from Belov et al (1994) were omitted from the fit.…”

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confidence: 99%

The sulfur depletion problem: upper limits on the H₂S₂, HS^·₂, and S₂gas-phase abundances toward the low-mass warm core IRAS 16293-2422

Martín-Doménech

Jiménez-Serra

Muñoz

et al. 2016

A&A

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Context. A fraction of the missing sulfur in dense clouds and circumstellar regions could be in the form of three species not yet detected in the interstellar medium: H 2 S 2 , HS . 2 , and S 2 according to experimental simulations performed under astrophysically relevant conditions. These S-S bonded molecules can be formed by the energetic processing of H 2 S-bearing ice mantles on dust grains, and subsequently desorb to the gas phase. Aims. The detection of these species could partially solve the sulfur depletion problem, and would help to improve our knowledge of the poorly known chemistry of sulfur in the interstellar medium. To this purpose we calculated the frequencies and expected intensities of the rotational transitions not previously reported, and performed dedicated ground-based observations toward the low-mass warm core IRAS 16293-2422, a region with one of the highest measured gas-phase H 2 S abundances. Methods. Observations in the submillimeter regime were obtained with the APEX 12 m telescope during 15 h of observation. A total of ∼16 GHz were covered in a range of about 100 GHz, targeting a wide selection of the predicted rotational transitions of the three molecules.Results. The 1σ noise rms values were extracted in the spectral regions where the targeted species should have been detected. These values were a factor of 2−7 lower than those reached by previous observations toward the same source, and allowed us to estimate a 1σ upper limit to their molecular abundances of ≤8.1 × 10 −9 , ≤1.1 × 10 −8 , and ≤2.9 × 10 −7 relative to H 2 , for H 2 S 2 , HS . 2 , and S 2 , respectively. Conclusions. The upper limit abundances of the three molecules containing the S 2 unit are up to two orders of magnitude lower than the H 2 S abundance in the source, and one order of magnitude lower than the expected abundances from the experimental simulations using ice analogs. Subsequent gas-phase chemistry after desorption could lower the abundances of the three species to undetectable levels in our observations.

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Pure Rotational Spectra of SO: Rare Isotopomers in the 80-GHz to 1.1-THz Region

Cited by 36 publications

References 13 publications

A line confusion-limited millimeter survey of Orion KL

A line confusion-limited millimeter survey of Orion KL

TIMASSS: the IRAS 16293-2422 millimeter and submillimeter spectral survey

The sulfur depletion problem: upper limits on the H₂S₂, HS^·₂, and S₂gas-phase abundances toward the low-mass warm core IRAS 16293-2422

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Pure Rotational Spectra of SO: Rare Isotopomers in the 80-GHz to 1.1-THz Region

Cited by 36 publications

References 13 publications

A line confusion-limited millimeter survey of Orion KL

A line confusion-limited millimeter survey of Orion KL

TIMASSS: the IRAS 16293-2422 millimeter and submillimeter spectral survey

The sulfur depletion problem: upper limits on the H2S2, HS·2, and S2gas-phase abundances toward the low-mass warm core IRAS 16293-2422

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The sulfur depletion problem: upper limits on the H₂S₂, HS^·₂, and S₂gas-phase abundances toward the low-mass warm core IRAS 16293-2422