Searching for trans ethyl methyl ether in Orion KL

Tercero, B.; Cernicharo, J.; López, Alicia; Brouillet, N.; Kolesníková, Lucie; Motiyenko, R. A.; Margulès, L.; Alonso, José L.; Guillemin, Jean‐Claude

doi:10.1051/0004-6361/201526255

Cited by 61 publications

(92 citation statements)

References 31 publications

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“…0 compared to 2 × 1 . 5, Tercero et al 2015) and a much better sensitivity (SV0 sensitivity is in the range 10-30 mJy beam −1 , Hirota et al 2012, compared to 2-8 mJy beam −1 in the present study). The data were re-calibrated using the provided python script (scriptforPI.py) in the Common Astronomy Software Applications (CASA) package V.4.2.2 (McMullin et al 2007).…”

Section: Observations and Data Processingsupporting

confidence: 43%

“…The coincidence of the two species is therefore not systematic and this different shape reflects an ongoing chemical evolution which deserves proper attention once the zero-spacing data is added. Similarly, Tercero et al (2015) mention a different peak position for 13 CH 3 OH and methyl formate along the ridge centered on the HC peak which they also interpret as ongoing transformation of methanol to methyl formate.…”

Section: Chemical Complexitymentioning

confidence: 96%

“…Naturally, interferometers have been used to separate the components, diminish the confusion, and help understand the ongoing evolution of the chemical and physical complex structure (e.g. Favre et al 2011a;Peng et al 2012Peng et al , 2017Brouillet et al 2013;Feng et al 2015;Tercero et al 2015).…”

Section: Introductionmentioning

confidence: 99%

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The complexity of Orion: an ALMA view

Pagani

Favre

Goldsmith

et al. 2017

A&A

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Context. We wish to improve our understanding of the Orion central star formation region (Orion-KL) and disentangle its complexity. Aims. We collected data with ALMA during cycle 2 in 16 GHz of total bandwidth spread between 215.1 and 252.0 GHz with a typical sensitivity of 5 mJy/beam (2.3 mJy/beam from 233.4 to 234.4 GHz) and a typical beam size of 1 . 7 × 1 . 0 (average position angle of 89 • ). We produced a continuum map and studied the emission lines in nine remarkable infrared spots in the region including the hot core and the compact ridge, plus the recently discovered ethylene glycol peak. Methods. We present the data, and report the detection of several species not previously seen in Orion, including n-and i-propyl cyanide (C 3 H 7 CN), and the tentative detection of a number of other species including glycolaldehyde (CH 2 (OH)CHO). The first detections of gGg ethylene glycol (gGg (CH 2 OH) 2 ) and of acetic acid (CH 3 COOH) in Orion are presented in a companion paper. We also report the possible detection of several vibrationally excited states of cyanoacetylene (HC 3 N), and of its 13 C isotopologues. We were not able to detect the 16 O 18 O line predicted by our detection of O 2 with Herschel, due to blending with a nearby line of vibrationally excited ethyl cyanide. We do not confirm the tentative detection of hexatriynyl (C 6 H) and cyanohexatriyne (HC 7 N) reported previously, or of hydrogen peroxide (H 2 O 2 ) emission. Results. We report a complex velocity structure only partially revealed before. Components as extreme as −7 and +19 km s −1 are detected inside the hot region. Thanks to different opacities of various velocity components, in some cases we can position these components along the line of sight. We propose that the systematically redshifted and blueshifted wings of several species observed in the northern part of the region are linked to the explosion that occurred ∼500 yr ago. The compact ridge, noticeably farther south displays extremely narrow lines (∼1 km s −1 ) revealing a quiescent region that has not been affected by this explosion. This probably indicates that the compact ridge is either over 10 000 au in front of or behind the rest of the region. Conclusions. Many lines remain unidentified, and only a detailed modeling of all known species, including vibrational states of isotopologues combined with the detailed spatial analysis offered by ALMA enriched with zero-spacing data, will allow new species to be detected.

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Section: Observations and Data Processingsupporting

confidence: 43%

Section: Chemical Complexitymentioning

confidence: 96%

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The complexity of Orion: an ALMA view

Pagani

Favre

Goldsmith

et al. 2017

A&A

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“…In space, COMs have been unambiguously identified in very different environments , such as toward the Galactic Centre in hot cores and giant molecular clouds (Hollis, Lovas & Jewell 2000;Martín-Pintado et al 2001;Requena-Torres et al 2006Belloche et al 2013), toward low-and high-mass proto-stars (Blake et al 1987;Neill et al 2014;Tercero et al 2015;Jørgensen et al 2012Jørgensen et al , 2016Caselli & Ceccarelli 2012;Coutens et al 2015;Taquet et al 2015;Rivilla et al 2016), molecular outflows (Arce et al 2008;Codella et al 2015), photon-dominated regions (Guzmán et al 2013), as well as toward dark cloud cores and pre-stellar cores (Marcelino et al 2007;Bacmann et al 2012;Ö berg et al 2010Cernicharo et al 2012;Vastel et al 2014;Jiménez-Serra et al 2016). With eight and 10 atoms, the simplest sugar, glycolaldehyde (HC(O)CH2OH, hereafter GA), and the simplest sugar alcohol, ethylene glycol (H2C(OH)CH2OH, hereafter EG), can be considered amongst the largest organic molecules detected so far in the interstellar medium (ISM).…”

Section: Introductionmentioning

confidence: 99%

Production of complex organic molecules:H-atom addition versus UV irradiation

Chuang

Fedoseev

Qasim

et al. 2017

Mon. Not. R. Astron. Soc.

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AB S TRAC TComplex organic molecules (COMs) have been identified in different environments in starforming regions. Laboratory studies show that COMs form in the solid state, on icy grains, typically following a 'non-energetic' (atom-addition) or 'energetic' (UV-photon absorption) trigger. So far, such studies have been largely performed for single processes. Here, we present the first work that quantitatively investigates both the relative importance and the cumulative effect of '(non-)energetic' processing. We focus on astronomically relevant CO:CH3OH = 4:1 ice analogues exposed to doses relevant for the collapse stage of dense clouds. Hydrogenation experiments result in the formation of methyl formate (MF; HC(O)OCH3), glycolaldehyde (GA; HC(O)CH2OH) and ethylene glycol (EG; H2C(OH)CH2OH) at 14 K. The absolute abundances and the abundance fractions are found to be dependent on the H-atom/CO:CH3 OHmolecule ratios and on the overall deposition rate. In the case that ices are exposed to UV photons only, several different COMs are found. Typically, the abundance fractions are 0.2 for MF, 0.3 for GA and 0.5 for EG as opposed to the values found in pure hydrogenation experiments without UV in which MF is largely absent: 0.0, 0.2-0.6 and 0.8-0.4, respectively. In experiments where both are applied, overall COM abundances drop to about half of those found in the pure UV irradiation experiments, but the composition fractions are very similar. This implies COM ratios can be used as a diagnostic tool to derive the processing history of an ice. Solid-state branching ratios derived here for GA and EG compare well with observations, while the MF case cannot be explained by solid-state conditions investigated here.

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“…A large number of organic molecules with up to 12 atoms have been detected thus far, for example, in the high-mass star-forming region Sagittarius (Sgr for short) B2(N) (Belloche et al 2009(Belloche et al , 2013. The Orion KL region is another high-mass star-forming region in which molecular complexity has been studied extensively (e.g., Tercero et al 2015, and references therein). IRAS 16293-2422 (e.g., Jørgensen et al 2012;Pineda et al 2012, and references therein) and NGC 1333-IRAS2A (Maury et al 2014) are corresponding examples of low-mass star-forming regions.…”

Section: Introductionmentioning

confidence: 99%

Rotational spectra of isotopic species of methyl cyanide, CH₃CN, in theirv₈= 1 excited vibrational states

Müller

Drouin

Pearson

et al. 2016

A&A

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Context. Methyl cyanide is an important trace molecule in space, especially in star-forming regions where it is one of the more common molecules used to derive kinetic temperatures. Aims. We want to obtain accurate spectroscopic parameters of minor isotopologs of methyl cyanide in their lowest excited 8 = 1 vibrational states to support astronomical observations, in particular, with interferometers such as ALMA. Methods. The laboratory rotational spectrum of methyl cyanide in natural isotopic composition has been recorded from the millimeter to the terahertz regions. Results. Transitions with good signal-to-noise ratios could be identified for the three isotopic species CH 13 3 CN, 13 CH 3 CN, and CH 3 C 15 N up to about 1.2 THz (J ≤ 66). Accurate spectroscopic parameters were obtained for all three species. Conclusions. The present data were already instrumental in identifying 8 = 1 lines of methyl cyanide with one 13 C in IRAM 30 m and ALMA data toward Sagittarius B2(N).

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Searching for trans ethyl methyl ether in Orion KL

Cited by 61 publications

References 31 publications

The complexity of Orion: an ALMA view

The complexity of Orion: an ALMA view

Production of complex organic molecules:H-atom addition versus UV irradiation

Rotational spectra of isotopic species of methyl cyanide, CH₃CN, in theirv₈= 1 excited vibrational states

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Searching for trans ethyl methyl ether in Orion KL

Cited by 61 publications

References 31 publications

The complexity of Orion: an ALMA view

The complexity of Orion: an ALMA view

Production of complex organic molecules:H-atom addition versus UV irradiation

Rotational spectra of isotopic species of methyl cyanide, CH3CN, in theirv8= 1 excited vibrational states

Contact Info

Product

Resources

About

Rotational spectra of isotopic species of methyl cyanide, CH₃CN, in theirv₈= 1 excited vibrational states