Observations of Warm Carbon Chain Chemistry in NGC 3576

Saul, M.; Tothill, N.; Purcell, Cormac

doi:10.1088/0004-637x/798/1/36

Cited by 6 publications

(6 citation statements)

References 43 publications

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“…Cazaux et al 2003;Sakai et al 2008;Taquet et al 2015). Besides the relatively small number of WCCC objects in low-mass star-forming regions, WCCC characteristics have also been seen in other environments, such as the starless core L1489 (Wu et al 2019) and in the giant HII region NGC 3576 (Saul et al 2015). A hot corino was also found in the high-mass star-forming region of Orion, HH212-MM1 (Codella et al 2016), but as with the other hot corinos, it is located far from massive stars.…”

Section: Introductionmentioning

confidence: 87%

Hunting for hot corinos and WCCC sources in the OMC-2/3 filament

Bouvier

López-Sepulcre

Ceccarelli

et al. 2020

A&A

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Context. Solar-like protostars are known to be chemically rich, but it is not yet clear how much their chemical composition can vary and why. So far, two chemically distinct types of Solar-like protostars have been identified: hot corinos, which are enriched in interstellar Complex Organic Molecules (iCOMs), such as methanol (CH 3 OH) or dimethyl ether (CH 3 OCH 3 ), and Warm Carbon Chain Chemistry (WCCC) objects, which are enriched in carbon chain molecules, such as butadiynyl (C 4 H) or ethynyl radical (CCH). However, none of these have been studied so far in environments similar to that in which our Sun was born, that is, one that is close to massive stars. Aims. In this work, we search for hot corinos and WCCC objects in the closest analogue to the Sun's birth environment, the Orion Molecular Cloud 2/3 (OMC-2/3) filament located in the Orion A molecular cloud. Methods. We obtained single-dish observations of CCH and CH 3 OH line emission towards nine Solar-like protostars in this region. As in other, similar studies of late, we used the [CCH]/[CH 3 OH] abundance ratio in order to determine the chemical nature of our protostar sample. Results. Unexpectedly, we found that the observed methanol and ethynyl radical emission (over a few thousands au scale) does not seem to originate from the protostars but rather from the parental cloud and its photo-dissociation region, illuminated by the OB stars of the region. Conclusions. Our results strongly suggest that caution should be taken before using [CCH]/[CH 3 OH] from single-dish observations as an indicator of the protostellar chemical nature and that there is a need for other tracers or high angular resolution observations for probing the inner protostellar layers.

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Section: Introductionmentioning

confidence: 87%

Hunting for hot corinos and WCCC sources in the OMC-2/3 filament

Bouvier

López-Sepulcre

Ceccarelli

et al. 2020

A&A

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“…The HC 3 N column density in IRAS 15398-3359 is 1.5x10 14 cm −2 (Wu et al in preparation). In the massive core WCCC source NGC 7536 the HC 5 N column density is 1x10 13 cm −2 which is derived from the detected line of HC 5 N J=11-10 (Saul et al 2015). The E up of the HC 5 N J=11-10 transition is 28.8 K.…”

Section: Carbon-chain Molecule Emission Characteristicsmentioning

confidence: 96%

“…3) is located at < 0.5 arcmin south of the P point. These deviations are due to different chemical and dynamical properties of different molecular species and can often be seen in molecular cores such as the NH 3 cores in Orion, Cepheus, and H 2 O maser sources as well as various gas cores in the carbon-chain-producing region NGC 3576 (Harju et al 1993;Wu et al 2006;Saul et al 2015, see also Fig. 7 and Sect.…”

Section: Spectral Lines and Emission Regionsmentioning

confidence: 99%

“…A second WCCC source, IRAS 15398-3359, was found by Sakai et al (2009) very shortly after the discovery of L1527. A massive star-forming region NGC 3576 was also revealed as a WCCC source according to the detected C 5 H J = 39/2 − 37/2 (Saul et al 2015).…”

Section: Introductionmentioning

confidence: 96%

“…Spectral lines of HC 3 N, HC 5 N, HC 7 N, and even HC 9 N have been seen in L1527. Furthermore, HC 3 N J=10-9 and HC 5 N J = 32 − 31, the latter being a very-high-energy excitation transition, were detected in the second WCCC source (Sakai et al 2008(Sakai et al , 2009Saul et al 2015;Benedettini et al 2012). HC 3 N J = 11 − 10 was detected in NGC 3576 (Saul et al 2015).…”

Section: Introductionmentioning

confidence: 97%

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A particular carbon-chain-producing region: L1489 starless core

Lin

Liu

et al. 2019

A&A

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We detected carbon-chain molecules (CCMs) HC 2n+1 N (n=1-3) and C 3 S in K u band as well as high-energy excitation lines including C 4 H N=9-8, J=17/2-15/2, 19/2-17/2, and CH 3 CCH J=5-4, K=2 in the 3 mm band toward a starless core called the eastern molecular core (EMC) of L1489 IRS. Maps of all the observed lines were also obtained. Comparisons with a number of early starless cores and WCCC source L1527 show that the column densities of C 4 H and CH 3 CCH are close to those of L1527, and the CH 3 CCH column densities of the EMC and L1527 are slightly higher than those of TMC-1. The EMC and L1527 have similar C 3 S column densities, but they are much lower than those of all the starless cores, with only 6.5% and 10% of the TMC-1 value, respectively. The emissions of the N-bearing species of the EMC and L1527 are at the medium level of the starless cores. These comparisons show that the CCM emissions in the EMC are similar to those of L1527, though L1527 contains a protostar. Although dark and quiescent, the EMC is warmer and at a later evolutionary stage than classical carbon-chain-producing regions in the cold, dark, quiescent early phase. The PACS, SPIRE, and SCUBA maps evidently show that the L1489 IRS seems to be the heating source of the EMC. Although it is located at the margins of the EMC, its bolometric luminosity and bolometric temperature are relatively high. Above all, the EMC is a rather particular carbon-chain-producing region and is quite significant for CCM science.

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Parsec scales of carbon chain and complex organic molecules in AFGL 2591 and IRAS 20126

Freeman,

Bottinelli,

Plume

et al. 2023

A&A

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Context. There is a diverse chemical inventory in protostellar regions leading to the classification of extreme types of systems. Warm carbon chain chemistry sources, for one, are the warm and dense regions near a protostar containing unsaturated carbon chain molecules. Since the presentation of this definition in 2008, there is a growing field to detect and characterise these sources. The details are lesser known in relation to hot cores and in high-mass star-forming regions - regions of great importance in galactic evolution. Aims. To investigate the prevalence of carbon chain species and their environment in high-mass star-forming regions, we have conducted targeted spectral surveys of two sources in the direction of Cygnus X - AFGL 2591 and IRAS 20126+4104. Methods. We observed these sources in frequency ranges around 85, 96, and 290 GHz with the Green Bank Telescope and the IRAM 30m Telescope. We have constructed a local thermodynamic equilibrium (LTE) model using the observed molecular spectra to determine the physical environment in which these molecules originate. We map both the observed spatial distribution and the physical parameters found from the LTE model. We also determine the formation routes of these molecules in each source using the three-phase NAUTILUS chemical evolution code. Results. We detect several lines of propyne, CH3CCH, and cyclopropenylidene, c-C3H2 as tracers of carbon chain chemistry, as well as several lines of formaldehyde, H2CO, and methanol, CH3OH, as a precursor and a tracer of complex organic molecule chemistry, respectively. We find excitation temperatures of 20−30 K for the carbon chains and 8−85 K for the complex organics. The observed abundances, used as input for the chemical evolution code, are 10−9 to 10−10 for both CH3CCH and CH3OH. The CH3CCH abundances are reproduced by a warm-up model, consistent with warm carbon chain chemistry, while the observed CH3OH abundances require a shock mechanism sputtering the molecules into the gas phase. Conclusions. Single-dish observations are useful for studying the envelope-scale chemistry of star-forming regions, including mechanisms such as warm carbon chain chemistry. As well, LTE models lend well to the wide-band maps obtained from these telescopes. The physical and chemical environment determined for complex hydrocarbons and complex organics lends understanding to high-mass star formation.

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Observations of Warm Carbon Chain Chemistry in NGC 3576

Cited by 6 publications

References 43 publications

Hunting for hot corinos and WCCC sources in the OMC-2/3 filament

Hunting for hot corinos and WCCC sources in the OMC-2/3 filament

A particular carbon-chain-producing region: L1489 starless core

Parsec scales of carbon chain and complex organic molecules in AFGL 2591 and IRAS 20126

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