Seeds of Life in Space (SOLIS). III. Zooming Into the Methanol Peak of the Prestellar Core L1544*

Punanova, A.; Caselli, P.; Feng, Siyi; Chacón-Tanarro, A.; Ceccarelli, C.; Neri, R.; Fontani, F.; Jiménez-Serra, Izaskun; Vastel, C.; Bizzocchi, L.; Pon, Andy; Vasyunin, A. I.; Spezzano, S.; Hily-Blant, Pierre; Testi, L.; Viti, S.; Yamamoto, Satoshi; Alves, F. O.; Bachiller, R.; Balucani, Nadia; Bianchi, E.; Bottinelli, S.; Caux, E.; Choudhury, R.; Codella, C.; Dulieu, F.; Favre, Cécile; Holdship, Jonathan; Al-Edhari, A. Jaber; Kahane, C.; Laas, J.; Leflóch, B.; López-Sepulcre, A.; Ospina-Zamudio, J.; Oya, Yoko; Pineda, Jaime E.; Podio, L.; Quenard, D.; Rimola, Albert; Sakai, Nami; Sims, Ian; Taquet, V.; Theulé, Patrice; Ugliengo, Piero

doi:10.3847/1538-4357/aaad09

Cited by 39 publications

(50 citation statements)

References 58 publications

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“…However, while the methanol peak in L1544 is located at ∼4000 au from the core center, the methanol blob in L1521F is found at roughly ∼1000 au. At this distance, methanol is clearly depleted in L1544 (Bizzocchi et al 2014;Vastel et al 2014;Jiménez-Serra et al 2014;Punanova et al 2018) due to the high density and low temperatures found at this distance in the core. Crapsi et al (2004) used the 1.2 mm continuum data of L1521F from the IRAM-30 m to estimate the density distribution under the assumption of spherical symmetry.…”

Section: On the Nature Of The Ch 3 Oh Blob In L1521fmentioning

confidence: 89%

“…In this context, Tafalla et al (2004) suggest that the ring-like morphology for CH 3 OH in prestellar cores is due to depletion of C-bearing species close to the dust emission peak. A189, page 3 of 11 A&A 635, A189 (2020) Interestingly enough, Punanova et al (2018) has observed a centrally peaked emission fragment for CH 3 OH around the center of the L1544 prestellar core and inferred that the methanol emission could arise from an accretion shock. Such structures are likely the result of dynamical gas interaction such as fragmentation (see Tokuda et al 2014).…”

Section: Methanol Channel Emission Mapsmentioning

confidence: 99%

“…This line does not appear in the IRAM-30 m data, probably due to heavy beam dilution. We also explored the L1544 NOEMA data (Punanova et al 2018) for this transition, which is not detected.…”

Section: Species Transitionmentioning

confidence: 99%

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Seeds of Life in Space (SOLIS)

Favre

Vastel

Jiménez-Serra

et al. 2020

A&A

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Aims. The Seeds Of Life In Space IRAM/NOEMA large program aims at studying a set of crucial complex organic molecules in a sample of sources with a well-known physical structure that covers the various phases of solar-type star formation. One representative object of the transition from the prestellar core to the protostar phases has been observed toward the very low luminosity object (VeLLO) L1521F. This type of source is important to study to link prestellar cores and Class 0 sources and also to constrain the chemical evolution during the process of star formation. Methods. Two frequency windows (81.6–82.6 GHz and 96.65–97.65 GHz) were used to observe the emission from several complex organics toward the L1521F VeLLO. These setups cover transitions of ketene (H2CCO), propyne (CH3CCH), formamide (NH2CHO), methoxy (CH3O), methanol (CH3OH), dimethyl ether (CH3OCH3), and methyl formate (HCOOCH3). Results. Only two transitions of methanol (A+, E2) have been detected in the narrow window centered at 96.7 GHz (with an upper limit on E1) in a very compact emission blob (~7′′ corresponding to ~1000 au) toward the northeast of the L1521F protostar. The CS 2–1 transition is also detected within the WideX bandwidth. Consistently with what has been found in prestellar cores, the methanol emission appears ~1000 au away from the dust peak. The location of the methanol blob coincides with one of the filaments that have previously been reported in the literature. The excitation temperature of the gas inferred from methanol is (10 ± 2) K, while the H2 gas density (estimated from the detected CS 2–1 emission and previous CS 5–4 ALMA observations) is a factor >25 higher than the density in the surrounding environment (n(H2) ≥ 107 cm−3). Conclusions. Based on its compactness, low excitation temperature, and high gas density, we suggest that the methanol emission detected with NOEMA is (i) either a cold and dense shock-induced blob that formed recently (≤ a few hundred years) by infalling gas or (ii) a cold and dense fragment that may just have been formed as a result of the intense gas dynamics within the L1521F VeLLO system.

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Section: On the Nature Of The Ch 3 Oh Blob In L1521fmentioning

confidence: 89%

Section: Methanol Channel Emission Mapsmentioning

confidence: 99%

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Seeds of Life in Space (SOLIS)

Favre

Vastel

Jiménez-Serra

et al. 2020

A&A

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“…As for CH 3 OH, it is also a species that has been found in PDRs as well as in molecular clouds (e.g. Leurini et al 2010;Guzmán et al 2013;Cuadrado et al 2017;Punanova et al 2018). Thus, an important contribution from the parental molecular cloud or from the surrounding PDR may occur when observing those molecules with single-dish telescopes.…”

Section: Introductionmentioning

confidence: 98%

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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“…The situation may not be that simple in this specific core. These are interferometric observations of methanol emission presented by [23], and they show that methanol emission is observed on one side of the core. This may imply that there is some illumination from this side.…”

mentioning

confidence: 65%

Pre-Biological Evolution of Organic Matter in the Universe

Wiebe¹

2019

Proceedings of Frontier Research in Astrophysics – III — PoS(FRAPWS2018)

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Seeds of Life in Space (SOLIS). III. Zooming Into the Methanol Peak of the Prestellar Core L1544*

Cited by 39 publications

References 58 publications

Seeds of Life in Space (SOLIS)

Seeds of Life in Space (SOLIS)

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

Pre-Biological Evolution of Organic Matter in the Universe

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