L483: Warm Carbon-chain Chemistry Source Harboring Hot Corino Activity

Oya, Yoko; Sakai, Nami; Watanabe, Yoshimasa; Higuchi, Aya E.; Hirota, Tomoya; López-Sepulcre, A.; Sakai, Takeshi; Aikawa, Yuri; Ceccarelli, C.; Leflóch, B.; Caux, E.; Vastel, C.; Kahane, C.; Yamamoto, Satoshi

doi:10.3847/1538-4357/aa6300

Cited by 97 publications

(163 citation statements)

References 43 publications

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“…While the CH 3 OH lines are detected near the continuum peak, the weak CCH lines are missing toward the continuum source, instead peaking at 0.55 ′′ from the continuum peak along the disk direction. The same phenomenon has been observed in other sources: in L1527, IRAS 15398-3359, and L483 the CCH is also depleted near the con-tinuum peak and has strong emission off the peak (Oya et al 2014;Sakai et al 2014;Oya et al 2017). The CCH molecule reacts with H 2 at warm temperatures (see e.g., Aikawa et al 2012) and could be destroyed by those gas phase reaction in the warm and dense inner envelope and/or frozen on the dust grain in the cold and dense disk.…”

Section: Molecular Linessupporting

confidence: 80%

“…Another stream toward the north direction looks like a mirror image of the eastward stream with respect to the disk midplane (the solid gray line in Figure 3), which could imply that the northward stream might trace the red-shifted outflow cavity wall. CCH emission along the outflow cavity walls is also found in L1527, IRAS 15398-3359, and L483 (Oya et al 2014;Sakai et al 2014;Oya et al 2017).…”

Section: Molecular Linesmentioning

confidence: 88%

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The Circumstellar Environment around the Embedded Protostar EC 53

Lee

Aikawa

et al. 2020

ApJ

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EC53 is an embedded protostar with quasi-periodic emission in the near-IR and sub-mm. We use ALMA high-resolution observations of continuum and molecular line emission to describe the circumstellar environment of EC 53. The continuum image reveals a disk with a flux that suggests a mass of 0.075 M ⊙ , much less than the estimated mass in the envelope, and an in-band spectral index that indicates grain growth to centimeter sizes. Molecular lines trace the outflow cavity walls, infalling and rotating envelope, and/or the Keplerian disk. The rotation profile of the C 17 O 3-2 line emission cannot isolate the Keplerian motion clearly although the lower limit of the protostellar mass can be calculated as 0.3 ± 0.1 M ⊙ if the Keplerian motion is adopted. The weak CH 3 OH emission, which is anti-correlated with the H 13 CO + 4-3 line emission, indicates that the water snow line is more extended than what expected from the current luminosity, attesting to bygone outburst events. The extended snow line may persist for longer at the disk surface because the lower density increases the freeze-out timescale of methanol and water.

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Section: Molecular Linessupporting

confidence: 80%

Section: Molecular Linesmentioning

confidence: 88%

The Circumstellar Environment around the Embedded Protostar EC 53

Lee

Aikawa

et al. 2020

ApJ

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“…Figure 1 shows a plot of NH 2 CHO against HNCO fractional abundances relative to molecular hydrogen, H 2 , for all the sources in the literature with reported values of column densities for these two molecules, as well as total H 2 column density values. 17,28,29,42,43,[45][46][47]62,64,72,73 Single-dish and interferometric ob- Figure 1 shows that there is a tight correlation between the two molecular species, which is almost linear and holds across several orders of magnitude in molecular abundance. This has led some authors to propose that HNCO and NH 2 CHO are chemically linked, with either both of them forming from a common precursor, or one forming from the other.…”

Section: Abundance Correlationsmentioning

confidence: 98%

Interstellar Formamide (NH₂CHO), a Key Prebiotic Precursor

López-Sepulcre

Balucani²,

Ceccarelli³

et al. 2019

ACS Earth Space Chem.

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Formamide (NH 2 CHO) has been identified as a potential precursor of a wide variety of organic compounds essential to life, and many biochemical studies propose it likely played a crucial role in the context of the origin of life on our planet. The detection of formamide in comets, which are believed to have -at least partially-inherited their current chemical composition during the birth of the Solar System, raises the question whether a non-negligible amount of formamide may have been exogenously delivered onto a very young Earth about four billion years ago. A crucial part of the effort to 1 arXiv:1909.11770v1 [astro-ph.SR] 25 Sep 2019 answer this question involves searching for formamide in regions where stars and planets are forming today in our Galaxy, as this can shed light on its formation, survival, and chemical re-processing along the different evolutionary phases leading to a star and planetary system like our own.The present review primarily addresses the chemistry of formamide in the interstellar medium, from the point of view of (i) astronomical observations, (ii) experiments, and (iii) theoretical calculations. While focusing on just one molecule, this review also more generally reflects the importance of joining efforts across multiple scientific disciplines in order to make progress in the highly interdisciplinary science of astrochemistry.

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“…CCH, c-C 3 H 2 , C 4 H). This dichotomy does not seem to be absolute as at least one source, the protostar L483, presents both hot corino and WCCC characteristics (Oya et al 2017). Understanding what causes this chemical diversity is a fundamental step in understanding the formation and the evolution of a planetary system like our own and, perhaps, to understand the appearance of life on Earth.…”

Section: Introductionmentioning

confidence: 99%

“…Some studies have been targeted on just one type of object (either hot corino or WCCC object; e.g. Caux et al 2011;Jø rgensen et al 2016;López-Sepulcre et al 2017;Oya et al 2017;Ospina-Zamudio et al 2018;Agúndez et al 2019;Bianchi et al 2019;Yoshida et al 2019), or one Table 1: Summary of the excitation temperatures (T ex ) and column densities (N tot ) of the different tracers of hot corinos (CH 3 OH) and WCCC objects (CCH and C 4 H) derived in previous surveys obtained with single-dish telescope observations. Object type Molecule Graninger et al 2016Lindberg et al 2016Higuchi et al 2018L1527 b IRAS 16293-2422 Higuchi et al (2018), Sakai et al (2008) (c) Van Dishoeck et al (1995), Sakai et al (2009) type of molecular tracer (Carbon-chain or iCOMs; e.g.…”

Section: Introductionmentioning

confidence: 99%

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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L483: Warm Carbon-chain Chemistry Source Harboring Hot Corino Activity

Cited by 97 publications

References 43 publications

The Circumstellar Environment around the Embedded Protostar EC 53

The Circumstellar Environment around the Embedded Protostar EC 53

Interstellar Formamide (NH₂CHO), a Key Prebiotic Precursor

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

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L483: Warm Carbon-chain Chemistry Source Harboring Hot Corino Activity

Cited by 97 publications

References 43 publications

The Circumstellar Environment around the Embedded Protostar EC 53

The Circumstellar Environment around the Embedded Protostar EC 53

Interstellar Formamide (NH2CHO), a Key Prebiotic Precursor

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

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Product

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Interstellar Formamide (NH₂CHO), a Key Prebiotic Precursor