Seeds Of Life In Space (SOLIS): The Organic Composition Diversity at 300–1000 au Scale in Solar-type Star-forming Regions<sup>*</sup>

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

doi:10.3847/1538-4357/aa961d

Cited by 130 publications

(103 citation statements)

References 138 publications

(226 reference statements)

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“…We make use of various Plateau de Bure Interferometer (PdBI) and NOrthern Extended Millimeter Array (NOEMA) datasets from four observational programs in the 1.3, 2, and 3mm bands and at different configurations. The properties of the transitions targeted in this work are summarised in Table 1. For the SOLIS data, the IRAS4A binary system was observed in three different Setups (1, 3, and 5) with the IRAM NOEMA interferometer during several tracks in June and September 2016 (see Table 1 of Ceccarelli et al 2017). Setup 1, 3, and 5 cover the frequency ranges from 80.…”

Section: Observationsmentioning

confidence: 99%

Seeds of Life in Space (SOLIS)

Taquet

Codella

Simone

et al. 2020

A&A

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Context. Low-mass protostars drive powerful molecular outflows that can be observed with millimetre and submillimetre telescopes. Various sulfuretted species are known to be bright in shocks and could be used to infer the physical and chemical conditions throughout the observed outflows.Aims. The evolution of sulfur chemistry is studied along the outflows driven by the NGC1333-IRAS4A protobinary system located in the Perseus cloud to constrain the physical and chemical processes at work in shocks. Methods. We observed various transitions from OCS, CS, SO, and SO 2 towards NGC1333-IRAS4A in the 1.3, 2, and 3mm bands using the IRAM NOrthern Extended Millimeter Array (NOEMA) and we interpreted the observations through the use of the Paris-Durham shock model. Results. The targeted species clearly show different spatial emission along the two outflows driven by IRAS4A. OCS is brighter on small and large scales along the south outflow driven by IRAS4A1, whereas SO 2 is detected rather along the outflow driven by IRAS4A2 that is extended along the north east -south west (NE-SW) direction. SO is detected at extremely high radial velocity up to +25 km s −1 relative to the source velocity, clearly allowing us to distinguish the two outflows on small scales. Column density ratio maps estimated from a rotational diagram analysis allowed us to confirm a clear gradient of the OCS/SO 2 column density ratio between the IRAS4A1 and IRAS4A2 outflows. Analysis assuming non Local Thermodynamic Equilibrium of four SO 2 transitions towards several SiO emission peaks suggests that the observed gas should be associated with densities higher than 10 5 cm −3 and relatively warm (T > 100 K) temperatures in most cases. Conclusions. The observed chemical differentiation between the two outflows of the IRAS4A system could be explained by a different chemical history. The outflow driven by IRAS4A1 is likely younger and more enriched in species initially formed in interstellar ices, such as OCS, and recently sputtered into the shock gas. In contrast, the longer and likely older outflow triggered by IRAS4A2 is more enriched in species that have a gas phase origin, such as SO 2 .

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Section: Observationsmentioning

confidence: 99%

Seeds of Life in Space (SOLIS)

Taquet

Codella

Simone

et al. 2020

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“…Walsh et al 2016;Favre et al 2018), as well as in low-and high-mass star-forming regions (e.g. Blake et al 1987;Fayolle et al 2015;Bergner et al 2017;Ceccarelli et al 2017;Ospina-Zamudio et al 2018;Bøgelund et al 2019). Meteorite measurements (Ehrenfreund et al 2001;Botta & Bada 2002), comet coma observations (Bockelée-Morvan et al 2000;Crovisier et al 2004;Biver et al 2014), and in situ Rosetta mission measurements (Le Roy et al 2015;Altwegg et al 2017) have revealed complex organic molecules, such as glycolaldehyde (CH 2 OHCHO), ethylene glycol ((CH 2 OH) 2 ), and glycine.…”

Section: Introductionmentioning

confidence: 99%

The ALMA-PILS survey: inventory of complex organic molecules towards IRAS 16293–2422 A

Manigand

Jørgensen

Calcutt

et al. 2020

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Context. Complex organic molecules are detected in many sources in the warm inner regions of envelopes surrounding deeply embedded protostars. Exactly how these species form remains an open question.Aims. This study aims to constrain the formation of complex organic molecules through comparisons of their abundances towards the Class 0 protostellar binary IRAS 16293-2422. Methods. We utilised observations from the Atacama Large Millimetre/submillimetre Array (ALMA) Protostellar Interferometric Line Survey (PILS) of IRAS 16293-2422. The species identification and the rotational temperature and column density estimation were derived by fitting the extracted spectra towards IRAS 16293-2422 A and IRAS 16293-2422 B with synthetic spectra. The majority of the work in this paper pertains to the analysis of IRAS 16293-2422 A for a comparison with the results from the other binary component, which have already been published. Results. We detect 15 different complex species, as well as 16 isotopologues towards the most luminous companion protostar IRAS 16293-2422 A. Tentative detections of an additional 11 isotopologues are reported. We also searched for and report on the first detections of methoxymethanol (CH 3 OCH 2 OH) and trans-ethyl methyl ether (t-C 2 H 5 OCH 3 ) towards IRAS 16293-2422 B and the follow-up detection of deuterated isotopologues of acetaldehyde (CH 2 DCHO and CH 3 CDO). Twenty-four lines of doubly-deuterated methanol (CHD 2 OH) are also identified. Conclusions. The comparison between the two protostars of the binary system shows significant differences in abundance for some of the species, which are partially correlated to their spatial distribution. The spatial distribution is consistent with the sublimation temperature of the species; those with higher expected sublimation temperatures are located in the most compact region of the hot corino towards IRAS 16293-2422 A. This spatial differentiation is not resolved in IRAS 16293-2422 B and will require observations at a higher angular resolution. In parallel, the list of identified CHD 2 OH lines shows the need of accurate spectroscopic data including their line strength. Article number, page 2 of 31 S. Manigand et al.: Inventory of complex organic molecules towards IRAS 16293-2422 A Notes. (a) e 0 , o 1 and e 1 corresponds to the three first torsional states. The notation of the quantum numbers is directly taken from Mukhopadhyay (2016). (b) This corresponds to the number indicated in the top-right corner of each panel in Figures D.1 and D.2. (c) W is the integrated intensity of the unblended lines, summed over the range [ν 0 − ∆ν FWHM , ν 0 + ∆ν FWHM ], given ∆ν FWHM = ν 0 FWHM c , with FWHM equal to 2.2 and 0.8 km s −1 for IRAS 16293A and B, respectively.

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“…Indeed, two chemically distinct types of Solar-like protostars have been identified. On the one hand, hot corinos (Ceccarelli et al 2000 are compact (< 100 au), dense (> 10 7 cm −3 ), and hot (> 100 K) regions, enriched in interstellar Complex Organic Molecules (hereafter iCOMs; for example, CH 3 OH, CH 3 CHO, HCOOCH 3 ; Herbst & Van Dishoeck 2009;Ceccarelli et al 2017). On the other hand, Warm Carbon Chain Chemistry (hereafter WCCC; Sakai et al 2008, Sakai & Yamamoto 2013 objects have an inner region deficient in iCOMs but a large (≈2000 au) zone enriched in carbon chain molecules (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

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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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Seeds Of Life In Space (SOLIS): The Organic Composition Diversity at 300–1000 au Scale in Solar-type Star-forming Regions^*

Cited by 130 publications

References 138 publications

Seeds of Life in Space (SOLIS)

Seeds of Life in Space (SOLIS)

The ALMA-PILS survey: inventory of complex organic molecules towards IRAS 16293–2422 A

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

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Seeds Of Life In Space (SOLIS): The Organic Composition Diversity at 300–1000 au Scale in Solar-type Star-forming Regions*

Cited by 130 publications

References 138 publications

Seeds of Life in Space (SOLIS)

Seeds of Life in Space (SOLIS)

The ALMA-PILS survey: inventory of complex organic molecules towards IRAS 16293–2422 A

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

Contact Info

Product

Resources

About

Seeds Of Life In Space (SOLIS): The Organic Composition Diversity at 300–1000 au Scale in Solar-type Star-forming Regions^*