The ALMA-PILS survey: the sulphur connection between protostars and comets: IRAS 16293–2422 B and 67P/Churyumov–Gerasimenko

Drozdovskaya, M. N.; Dishoeck, E. F. van; Jørgensen, J. K.; Calmonte, Ursina; Wiel, M. H. D. van der; Coutens, A.; Calcutt, H.; Müller, H. S. P.; Bjerkeli, P.; Persson, M. V.; Wampfler, S. F.; Altwegg, Kathrin

doi:10.1093/mnras/sty462

Cited by 96 publications

(155 citation statements)

References 105 publications

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“…The PILS Band 7 data also cover the J = 4 − 3 transition of DC 15 N and a tentative assignment can be made at an implied column density of 7.5 × 10 12 cm −2 . This would correspond to a D/H ratio of about 3 per cent, which is in-line with other measurements of D/H ratios from PILS (e.g., Drozdovskaya et al 2018;Jørgensen et al 2018). Conversely, if the HCN column density had been grossly underestimated, the D/H ratio would need to be much lower for this species in particular.…”

Section: A2 Hcn and Hncsupporting

confidence: 87%

Ingredients for solar-like systems: protostar IRAS 16293-2422 B versus comet 67P/Churyumov–Gerasimenko

Drozdovskaya

Dishoeck

Rubin

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Our modern day Solar System has 4.6 × 10 9 yrs of evolution behind it with just a few relics of its birth conditions remaining. Comets are thought to be some of the most pristine tracers of the initial ingredients that were combined to produce the Earth and the other planets. Other low-mass protostars may be analogous to our proto-Sun and hence, could be used to study the building blocks necessary to form Solar-like systems. This study tests this idea on the basis of new high sensitivity, high spatial resolution ALMA data on the protoplanetary discscales (∼ 70 au) of IRAS 16293-2422 and the bulk composition of comet 67P/Churyumov-Gerasimenko, as determined for the first time with the unique in situ monitoring carried out by Rosetta. The comparative analysis of the observations from the Protostellar Interferometric Line Survey (PILS) and the measurements made with Rosetta Orbiter Spectrometer for Ion and Neutral Analysis (ROSINA) shows that the relative abundances of CHO-, N-, and Sbearing molecules correlate, with some scatter, between protostellar and cometary data. A tentative correlation is seen for the first time for P-and Cl-bearing compounds. The results imply that the volatile composition of cometesimals and planetesimals is partially inherited from the pre-and protostellar phases of evolution.

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Section: A2 Hcn and Hncsupporting

confidence: 87%

Ingredients for solar-like systems: protostar IRAS 16293-2422 B versus comet 67P/Churyumov–Gerasimenko

Drozdovskaya

Dishoeck

Rubin

et al. 2019

Monthly Notices of the Royal Astronomical Society

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127

102

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“…We hereafter assume a gas temperature of 100 K for the continuum peak, based on the dust temperature distribution reported by Rocha & Pilling (2018). Table 4 also shows previously reported results for comparison: the shocked outflow in L1157 (L1157 B1; Bachiller & Pérez Gutiérrez 1997), the protostar and the outflow of NGC1333 IRAS 2 (Wakelam et al 2005), and the envelope gas of the low-mass protostellar source IRAS 16293-2422 Source B (Drozdovskaya et al 2018). In low-mass protostellar sources, SO is generally thought to be abundant in shocked regions.…”

Section: Abundance Ratios Of the S-bearing Speciesmentioning

confidence: 97%

Sulfur-bearing Species Tracing the Disk/Envelope System in the Class I Protostellar Source Elias 29

Oya

López-Sepulcre

Sakai

et al. 2019

ApJ

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We have observed the Class I protostellar source Elias 29 with Atacama Large Millimeter/submillimeter Array (ALMA). We have detected CS, SO, 34 SO, SO 2 , and SiO line emissions in a compact component concentrated near the protostar and a ridge component separated from the protostar by 4 (∼ 500 au). The former component is found to be abundant in SO and SO 2 but deficient in CS.The abundance ratio SO/CS is as high as 3 +13 −2 ×10 2 at the protostar, which is even higher than that in the outflow-shocked region of L1157 B1. However, organic molecules (HCOOCH 3 , CH 3 OCH 3 , CCH, and c-C 3 H 2 ) are deficient in Elias 29.We attribute the deficiency in organic molecules and richness in SO and SO 2 to the evolved nature of the source or the relatively high dust temperature ( > ∼ 20 K) in the parent cloud of Elias 29. The SO and SO 2 emissions trace rotation around the protostar. Assuming a highly inclined configuration (i ≥ 65 • ; 0 • for a face-on configuration) and Keplerian motion for simplicity, the protostellar mass is estimated to be (0.8 -1.0) M . The 34 SO and SO 2 emissions are asymmetric in their spectra; the blue-shifted components are weaker than the red-shifted ones.Although this may be attributed to the asymmetric molecular distribution, other possibilities are also discussed.

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“…The ALMA Protostellar Interferometric Line Survey 1 (PILS, Jørgensen et al 2016) performed an unbiased spectral survey of the system in Band 7, demonstrating the strength of ALMA for detecting new complex species towards the most compact component IRAS 16293B of the system, including CH 3 Cl (Fayolle et al 2017), CH 3 NC (Calcutt et al 2018a), HONO (Coutens et al 2019), NH 2 CN (Coutens et al 2018), and CH 3 NCO (Ligterink et al 2017). In addition, many deuterated and less abundant isotopologues have been found for the first time in the interstellar medium (ISM) towards this source, including NHDCHO, NH 2 CDO , NHDCN (Coutens et al 2018), CHD 2 CN (Calcutt et al 2018b), deuterated and 13 C isotopologues of CH 2 OHCHO, deuterated ethanol (C 2 H 5 OH), ketene (CH 2 CO), acetaldehyde (CH 3 CHO) and formic acid (HCOOH) , OC 33 S 1 The reduced dataset and all the publications are available on the website http://youngstars.nbi.dk/PILS/ (Drozdovskaya et al 2018), and doubly deuterated methyl formate (CHD 2 OCHO; Manigand et al 2018). This paper aims to study the O-bearing COMs in the other protostar IRAS 16293A of the binary system and to compare their abundances with IRAS 16293B.…”

Section: Introductionmentioning

confidence: 99%

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

Manigand

Jørgensen

Calcutt

et al. 2020

A&A

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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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The ALMA-PILS survey: the sulphur connection between protostars and comets: IRAS 16293–2422 B and 67P/Churyumov–Gerasimenko

Cited by 96 publications

References 105 publications

Ingredients for solar-like systems: protostar IRAS 16293-2422 B versus comet 67P/Churyumov–Gerasimenko

Ingredients for solar-like systems: protostar IRAS 16293-2422 B versus comet 67P/Churyumov–Gerasimenko

Sulfur-bearing Species Tracing the Disk/Envelope System in the Class I Protostellar Source Elias 29

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

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