Which molecule traces what: Chemical diagnostics of protostellar sources

Abstract

Context. The physical and chemical conditions in Class 0/I protostars are fundamental in unlocking the protostellar accretion process and its impact on planet formation. Aims. The aim is to determine which physical components are traced by different molecules at subarcsecond scales (<100–400 au). Methods. We used a suite of Atacama Large Millimeter/submillimeter Array (ALMA) datasets in band 6 (1 mm), band 5 (1.8 mm), and band 3 (3 mm) at spatial resolutions 0.″5–3″ for 16 protostellar sources. For a subset of sources, Atacama Compact Array (ACA) data at band 6 with a spatial resolution of 6″ were added. The availability of low- and high-excitation lines and data on small and larger scales, is important to understand the full picture. Results. The protostellar envelope is well traced by C18O, DCO+, and N2D+, which stems from the freeze-out of CO governing the chemistry at envelope scales. Molecular outflows are seen in classical shock tracers such as SiO and SO, but ice-mantle products such as CH3OH and HNCO that are released with the shock are also observed. The molecular jet is a key component of the system. It is only present at the very early stages, and it is prominent not only in SiO and SO, but occasionally also in H2CO. The cavity walls show tracers of UV-irradiation such as C2H, c-C3H2 and CN. In addition to showing emission from complex organic molecules (COMs), the hot inner envelope also presents compact emission from small molecules such as H2S, SO, OCS, and H13CN, which most likely are related to ice sublimation and high-temperature chemistry. Conclusions. Subarcsecond millimeter-wave observations allow us to identify these (simple) molecules that best trace each of the physical components of a protostellar system. COMs are found both in the hot inner envelope (high-excitation lines) and in the outflows (lower-excitation lines) with comparable abundances. COMs can coexist with hydrocarbons in the same protostellar sources, but they trace different components. In the near future, mid-infrared observations with JWST–MIRI will provide complementary information about the hottest gas and the ice-mantle content, at unprecedented sensitivity and at resolutions comparable to ALMA for the same sources.

Chemical and Physical Characterization of the Isolated Protostellar Source CB68: FAUST IV

“…Although the isolated sources CB 68 and B335 both show a hybrid chemical nature, we should note that a hybrid chemical nature is not specific to isolated sources. Indeed, a hybrid chemistry is reported for L483 (Oya et al 2017), and a hint of it is also seen in Serpens SMM 3 (Tychoniec et al 2021). Nevertheless, the simple physical and chemical structures of isolated sources can be used as the best testbed to study chemical evolution during protostellar evolution without the influence of nearby young stellar objects.…”

A VLA View of the Flared, Asymmetric Disk around the Class 0 Protostar L1527 IRS

“…similar north-south asymmetry has previously been seen in emission from various molecular lines that have a strong contribution from the disk, for example, 13 CO 2-1 (van't Hoff et al 2018), C 18 O 2-1 (Aso et al 2017;van't Hoff et al 2018), C 17 O 2-1 (van't Hoff et al 2020, CS 5-4, H 2 CO 5 1,5 − 4 1,4 (Sakai et al 2014a), and c-C 3 H 2 9 1,8 − 8 2,7 (Sakai et al 2014b). Transitions with a strong envelope component display a more symmetric intensity profile, even when a different line for the same molecule traces the disk, for example, CCH 3-2 (Sakai et al 2014a) , c-C 3 H 2 5 2,3 − 4 3,2 (Sakai et al 2014b), and CN 2-1 (Tychoniec et al 2021).…”

Importance of source structure on complex organics emission

“…In other examples in the literature, sources with disks show no or a lower emission of complex organic molecules. For example, Tychoniec et al (2021) observed a large resolved dust structure in the Class 0 source Serpens SMM3, perpendicular to the outflow that might be a disk, but failed to find strong emission of methanol or complex species towards this source, despite the high luminosity of the source (L bol 28 L ). Artur de la Villarmois et al (2019) found no methanol emission towards 12 Class I protostars hosting disks that they observed in the Ophiuchus molecular cloud.…”