Chemical survey of Class I protostars with the IRAM-30 m

Abstract

Context. Class I protostars are a bridge between Class 0 protostars (≤105 yr old), and Class II (≥106 yr) protoplanetary disks. Recent studies show gaps and rings in the dust distribution of disks younger than 1 Myr, suggesting that planet formation may start already at the Class I stage. To understand what chemistry planets will inherit, it is crucial to characterize the chemistry of Class I sources and to investigate how chemical complexity evolves from Class 0 protostars to protoplanetary disks. Aims. There are two goals: (i) to perform a census of the molecular complexity in a sample of four Class I protostars, and (ii) to compare the data with the chemical compositions of earlier and later phases of the Sun-like star formation process. Methods. We performed IRAM-30 m observations at 1.3 mm towards four Class I objects (L1489-IRS, B5-IRS1, L1455-IRS1, and L1551-IRS5). The column densities of the detected species were derived assuming local thermodynamic equilibrium (LTE) or large velocity gradients (LVGs). Results. We detected 27 species: C-chains, N-bearing species, S-bearing species, Si-bearing species, deuterated molecules, and interstellar complex organic molecules (iCOMs; CH3OH, CH3CN, CH3CHO, and HCOOCH3). Among the members of the observed sample, L1551-IRS5 is the most chemically rich source. Different spectral profiles are observed: (i) narrow lines (~1 km s−1) towards all the sources, (ii) broader lines (~4 km s−1) towards L1551-IRS5, and (iii) line wings due to outflows (in B5-IRS1, L1455-IRS1, and L1551-IRS5). Narrow c-C3H2 emission originates from the envelope with temperatures of 5–25 K and sizes of ~2′′−10′′. The iCOMs in L1551-IRS5 reveal the occurrence of hot corino chemistry, with CH3OH and CH3CN lines originating from a compact (~0.′′15) and warm (T > 50 K) region. Finally, OCS and H2S seem to probe the circumbinary disks in the L1455-IRS1 and L1551-IRS5 binary systems. The deuteration in terms of elemental D/H in the molecular envelopes is: ~10−70% (D2CO/H2CO), ~5−15% (HDCS/H2CS), and ~1−23% (CH2DOH/CH3OH). For the L1551-IRS5 hot corino we derive D/H ~2% (CH2DOH/CH3OH). Conclusions. Carbon chain chemistry in extended envelopes is revealed towards all the sources. In addition, B5-IRS1, L1455-IRS1, and L1551-IRS5 show a low-excitation methanol line that is narrow and centered at systemic velocity, suggesting an origin from an extended structure, plausibly UV-illuminated. The abundance ratios of CH3CN, CH3CHO, and HCOOCH3 with respect to CH3OH measured towards the L1551-IRS5 hot corino are comparable to that estimated at earlier stages (prestellar cores, Class 0 protostars), and to that found in comets. The deuteration in our sample is also consistent with the values estimated for sources at earlier stages. These findings support the inheritance scenario from prestellar cores to the Class I phase when planets start forming.

Molecular Mapping of DR Tau’s Protoplanetary Disk, Envelope, Outflow, and Large-scale Spiral Arm

“…Although SO is detected in DR Tau, it has otherwise rarely been detected in Class II disks, especially those hosted by T Tauri stars (e.g., Guilloteau et al 2016;Semenov et al 2018;Le Gal et al 2021). It is commonly detected, though, in younger, embedded Class 0 and I systems (e.g., Sakai et al 2014;Le Gal et al 2020;Garufi et al 2022;Mercimek et al 2022). In addition, Sturm et al (2022) found that gas-phase carbon is not as severely depleted in DR Tau as in other Class II disks that have been observed, although it is still more depleted than Class 0/I systems.…”

Molecular Mapping of DR Tau's Protoplanetary Disk, Envelope, Outflow, and Large-Scale Spiral Arm

“…Although SO is detected in DR Tau, it has otherwise rarely been detected in Class II disks, especially those hosted by T Tauri stars (e.g., Guilloteau et al 2016;Semenov et al 2018;Le Gal et al 2021). It is commonly detected, though, in younger, embedded Class 0 and I systems (e.g., Sakai et al 2014;Le Gal et al 2020;Garufi et al 2022;Mercimek et al 2022). In addition, Sturm et al (2022) found that gas-phase carbon is not as severely depleted in DR Tau as other Class II disks that have been observed, although it is still more depleted than Class 0/I systems.…”

Stratified Distribution of Organic Molecules at the Planet-formation Scale in the HH 212 Disk Atmosphere

“…Thus the water snowline can be located around or slightly outside the centrifugal barrier. (Mercimek et al 2022), references therein. It is possible that H 2 CO is formed by hydrogenation to CO frozen in the ice mantle on dust grains and then CH 3 OH is formed from it with the addition of two H atoms (Charnley 2004).…”