A chemical inventory of the disk around the class 0 protostar L1527 IRS with ALMA
4 affiliations
- 1Department of Physics and Astronomy, Purdue University, West-Lafayette, IN, United States
- 2Leiden Observatory, Leiden University, Leiden, Netherlands
- 3National Radio Astronomy Observatory, Charlottesville, VA, United States
- 4Institute of Astronomy, National Tsing Hua University, Hsinchu, Taiwan
Abstract
Planet formation starts in disks that are still embedded within their natal envelopes. Here, we compile an extensive inventory of the chemical composition of the disk and envelope (<3500 au) around the Class 0 protostar L1527 IRS. Using all publicly available ALMA (Atacama Large Millimeter/submillimeter Array) data, we report the detection of 40 molecules, including isotopologues. Of these, 23 are different molecular species and 29 are reported here for the first time toward L1527 in ALMA observations. CH3OH is the only complex organic molecule detected, while the hydrocarbon CH3CCH is the largest molecule detected. Overall, only a few programs are sensitive enough to detect emission unambiguously originating from the disk based on the kinematics. Nitrogen-bearing molecules are predominantly detected on more extended scales, while hydrocarbons show a distinct tail roughly along the southeastern outflow cavity wall, probably due to a stronger UV field in the eastern outflow lobe. The L1527 IRS protostellar system is not rich in sulfur-bearing molecules, with only strong emission observed for CS and SO. Overall, the envelope appears dominated by a carbon-rich chemistry, which seems to transition into an oxygen-rich chemistry in the disk. We calculate column densities of all detected species, providing a starting point to quantify the chemical diversity among young disks and the chemical evolution of the planet-forming material.
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BibTeX
@article{hoff2026chemical,
title = {{A chemical inventory of the disk around the class 0 protostar L1527 IRS with ALMA}},
author = {Merel L. R. van ’t Hoff and Łukasz Tychoniec and John J. Tobin and Daniel Harsono},
journal = {Frontiers in Astronomy and Space Sciences},
year = {2026},
month = oct,
doi = {10.3389/fspas.2026.1885693},
url = {https://doi.org/10.3389/fspas.2026.1885693},
note = {CC BY},
}
RIS
TY - JOUR
TI - A chemical inventory of the disk around the class 0 protostar L1527 IRS with ALMA
AU - Merel L. R. van ’t Hoff
AU - Łukasz Tychoniec
AU - John J. Tobin
AU - Daniel Harsono
PY - 2026
DA - 2026/10/28
JO - Frontiers in Astronomy and Space Sciences
DO - 10.3389/fspas.2026.1885693
UR - https://doi.org/10.3389/fspas.2026.1885693
AB - Planet formation starts in disks that are still embedded within their natal envelopes. Here, we compile an extensive inventory of the chemical composition of the disk and envelope (<3500 au) around the Class 0 protostar L1527 IRS. Using all publicly available ALMA (Atacama Large Millimeter/submillimeter Array) data, we report the detection of 40 molecules, including isotopologues. Of these, 23 are different molecular species and 29 are reported here for the first time toward L1527 in ALMA observations. CH3OH is the only complex organic molecule detected, while the hydrocarbon CH3CCH is the largest molecule detected. Overall, only a few programs are sensitive enough to detect emission unambiguously originating from the disk based on the kinematics. Nitrogen-bearing molecules are predominantly detected on more extended scales, while hydrocarbons show a distinct tail roughly along the southeastern outflow cavity wall, probably due to a stronger UV field in the eastern outflow lobe. The L1527 IRS protostellar system is not rich in sulfur-bearing molecules, with only strong emission observed for CS and SO. Overall, the envelope appears dominated by a carbon-rich chemistry, which seems to transition into an oxygen-rich chemistry in the disk. We calculate column densities of all detected species, providing a starting point to quantify the chemical diversity among young disks and the chemical evolution of the planet-forming material.
SN - 2296-987X
ER -