2025-07-24 マックス・プランク研究所（MPG）
This artist’s impression shows the planet-forming disc around the star V883 Orionis. In the outermost part of the disc volatile gases are frozen out as ice, which contains complex organic molecules. An outburst of energy from the star heats the inner disc to a temperature that evaporates the ice and releases the complex molecules, enabling astronomers to detect it. The inset image shows the chemical structure of complex organic molecules detected and presumed in the protoplanetary disc (from left to right): propionitrile (ethyl cyanide), glycolonitrile, alanine, glycine, ethylene glycol, acetonitrile (methyl cyanide).
© Credit: ESO/L. Calçada/T. Müller (MPIA/HdA) (CC BY 4.0)
＜関連情報＞
- https://www.mpg.de/24451940/prebiotic-molecules-v883ori
- https://iopscience.iop.org/article/10.3847/2041-8213/adec6e
- https://iopscience.iop.org/article/10.3847/1538-3881/adc998
- https://iopscience.iop.org/article/10.3847/1538-4357/adb486
V883 Ori原始惑星円盤におけるエチレングリコールとグリコニトリルの深部探索 A Deep Search for Ethylene Glycol and Glycolonitrile in the V883 Ori Protoplanetary Disk
Abubakar M. A. Fadul, Kamber R. Schwarz, Tushar Suhasaria, Jenny K. Calahan, Jane Huang, and Merel L. R. van ’t Hoff
The Astrophysical Journal Letters Published: 2025 July 24
DOI:10.3847/2041-8213/adec6e
Abstract
Ethylene glycol (CH2OH)2; hereafter EG) and glycolonitrile (HOCH2CN; hereafter GN) are considered molecular precursors of nucleic acids. EG is a sugar alcohol and the reduced form of glycolaldehyde (CH2(OH)CHO; hereafter GA). GN is considered a key precursor of adenine formation (nucleotide) and can be a precursor of glycine (amino acid). Detections of such prebiotic molecules in the interstellar medium are increasingly common. How much of this complexity endures to the planet formation stage, and thus is already present when planets form, remains largely unknown. Here we report Atacama Large Millimeter/submillimeter Array observations in which we tentatively detect EG and GN in the protoplanetary disk around the outbursting protostar V883 Ori. The observed EG emission is best reproduced by a column density of 3.63+0.11-0.12×1016㎝-2 and a temperature of at least 300 K. The observed GN emission is best reproduced by a column density of 3.37+0.09-0.09×1016㎝-2 and a temperature of 88+1.2-1.2 K. Comparing the abundance of EG and GN relative to methanol in V883 Ori with other objects, V883 Ori falls between hot cores and comets in terms of increasing complexity. This suggests that the buildup of prebiotic molecules continues past the hot core phase into the epoch of planet formation. Nascent planets in such environments may inherit essential building blocks for life, enhancing their potential habitability. Further observations of this protoplanetary disk at higher spectral resolution are required to resolve blended lines and to confirm these tentative detections.
V883 Oriの原始惑星円盤における複雑な有機分子の深層検索 A Deep Search for Complex Organic Molecules toward the Protoplanetary Disk of V883 Ori
Abubakar M. A. Fadul, Kamber R. Schwarz, Merel L. R. van ’T Hoff, Jane Huang, Jennifer B. Bergner, Tushar Suhasaria, and Jenny K. Calahan
The Astronomical Journal Published: 2025 May 14
DOI:10.3847/1538-3881/adc998
Abstract
Complex organic molecules (COMs) in the form of prebiotic molecules are potential building blocks of life. Using Atacama Large Millimeter/submillimeter Array Band 7 observations in spectral scanning mode, we carried out a deep search for COMs within the disk of V883 Ori, covering a frequency range of ∼348–366 GHz. V883 Ori is an FU Orionis object currently undergoing an accretion burst, which increases its luminosity and consequently increases the temperature of the surrounding protoplanetary disk, facilitating the detection of COMs in the gas phase. We identify 26 molecules, including 14 COMs and 12 other molecules, with first detection in this source of the molecules CH3OD, H2C17O, andH132CO . We searched for multiple nitrogen-bearing COMs,CH3CN as was the only N-bearing COM that had been identified so far in this source. We also detect CH3CN , and tentatively detect CH3CH2CN,CH2CHN , CH3NCO, and NH2CHO. We compare the abundances relative to methanol (CH3OH) with those in the handful of objects with previous detections of these species: the Class 0 protostars IRAS 16293-2422 A, IRAS 16293-2422 B, and B1-c; the high-mass star-forming region Sagittarius B2 (North) (Sgr B2(N)); the solar system comet 67P/Churyumov-Gerasimenko (67P/C-G); and the protoplanetary disk of Oph-IRS 48. We report ∼1–3 orders of magnitude higher abundances compared to Class 0 protostars and ∼1–3 orders of magnitude lower abundances compared to the protoplanetary disk, Sgr B2(N), and 67P/C-G. These results indicate that the protoplanetary disk phase could contribute to the buildup of COMs.
固体状態エタノールアミンのLyα処理：糖とペプチド誘導体の潜在的前駆体 Lyα Processing of Solid-state Ethanolamine: Potential Precursors to Sugar and Peptide Derivatives
T. Suhasaria, S. M. Wee, R. Basalgète, S. Krasnokutski, C. Jäger, K. Schwarz, and Th. Henning
The Astrophysical Journal Published: 2025 March 18
DOI:10.3847/1538-4357/adb486
Abstract
Ethanolamine (EA), a key component of phospholipids, has recently been detected in the interstellar medium within molecular clouds. To understand this observation, laboratory studies of its formation and destruction are essential and should be complemented by astrochemical models. This study investigates the photostability of EA ice under Lyα (10.2 eV) irradiation at 10 K, and explores its potential role in the formation of simple and complex organic molecules (COMs) in molecular clouds. The UV-destruction cross section of EA was estimated to be (4.7 ± 0.3) × 10−18 cm2, providing insight into its half-life of 6.5 × 107 yr in dense interstellar clouds. Fourier transform infrared spectroscopy and quadrupole mass spectrometry were used to identify various photoproducts, with their formation pathways discussed. Ethylene glycol and serine were tentatively detected during the warming-up process following irradiation, suggesting that EA could contribute to the formation of prebiotic molecules such as sugars, peptides, and their derivatives. High-mass signals detected in the mass spectrometer suggest the presence of several COMs, and further analysis of residues at room temperature is planned for future work. The results suggest that EA could contribute to the formation of prebiotic molecules in space, with implications for the origin of life.
