Details

Autor(en) / Beteiligte

• Codella, C
• López-Sepulcre, A
• Ohashi, S
• Chandler, C J
• De Simone, M
• Podio, L
• Ceccarelli, C
• Sakai, N
• Alves, F
• Durán, A
• Fedele, D
• Loinard, L
• Mercimek, S
• Murillo, N
• Zhang, Y
• Bianchi, E
• Bouvier, M
• Busquet, G
• Caselli, P
• Dulieu, F
• Feng, S
• Hanawa, T
• Johnstone, D
• Lefloch, B
• Maud, L T
• Moellenbrock, G
• Oya, Y
• Svoboda, B
• Yamamoto, S

Titel

FAUST VI. VLA1623−2417 B: a new laboratory for astrochemistry around protostars on 50 au scale

Ist Teil von

• Monthly notices of the Royal Astronomical Society, 2022-07, Vol.515 (1), p.543-554

Ort / Verlag

Oxford University Press

Erscheinungsjahr

2022

Link zum Volltext

Quelle

EZB Free E-Journals

Beschreibungen/Notizen

• ABSTRACT The ALMA (Atacama Large Millimeter Array) interferometer, with its unprecedented combination of high sensitivity and high angular resolution, allows for (sub-)mm wavelength mapping of protostellar systems at Solar system scales. Astrochemistry has benefitted from imaging interstellar complex organic molecules in these jet–disc systems. Here, we report the first detection of methanol (CH3OH) and methyl formate (HCOOCH3) emission towards the triple protostellar system VLA1623−2417 A1+A2+B, obtained in the context of the ALMA Large Programme FAUST (Fifty AU STudy of the chemistry in the disc/envelope system of solar-like protostars). Compact methanol emission is detected in lines from Eu = 45 K up to 61 K and 537 K towards components A1 and B, respectively. Large velocity gradient analysis of the CH3OH lines towards VLA1623−2417 B indicates a size of 0.11–0.34 arcsec (14–45 au), a column density $N_{\rm CH_3OH}$ = 1016–1017 cm−2, kinetic temperature ≥ 170 K, and volume density ≥ 108 cm−3. A local thermodynamic equilibrium approach is used for VLA1623−2417 A1, given the limited Eu range, and yields Trot ≤ 135 K. The methanol emission around both VLA1623−2417 A1 and B shows velocity gradients along the main axis of each disc. Although the axial geometry of the two discs is similar, the observed velocity gradients are reversed. The CH3OH spectra from B show two broad (4–5 km s−1) peaks, which are red- and blueshifted by ∼ 6–7 km s−1 from the systemic velocity. Assuming a chemically enriched ring within the accretion disc, close to the centrifugal barrier, its radius is calculated to be 33 au. The methanol spectra towards A1 are somewhat narrower (∼ 4 km s−1), implying a radius of 12–24 au.