A new, rotating hot corino in Serpens. (arXiv:1906.08848v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Martin_Domenech_R/0/1/0/all/0/1">R. Martin-Domenech</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oberg_K/0/1/0/all/0/1">K.I. Oberg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bergner_J/0/1/0/all/0/1">J.B. Bergner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jorgensen_J/0/1/0/all/0/1">J.K. Jorgensen</a>
We have observed 29 transitions corresponding to 12 distinct species and 7
additional isotopologs toward the deeply embedded Class 0 young stellar object
Ser-emb 1 with the Atacama Large Millimeter Array at 1 mm. The detected species
include CH3OH and two complex organic molecules, CH3OCH3 and CH3OCHO. The
emission of CH3OH and the two COMs is compact, and the CH3OH rotational
temperature is 261 (46) K, implying that Ser-emb 1 hosts a hot corino. The
derived CH3OH, CH3OCH3 and CH3OCHO column densities are at least 1.2 (0.4)E17
cm-2, 9.2 (3.8)E16 cm-2, and 9.1 (3.6)E16 cm-2, respectively, comparable to the
values found for other Class 0 hot corinos. In addition, we observe evidence of
rotation at compact scales: two of the more strongly detected lines,
corresponding to C18O and H2CO present spatially resolved red- and blue-shifted
compact emission orthogonal to the direction of a jet and outflow traced by CO,
SiO, and several other molecules. The spatial coincidence of the hot corino
emission and a possible disk in a compact region around the central protostar
suggests that these structures may be physically and/or chemically related.
We have observed 29 transitions corresponding to 12 distinct species and 7
additional isotopologs toward the deeply embedded Class 0 young stellar object
Ser-emb 1 with the Atacama Large Millimeter Array at 1 mm. The detected species
include CH3OH and two complex organic molecules, CH3OCH3 and CH3OCHO. The
emission of CH3OH and the two COMs is compact, and the CH3OH rotational
temperature is 261 (46) K, implying that Ser-emb 1 hosts a hot corino. The
derived CH3OH, CH3OCH3 and CH3OCHO column densities are at least 1.2 (0.4)E17
cm-2, 9.2 (3.8)E16 cm-2, and 9.1 (3.6)E16 cm-2, respectively, comparable to the
values found for other Class 0 hot corinos. In addition, we observe evidence of
rotation at compact scales: two of the more strongly detected lines,
corresponding to C18O and H2CO present spatially resolved red- and blue-shifted
compact emission orthogonal to the direction of a jet and outflow traced by CO,
SiO, and several other molecules. The spatial coincidence of the hot corino
emission and a possible disk in a compact region around the central protostar
suggests that these structures may be physically and/or chemically related.
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