Volume 651, July 2021
|Number of page(s)||1|
|Section||Interstellar and circumstellar matter|
|Published online||01 July 2021|
Studying star-forming processes at core and clump scales: the case of the young stellar object G29.862−0.0044 (Corrigendum)
CONICET – Universidad de Buenos Aires. Instituto de Astronomía y Física del Espacio CC 67,
Buenos Aires, Argentina
2 Isaac Newton Group of Telescopes, 38700, La Palma, Spain
3 Instituto de Astrofísica de Canarias (IAC) and Universidad de La Laguna, Dpto. Astrofísica, Spain
4 Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile
Key words: stars: formation / stars: protostars / ISM: jets and outflows / ISM: molecules / errata, addenda
In the original article, a molecular emission line was not correctly identified. One of the used pieces of millimeter data obtained from the Atacama Large Millimeter Array database was incorrectly identified as the CH3OCHO 20(2,19)–19(2,18)E line. The analyzed emission corresponds to the cyano radical (CN) N = 2–1, J = 5∕2–3/2, F = 7∕2–5/2 line at 226874.764 MHz, which can be blended with the F = 5∕2–3/2 and F = 3∕2–1/2 lines at 226874.183 and 226875.896 MHz, respectively. Hence, in Figs. 4, 5 and 7 of the original paper, the CN integrated emission is presented.
This misunderstanding does not alter any conclusion made in the original paper. The discussion regarding the morphology of the integrated CH3OCHO emission and its relations with the infrared data still applies to the CN emission in the same way. As some works show (Han et al. 2015; Qiu et al. 2012; Zapata et al. 2008; Beuther et al. 2004), extended CN emission is usually detected towards molecular cores and star-formingregions, and this type of emission usually extends in filaments and concentrates in knots as is the case in G29.862−0.0044. In a following, paper we will study the CN emission towards a large sample of molecular cores, including this particular source (Paron et al., in prep.).
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- Zapata, L. A., Palau, A., Ho, P. T. P., et al. 2008, A&A, 479, L25 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
© ESO 2021
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