Erratum

Author(s)

C. Gieser, Manuel Güdel

Abstract

In the original article (Gieser et al. 2023), in Sect. 3.3 an error occurred in the code of the calculation of the H2 line-integrated intensities estimated from a Gaussian fit. Due to this mistake, we overestimated the H2 line-integrated intensities by a factor of (λ[μm])2. The observed line-integrated intensities were used to estimate the H2 temperature and column density, with a warm and hot component. While the conclusions of the study remain qualitatively unchanged, here we provide correct values for the line-integrated intensities as well as for the H2 temperatures and column densities. The corrected H2 excitation diagram results toward source mmA1 and source B is shown in Fig. 1, corresponding to Fig. 5 in the original paper. The warm and hot temperature components toward mmA1 are ≈560K and ≈2600 K, respectively. The total column density, considering the contribution from both temperature components, is N_warm+hot ≈ 1.39 × 10²¹ cm^-2. Toward source B, we find a higher column density but a lower temperature. The full temperature and column density maps are shown in Fig. 2 (Fig. 6 in the original paper), where the results for the cold component (left column) remain unchanged. With the corrected values, the H2 column densities of the warm component are about two magnitudes lower compared to the cold component. The temperature of the warm component ranges between 250K and 600 K. In the hot component, the column densities are about two orders of magnitude lower, of namely N_hot ≈ 10¹⁹ cm^-2, compared to the warm component and the temperatures are 1000.2500 K. The median temperature is 440K and 1700K for the warm and hot component, respectively, and the median column density is 8.7 × 10²⁰ cm^-2 and 5.8 × 10¹⁸ cm^-2, respectively. In absolute numbers, the median uncertainties are log δN_warm = 0.24 log cm^-2, log δN_hot = 0.73 log cm^-2, δT_warm = 60 K, and δThot = 680 K. Tables 1 (line-integrated intensities) and 2 (excitation diagram results) show corrected versions of Tables A.1 and A.2 of the original paper, respectively. In Sect. 4.1 of the original paper, we compared the derived H2 column densities of IRAS 23385 to the L1157 outflow (Nisini et al. 2010). With the corrected values, we find that the H2 column densities of IRAS 23385 are not four, but two to three orders of magnitude higher. With JWST we are, for the first time, able to probe high-column density regions (>1021 cm.2) thanks to the higher angular resolution.

Organisation(s)

Department of Astrophysics

External organisation(s)

Max-Planck-Institut für extraterrestrische Physik, Max-Planck-Institut für Astronomie

Journal

Astronomy and Astrophysics

Volume

685

No. of pages

4

ISSN

0004-6361

DOI

https://doi.org/10.1051/0004-6361/202450520e

Publication date

05-2024

Peer reviewed

Yes

Austrian Fields of Science 2012

103003 Astronomy, 103004 Astrophysics

ASJC Scopus subject areas

Astronomy and Astrophysics, Space and Planetary Science

Portal url

https://ucrisportal.univie.ac.at/en/publications/8d59b954-8121-4676-822d-ec0c2be7b7f5