Detection of amino acetonitrile in Sgr B2(N)

¹ Max-Planck Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany e-mail: [belloche;kmenten;ccomito;schilke;sthorwirth;chieret]@mpifr-bonn.mpg.de
² I. Physikalisches Institut, Universität zu Köln, Zülpicher Str. 77, 50937 Köln, Germany e-mail: hspm@ph1.uni-koeln.de

³ National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903-2475, USA e-mail: jott@nrao.edu
⁴ California Institute of Technology, 1200 E. California Blvd., Caltech Astronomy, 105-24, Pasadena, CA 91125-2400, USA
⁵ CSIRO Australia Telescope National Facility, Cnr Vimiera & Pembroke Roads, Marsfield NSW 2122, Australia

Abstract

Aims. A small error was recently found in the program used to compute the integrated intensities in the article Belloche et al. (2008, A&A, 482, 179).

Methods. We provide new versions of Fig. 2 and Tables 3, 5, and 7 with the correct integrated intensities.

Results. The conclusions drawn by Belloche et al. (2008) are not significantly affected by these corrections. Only the mass, density, and central H₂ column density of the compact source emitting the amino acetonitrile lines appear to have been underestimated by 30–40%. This led to an overestimate of the abundance of amino acetonitrile by the same amount. However, the magnitude of this correction is less than the estimated uncertainties on these parameters.