Detection of amino acetonitrile in Sgr B2(N)
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: email@example.com
3 National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903-2475, USA e-mail: firstname.lastname@example.org
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
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.
Key words: astrobiology / astrochemistry / line: identification / stars: formation / ISM: individual objects: Sagittarius B2 / errata, addenda
© ESO, 2008