SIMBAD references

2008A&A...482..179B - Astronomy and Astrophysics, volume 482, 179-196 (2008/4-4)

Detection of amino acetonitrile in Sgr B2(N).

BELLOCHE A., MENTEN K.M., COMITO C., MUELLER H.S.P., SCHILKE P., OTT J., THORWIRTH S. and HIERET C.

Abstract (from CDS):

Amino acids are building blocks of proteins and therefore key ingredients for the origin of life. The simplest amino acid, glycine (NH2CH2COOH), has long been searched for in the interstellar medium but has not been unambiguously detected so far. At the same time, more and more complex molecules have been newly found toward the prolific Galactic center source Sagittarius B2. Since the search for glycine has turned out to be extremely difficult, we aimed at detecting a chemically related species (possibly a direct precursor), amino acetonitrile (NH2CH2CN). With the IRAM 30 m telescope we carried out a complete line survey of the hot core regions Sgr B2(N) and (M) in the 3mm range, plus partial surveys at 2 and 1.3mm. We analyzed our 30m line survey in the LTE approximation and modeled the emission of all known molecules simultaneously. We identified spectral features at the frequencies predicted for amino acetonitrile lines having intensities compatible with a unique rotation temperature. We also used the Very Large Array to look for cold, extended emission from amino acetonitrile. We detected amino acetonitrile in Sgr B2(N) in our 30m telescope line survey and conducted confirmatory observations of selected lines with the IRAM Plateau de Bure and the Australia Telescope Compact Array interferometers. The emission arises from a known hot core, the Large Molecule Heimat, and is compact with a source diameter of 2" (0.08pc). We derived a column density of 2.8x1016cm–2, a temperature of 100K, and a linewidth of 7km/s. Based on the simultaneously observed continuum emission, we calculated a density of 1.7x108cm–3, a mass of 2340M, and an amino acetonitrile fractional abundance of 2.2x10–9. The high abundance and temperature may indicate that amino acetonitrile is formed by grain surface chemistry. We did not detect any hot, compact amino acetonitrile emission toward Sgr B2(M) or any cold, extended emission toward Sgr B2, with column-density upper limits of 6x1015 and 3x1012–14cm–2, respectively. Based on our amino acetonitrile detection toward Sgr B2(N) and a comparison to the pair methylcyanide/acetic acid both detected in this source, we suggest that the column density of both glycine conformers in Sgr B2(N) is well below the best upper limits published recently by other authors, and probably below the confusion limit in the 1-3mm range.

Abstract Copyright:

Journal keyword(s): astrobiology - astrochemistry - line: identification - stars: formation - ISM: individual objects: Sagittarius B2 - ISM: molecules

VizieR on-line data: <Available at CDS (J/A+A/482/179): maps.dat fig/*>

Errata: erratum vol. 492, p.769 (2008)

CDS comments: Paragraph. 2.3 PKS 1759-39 not identified.

Simbad objects: 31

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