HCOOCH₃ as a probe of temperature and structure in Orion-KL^{⋆,⋆⋆,⋆⋆⋆}

¹ Université de Bordeaux, OASU, 2 rue de l’Observatoire, BP 89, 33271 Floirac Cedex, France
e-mail: favre@phys.au.dk; despois@obs.u-bordeaux1.fr, brouillet@obs.u-bordeaux1.fr, baudry@obs.u-bordeaux1.fr
² CNRS, UMR 5804, Laboratoire d’Astrophysique de Bordeaux, 2 rue de l’Observatoire, BP 89, 33271 Floirac Cedex, France
³ Observatoire de Paris, LERMA, 61 Av. de l’Observatoire, 75014 Paris, France
e-mail: francoise.combes@obspm.fr
⁴ Institut de Radioastronomie Millimétrique, Domaine Universitaire, 300 rue de la piscine, 38400 St Martin d’Hères, France
e-mail: guelin@iram.fr
⁵ National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903-2475, USA
e-mail: awootten@nrao.edu
⁶ Laboratoire de Physique des Lasers, Atomes et Molécules, Université de Lille1, UMR 8523, 59655 Villeneuve d’Ascq Cedex, France
e-mail: georges.wlodarczak@univ-lille1.fr

Received: 6 July 2010
Accepted: 4 March 2011

Abstract

Context. The Orion Kleinmann-Low nebula (Orion-KL) is a complex region of star formation. Whereas its proximity allows studies on a scale of a few hundred AU, spectral confusion makes it difficult to identify molecules with low abundances.

Aims. We studied an important oxygenated molecule, HCOOCH₃, to characterize the physical conditions, temperature, and density of the different molecular source components. Methyl formate presents strong close rotational transitions covering a wide range of energy, and its emission in Orion-KL is not contaminated by the emission of N-bearing molecules. This study will help in the future 1) to constrain chemical models for the formation of methyl formate in gas phase or on grain mantles and 2) to search for more complex or prebiotic molecules.

Methods. We used high-resolution observations from the IRAM Plateau de Bure Interferometer to reduce spectral confusion and to better isolate the molecular emission regions. We used twelve data sets with a spatial resolution down to 1.8″  ×  0.8″. Continuum emission was subtracted by selecting apparently line-free channels.

Results. We identify 28 methyl formate emission peaks throughout the 50″ field of observations. The two strongest peaks, named MF1 and MF2, are in the Compact Ridge and in the southwest of the Hot Core, respectively. From a comparison with single-dish observations, we estimate that we miss less than 15% of the flux and that spectral confusion is still prevailing as half of the expected transitions are blended over the region. Assuming that the transitions are thermalized, we derive the temperature at the five main emission peaks. At the MF1 position in the Compact Ridge we find a temperature of 80 K in a 1.8″  ×  0.8″ beam size and 120 K on a larger scale (3.6″  ×  2.2″), suggesting an external source of heating, whereas the temperature is about 130 K at the MF2 position on both scales. Transitions of methyl formate in its first torsionally excited state are detected as well, and the good agreement of the positions on the rotational diagrams between the ground state and the v_t = 1 transitions suggests a similar temperature. The LSR velocity of the gas is between 7.5 and 8.0 km s^-1 depending on the positions and column density peaks vary from 1.6  ×  10¹⁶ to 1.6  ×  10¹⁷ cm^-2. A second velocity component is observed around 9−10 km s^-1 in a north-south structure stretching from the Compact Ridge up to the BN object, and this component is warmer at the MF1 peak. The two other C₂H₄O₂ isomers are not detected, and the derived upper limit for the column density is  ≤3  ×  10¹⁴ cm^-2 for glycolaldehyde and  ≤2  ×  10¹⁵ cm^-2 for acetic acid. From the 223 GHz continuum map, we identify several dust clumps with associated gas masses in the range 0.8 to 5.8 M_⊙. Assuming that the methyl formate is spatially distributed as the dust is, we find relative abundances of methyl formate in the range  ≤0.1  ×  10^-8 to 5.2  ×  10^-8. We suggest a relation between the methyl formate distribution and shocks as traced by 2.12 μm H₂ emission.