Volume 475, Number 2, November IV 2007
|Page(s)||549 - 558|
|Section||Interstellar and circumstellar matter|
|Published online||04 September 2007|
Energetic radiation and the sulfur chemistry of protostellar envelopes: submillimeter interferometry of AFGL 2591 *
Institute of Astronomy, ETH, 8092 Zurich, Switzerland e-mail: firstname.lastname@example.org
2 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
3 Max-Planck Institut für Radioastronomie, auf dem Hügel 69, 53121 Bonn, Germany
4 Netherlands Institute for Space Research (SRON), Landleven 12, 9747 AD Groningen, The Netherlands
5 Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands
Accepted: 31 August 2007
Context.The chemistry in the inner few thousand AU of accreting envelopes around young stellar objects is predicted to vary greatly with far-UV and X-ray irradiation by the central star.
Aims.We search for molecular tracers of high-energy irradiation by the protostar in the hot inner envelope.
Methods.The Submillimeter Array (SMA) has observed the high-mass star forming region AFGL 2591 in lines of CS, SO, HCN, HCN( = 1), and HC15N with 0.6'' resolution at 350 GHz probing radial scales of 600-3500 AU for an assumed distance of 1 kpc. The SMA observations are compared with the predictions of a chemical model fitted to previous single-dish observations.
Results.The CS and SO main peaks are extended in space at the FWHM level, as predicted in the model assuming protostellar X-rays. However, the main peak sizes are found smaller than modeled by nearly a factor of 2. On the other hand, the lines of CS, HCN, and HC15N, but not SO and HCN( = 1), show pedestal emissions at radii 3500 AU that are not predicted. All lines except SO show a secondary peak within the approaching outflow cone. A dip or null in the visibilities caused by a sharp decrease in abundance with increasing radius is not observed in CS and only tentatively in SO.
Conclusions.The emission of protostellar X-rays is supported by the good fit of the modeled SO and CS amplitude visibilities including an extended main peak in CS. The broad pedestals can be interpreted by far-UV irradiation in a spherically non-symmetric geometry, possibly comprising outflow walls on scales of 3500-7000 AU. The extended CS and SO main peaks suggest sulfur evaporation near the 100 K temperature radius. The effects of the corresponding abundance jumps may be reduced in visibility plots by smoothing due to inhomogeneity at the evaporation radius, varying by ±10% or more in different directions.
Key words: accretion, accretion disks / stars: formation / submillimeter / astrochemistry / ISM: molecules / X-rays: ISM
© ESO, 2007
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