A High Spectral Resolution VLBI Study of the 12 GHz Methanol Masers in W3(OH): Their Submilliarcsecond Structure and Clues on Saturation

Details A High Spectral Resolution VLBI Study of the 12 GHz Methanol Masers in W3(OH): Their Submilliarcsecond Structure and Clues on Saturation A High Spectral Resolution VLBI Study of the 12 GHz Methanol Masers in W3(OH): Their Submilliarcsecond Structure and Clues on Saturation

Feb 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003apj...583..776m&link_type=abstract

The Astrophysical Journal, Volume 583, Issue 2, pp. 776-788.

Astronomy and Astrophysics

Astronomy

12

Ism: H Ii Regions, Ism: Individual: Alphanumeric: W3, Ism: Molecules, Masers- Radio Lines: Ism, Stars: Formation

Scientific paper

This paper reports on the results of high velocity resolution (0.02 km s-1) VLBA observations of the 12 GHz methanol masers toward the ultracompact (UC) H II region W3(OH). About 50 maser features are detected, and their emission is resolved both in velocity and in space (with an angular resolution of ~1 mas). The maser feature spectra are very well reproduced by single Gaussian profiles, and a narrow distribution for the FWHM line widths is found from 0.14 to 0.32 km s-1. The measured brightness temperatures distribute over the range 1010to2×1012 K.
By performing elliptical Gaussian fits, the spot parameters (peak position, intensity, and FWHM sizes) in the high velocity resolution maps were derived. The highest brightness temperatures occur in correspondence with the smallest spots, with FWHM size <=4 AU. For all the maser features, it is found that the channel peak positions vary smoothly with the velocity, delineating straight or arclike distributions projected onto the sky. In most cases, the channel (line-of-sight) velocities vary linearly with the peak positional shifts, with measured gradients in the range 0.05-0.65 km s-1 mas-1 (0.02-0.30 km s-1 AU-1).
Most of the maser spot spectra have very small deviations from a Gaussian profile, <=2×10-3, and a trend for decreasing deviations with increasing intensities is noted. In most cases, the kurtosis of the spectral profiles is positive, with the most accurate values concentrated in the range 0.1-0.5. Comparison of these results with recent calculations of the deviations from a Gaussian profile that occur across the line profile of a linear maser (as a result of the amplification process) suggests that the 12 GHz CH3OH masers are below the threshold, I0, at which line rebroadening occurs. However, the model predicts deviations from a Gaussian profile significantly smaller than the observed values, and this discrepancy needs to be investigated. In particular, the calculations of the deviations from a Gaussian profile should take into account the effects of a velocity gradient through the maser features (evidenced by our observations) that will influence the spectral profile. The maximum output given by the pump rate of saturated masers may account for the observational result that the highest intensities are found in correspondence with the smallest sky-projected spot areas.

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