Observations of the H_2O Maser Emission from the LINER Nucleus in NGC 1052

Details Observations of the H_2O Maser Emission from the LINER Nucleus in NGC 1052 Observations of the H_2O Maser Emission from the LINER Nucleus in NGC 1052

Dec 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aas...189.8906b&link_type=abstract

American Astronomical Society, 189th AAS Meeting, #89.06; Bulletin of the American Astronomical Society, Vol. 28, p.1392

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We present single-dish monitoring observations and a VLBA map of the 22 GHz H_2O megamaser emission from the LINER nucleus of NGC 1052. H_2O megamasers are associated with active galaxies and are typically composed of many narrow ( ~ a few km s(-1) FWHM) emission features, but the profile of the H_2O emission from NGC 1052 is broad ( ~ 80 km s(-1) FWHM) with no evidence for narrow peaks. Currently, one other source (TXFS 2226-184) is known to have an H_2O profile similar to that of NGC 1052. These are the only elliptical galaxies with detected H_2O sources. Using single-dish telescopes, we have periodically observed the maser in NGC 1052 for nearly 2 years. The velocity centroid of the broad feature has drifted ~ 50 km s(-1) redward during this time. Velocity drifts of the narrow H_2O maser features in the active galaxy NGC 4258 (and perhaps NGC 2639) have been ascribed to orbital motions of gas in a nuclear molecular disk, and it has been unclear whether the changing H_2O profile in NGC 1052 has a similar dynamical origin. Our VLBA map of the nuclear 22 GHz continuum and H_2O maser features shows that the masers are aligned along the same axis as the continuum jet, hence the masers may not be associated with a nuclear accretion disk. The masers are found primarily in two clumps separated by 0.03 pc (0.4 mas), assuming a distance of 17.8 Mpc. The mean line-of-sight velocity between the clumps differs by ~ 50 km s(-1) . The velocity ``drift'' detected in the single-dish spectra may thus be caused by variations in the relative strengths of these two maser clumps.

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