THE MEGAMASER COSMOLOGY PROJECT. VI. OBSERVATIONS OF NGC 6323
C. Y. KuoAcademia Sinica Institute of Astronomy and Astrophysics, P.O. Box 23-141, Taipei 10617, TaiwanJ. A. BraatzNational Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USAK. Y. LoNational Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USAM. J. ReidHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAS. H. SuyuAcademia Sinica Institute of Astronomy and Astrophysics, P.O. Box 23-141, Taipei 10617, TaiwanD. W. PesceDepartment of Astronomy, University of Virginia, Charlottesville, VA 22904, USAJ. J. CondonNational Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USAC. HenkelAstronomy Department, Faculty of Science, King Abdulaziz University, P.O. Box 80203, Jeddah, Saudi ArabiaC. M. V. ImpellizzeriNational Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USA
2015en
ABI
Annotatsiya
We present observations of the H2O megamasers in the accretion disk of NGC 6323. By combining interferometric and spectral monitoring data, we estimate H$_{0} = 73^{+26}_{-22}$ km/s/Mpc, where the low strength of the systemic masers (<15 mJy) limits the accuracy of this estimate. The methods developed here for dealing with weak maser emission provide guidance for observations of similar sources, until significant increases in radio telescope sensitivity, such as anticipated from the next generation Very Large Array, are realized.
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