2005
DOI: 10.1007/s10511-005-0022-7
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Properties of OH Megamaser Galaxies in the Radio Continuum. II. Data Analysis

Abstract: The properties of OH megamaser galaxies in the radio continuum are discussed. Many radio sources in OH megamaser galaxies exhibit relatively flat ( -0.5 ≥ α ) radio spectra between frequencies of 1.49 and 8.44 GHz along with high brightness temperatures ( 4 10 ≥ b T K). In these galaxies the line and radio continuum fluxes are not correlated. The continuum radio emission of OH megamasers is predominantly nonthermal and is associated either with an active nucleus or with compact star formation. The thermal comp… Show more

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Cited by 9 publications
(18 citation statements)
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“…Since the principle for selecting the galaxies in the present sample is their megamaser activity and many of them have relatively flat spectral indices and high brightness temperatures [1], we may assume that the megamaser activity and nuclear activity are interrelated. Furthermore, the observed correlations between the variables L 2-10keV , W, and L 1.49 (Table 2) suggest the presence of AGN in these galaxies.…”
Section: Discussionmentioning
confidence: 99%
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“…Since the principle for selecting the galaxies in the present sample is their megamaser activity and many of them have relatively flat spectral indices and high brightness temperatures [1], we may assume that the megamaser activity and nuclear activity are interrelated. Furthermore, the observed correlations between the variables L 2-10keV , W, and L 1.49 (Table 2) suggest the presence of AGN in these galaxies.…”
Section: Discussionmentioning
confidence: 99%
“…) [1]. The observed flat radio spectra and high brightness temperatures suggest the presence of an active nucleus (AGN) in these galaxies, although some megamasers may be associated with active star formation (SB).…”
Section: Introductionmentioning
confidence: 92%
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“…Therefore, It is surprising that these entirely different methods of calculating the slope of L 2-10keV as a function of M c yield essentially the same result (1.27 and 1.28).Furthermore, Eq. (2) of Ref 23. can be used to calculate the expected widths of the lines for the four galaxies, for which the required parameters of their rotating disks have been measured by VLBI observations.…”
mentioning
confidence: 99%