2020
DOI: 10.1051/0004-6361/201937407
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Abstract: Context. Water megamaser emission at 22 GHz has proven to be a powerful tool for astrophysical studies of active galactic nuclei (AGN) because it allows an accurate determination of the mass of the central black hole and of the accretion disc geometry and dynamics. However, after searches among thousands of galaxies, only about 200 of them have shown such spectroscopic features, most of them of uncertain classification. In addition, the physical and geometrical conditions under which a maser activates are stil… Show more

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Cited by 9 publications
(11 citation statements)
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References 92 publications
(64 reference statements)
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“…The detection rate of very luminous AGN-origin megamaser 183 GHz H 2 O emission is low (1/8 = 12.5%). The detection rates of 22 GHz H 2 O 6 1,6 -5 2,3 megamaser emission in previously conducted ex- tensive surveys are also low ( 10%) for active galaxies (e.g., Braatz et al 1997;Hagiwara et al 2002;Greenhill et al 2003;Braatz et al 2004;Henkel et al 2005), but can increase (10-50%) if only highly obscured AGNs are observed (e.g., Kondratko et al 2006;Yamauchi et al 2017;Castangia et al 2019;Kuo et al 2020;Panessa et al 2020). Observations of a larger number of nearby (U)LIRGs that are diagnosed to host luminous obscured AGNs, are needed to better constrain how the detection rates of very luminous 183 GHz H 2 O megamaser emission differ from those of 22 GHz H 2 O magamaser emission.…”
Section: Summary Of the 183 Ghz H 2 O Emissionmentioning
confidence: 92%
“…The detection rate of very luminous AGN-origin megamaser 183 GHz H 2 O emission is low (1/8 = 12.5%). The detection rates of 22 GHz H 2 O 6 1,6 -5 2,3 megamaser emission in previously conducted ex- tensive surveys are also low ( 10%) for active galaxies (e.g., Braatz et al 1997;Hagiwara et al 2002;Greenhill et al 2003;Braatz et al 2004;Henkel et al 2005), but can increase (10-50%) if only highly obscured AGNs are observed (e.g., Kondratko et al 2006;Yamauchi et al 2017;Castangia et al 2019;Kuo et al 2020;Panessa et al 2020). Observations of a larger number of nearby (U)LIRGs that are diagnosed to host luminous obscured AGNs, are needed to better constrain how the detection rates of very luminous 183 GHz H 2 O megamaser emission differ from those of 22 GHz H 2 O magamaser emission.…”
Section: Summary Of the 183 Ghz H 2 O Emissionmentioning
confidence: 92%
“…Moreover, the maser detection rate could increase significantly in a criterion exploiting MIR and X-ray sample (Castangia et al 2016(Castangia et al , 2019. Panessa et al (2020) found the maser detection rate tend to be much higher in type 2 and Compton-thick AGNs (Further discussion in §5.4). In this studies, we focus on improving maser detection rate using MIR spectra.…”
Section: Maser Detection Ratementioning
confidence: 94%
“…We adopted the total maser sample of 161 targets from Kuo et al (2018) with classification. In order to get a complete maser type classification, we also cross-matched maser catalogue from Panessa et al (2020) and replenish the additional maser types (e.g. jet/outflow).…”
Section: Sample Of Water Megamaser Galaxiesmentioning
confidence: 99%
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