THE MEGAMASER COSMOLOGY PROJECT. VIII. A GEOMETRIC DISTANCE TO NGC 5765b

Gao, F.; Braatz, J. A.; Reid, M. J.; Lo, K. Y.; Condon, J. J.; Henkel, C.; Kuo, C. Y.; Impellizzeri, C. M. V.; Pesce, Dominic W.; Zhao, Wei

doi:10.3847/0004-637x/817/2/128

Cited by 92 publications

(117 citation statements)

References 23 publications

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“…The host galaxies are ∼L * spirals with Hubble types S0-Sbc, while the derived M BH have values ranging from 10 6 to 10 8  M (e.g., Greene et al 2010;Kuo et al 2011). Here we add * s measurements for seven galaxies, whose M BH are presented in Gao et al (2016aGao et al ( , 2016b and W. Zhao et al (2016, in preparation) (Table 1).…”

Section: Megamaser Disk Galaxies Sample and Observationsmentioning

confidence: 99%

Megamaser Disks Reveal a Broad Distribution of Black Hole Mass in Spiral Galaxies

Greene

Seth

Kim

et al. 2016

ApJL

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106

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We use new precision measurements of black hole (BH) masses from water megamaser disks to investigate scaling relations between macroscopic galaxy properties and supermassive BH mass. The megamaser-derived BH masses span 10 6 -10M , while all the galaxy properties that we examine (including total stellar mass, central mass density, and central velocity dispersion) lie within a narrower range. Thus, no galaxy property correlates tightly with M BH in ∼L * spiral galaxies as traced by megamaser disks. Of them all, stellar velocity dispersion provides the tightest relation, but at fixed * s the mean megamaser M BH are offset by −0.6 ± 0.1 dex relative to early-type galaxies. Spiral galaxies with non-maser dynamical BH masses do not appear to show this offset. At low mass, we do not yet know the full distribution of BH mass at fixed galaxy property; the non-maser dynamical measurements may miss the low-mass end of the BH distribution due to an inability to resolve their spheres of influence and/or megamasers may preferentially occur in lower-mass BHs.

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Section: Megamaser Disk Galaxies Sample and Observationsmentioning

confidence: 99%

Megamaser Disks Reveal a Broad Distribution of Black Hole Mass in Spiral Galaxies

Greene

Seth

Kim

et al. 2016

ApJL

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106

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“…Uncertainties are quoted at the 90% confidence limit, unless stated otherwise. No cosmology was assumed to derive luminosities, since we use the angular diameter distance to NGC 5765B (126.3 Mpc, Gao et al 2016) and its redshift (z = 0.02754, Ahn et al 2012).…”

Section: Introductionmentioning

confidence: 99%

Measuring the Obscuring Column of a Disk Megamaser AGN in a Nearby Merger

Masini

Comastri

Hickox

et al. 2019

ApJ

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Active Galactic Nuclei (AGNs) hosting disk water megamasers are well known to be obscured by large amounts of gas, likely due to the presence along the line of sight of an almost edge-on disky structure orbiting the supermassive black hole. Correcting for the high obscuration is crucial to infer parameters intrinsic to the source, like its luminosity. We present a broadband X-ray spectral analysis of a water megamaser AGN in an early merger (NGC 5765B), combining Chandra and NuSTAR data. NGC 5765B is highly Compton-thick and reflectiondominated, following the general trend among disk megamasers. Combining the exquisite black hole mass from masers with our X-ray spectroscopy, the Eddington ratio of the megamaser is estimated to be in the 2 − 14% range, and its robustness is confirmed through SED fitting.

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“…Gao et al (2016)). The observational signature of a back-side maser would be an acceleration in the opposite sense of the front-side systemic maser acceleration (i.e., negative acceleration under the convention that positive velocities are redshifted).…”

Section: Back-side Masers In Edge-on Disksmentioning

confidence: 99%

How to Detect Inclined Water Maser Disks (and Possibly Measure Black Hole Masses)

Darling

2017

ApJ

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We describe a method to identify inclined water maser disks orbiting massive black holes and to potentially use them to measure black hole masses. Due to the geometry of maser amplification pathways, the minority of water maser disks are observable: only those viewed nearly edge-on have been identified, suggesting that an order of magnitude additional maser disks exist. We suggest that inward-propagating masers will be gravitationally deflected by the central black hole, thereby scattering water maser emission out of the disk plane and enabling detection. The signature of an inclined water maser disk would be narrow masers near the systemic velocity that appear to emit from the black hole position, as identified by the radio continuum core. To explore this possibility, we present high resolution (0.07 ′′ -0.17 ′′ ) Very Large Array line and continuum observations of 13 galaxies with narrow water maser emission and show that three are good inclined disk candidates (five remain ambiguous). In the best case, for CGCG 120−039, we show that the maser and continuum emission are coincident to within 3.5 ± 1.4 pc (6.7 ± 2.7 milliarcsec). Subsequent very long baseline interferometric maps can confirm candidate inclined disks and have the potential to show maser rings or arcs that provide a direct measurement of black hole mass, although the mass precision will rely on knowledge of the size of the maser disk.

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THE MEGAMASER COSMOLOGY PROJECT. VIII. A GEOMETRIC DISTANCE TO NGC 5765b

Cited by 92 publications

References 23 publications

Megamaser Disks Reveal a Broad Distribution of Black Hole Mass in Spiral Galaxies

Megamaser Disks Reveal a Broad Distribution of Black Hole Mass in Spiral Galaxies

Measuring the Obscuring Column of a Disk Megamaser AGN in a Nearby Merger

How to Detect Inclined Water Maser Disks (and Possibly Measure Black Hole Masses)

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