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Very Long Baseline Interferometry imaging of H2O maser emission in the nearby radio galaxy NGC 4261
Astrophysics of Galaxies · Submitted 26 Apr 2023
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim A positional coincidence between H2O maser emission and an ionized gas disk implies that the H2O maser emission arises from the near side of the disk, amplifying continuum emission from the background receding jet.
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We report dual-frequency very long baseline interferometry (VLBI) observations at 22 and 43 GHz toward the nucleus of a nearby radio galaxy NGC 4261. In particular, we present a VLBI image of the 22 GHz H2O maser line and its location in the circumnuclear region of NGC 4261. H2O maser emission is marginally detected above the three times the rms level within a velocity range of approximately 2250-2450 km/s, slightly red-shifted with respect to the systemic velocity. H2O maser emission is located approximately 1 milliarcsecond (mas) east of the brightest continuum component at 22 GHz, where the continuum spectrum is optically thick, that is at the free-free absorbed receding jet by ionized gas. A positional coincidence between H2O maser emission and an ionized gas disk implies that the H2O maser emission arises from the near side of the disk, amplifying continuum emission from the background receding jet. If the disk axis is oriented 64 degree relative to the line of sight, the H2O maser emission is expected to be at a mean radius of 0.3 pc in the disk. The broad line width of the H2O maser emission can be attributed to complex kinematics in the immediate vicinity of the supermassive black hole (SMBH), including ongoing gas infall onto the SMBH, turbulence, and outflow. This is analogous to the multi-phase circumnuclear torus model in the nearest radio-loud H2O megamaser source NGC 1052. An alternative explanation for H2O maser association is the shock region between the jet and the ambient molecular clouds. However, this explanation fails to describe the explicit association of H2O maser emission only with the free-free absorbed receding jet.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We report dual-frequency very long baseline interferometry (VLBI) observations at 22 and 43 GHz toward the nucleus of a nearby radio galaxy NGC 4261. | contribution 0.72 | 0.97 | 0.04 | asserted 0.99 |
| s1 | In particular, we present a VLBI image of the 22 GHz H2O maser line and its location in the circumnuclear region of NGC 4261. | contribution 0.93 | 0.96 | 0.09 | asserted 1.00 |
| s2 | H2O maser emission is marginally detected above the three times the rms level within a velocity range of approximately 2250-2450 km/s, slightly red-shifted with respect to the systemic velocity. | result 1.00 | 0.94 | 0.08 | asserted 0.84 |
| s3 | H2O maser emission is located approximately 1 milliarcsecond (mas) east of the brightest continuum component at 22 GHz, where the continuum spectrum is optically thick, that is at the free-free absorbed receding jet by ionized gas. | result 0.91 | 0.90 | 0.18 | asserted 1.00 |
| s4 | A positional coincidence between H2O maser emission and an ionized gas disk implies that the H2O maser emission arises from the near side of the disk, amplifying continuum emission from the background receding jet. | interpretation 1.00 | 0.71 | 0.53 | hedged possibility 0.59 |
| s5 | If the disk axis is oriented 64 degree relative to the line of sight, the H2O maser emission is expected to be at a mean radius of 0.3 pc in the disk. | interpretation 0.91 | 0.46 | 0.10 | hedged possibility 0.84 |
| s6 | The broad line width of the H2O maser emission can be attributed to complex kinematics in the immediate vicinity of the supermassive black hole (SMBH), including ongoing gas infall onto the SMBH, turbulence, and outflow. | interpretation 0.99 | 0.68 | 0.12 | hedged possibility 0.75 |
| s7 | This is analogous to the multi-phase circumnuclear torus model in the nearest radio-loud H2O megamaser source NGC 1052. | interpretation 0.83 | 0.12 | 0.07 | asserted 0.94 |
| s8 | An alternative explanation for H2O maser association is the shock region between the jet and the ambient molecular clouds. | interpretation 0.95 | 0.10 | 0.03 | hedged possibility 0.73 |
| s9 | However, this explanation fails to describe the explicit association of H2O maser emission only with the free-free absorbed receding jet. | interpretation 0.97 | 0.55 | 0.09 | asserted 1.00 |
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Original abstract
We report dual-frequency very long baseline interferometry (VLBI) observations at 22 and 43 GHz toward the nucleus of a nearby radio galaxy NGC 4261. In particular, we present a VLBI image of the 22 GHz H2O maser line and its location in the circumnuclear region of NGC 4261. H2O maser emission is marginally detected above the three times the rms level within a velocity range of approximately 2250-2450 km/s, slightly red-shifted with respect to the systemic velocity. H2O maser emission is located approximately 1 milliarcsecond (mas) east of the brightest continuum component at 22 GHz, where the continuum spectrum is optically thick, that is at the free-free absorbed receding jet by ionized gas. A positional coincidence between H2O maser emission and an ionized gas disk implies that the H2O maser emission arises from the near side of the disk, amplifying continuum emission from the background receding jet. If the disk axis is oriented 64 degree relative to the line of sight, the H2O maser emission is expected to be at a mean radius of 0.3 pc in the disk. The broad line width of the H2O maser emission can be attributed to complex kinematics in the immediate vicinity of the supermassive black hole (SMBH), including ongoing gas infall onto the SMBH, turbulence, and outflow. This is analogous to the multi-phase circumnuclear torus model in the nearest radio-loud H2O megamaser source NGC 1052. An alternative explanation for H2O maser association is the shock region between the jet and the ambient molecular clouds. However, this explanation fails to describe the explicit association of H2O maser emission only with the free-free absorbed receding jet.
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