The OH Megamaser galaxy IRAS11506−3851: an AGN and star formation revealed by multiwavelength observations

Hekatelyne, C.; Riffel, Rogemar A.; Storchi‐Bergmann, Thaisa; Kharb, P.; Robinson, Andrew; Sales, Dinalva A.; Cassanta, Claudia M.

doi:10.1093/mnras/staa2479

Cited by 10 publications

(12 citation statements)

References 55 publications

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“…The OHM galaxies could either represent a transition stage between a starburst and the emergence of an AGN through the merging process (Peng et al 2020) or harbor a recently triggered AGN (Hekatelyne et al 2020). IIZw 096 is the second object to co-host both water and OH megamasers, and these dual-megamasers might be only emerging during a brief phase of the galaxy evolution (e.g., from starburst nucleus to an AGN, see Wiggins et al 2016).…”

Section: Radio Continuummentioning

confidence: 99%

“…The dominant energy source in the central regions of OHM galaxies usually presents the features of a starburst and an active galactic nucleus (AGN), and in turn the radio continuum emission is produced from these activities. Based on multi-band observations, Hekatelyne et al (2020) present a hypothesis that OHM galaxies harbor a recently triggered AGN. High-resolution observations might be essential to determine whether OHM galaxies are hosting an AGN or compact starburst, and their connections with merging stages and other environmental parameters (see Peng et al 2020, and references therein).…”

Section: Introductionmentioning

confidence: 99%

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Radio properties of the OH megamaser galaxy IIZw 096

Sotnikova

et al. 2022

A&A

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Based on the two-epoch European Very Long Baseline Interferometry (VLBI) Network (EVN) archive data from OH line observations of IIZw 096, we confirm that the high-resolution OH emission in this source mainly comes from two spots (OH1 and OH2) of component (comp) D1 of this merging system. We found no significant variations in the OH 1667 MHz line emission, including flux densities and peak positions. The OH 1665 MHz line emission is detected at about the 6σ level in the OH1 region by combining two epochs of EVN observations. By using archival data from the Very Long Baseline Array (VLBA), Very Large Array (VLA), and Atacama Large Millimeter Array (ALMA) observations, we investigated the properties of the environment of this component through H I, CO(3-2), and HCO+(4-3) lines and the multi-band radio continuum emission. We found that the comp D1 shows the brightest CO, HCO+ line emission, as well as multi-band radio continuum emission. The environment around D1 shows no clear velocity structure associated with circular motions, making it different from most other OH megamasers (OHMs) in the literature, which might have been caused by an effect during the merger stage. Meanwhile, we found that the CO emission shows three velocity structures around D1, including the central broad full width at half maximum (FWHM) region, the double-peak region where the CO line profile shows two separated peaks, and the region of the high-velocity clouds where the CO line peaks at a high velocity (∼11 000 km s−1). Similarly, H Iobservations in absorption also show high-velocity clouds around the D1 region, which might be due to inflows caused by the merging of two or more galaxy components. Based on the high-resolution K-band VLA and L-band VLBA observations of the radio continuum emission, we derived the brightness temperature in the range 105 K–106 K, which is consistent with other starburst dominant OHM sources in the literature. The multi-band VLA observations show that the radio continuum emission of comp D might also have contributions from free-free emission in addition to synchrotron emission. As a consequence, these results support a starburst origin for the OHMs, without the presence of an active galactic nucleus (AGN).

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Section: Radio Continuummentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Radio properties of the OH megamaser galaxy IIZw 096

Sotnikova

et al. 2022

A&A

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“…We found LHα, out = (2.4±0.2)×10 40 erg s −1 for the outflow component and L Hα, disc = (8.7 ± 0.3) × 10 40 erg s −1 for the gas disc component. We used these values to estimate the mass of ionised gas with the equation (Hekatelyne et al 2020):…”

Section: Ionised Gas Outflowsmentioning

confidence: 99%

IFU observations of the inner 200 pc of NGC 4546: gas rotation, non-circular motions, and ionized outflows

Heckler

Ricci

Riffel

2022

Monthly Notices of the Royal Astronomical Society

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We present a detailed analysis of the ionised gas distribution and kinematics in the inner ∼ 200 pc of NGC 4546, host of a Low Luminosity Active Galactic Nucleus (LLAGN). Using GMOS−IFU observations, with a spectral coverage of 4736−6806 Å and an angular resolution of 0.7 arcsec, we confirm that the nuclear emission is consistent with photoionisation by an AGN, while the gas in the circumnuclear region may be ionised by hot low-mass evolved stars. The gas kinematics in the central region of NGC 4546 presents three components: (i) a disc with major axis oriented along a position angle of 43○ ± 3○, counter rotating relative to the stellar disc; (ii) non-circular motions, evidenced by residual velocities of up to 60 km s−1, likely associated to a previous capture of a dwarf satellite by NGC 4546; and (iii) nuclear outflows in ionised gas, identified as a broad component (σ ∼ 320 km s−1) in the line profiles, with a mass outflow rate of $\dot{M}_{\rm out} = 0.3 \pm 0.1$ M⊙ yr1 and a total mass of Mout = (9.2 ± 0.8) × 103 M⊙ in ionised gas, corresponding to less than 3 per cent of the total mass of ionised gas in the inner 200 pc of NGC 4546. The kinetic efficiency of the outflow is roughly 0.1 per cent, which is smaller than the outflow coupling efficiencies predicted by theoretical studies to AGN feedback become efficient in suppressing star formation in the host galaxy.

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“…Either way, these phenomena, resulting in outflows of matter into the interstellar medium or inflows towards the nuclear region, play a major role in galaxy evolution. Hekatelyne et al (2020) present a hypothesis that OHM galaxies harbour recently triggered AGNs. Similarly, OHM galaxies could also be a transition stage between a starburst and the emergence of an AGN along the sequence of galaxy evolution (Peng et al 2020).…”

Section: Introductionmentioning

confidence: 97%

Radio continuum properties of OH megamaser galaxies

Sotnikova,

Wu,

Mufakharov

et al. 2021

Preprint

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We present a study of the radio continuum properties of two luminous/ultraluminous infrared galaxy samples: the OH megamaser (OHM) sample (74 objects) and the control sample (128 objects) without detected maser emission. We carried out pilot observations for 140 objects with the radio telescope RATAN-600 at 1.2, 2.3, 4.7, 8.2, 11.2, and 22.3 GHz in 2019-2021. The OHM sample has two times more flat-spectrum sources (32 per cent) than the control sample. Steep radio spectra prevail in both samples. The median spectral index at 4.7 GHz α 4.7 = −0.59 for the OHM sample, and α 4.7 = −0.71 for the non-OHM galaxies. We confirm a tight correlation of the far-infrared (FIR) and radio luminosities for the OHM sample. We found correlations between isotropic OH line luminosity L OH and the spectral index α 4.7 (ρ=0.26, p-val.=0.04) and between L OH and radio luminosity P 1.4 (ρ=0.35, p-val.=0.005). Reviewing subsamples of masers powered by active galactic nuclei (AGNs) and star formation revealed insignificant differences for their FIR and radio properties. Nonetheless, AGN-powered galaxies exhibit larger scatter in a range of parameters and their standard deviations. The similarities in the radio and FIR properties in the two samples are presumably caused by the presence of a significant amount of AGN sources in both samples (47 and 30 per cent in the OHM and control samples) and/or possibly by the presence of undetected OH emission sources in the control sample.

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The OH Megamaser galaxy IRAS11506−3851: an AGN and star formation revealed by multiwavelength observations

Cited by 10 publications

References 55 publications

Radio properties of the OH megamaser galaxy IIZw 096

Radio properties of the OH megamaser galaxy IIZw 096

IFU observations of the inner 200 pc of NGC 4546: gas rotation, non-circular motions, and ionized outflows

Radio continuum properties of OH megamaser galaxies

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