The Cavity of 3CR 196.1: H<i>α</i> Emission Spatially Associated with an X-Ray Cavity

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dc.contributor.authorJimenez-Gallardo, A.
dc.contributor.authorSani, E.
dc.contributor.authorRicci, F.
dc.contributor.authorMazzucchelli, C.
dc.contributor.authorBalmaverde, B.
dc.contributor.authorMassaro, F.
dc.contributor.authorCapetti, A.
dc.contributor.authorForman, W. R.
dc.contributor.authorKraft, R. P.
dc.contributor.authorVenturi, G.
dc.contributor.authorGendron-Marsolais, M.
dc.contributor.authorPrieto, M. A.
dc.contributor.authorMarconi, A.
dc.contributor.authorPena-Herazo, H. A.
dc.contributor.authorBaum, S. A.
dc.contributor.authorO'Dea, C. P.
dc.contributor.authorLovisari, L.
dc.contributor.authorGilli, R.
dc.contributor.authorTorresi, E.
dc.contributor.authorPaggi, A.
dc.contributor.authorMissaglia, V.
dc.contributor.authorTremblay, G. R.
dc.contributor.authorWilkes, B. J.
dc.date.accessioned2025-01-20T21:00:54Z
dc.date.available2025-01-20T21:00:54Z
dc.date.issued2022
dc.description.abstractWe present a multifrequency analysis of the radio galaxy 3CR 196.1 (z=0.198), associated with the brightest galaxy of the cool-core cluster CIZAJ0815.4-0303. This nearby radio galaxy shows a hybrid radio morphology and an X-ray cavity, all signatures of a turbulent past activity, potentially due to merger events and active galactic nuclei (AGN) outbursts. We present results of the comparison between Chandra and Very Large Telescope Multi-Unit Spectroscopic Explorer data for the inner region of the galaxy cluster, on a scale of tens of kpc. We discovered H alpha + [N ii]lambda 6584 emission spatially associated with the X-ray cavity (at similar to 10 kpc from the galaxy nucleus) instead of with its rim. This result differs from previous discoveries of ionized gas surrounding X-ray cavities in other radio galaxies harbored in galaxy clusters and could represent the first reported case of ionized gas filling an X-ray cavity, either due to different AGN outbursts or to the cooling of warm (10(4) < T <= 10(7) K) AGN outflows. We also found that the H alpha, [N ii]lambda lambda 6548, 6584, and [S ii]lambda lambda 6718, 6733 emission lines show an additional redward component, at similar to 1000 km s(-1) from rest frame, with no detection in H beta or [O iii]lambda lambda 4960, 5008. We believe the most likely explanation for this redward component is the presence of a background gas cloud as there appears to be a discrete difference of velocities between this component and the rest frame.
dc.fuente.origenWOS
dc.identifier.doi10.3847/1538-4357/aca08b
dc.identifier.eissn1538-4357
dc.identifier.issn0004-637X
dc.identifier.urihttps://doi.org/10.3847/1538-4357/aca08b
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/92769
dc.identifier.wosidWOS:000923121200001
dc.issue.numero2
dc.language.isoen
dc.revistaAstrophysical journal
dc.rightsacceso restringido
dc.titleThe Cavity of 3CR 196.1: H<i>α</i> Emission Spatially Associated with an X-Ray Cavity
dc.typeartículo
dc.volumen941
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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