Can the cosmic-ray driven dynamo model explain the observations of the polarized emission of edge-on galaxies ? [PDF]
, 2008 In the present paper we construct maps of polarized synchrotron radio emission of a whole galaxy, based on local models of the cosmic ray (CR) driven dynamo.
Barbara Kulesza-Żydzik +25 more
core +2 more sources
A CO Funnel in the Galactic Centre: Molecular Counterpart of the Northern Galactic Chimney?
, 2023 We report the discovery of a velocity coherent, funnel shaped ^13CO emission feature in the Galactic centre (GC) using data from the SEDIGISM survey. The molecular cloud appears as a low velocity structure (V_LSR=[-3.5, +3.5] km/s) with an angular extent
Banda-Barragan, W. E. +9 more
core +1 more source
Radio Galaxy NGC 1265 unveils the Accretion Shock onto the Perseus Galaxy Cluster
, 2011 We present a consistent 3D model for the head-tail radio galaxy NGC 1265 that explains the complex radio morphology and spectrum by a past passage of the galaxy and radio bubble through a shock wave. Using analytical solutions to the full Riemann problem
Battaglia +25 more
core +1 more source
CHANG-ES XXXIV: Magnetic Field Structure in Edge-On Galaxies Characterising large-scale magnetic fields in galactic halos [PDF]
A&A 696, A112 (2025)Understanding galactic magnetic fields is essential for interpreting feedback processes in galaxies. Despite their importance, the exact structure of these fields, particularly in galactic halos, remains unclear. Accurate descriptions are crucial for understanding the interaction between star formation and halo magnetisation.
arxiv +1 more source
Galactic and Extragalactic Magnetic Fields
, 2009 The strength of the total magnetic field in our Milky Way from radio Zeeman and synchrotron measurements is about 6 muG near the Sun and several mG in dense clouds, pulsar wind nebulae, and filaments near the Galactic Center.
Felix A. Aharonian +3 more
core +1 more source
The peculiar radio galaxy 3C 433
, 1983 Radio, optical, and x-ray observations are presented of the peculiar radio galaxy 3C 433. Two basic features characterize the radio morphology: namely, a striking asymmetry in the strength and shape of the radio emission and an overall x-shaped structure.
W. Breugel +4 more
semanticscholar +1 more source
, 2017 We use a phenomenological model to show that black hole growth in the local Universe (z < 0.1) can be described by two separate, mass independent Eddington ratio distribution functions (ERDFs).
Caplar, Neven +5 more
core +1 more source
GMRT study of X-shaped radio sources [PDF]
arXiv, 2008 Context. The nature of X-shaped sources is a matter of considerable debate in the literature: it has even been proposed that they provide evidence for black-hole-mergers/spin-reorientation, and therefore constrain the rate of strong gravitational wave events. Aim. To explore the nature of these X-shaped radio galaxies. Method.
arxiv
The Hot Atmospheres of X-shaped Radio Galaxies [PDF]
, 2011 We present an observational and numerical study of X-shaped radio galaxies, a subset of the double-lobed radio galaxies with a second set of lobes or "wings".
Hodges-Kluck, Edmund
core
Cosmic ray feedback in galaxies and galaxy clusters: A pedagogical introduction and a topical review of the acceleration, transport, observables, and dynamical impact of cosmic rays. [PDF]
Astron Astrophys Rev, 2023 Ruszkowski M, Pfrommer C.
europepmc +1 more source