The properties of FR0 radio galaxies as intermediate objects in the evolution of radio galaxies
| Autor: | Garofalo, David, Singh, Chandra B., Harmon, Eddie, Williams, Michael, Castillo, Luis Rojas |
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| Rok vydání: | 2024 |
| Předmět: | |
| Druh dokumentu: | Working Paper |
| Popis: | The counter-rotation between black holes and accretion disk configuration was introduced over a decade ago to elucidate the nature of the radio loud/radio-quiet dichotomy and the jet-disk connection, but has since been applied to a plethora of observations across space and time. We briefly review the paradigm in which counter-rotation is key for the triggering of radio galaxies and its observational support, then apply it to a series of observations concerning FR0 radio galaxies. FR0 radio galaxies appear to be radio galaxies in transition, with low-spinning black holes and thus weaker but tilted jets with respect to an earlier radio quasar phase. As a result, FR0 radio galaxies are prescribed to be in an earlier phase of star formation suppression in radio galaxies, compared to a later phase that is unlikely to be less than tens of millions of years in the future if they have enough accretion fuel to evolve into more powerful FRI radio galaxies. FR0 radio galaxies will have a greater or lesser star formation suppression feedback effect depending on how long they live. Tilted jets also enhance stellar velocities in the bulge. Because FR0 jet lengths are of the same order of magnitude as the radius of the stellar bulge, FR0 jets are prescribed to have begun, more or less recently depending on their age, to affect stellar velocity dispersions as well. As a result, they will be associated with dispersion values that tend to be larger than for characteristically non-jetted active galaxies, but smaller than giant radio galaxies such as M87 that have experienced a long-term tilted and more powerful FRI jet. With these ideas it is possible to make a coarse-grained prediction for the slope of the M-{\sigma} plane for FR0 radio galaxies with values between 4 and 8. Comment: 13 pages, 4 Figures, Accepted for publication in the Journal of High Energy Astrophysics |
| Databáze: | arXiv |
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