M87 at 90 Centimeters: A Different Picture

By F. Owen, J. Eilek, N. Kassim. 2000

312 citations recorded by the source corpus.

We report new radio imaging of the large-scale radio structure of M87 with the VLA at 90 cm. These new images show the complex structure of the radio emission more clearly than previous attempts, some of which date back to the 1940s. The images suggest that the outward flow from the M87 nucleus extends well beyond the 2 kpc jet. Two "bubbles" of synchrotron emission appear to be inflated by this flow. A simple model of the emission, combined with our knowledge of the inner jet, suggest that the energy input into this region from the M87 nucleus exceeds the energy being radiated away as X-rays. This argues that the region within 40 kpc of the center of M87 is currently dominated by energy input from the M87 nucleus. The gas in the region is expanding, not flowing inward as is envisioned in the cooling flow model.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/3cda5efb6f0487cff23d09bd8e0e042c04ca21bc

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Citations in the corpus

Heating cooling flows with jets (2003, background): “…inward to take up the volume vacated by ejected gas; (3) gas at all radii is heated by being turbulently mixed with the extremely hot shocked jet material; (4) the radio map of Owen et al. (2000) strongly suggests that, in Virgo, shocked jet material is distributed throughout the inner ∼40 kpc.”
Supermassive black holes in elliptical galaxies: switching from very bright to very dim (2005, background): “In this state the kinetic power of radio emitting outflows can significantly exceed their radiative power both in AGNs and binaries (e.g. Owen et al. 2000; Gallo et al. 2003).”
Reflections of Active Galactic Nucleus Outbursts in the Gaseous Atmosphere of M87 (2003, methodology): “Owen et al. (2000) used the radio observations to derive a minimum value of the instantaneous energy input by the jet of a few ; 1044 ergs s 1.”
High-Frequency VLBI Imaging of the Jet Base of M87 (2007, background): “…scales (0.1 pc to 80 kpc), the jet and radio halo have been intensively observed in the radio between 90 cm and 7mm with theVLA (Biretta et al. 1995;Owen&Biretta 1999;Owen et al. 2000) andwithVLBI (Reid et al. 1982, 1989; Junor&Biretta 1995; Biretta et al. 2002; Ly et al. 2004; Dodson et al. 2006).”
A Review of Bondi-Hoyle-Lyttleton Accretion (2004, background): “However, higher resolution observations by Owen et al. (2000) suggest that this simple picture is not sufficient.”
Dynamics and high-energy emission of the flaring HST-1 knot in the M 87 jet (2006, background): “1 shows the deprojected positions of different knots (starting from HST-1 to C) of the M 87 jet,1 assuming the jet viewing angle to be θ = 20◦ (Bicknell & Begelman 1996; Heinz & Begelman 1997), and the minimum pressure of these knots (a sum of the pressure due to ultrarelativistic radiating electron”
Self-regulated growth of supermassive black holes by a dual jet-heating active galactic nucleus feedback mechanism: methods, tests and implications for cosmological simulations (2011, background): “This mode is clearly associated with mechanical feedback where most of the energy is powered by the jet mechanism and largely overwhelms the X-ray contribution from the nucleus, as in the well-studied case of M87 (Owen et al. 2000).”
Filaments, Bubbles, and Weak Shocks in the Gaseous Atmosphere of M87 (2006, background): “M87 shows a remarkably ‘‘organized’’ and coherent structure in the eastern arm characteristic of a rising buoyant bubble transformed into a torus in both the X-ray and radio images (see Owen et al. 2000 and Churazov et al. 2001) and a second southwestern arm in both radio and X-ray.”
Evolution of Buoyant Bubbles in M87 (2000, background): “The two latter mechanisms were also discussed by Owen et al. (2000) to explain the radio emission of the outer M87 halo.”
Is the Giant Radio Galaxy M 87 a TeV Gamma-Ray Emitter? (2003, background): “The power of the non-thermal jet is estimated to be as high as a few 1044 erg s−1 (Owen et al. 2000a).”