Jets and Lobes In Seyfert Galaxies Beatriz Mingo University of - PowerPoint PPT Presentation

Jets and Lobes In Seyfert Galaxies Beatriz Mingo University of Hertfordshire Supervisors: Martin Hardcastle (Univ. of Hertfordshire) Judith Croston (Univ. of Southampton) Elias Brinks (Univ. of Hertfordshire) The Fermi Bubbles: Theory and Observations Collaborators: KIPAC, 2013 Dan Dicken (IAS), Dan Evans (CFA) Ralph Kraft (CFA), Preeti Kharb (RIT), Ananda Hota (Sinica), Emil Lenc (CSIRO)

Outline ● Small jets and lobes and where to find them ● Diagnostics ● What we see – Mrk 6 – NGC 6764 – Circinus – Other examples ● Consequences ● Caveats and the parallel with the Fermi bubbles ● Conclusions Beatriz Mingo - The Fermi Bubbles - KIPAC 2013

Jets and lobes in small sources ● Why? – RL phase affects environment dramatically: possibly fundamental to understand SF triggering/quenching and AGN feedback ● Where? – Low z for max spatial resolution and S/N ● Low power systems ● Early stage high-power systems (less likely in spirals, but see e.g. Hota et al. 2011) ● How? – X-rays + radio to study extended structure Beatriz Mingo - The Fermi Bubbles - KIPAC 2013

Seyferts and Spirals ● ~30 known Seyferts with extended radio structures (e.g. Hota & Saikia 2006, Gallimore et al. 2006) – Not all Seyferts are spirals! – Few examples of powerful radio galaxies in spirals (Hota et al. 2011, Keel et al. 2006) ● ISM disrupts jet (Ledlow et al. 2001) ● Poorer environments (but see e.g. Best 2004) ● Smaller BH mass (e.g. Sabater et al. 2013) – Jets may not be directly visible but they may still be there... Beatriz Mingo - The Fermi Bubbles - KIPAC 2013

Seyferts and Spirals ● Jets and lobes in Seyferts are typically a few kpc long, radio cores are very weak (e.g. Middelberg 2004) ● Apparent offset between SF and AGN activity – 50-100 Myr in Seyferts, Davies et al. 2007 – ~250 Myr in the general AGN population, Wild et al. 2010 – “Instant” feedback (~1 Myr) between Sgr A* and the CMZ ~6 Myr ago? Zubovas & Nayakshin 2012 Beatriz Mingo - The Fermi Bubbles - KIPAC 2013

Shocks in radio galaxies: Centaurus A ● Original motivation: from min E arguments we know RG lobes have to drive shocks ● Nearest radio galaxy (3.7 Mpc) ● Restarting source (outer structures ~600 kpc in projection) ● X-ray shell around SW inner 1 kpc lobe (Kraft et al. 2003) Beatriz Mingo - The Fermi Bubbles - KIPAC 2013

Centaurus A ● Thermal emission → shock conditions Thermal ● Pressure jump ~10x near the nucleus → M~2.8, V~860 km/s ● Best example of shocks, IC in the lobes – IC is elusive! E.g. in Non-thermal Circinus IC X-ray L is ~100x smaller than the thermal L Beatriz Mingo - The Fermi Bubbles - KIPAC 2013

Bubbles and shocks in small sources ● Jet → ISM E transfer ● Overpressure, T jump – Age ~ 10 6 -10 8 yr → shocks – E ~ 10 56 erg, equiv – M ~ 3-6 to ~10 5 SN Centaurus A (Kraft et al. 2003, ● Energetics (Jet + lobes/bubbles + shock) Croston et al. 2009) ● Timescales ● Feedback, SF triggering/quenching ● Power/mass scaling ● Morphology dependence Beatriz Mingo - The Fermi Bubbles - KIPAC 2013

Markarian 6 Markarian 6 Mingo et al. 2011 ● Mrk 6, IC450 – Early type (S0) – Sy 1.5 – D ~78 Mpc – Outer lobes ~7.5 kpc L(1.4GHz) = 1.7x10 23 W/Hz/sr Beatriz Mingo - The Fermi Bubbles - KIPAC 2013

Markarian 6 ● Rankine-Hugoniot shock conditions (strong)  shell = 4  out – Constraints on external kT, Z, consistent with O'Sullivan et al. (2001, 2003) kT (keV) Ne (cm^-3) P (Pa) Shells (N/S) 0.94 1.62/1.98 x10 -2 4.5/5.5x10 -12 ISM ~0.2 2.2-15x10 -3 1.3x10 -13 Mach number: 3.9 (+1.9 -1.0) Total E (thermal + kinetic): 2.6-4.6x10 56 erg → thermal >> kinetic Timescale: 0.3-1.1x10 7 years → jet power 1-7x10 42 erg/s M(BH): ~3x10 8 M(Sun) (Marconi & Hunt 2003) → P(Bondi) ~1.8x10 41 erg/s (1 keV ~ 1.6 MK) Beatriz Mingo - The Fermi Bubbles - KIPAC 2013

NGC 6764 Croston et al. 2008, Hota & Saikia 2006, ● Barred spiral, Seyfert 2, Kharb et al. 2010 starburst ● D ~32.8 Mpc ● Lobes ~2.6 kpc L(1.4GHz) = 1.12x10 21 W/Hz/sr Beatriz Mingo - The Fermi Bubbles - KIPAC 2013

NGC 6764 ● The X-ray bubbles are 2x more luminous than the starburst wind → jet-driven shock ● V~740 km/s, E~10 56 erg, t~10 6 yr ● Emission is not clearly edge-brightened, perhaps because of very dense ISM Beatriz Mingo - The Fermi Bubbles - KIPAC 2013

The Circinus galaxy HST+Chandra ● D ~4 Mpc 2MASS ● Sy 2 ● L (1.4GHz) =2.2x10 20 W/Hz/sr ● M ~10 11 M Sol ATCA 13cm Beatriz Mingo - The Fermi Bubbles - KIPAC 2013

The Circinus galaxy Mingo et al. 2012 Beatriz Mingo - The Fermi Bubbles - KIPAC 2013

Circinus Beatriz Mingo - The Fermi Bubbles - KIPAC 2013

Circinus  out   1 Shock heating − 1 = 4 Synchrotron  shell M =   S =  2 e B = 5 × 10 8 4  1  T shell / T out − 1  s 2  m e c B 2  2  Photoionization Hotspot AGN Enhanced synchrotron (compression + B amplification) Beatriz Mingo - The Fermi Bubbles - KIPAC 2013

Circinus ● Circinus is shocking – Photoionization, star-driven bubble ruled out – Radio sp. Index changes → hotspots ● Shock is jet-driven ● Power – kT_W=0.74 keV, kT_E=0.8-1.8 keV; kT_ext=0.1-0.2 keV – V~900-950 km/s, M~2.7- 5.3 – E_tot (thermal + kinetic) ~2x10 55 erg – Age of the shells: ~10 6 yr Beatriz Mingo - The Fermi Bubbles - KIPAC 2013

Other sources ● NGC 1068 (Young et. el. 2001) ● M 51 (Terashima & Wilson 2001) – V~690 km/s, E_th~10 54 erg (< E_kin) ● NGC 3079 – Coexistence of jet-driven and star-driven outflows (Cecil et al. 2001, Irwin & Saikia 2001 ) ● See also Hota & Saikia 2006 Beatriz Mingo - The Fermi Bubbles - KIPAC 2013

Power scaling System Type L 1.4 GHz W/Hz/sr E_tot (erg) 1.5x10 23 10 57 Cen A E 1.2x10 23 2x10 56 NGC 3801 E M 51 Sb 1.5x10 21 >10 54 1.7x10 23 3-5x10 56 Mrk 6 S0 1.1x10 21 10 56 NGC 6764 Sb 2.2x10 20 2x10 55 Circinus Sb That is 10 4 -10 6 SN explosions! (assuming 10 51 erg SN) → environment must be affected e.g. in NGC 3801 this E corresponds to the total thermal E in the ISM within 11 kpc, and 25% of the E within 30 kpc (Croston et al. 2007) Beatriz Mingo - The Fermi Bubbles - KIPAC 2013

Caveats ● Small structures hard to resolve at large distances → statistics limited ● ~50% of Sy 2 have a nuclear starburst (Hota & Saikia 2006) → complicated to disentangle! ● No way to detect IC gamma-rays in these systems (not enough spatial resolution) ● Abundance is often poorly constrained (from X- ray spectra) ● Equipartition? Beatriz Mingo - The Fermi Bubbles - KIPAC 2013

Consequences for the Fermi bubbles ● Power scaling works → can help determine constraints on E, timescales, feedback ● Unlikely that similar structures can be detected in other galaxies in X-rays or gamma rays → radio may be the way to go, but also limited by spatial resolution ● Timing is crucial, but if we understand merger- SF-AGN-SF timescales we can constrain values for structures that are no longer detectable Beatriz Mingo - The Fermi Bubbles - KIPAC 2013

Conclusions ● Shocks and bubbles are common in Seyferts (so are starbursts, however!) ● E transfer is substantial and likely to affect the evolution of the host galaxy ● Direct detection of other Fermi bubbles is unlikely, but what we learn from other systems can be extrapolated due to power scaling ● We need more data and better telescopes :) Beatriz Mingo - The Fermi Bubbles - KIPAC 2013