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

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

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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

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Beatriz Mingo

University of Hertfordshire Supervisors: Martin Hardcastle (Univ. of Hertfordshire) Judith Croston (Univ. of Southampton) Elias Brinks (Univ. of Hertfordshire) Collaborators: Dan Dicken (IAS), Dan Evans (CFA) Ralph Kraft (CFA), Preeti Kharb (RIT), Ananda Hota (Sinica), Emil Lenc (CSIRO)

Jets and Lobes In Seyfert Galaxies

The Fermi Bubbles: Theory and Observations KIPAC, 2013

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Beatriz Mingo - The Fermi Bubbles - KIPAC 2013

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
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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

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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...

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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

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Beatriz Mingo - The Fermi Bubbles - KIPAC 2013

Shocks in radio galaxies: Centaurus A

1 kpc

  • 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

lobe (Kraft et al. 2003)

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Beatriz Mingo - The Fermi Bubbles - KIPAC 2013

Centaurus A

  • Thermal emission →

shock conditions

  • 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

Circinus IC X-ray L is ~100x smaller than the thermal L

Thermal Non-thermal

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Beatriz Mingo - The Fermi Bubbles - KIPAC 2013

Bubbles and shocks in small sources

  • Jet → ISM E transfer

– Age ~ 106-108 yr – E ~ 1056 erg, equiv

to ~105 SN

  • Energetics (Jet + lobes/bubbles + shock)
  • Timescales
  • Feedback, SF triggering/quenching
  • Power/mass scaling
  • Morphology dependence
  • Overpressure, T jump

→ shocks

– M ~ 3-6

Centaurus A (Kraft et al. 2003, Croston et al. 2009)

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Beatriz Mingo - The Fermi Bubbles - KIPAC 2013

Markarian 6 Markarian 6

  • Mrk 6, IC450

– Early type (S0) – Sy 1.5 – D ~78 Mpc – Outer lobes ~7.5 kpc

L(1.4GHz) = 1.7x1023 W/Hz/sr Mingo et al. 2011

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Beatriz Mingo - The Fermi Bubbles - KIPAC 2013

Markarian 6

  • Rankine-Hugoniot shock conditions (strong)

– Constraints on external kT, Z, consistent with

O'Sullivan et al. (2001, 2003)

 shell  out =4

Ne (cm^-3) P (Pa) Shells (N/S) 0.94 ISM ~0.2 kT (keV) 1.62/1.98 x10-2 4.5/5.5x10-12 2.2-15x10-3 1.3x10-13

Mach number: 3.9 (+1.9 -1.0) Total E (thermal + kinetic): 2.6-4.6x1056 erg → thermal >> kinetic Timescale: 0.3-1.1x107 years → jet power 1-7x1042 erg/s M(BH): ~3x108 M(Sun) (Marconi & Hunt 2003) → P(Bondi) ~1.8x1041 erg/s

(1 keV ~ 1.6 MK)

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Beatriz Mingo - The Fermi Bubbles - KIPAC 2013

NGC 6764

  • Barred spiral, Seyfert 2,

starburst

  • D ~32.8 Mpc
  • Lobes ~2.6 kpc

L(1.4GHz) = 1.12x1021 W/Hz/sr Croston et al. 2008, Hota & Saikia 2006, Kharb et al. 2010

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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~1056 erg,

t~106 yr

  • Emission is not clearly

edge-brightened, perhaps because of very dense ISM

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Beatriz Mingo - The Fermi Bubbles - KIPAC 2013

The Circinus galaxy

HST+Chandra 2MASS ATCA 13cm

  • D ~4 Mpc
  • Sy 2
  • L(1.4GHz) =2.2x1020

W/Hz/sr

  • M ~1011 MSol
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Beatriz Mingo - The Fermi Bubbles - KIPAC 2013

The Circinus galaxy

Mingo et al. 2012

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Beatriz Mingo - The Fermi Bubbles - KIPAC 2013

Circinus

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Beatriz Mingo - The Fermi Bubbles - KIPAC 2013

Circinus

AGN Photoionization

Shock heating

Hotspot Synchrotron

S= 2e B 2me c =5×108 B2 s M = 41T shell /T out−1 2 out shell  1 −1=4

Enhanced synchrotron (compression + B amplification)

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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) ~2x1055 erg – Age of the shells: ~106 yr

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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~1054 erg (< E_kin)

  • NGC 3079

– Coexistence of jet-driven and star-driven

  • utflows (Cecil et al. 2001, Irwin & Saikia 2001

)

  • See also Hota & Saikia 2006
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Beatriz Mingo - The Fermi Bubbles - KIPAC 2013

Power scaling

System Type E_tot (erg) E NGC 3801 E M 51 Sb S0 NGC 6764 Sb Sb L 1.4 GHz W/Hz/sr Cen A 1.5x1023 1057 1.2x1023 2x1056 1.5x1021 >1054 Mrk 6 1.7x1023 3-5x1056 1.1x1021 1056 Circinus 2.2x1020 2x1055

That is 104-106 SN explosions! (assuming 1051 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)

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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?
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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

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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 :)