Qusar feedback revealed by giant molecular outflows

arXiv:1006.1655arXiv:1006.1655

Feruglio et al.Feruglio et al.

The Star–Gas–Star Cycle

1) Stars are born in molecular

clouds…

3) They return much of their content into interstellar medium through stellar winds and when they explode…

2) They shine and produce heavier elements in nuclear fusion…

It is not easy to stop the gas from exploding stars: after supernova explosion, ionized gas flies out at speeds of several thousands kilometers – much faster than the escape velocity from the galaxy.

Multiple supernovae create huge hot bubbles that can blow out of disk.

Gas clouds cooling in the halo can rain back down on disk.

The matter in our Galaxy emits different kinds of radiation, depending on what stage of the star–gas–star cycle it is in.

Mrk 231 is classified as a low

ionization BAL quasar (weak [OIII])

• A Central compact radio core• Pc-scale jets

Ulvestad et al. ApJ, 1999

• Mrk 231: The ultraluminous infrared galaxy

• Distance~170 Mpc or z=0.042

• A powerful AGN is hosted in the galaxyCanalizo et al. ApJ, 2000Davies et al. ApJ, 2004

BeppoSAX and XMM-Newton :

N(H)~2E24 cm-2

L(2-10 keV)~1E44 erg/s ~1/100 L(IR=1E46 erg/s)

0.5—2 keV 4.5—10 keV

Braito et al. 2004 A&A

Herschel PACS:

The molecular outflow:

ISM processing by

advanced starbursts.

The massive molecular

outflow shows velocities

out to at least 1400 km/s.

Fischer et al. A&A, 2010

• IRAM PdBI: 5*15m

• Band width~1GHzThe starbursting disk is nearly face-on

Narrow core component: FWHM~180km/s

Broad component: FWHM~870km/s, FWZI~1500km/s

arXiv:1006.1655arXiv:1006.1655

Mrk 2311’’~0.9kpc@186 Mpc, M(gas)~1E10 Msun, M(BH)~6E8 Msun,M(outflow)~5.8E8 Msun, n(0.6 kpc)~25 cm-3, v~700 km/s, dM(outflow)/dt~2E3 Msun/yr > dM(SF)/dt~2E2 Msun/yr To quench star formation in the regions of 1 kpc The SF ceases and the starburst fades in t<1E7 yrdE(outflow)/dt~4E44 erg/s~6% L(Eddington)

E(injected)~6E57 erg ~1E4 E(SNe) A highly supersonic shock transports outwards the energy accumulated

in the centre by radiatively accelerated nuclear winds

arXiv:1006.1655arXiv:1006.1655

Lapi et al. ApJ, 2005Lapi et al. ApJ, 2005

Have a good dinner!