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Qusar feedback revealed by giant molecular outflows

Qusar feedback revealed by giant molecular outflows. arXiv:1006.1655 Feruglio et al. The Star–Gas–Star Cycle. 3) They return much of their content into interstellar medium through stellar winds and when they explode…. 1) Stars are born in molecular clouds ….

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Qusar feedback revealed by giant molecular outflows

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  1. Qusar feedback revealed by giant molecular outflows arXiv:1006.1655 Feruglio et al.

  2. The Star–Gas–Star Cycle 3) They return much of their content into interstellar medium through stellar winds and when they explode… 1) Stars are born in molecular clouds… 2) They shine and produce heavier elements in nuclear fusion…

  3. 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.

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

  5. 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

  6. Mrk 231: The ultraluminous infrared galaxy • Distance~170 Mpc or z=0.042 • A powerful AGN is hosted in the galaxy Canalizo et al. ApJ, 2000 Davies et al. ApJ, 2004

  7. 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

  8. 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

  9. arXiv:1006.1655 • IRAM PdBI: 5*15m • Band width~1GHz The starbursting disk is nearly face-on Narrow core component: FWHM~180km/s Broad component: FWHM~870km/s, FWZI~1500km/s

  10. arXiv:1006.1655 Mrk 231 1’’~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 yr dE(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 Lapi et al. ApJ, 2005

  11. Have a good dinner!

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