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Galaxy feedback in 3D

Galaxy feedback in 3D. Roberto Maiolino. Discrepancy between halo mass functions and stellar/baryons mass function. Feedback is the key: - reducing SF efficiency (gas heating+turbulence ) - removing baryons. SNe Radiation pressure Photoionization. Star formation feedback.

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Galaxy feedback in 3D

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  1. Galaxy feedback in 3D Roberto Maiolino

  2. Discrepancy between halo mass functions and stellar/baryons mass function Feedback is the key: - reducing SF efficiency (gas heating+turbulence) - removing baryons

  3. SNe Radiation pressure Photoionization Star formation feedback Turbulence Velocity dispersion (Q>1) Blast wave Radiation pressure Quasar mode Radio mode AGN feedback

  4. Star formation feedback SNe & radiation pressure driven outflows

  5. The importance of tracing outflows in multiple phases NGC 253 Herschel PACS PAH (Spitzer) M82 NIR Ha X-rays (Chandra) CO~170 km/s (ALMA) X-rays Bolatto+13 turbulent outflow [CII]158um (Herschel) galaxy rotation velocity field velocity dispersion . Mout ~ 1-2 SFR Contursi+13, Kreckel+14

  6. Investigating outflows as a function of M* and SFR(breaking the M*-SFR degernarcy) 160,000 SDSS galaxies sorted into 50 bins in the M*- SFR parameter space Main Sequence Cicone+14 Lowest M* ≈ 2 x 107 M Lowest SFR ≈ 2 x 10-3 Myr-1

  7. THE LINE-OF-SIGHT VELOCITY DISTRIBUTIONS [OIII] Trends with M* at a fixed SFR Hα+[NII] STARS v [km/s] Cicone+14

  8. THE LINE-OF-SIGHT VELOCITY DISTRIBUTIONS [OIII] Trends with SFR at a fixed M* Hα+[NII] STARS v [km/s]

  9. OUTFLOW PROPERTIES Stacking grid colour-coded with the excess of gas velocity with respect to stars which traces non-virial motion of gas (due to outflows) [OIII] • vGAS – vSTARincreases with SFR and sSFR • Expected for star formation-driven outflows • vGAS– vSTARdecreases with M* for fixed SFR • Qualitatively agrees with models • Agreement with indirect observations of feedback (e.g. mass-metallicity relation) v[OIII] - vSTARS Hα vHα- vSTARS

  10. OUTFLOW PROPERTIES Cicone+14 Outflows are detected only above the main sequence of star formation v[OIII] - vSTARS • Sharp increase of outflows at • SFR > SFRMS • Outflows eventually quench star formation and lower the SFR, bringing the galaxy back on the MS • Self-adjusting mechanism that may explain the tightness of the MS v[OIII] – vSTARS[km/s] ΔMS = offset from the Main Sequence

  11. Next steps:- 3D on large samples of galaxies required to obtain outflow rate and PK  SDSS4-MANGA- Investigate the Atomic (NaI) and Molecular componentsin 3D v[OIII] - vSTARS • Sharp increase of outflows at • SFR > SFRMS • Outflows eventually quench star formation and lower the SFR, bringing the galaxy back on the MS • Self-adjusting mechanism that may explain the tightness of the MS v[OIII] – vSTARS[km/s] ΔMS = offset from the Main Sequence

  12. Star formation feedback at high redshift

  13. 3D resolved Integrated z~2 z~3 Steidel+10 Bradshaw+13 Diamond-Stanic+12 Genzel+12 . M ~ 1-2 Outflow load factor SFR

  14. Feedback in the early Universe The need of feedback becomes dramatic at high-z Photoionization the main driver? Need to trace both ionized and neutral ISM at high-z e.g.[CII], [CI], CO e.g. Lya,Ha

  15. Williams+14 Lya emitter at z=4.7 SFR ~ 20 M/yr Lya(FORS2) SMG [CII]158mm (ALMA) Lya QSO Neutral-cold gas ([CII]) probably account just for a small fraction of the whole galaxy traced by Lya But peculiar environment (QSO)…

  16. Vanzella+12 Star forming galaxy at z=7.1 (reionization epoch) SFR ~ 9 M/yr Y-band (Lya+UV)

  17. [CII]158mm (~neutral cold gas) detected at z=7.1 with ALMA 5 kpc beam 0.5”x0.7” Maiolino+14 Star forming galaxy at z=7.1 (reionization epoch) SFR ~ 9 M/yr Y-band (Lya+UV)

  18. FWHM 8 km/s! [CII] (ALMA) 5 kpc beam 0.5”x0.7” Star forming galaxy at z=7.1 (reionization epoch) SFR ~ 9 M/yr

  19. FWHM 8 km/s! [CII] (ALMA) 5 kpc beam 0.5”x0.7” vel. dispersion velocity km/s km/s Mdyn ~ 3 107M

  20. FWHM 8 km/s! [CII] (ALMA) 5 kpc 3kpc [CII] Lya+UV offset ~3 kpc beam

  21. galaxy mostly photoionized + accreting clumps of cold gas …as expected by models of primeval galaxies Vallini+13

  22. AGN feedback “Quasar mode”

  23. Quasar-driven outflows detected in the atomic neutral and ionized component Mrk231 Mrk231 Narrow Ha [NII] [NII] 1200 km/s Fl (normalized) NaI Broad Ha (outflow) 6100 lambda 6160 Wavelength (Å) 2kpc velocity [km/s] velocity [km/s] Rupke+11,13, Spoon+11, Muller-Sanchez+11

  24. Evidence for massive quasar-driven molecular outflows OH P-Cygni profiles CO(1-0) high velocity wings 1200 km/s Mrk231 l (mm) Fischer+10 Sturm+11 Feruglio+10,13 Cicone+14 blue wing 5kpc Massive molecular outflows (~1000 M/yr) Extended on kpc scales PK ~ 0.05 LAGN Momentum rate ~ 20 LAGN/c …as expected (and required) by models

  25. CO(1-0) Mrk231 The importance of high resolution 3D spectroscopy 600 – 800 km/s Recurrent explosive process Energy driven quasar outflows 1kpc 600 – 800 km/s 1kpc 800 – 1000 km/s CO(1-0) IRAM - PdBI CO(2-1) Feruglio+, in prep.

  26. Simulations: only diffuse gas is ejected, no dense gas … AGN not really capable of quenching star formation? Gabor+14 Actually a lot of dense (~105 cm-3) gas is observed in the outflow… Aalto+12 …actually there is more dense gas in the outflow (relative to diffuse) than in the disk!

  27. Alternative scenario: molecular outflowing clouds condensed out of the shocked ouflowinggas… … would be consistent with AGN only ejecting diffuse gas and the detection of dense outflowing gas… but 3D info: Zubovas & King ‘13 Cicone+12 outflow size [kpc] log (critical density) [cm-3] Expected Observed n n

  28. AGN feedback at high-z (that’s what is really needed to account for local massive ellipticals)

  29. Ha (SFR) z=2.4 z=3.0 Bourget +2012, 2013 V[OIII] >300km/s (outflow) z=6.4 Sizes >10 kpc . Cano Diaz+12 Moutflowup to >3000 M/yr [CII] Depletion timescales < 107 yr z=3 Maiolino+12, Cicone+14 Forster-Schreiber+13 Cimatti et al. 13 Weiss+13 Alexander+10

  30. “Quasar mode” Cleaning the galaxy Keeping the galaxy clean “Radio mode”

  31. Evidence for radio-mode AGN feedback in LOCAL galaxies (maintenance mode) radio Heating ~ Cooling It works! … Really? optical + radio

  32. Having, ON AVERAGE, balance between heating and cooling does not mean that some regions cannot undergo overheating and other OVERCOOLING Streams of cooling molecular gas towards the center of Perseus Salome’+11 Russel+14 Hamer+14

  33. “Quasar-feedback” phase driven by jets? Wagner & Bicknell 2011, 2012

  34. SCIENCE (today) see also Morganti+03,05, Emonts+03 blueshifted 21cm absorption 4C12.50

  35. ALMA CO(1-0)

  36. Observational evidence and characterization of feedback in galaxies: green field lots of open questions rapid growth expected in the coming few years thanks to the new 3D facilities

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