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Quenched and Quenching Galaxies at Low to High Redshifts

Quenched and Quenching Galaxies at Low to High Redshifts. S .M. Faber & UCSC and CANDELS collaborators Dekel60 Fest December 13 , 2011. M31: UV GALEX. Quenching Scenarios for Central Galaxies. Halo-based  Massive halo quenching: “cold flows” to hot

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Quenched and Quenching Galaxies at Low to High Redshifts

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  1. Quenched and Quenching Galaxies at Low to High Redshifts S.M. Faber & UCSC and CANDELS collaborators Dekel60 Fest December13, 2011 M31: UV GALEX

  2. Quenching Scenarios for Central Galaxies • Halo-based •  Massive halo quenching: “cold flows” to hot • halos + AGN (“radio mode”) • Bulge-building • Major merger -> starburst + AGN • Minor mergers + AGN • Disk instability + AGN • Disk secular evolution + AGN • Morphological quenching (Toomre Q) • Hopping/rejuvenation • Mergers • Stochastic accretion Correlate with halo properties Correlate with galaxy properties

  3. Part I: Quenching of central SDSS galaxies at z ~ 0 with halo mass vs. stellar mass  Joanna Woo & AvishaiDekel Joanna

  4. Probability of quenching vs. M* and Mhalo Contours run vertically. Quenching correlates better with halo mass than with stellar mass. Wooet al. 2011

  5. Part II: HST UV images of nearby Green Valley galaxies  Jerome Fang, SamirSalim, S. M. Faber, et al. Jerome

  6. HST UV images of SDSS green valley galaxies • 20 galaxies imaged with HST SBC. •  Sample lies in bluer part of green valley. Fang, Salim et al. 2011

  7. HST FUV images Fang, Salim et al. 2011

  8. HST sample vs. general green valley Many more GV galaxies with similar properties. Fang, Salim et al. 2011

  9. Colors imply underlying substrate of older stars ESFETGs Mass-matched in blue cloud Fang, Salim et al. 2011 Fang, Salim et al. 2011

  10. HST FUV images Fang, Salim et al. 2011

  11. GALEX: M31

  12. Part III: Structure of AEGIS galaxies on Red Sequence vs. Blue Cloud at z ~ 0.8  Edmond Cheung, Liz McGrath, & David Koo Edmond

  13. Try different combinations of mass and radius Cheung et al. 2011 Mass M/reff M/reff2 DEEP2 survey: spec z’s and photoz’s. Redshift range z = 0.5-0.8.

  14. None work perfectly. There is always overlap region. Surface density Kauffmann+06 Cheung et al. 2011 Mass M/reff M/reff2 DEEP2 survey: spec z’s and photoz’s. Redshift range z = 0.5-0.8.

  15. Is there a second structural variable? Cheung et al. 2011 Cheung et al. 2011 DEEP2 survey: spec z’s and photoz’s. Redshift range z = 0.5-0.8.

  16. AEGIS galaxies have bulge-disk decompositions using GIM2D. In the overlap region, the color change is accompanied by structural changes. Stellar mass becomes more concentrated. Bulge M* is higher U-B Bulge radius is smaller U-B Bulge M*/re is lower U-B Cheung et al. 2011

  17. Sersic index: looks like a threshold, except for outliers See also Bell+08, Bell+11 outliers Cheung et al. 2011

  18. Inner mass surface density increases across color divide • Rejuvenation model no good; one way trip •  Structure is better predictor of quenching than halo or stellar mass McGrath, Koo et al. 2011

  19. Part IV: Pre- and post-quenched galaxies in CANDELS at z ~ 2  Mark Mozena, Tao Wang, JS Huang, and CANDELS team Mark

  20. Color-mass diagram: CANDELS/ERS in GOODS-S Visual classes: Z = 1.5-2.5 ✖ Spheroid ✖ Mixed or Irr ✖ Disk Note color-mass relation already at z~2! Mozena et al. 2011

  21. Massive galaxies > 1010.8Mat z~2 in Gini/M20 WFC3-IR images from CANDELS and ERS in GOODS-S • Half quenched, half star-forming. • Strong correlation with morphology. • These SFR galaxies will all be quenched by z~1. Quiescent Star-forming Wang et al. 2011

  22. Radius-mass diagram: GOODS-S Also Cirasuolo et al. 2011 Visual classes: ✖ Spheroid Z = 1.5-2.5 ✖ Mixed or Irr ✖ Disk Mozena et al. 2011

  23. Radius-mass diagram: GOODS-S Also Cirasuolo et al. 2011 Visual classes: ✖ Spheroid Z = 1.5-2.5 ✖ Mixed or Irr ✖ Disk Almost bimodal! Mozena et al. 2011

  24. Radius-mass diagram: GOODS-S Also Cirasuolo et al. 2011 Visual classes: ✖ Spheroid Z = 1.5-2.5 ✖ Mixed or Irr ✖ Disk X5 Mozena et al. 2011

  25. Conclusions: There exist structural parameters that are better predictors of quenching than either halo or stellar mass. An indispensible ingredient in the quenching processat all redshiftsis either caused by (or leaves its imprint on) the stellar mass distribution – stars move to center. At low z, this process does not involve major mergers or a large change in radius. At high z, gross shrinkage in radius of x5 occurs. Is the process the same or different at high z?

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