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Exploring the formation epoch of massive galaxies

Exploring the formation epoch of massive galaxies. Michele Cirasuolo. Institute for Astronomy, University of Edinburgh. Ross J. McLure, James S. Dunlop. O.Almaini, S. Foucaud, C. Simpson, I. Smail, K. Sekiguchi, M. Watson, M. Page, P. Hirst. Hopkins 2006.

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Exploring the formation epoch of massive galaxies

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  1. Exploring the formation epoch of massive galaxies Michele Cirasuolo Institute for Astronomy, University of Edinburgh Ross J. McLure, James S. Dunlop O.Almaini, S. Foucaud, C. Simpson, I. Smail, K. Sekiguchi, M. Watson, M. Page, P. Hirst

  2. Hopkins 2006 Delineating cosmic star-formation history 1) Direct observation of star-formation activity with z

  3. Delineating cosmic star-formation history 1) Direct observation of star-formation activity with z 2) From the fossil record (e.g. Heavens et al. 2004)

  4. Delineating cosmic star-formation history 1) Direct observation of star-formation activity with z 2) From the fossil record (e.g. Heavens et al. 2004) 3) By measuring stellar mass in place as a function of z • Needs • deep near-mid infrared surveys • with • multi-frequency supporting data

  5. UKIRT Infra-red Deep Sky Survey Deep IR surveys e.g. K20, FIRES, MUNICS, GDDS, K21, GMASS, GOODS...

  6. UDS FIRES UKIDSS Ultra Deep Survey Courtesy of Omar Almaini

  7. UKIDSS Ultra Deep Survey

  8. GALEX FUV,NUV SUBARU B,V,R,I,z CFHT u,g,r,i,z UKIRTJ, KSpitzer IRAC3.6, 4.5 μm 16 wavebands photometry available UKIDSS Ultra Deep SurveyCirasuolo et al. 2006, 2007 K(AB) = K(Vega) +1.9 ~50,000 IR-selected galaxies with K(AB) < 23 over an area of 0.7 sq. deg • And by the beginning of next year: • H band data UKIRT • Deeper u-band from CFHT • 300h with Spitzer IRAC and MIPS 24μm • 290h VLT time with VIMOS and FORS

  9.  = 0.036 Quality of the dataset ~1200 galaxies with good quality spectra <3% of outliers

  10. Schechter function with Luminosity evolution + Density evolution Local K-band LF from 2MASS Evolution of the near-IR galaxy LF 50,000 galaxies with K(AB)  23.0 0.5<z<1.0 1.0<z<1.5 1.5<z<2.0 2.5<z<3.0 2.0<z<2.5 3.0<z<4.0 MK (AB)

  11. Evolution of the near-IR galaxy LF Comparison with some results in literature Saracco et al. 2006 Caputi et al. 2006 Pozzetti et al. 2003 0.5<z<1.0 1.0<z<1.5 1.5<z<2.0 2.5<z<3.0 2.0<z<2.5 3.0<z<4.0 MK (AB)

  12. Evolution of the near-IR galaxy LF Comparison with semi-analytical models De Lucia 2006 Bower 2006 0.5<z<1.0 1.0<z<1.5 1.5<z<2.0 2.5<z<3.0 2.0<z<2.5 3.0<z<4.0 MK (AB)

  13. Early type Late type Baldry et al. 2004 Bell et al. 2004 Combo-17 R < 24 The colour bimodality Well studied in the local Universe Visvanathan & Sandage 1977; Bower et al. 1992; Starteva et al. 2001; Baldry et al. 2004 Extended up to z  1 Bell et al. 2004; Willmer et al. 2005; Franzetti et al. 2006

  14. Reddening Star formation The evolution of colour bimodality Primary selection in K-band  No bias against red objects Confirm the luminosity dependent colour bimodality at z<1 Strength decreases with redshift and seems to disappears by z>1.5

  15. LF by colour type

  16. The most massive galaxies

  17. The most massive galaxies Local space density 15 – 20 % of local massive galaxies in place before z~3 MCDM > 2 x 1012 M8 GOODS (Caputi et al. 2006) The assembling of 80% of massive galaxies occurs in the range 1 < z < 3 MCDM > 5 1012 M8 M* > 1011 M 

  18. S850 > 6 mJy S850 < 6 mJy The obscured growth Central 400 arcmin2 of the UDS observed by SCUBA as part of SHADES Survey Secure ID from radio map at 1.4GHz (Ivison et at. 2007)

  19. The very high-z Universe Mstars > 5 x 1010 M8 McLure, Cirasuolo, Dunlop et al., 2006, MNRAS

  20. MF at z=0 (Cole 2001) Trieste model (Granato 2004) Durham model (Bower 2006) Comparison with models Uncertainties on IMF, 8 McLure, Cirasuolo, Dunlop et al., 2006, MNRAS

  21. Preliminary results at z~6 McLure, Cirasuolo, Dunlop et al., in prep.

  22. In the near future: • 300h Spitzer MIPS and IRAC • VLT spectra with both VIMOS & FORS Better determination of masses star-formation, environment Search for high-z galaxies. … and a bit later: • SCUBA2, Hershel, VISTA, LOFAR, ALMA etc. • and hopefully SPACE (see M. Robberto’s poster) Conclusions and future prospects • Strong evolution of the LF with a brightening of ~1 mag between z=0 and z~4 • Nearly 80% of massive galaxies are already in place at z>1 • At low-z the massive systems are red and passive evolving • At z  1 star-formation in most of massive galaxies • Down-sizing mass assembly of sub-mm galaxies

  23. R=25.1 R=24.1 Bundy et al. 2006

  24. VVDS

  25. Stern et al. 2006

  26.  = 0.036 Quality of the dataset ~1200 galaxies with good quality spectra <3% of outliers

  27. Less affected by dust extinction Why Deep IR surveys ? Better tracer of the mass in stars LV LK

  28. S850 > 6 mJy S850 < 6 mJy Masses of Sub-mm galaxies Central 400 arcmin2 of UDS observed by SCUBA ID from radio map at 1.4GHz (Ivison et at. 2007)

  29. Local space density 15 – 20 % of local massive galaxies in place before z~3 The assembling of 80% of massive galaxies occurs in the range 1 < z < 3 Space density MCDM > 2 x 1012 M8 MCDM > 1013 M8

  30. Goods UDS Burst model

  31. Bundy et al. 2006

  32. Mass function

  33. Spectr. data from Simpson; Akiyama; Smail

  34. Age = 7Gyr Age = 1Gyr with ~ 10% of the mass

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