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The GOOD NICMOS Survey (GNS): Observing Massive Galaxies at z > 2

The GOOD NICMOS Survey (GNS): Observing Massive Galaxies at z > 2. Christopher J. Conselice (University of Nottingham) with Asa Bluck, Ruth Gruethbacher, Amanda Bauer, Fernando Buitrago (Nottingham) + others.

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The GOOD NICMOS Survey (GNS): Observing Massive Galaxies at z > 2

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  1. The GOOD NICMOS Survey (GNS): Observing Massive Galaxies at z > 2 Christopher J. Conselice (University of Nottingham) with Asa Bluck, Ruth Gruethbacher, Amanda Bauer, Fernando Buitrago (Nottingham) + others

  2. Motivation: Nearly all massive galaxies are formed by z~1 - 1.5 Results from Palomar Observatory Wide-Field Infrared Survey (POWIR) +DEEP2 Redshifts (Conselice et al. 2007) Cole et al. (2001) z~0 comparison Massive galaxies must form at > 1.5

  3. Also, there are too many massive galaxies in comparison to models Millennium simulation Prediction for 11 < log M < 11.5 Prediction for log M > 11.5 Conselice et al. (2007) Vast under prediction in models compared to observations

  4. Can detect log M = 9.5 galaxies to z = 3

  5. GOODS z GNS H

  6. log M > 11

  7. Size evolution for GNS galaxies Buitrago et al. (2008), ApJ, 687, 61 ALL massive galaxies at z > 2 are compact

  8. Galaxy sizes continue to decrease at higher redshifts Major mergers cannot explain Buitrago et al. 2008

  9. What is the role of AGN in galaxy formation? Can investigate with our sample using X-ray selected AGN Hosted by log M > 11 galaxies at 0.4 < z < 6 within the DEEP2/Palomar and GNS fields Method - find X-ray luminous AGN that are more luminous than L_X > 2.35 * 10^43 erg/s - create volume limited samples Using X-ray luminosities to calculate the black hole mass

  10. Co-evolution of black hole mass and galaxy mass Haring & Rix 04 If we assume that average black hole eta efficiency is the same at low and high redshift, or increasing with higher redshift then M_*/M_bh > 600 (compared to 1000 in local universe) Bluck, Conselice et al. (2010) in prep

  11. Can place constrains on time-scales for AGN activity based on M_* M_BH relation Rate = life-time/f_AGN Reveals that > 1/4 of massive galaxies have an AGN > 10^43 erg/s at 0.4 < z < 3

  12. The star formation rates as a function of stellar mass Galaxies with masses log M > 11 will roughly double in stellar mass due to star formation Ave. starformation rate for log M > 11 galaxies is roughly constant at 1.5 < z < 3 rhen declines at z < 1.5 Mass added from SF ~ Mass from major merging

  13. What factors drive the evolution of galaxies? Relation between environment and color at z < 1 for a log M > 10.25 sample

  14. Much stronger relation between color and stellar mass of the galaxy

  15. Galaxy properties do not strongly depend on the total environment as measured by halo mass of group/cluster

  16. See at higher redshifts as well for galaxies with log M > 9.5 Holds up to z =3 Individual galaxy mass is most important property for determining its formation history Gruethbacher, Conselice et al. (2010) in prep

  17. Summary Very deep NICMOS/HST imaging (GNS) to study galaxies at z > 2 to connect with galaxies at z < 1.5 with previous deep NIR surveys Examination of the major merger history, the AGN history and how enviroment vs. mass effects the formation of galaxies Massive galaxies become more compact at progressively higher redshifts and over 1/4th of massive galaxies at z < 3 have hosted an AGN. Log M > 11 galaxies double in mass due to star formation over ~2 Gyr period 1.5 < z < 3, similar increase due to major mergers Galaxy stellar mass most important driver of galaxy formation up to z=3

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