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PI Total time #CoIs, team

The co-evolution of SMBHs and galaxies

daryl-wilcox
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PI Total time #CoIs, team

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  1. The co-evolution of SMBHs and galaxies To measure accurate BH masses via gas kinematics of a sample of massive z≈2.4 galaxies expected to host massive BHs. Upon comparison with the local M- relation, determine whether there has been evolution since z=0. The BH masses will be measured using resolved gas dynamics of the H+[NII] lines, thus allowing us to take advantage of the ELT diffraction limited resolution of ~13 mas in the K-band PI Total time #CoIs, team Margrethe Wold 30h (ELT 42m) 2-4 co-Is

  2. Scientific Rationale Woo et al (2006) NGC 2787 Hubble Heritage Gallery M -  relation in the distant universe - BH mass and bulge stellar dispersion are closely linked : M 4 - M -  relation is an important tool - BHs and AGN activity essential ingredients of galaxy formation - how does M and  relate in the distant universe?

  3. Barth (2003) BH sphere of influence: Rg = GM / 2 Immediate objective - Obtain BH masses via H+[NII] gas kinematics within/close to Rg in a sample of massive radio galaxies at z~2.4 • At z=2.4, H+[NII] lies in the K-band, and 42m ELT has D=13.2 mas • Choose radio galaxies because we expect them to have massive BHs  Rg  13 mas (range 6-52 mas depending on ) D

  4. ELT Justification: require high spatial resolution. Two slitpos per object, f~10-19 erg/s/cm2/Å, SNR = 10-20  ~3 hrs/galaxy Legacy Value: central gas kinematics from spectra Data Reduction: requires careful modeling of bulge and black hole potential. Need a high-res K-band image for modeling the bulge potential

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