Jeyhan Kartaltepe - NOAOCOSMOS Meeting IfA, Honolulu, HI2010 June 8D. Sanders, V. Smolcic, L. Kewley, M. Salvato, P. Capak, E. Le Floch, H. Aussel, D. Frayer et al.

Paper ISEDs Kartaltepe et al. 2010, ApJ, 709, 572Paper II Morphology re-submitted, should hear back any dayNextThe Starburst-AGN Connection Among COSMOS (U)LIRGsFocus on optical spectroscopy out to z~1

Starburst/AGN activity are directly linkedTogether may regulate black hole/bulge growth in galaxiesLuminous infrared galaxies have high luminosities due to dust enshrouded SF/AGN activityEach contribute to the bolometric luminosityHow can we separate the two?What can we do with existing optical spectroscopy?

1503 sources with 0 < z < 3Spectroscopy for ~40%zCOSMOS, DEIMOS, etc.Eventual goal: correlate activity with luminosity/morphology

ULIRGsLIRGsHyLIRGsRedshift (z)

X-ray luminosityRadio powerSED shape (i.e., Power-law)IRAC colorsInfrared to optical ratio (e.g., Fiore et al. 2008, Dey et al. 2008)

Spectroscopic diagnostics

5% at low LIR>70% for ULIRGs100% for HyLIRGslog (LIR)

At low redshift, can classify 135 galaxies using standard line diagnostics 0 < z < 0.5 (where Ha still observable, 18% of sample at these redshifts)log(LIR) = 8.8 11.7, = 10.6

8 (6%) classified as AGN34 (25%) classified as composite93 (69%) classified as star forming Many more sources identified as AGN through spectroscopy than other selection methods

AGNDEEP2: e.g., Montero-Dorta et al. 2009 380 sources (0 < z < 1)8 sources selected2 X-ray detectedAnother 2 (z

Smolcic et al. 2006, 2008 Correlation between rest-frame color and galaxys position on BPT diagram for radio selected sources

P1 color (derived from modified Stromgren system for SDSS galaxies) correlates with metallicity and stellar population, P2 with dust

P1 > 0.15 AGN selection

Appears to work well at low z, results at high z are untested Is there redshift evolution? Can composites be separated?

DEEP2: e.g.,Yan et al. 2006; Willmer et al. 2006; Montero-Dorta et al. 2009 218 Sources (0 < z < 1)22 sources selectedNone are AGN by other methods8 overlap with low-z sample4 SF on all 3 diagramsOther 4 are either Seyferts, LINERS, or composites on 2 out of 3

Incorporate new spectra DEIMOS, 20k sample, etc.Further tests Evolution of P1 with redshiftLamareille et al. (2004, 2010) diagnosticsX-ray stackingCompare diagnostics with SDSS in the local universez > 1 ?NIR Spectroscopy (FMOS, MOSFIRE, MOIRCS, FLAMINGOS2, etc.)

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