Lisa Kewley - kewley@ifa.hawaii.edu

Lisa Kewley (IfA, U.Hawaii)

Collaborators: C. Kobulnicky (U.Wyoming), M. Geller (SAO), Collaborators: C. Kobulnicky (U.Wyoming), M. Geller (SAO), B. Barton (UC Irvine), R. Jansen (ASU)B. Barton (UC Irvine), R. Jansen (ASU)

Lisa Kewley - kewley@ifa.hawaii.edu

MotivationMotivation Metallicity diagnosticsMetallicity diagnostics Local samples: Local samples: NFGSNFGS

Galaxy PairsGalaxy Pairs

Intermediate-z: GOODSIntermediate-z: GOODS Metallicity History 0<z<1Metallicity History 0<z<1 Future DirectionsFuture Directions

SummarySummary

Lisa Kewley - kewley@ifa.hawaii.edu

MotivationMotivation 1. Metallicity history of star-forming galaxies1. Metallicity history of star-forming galaxies still largely theoretical.

Nagamine et al. (2001)

Lisa Kewley - kewley@ifa.hawaii.edu

data from Teplitz et al. (2003)filled = [OII]filled = [OII]unfilled = Hunfilled = H

K98 [OII] SFRK98 [OII] SFR

Our [OII] SFROur [OII] SFRlog(O/H)+12~8.6AV=1also: Rosa-Gonzalez, Terlevich, & Terlevich (2002)

Our [OII] SFROur [OII] SFRlog(O/H)+12~8.8AV=1

MotivationMotivation2. [OII] SF History2. [OII] SF History

Kewley, Geller & Jansen (2004)

Lisa Kewley - kewley@ifa.hawaii.edu

Kewley & Dopita (2002, ApJS, 142, 35)

Metallicity DiagnosticsMetallicity Diagnostics

“R23”

Lisa Kewley - kewley@ifa.hawaii.edu

Metallicity Diagnostics - [NII]/HMetallicity Diagnostics - [NII]/H

Kewley & Dopita (2002, ApJS, 142, 35)

also: Denicolo, Terlevich & Terlevich (2002, MNRAS, 330, 69)

R23 and [NII]/H re-parameterized Kobulnicky & Kewley (2004,ApJ, 617, 240)

Lisa Kewley - kewley@ifa.hawaii.edu

Local Sample: Local Sample: NFGSNFGS

198 galaxies objectively selected from the CfA galaxy survey (Davis & Peebles 1983, Huchra et al. 1983)

full range in Hubble type

full range of absolute magnitudes in CfA survey

See Jansen et al. (2000) http://cfa-www.harvard.edu/~jansen/nfgs/nfgssample.html

Lisa Kewley - kewley@ifa.hawaii.edu

Local Sample: Galaxy PairsLocal Sample: Galaxy Pairs

502 galaxies objectively selected from the CfA redshift catalog (v < 2300 km/s, v < 1035 km/s, D < 77 h-1 Mpc)

Nuclear spectra for ~200 galaxies in pairs (Barton et al. 2000)

EWs + stellar population synthesis “burst timescale’’ (Barton et al. 2003)

Lisa Kewley - kewley@ifa.hawaii.edu

NFGS & Galaxy PairsNFGS & Galaxy Pairs

Pairs

NFGS

Nuclear Spectra:Requires Aperture

Correction

Lisa Kewley - kewley@ifa.hawaii.edu

Aperture CorrectionAperture Correction

Correction ~ 0.13 dexbut may vary between 0-0.4 dex

Kewley, Geller, & Jansen 2005, PASP, 117, 227

Lisa Kewley - kewley@ifa.hawaii.edu

GOODS Survey: 0.3 < z< 1 GOODS Survey: 0.3 < z< 1

204 galaxies with metallicity-quality spectra204 galaxies with metallicity-quality spectra

Metallicities calculated using EWsMetallicities calculated using EWs

Upper RUpper R2323 branch assumed branch assumed

AAvv=1 assumed if no H=1 assumed if no H

See Kobulnicky & Kewley (2004, ApJ, 617, 240)

Lisa Kewley - kewley@ifa.hawaii.edu

GOODS Survey: 0.3 < z< 1 GOODS Survey: 0.3 < z< 1

Kobulnicky & Kewley (2004, ApJ, 617, 240)

Lisa Kewley - kewley@ifa.hawaii.edu

GOODS Survey: 0.3 < z< 1 GOODS Survey: 0.3 < z< 1

Kobulnicky & Kewley (2004, ApJ, 617,240)

Lisa Kewley - kewley@ifa.hawaii.edu

ConclusionsConclusions

Galaxy pairs nuclei span larger metallicity range Galaxy pairs nuclei span larger metallicity range than NFGS:than NFGS: less enriched - dynamical mixing?less enriched - dynamical mixing?

Preliminary Metallicity History Preliminary Metallicity History (for star-forming galaxies)(for star-forming galaxies) Metallicity evolution observed....Metallicity evolution observed....

but more work to do...but more work to do...

Lisa Kewley - kewley@ifa.hawaii.edu

Pairs

GOODSassumes upper branch

LBGs: Pettini et al. (2001)Shapley et al. (2004)Kobulnicky & Koo(2000)

Future Directions: 0<z<3Future Directions: 0<z<3

Lisa Kewley - kewley@ifa.hawaii.edu

Future DirectionsFuture Directions

Near-IR Spectra (RNear-IR Spectra (R2323 degeneracy, A degeneracy, Avv))

Modelling of emission-line selection effectsModelling of emission-line selection effects

More galaxies!More galaxies!