SEARCH CENTER FOR SPACE AND COSMIC EVOLUTION Toaru Nagao (Ehime Univ.)
Population Ill Recombination Big Banq z=1100 BigBang Nucleosynthesis ～ first hydrogen ~ first helium First Heavy Elements ~ first stars, first suparnovae ～ second generations ~ third, fourth, …. ~ earth-like planets ～ life, human, & you
. (1) Metallicity Evolution of Galaxies ~ Luminosity-metallicity & mass-metallicity relations ~ Toward high-z universe up to z=3 ~ Comparison with model predictions (2) Search for "Population LET" Galaxies ~ Population ILI at z < 10 !2 ~ Expected "observational" properties of PopIEI ~ Subaru searches for PopLII galaxies (3) Future Prospects ~ Metallicity at z > 3 (by focusing on AGNs?) ~ Searching for PopEEI galaxies with… ?? ~ My personal interests
Metallicit 0.5 b 0.0 88 Z (10²) b • log Mtot e 10 Mass Metallicity Measurements of Galaxies 4000 5000 6500 7000 4500 5500 6000 (Å) F(H ) = S N  N  h v α(I) dV F(O ) = $ Ngo Ne h v goo(Z) dV F(O+) = S No+ N hv go+(T) dV E(O 2+) = S. No2+ Ne h v qo2+(T) dV focusing on "O/H" = (00+0++02++ ) We need to know emission-line fluxes and gas temperature
O²+ Grotrian diagram [Omi]4363 is available only in nearby galaxies... 6500 5000 4000 4500 5500 6000 7000 (Å) λ
log}([0 III] λ5007/Hβ)/([N II] λ6583/Hα)}
"Luminosity-Mefallicity Relation" "Mass-Metalltcity Relation"
M-Z relation, for 6 decades in stellar mass. Assuming "closed be
Evolving L-Z relation !!
8.8 8.6 Log (0/F 8.4 8.2 M B Log (Motar/Mg)
CDFaC9 0=3.21 K ar=22 int＝3.3h 15 [ OIII ] 12+log(0/H) 1.8 1.9 [ μm ] Aobserved Calibration: Nagao ei al. (2006年)
Maiolino, Nagao, et al., (2008) own-sizing chemical evolution
2008 log M, [Mo] log M, [Mo]
20 25 15 - 10 redshift Scannapieco et al. (2003) Yoshida et al. (2003)
Pop III: Salpeter IMF (1-500 Mg) Schaerer (2002) The earliest phase (with PopIII) of the galaxy evolution is characterized by strong H I and He II emission lines ! Yoshida et al. (2003)
Nagao et al. (2004) Subary/OHS J-band spectroscopy 54 ksec (3 nights) integration (!!!) → no detection… SDF i-drop with huge EW Ly α : see also Nagao et al. (2005a, 2007)
811 LBGs at z=3 (Shapley et al. 2003) He II emission !? Evidence of PopIII !? (Jimenez & Haiman 2006) Just a stellar feature? (mentioned by Shapley+03) ...let's see LAEs, instead of LBGs.. 11 LAEs at z=4.5 (Dawson et al. 2004) No He II em 1550 1540 1560 Rest Wavelength (Å) 1630 1640 Rest Wavelength (Å) (10-18er 1300 1000 1100 1200 1400 1500 1600 1700 Rest Wavelength (Å) CIV  λ1549 Hell   λ1640 Relative 1530 1570 1620 1650 1660
. Maiolino, Nagao, et al., (2008) Going beyond z=3 !2 Is it really interesting !? . Is it really feasible !? CDFaC9 CDFaC9 (Å) 7.5 8 8.5 9 7 12 + log(0/H)
Maiolino, Nagao, et al., (2008) Going beyond z=3 !2 Is it really interesting !? . Is it really feasible !? Let's try with TMT Or, focusing AGNs !? Or', waiting for JWST !?
.. Maiolino, Nagao, et al., (2008) : Z=0 (Zero Metallicity) Still search for PopLIT [2 Let's wait for HSC . Follow-up with JWST 2+log(0/
Z 0 (Zero Metalicity) Extremely Metal-Poor Gals : Now Surveys on Going... Studying Earliest Phase of Chemical Evolution through "Relative" element abundance ratios
12 + log (0/H)
Summary
: (1) Metallicity Measurements of Galaxies ~ Downsizing evolution of the M-Z relation © z<3 ~ Inconsistent with Theoretical Models (2) Observational Study to Search for PopLIE ~ Possibly interesting even at z<10 ~ He II emission is the most powerful diagnostic line ~ Multi-NB imaging → Meaningful limit on SFRD e pin (3) Open Issues  : ~ Metallicity © z>3: [Ne lll] method, AGNs, or JWST ~ HSC may find PopEEE candidates ⇒ JWST ~ Relative element abundance ratios (especially in XMPGs) Collaborators Roberto Maiolino     . (Rome Observatory Alessandro Marconi. (Florence,Univ.) Matt Malkan - Ly Chun (Geneve Observatory) Daniel Schaerer (Tokyo Univ.) Kentaro. Motohara Nobunari Kashikawa  (NAOT Yoshiaki Taniquchi (Ehime Univ.) Takashi Murayama @lohoku Univ.) The AMAZE collaboration . Subary Deep Field project and much more.. ACE AND COSMIC EVO