1. Galactic Astronomy 銀河物理学特論 I Lecture 3-5: Evolution of dynamical structure of galaxies Seminar: Forster Schreiber et al. 2009, ApJ, 706, 1364 Lecture: 2012/01/30

2.  arcsec Rest-B 0<z<1: Morphology of z~1 star-forming galaxies (Luminous IR Galaxies) Konishi et al. 2011, PASJ, 63, 363

3.  SFR fraction （●:▲:○:△） 0.64:0.14:0.19:0.03  For galaxies with SFR > ~ 19 M sun yr -1 (24 mm limit), 70% are LIRGs.  No active star formation among non-LIRG bulge dominated galaxies LIRGs dominate star formation rate density z ~ 1. M s ≥ 10 10 M sun LIRGs have morphologies similar to disk galaxies ○ non-LIRG disk △ non-LIRG bulge ● X-ray ● LIRG disk ▲ LIRG bulge 24  m completeness limit E/S0 S0/a-Sb Sbc-Sd SDSSemlines 0<z<1: Morphology of z~1 star-forming galaxies (Luminous IR Galaxies) Konishi et al. 2011, PASJ, 63, 363

4. Between 0<z<1 : Disk galaxies : Disk-size 0<z<1: Size evolution of disk galaxies The absolute magnitude – size relation (i.e. surface brightness) shows evolution but no evolution in the stellar mass – size relation (i.e. surface stellar mass density) (Barden et al. 2005, ApJ, 635, 959)

5. Between 0<z<1 : Disk galaxies : Disk dynamics 0<z<1: Evolution of the Tully-Fisher relation Disk galaxy dynamics with VLT/GIRRAFFE multi-IFU w/o AO Flores et al. 2006, A&A, 455, 107 (0.4<z<0.75, disk galaxies), 35% pure-rotating disks following local-TF relation, 65% disturbed rotation, complex kinematics ? IMAGES: Yang et al. (2008, A&A, 477, 789), Neichel et al. (2008, A&A, 484, 159), Puech et al. (2008, A&A, 484, 173) Neichel+08 : 12/22 spiral morphology galaxies have PR or CK velocity fields Peuch+08 : 2 times increase of stellar mass necessary to match the local K-band TF relation ？ Yang+08; RD (blue), PR (green), CK (red) Distance between model and observed peaks of velocity dispersion (pixel=0.52”) Velocity dispersion ratio between model and observation at the model peak position Puech+08; Solid line: local TF relation

6. 0<z<1 : Disk galaxies : Bar-fraction Sheth et al. (2008, ApJ, 675, 1141) COSMOS HST images sample Fraction of barrd spiral galaxies (bar-fraction) shows rapid increase between z=1 and 0. The increase is more rapid for galaxies with smaller stellar mass. Black: z=0.14-0.37 Blue: z=0.37-0.60 Red: z=0.60-0.84

7. 0<z<1 : Early-type (E+S0) galaxies Treu et al. 2005, ApJ, 633, 175, 0.2<z<1.2 field E+S0 (GOODS-N) Offset from local FP (sigma-SB-Re) is d(logM/L)/dz=-0.4 for logM* >11.5 and 0.5>d(logM/L)/dz>-1 for logM*<11. Such offsets are consistent with passive evolution with zf=5 and zf=1-2, respectively. E+S0 galaxies in clusters of galaxies show offset of d(logM/L)/dz=-0.46, larger evolution than field samples. van der Wel & van der Marel (2008, ApJ, 684, 260) 0.6<z<1.2 field E+S0 (V/sigma)* vs. MB relation and (V/sigma)* vs. Ellipticity relation can be explained with passive evolution models. Fainter elliptical galaxies show larger fraction of galaxies with large (V/sigma)* and large ellipticity. van der Wel et al. (2008, ApJ, 688, 48) 0.8<z<1.2 field+cluster E+S0 Evolution of the Re vs. Mdyn relation. Re is about half at the same Mdyn.

8. Between 0<z<1 : Disk galaxies : Disk dynamics IFU (+AO) spectroscopic observations of high-redshift galaxies： image slicer VLT SINFONI

9. Z~3 ; structure n Most of the LBGs (+an RadioG +DRGs) are fitted well with Sersic profiles with n<2. (Akiyama et al. 2008, ApJS, 175, 1)

10. Z~3: Dynamics Stark et al. 2008 Nature, 455, 755; z=3.07 lensed galaxy Thanks to gravitational lensing and LGSAO, effective spatial resolution was very high (20- 40mas = 150-300pc resolution). Smooth velocity shear field support the rotational structure of the galaxy. +-50km/s rotation (inner 0.5kpc) + flat rotation curve, logMdyn=9.3 vs. logMstr=9.8 Sigma=54km/s, v/sigma=1.2 (heating by star- formation activity ?), 4.4 Msolar/yr/kpc2 (Similar to nuclear Star burst in local galaxies) 12+log(O/H)=8.6 = 0.9Zsolar, CO luminosity-gas mass conversion factor <0.8; ~local LIRG (1) << local spiral (5)

11. Z~3: Dynamics Law et al. (2009, ApJ, 697, 2057) 12 galaxies at z=2.0-2.5 and 1 galaxy at z=3.3 ([OIII]) observed with Keck LGS-AO (typical resolution 0.15”) + OSIRIS with 1.0-4.5hours with 100/150mas FWHM (50mas sampling). Mean velocity (black) vs. velocity dispersion (red)

12. Z~3: Dynamics Law et al. (2009, ApJ, 697, 2057) V(shear) as a function of stellar mass. Horizontal dashed line represents the typical velocity dispersion (70km/s). V(shear) as a function of gas mass fraction (Mgas/(Mgas+Mstar), Mgas estimated with Ha luminosity)

13. Z~3 : Summary I Rotation supported or velocity dispersion supported ? Large stellar mass galaxies are rotation dominated ? Large velocity dispersion imply large Jean’s mass resulting big star- forming complexes (Elmegreen et al 2008, next slide). Thick disk ? : hz/R = 0.5(sigma/v)^2 Toomre’s Q parameter is small : globally-unstable disks. Q= sigma k / 3.36 G Sigma MW: sigma=30km/s, Sigma=50Msolar/pc^2, k=36km/s/kpc -> Q=1.4 High-z: sigma=50-100km/s, Sigma=300Msolar/pc^2, k=V/R=30km/s/kpc resulting Q=0.2