Mahalo-Subaru から Gracias-ALMA へ ALMA high-z workshop (NAOJ Mitaka, 12 June 2012) Mahalo-Subaru から Gracias-ALMA へ De nada ! Mahalo ! Gracias ! He mae iki ! Tadayuki Kodama (Subaru Telescope), Ken-ichi Tadaki (NAOJ/Univ of Tokyo), Yusei Koyama (Durham Univ.), Masao Hayashi (NAOJ), et al.

MApping HAlpha and Lines of Oxygen with Subaru “MAHALO-Subaru” MApping HAlpha and Lines of Oxygen with Subaru NB mapping of star forming galaxies at the peak epoch of galaxy formation Pilot obs (5 nights) + Intensive (10 nights @S10B-11A) + Normal (3 nights @S11B) Hayashi+ in prep. Koyama+ in prep. Hayashi+ ‘12 Tadaki+ in prep. Tadaki+ in prep. Kodama, T. (PI), Hayashi, M., Koyama, Y., Tadaki, K., Tanaka, I., et al.

Unique sets of Narrow-Band Filters on Suprime-Cam and MOIRCS The existing Suprime-Cam NB-filters capture emission lines from known good targets. The MOIRCS NB-filters were specifically designed for good targets at frontier redshifts. 4 narrow-band filters 7 narrow-band filters FWHMs correspond to ±1000-3000km/s

Why 1.5 < z < 2.5 ? （4 >Tuniv(Gyr) > 2.5） The peak epoch of star formation and AGN activities. The formation epoch of massive galaxies (SMG, red sequence). The Hubble sequence also emerges. Number density of AGNs Cosmic star formation rate density Fan et al. (2006) Hopkins and Beacom (2006) ※z~2.8 is the upper limit where we can capture Hα (~2.5μm) from the ground.

Inside-out propagation of star forming activities in clusters □ Hα emitters at z=0.81 (RXJ1716) □ [OII] emitters at z=1.46 (XCS2215) phot-z members ● 0.5 x R200 0.5 x R200 Lx=2.7×1044 erg/s Lx=4.4×1044 erg/s Koyama, et al. (2010) Hayashi, et al. (2010) Star forming activity in the core is much higher in the higher redshift cluster!

USS1558-003 proto-cluster at z=2.53 NB2315 Ks 8” N E Hα emitters 3.4 hrs integration on NB2315 (Hα) 0.4-0.5” seeing radio galaxy NB2315 Ks clump Hayashi et al. (2012) submitted

Hα emitters in two high-z proto-clusters at z>2 『赤いエミッター』は特に高密度領域に集中！ NB2315/MOIRCS NB2071/MOIRCS Koyama et al. (in prep) Hayashi et al. (2012) 　　　　　　　　　赤いHαエミッターの正体は？ Dusty+SF（星形成モード）? or Passive+AGN（AGN活動性）?

一般フィールドにおけるHα輝線銀河探査 Tadaki et al., in prep.

Tadaki + (in prep)

We need to resolve “forming galaxies” both spatially and kinematically, and at both Opt-NIR and Submm-Radio Mergers (environment)? Nucleated starburst + AGN ? Disordered Kinematics ? or Secular evolution? Disk-wide accretion & starburst? Rotation/pressure supported? AO and HST/JWST imaging (mergers or disk?) IFU spectroscopy (outflow? AGN? chemical evolution?) ALMA (dense gas distribution? SF mode? kinematics?)

Resolving power and FoV of our facilities Subaru+AO188 0.06-0.1”@2μm (~0.5-1kpc @z>1), 1 arcmin (FoV) Subaru+GLAO 0.2” @2μm (~1.5kpc), 15 arcmin JWST 0.05” @2μm (~0.5kpc), 3 arcmin TMT+AO 0.015” @2μm (~0.1kpc), 15 arcsec ALMA 0.01-0.1”@Submm (0.1-1kpc), 10arcsec-1arcmin (0.08-0.6” in cycle-1)

銀河形成解剖ワークショップ (Hilo, Hawaii, 2012/5/29-31)

SINS Survey z~2 UV selected galaxies; VLT/SINFONI w/o AO; Vc/σ~2-4 Foerster-Schreiber et al. (2009)

Signatures of outflows (500-1000km/s) blue wing = outflow blue wing = outflow Genzel et al. (2011)

Clumpyな形成途上銀河 (IFU + HST)

クランプの多様性、星形成モード、ダスト吸収の違い？ HAE @ z=2.2 @ SXDF-CANDELS Tadaki + (in prep)

ダストに隠された星形成 + 分子ガス量 + 高い空間分解能 (<0.1”) ALMAの役割 ダストに隠された星形成 + 分子ガス量 + 高い空間分解能 (<0.1”) 　可視～近赤外の観測では、どれほどの星形成活動を見逃しているか？ ＊バーストモードでは強いダスト吸収が予想される（Hαでも＞３等）。 ＊環境による依存性がありそう。 （ALMA：10Msun/yr @z>2) 　どこにどれだけの分子ガスがあり、進化段階や星形成モードは? ＊遠方銀河の進化段階（ガス-to-星質量）は？化学進化との比較は？ ＊星形成効率、モードは（ガス-to-星形成率）？環境の違いはあるか？ 　＊銀河中心部にガスが落ち込みバーストしているか、 　　　それともディスクやクランプで星形成をしているか？ 　ガスの運動（アウトフロー）は？ 　＊銀河風（アウトフロー）や回転はいつおこるか？ 　＊AGNジェット（分子流）は？

Double Sequence: “disk” mode + “starburst” mode SFE= Daddi et al. (2010) 赤い星形成銀河はバーストモードにあるのか？銀河中心部でバースト？環境依存性？

Lines of Oxygen with Subaru USS1558 proto-cluster (z=2.53) “Mahalo-Subaru” L: SFR>100M☉/yr M: > 50 M☉/yr S: < 50 M☉/yr MApping HAlpha and Lines of Oxygen with Subaru “Gracias-ALMA” GRAphing CO Intensity And Submm with ALMA CO(32) @ z~2.5 @100GHz  Mgas Dust conti. @450 μm–1.1 mm  Dusty SFR resolving spatially (<0.1”), kinematically (~50km/s) ｛ SFE ( SFR／Mgas ) ALMA FoV f(gas) ( Mgas／Mgas+Mstar ) Distribution and Motion of Gas  Merger induced starburst at the center? or Extended star formation over the disk?

GRAphing CO Intensity And Submm with ALMA “Gracias-ALMA” GRAphing CO Intensity And Submm with ALMA Mapping gas and dust at the peak epoch of galaxy formation and evolution CO(21) for z~1.5, CO(32) for z~2.5 @~100GHz SFR~50M☉/yr (4hrs, 5σ) Dust continuum @450 μm–1.1 mm @ z>1.5 SFR~15M☉/yr (40min, 5σ) ------------------------------------------------------------------------------------------------------------------------- Target z RA(J2000) Dec(J2000) line@GHz dust continuum ------------------------------------------------------------------------------------------------------------------------- XCSJ2215.9-1738 1.457 22 15 58.5 -17 38 02.5 CO(2-1)@94 Band-6,9 CL0332-2742 1.61 03 32 30.0 -27 42 36 CO(2-1)@88 Band-6,9 CIGJ0218.3-0510 1.62 02 18 21.3 -05 10 27 CO(2-1)@88 Band-6,9 cluster PKS1138-262 2.156 11 40 48.60 -26 29 08.5 CO(3-2)@110 Band-6,9 4C23.56 2.483 21 07 14.82 +23 31 45.0 CO(3-2)@99 Band-6,9 USS1558-003 2.527 16 01 17.30 -00 28 48.0 CO(3-2)@98 Band-6,9 ------------------------------------------------------------------------------------------------------------------------- SXDF/UDS 2.19 02 18 00 -05 00 00 CO(3-2)@108 Band-6,9 2.53 CO(3-2)@98 Band-6,9 field ------------------------------------------------------------------------------------------------------------------------- < 0.1” (<1kpc) : centralized, disturbed or disk-wide gas distribution? < 50km/s: gas in-/out-flow, rotating disk or disturbed motions? Internal structures:

原始銀河団では、一度に複数のターゲットが観測できる！ 例 Band-3 (CO) Band-6 (dust) 1558-003 (z=2.53) proto-cluster

The End