The environment of SMGs Yuichi Matsuda (NAOJ/ALMA) Key Ques5on How - PowerPoint PPT Presentation

The environment of SMGs Yuichi Matsuda (NAOJ/ALMA)

Key Ques5on How do SMGs relate to Lya emi>ng gaseous haloes (LABs) and protoclusters? • ALMA observaFons of giant (>100 kpc) LABs in the SSA22 protocluter at z=3.1 • SCUBA-2 survey of HSC-selected z=4 protoclusters

How do SMGs relate to LABs? Talks by Chapman, Karim , Frayer and Casey P o sters by Dannerbauer and Ao

How is the ambient gas of real SMGs? 100 10 19 50 z (kpc) 0 10 18 −50 −100 z=3.0 z=2.8 z=2.6 Narayanan+15 1 H g cm − 2 100 10 17 50 z (kpc) 0 −50 10 16 −100 z=2.5 z=2.2 z=2.0 −100 −50 0 50 100 −100 −50 0 50 100 −100 −50 0 50 100 k (kpc) x (kpc) x (kpc)

How is the ambient gas of real SMGs? Narayanan+15 100 10 19 50 z (kpc) 0 10 18 −50 SSA22 LAB1 at z=3.1 −100 z=3.0 z=2.8 z=2.6 1 H g cm − 2 Steidel+00, Matsuda+04 100 10 17 50 z (kpc) 0 −50 10 16 −100 z=2.5 z=2.2 z=2.0 −100 −50 0 50 100 −100 −50 0 50 100 −100 −50 0 50 100 k (kpc) x (kpc) x (kpc)

Strong connec5on between SMG and LAB SSA22 LAB01 (Chapman+01, 04) S 850 =17mJy source!! One of the brightest (un-lensed) SMGs.

SMA / SCUBA-2 Observa5ons SMA map (Matsuda+07) SCUBA-2 map (Geach+14) S880<4.2mJy (3-sigma) S850=4.6+/-1.1mJy

SCUBA 850um Observa5ons ~1.5mJy ~5mJy ~15mJy Geach+05 LAB01 LAB02 LAB05 LAB18 See also Hine+16 and Ao+17

ALMA 860um Observa5ons (w/ Kohno, Hatsukade, Ikarashi, Umehata, Ao, Kato, Smail, Geach, Hine, Chapman, Alexander, Steidel) ALMA Band 7 FoV ALMA Band 7 FoV ALMA Band 7 FoV ALMA Band 7 FoV LAB02 LAB05 LAB18 LAB01 100 kpc 100 kpc LAB01 LAB02 LAB05 LAB18 1" Taper 1" Taper 1" Taper 1" Taper Lya Lya ~1mJy Lya Lya 1 ~2mJy ~1-4mJy ~0.5mJy 2 0.3 0.5 0.3 0.5 0.3 0.5 0.3 0.5 1 1 1 2 3 3 4 rms=74microJy/beam rms=74microJy/beam rms=75microJy/beam rms=75microJy/beam See also Ao’s poster, Alexander+16, Geach+16 and Umehata+17

ALMA 860um Observa5ons (w/ Kohno, Hatsukade, Ikarashi, Umehata, Ao, Kato, Smail, Geach, Hine, Chapman, Alexander, Steidel) ALMA showed that all the observed 4 giant (>100 kpc) LABs consist of single or mulFple SMGs. LAB01 LAB02 LAB05 LAB18 1" Taper 1" Taper 1" Taper 1" Taper Lya Lya ~1mJy Lya Lya 1 ~2mJy ~1-4mJy ~0.5mJy 2 0.3 0.5 0.3 0.5 0.3 0.5 0.3 0.5 1 1 1 2 3 3 4 rms=74microJy/beam rms=74microJy/beam rms=75microJy/beam rms=75microJy/beam See also Ao’s poster, Alexander+16, Geach+16 and Umehata+17

SSA22 LAB01 Geach+16 ALMA HST MUSE(Lya) Umehata+17

How do SMGs relate to protoclusters? Talks by Chapman, Viera, Casey and Umehata P o sters by Lee, Cheng , Champagne and Dannerbauer

HSC protocluster survey (Toshikawa+) Overdensity map WIDE-GAMA15H R.A. (comoving Gpc) 0 . 0 0 . 2 0 . 4 0 . 6 0 . 8 1 . 0 1 . 2 1 . 4 1 . 6 1 . 8 6 0 . 4 Decl. (comoving Gpc) 1 overdensity ( σ ) 4 Decl. (degree) 0 . 3 0 2 0 . 2 − 1 0 . 1 0 − 2 0 . 0 − 2 224 222 220 218 216 214 212 R.A. (degree) average 10 − 1 random 179 protocluster candidates protocluster 10 − 2 candidates are identified from the S16A fraction HSC dataset (S eff =121deg 2 ). 10 − 3 10 − 4 We selected 6 highest (>7-σ) overdensiFes at z~4 which are expected to grow into 10 − 5 galaxy clusters of > 10 14 M ⊙ by z=0 with the probability of > 90% − 2 0 2 4 6 8 10 overdensity ( σ )

SCUBA-2 mapping (z~4 HSC PCs) (w/ Toshikawa, Lee, Ishida, Fujimoto, Kohno, Umehata, Ao, Smail, Clements, Geach, Chapman, Blain, Edge, Gear) We will investigate the distribution/properties of SMGs in protoclusters. ∆ R.A. (physical Mpc) 2 1 0 − 1 − 2 2 1 0 − 1 − 2 2 1 0 − 1 − 2 2 4 ◯ LBGs 6 1 ● SMGs 2 ∆ Decl. (physical Mpc) 0 0 ∆ Decl. (arcmin) overdensity ( σ ) − 2 4 − 1 − 4 − 2 2 2 4 1 2 0 0 0 − 2 − 1 − 4 − 2 − 2 4 2 0 − 2 − 4 4 2 0 − 2 − 4 4 2 0 − 2 − 4 ∆ R.A. (arcmin) ALMA follow-up of 67 SCUBA-2 sources (Toshikawa+, Cycle5)

Radial Distribu5on Bright SMGs tend to lie near the centre of z~4 protocluster? bright ~10cMpc 10 S 850 µ m (mJy/beam) 8 6 4 faint 2 0 1 2 3 4 5 centre outskirt R (arcmin)

Conclusions & Summary • How do SMGs relate to LABs and protoclusters? • ALMA showed that all the observed 4 giant (>100 kpc) LABs consist of single or mulFple SMGs. • SCUBA-2 showed a hint that bright SMGs are associated with UV-selected z=4 protoclusters. • Future direcFon: How do SMGs related with Cosmic Web? -> Talk by Casey

How can we rebrand SMGs? From Hodge’s talk • Do we need to rename SMGs? Good examples: Large scale structure -> Cosmic Web Smooth gas accreFon -> Cold Stream Gaseous halo -> Circum galacFc medium