ADF22: ALMA Deep Field in SSA22 Hideki Umehata (Open University of - PowerPoint PPT Presentation

ADF22: ALMA Deep Field in SSA22 Hideki Umehata (Open University of Japan / University of Tokyo) With Y. Matsuda, Y. Tamura, K. Kohno, R.J. Ivison, I. Smail, M. Swinbank, M. Kubo, K. Nakanishi, D.M. Alexander, et al.

Motivation: Environmental Dependence § Importance of Environment ● Are there environmental dependence, which is clear at lower-z? ● How do SMGs obtain their fuels? What is the trigger? 6 0 3 2 z Toft+14 2

SMGs within a proto-cluster Daddi+09 - A number of works reported SMGs in galaxy overdensity. (e.g., Blain+04, Chapman+04, Daddi+09, Tamura+09, Walter+12, HU+2014, Dannerbauer+14, Smail+14, Casey+15, Plank Collaboration+15, Kato+16, Clements+16) 3 (But see also Chapman+09, Miller+15)

Target: SSA22 Proto-cluster § Surface number density map of z=3 . 09 LAEs Tamura+09, Nature -> Spatial correlation between SMGs and the LAEs ASTE AzTEC/ASTE, SCUBA2, Herschel/SPIRE 4

Target: SSA22 Proto-cluster § Surface number density map of z=3 . 09 LAEs HU+14 -> concentration of z=3 candidate SMGs ASTE AzTEC/ASTE, SCUBA2, Herschel/SPIRE 5

ALMA Deep Field in SSA22 Matsuda+05 Strategy: 1. Contiguous Mapping of the proto-cluster core. 2. Tracing multi-phase phenomena Dust Molecular Gas Diffuse Gas ● 1.1mm ● CO(3-2) ● Lyα Continuum CO(9-8) ● 6 arcmin^2 IFU (partly CO(1-0)) (2’ x 3’) ● 20 arcmin^2 (6’ x 3’) ● 7 arcmin^2 ( NB Images for (2’ x 3’) wide field) ALMA ALMA Subaru MUSE JVLA 6

1.1mm Continuum Survey 7

ADF22: Survey Area Tamura e al. 2009 HU et al. 2014 24 ′ 00 . 0 ′′ 0 . 0030 21 ′ 00 . 0 ′′ Cy4 Cy2 0 . 0024 18 ′ 00 . 0 ′′ Dec (J2000) Jy/Beam 0 . 0018 15 ′ 00 . 0 ′′ 0 . 0012 0 . 0006 +0 ◦ 12 ′ 00 . 0 ′′ 0 . 0000 − 0 . 0006 2 ′ − 0 . 0012 − 0 . 0018 18 m 00 . 00 s 45 . 00 s 30 . 00 s 15 . 00 s 22 h 17 m 00 . 00 s In total, ~20 arcmin^2 RA (J2000)

AzTEC 1.1mm Image 6 ‘x3’ Tamura+09, HU+14 1σ = 0.7-1.3 mJy/Beam

SCUBA2 850um Image 6 ‘x3’ Geach+17 1σ = 1.2 mJy/Beam (! 850um!)

AzTEC/SCUBA2/ALMA View 2 ‘x3’for each - (bright) ALMA sources in general trace the AzTEC/SCUBA2 sources. - At the same time, significant portion of SMGs should be missed.

ADF22 1.1mm Image Frequency 263 GHz Area 7 arcmin^2 Angular res. 0.5-1.0” RMS 60 uJy/Beam 1’ HU+15; 17b

ALMA sources: Securely detected HU+17b ● 18 sources with >5sigma ● S_1.1mm = 0.4 – 5.6 mJy (5-58 σ ) 13

[OIII]5007 Redshifts of ALMA sources by MOIRCS ADF22 . 11 at z=3 . 093 Kubo, HU, et al. 2016 ADF22 . 16 at z=3 . 085 ADF22 . 1 at z=3 . 0915 CO(3-2) Yun et al. in prep by LMT 90 80 ● We have determined z_spec for 13/18 ALMA sources. ● 12 ALMA sources are at z=3.085-3.097 (and some more candidates). 14

Multiplicity of ‘classical’ SMGs HU+17b AzTEC: 0~3σ ● Multiple ‘individual’ SMGs consist some of bright ‘classical’ SMGs . ● Physically associated SMG groups can account for some portion of them . 15

● 8 X-ray AGNs at z=3 . 09 AGN (Lx ~10^44 erg/s) AGN ● 6/8 with 1 . 1mm emission AGN AGN AGN AGN AGN AGN X-ray ALMA Soft B: Red Hard B: Blue 16 16 (Lehmer+2009)

SMGs in the cosmic structure HU+15 (cf. Matsuda+05) ● An extremely-rich SMG cluster is found in a node of the cosmic web. ● The most active star-formation and SMBH growth “simultaneously” occur at the center of the z=3.1 proto-cluster. 17

Molecular Gas Survey 18

Frequency Coverage ← CO(9-8) ← CO(3-2) ← CO(1-0) 19

ALMA Observation Band3 Frequency 84-88 GHz, 96-100 GHz Area 7 arcmin^2 Angular res. 0.8-0.9” 20

Summary ALMA multi-band contiguous mapping is ongoing in SSA22. - Multiplicity is caused by physically associated pairs/groups in this field. - The volume density of SMGs, X-ray AGNs, and molecular gas reservoirs are > ~x100 higher than the general field. - There might be multiple paths to ignite and sustain starbursts activity at the proto-cluster core. Question Where and how do SMGs form within cosmic structure? 21