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

Hideki Umehata (Open University of Japan / University of Tokyo)

ADF22: ALMA Deep Field in SSA22

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

2

§ Importance of Environment

• Are there environmental dependence, which is clear at lower-z?
• How do SMGs obtain their fuels? What is the trigger?

2 3 6 z Toft+14

SMGs within a proto-cluster

3

• 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) (But see also Chapman+09, Miller+15) Daddi+09

Target: SSA22 Proto-cluster

4

§ Surface number density map of z=3.09 LAEs

AzTEC/ASTE, SCUBA2, Herschel/SPIRE

Tamura+09, Nature

• > Spatial correlation between SMGs and the LAEs

ASTE

Target: SSA22 Proto-cluster

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§ Surface number density map of z=3.09 LAEs

AzTEC/ASTE, SCUBA2, Herschel/SPIRE

HU+14

• > concentration of z=3 candidate SMGs

ASTE

ALMA Deep Field in SSA22

6

• 1.1mm

Continuum

• 20 arcmin^2

(6’ x 3’)

Dust

• CO(3-2)

CO(9-8) (partly CO(1-0))

• 7 arcmin^2

(2’ x 3’)

Molecular Gas

• Lyα
• 6 arcmin^2 IFU

(2’ x 3’) ( NB Images for wide field)

Diffuse Gas

Strategy:

• 1. Contiguous Mapping of the proto-cluster core.
• 2. Tracing multi-phase phenomena

ALMA ALMA JVLA Subaru MUSE

Matsuda+05

1.1mm Continuum Survey

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22h17m00.00s 15.00s 30.00s 45.00s 18m00.00s

RA (J2000)

+0◦12′00.0′′ 15′00.0′′ 18′00.0′′ 21′00.0′′ 24′00.0′′

Dec (J2000) 2 ′ −0.0018 −0.0012 −0.0006 0.0000 0.0006 0.0012 0.0018 0.0024 0.0030 Jy/Beam

ADF22: Survey Area

Cy2

Tamura e al. 2009 HU et al. 2014

Cy4 In total, ~20 arcmin^2

AzTEC 1.1mm Image

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

SCUBA2 850um Image

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

AzTEC/SCUBA2/ALMA View

• (bright) ALMA sources in general trace the AzTEC/SCUBA2 sources.
• At the same time, significant portion of SMGs should be missed.

2 ‘x3’for each

ADF22 1.1mm Image

1’

Frequency 263 GHz Area 7 arcmin^2 Angular res. 0.5-1.0” RMS 60 uJy/Beam

HU+15; 17b

ALMA sources: Securely detected

13

• 18 sources with >5sigma
• S_1.1mm = 0.4 – 5.6 mJy (5-58σ)

HU+17b

Redshifts of ALMA sources

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• We have determined z_spec for 13/18 ALMA sources.
• 12 ALMA sources are at z=3.085-3.097 (and some more candidates).

ADF22.11 at z=3.093 ADF22.16 at z=3.085

Kubo, HU, et al. 2016 80 90

ADF22.1 at z=3.0915

Yun et al. in prep

[OIII]5007 by MOIRCS CO(3-2) by LMT

15

AzTEC: 0~3σ

Multiplicity of ‘classical’ SMGs

• Multiple ‘individual’ SMGs consist some of bright ‘classical’ SMGs.
• Physically associated SMG groups can account for some portion of them.

HU+17b

16 16

AGN AGN AGN AGN AGN AGN

X-ray

Soft B: Red Hard B: Blue (Lehmer+2009)

ALMA

• 8 X-ray AGNs at z=3.09

(Lx ~10^44 erg/s)

• 6/8 with 1.1mm emission

AGN AGN

• An extremely-rich SMG cluster is found in a node of the cosmic web.
• The most active star-formation and SMBH growth “simultaneously”
• ccur at the center of the z=3.1 proto-cluster.

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SMGs in the cosmic structure

HU+15 (cf. Matsuda+05)

Molecular Gas Survey

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Frequency Coverage

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← CO(9-8) ← CO(3-2) ← CO(1-0)

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ALMA Band3

Observation

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

Summary

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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?