High-z protocluster candidates with Planck, Herschel & Spitzer - - PowerPoint PPT Presentation

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High-z protocluster candidates with Planck, Herschel & Spitzer - - PowerPoint PPT Presentation

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High-z protocluster candidates with Planck, Herschel & Spitzer Clment Martinache, Institut d'Astrophysique Spatiale, Univ. Paris-Sud, CNRS, Univ. Paris- Saclay Collaborators : Herv Dole, Alessandro Rettura, Benjamin Clarenc & SPHerIC

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10/06/16 Clément Martinache 1

High-z protocluster candidates with Planck, Herschel & Spitzer

1 - Motivations 2 – z~2 structures with Planck & Herschel 3 – SPHerIC : Spitzer Planck Herschel Infrared Clusters 4 – Millimetric follow-up Clément Martinache, Institut d'Astrophysique Spatiale, Univ. Paris-Sud, CNRS, Univ. Paris-

Saclay Collaborators : Hervé Dole, Alessandro Rettura, Benjamin Clarenc & SPHerIC collaboration.

Paris, Oct. 2016 - High Redshift (proto)Clusters: anecdotal or important phases ?

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1/ Motivations

z > 1.5 – 2. Crucial epoch in star formation history

  • f cluster galaxies

Hundreds of candidates, few confirmed.

This talk : sample of 84 candidates biased toward intense star-formation

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2/ Searching for z~2 structures with Planck and Herschel

Planck/HFI assets :

  • 353, 545, 857 GHz bands probe

dusty star formation at z~2.

  • All sky (Rare objects, 10-1 deg-2)
  • HFI beam comparable to z~2 structures

angular size. (5' ↔ 2.5Mpc) Method principle: Detect excess emission at 545 GHz.

Color lines : MBB, β = 1.5, T=30K Planck Intermediate Paper, XXXIX (submitted)

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2/ Searching for z~2 structures with Planck and Herschel

Planck/HFI assets :

  • 353, 545, 857 GHz bands probe

dusty star formation at z~2.

  • All sky (Rare objects, 10-1 deg-2)
  • HFI beam comparable to z~2 structures

angular size. (5' ↔ 2.5Mpc) Method principle: Detect excess emission at 545 GHz. → 2151 candidates (Planck list of high-z sources)

  • z~2 and SFR ~ 30 000 M⊙

.yr-1 from MBB fits.

Color lines : MBB, β = 1.5, T=30K Planck Intermediate Paper, XXXIX (submitted)

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2/ Searching for z~2 structures with Planck and Herschel

  • 228 candidates followed up with

Herschel/SPIRE

  • Only 4 galactic cirrus
  • Large overdensities of SPIRE red

sources associated with Planck. (50% sample >10σ ; S350μm /S250μm > 0.7 ;

S500μm /S350μm > 0.6)

  • SFR ~ 700 M⊙

.yr-1 per source. Total compatible with Planck

  • Photo-z ~ 2 (compatible with Planck)

Planck Intermediate Paper XXVII

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2/ Searching for z~2 structures with Planck and Herschel

  • 232 candidates followed up with

Herschel/SPIRE

  • Only 4 galactic cirrus
  • Large overdensities of SPIRE red

sources associated with Planck. (50% sample >10σ ; S350μm /S250μm > 0.7 ;

S500μm /S350μm > 0.6)

  • SFR ~ 700 M⊙

.yr-1 per source. Total compatible with Planck

  • Photo-z ~ 2 (compatible with Planck)

Planck Intermediate Paper XXVII White : Planck source 50% emission contour Yellow : Red sources overdensity contours (>2 σ)

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2/ Searching for z~2 structures with Planck and Herschel

  • 232 candidates followed up with

Herschel/SPIRE

  • Only 4 galactic cirrus
  • Large overdensities of SPIRE red

sources associated with Planck. (50% sample >10σ ; S350μm /S250μm > 0.7 ;

S500μm /S350μm > 0.6)

  • SFR ~ 700 M⊙

.yr-1 per source. Total compatible with Planck

  • Photo-z ~ 2 (compatible with Planck)

Planck Intermediate Paper XXVII White : Planck source 50% emission contour Yellow : Red sources overdensity contours (>2 σ)

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2/ Searching for z~2 structures with Planck and Herschel

  • 228 candidates followed up with

Herschel/SPIRE

  • Only 4 galactic cirrus
  • Large overdensities of SPIRE red

sources associated with Planck. (50% sample >10σ ; S350μm /S250μm > 0.7 ;

S500μm /S350μm > 0.6)

  • SFR ~ 700 M⊙

.yr-1 per source. Total compatible with Planck

  • Photo-z ~ 2 (compatible with Planck)

Planck Intermediate Paper XXVII

N 0 1 2 3 4 5 Redshift z

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2/ Searching for z~2 structures with Planck and Herschel

  • 228 candidates followed up with

Herschel/SPIRE

  • Only 4 galactic cirrus
  • Large overdensities of SPIRE red

sources associated with Planck. (50% sample >10σ ; S350μm /S250μm > 0.7 ;

S500μm /S350μm > 0.6)

  • SFR ~ 700 M⊙

.yr-1 per source. Total compatible with Planck

  • Photo-z ~ 2 (compatible with Planck)

Planck Intermediate Paper XXVII

35K 25K 0 500 1000 1500 2000 SFR per source (M⊙ .yr-1) N

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3/ SPHerIC : Spitzer Planck Herschel Infrared Clusters

2 programs (GO9, GO11), 70h of observations, 90 candidates followed-up.

Planck (PHZ): 2151 candidates Herschel : 228 candidates

SPHerIC: 84 candidates

30' x 30'

353, 545, 857 GHz 250, 350, 500 μm 3.6, 4.5 μm ~5' ~20'' ~2'' Densité de flux (log) 100 101 102 103 λ (log) IRAC bands HFI & SPIRE bands SF galaxy z~2

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3/ Searching for structures with Spitzer

  • Color-cut selects high-z galaxies :

[3.6]-[4.5]>-0.1 → z>1.3 (Papovich, 2008, ApJ, 676:206)

SPHerIC : Search for overdensities of such sources around SPIRE sources (biased toward intense star-formation)

  • Search for structures as overdensities of such sources : hundreds of candidates.

e.g. Rettura et al., 2014, ApJ, 797:109 ; Muzzin et al. 2013, ApJ, 767:39 ; Wylezalek, 2013 – ApJ, 769:79.

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3/ SPHerIC

26 red sources.arcmin-

White circle: radius 1', centered on SPIRE emission FoV = 2.4' x 2.4' Grey/black line : SPIRE Emission contour (3 σ) (250/350 μm) Dashed colored lines : Overdensity contours 2.5, 3... 4.5 σ Red/Blue crosses : Red/Blue IRAC sources

From SPIRE : z~2, SFR ~ 700 M⊙ .yr-1

  • Calculate source density in 1'

radius circle centered on the brightest red SPIRE source.

  • Corresponds to overdensity of red

IRAC sources ?

  • How many IRAC sources are

responsible for the SPIRE emission ?

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μ+3σ

3/ SPHerIC

ΣSpUDS + 3σSpUDS ΣSpUDS Random 1' radius circles in SpUDS. SpUDs : control field, ~ 1 deg2

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3/ SPHerIC

ΣSpUDS + 3σSpUDS ΣSpUDS Wylezalek, 2013 – ApJ, 769:79. CARLA : Clusters Around Radio-Loud AGN. Wylezalek, 2014 – ApJ, 786:717. 27% are 3σ

  • verdense
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3/ SPHerIC

ΣSpUDS + 3σSpUDS ΣSpUDS 76% are 3σ

  • verdense !
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3/ SPHerIC : differential radial density profiles

Mean density SpUDS

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3/ SPHerIC : differential radial density profiles

  • SPIRE emission

associated to IRAC red sources overdensity

  • Large scale
  • verdensity

Mean density SpUDS

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3/ SPHerIC

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3/ SPHerIC : Color-Magnitude Diagrams.

55% fields with dispersion < 0.15 and median >0.1

Blue : 1 σ dispersion ; Black line : median ; black points : sources at r<1' from SPIRE emission.

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3/SPHerIC : Photometric redshift estimation

IRAC Color = Redshift estimator Photometric Redshift From COSMOS photometric data. Couleur = Nb galaxies [ 3 . 6 ]

  • [

4 . 5 ] Redshift

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3/ SPHerIC : Photometric redshift estimation

From median color sources r<1' from SPIRE source, [4.5]<22.

Photometric redshifts

Grayed : z>1.7 (plateau [3.6]-[4.5] vs. z)

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3/SPHerIC : Photometric redshift estimation

Photometric redshifts

Grayed : z>1.7 (plateau [3.6]-[4.5] vs. z) Rettura et al., 2014, ApJ, 797:109 Clusters in the SSDF.

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4/ Millimeter Follow-up

SFR ~ 1700 M⊙ .yr-1 (SPIRE) z=2.153 EMIR/30m - IRAM Mmol = 2.6+/-0.5 1011 M⊙ Tdepletion, gaz ~ 108 years

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4/ Millimeter Follow-up

SFR ~ 1700 M⊙ .yr-1 (SPIRE) Δv = 800 km.s-1 ! (Preliminary !) z=2.153 z=2.161 EMIR/30m - IRAM Mmol = 2.6+/-0.5 1011 M⊙ Tdepletion, gaz ~ 108 years

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4/ Millimeter Follow-up

SFR ~ 1700 M⊙ .yr-1 (SPIRE) Δv = 800 km.s-1 ! (Preliminary !) z=2.153 z=2.161 EMIR/30m - IRAM Mmol = 2.6+/-0.5 1011 M⊙ Tdepletion, gaz ~ 108 years 4 SPIRE sources in 3 Planck sources confirmed (z=1.32, 2.15, 2.15, 2.36 ). 1 awaiting confirmation (z=2.55). NOEMA data on z=2.36 candidate. ALMA data on another candidate. mm interferometry → identify star forming galaxies.

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Conclusions

  • Unique sample biased toward the most intense

star forming regions at z~2.

  • Spitzer reveals large overdensities of high-z

galaxies.

  • First spectroscopic redshifts arriving.
  • Need ground based NIR and HST-GRISM

spectroscopy