Connecting SFG and DH at z=4-7 by the Clustering
Analysis of Subaru/HSC & Hubble Data	Yuichi Harikane (The University of Tokyo)
Masami Ouchi, Yoshiaki Ono, Takatoshi Shibuya+ Subaru/HSC Survey teamOutline	• Introduction of SHMR
• Hubble & HSC Data and LBG Selection• Clustering Analysis with HOD Model• Results of Halo Mass, SHMR, BCE• Future Prospect with HSC	

Galaxy-Dark Matter Connection: SHMR	• Dark matter halo is important in galaxy formation.
– Gas cooling is efficient in 1010-1013 Msun halo.
– SN and AGN feedback in low and high mass halo.	

Gas coolingGas heating
and outflow

Star formation
GalaxyDark matter halo

Galaxy-Dark Matter Connection: SHMR	
• Stellar-to-halo mass ratio (SHMR=M*/Mh) canprobe galaxy-dark matter connection.
• SHMR @ z>2 is not investigated by galaxyclustering.	

Feedback	  from	  AGN?	  

Evolu;on	  Eﬃciently	  Star	  Formed	  Leauthaud+12	  Foucaud+!0
Behroozi+13b

Our Strategy	

Hubble	   Subaru/HSC	  h7p://www.spacetelescope.org/	 h7p://subarutelescope.org/	Our Strategy	

LARGE sample covering WIDE luminosity range	Clustering	  Analysis	  w/	  HOD	SHMR evolution	Data & Sample Selection	
Lyman break galaxy (LBG) selection @z~4, 5, 6, 7	
UDF12	 AEGIS	COSMOS	 UDS	
N=45

N=416

N=403

N=346
z~5 selection	

GN-Deep	
GN-Wide	
GS-Deep	
GS-Wide	
N=1966 N=1071

N=1552 N=594

HFF-A2744P	
HFF-M0416P	 HSC-XMM	
N=45

N=94

N=440

Total of ~7000 LBGs @z=4-7 !!	

Ono,	  Y.	  in	  prep

Clustering Analysis w/ HOD Model	
Calculate Angular Correlation Function in Each Sample Bin	z~5 mUV<25.0
Subaru/HSC	z~4 mUV<27.6
Hubble 	z~5 mUV<27.2Hubble	

z~6 mUV<27.4Hubble	

z~7 mUV<28.4Hubble	

Clustering Analysis w/ HOD Model	
Calculate Angular Correlation Function in Each Sample Bin	z~4 mUV<27.6Hubble 	

Fit w/ Halo Occupation Distribution (HOD) Model Prediction	

Estimate Dark Halo Mass 	Results: Dark Halo Mass	• Dark halo mass is consistent with previous
clustering results (Lee+06, Hamana+04).	
● z~4 (this work)● z~5 (this work)○ z~5 (this work; HSC)
● z~6 (this work)● z~7 (this work)▲ z~4 (Lee+06)▲ z~5 (Lee+06)▼ z~4 (Hamana+04)▼ z~5 (Hamana+04)*Hamana+04 provides no error
about Mh in paper

Results: SHMR	
ー z~0 (AM; Behroozi+13)● z~4 (this work)● z~5 (this work)○ z~5 (this work; HSC)
● z~6 (this work)● z~7 (this work)--- z~4 (AM; Behroozi+13)--- z~5 (AM; Behroozi+13)--- z~6 (AM; Behroozi+13)--- z~7 (AM; Behroozi+13)• Decrease from z~0 to z~4.
• Increase from z~4 to z~7 ?
• SHMR evolution confirmed by clustering.

Results: Baryon Conversion Efficiency	
Baryon conversion efficiency (BCE) =is calculated by N-body simulation results(we use the formulation in Behroozi+13).
● z~4 (this study)● z~5 (this study)○ z~5 (this study HSC)
● z~6 (this study)● z~7 (this study)

Results: Baryon Conversion Efficiency	
Baryon conversion efficiency (BCE) =is calculated by N-body simulation results(we use the formulation in Behroozi+13).

Increase up to 1012 Msun @z~4
due to less SN feedback	● z~4 (this study)● z~5 (this study)○ z~5 (this study HSC)
● z~6 (this study)● z~7 (this study)▼ z~4 (AM; Behroozi+13)▼ z~5 (AM; Behroozi+13)▼ z~6 (AM; Behroozi+13)▼ z~7 (AM; Behroozi+13)

Future Prospects	
HSC	

20000000
15000000h7p://subarutelescope.org/	

~20 Million LBGs
@ z=4-7	

Full HSC	

10000000x2000	

5000000
0

Present

Full HSC

Present	z~4	Summary	The SHMR evolution is confirmed by the clustering.
SHMR decreases @z~0→4 and increases @z~4→7.

BCE increases with increasing Mh up to 1012 Msun z~4.
Star formation is more efficient at higher halo mass due toless SN feedback.

Evolu;on	  Increase up to 1012 Msun @z~4