VARIOUS COSMIC ENVIRONMENTS OF NORTHERN HEMISPHERE SKY

Transcription

1 IRAM/30m, NOEMA VARIOUS COSMIC ENVIRONMENTS OF NORTHERN HEMISPHERE SKY -FOR THE ANTICIPATED STUDIES USING NOEMA/IRAM- Minju Lee (PD) (Nagoya U. /NAOJ MPE from this November)

2 Contents 2

3 Formation of the Hubble sequence Kormendy & Ho 2013 environment time, metallicity, etc mass 3

4 Mass vs environment ( nature or nurture ) mass massive galaxies : red-and-dead and morphologically early-type environment S0+Es are abundant in denser regions Cappellari+16 Houghton+15 (revision of Dressler 1980) Need to understand both the dependence 4

5 GAS FOR TRACING SF ACTIVITY [1] FIELD STUDIES IN RECENT FIVE YEARS

6 Gas content Gas fraction Depletion time (SFE) Tacconi+17 z=1 z=1 z=0 z=3 z=0 z=3 increasing decreasing(increasing) 6

7 Gas kinematics Disks galaxies at high-z have higher velocity dispersion (disordered rotation) Turner+17 Wisnioski+15 Tight Wisnioski+15 connection to the evolution of gas content and kinematic properties 7

8 GAS FOR TRACING SF ACTIVITY [2] WHAT ABOUT GALAXIES IN HIGH-Z PROTOCLUSTERS?

9 Probing protoclusters in context Definition : progenitor of present-day clusters easy-definition in simulations but difficult, observationally z=1-3 : The peak formation epoch for galaxies and clusters By z~1, clusters already have quenched population comparable to local galaxies on the massive-end If galaxies are quenched, they might be preferentially located in the denser environment z>3 : Necessary to understand the formation mechanisms of progenitors of early-type galaxies Balogh+16 Chiang+17 Probing clusters and their progenitors is also important to give a constraint on cosmology 9

10 Why difficult? Bacall & Chen

11 Why difficult? Thus the number of protoclusters probed is very limited for high Chiang+2013 redshift 11

12 A case study protocluster 4C at z=2.5) color : SMGs discovered AzTEC/ASTE at 1.1 mm blue circles : HAEs By courtesy of K. Tadaki Radio galaxy 4C23.56 Overdensities of HAE near radio galaxy by narrow-band filter technique (Tanaka+11) Overlap with SMGs : dusty star formation? 12

13 A long history from AzTEC, to PdBI, and to ALMA AzTEC/ASTE 1.1 mm and PdBI observations at 1.8 mm (before ALMA era) 13

14 ALMA observations Band 3 (3 mm, CO(3-2)) & Band 6 (1.1 mm) Band 4 (2 mm, CO(4-3)) resolution ( x ) Cycle 1 (Band 6) 0.78x0.68 Cycle 2 (Band 3) 0.91x0.66 Cycle 3 (Band 4) 0.52x0.32 noise level mjy/beam Number of observed HAEs On-source /pointing ~ 4 min ~ 1 hr ~ 1.3 hr 0.17 mjy/beam (100 km/s) 0.14 mjy/beam (100 km/s) 14

15 Gas content Average gas fraction for the protocluster fgas~0.5 (tentatively large scatter, though limited number) Average gas fraction for the field from PHIBSS-I fgas~0.5 Lee+17 15

16 Comparing samples (gas content) Noble+17 16

17 Comparing samples (gas content) Stach+17 17

18 Comparing samples (gas content) Coogan+18 18

19 Would I use NOEMA for 4C23 protocluster? ~ from GENERAL/NOEMA-Phase-A.pdf 19

20 Don t worry! : Important learnings from the case study <INSUFFICIENT ABSOLUTE NUMBER!> Why not NOEMA/ IRAM 30-m for the high-δ northern sky? NOTE, AGAIN THE NUMBER DENSITY OF MASSIVE HALO IS SMALL 20

21 CANDIDATE (PROTO)CLUSTERS IN NORTHERN HEMISPHERE

22 z>3 Candidate 1. HDF-N at z=5.183 Barger+15 Walter+12 +JWST and Hughes+98 22

23 z>1 Candidate 2. Herschel & Planck candidates with wideband features in NOEMA Greenslade+18 23

24 First Herschel & Planck cluster candidates Clements+14 24

25 Greenslade+18 Indeed roughly ~1/2 is missed if we only investigate candidates in southern hemispheres (~10-20% if δ>40) Or, it could be more are missed, e.g., Planck intermediate results. XXVI (2015A&A...582A..29P) 25

26 z~1-3 or perhaps, below Candidate 3. Planck and NIKA2/IRAM for SZ-clusters 26

27 Candidate 4. Protoclusters found by HSC-SSP/ Subaru HSC-D R.A. HSC-W DEC HSC-D/UD Galactic Extinction E(B-V) 27

28 VOIDS IN NORTHERN SKY

29 Voids at lower redshifts See also Fraser-McKelvie+16 for IFU 29

30 Conclusions Larger number in norther sky with spec-z ESA and the Planck Collaboration 30

31 THANK YOU!