SWIMS-18, PFS 2 , and ULTIMATE-K Tadayuki Kodama (Tohoku Univ.) - - PowerPoint PPT Presentation

A galaxy cluster RXJ0152 at z=0.83 (Subaru/Suprime-Cam)

Tadayuki Kodama (Tohoku Univ.)

HSC-HSC/PFS-PFS, Mahalo-Subaru, SWIMS-18, and ULTIMATE-Subaru teams

SWIMS-18, PFS2, and ULTIMATE-K

NIR Wide-Field Workshop NAOJ Mitaka2019/7/1-2

What accelerates/quenches star formation since z~5 ?

Redshift (z) Cosmic age (Gyr) 14 12 10 8 6 4 2 0

Star formation rate density

First galaxies Reionization

Morphology of galaxies established Formation of galaxy clusters Formation of the Earth

Quenching Peaking Accelerating

SWIMS-18, ULTIMATE-K HSC2, PFS2

Quenching mechanisms

SDSS (z~0), Peng et al. (2010)

Mass and Environmental Q.

When does this relation first appear? How does it evolve with cosmic time? What are the relative importance of the above physical processes as a func. of time, mass and environ.?

Overdensity Mass Red fraction Mass: AGN Q., Halo Q., Morphological Q. Environ.: RP strip., Tidal strip., Mergers

CL0016 cluster (z=0.55) (Tanaka, M. et al. 2009)

PFS Millenium Simulation

(Springel et al. 2005)

~1,200 redshifts from spectroscopy red are cluster members, while blue are non-members LSS around the richest cluster at z=0.55

HSC, PFS, ULTIMATE, SWIMS are powerful to probe LSSs

Suprime-Cam 7-pointings

1.3= 75 Mpc (z=1), 100 Mpc (z=1.5), 118 Mpc (z=2) in co-moving HSC ULTIMATE SWIMS

• 6 Narrow-Band Filters (NBF)

SFR limited sample and AGNs at z=0.9, 1.5, 2.3, 3.3. Hα & [OIII] dual emitters with pair NBFs.

• 9 Medium-Band Filters (MBF)

Stellar mass limited sample at 1<z<5 with improved phot-z (Δz/(1+z) ~ 0.01).

• 3 Broad-Band Filters (BBF)

à Tracking the cosmic histories of “mass assembly” and “star formation/AGN activities” back to z~3-5.

SWIMS-18

Super multi-λ (NIR) imaging survey of the Cosmic Noon

• ver a 1-deg2 unbiased field + some high density regions
• n Subaru (8.2m; 2018-2022) and TAO (6.5m; 2022-)

SWIMS is a new wide-field, two-band-simultaneous NIR camera and spectrograph for TAO 6.5m telescope in Chile, and saw the first light at Subaru in Hawaii in 2018.

Dual emitters ([OIII] & Hα) with 4 pair NBFs à Redshift identification, SFR, Ionization states

SFR-limited sample at z=0.9, 1.5, 2.3, and 3.3

4C65.22(z=1.52) 4C65.22(z=1.52)

Six Narrow-band filters (NBF)

cluster field cluster

[OIII]/Hα ratio à Ionization State

Shimakawa et al. (2014b) SDSS

High-z > Low-z

(z~2)

(HβàHα conversion) (stacked)

Both higher sSFR and lower metallicity are contributing to much higher ionization states

• f high-z SF galaxies.

(Kewley et al. 2013)

SWIMS-18 can do this only by imaging !

• g ([OIII]/Hα)

(Dust extinction will be corrected with SED)

BB filters λ λc FWHM (µm) (µm) (µm) J 1.17–1.33 1.25 0.16 H 1.48–1.78 1.63 0.30 Ks 1.99–2.30 2.15 0.30

Will open a new window to 4<z<5 with K1,K2,K3 ! M*-limited sample of galaxies up to z~5

Nine Medium-band filters (MBF)

SWIMS-18 MBFs

J1,J2,J3,Hs,Hl, Ks ZFOURGE (Magellan)

Improved measurements of phot-z and SED-based Av.

Massive quiescent galaxies with strong Balmer abs. lines at z~4

ZF-COSMOS-20115 at z=3.717, 1.51011M,

Keck/MOSFIRE: 4 and 7 hours in the H and K band, respectively.

We can extend this survey to z~5 with deep MB imaging with SWIMS-18/ULTIMATE The existence of such massive high-z monsters, and/or their old stellar populations, can put strong constraints on cosmology & galaxy formation theory.

K(AB) = 22.4

Glazebrook et al. (2017; Nature) age ~ 0.7Gyr, SF < 0.25Gyr

See also Schreiber+’18 for more (24) samples

Hunting High-z Monsters !

We will get to 23.8-24.1 AB in 1 hour exposure (5σ) each for K1, K2, and K3. à 1 deg^2 is 7x7 pointings with SWIMS/TAO in 15-30 nights (depending on the # of detectors). 15 high-z (z~4) quiescent galaxies in Straatman+ with K<24 in 360 arcmin^2. à 150 in 1 deg^2. Double that for massive SFGs. ~40 really bright ones like ZF-20115! If we assume evolution from z=4 to z=5,

• ie. extrapolation of Straatman+,

this could be a factor of 3 less.

Some numbers:

Straatman et al. (2014), ZFourge survey

GOLDRUSH

(g-dropouts) 179 proto-clusters at z~3.8 over 121 deg2 using HSC-SSP-Wide

Toshikawa et al. (2017), Onoue et al. (2017)

Proto-clusters at 2<z<6 with LBGs over 1,400 deg2 (HSC-SSP-W)

ULTIMATE will provide rest-frame optical view of these proto-clusters (e.g. M*, SFR)

• For compact QGs ⇒ Sensitivity gain (~2x)!
• For extended SFGs ⇒ Anatomy (bulge & clumps)!

0.2” ⇔ 1.5kpc at 1<z<3 (~ 1/3-1/2 Re for SFGs)

w/ GLAO (~0.2”) Seeing limited (~0.5”) A star-forming galaxy at z~2

ULTIMATE-Subaru

Why 0.2” ?

Suzuki et al. (2019)

Spatially resolved M* and SFR distributions at z~2 w/AO

High-mass, M* High-mass, SFR Low-mass, M* Low-mass, SFR *Inside-out SF/quenching rather than compaction in massive galaxies? *No clear environmental dependence in radial profiles? Stacked images (Ks and NB) with FWHM=0.15-0.25” by IRCS+AO/Subaru

Radial profiles M* SFR sSFR

Galaxy Anatomy with Narrow-Band AO imaging with Subaru (GANBA)

1arcmin2 (IRCS) à 200 arcmin2 (ULTIMATE)

• 0.75 mag deeper (point-source), 8 times wider FoV than the

current instrument MOIRCS, and 0.2” spatial resolution.

• NB survey with 0.2” seeing (Extension of MAHALO/GANBA)

Propagation/quenching of SF in galaxies with Hα,[OIII] map for 1,000s of SFGs at 2<z<3.7 with a 1.6kpc resolution.

• MB survey (K1, K2, K3 (+Ks)) (Extension of SWIMS-18)

10 hrs exp. (26mag; 5σ)/FoV/band = 640hrs/deg2 for 4 filters Mass assembly history back to z~5 with Balmer break galaxies at 4<z<5 of ~4,000 / deg2 (?)

• WFIRST/EUCLID only up to 2µm.

JWST has much narrower FoV (2.2’2.2’2 = 1/20 ULTIMATE).

ULTIMATE-K survey

NB/MB/Ks wide-field imaging with GLAO+WFI (14’) over 2deg2

Mass assembly history of galaxies: Stellar mass functions back to z~5

Muzzin et al. (2013)

100K galaxies over a 1.62 deg2 field down to Ks=23.4 (AB)

Down to 1 (2) x 1010 M back to z~4 (5) with ULTIMATE K1-K3 imaging (5hr/band)

ULTRA-VISTA (COSMOS)

? ?

z=4 z=4 z=5 ? z=5 ?

van der Wel et al. (2014) Star forming Quiescent

Size and profile evolution of massive galaxies back to z~5

0.2” diameter at K (ULTIMATE) à r~0.75kpc at z=2-3

z~5

Mstars= 3 1011 M (z=0)

Massive galaxies’ radial profiles

r=0.1” van Dokkum et al. (2010) natural seeing (0.5” in diameter)

• Mass limited sample (>109 M) back to z~10

Phot-z with WISH (2-5µm) + WFIRST (1-2µm) + HSC (<1µm)

• SFR limited sample back to z~7

Hα/[OIII] emitters with NB filters or grism spec. (2-5µm) à “Mass assembly history” on LSS-galaxy scales all the way from z=10 to the present-day.

Now dedicated to 2~5μm, and coordinated with WFIRST (1~2μm)!? WISH was a planned 1.5-m class space telescope mission for 1-5μm with a FoV of 0.24 sq. deg. (PI. Yamada T. [JAXA]) Highly complementary to JWST in FoV !

(Long)

• II

WSECOND

JAXA small-class mission (~2030)? 1.2m?

WISH Ultra Deep Survey (UDS) Mstars = 108 M (z=1) ~ 109 M (z=8)

WISH can detect building blocks of galaxies out to z~8

Based on Kodama et al.’s (1999) model 10-20 hours/band

109 M 1010 M

green valley blue cloud red sequence

Two galaxy populations Hybrid cluster finder

Hyb ybrid Sea earc rch f for r Clu lusters with HSC

red sequence blue cloud HSC2 is a large, systematic cluster survey with little selection bias to z~1.7 The conventional red seq. technique alone will bias your sample of galaxy clusters. HSC-SSP (Deep and Ultra-Deep layers; 27 deg2) (narrow-band) (broad-band color)

Red sequence galaxies at 0.8<z<0.9

Yamamoto, N., TK, et al., in prep.

Panoramic Large scale structures!

[OIII] line emitters at 0.82<z<0.86

Blue peaks do not necessarily host red seq. galaxies.

Yamamoto, N., TK, et al., in prep.

Balmer absorption lines are excellent tracers for recently-quenched/PSB galaxies (e.g., E+A, k+a, a+k…)

Post-starburst galaxies (E+A/k+a)

Key targets: Recently-quenched galaxies in/around clusters and with various M*

PFS-SSP may not sample galaxies in high density regions very efficiently. We aim to go for a separate, dedicated program to follow-up the HSC selected clusters (e.g. intensive program~40nights). We can access to these lines back to z~2 with PFS and to z~4.5 with ULTIMATE Constraints on the recent star formation histories (quenching time-scale, and w/ or w/o starburst).

Pano anoram amic Fol

• llow
• w-up

up Spect ctrosco scopy with PFS (PFS2)

We can access to these lines to z=1.5 (Mg/Fe) ~ z=2 (Hδ) with PFS and z=3.5-4.5 with ULTIMATE Couch & Sharples (1987) Simple truncation w/o starburst Truncation w/ starburst

Absorption line diagnostic of recently-quenched (PSB) galaxies

− to constrain the timescales of star-formation/quenching −

Balmer absorption lines (A-type stars) à timescale of quenching, existence of starburst

Kriek+ (2016)

Mg/Fe ratio à timescale of SF before quenching

[nm]

α enhancement à short timescale

z=2.1

• r D4000

Kewley+ (2015b)

Separation between ionization parameter (q) and metallicity (O/H)

[OIII]/Hβ vs. [NII]/[SII]

Emission line diagnostic of star forming galaxies

z<0.9 (z<1.5 for R23) with PFS and z<2.6 (3.8) with ULTIMATE

Fukagawa et al. (2016)

Z/Z

fgas

Chemical evolution models with in/out-flows η: mass loading factor a: accretion efficiency

We can put constraints on gaseous flows from chemical evolution, and explore their environmental and mass dependences. fgas can be obtained with ALMA

• to explore environmental depend. of metallicities due to gas inflow/outflows -

Summary

• HSC2 is now discovering 100s of new clusters at 0.4<z<1.7,

including young (blue), dual (red+blue) and old (red) clusters, and 1,000s of recently-quenched galaxies (or PSBs) across various environments and stellar masses.

• PFS2 will intensively follow-up HSC2 and characterize the

quenching processes as a function of mass and environment.

• SWIMS-18 and ULTIMATE-Subaru will search for massive

monsters and proto-clusters out to z~5 !

• ULTIMATE-Subaru will resolve and identify how the star

formation and quenching are propagated within galaxies.

• Is it OK if WISH is forever a wish?

à LoI to be led by A.Inoue !