NIR Wide-Field Workshop � NAOJ Mitaka � 2019/7/1-2 � SWIMS-18, PFS 2 , and ULTIMATE-K Tadayuki Kodama (Tohoku Univ.) HSC-HSC/PFS-PFS, Mahalo-Subaru, SWIMS-18, and ULTIMATE-Subaru teams A galaxy cluster RXJ0152 at z=0.83 (Subaru/Suprime-Cam)
What accelerates/quenches star formation since z~5 ? SWIMS-18, ULTIMATE-K HSC 2 , PFS 2 Redshift (z) Star formation rate density Peaking Quenching Accelerating First galaxies Morphology of galaxies established Formation of galaxy clusters Reionization Formation of the Earth 14 12 10 8 6 4 2 0 Cosmic age (Gyr)
Red fraction Quenching mechanisms Mass and Environmental Q. Mass: AGN Q., Halo Q., Morphological Q. Overdensity Environ.: RP strip., Tidal strip., Mergers 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.? Mass SDSS (z~0), Peng et al. (2010)
HSC, PFS, ULTIMATE, SWIMS are powerful to probe LSSs 1.3 � = 75 Mpc (z=1), 100 Mpc (z=1.5), 118 Mpc (z=2) in co-moving CL0016 cluster (z=0.55) Millenium Simulation (Tanaka, M. et al. 2009) (Springel et al. 2005) Suprime-Cam 7-pointings ULTIMATE SWIMS PFS HSC LSS around the richest cluster at z=0.55 ~1,200 redshifts from spectroscopy red are cluster members, while blue are non-members
S W I M S-18 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. Super multi- λ (NIR) imaging survey of the Cosmic Noon over a 1-deg 2 unbiased field + some high density regions on Subaru (8.2m; 2018-2022) and TAO (6.5m; 2022-) • 6 Narrow-Band Filters (NBF) SFR limited sample and AGNs at z=0.9, 1.5, 2.3, 3.3. H α & [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.
Six Narrow-band filters (NBF) SFR-limited sample at z=0.9, 1.5, 2.3, and 3.3 4C65.22(z=1.52) 4C65.22(z=1.52) Dual emitters ([OIII] & Hα) with 4 pair NBFs à Redshift identification, SFR, Ionization states
[OIII]/H α ratio à Ionization State SWIMS-18 can do this only by imaging ! High-z > Low-z Both higher sSFR and � og ([OIII]/Hα) lower metallicity are contributing to much higher ionization states of high-z SF galaxies. (Kewley et al. 2013) SDSS cluster (stacked) (Dust extinction will be (z~2) cluster corrected with SED) (Hβ à Hα conversion) field Shimakawa et al. (2014b)
Nine Medium-band filters (MBF) M*-limited sample of galaxies up to z~5 BB filters FWHM λ λ c ( µ m) ( µ m) ( µ m) J 1.17–1.33 1.25 0.16 H 1.48–1.78 1.63 0.30 K s 1.99–2.30 2.15 0.30 Improved measurements of phot-z and SED-based Av. Will open a new window to 4<z<5 with K1,K2,K3 ! J1,J2,J3,Hs,Hl, Ks ZFOURGE (Magellan) SWIMS-18 MBFs
Hunting High-z Monsters ! Massive quiescent galaxies with strong Balmer abs. lines at z~4 ZF-COSMOS-20115 at z=3.717, 1.5 � 10 11 M � , K(AB) = 22.4 Glazebrook et al. (2017; Nature) See also Schreiber+’18 for more (24) samples age ~ 0.7Gyr, � SF < 0.25Gyr 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.
Some numbers: 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. Straatman et al. (2014), ZFourge survey
GOLDRUSH Proto-clusters at 2<z<6 with LBGs over 1,400 deg 2 (HSC-SSP-W) 179 proto-clusters at z~3.8 over 121 deg 2 using HSC-SSP-Wide ( g -dropouts) Toshikawa et al. (2017), Onoue et al. (2017) ULTIMATE will provide rest-frame optical view of these proto-clusters (e.g. M*, SFR)
ULTIMATE-Subaru Why 0.2” ? 0.2” ⇔ 1.5kpc at 1<z<3 (~ 1/3-1/2 Re for SFGs) For compact QGs ⇒ Sensitivity gain (~2x)! • For extended SFGs ⇒ Anatomy (bulge & clumps)! • A star-forming galaxy at z~2 Seeing limited (~0.5”) w/ GLAO (~0.2”)
G alaxy A natomy with N arrow- B and A O imaging with Subaru ( GANBA ) Spatially resolved M* and SFR distributions at z~2 w/AO Stacked images (Ks and NB) with FWHM=0.15-0.25” by IRCS+AO/Subaru Low-mass, M* High-mass, M* High-mass, SFR Low-mass, SFR Suzuki et al. (2019) Radial profiles sSFR SFR M* 1arcmin 2 (IRCS) à *Inside-out SF/quenching rather than compaction in massive galaxies? 200 arcmin 2 (ULTIMATE) *No clear environmental dependence in radial profiles?
ULTIMATE-K survey NB/MB/K s wide-field imaging with GLAO+WFI (14’) over 2deg 2 • 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 H α ,[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; 5 σ )/FoV/band = 640hrs/deg 2 for 4 filters Mass assembly history back to z~5 with Balmer break galaxies at 4<z<5 of ~4,000 / deg 2 (?) • WFIRST/EUCLID only up to 2µm. JWST has much narrower FoV ( 2.2’ � 2.2’ � 2 = 1/20 ULTIMATE ).
Mass assembly history of galaxies: Stellar mass functions back to z~5 ULTRA-VISTA (COSMOS) Muzzin et al. (2013) 100K galaxies over a 1.62 deg 2 field down to K s =23.4 (AB) z=4 ? z=4 ? z=5 ? z=5 ? Down to 1 (2) x 10 10 M � back to z~4 (5) with ULTIMATE K1-K3 imaging (5hr/band)
Size and profile evolution of massive galaxies back to z~5 van Dokkum et al. (2010) van der Wel et al. (2014) M stars = 3 � 10 11 M � (z=0) Massive galaxies’ radial profiles z~5 Star forming natural seeing Quiescent (0.5” in diameter) r=0.1” 0.2” diameter at K (ULTIMATE) à r~0.75kpc at z=2-3
(Long) -II WSECOND 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]) Now dedicated to 2~5μm, and coordinated with WFIRST (1~2μm)!? JAXA small-class mission (~2030)? 1.2m? Highly complementary to JWST in FoV ! Mass limited sample ( > 10 9 M � ) back to z~10 • Phot-z with WISH (2-5µm) + WFIRST (1-2µm) + HSC (<1µm) • SFR limited sample back to z~7 H α /[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.
WISH can detect building blocks of galaxies out to z~8 WISH Ultra Deep Survey (UDS) M stars = 10 8 M � (z=1) ~ 10 9 M � (z=8) 10 10 M � 10 9 M � 10-20 hours/band Based on Kodama et al.’s (1999) model
Hyb ybrid Sea earc rch f for r Clu lusters with HSC HSC-SSP (Deep and Ultra-Deep layers; 27 deg 2 ) Hybrid cluster finder Two galaxy populations blue cloud (narrow-band) red sequence green valley blue cloud red sequence (broad-band color) The conventional red seq. technique alone will bias your sample of galaxy clusters. HSC 2 is a large, systematic cluster survey with little selection bias to z~1.7
Red sequence galaxies at 0.8<z<0.9 Panoramic Large scale structures! Yamamoto, N., TK, et al., in prep.
[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.
Pano anoram amic Fol ollow ow-up up Spect ctrosco scopy with PFS ( PFS 2 ) Key targets: Recently-quenched galaxies in/around clusters and with various M* Post-starburst galaxies (E+A/k+a) Balmer absorption lines are excellent tracers for recently-quenched/PSB galaxies (e.g., E+A, k+a, a+k…) 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). 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).
Absorption line diagnostic of recently-quenched (PSB) galaxies − to constrain the timescales of star-formation/quenching − Balmer absorption lines (A-type stars) Mg/Fe ratio à timescale of quenching, existence of starburst à timescale of SF before quenching Kriek+ (2016) Couch & Sharples (1987) Truncation w/ starburst Simple truncation w/o starburst z=2.1 α enhancement à short timescale or D4000 [nm] 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
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