MACSJ0717.5+374 - PowerPoint PPT Presentation

≲ ≳ 近赤外線広視野撮像分光で探る 銀河と銀河間物質の共進化 MACSJ0717.5+374 Masami Ouchi 5 Credit:NASA, ESA and the HST Frontier Fields team (STScI) ICRR, U. Tokyo

Subaru Hyper Suprime-Cam (HSC) Survey 1/10 of the Early HSC Data More than 1 million galaxies at z=4-6 . Survey volume 100x higher than prev. obs. (1.4Gpc 3 ) → First step for statistical astronomy with early galaxies Pioneering optical wide-field (WF) imaging survey

Example: UV Luminosity Function Ono et al. (2018) Precision UV luminosity function (LF) → Bridging the LFs of galaxies and SDSS QSOs. • Subtraction of the AGN LFs • → LF excess: Not Schechter+Lensing, but double powerlaw. New indicator for bright-galaxy feedback (e.g. Ren+19) → PFS confirmation R. Bouwens (Leiden Univ.) “Your figures … will likely appear in many textbooks and • reviews for many years to come.”

Extending the HSC Optical WF Imaging to the Optical-NIR (Imaging) Spec Survey Subaru/Prime Focus Spec (PFS) WFIRST 2400 fibers FoV: Φ1.3deg 0.38-1.25 μm https://wfirst.gsfc.nasa.gov/index.html →Two important missing pictures in galaxy formation studies

1) Missing Picture of Galaxy Formation: Large-Scale Galaxy-IGM Interplay QSO/galaxy spec. studies Cantalupo+14 Westmoquette+14 Mass accretion CGM Reionization HI gas Galaxy LSS (ISM) (IGM) Metal, Radiation Metal enrichment→0.1%Zo SF, Outflow

Subaru/HSC H Lyα Intensity Mapping Cross-Correlation with the LAEs Lyα Emission HSC Results Kakuma et al. 2019 HSC: Largely extended Lyα emission with a size of 200-1000 comoving kpc • (about 5 times larger than virial radius of dark matter halo) →CGM to IGM → Physical origin? Associated dwarf galaxies or unknown Lyα sources? Comparison with z=5.7 and 6.6 results Inflow or outflow??

Metal in the CGM/IGM Fujimoto et al. 2019 10-kpc [CII]158μm halo at z=5.153-7.142 • C + gas extended 5x more than SFR regions (FIR/UV cont.) – → Outflow remnants (made in the first 1 Gyr) • Interestingly, comparable with Lya halo (cold gas?) Simulations do not explain the halo • Missing physical pic. in model → importance of cold-mode outflow?

Revealing the CGM/IGM Metal and Ion State By Intensity Mapping WFIRST NIR Grism Spectra • Ha: z=0.2-1.9 (cf. z=0.2-0.4 for HSC) • [OII]3727: z=1.1-4.2 (cf. z=1.2-1.4 for HSC) → Need WFIRST feasibility studies with these HSC res. (before WFIRST; PRIME NIR NB?; Suzuki san’s talk) Hayashi+18 Extending the hydrogen Lya study to Ha, OIII, OII lines with the Subaru/HSC • data with Hayashi+18’s low-z emitters (Sugahara+) – Fluorescence vs. scattering for hydrogen (via Ha/Lya ratio) – Metal distribution and ionization status (via OII intensity and OIII/OII ratio)

Combining the PFS Hydrogen (HI) Tomography Map Mukae et al. in prep. Mammoth-1 (QSO2) z=2.3 Combining PFS HI Map with the WFIRST Spec Map HI (PFS) vs. HII/OII/OIII (WFIRST) [+FUV abs (PFS)] HI poor → Need WFIRST feasibility studies cosmic avg. ? • Lyα Blob (MAMMOTH-1) resides in the regular QSO environment • QSO proximity zone HI rich – except for one QSO (young QSO?)

PFS Spectroscopy at 〜 1μm First Detection of EoR HI 21cm Signal Anti-correlation Correlation Galaxies (LAEs) in Galaxies (LAEs) And HI gas(21cm) ionized bubbles (no 21cm) Reionization (simulations) Kubota et al. 2018 3D distribution of LAEs w z(Lyα)→EoR signposts • – LAE data: HSC→ PFS spec. Galaxies (blue dots),ionized bubbles (orange) – 21 cm data: SKA-1 (2023-) (Iliev+06) LAE-21cm cross-correlation • – EoR HI 21cm signal (>5σ detection) – Turnover scale→ionized bubble (3-5σ level)

2) Missing Picture of Galaxy Formation: First Generation Stars/Star Clusters Initial fluctuation Galaxies time • First generation stars/star clusters → Missing piece • Very low-mass system in the early universe

Identifying First Star Clusters Kikuchihara et al. (2019) Very rare (short event x high μ) → Need wide-field searches z 〜 6-7 z 〜 8 z 〜 9 Ishigaki et al. (2015) • Gravitational Lensing + Ultra Deep HST/Spitzer Imaging (HFF) → Early Globular Cluster Candidates (r e ~30pc M * ~10 6 Mo)

WFIRST Search for First Stars/Star-Clusters z>6 M*=2x10 4 Mo μ>300 10 pc Surace et al. (2019 ） Zackrisson et al. (2015 ） • WFIRST wide-field deep NIR imaging • Candidates→ Deep follow-up NIR spec. w TMT (e.g. HeII1640) – Challenges : Candidate selection and spec. conf. (cf. HMXB)

Roles of WFIRST and the Other Telescopes UV LF (expected) LUVOIR (15.1 m) JWST(6.5m) z 〜 10 WFIRST(2.4m) Kikuchihara+ for request of J. O’Meara &M. Postman JWST (+w cluster lensing) will identify early massive galaxies m>-20 • WFIRST: Most massive galaxies and high-μ lensed low mass galaxies m<-20 • LUVOIR: Early stellar clusters (m~ -12 mag) with no lensing magnification •

Summary • Next generation NIR WF imaging & spec. w PFS+WFIRST Extending the previous/on-going studies – Optical WF imaging (HSC) and NIR/Submm obs (HST+ALMA) 1) Galaxy-IGM interplay – HII and metal revealed by intensity mapping (WFIRST spec.) x HI Tomography x FUV metal abs. (PFS spec.) – EoR HI detection and ionized bubble (PFS spec.) x SKA-1 HI 21cm data for cross-correlation 2) First-generation stars/star clusters – Wide-field NIR imaging search for high-μ first star[cluster] (WFIRST) – Roles of WFIRST and the other telescopes