MACSJ0717.5+374 - - PowerPoint PPT Presentation

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MACSJ0717.5+374 - - PowerPoint PPT Presentation

Dec 16, 2023 504 likes •675 views

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

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Credit:NASA, ESA and the HST Frontier Fields team (STScI)

Masami Ouchi ICRR, U. Tokyo

MACSJ0717.5+374 5

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

≲ ≳

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Subaru Hyper Suprime-Cam (HSC) Survey

More than 1 million galaxies at z=4-6 . Survey volume 100x higher than prev. obs. (1.4Gpc3) → First step for statistical astronomy with early galaxies Pioneering optical wide-field (WF) imaging survey 1/10 of the Early HSC Data

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Example: UV Luminosity Function

  • 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.” Ono et al. (2018)

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→Two important missing pictures in galaxy formation studies

WFIRST

https://wfirst.gsfc.nasa.gov/index.html

2400 fibers FoV: Φ1.3deg 0.38-1.25 μm

Extending the HSC Optical WF Imaging to the Optical-NIR (Imaging) Spec Survey

Subaru/Prime Focus Spec (PFS)

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1) Missing Picture of Galaxy Formation: Large-Scale Galaxy-IGM Interplay

Cantalupo+14 Westmoquette+14

Galaxy (ISM) LSS (IGM)

CGM

HI gas Metal, Radiation

Mass accretion SF, Outflow Metal enrichment→0.1%Zo Reionization

QSO/galaxy spec. studies

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Subaru/HSC H Lyα Intensity Mapping Cross-Correlation with the LAEs

  • 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?

Lyα Emission HSC Results Comparison with z=5.7 and 6.6 results Inflow or outflow?? Kakuma et al. 2019

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Metal in the CGM/IGM

  • 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?

Fujimoto et al. 2019

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Revealing the CGM/IGM Metal and Ion State By Intensity Mapping

  • 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)

Hayashi+18

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)

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HI poor HI rich

  • Lyα Blob (MAMMOTH-1) resides

in the regular QSO environment

  • QSO proximity zone

– except for one QSO (young QSO?)

cosmic avg.? Mukae et al. in prep.

z=2.3

Combining the PFS Hydrogen (HI) Tomography Map

Mammoth-1 (QSO2)

Combining PFS HI Map with the WFIRST Spec Map HI (PFS) vs. HII/OII/OIII (WFIRST) [+FUV abs (PFS)] → Need WFIRST feasibility studies

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  • 3D distribution of LAEs w z(Lyα)→EoR signposts

– LAE data: HSC→ PFS spec. – 21 cm data: SKA-1 (2023-)

  • LAE-21cm cross-correlation

– EoR HI 21cm signal (>5σ detection) – Turnover scale→ionized bubble (3-5σ level)

Anti-correlation

Galaxies (LAEs) in ionized bubbles (no 21cm)

Correlation

Galaxies (LAEs) And HI gas(21cm) Galaxies (blue dots),ionized bubbles (orange) (Iliev+06)

Reionization (simulations)

PFS Spectroscopy at 〜1μm First Detection of EoR HI 21cm Signal

Kubota et al. 2018

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2) Missing Picture of Galaxy Formation: First Generation Stars/Star Clusters

  • First generation stars/star clusters → Missing piece
  • Very low-mass system in the early universe

time Initial fluctuation Galaxies

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Identifying First Star Clusters

  • Gravitational Lensing + Ultra Deep HST/Spitzer Imaging (HFF)

→ Early Globular Cluster Candidates (re~30pc M*~106Mo)

Kikuchihara et al. (2019) z〜6-7 z〜8 z〜9

Very rare (short event x high μ) → Need wide-field searches

Ishigaki et al. (2015)

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WFIRST Search for First Stars/Star-Clusters

  • 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)

Zackrisson et al. (2015） Surace et al. (2019） z>6 M*=2x104 Mo μ>300 10 pc

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JWST(6.5m) LUVOIR (15.1 m) WFIRST(2.4m)

z〜10

Roles of WFIRST and the Other Telescopes

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

UV LF (expected)

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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