Search for metal-absorber host galaxies near the Epoch of - PowerPoint PPT Presentation

Cosmic Shadow 2018 @ Ishigaki 24-25 Nov 2018 Search for metal-absorber host galaxies 
 near the Epoch of Reionization Daichi Kashino (ETH Zurich) Collaborations with S. Lilly, R. Simcoe, R. Bordoloi Background image: simulation by K.Hasegawa

Cosmic Shadow @ Ishigaki 24-25 Nov 2018 Daichi Kashino, ETH Zurich Recent report by Becker et al. 2018 LAE survey with NB816 (z=5.7) in the fj eld of QSO0148+0600, corresponding to the long dark trough. z 5.5 5.6 5.7 5.8 5.9 0.5 1.0 NB816 High- τ HI is likely to be associated with 
 Filter Transmission 0.4 0.8 Normalized Flux 0.3 0.6 high LAE surface density. Ly β forest 0.2 0.4 0.1 0.2 0.0 0.0 The fm uctuating- Γ HI model is preferred. 7900 8000 8100 8200 8300 8400 λ (Å) LAE distribution Surface density

Cosmic Shadow @ Ishigaki 24-25 Nov 2018 Daichi Kashino, ETH Zurich Recent report by Becker et al. 2018 LAE survey with NB816 (z=5.7) in the fj eld of QSO0148+0600, corresponding to the long dark trough. z 5.5 5.6 5.7 5.8 5.9 0.5 1.0 Is this really the evidence of a negative Σ gal - τ e ff correlation? NB816 High- τ HI is likely to be associated with 
 Filter Transmission 0.4 0.8 Normalized Flux 0.3 0.6 high LAE surface density. Ly β forest 0.2 0.4 Are LAEs really suited to this kind of study? 0.1 0.2 0.0 0.0 The fm uctuating- Γ HI model is preferred. Ly α emission is de fj nitely suppressed in such high τ e ff regions. 7900 8000 8100 8200 8300 8400 λ (Å) Are LAEs really tracing the underlying density fj eld? 
 LAE distribution Surface density Complimentary surveys of other types of galaxies are required. Only a single point in the Σ gal vs τ HI plane. More data points across a wide range of τ HI are required to see the correlation.

Cosmic Shadow @ Ishigaki 24-25 Nov 2018 Daichi Kashino, ETH Zurich Approved in S18B, S19A Subaru/HSC: 
 Revealing the τ HI — Σ gal relation over large scales LBG selection with r, i, z (z<=25.7), aiming to detect N ~250 per HSC FoV Target quasars Predicted constraints ( Δ z=0.15, ~70cMpc) τ e fg ( Δ z =0.15) for our targets within 5.4<z<6.0 Over-dense regions Σ LBG (M UV <-21, R <10 arcmin) [arcmin -2 ] high τ e fg targets: J0148+0600 J0842+1218 Mean Σ LBG Mean Σ LBG for low- τ e fg for high- τ e fg J0422-1927 low τ e fg targets: Fluct. T IGM J1137+3549 J1602+4228 E fg ective opacity τ e fg Fluct. Γ HI Voids Realistic LBG selection ( σ z =0.1) and contamination are considered. Range of interest τ e fg over Δ z =0.15 (eq. 70 cMpc) at z=5.7 Redshift Collaboration with Kashikawa-san’s LAE survey in QSO fj elds 
 => direct test of possible suppression of LAE/LBG where we know τ e ff

Cosmic Shadow @ Ishigaki 24-25 Nov 2018 Daichi Kashino, ETH Zurich Today’s talk 1. Background 2. Our projects starting up right now 
 using JWST, ALMA and MUSE 3. Summary

Background

Cosmic Shadow @ Ishigaki 24-25 Nov 2018 Daichi Kashino, ETH Zurich Metal absorption systems back to z~6 • High-z quasars started to be found by SDSS back to z~6 around 2000, and recently, many z~6 quasars (O(10 2 )) are being discovered by various wide surveys. • Astronomers have studied metal pollution of the IGM and metal budget of the Universe using absorption lines seen in quasar spectra. A downward trend in Ω CIV / Ω S SiIV discovered at z>5. What cause the decline in Ω CIV at z>5 ? • the evolution of metal abundance? 3.— (C ) as a function of redshift plotted from the data of Table 1 • change in ionization condition? see also e.g., Simcoe 06, Simcoe+11, Becker+06, 09, 11, Ryan-Weber+09, 4.—Same as Fig. 3, but for Si Songaila 00 Codoreanu+18 D’Odorico+10,13, Chen+17, Bosman+17

Cosmic Shadow @ Ishigaki 24-25 Nov 2018 Daichi Kashino, ETH Zurich Metal absorption systems back to z~6 Excess of low-ionization O I (+SiII, CII) systems at z>5.5 (Becker+06) 
 — Evidence of change in ionization background low-ion. systems (O I ) high-ion. systems (C IV ) MgII systems Compilation from the literature The evolution of Ω ion of low-ionization 
 Codoreanu+18 ions remains poorly constrained.

Cosmic Shadow @ Ishigaki 24-25 Nov 2018 Daichi Kashino, ETH Zurich Host galaxies of metal absorption systems At intermediate redshifts (Simcoe+06) z~2.3 Possible hosts of a strong Ly α + C IV absorber found up to ~320 pkpc from the quasar sightline. 
 (but, can we say they are really hosts with such large b ?) Remarkable metal enhancement at ~100 pkpc. c p k p − 1 h 0 0 5 = R Background IGM At further higher redshifts, 
 spectroscopy is more challenging…

Cosmic Shadow @ Ishigaki 24-25 Nov 2018 Daichi Kashino, ETH Zurich Few identi fj cations at z ≳ 4 Possible identi fj cation HST WFC3 1.6 μ m via Ly α at z=5.7 
 (b=79 pkpc, dv= − 240 km/s) QSO But no consistent detection is found in a MUSE cube 
 (preliminary) 30 arcsec = 176 pkpc Díaz+11 Alternative tracer at 
 z=4.258, b=42 pkpc z=3.798, b=18 pkpc (DLA) high redshifts 
 SFR=110±10 M ⊙ /yr SFR=24±8 M ⊙ /yr . [CII]158 μ m 
 . with ALMA f Neeleman+17, Science

Cosmic Shadow @ Ishigaki 24-25 Nov 2018 Daichi Kashino, ETH Zurich 
 Few identi fj cations at z ≳ 4 Possible identi fj cation HST WFC3 1.6 μ m via Ly α at z=5.7 
 On the other hand, 
 (b=79 pkpc, dv= − 240 km/s) there have been many observations that failed to detect possible QSO DLA and/or metal absorption systems. 
 But no consistent detection is found in a MUSE cube 
 Our knowledge is still very limited: (preliminary) 30 arcsec = 176 pkpc Díaz+11 How far does the enriched gas extend from galaxies? • Alternative tracer at 
 What processes occur in and around galaxies? • z=4.258, b=42 pkpc z=3.798, b=18 pkpc (DLA) high redshifts 
 SFR=110±10 M ⊙ /yr SFR=24±8 M ⊙ /yr What causes the change in the ionization condition . • [CII]158 μ m 
 . with ALMA at z~5.5 ? f Neeleman+17, Science

Our projects starting up right now - JWST/NIRCam WFSS as an ultimate study - ALMA and MUSE to search for absorber hosts

Cosmic Shadow @ Ishigaki 24-25 Nov 2018 Daichi Kashino, ETH Zurich Our GTO program: Exploring the end of cosmic reionization PI Simon Lilly, ETH Zurich In collaboration with Rob Simoe, Rongmon Bordoloi (MIT)

Cosmic Shadow @ Ishigaki 24-25 Nov 2018 Daichi Kashino, ETH Zurich Instrument What we can do? Near-InfraRed • Imaging at 0.6 − 5.0 μ m in two 2.2’ x 2.2’ FoVs Camera 
 • Wide- fj eld Slitless spectroscopy (WFSS; R~1000) NIRCam • Coronagraphic imaging • Imaging at 5.6 − 25.5 μ m in 74" × 113" FOV Mid-InfraRed • Low-resolution slitted and slit less spectroscopy Instrument 
 • IFU spectroscopy in 4.9 − 28.8 μ m MIRI • Coronagraphic imaging Near-InfraRed • MOS with multi-shutter assembly at 0.6 − 5.3 μ m Spectrograph 
 • 3” x 3” IFU spectroscopy NIRSpec • High contrast single object spectroscopy • Low-res. (R~150) WFSS in 0.8 − 5.0 μ m (2.2’ x 2.2’ FoV) Near InfraRed Imager and Slitless • Single object slit less spectroscopy Spectrograph • Aperture-masking interferometry (beyond λ /D) NIRISS • Imaging at 0.9 and 5.0 μ m

Cosmic Shadow @ Ishigaki 24-25 Nov 2018 Daichi Kashino, ETH Zurich Primary survey camera: NIRCam (PI Marcia Rieke) • Simultaneous dichroic imaging of 0.6 - 2.3 µm and 2.4 - 5.0 µm, 
 over two 2.2’ x 2.2’ FoVs • Wide- fj eld Slitless spectroscopy (WFSS; R~1000) in long-wavelength • Coronagraphic imaging

Cosmic Shadow @ Ishigaki 24-25 Nov 2018 Daichi Kashino, ETH Zurich Wide- fj eld slitless spectroscopy with NIRCam “ Slitless ” spectroscopy with grism ➡ We can obtain spectra for all objects in the FoV simultaneously JWST NIRCAM ~ 4.1 μ m • No pre-imaging and mask design • No (little) bias due to pre-sample selection • No slit loss from N. Prizkal’s slide (2018)