Summary of WISH Filter Set and Sensitivity: Filters suitable for various scientific case Filters cover wavelength range of 1-5µm without any gaps Narr

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1 Summary of WISH Survey Plan Kiyoto Yabe (NAOJ)

2 Summary of WISH Filter Set and Sensitivity: Filters suitable for various scientific case Filters cover wavelength range of 1-5µm without any gaps Narrower filters in bluer wavelength region Y J H K L M (6) IRAC1 IRAC2 WISH standard filter set

3 Summary of WISH Filter Set and Sensitivity: Narrow band filters are under consideration Slitless spectroscopy is also under consideration as option WISH narrow-band filter set

4 WISH mini international workshop (Mar. 2013) フィルタのバンドパス部分以外の波長域でのリークは天体は点源とし aperture 直径は各フィルタの中心波 Summary of WISH Filter Set and Sensitivity: 的な PSF が達成された場合はより小さい aperture の方 PSF は理想的な場合よりはひろがるであろうことまひろがりを持つことから上記の設定で計算を行う Limiting magnitudes for the WISH broad band filters 黄道光は黄極付近での場合 in Filter ( 章参照) とその 3 倍 Reaching 28 mag (AB) in hrs exposure 行う天域としては黄道光の強度は黄極の 3 倍未満で Shallower limiting magnitudes in Filter 5-6 (>50hrs for 28 mag) Fig に 3σ 限界等級を示すまた Table には級と 28 AB 等級に到達するのに要する on-source 積分時間に要する積分時間) を示す Filter 0 から 4 については 10 等級に到達できることが分かるなお 300 秒の積分でほぼ 5σ 限界等級は 3σ の場合より約 0.56 等明るくなる 3 Ecliptic pole Filter λcenter 10h exp. hours to reach [µm] 3σ mag. 28 AB mag e ( ) 表 : on-source 10 時間積分で到達する 3σ 限界等級および 28AB ( : Filter 6 は 27AB mag. に到達するのに要する積分時間)

5 WISH mini international workshop (Mar. 2013) Summary of WISH Filter Set and Sensitivity: Limiting magnitudes for the WISH narrow band filters Shallower than the those for the broad band filters Reaching 26 mag (AB) in ~20 hrs exposure in NB Filter Name λcenter FWHM R 10h1 50h2 Re NB NBF NB NBF NB NBF NB NBF NB NBF NBF NBF NB441 NB497 z 表 : 狭帯域フィルタセット案 (1) z はターゲットとなる Lyα 輝線銀河の赤方偏移よび NB497 については Hα の赤方偏移 1: on-source 積分時間 10 時間での点源 3σ 限界等級間での点源 3σ 限界等級

6 Summary of WISH Science Goals: Main scientific goals Survey of galaxies at z>7 including high-z QSOs and GRBs Exploring the 1st generation of galaxies Galaxy formation and evolution Cosmic re-ionization process NIR survey of Type-Ia SNe at high redshift Light curves of SNe by multiple observations History of cosmic expansion and dark energy Broad study on galaxies at z<7 Galactic objects (bulge astrometry, open clusters, disk dynamics) Extrasolar planes (transit objects, micro-lensing) Objects in solar system (H2O ice on asteroids)

7 Expected numbers of galaxies at z>7: Searching for galaxies at z>7 with dropout technique WISH filter set with sharp cutoff Galaxies at z=8-9 as filter0(1.0µm)-dropout Galaxies at z=11-12 as filter1(1.4µm)-dropout Galaxies at z=13-17 as filter2(1.8µm)-dropout Expected number of the galaxy detections w/o LF evolution w/ LF evolution (empirical, from DMH, SAM) ~600, ~50, and ~1 galaxies per 1 deg 2 at z=8-9, z=11-12, and z=14-17, respectively, are expected * The expected detection numbers per 1deg 2 z No LF evolution LF evolution (empirical) LF evolution (DMH) LF evolution (SAM) 0-drop drop drop

8 Survey Strategy: Deep Extreme Deep Survey Ultra Deep Survey Ultra Wide Survey Wide +Deep Filter5, Narrow Band, etc. Survey strategy (total 5 years) Ultra Deep Survey (UDS) ~28 AB mag in Filter 0, 1, 2, 3, 4 ~100 deg 2 ~1500 days ~10 deg 2 for Filter 5 Ultra Wide Survey (UWS) ~25 AB mag in Filter 1, 2, 3 (+4?) ~1000 deg 2 ~50 days Extreme Deep Survey (EDS) ~30 AB mag in Filter 1, 2, 3, 4? 1FoV (~0.25 deg 2 ) ~20 days NB filter surveys and other scientific observations TBD

9 Possible Survey Fields: Field selection Requirements Low zodiacal background (how far from ecliptic plane) Visibility from L2 (ecliptic pole is ideal) Multi-wavelength data (especially deep optical data) Field candidates Hyper Suprime-Cam (HSC) Multi-wavelength data (g, r, i, z, y-bands) Deep and Wide survey (~30 deg. for Deep and ~1400 deg. for Wide) Most fields are near ecliptic plane (Dec.~0 deg.) Target fields cf. Subaru/Hyper Suprime-Cam Deep Survey fields (slide by M. Tanaka-san)

Visibility: Angle of the telescope toward and against the sun is limited Power supply from solar puddle Thermal environment of satellite bus Size of the sun shield WISH Sun The range of the sky that

10 Visibility: Angle of the telescope toward and against the sun is limited Power supply from solar puddle Thermal environment of satellite bus Size of the sun shield WISH Sun The range of the sky that the telescope can see at some point can also be limited The visibility is roughly estimated with the following assumptions Available angle: 0 deg. toward and 20 deg. against the sun 1 year = 360 days Orbit at L2 point is neglected

11 Visibility: Visibility map for a given coordinate (R.A. and Dec.), showing the number of visible days Higher (lower) visibility near ecliptic pole (plane)

12 Visibility: Visibility at HSC Deep Survey fields (near the equator) Visible for ~45 days per year (except for ELAIS-N1) The number of days continuously visible is ~20 days HSC-D1(XMM-LSS) HSC-D2(COSMOS) HSC-D3(ELAIS-N1) HSC-D4(DEEP2-3) Field Number Day [arbitrary]

13 Visibility: Visibility at the ecliptic poles (EPs) Visible for ~180 days per year The number of days continuously visible is ~180 days 3 NEP SEP Field Number Day [arbitrary]

14 Visibility: Visibility map for a given coordinate (R.A. and Dec.), showing the number of visible days (in case of the available angle of -5 deg. toward the Sun and 30 deg. against the Sun)

15 Visibility: Visibility at HSC Deep Survey fields (in case of the available angle of -5 deg. toward the Sun and 30 deg. against the Sun) 7 6 HSC-D1(XMM-LSS) HSC-D2(COSMOS) HSC-D3(ELAIS-N1) HSC-D4(DEEP2-3) 5 Field Number Day [arbitrary]

16 Possible Survey Fields: Visibility near the equator days per year continuous days per year Not ideal for the SN surveys SN surveys require >5 different observations every 10 days >40 continuous days are necessary Visibility near Ecliptic pole is good Possible Survey Plan HSC-Deep Fields XMM-LSS, COSMOS, DEEP2 ~20 deg 2 (~7 deg 2 each) Deep optical data available Other fields near EP ~80 deg 2 Deep optical data unavailable WISH-Deep Field with HSC? Target fields

17 Summary: WISH survey strategy Ultra Deep Survey (UDS) ~28 AB mag in Filter 0, 1, 2, 3, 4 ~100 deg 2 (~10 deg 2 for Filter 5) in ~1500 days Ultra Wide Survey (UWS) ~25 AB mag in Filter 1, 2, 3 (+4?) ~1000 deg 2 in ~50 days Extreme Deep Survey (EDS) ~30 AB mag in Filter 1, 2, 3, 4? 1FoV (~0.25 deg 2 ) in xx days? Narrow Band survey and other scientific observations? Possible survey fields for UDS (100 deg 2 ) ~20 deg 2 in HSC-Deep fields ~80 deg 2 in fields near ecliptic poles Possibility of WISH Deep Survey with Subaru/HSC?

29-30等ABまで観測するExtremely Deep Survey (EDS)の可能性や狭帯域フィター/グリズムによるサーベイその他のサイエンスケース

2013) es in the first case and no z 10 candidates (i.e., an upper ble 1: 2010 年 7 月時点での WISH R(in)=0.

2um y density determinations are converted into SFR the Madau et al.

from 0.1 M& and 125 M& ). As often 図11. WISH検出器の焦 ma et al. 2007; Stanway et al.

mate of the SFR (by factors of 2) for galaxies が抜けた検出器配置を young ages.

2010a, 2010b; Oesch et al. 2010a; イを行なうことができ. 2010; Bunker et al.

7 galaxies is likely small, ction for dust is made in computing the SFR 7.

(2005), Reddy & Steidel (2009), and 2009).

ディザによって均一な深さナツ型の円周が焦点面でグレーの部分が n Figure 16.

respectively, Multiple can ofprovide us almost e same limiting luminosity at z 4.

0等(AB) 100平方度 150 uniform field of respectively, views.

2 広帯域フィルタセット This provides some measure of how substantial is still under

19 29-30等ABまで観測するExtremely Deep Survey (EDS)の可能性や狭帯域フィター/グリズムによるサーベイその他のサイエンスケース例えば銀河面どに対するサーベイ案についても現在検討中である Additional Information: re 1σ (68% confidence). ons and limits from Bouwens et al. (2011) and assume WISH miniare international workshop (Mar. 2013) es in the first case and no z 10 candidates (i.e., an upper ble 1: 2010 年 7 月時点での WISH R(in)=0.2deg 基本仕様 2.2um y density determinations are converted into SFR the Madau et al. (1998) conversion factor eter initial mass function (IMF; with a stellar anging from 0.1 M& and 125 M& ). As often 図11. WISH検出器の焦 ma et al. 2007; Stanway et al. 2005; Bouwens is conversion factor assumes that the SFRs 置(左)とディザリング relatively constant for!100 Myr prior to の例(右) WISHでは視 nsequently, use of this conversion would result mate of the SFR (by factors of 2) for galaxies が抜けた検出器配置を young ages. るがディザリングを ry blue UV-continuum slopes β of z! 7 ることで均一な深さの ouwens et al. 2010a, 2010b; Oesch et al. 2010a; イを行なうことができ. 2010; Bunker et al. 2010; see also Bouwens dust extinction in z! 7 galaxies is likely small, ction for dust is made in computing the SFR 7. At z " 6, we adopt the dust corrections given h et al. (2005), Reddy & Steidel (2009), and 2009). Our SFR density are included Figure 2: estimates ディザパターンの例中心部が抜けた特殊な検出器配置でもディザによって均一な深さナツ型の円周が焦点面でグレーの部分が n Figure 16. サーベイを行うことができる 2k 2k 4 の検出器クラスター Peculiar フィルター数限界等級サーベイ面積サーベ nosity densities we findfocal to 17.7plane AB magon at WISH telescope: する 8 are just 32% and dithering 18%, respectively, Multiple can ofprovide us almost e same limiting luminosity at z 4. The SFR Ultra Deep Survey (UDS) 等(AB) 100平方度 150 uniform field of respectively, views. However, detailed to these limits are just 6% and 4%, 1.2 広帯域フィルタセット This provides some measure of how substantial is still under strategy of the dithering ミッション提案書での標準フィルタセットとして以下を定義するこれはこれまでの has been in the 1 Gyr from z 7 8 to z Ultra 4 Broad-band Wide Survey (UWS) 等(AB) 1000平方度 50consideration. se was nearing its peak SFR density at 3z と呼んでいたものと同じである 2 3. 検討でセット 4 x 2kx2k FPA 1 Name λcenter Densities from the Stellar Mass Density [µm] g to compare the present SFR density determifilterof0stellar1.040 t inferred from recent estimates mass (Labbe et al. 2010a, 2010b; Stark1 et al ; Filter FWHM [µm] w0 表2. WISHサーベイプラン(案)まとめ w1 R Diff. Limit Ref. Name [µm] [µm] [!! ] WBF0300_ WBF0300_01

20 Additional Information: redshift LF Empirical DMH SAM 0-dropout 8 9 4,000 1, dropout , dropout , Table 2.2: Lyman Break 1 3σ 28.0 AB N / FoV. Filter Name λ c z LAE 10hrs 50 hrs Table 2.4: 10 /50 1 LAE

21 Possible Survey Fields: Target fields cf. Subaru/Hyper Suprime-Cam Deep Survey areas (slide by M. Tanaka-san)

22 Additional Information:

Contents 1. Ia? 2. Ia 3. WISH Ia cosmology 4. WISH Ia + rate 5.

Type Ia Supernova Survey w/ WISH Contents 1. Ia? 2. Ia 3. WISH Ia cosmology 4. WISH Ia + rate 5. Contents 1. Ia? 2. Ia 3. WISH Ia cosmology 4. WISH Ia + rate 5. Type Ia Supernova + +?? (single degenerate)?