Summary of WISH Survey Plan Kiyoto Yabe (NAOJ)
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 0 1 2 3 4 5 (6) IRAC1 IRAC2 WISH standard filter set
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
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 (7.1 0-4章参照) とその 3 倍 Reaching 28 mag (AB) in 10-20 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. 2.14.2 に 3σ 限界等級を示す また Table 2.14.2 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. 0 1.040 28.24 6.50 1 1.360 28.16 7.50 2 1.775 28.02 9.67 3 2.320 27.89 12.25 4 3.030 27.71 17.08 5 3.965 26.95 69.67 5e 4.215 26.80 90.42 6 4.500 26.20 43.83( ) 表 2.14.2: 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)
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 0-3 2.1 Name λcenter FWHM R 10h1 50h2 Re NB110 1.095 8.0 0.015 73.0 25.69 26.57 NBF NB134 1.340 10.0 0.019 70.5 25.72 26.60 NBF NB158 1.580 12.0 0.022 71.8 25.62 26.50 NBF NB195 1.945 15.0 0.027 72.0 25.47 26.35 NBF NB219 2.188 17.0 0.031 70.6 25.40 26.28 NBF 4.4052 5.71 0.063 69.9 24.50 NBF 4.9720 6.58 0.071 70.0 23.53 NBF NB441 NB497 z 表 2.14.10: 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
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)
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 8-9 4000 1690 852.3 631.2 1-drop 11-12 2393 104.2 4.116 49.7 2-drop 14-17 1249 0.723 0.003 1.071
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
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 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
Visibility: Visibility map for a given coordinate (R.A. and Dec.), showing the number of visible days Higher (lower) visibility near ecliptic pole (plane)
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 7 6 5 HSC-D1(XMM-LSS) HSC-D2(COSMOS) HSC-D3(ELAIS-N1) HSC-D4(DEEP2-3) Field Number 4 3 2 1 0 0 50 100 150 200 250 300 350 Day [arbitrary]
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 2 1 0 0 50 100 150 200 250 300 350 Day [arbitrary]
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)
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 4 3 2 1 0 0 50 100 150 200 250 300 350 Day [arbitrary]
Possible Survey Fields: Visibility near the equator 40-80 days per year 20-40 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
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 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 case. @ 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) 5 28.0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) 3-4 25.0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.1.360 2009; Filter FWHM [µm] 0.280 0.360 w0 表2. WISHサーベイプラン(案)まとめ w1 R Diff. Limit Ref. Name [µm] [µm] [!! ] 0.900 1.180 3.714 0.174 WBF0300_00 1.180 1.540 3.778 0.228 WBF0300_01
Additional Information: redshift LF Empirical DMH SAM 0-dropout 8 9 4,000 1,690 852.3 631.2 1-dropout 11 12 2,393 104.2 4.116 49.7 2-dropout 14 17 1,249 0.723 0.003 1.071 Table 2.2: Lyman Break 1 3σ 28.0 AB N / FoV. Filter Name λ c z LAE 10hrs 50 hrs 0200-00 1.092 8.0 12.3 21.3 0200-01 1.336 10.0 1.6 5.2 0200-02 1.580 12.0 5.5 10 3 0.09 0300-00 1.095 8.0 2.1 16.6 0300-01 1.340 10.0 0.22 2.3 0300-02 1.580 12.0 5.1 10 3 0.10 Table 2.4: 10 /50 1 LAE
Possible Survey Fields: Target fields cf. Subaru/Hyper Suprime-Cam Deep Survey areas (slide by M. Tanaka-san)
Additional Information: