Absorption line studies with Cross-correlation Intensity Mapping 鹿熊亮太 The University of Tokyo ICRR
Absorption line studies with Cross-correlation Intensity Mapping かくま 鹿熊 鹿熊亮太 The University of Tokyo ICRR
■ Today's agenda ① My study - Ly α -emission Cross-correlation Intensity Mapping ② Absorption line studies with Cross-correlation Intensity Mapping - Review of "Croft et al. 2018" - Ly α -forest Cross-correlation Intensity Mapping - Future study
INTRODUCTION Absorption vs. Emission Absorption neutral ���������� Diffuse Emission scattering neutral Enormous Ly α Lyman- α Halo Nebulae Ly α UV c p Galaxy k 0 0 4 a S/N -2 csec ) ionized ~40kpc b N 10 ′′ (~83 kpc) Momose +14 E Cantalupo +14 Matter distribution Absorption & Emission Physical property Cosmic S Shadow 2 2018 @ @ I Ishigaki-is island Ryota Kakuma �
Breysse+16 Correlation Cross INTRODUCTION Cross-Correlation Intensity Mapping not resolved z - known Cross Correlation Source Intensity position Map r SB mean r distance Noise & contamination SB mean of pixels which are ��� → 0 separated by r from LAEs Cosmic S Shadow 2 2018 @ @ I Ishigaki-is island Ryota Kakuma �
Cross Correlation 1. MY STUDY : ANALYSIS Data The Hyper-Suprime-Cam Strategic Subaru Program (s18a data release) ü Mask Area : • Bright source • Detected (S/N > 5) 4 deg 2 ü 5 σ clipping UD SXDS UD COSMOS Source position Intensity Map NB816 Image z = 5.7 LAEs (z=5.7 Ly α map) (N = 425) NB921 Image z = 6.6 LAEs (z=6.6 Ly α map) (N = 396) Cosmic S Shadow 2 2018 @ @ I Ishigaki-is island Ryota Kakuma �
Correlation Cross <latexit sha1_base64="8PjUDwhkA9xY5dZl4M+z+S8PNJw=">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</latexit> <latexit sha1_base64="8PjUDwhkA9xY5dZl4M+z+S8PNJw=">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</latexit> <latexit sha1_base64="8PjUDwhkA9xY5dZl4M+z+S8PNJw=">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</latexit> <latexit sha1_base64="8PjUDwhkA9xY5dZl4M+z+S8PNJw=">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</latexit> 1. MY STUDY : ANALYSIS Cross-Correlation and systematics r r ��� ! "# LAE G-drop galaxies " # " # 1 1 ξ IM = w r,i f r,i w r,i f r,i − P P r,i w r,i r,i w r,i LAE G − drop Test for All systematic errors Source position Intensity Map Cross l PSF Correlation NB Images G-dropout l Sky subtraction (NB816, NB921) (z ~4) l Unknown systematics Same number and mag. distribution as LAEs Cosmic S Shadow 2 2018 @ @ I Ishigaki-is island Ryota Kakuma �
1. MY STUDY : RESULT RESULT MUSE LAH LAE × z6.6 Ly α Kakuma et al. in prep. LAE × z5.7 Ly α l Consistent with Ly α Halo studies at ≲ 20 pkpc scale l More extending to ~ 100kpc Cosmic S Shadow 2 2018 @ @ I Ishigaki-is island Ryota Kakuma �
1. MY STUDY : RESULT S18a data release ❑ I told some of you different result from HSC-SSP s17a release s17a s18a Kakuma et al. in prep. ❑ HSC-SSP s18a data was released this summer l Difference : Global Sky Subtraction global sky subtraction Ø Large mesh grid size Ø Estimate sky revel beyond each patches ü May be better than previous method… (still checking) # with very large binSize Cosmic S Shadow 2 2018 @ @ I Ishigaki-is island Ryota Kakuma �
1. MY STUDY : DISCUSSION Origin of diffuse Ly α emission Ly α H α UV (continuum) Galaxy Cold gas Scattering Outflow Fluorescent Clustering streams ❑ Many possibility and Many explanation (observation & simulation) ü We need multiple information Zheng +11 Cosmic S Shadow 2 2018 @ @ I Ishigaki-is island Ryota Kakuma ��
2. Absorption line studies with Cross-correlation Intensity Mapping : Croft et al. +18 Croft et al. 2016 ❑ Cross-correlation between Ly α emission (SDSS fiber spectra) × Quasar Croft +16 l Extended Ly α emission to ~15 cMpc l Clustering of galaxies ❑ Problem Ø Very high ! SFR (~0.3 @ z = 2.5) Ø Light from other quasars spatially clustered can contaminate nearby galaxy fibers Revised in Croft et al. 2018 Cosmic S Shadow 2 2018 @ @ I Ishigaki-is island Ryota Kakuma ��
2. Absorption line studies with Cross-correlation Intensity Mapping : Croft et al. +18 Croft et al. 2018 Croft +18 Ly α forest × Quasar ❑ Cross-correlation between Ly α emission × Quasar and Ly α forest × Quasar l Ly α forest : a tracer of the density field Model signal from Ø Sensitive to very large scale Observed flux galaxy clustering Ly α nebulae Fitted Continuum l No detection around QSO ❑ Consistent with extrapolation of quasar nebulae Ly α emission × Quasar Fluorescent emission from Quasar Cosmic S Shadow 2 2018 @ @ I Ishigaki-is island Ryota Kakuma ��
2. Absorption line studies with Cross-correlation Intensity Mapping Future study ❑ We can cross-correlate with ANYTHING . l Absorption line × Quasar, Galaxy, emission (Ly α , metal line), e.t.c. ❑ Synergy between absorption and emission l Large scale matter distribution and physical condition u Ongoing or upcoming survey Ø HETDEX : 420 deg 2 , 350 –550 nm Ø LAEPAU : 100deg 2 , 40NB+5BB,450-850nm Ø J-PAS : 8000 deg 2 , 56 NB Ø SPHEREx : Allsky, spectra, resoluton: 6" u Already available data Ø SDSS fiber, Subaru NB, etc. Cosmic S Shadow 2 2018 @ @ I Ishigaki-is island Ryota Kakuma ��
Summary ① My study Kakuma et al. ❑ NEW sky estimating method in prep. l Still checking now ❑ Ly α halo may be more extending ❑ We needs multiple information ② Absorption line studies w/ Cross-correlation Intensity Mapping ❑ Complemental study to trace a matter density distribution l Abs. : neutral gas, Emi. : ionized gas (+ neutral gas) ❑ Many available and upcoming valuable data-set Cosmic S Shadow 2 2018 @ @ I Ishigaki-is island Ryota Kakuma ��
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