Accelerated Evolution of Lya LF at z>7 and the Physical Pictures Akira Konno (Univ. of Tokyo, ICRR) Co-Investigators: M. Ouchi, Y. Ono, K. Shimasaku, T.

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Presentation transcript:

Accelerated Evolution of Lya LF at z>7 and the Physical Pictures Akira Konno (Univ. of Tokyo, ICRR) Co-Investigators: M. Ouchi, Y. Ono, K. Shimasaku, T. Shibuya, H. Furusawa, K. Nakajima, Y. Naito, R. Momose, S. Yuma and M. Iye (arXiv: )

Introduction Lya LF evolves from z=6.6 or not ? Lya damping wing absorption of HI in IGM Sharp or extended reionization history ? ⇒ z=7.3 LAE survey address these issues. Shibuya+ 12 z=6.6 z=5.7 z~7.3 (Hibon,Tilvi, Krug) z~7.3 (Ota, Shibuya) Ouchi+ 10 Redshift Neutral Fraction x(HI) QSO LAE/ GRB CMB ?

Konno+ 14 Subaru/S-Cam NB101 Obs. 1)NB101 … more sensitive to line emission than NB1006 2)Total exp. time : 106 hrs … Ultra-deep survey ⇒ Detect very faint LAEs at z=7.3 5-sigma limiting L(Lya) = 2.4 x erg/s … comparable with z=3-6 LAE survey … ~4x deeper than Subaru z~7.3 survey

z=7.3 LAE sample Field … SXDS and COSMOS (Total : ~0.5 deg 2 ) SXDS : 3 LAEs COSMOS : 4LAEs … Total : 7 LAEs Expect ~65 LAEs in case of no evolution from z=6.6. Konno+ 14

Inner : 68% CL Outer : 90% CL z=7.3 (This Study) z=5.7 (Ouchi+ 08) z=6.6 (Ouchi+ 10) Konno+ 14 z=7.3 (This Study) z=6.6 (Ouchi+ 10) Konno+ 14 Conclude that Lya LF decrease from z=6.6 to 7.3 at >90% confidence level. ( Shown by previous studies ; e.g. Clement+12 ) Evolution of Lya LF at z=

Lya luminosity density UV luminosity density ~ SFRD This Study Ouchi +08, 10 Ellis+ 13 Bouwens+14 Konno+ 14 arXiv: Evolution of Lya LF is accelerated at z>7. No such rapid decrease of UV LF at z~7, but only for z~8. Different from a pure SFR decrease but related to Lya escape + production and/or cosmic reionization Accelerated Evolution of Lya LF

Model C Model B Model A Choudhury+08 models Konno+ 14 Imprecations from Lya LF Evolution x(HI) = … consistent with previous studies Compare our x(HI) with CMB results using theoretical models. Our x(HI) → Model A & B … inconsistent with CMB results WMAP result → Model C … x(HI) is higher than Model C A tension between our x(HI) and CMB results ? o Clumpy HI clouds o Increase of f_esc of LyC (Bolton & Haehnelt 2013) (Dijkstra+ 2014)

Summary Ultra-deep Subaru/S-Cam NB101 imaging survey allow us to detect very faint z=7.3 LAEs. o L(Lya) = 2.4 x erg/s … comparable with z=3-6 survey … ~4x deeper than z~7.3 survey (1)Evolution of Lya LF at z= at >90% CL (2) Accelerated evolution of Lya LF beyond z=7 There is a tension between our x(HI) = and CMB results ? o Support new physical pictures high-z LAE survey with HSC → PFS, JWST, TMT etc…