1. Yuichi Matsuda (NAOJ) 松田 有一（国立天文台） Ly-alpha morphology-density relation @ high-z 1

2. 1)Subaru / S-Cam survey shows a hint of Ly-alpha morphology-density relation at high-z. 2)Current observations are limited to extremely bright Ly- alpha blobs. 3)TMT will be able to study the morphology of the circum galactic medium of more normal galaxies at high-z. Summary 2

3. Ly-alpha imaging of the CGM Lya imaging is a promising way to see the 2D morphology of the gaseous structure around high-z galaxies (Chris Martin’s talk). 3 Dekel et al. (2009), van de Voort et al. (2011)

4. Subaru Telescope + Suprime-Cam + Narrow-band filter 8.2 m 27’ x 34’ 21 x 17 cm R ~ 80 http://www.naoj.org/ Subaru / S-Cam Lya Survey at z=3  2.4 sq deg deep Lya imaging survey (Yamada+12)  12 pointings (SSA22 + 6 surrounding fields, Subaru Deep Field, GOODS-N, Subaru-XMM Deep Survey Fields)  1-sigma Lya surface brightness~10 -18 erg s -1 cm -2 arcsec -2  2200 Lya emitters (Yamada+12)  14 giant (>100kpc) Lya nebulae (Matsuda+11) 4

5.  2.4 sq deg deep Lya imaging survey (Yamada+12)  12 pointings (SSA22 + 6 surrounding fields, Subaru Deep Field, GOODS-N, Subaru-XMM Deep Survey Fields)  1-sigma Lya surface brightness~10 -18 erg s -1 cm -2 arcsec -2  2200 Lya emitters (Yamada+12)  14 giant (>100kpc) Lya blobs (Matsuda+11) 300 kpc Subaru / S-Cam Lya Survey at z=3 5

6. The areas of blobs are measured above a threshold of 1.4x10 -18 erg/s/cm 2 /arcsec 2. The circles have diameters of the major axis of the Lya blobs. 6 300 kpc Filamentary & Spherical Lya blobs Filamentary Spherical 20 25 30 35 40 45 50 55 (% ) N S S S S S F FFF F F F F F

7. Subaru / S-Cam Lya Survey at z=3 Faucher-Giguere+11 200 kpc Matsuda+11 ObservationSimulation Spherical? Covering Factor ~60%

8. Subaru / S-Cam Lya Survey at z=3 Faucher-Giguere+11 200 kpc Matsuda+11 Filamentary? ObservationSimulation Covering Factor ~20%

9.  2.4 sq deg deep Lya imaging survey (Yamada+12)  12 pointings (SSA22 + 6 surrounding fields, Subaru Deep Field, GOODS-N, Subaru-XMM Deep Survey Fields)  1-sigma Lya surface brightness~10 -18 erg s -1 cm -2 arcsec -2  2200 Lyman-alpha emitters (Yamada+12)  14 giant (>100kpc) Lyman-alpha nebulae (Matsuda+11) Subaru / S-Cam Lya Survey at z=3 9

10. Fraction Surface Over Density of Lya Emitters (<5 Mpc) Field Protocluster Lya Morphology Density Relation? 10

11. Local Morphology Density Relation Dressler 80 Fraction Surface Density of galaxies 11 S + Irr E + S0 Field Cluster

12. Filamentary Lya blobs may relate to disc galaxy formation via cold streams in the field. Spherical Lya blobs may relate elliptical galaxy formation in hot haloes in proto-cluster. 12 Fraction Over Density Lya Morphology Density Relation?

13. Current observations are limited to extremely bright Lya blobs (only 14 sources!!). It is difficult to study the Lya morphologies of fainter normal galaxies individually. 13 Fraction Over Density Lya Morphology Density Relation?

14. 14 20” 150kpc High Low LAE surface density (5 Mpc/h smoothing) Stacking analysis of 2200 LAEs

15. 15 The Lya radial profile of the field LAEs has a steeper slope. Do the field LAEs (and LBGs) also have filamentary CGM structure? If so, TMT will be able to detect the Lya emitting filaments around LAEs and LBGs. 8m 10hrs 30m 10hrs

16. 1)Subaru / S-Cam survey shows a hint of Ly-alpha morphology-density relation at high-z. 2)Current observations are limited to extremely bright Lya sources. 3)TMT will be able to study the morphology of the circum galactic medium of more normal galaxies at high-z. Summary 16

17. Conclusion Ly-alpha imaging is a promising way to study gaseous structure around high-z galaxies. Subaru / S-Cam survey shows a hint of Ly- alpha morphology-density relation at high-z but the survey is limited to extreme cases. TMT will be able to observe the gaseous structure around more normal galaxies. 17

18. 1)Subaru / Suprime-Cam survey at z=3 shows a hint of Lyman-alpha morphology density relation. 2)Filamentary Lya nebulae are found in the field, while spherical nebulae are dominant in overdense regions. 3)Filamentary nebulae may relate to disc formation via cold streams in the field while the spherical nebulae may relate to spheroid formation in hot haloes in the proto-cluster. Summary 18

19. Radial profile of stacked Lya image of 92 LBGs at z=2-3 Surface brightness threshold ~10 -19 erg s -1 cm -2 arcsec -2 Lya All UV-continuum selected galaxies at z=2-3 have diffuse extended Lya halos Current survey threshold Steidel+11 20” 150kpc But the data are from galaxy over-densities

20. What determines Lya spatial extent? 20 Study Lya halos using 2128 LAEs at z=3.1 as a function of environment and UV luminosity (Matsuda+12) LAE surface density (5 Mpc/h smoothing) Low High Bright Faint Central UV Luminosity

21. Future Subaru HSC Survey Hyper Suprime-Cam (1.5 deg diameter) Subaru Strategic Program (300 nts in 5yrs) Survey starts from Spring 2014 Including Deep z=2-7 Lya imaging in ~30 sq deg http://www.naoj.org/Projects/HSC/surveyplan.html Subaru Telescope + Hyper Suprime-Cam + Narrow-band filter 8.2 m 90 arcmin diameter 60 cm diameter 21

22. 22 Exponential fitting

23. 23 Bright Faint Central UV luminosity 20” 150kpc

24. 24

25. 25 Exponential scale length Low High LAE surface density (5 Mpc/h smoothing) Faint Bright Central UV luminosity Exponential fitting