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Keck / DEIMOS Spectroscopy of Ly α blobs at z=3.1

Keck / DEIMOS Spectroscopy of Ly α blobs at z=3.1. Yuichi MATSUDA (Kyoto Univ.) Toru YAMADA (NAOJ) Tomoki HAYASHINO, Ryosuke YAMAUCHI, Yuki NAKAMURA (Tohoku Univ.). Ly α blobs (LABs). Diffuse and large Ly α nebulae at high-z (Keel et al. 1999, Steidel et al. 2000,Francis et al. 2001)

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Keck / DEIMOS Spectroscopy of Ly α blobs at z=3.1

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  1. Keck / DEIMOS Spectroscopy of Lyα blobs at z=3.1 Yuichi MATSUDA (Kyoto Univ.) Toru YAMADA (NAOJ) Tomoki HAYASHINO, Ryosuke YAMAUCHI, Yuki NAKAMURA (Tohoku Univ.)

  2. Lyα blobs (LABs) • Diffuse and large Lyαnebulae at high-z (Keel et al. 1999, Steidel et al. 2000,Francis et al. 2001) • LABs live in proto-cluster regions (Palunas et al. 2004, Matsuda et al. 2004) • A significant fraction have FIR dust emission (Chapman et al. 2001, Smail et al. 2003, Geach et al. 2005) The site of massive galaxy formation?

  3. Lyα emitters (LAEs) • Compact Lyαnebulae at high-z (Pascarelle et al. 1998, Venemans et al. 2005) • Young and low stellar mass (Yamada et al. 2001) • No bright FIR dust emission (De Breuck et al. 2003) Building blocks of galaxies?

  4. Connection between LAB & LAE very deep SCAM Narrowband image detection of many diffuse & extended Lyαnebulae (Matsuda et al. 2004) Continuous distribution!!

  5. Keck/DEIMOS Spectroscopic targets (37) Wide range of spatial extents, average surface brightness, & luminosity 36 LABs / LAEs + 1 [OII] emitter

  6. Lyα spatial extent vs Lyα velocity width strong correlation LABs (>16arcsec2) v(FWHM) > 500 km/s

  7. Interpretation of the Lyα velocity width Case 1 : Motion of gravitationally bounded gas clouds dynamical mass (LAB) ~1012 - 1013 Msun Case 2 : Gas outflow (superwind) starburst age several x 107 yr stellar mass (LAB) several x 1010 Msun LABs are hosted in the massive systems!!

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