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2011/11/28

Galactic Astronomy 銀河物理学特論 I Lecture 3-1: Statistical survey of high-redshift galaxies Seminar: Steidel et al. 1999, ApJ, 519, 1 Lecture:. 2011/11/28. U-dropout LBGs:

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2011/11/28

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  1. Galactic Astronomy銀河物理学特論 ILecture 3-1: Statistical survey of high-redshift galaxiesSeminar: Steidel et al. 1999, ApJ, 519, 1 Lecture: 2011/11/28

  2. U-dropout LBGs: Statistical survey for z=3 galaxies was conducted utilizing the fact that ”Lyman limit” comes to the wavelength range between U- and G-band. The success of the survey with spectroscopic confirmation of ~1,000 galaxies at z~3 with Keck telescope established the new method to explore the universe at z>1. Steidel et al. 2003, ApJ, 592, 728 First paper, Steidel et al. 1996, ApJ, 462, L17

  3. G-dropout LBGs: The same U-dropout selection method extended to longer wavelength range to search for galaxies at higher redshift range. G-dropout, B-dropout, V-dropout, i-dropout,,, Steidel et al. 1999, ApJ, 519, 1

  4. Applying the U-dropout method to galaxies at lower redshift range z~3: In order to select galaxies at z>3, the U-dropout selection criteria was extended to bluer U-G color range. The method is called BM/BX method. Steidel et al. 2004, ApJ, 604, 534

  5. Population of galaxies z~3 which cannot be selected with U-drop LBG method ?: Large spectroscopic survey revealed a population of galaxies which are at z~3 but cannot be selected with LBG method. Le Fevre et al. 2005, Nature 437, 519

  6. Population of galaxies at z~3 which cannot be selected with U-drop LBG method ?: Distant Red Galaxies (DRGs) Search for high redshift galaxies with 4000A break and/or Balmer jump in the NIR wavelength range. Vam Dokkum et al. 2003, ApJ, 587, L83 ForsterSchreiber et al. 2004, ApJ, 616, 40 Franx et al. 2003, ApJ, 587, L79

  7. Population of galaxies at z~3 which cannot be selected with U-drop LBG method ?: BzK galaxies Dropout-selection method can only select galaxies with relatively blue color. More complete sample of galaxies can be made with selecting galaxies using 4000A or Balmer break. Reddening vector is along the tilted lilne. Daddi et al. 2004, ApJ, 617, 746

  8. Lyman Alpha Emitter: Ajiki et al. 2003, ApJ, 126, 2091 Kashikawa et al. 2006, ApJ, 648, 7

  9. Lyman Alpha Emitter: Galaxies selected as LAE have relatively weak continuum emission and their estimated stellar mass is small. Gawiser et al. 2006, ApJ, 642, L13

  10. H Alpha Emitter: Geach et al. 2008, MNRAS, 388, 1473

  11. Sub-mm galaxies: Due to the SED shape in the FIR wavelength range, the flux in the sub-mm wavelength range does not simply decrease with redshift. Blain et al. 2002, PhR, 369, 111

  12. Sub-mm galaxies: Chapman et al. 2005, ApJ, 622, 772 Wang et al. 2009, ApJ, 690, 319

  13. Comparing galaxies selected by various methods: Grazian et al. 2007, A&A, 465, 393

  14. Comparing various galaxies with clustering strength. Ichikawa et al. 2007 PASJ, 59, 1081

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