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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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
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
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
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
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
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
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
Ajiki et al. 2003, ApJ, 126, 2091
Kashikawa et al. 2006, ApJ, 648, 7
Galaxies selected as LAE have relatively weak continuum emission and their estimated stellar mass is small.
Gawiser et al. 2006, ApJ, 642, L13
Geach et al. 2008, MNRAS, 388, 1473
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
Chapman et al. 2005, ApJ, 622, 772
Wang et al. 2009, ApJ, 690, 319
Grazian et al. 2007, A&A, 465, 393
Ichikawa et al. 2007
PASJ, 59, 1081