1 / 14

2011/12/12

Galactic Astronomy 銀河物理学特論 I Lecture 3-2: Evolution of Luminosity Functions of Galaxies Seminar: Lily et al. 1995, ApJ, 455, 108 Lecture:. 2011/12/12. Local universe: Luminosity Function of Each Morphological Type

tallis
Download Presentation

2011/12/12

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript


  1. Galactic Astronomy銀河物理学特論 ILecture 3-2: Evolution of Luminosity Functions of GalaxiesSeminar: Lily et al. 1995, ApJ, 455, 108 Lecture: 2011/12/12

  2. Local universe: Luminosity Function of Each Morphological Type The overall shapes of the luminosity functions are well described with Schechter luminosity funtion. Phi(L) = (Phi*/L*) (L/L*)^alpha exp(-L/L*) Three parameters: Normalization (Phi*), characteristic luminosity (L*, knee of LF), faint end slope (alpha). Nakamura et al. 2003, ApJ, 125, 1682

  3. Local universe: Luminosity Function of Each Morphological Type Total luminosity = Phi* L* Gamma(2+alpha) Is dominated by galaxies around the “knee” of the luminosity function if alpha>-2. Density evolution: Phi* changes Luminosity evolution L* changes Nakamura et al. 2003, ApJ, 125, 1682

  4. CFHT-Multi-Object-Spectrograph: Multi slit spectroscopy Multi object spectrograph used for the Canada-France Redshift Survey. The system use multi slit mask to observe many objects at once. http://www.cfht.hawaii.edu/Instruments/Spectroscopy/SIS/Manual/chapter2_5.html#81 LeFevre et al. 1995, ApJ, 455, 60

  5. Hawaii-survey: Galaxy spectroscopic survey with Keck/LRIS. On the contrary to the low-redshift universe, even K-band bright massive galaxies show large SFR at high-redshifts. Cowie et al. 1996, ApJ, 112, 839

  6. Rest-frame UV-luminosity function and star formation rate density in the universe: Reddy et al. 2008, ApJS, 175, 48 Madau et al. 1996, MNRAS, 283, 1388

  7. COMBO-17: In stead of conducting massive spectroscopic survey, they attached 12 narrow-band and 5 broad-band filters to 2m telescope and conducted multi-color survey in wide field. They determined the redshifts of galaxies with multi-band “photometric” redshifts. They discuss the evolution of luminosity function dividing their sample with SED type. Wolf et al. 2003, A&A, 401, 73

  8. The K20 survey: Evolution of luminosity function is discussed with galaxy samples selected based on K-band magnitude. Most of the previous surveys use optical selections, but NIR selection is better to select galaxies based on their stellar mass. Pozzetti et al. 2003, A&A, 402, 837

  9. The DEEP survey: Large spectroscopic survey with 8-10m class telescope with Keck DEIMOS Blue galaxies Red galaxies Willmer et al. 2006, ApJ, 647, 853

  10. The VIMOS-VLT deep survey (VVDS): Evolution of galaxy luminosity function evaluated with spectroscopic redshift survey with VLT/VIMOS. Ilbert et al. 2005, A&A, 439, 863

  11. GOODS: Hubble Space Telescope wide field survey with Advanced Camera for Surveys. Dahlen et al. 2005, ApJ, 631, 126

  12. GOODS: Wide field of view of HST/ACS makes possible to evaluate evolution of luminosity function as a function of galaxy morphology. Ilbert et al. 2006, A&A, 453, 809

  13. Extending to higher and higher redshifts: Bouwens et al. 2011,

  14. Summary: Spectroscopic survey: + Single-band or Two-bands imaging data: (CFHT) Red or Blue galaxies + Multi-color data (Keck LRIS): evolution by SED type + Wide field NIR imaging data (ex. MOIRC): galaxy selection based on their stellar mass        (+establishment of photometric redshift estimation) + “Massive” redshift survey with 8-10m class multi-slit spectrograph (Keck/DEIMOS, VLT/VIMOS) + Availability of high-resolution imaging data from HST in the optical band:luminosity function by morphological type + Longer wavelength data from Spitzer/IRAC: The discussion on “luminosity” function moved into the discussion on “stellar mass” function. The results can be compared with the theoretical cosmological models of galaxy formation more directly.

More Related