warm dust in the most distant quasars
Download
Skip this Video
Download Presentation
Warm Dust in the Most Distant Quasars

Loading in 2 Seconds...

play fullscreen
1 / 17

Warm Dust in the Most Distant Quasars - PowerPoint PPT Presentation


  • 90 Views
  • Uploaded on

Warm Dust in the Most Distant Quasars. Ran Wang Department of Astronomy, Peking University, China. Introduction. Why looking for dust at z~6 The mass of dust in the earliest and most massive galaxies: dust formation within 1 Gyr.

loader
I am the owner, or an agent authorized to act on behalf of the owner, of the copyrighted work described.
capcha
Download Presentation

PowerPoint Slideshow about ' Warm Dust in the Most Distant Quasars' - slade-sampson


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.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.


- - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - -
Presentation Transcript
warm dust in the most distant quasars

Warm Dust in the Most Distant Quasars

Ran Wang

Department of Astronomy, Peking University, China

introduction
Introduction
  • Why looking for dust at z~6
    • The mass of dust in the earliest and most massive galaxies: dust formation within 1 Gyr.
    • The dust temperature, distribution, and Luminosity: dust heating quasar systems.

 FIR luminosity SFR  evolutionary stage of the black hole – bulge system.

slide3
Introduction

Marconi & Hunt. (2002)

Tremaine et al. (2002)

MBH~10-3MBulge

MBH~σ4

sample
Sample
  • There are totally Thirty-three quasars discovered at z~6.
    • z=5.71 to 6.43
    • M_1450A < -25.0
  • Twenty-two from the SDSS survey of ~8000 deg^2 area, with m1450A < 20.
  • Nine from deeper optical imaging with m1450A>20, Jiang et al. 2007; Willott et al. 2007
  • IR (Spitzer) + optical: one; Cool et al. (2006)
  • Radio (FIRST) + optical: one; McGreer et al. (2006)

Most of these objects were optically selected from the SDSS survey

Represent the most luminous quasar population at z~6.

observations
Observations

MAMBO IRAM-30m

SHARC-II CSO

the average fir and radio emission
The average FIR and radio emission

Wang et al. (2008 submitted)

FIR-millimeter spectral index ~2

star formation in the mm non detections
Star formation in the mm non-detections
  • The average FIR luminosity: 1.2x1012 Lsun
    • Even 50% of the FIR emission from star formation, the star formation rate => 200 Msun yr-1
    • The major bulge building stage via starburst has been finished ?
slide9
The bright millimeter detections
  • The FIR emission exceeds that of the local quasar template.
  • The FIR SED is consistent with optically thin gray-body emission from 40 ~ 50 K dust.
  • The FIR-to-radio SED is consistent with that of typical star forming galaxies.
  • Dust mass: ≥108 Msun
  • FIR luminosity ~ 1013 Lsun
luminosity correlation l fir l bol
Luminosity correlation LFIR - LBol

Wang et al. (2008 in press)

star formation in the z 6 quasars
Star formation in the z~6 quasars
  • The mm and CO detected quasars at z~6:
    • FIR emission from 40 ~ 50 K warm dust.
    • Properties similar to that of star forming galaxies.
    • Derived star formation rate: ≥ 103 Msun yr-1
    • Active bulge building via massive star formation co-eval with SMBH accretion.
slide14
LFIR & Lya emission

Omont et al. (1996): Three kinds of spectra from z>4 quasars

l fir lya emission
LFIR & Lya emission

Wang et al. (2008 in press)

  • Quasars at z~6:
  • Most of the millimeter detections tend to have log(EW)Lya < 1.5.
  • The origin of this effect is not clear yet.
  • More observations…
slide16
Summary
  • We studied the (sub)millimeter emission from the host galaxies of quasars at z~6.
  • About 30% of these sources have been detected in warm dust continuum at 1.2 mm.
  • The average FIR-to-radio SED of the non-detected sources is comparable to that of local optical quasars.
  • Obvious FIR excesses in the SEDs of the strong millimeter detections.
  • FIR dust heating dominated by Star formation at a rate of a few 1000 Msun yr-1 .
  • The millimeter detected quasars tend to have weak UV line emission.
introduction the discovery of z 6 quasars
Introduction – The discovery of z~6 quasars

1148+5251 z=6.42

Bertoldi et al. (2003)

Beelen et al. 2006

ad