1 / 4

Emission line astrophysics at high z

Emission line astrophysics at high z. What can we learn from the emission line spectra of (very) young star forming galaxies at high z? Colour-redshift loci determined predominantly by the emission lines Will appear as Lyman forest dropouts at high z

chesna
Download Presentation

Emission line astrophysics at high z

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. Emission line astrophysics at high z • What can we learn from the emission line spectra of (very) young star forming galaxies at high z? • Colour-redshift loci determined predominantly by the emission lines • Will appear as Lyman forest dropouts at high z • Indicators of chemical abundances and IMF of ionizing stars Towards Pop III? GOODS science

  2. GOODS CDF-S BViz GOODS science

  3. GOODS ACS (V1.7) #6746 • zAB = 24.43 • z = 5.6 • r ~ 1kpc • cf. Lynx • F814WAB = 23.1 • z = 3.36 • Dm(Dz)=1.32 Lya NIV] CIV GOODS science

  4. The nebular continuum (light blue line) is simply scaled from the observed Hb flux with no reddening S99 population models are for 107 Msun with a Salpeter IMF (a = 2.35; 1–100Msun) and Z/Zsun = 0.05 They produce ~ 20 x too few ionizing photons GOODS science

More Related