slide1 n.
Download
Skip this Video
Loading SlideShow in 5 Seconds..
PI Total time #CoIs, team PowerPoint Presentation
Download Presentation
PI Total time #CoIs, team

Loading in 2 Seconds...

play fullscreen
1 / 10

PI Total time #CoIs, team - PowerPoint PPT Presentation


  • 94 Views
  • Uploaded on

The cosmic star formation rate from SNe Use SNe (Ia and core-collapse) to determine the cosmic SFR up to z~6 as derived from stars with 3 M  < M < 40 M  This is much more accurate than using UV flux or H  methods (which give information on stars with M > 40 M  )

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 'PI Total time #CoIs, team' - tasya


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
slide1

The cosmic star formation rate from SNe

Use SNe (Ia and core-collapse) to determine the cosmic SFR up to z~6 as derived from stars with 3 M < M < 40 M This is much more accurate than using UV flux or H methods (which give information on stars with M > 40 M)

As a “bonus” these observations will also allow to probe different cosmological models (e.g. alternatives to )

PI

Total time

#CoIs, team

  • Roberto Gilmozzi
  • 90n (ELT 42m)
  • 10-15 people. Expertise:
  • photometry
  • spectroscopy
  • theoretical interpretation
slide3

Why SNe?

~10%

~90%

40

90% of the ionizing flux comes from stars > 40 M

slide4

SN rate  Star formation Rate

Both the Halpha fluxes and the UV fluxes

measure only the very upper part of the

IMF [>40 M 8% (> 8M)]

therefore:

  • They are NOT good star formation rate indicators because
  • they require a huge extrapolation to lower masses
  • the extrapolation depends on the value of Mup which is not well known and may be not a constant quantity in different environment (Bressan et al. 2002) or at different z (Heger et al. 2002)
slide5

SNe provide a measurements of

the star formation rate which is:

1. Independent of other possible determinations

2. More direct, because the IMF extrapolation is

much smaller

3. More reliable because it is based on counting

SN explosions rather than relying on identifying

and measuring the sources of ionization (if using

H-alpha flux) or the sources of UV continum

slide6

SN Rate as Tracer of Star Formation Rate

a) The rate of core collapse SNe (II & Ib/c) is a direct measurement of the death rate of stars M>8 M (>40 M? Normal II SNe? Normal or Peculiar Ic/b? Collapsars?)

b) The rate of type Ia SNe provide the history of star formation of moderate mass stars, 3-8 M

c) The evolution of the rate can clarify the nature of the progenitors of type Ia SNe (WD+WD or WD+MS) (Madau, Della Valle & Panagia 1998)

simulation of a very large program 950 hours
Simulation of a VERY large program (950 hours!)
  • Simulations of ELT observations yield:
    • Jx3+Hx3+Kx7: ~ 200 SNe (extrapolating Miralda & Riess 1997) or ~ 350 SNe (MDP 1998) up to z ~ 6 in 50 2’x2’ fields
      • Light curves, photometric redshifts (galaxy & SN)
    • Spectroscopy ~50: ~ 50-80 SNe at z < 2.5
  • Spectral classification:
    • SNe Ia visible up to z ~ 5
      • Blind below 2400A, K last useful band
    • SNe II visible up to z ~ 6
      • Strong UV emitters (time-dilated UV flash)
slide10

ELT Justification: Magnitude of objects (today: z ~ 1)

Legacy Value: Evolution of cosmological parameters, evolution of SN progenitors

Data Reduction: Challenge: parent galaxy subtraction (eased by working at the diffraction limit, i.e. low surface brightness per pixel)