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Hα@z=0.24: SFRdensity Pascual et al 2001; 2007 CAHA 2.2m & INT 2.5m ~1 sqr deg 8200 Å 0.5% NB F > 4 10 -16 erg/s/cm2 EW(Hα+[NII]) > 20 Å Jesús Gallego – UCM Granada 2008 20
Hα@z=0.24: Disk-like objects Pascual et al 09 WHT 4.2m ~20 objects Phot-z’s Jesús Gallego – UCM Granada 2008 21
- Page 1 and 2: An Hα approach to the evolution of
- Page 3 and 4: Observational tests: The cosmic SFR
- Page 5 and 6: Galaxy evolution: SFR tracers SFR [
- Page 7 and 8: Downsizing since z
- Page 9 and 10: Open questions How the overall pic
- Page 11 and 12: The Hα approach Evolution of the
- Page 13 and 14: Redshifts considered z=0.02 6563Å
- Page 15 and 16: Redshifts considered z=0.02 6563Å
- Page 17 and 18: Redshifts considered z=0.02 6563Å
- Page 19: Redshifts considered z=0.02 6563Å
- Page 23 and 24: Hα@z=0.24: Contaminants • Ugriz
- Page 25 and 26: Contaminants • 2 objects are sele
- Page 27 and 28: Hα @ z=0.40: SFRdensity Jesús
- Page 29 and 30: Photo-redshifts Villar et al 08 Se
- Page 31 and 32: Hα Luminosity Function @ z=0.8 Vil
- Page 33 and 34: Hα@z=0.8: Field-to-field variance
- Page 35 and 36: Hα-based Madau plot Villar et al 0
- Page 37 and 38: On the nature of Hα @ z=0.8 Most
- Page 39 and 40: Hα @ z=0.8 IRAC data for stellar m
- Page 41 and 42: EW(OII) vs. M B Disk-like spectros
- Page 43 and 44: On the nature of Hα @ z=0.8 A. Sá
- Page 45 and 46: SFR tot - M* relation Massive galax
- Page 47 and 48: The first quantification of downsiz
- Page 49 and 50: Future studies @ z>1.5 Jesús G
- Page 51 and 52: FISIR: a fully criogenic TF in the
Hα@z=0.24: SFRdensity<br />
Pascual et al 2001; 2007<br />
CAHA 2.2m &<br />
INT 2.5m<br />
~1 sqr deg<br />
8200 Å<br />
0.5% NB<br />
F > 4 10 -16<br />
erg/s/cm2<br />
EW(Hα+[NII])<br />
> 20 Å<br />
<br />
<br />
<br />
Jesús Gallego – UCM Granada 2008 20
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