“artists can color the sky red because they know it’s blue. those of us who aren’t artists...
TRANSCRIPT
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“Artists can color the sky redbecause they know it’s blue.Those of us who aren’t artists must colorthings the way they are or people mightthink we’re stupid.”
Jules Feiffer
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Red Galaxiesat
High Redshift
Stijn Wuyts, Marijn Franx, Pieter van Dokkum,Ivo Labbé, Natascha Förster Schreiber, Greg Rudnick,TJ Cox, Phil Hopkins, Brant Robertson, Lars Hernquist
• When did the stars in galaxies form?• How was the mass in galaxies assembled?
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• When did the stars in galaxies form?• How was the mass in galaxies assembled?
Ingredients & History From colors to physics Evolution
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Telescopes
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Telescopes
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Galaxy interactions
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Galaxy interactions-simulations-
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Galaxy interactions-simulations-
Holmberg 1941
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Galaxy interactions-simulations-
Holmberg 1941 Springel et al.
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Quasars&
Black Holes
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Richards et al. 2005
Quasars
&
Black Holes
Schmidt 1963
2dF-SDSS LRG and QSO Survey
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Genzel et al.
Quasars
&
Black Holes
Schmidt 1963
Häring & Rix 2004
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Normal galaxies
Hubble 1926Hubble 1936
• HDFS (5 arcmin2)• MS 1054-03 (25 arcmin2)• CDFS (113 arcmin2)
Labbé et al. 2003
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Normal galaxies
Hubble 1926Hubble 1936
• HDFS (5 arcmin2)• MS 1054-03 (25 arcmin2)• CDFS (113 arcmin2)
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Stellar population synthesis
Wood 1966
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Evolutionary stellar population synthesis
Bruzual & Charlot 2003
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Evolutionary stellar population synthesis
Star formation historySSP, exponentially declining (τ300), CSF
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Evolutionary stellar population synthesis
Dust screen (Calzetti et al. 2000)
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SED modeling - results
Red galaxies at high redshift do not form a uniform population.
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Red galaxies at high redshift dominate at the high mass end.
SED modeling - results
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Red galaxies dominate the total IR emission at high redshift.
SED modeling - results
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Testing SED modeling with simulations
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• Wide range of spectral types• Have real universe equivalents
Testing SED modeling with simulations
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Mismatch real vs. template SFH→ Impossible to correct for difference light- vs. mass-weighted
Impact of star formation history
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Impact of dust
Increased extinction towards young stellar regionsreduces offset light- vs. mass-weighted properties.
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Mismatch real vs. template SFH→ Impossible to correct for difference light- vs. mass-weighted→ Less severe in the presence of age-dependent extinction
Impact of dust
Intrinsic Attenuated
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Every observer is limited by the light he/she receives.
Impact of dust
Eff
ectiv
e re
dden
ing
Effective extinction
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Input: Calzetti, MW or SMC reddening curveEffective reddening: greyer than Calzetti
Impact of dust
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Modeling sub-solar stellar populationswith solar-metallicity templates.→ underestimate reddening → underestimate extinction
Impact of metallicity
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Real: Stars + AGN → Recovered: younger & dustier stellar pop.
Impact of AGN
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Testing SED modeling with simulations: results
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An evolutionary scenario
Sanders et al. 1988
ULIRG(L > 1012Lsun)
QSO
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An evolutionary scenario
Hopkins et al. 2006
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Quasar to galaxy demographics
Hopkins et al. 2006
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Quasar to galaxy demographics
Hopkins et al. 2006
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Abundance of massive galaxies
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Mass function
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Colors of massive galaxies
V-J
U-V
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Colors of massive galaxies – by type
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Colors of massive galaxies – by type
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Selecting by specific star formation rate
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Abundance of massive galaxies – by type
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Pair statistics
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Red Galaxiesat
High Redshift
Observations• Diversity at high redshift• Evolutionary scenario involving merger-triggered QSOs• Abundance of massive galaxies OK• Colors of dusty red galaxies not reproduced
Conclusions
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Emlen 1967, 1970
After man, the indigo bunting is the best documented example of a speciesthat in its earthly life uses celestial bodies outside the solar system.
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• When did the stars in galaxies form?• How was the mass in galaxies assembled?
Ingredients & History From colors to physics Evolution