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On the last 10 billion years of stellar mass growth in star-forming - - PowerPoint PPT Presentation

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On the last 10 billion years of stellar mass growth in star-forming galaxies z szomoru+11 Log(SFR/M*) Sam Leitner (University of Chicago) Advisor: Andrey Kravtsov Santa Cruz Galaxy Workshop, August 2011 z0 A persistent SDSS SFR-M *

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On the last 10 billion years of stellar mass growth in star-forming galaxies

Sam Leitner (University of Chicago)

Advisor: Andrey Kravtsov

Santa Cruz Galaxy Workshop, August 2011

szomoru+11

Log(SFR/M*)

z

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Small scatter in SFR at M*:

  • z≈0 in SDSS (e.g. Brinchmann+04)
  • z≈0 in local dwarfs (Lee+11)
  • z≈2 in M* >1010 (e.g. Rhodighiero+11)

A persistent SFR main sequence

SFR-M* SFR-M*

Dwarfs

SDSS

Salim+07 Lee+11 Rhodighiero+11

z≈0 z≈2 σ=0.24dex z≈0

log (SFR) log (SFR/M*)

log (M*) log (M*)

log (SFR/M*)

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Main Sequence Integration

stellar mass fraction formed

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Main Sequence Integration

stellar mass fraction formed

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Main Sequence Integration

stellar mass fraction formed

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Main Sequence Integration

stellar mass fraction formed

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Small scatter in SFR at M*:

  • z≈0 in SDSS (e.g. Brinchmann+04)
  • z≈0 in local dwarfs (Lee+11)
  • z≈2 in M* >1010 (e.g. Rhodighiero+11)

A persistent SFR main sequence

SFR-M* SFR-M*

Dwarfs

SDSS

Salim+07 Lee+11 Rhodighiero+11

σ=0.24dex

z≈0 z≈2 z≈0

log (SFR) log (SFR/M*)

log (M*) log (M*)

log (SFR/M*)

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SLIDE 8

Small scatter in SFR at M*:

  • z≈0 in SDSS (e.g. Brinchmann+04)
  • z≈0 in local dwarfs (Lee+11)
  • z≈2 in M* >1010 (e.g. Rhodighiero+11)

A persistent SFR main sequence

SFR-M* SFR-M*

Dwarfs

SDSS

Salim+07 Lee+11 Rhodighiero+11

σ=0.24dex

z≈0 z≈2 z≈0

log (SFR) log (SFR/M*)

log (M*) log (M*)

log (SFR/M*)

z≈0

SFR

z≈2

Wuyts+11

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SFR(1011Mʘ,z)/M*[1/Gyr]

10 1 0.1 0.01

Observations: normalization of SFR-M*

Salim et al. 2007; Noeske et al. 2007b; Elbaz et al. 2007; Pannella et al. 2009; Daddi et al. 2007; Dunne et al. 2009; Oliver et al. 2010; Rodighiero et al. 2010a Karim et al. 2011;

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SFR(1011Mʘ,z)/M*[1/Gyr]

10 1 0.1 0.01

Observations: normalization of SFR-M*

Salim et al. 2007; Noeske et al. 2007b; Elbaz et al. 2007; Pannella et al. 2009; Daddi et al. 2007; Dunne et al. 2009; Oliver et al. 2010; Rodighiero et al. 2010a Karim et al. 2011;

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Observations: slope SFR/M*~M*

β

β 0.0

  • 0.2
  • 0.4
  • 0.6

0.4 0.2 smaller galaxies grow faster (implies downsizing)

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Observations: slope SFR/M*~M*

β

β 0.0

  • 0.2
  • 0.4
  • 0.6

0.4 0.2 smaller galaxies grow faster (implies downsizing)

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108 109 1010 1011

Typical stellar mass growth from main sequence integration

Extrapolated data Unreliable(ρSFR≠∆ρ*) Robust early growth

star formation histories stellar mass growth

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Quantifying the late formation of star forming galaxies

z15%: M(z)=0.15M*(z=0)

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Quantifying the late formation of star forming galaxies

z15%: M(z)=0.15M*(z=0)

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Quantifying the late formation of star forming galaxies

z15%: M(z)=0.15M*(z=0) stellar mass at z=1

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Stellar mass growth from spectra

star formation histories stellar mass growth

Averaged SED-based SFHs of ~50,000 SDSS star-forming galaxies of 1010.5-1011Mʘ from the VESPA Database

<M*>=6x1010Mʘ

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Mimicking age uncertainty

SSPs with typical SDSS signal-to noise are not distinguished over <0.5dex:

Tests show little bias, but resolution~1dex for non-SSPs with unknown metallicity

  • >Smooth by σ=0.5dex in log-age

Main Sequence Integration MSI+age uncertainty

Ocvirk+06

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Main sequence integration and SEDs

<M*>=6x1010Mʘ

Main Sequence Integration MSI+age uncertainty

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Main sequence integration and SEDs

<M*>=2x1010Mʘ

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Main sequence integration and SEDs

<M*>=5x109Mʘ

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Main sequence integration and SEDs

<M*>=2x108Mʘ

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Consistency between SEDs and the main sequence

<M*>=5x109Mʘ <M*>=6x1010Mʘ <M*>=2x1010Mʘ <M*>=2x108Mʘ

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A transition at low masses?

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A transition at low masses? An SED/CMD discrepancy?

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Summary and Conclusions

  • The main sequence of star formation can be integrated to calculate

stellar mass growth in star forming galaxies back to 10-20% of current stellar masses.

  • Less than 15% of stellar mass (median bulge mass) is in place in star

forming galaxies of about M*=1-5x1010 SFGs at z>2.

  • SED-based star formation histories are consistent with SFR-M* and

its evolution after accounting for age uncertainties.

  • Local CMD-analyzed dwarfs formed early(?) compared to SED and

main sequence extrapolations.

  • Details: merging, ρSFR≠∆ρ* , effect of scatter in SFR-M*, other high

S/N SED- and CMD-based disk observations. arXiv:1108.0938

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Merging and Scatter

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The effect of age resolution on mass growth in SED-based SFHs