Bruno Henriques (Zwicky Fellow, ETH Zurich) Fu et al. (2010, 2011, - - PowerPoint PPT Presentation

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Feb 02, 2024 579 likes •806 views

A self-consistent model of galaxy formation with resolved discs (Henriques, Yates, Fu, Kauffmann, Thomas, White, 2017, in prep.) Bruno Henriques (Zwicky Fellow, ETH Zurich) Fu et al. (2010, 2011, 2013), Yates et al (2013), Henriques et al. (2013,

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A self-consistent model of galaxy formation with resolved discs

Bruno Henriques (Zwicky Fellow, ETH Zurich)

(Henriques, Yates, Fu, Kauffmann, Thomas, White, 2017, in prep.) Fu et al. (2010, 2011, 2013), Yates et al (2013), Henriques et al. (2013, 2015)

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Why we need SN feedback?

The underlying distribution of dark matter is determinant.

The most important problems in galaxy formation can be identified in a model just with accretion and cooling

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Gas Reincorporation

longer reincorporation time-scales for gas ejected by SN in low mass galaxies

Henriques et al. 2013 in agreement with Oppenheimer & Dave 2008

lower number density at early times, stronger build up at later times

hydro should correctly follow the gas flows

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Henriques et al. 2015

SN energy used 100% used

halo

Mass-loading

ut of the halo
ut of the disc

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exponential profile with rd scaling with current halo spin

Galaxy formation with resolved discs

cold gas stars

H2 based star formation H2 Formation Radial inflow detailed chemical enrichment model Cooling separation between H2, HI and ionised (Henriques, Yates, Fu, Kauffmann, Thomas, White, 2017, in prep.)

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cold gas

Cooling forms HI which settles into an exponential disk

Galaxy formation with resolved discs

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cold gas

Cooling forms HI which settles into an exponential disk

HI formation and conversion into H2

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Theoretical studies show HI H2 conversion depends mostly on gas surface density

Krumholz et al. 2009: Blitz & Rosolowsky:

HI formation and conversion into H2

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Star Formation

Kennicutt 1998

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Radial Inflow

Cold gas is denser in the centre of disks star formation happens at the centre radial inflow of gas is required to avoid H2 depletion in the centre

NO INFLOW WITH INFLOW H2 H2

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Detailed Chemical Enrichment

Mmetals=yM* Yates et al. (2013) Detailed chemical enrichment model:

the mass of each element produced in stars of different masses (i.e. ages) and initial metallicities is computed.

SN-Ia

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exponential profile with rd scaling with current halo spin

Galaxy formation with resolved discs

cold gas stars

H2 based star formation H2 Formation Radial inflow detailed chemical enrichment model Cooling separation between H2, HI and ionised (Henriques, Yates, Fu, Kauffmann, Thomas, White, 2017, in prep.)

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Masses and SFRs

Over all shape of the stellar mass function is unaffected because changing the SFE just moves everything left or right. SFRs of low mass galaxies are higher, because there is no surface density threshold for star formation.

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Cold Gas Properties

you can have less gas and still form stars

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Structural Properties

A model in which the sizes are given by the angular momentum of the halo works. morphologies not terrible either

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Stellar and Gas Phase Metallicities

Gradients are not as steep as observed. Can be if we blow out all the metals in low mass galaxies, but then normalisation too low. Do we trust the normalization?

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Gradients - Comparison with CALIFA

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Gradients - Comparison with MaNGA

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Summary

We now have a self-consistent analytic model of galaxy formation with resolved properties: cooling; HI and H2; H2 based SF; radial inflow; chemical enrichment Global properties look as good as in Henriques et al. 2015: SMFs, SFRs, sizes, morphologies, better gas properties. In low-mass galaxies there is a tension between global gas metallicity and flat gradients: need to blow out metals in the centre too low global metallicity