Relations between the Sizes of Galaxies and Their Dark Matter Halos at Redshifts 0 <z <3

Kuang Han Huang, S. Michael Fall, Henry C. Ferguson, Arjen Van Der Wel, Norman Grogin, Anton Koekemoer, Seong-Kook Lee, Pablo G. Pérez-González, Stijn Wuyts

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We derive relations between the effective radii R eff of galaxies and the virial radii R 200c of their dark matter halos over the redshift range 0 <z <3. For galaxies, we use the measured sizes from deep images taken with Hubble Space Telescope for the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey; for halos, we use the inferred sizes from abundance matching to cosmological dark matter simulations via a stellar mass-halo mass (SMHM) relation. For this purpose, we derive a new SMHM relation based on the same selection criteria and other assumptions as for our sample of galaxies with size measurements. As a check on the robustness of our results, we also derive R eff-R 200c relations for three independent SMHM relations from the literature. We find that galaxy R eff is proportional on average to halo R 200c, confirming and extending to high redshifts the z = 0 results of Kravtsov. Late-type galaxies (with low Sérsic index and high specific star formation rate (sSFR)) follow a linear R eff-R 200c relation, with effective radii at 0.5 <z <3 close to those predicted by simple models of disk formation; at z <0.5, the sizes of late-type galaxies appear to be slightly below this prediction. Early-type galaxies (with high Sérsic index and low sSFR) follow a roughly parallel R eff-R 200c relation, ∼0.2-0.3 dex below the one for late-type galaxies. Our observational results, reinforced by recent hydrodynamical simulations, indicate that galaxies grow quasi-homologously with their dark matter halos.

Original languageEnglish
Article number6
JournalAstrophysical Journal
Issue number1
Publication statusPublished - 17 Mar 2017


  • galaxies: evolution
  • galaxies: high-redshift
  • galaxies: structure
  • methods: data analysis

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science


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