Dark Matter Dictates the Stellar Envelopes of Super Massive - PowerPoint PPT Presentation

May 06, 2023 •118 likes •326 views

Dark Matter Dictates the Stellar Envelopes of Super Massive Galaxies Song Huang Song Huang (UC Santa Cruz) Alexie Leauthaud (UC Santa Cruz) Felipe Ardila, Jenny Greene, Andrew Hearin, Peter Behroozi, Benedikt Diemer, Annalisa Pillepich and

Dark Matter Dictates the Stellar Envelopes of Super Massive Galaxies Song Huang Song Huang (UC Santa Cruz) Alexie Leauthaud (UC Santa Cruz) Felipe Ardila, Jenny Greene, Andrew Hearin, Peter Behroozi, Benedikt Diemer, Annalisa Pillepich and the HSC collaboration
Dark Matter Dictates Accretion onto Massive Galaxies HSC
HSC survey Wide + Deep + Lensing Rare objects Dark Matter Halos Faint outskirts
A Large Sample of Super Massive Galaxies 3000 galaxies with M * >10 11.6 M ⊙ 0.2 < redshift < 0.5 1D surface brightness profile M 100 M 10
Stellar Profiles of Super Massive Galaxies Profiles detected to 100 kpc for individual galaxies no stacking! 28 mag/arcsec 2 Huang et al. 2018a
Stellar Profiles of Super Massive Galaxies 1. Massive Galaxies are not self similar   2. Large scatter in the outskirts (can be measured in HSC!)   Intrinsic scatter 3. Diversity of massive galaxy outskirts
I n t r i n s i c s c a t t e r Is the scatter amongst profiles (diversity of stellar envelopes) connected to dark matter halo mass? Assembly of outer galaxy ⇔ assembly of dark matter halo?
Galaxy galaxy weak lensing Measures the coherent distortion pattern in the shapes of background galaxies Directly measures the dark matter halo mass of galaxies ensembles ΔΣ [M ⊙ /pc 2 ] R R [Mpc]
M 10kpc and M 100kpc Masses
M 10kpc and M 100kpc Masses M 100
M 10kpc and M 100kpc Masses M 10 M 100
Diversity of Stellar Envelopes M 10 M 100 (or M max )
Diversity of Stellar Envelopes M 10 M 100 (or M max )
M10 ⟺ M100 ⟺ M halo
M10 ⟺ M100 ⟺ M halo How is halo mass (M halo ) extracted from the lensing signal? Full forward model Semi-empirical galaxy model “the Universe Machine” (Behroozi et al 2018) ⟺
Larger Envelopes = Larger Dark Matter Halo (Halo mass dependence of the mass-size relation) In situ Ex situ
Top 1/3 Mass within 10 kpc Middle 1/3 Bottom 1/3 Mass within 100 kpc Huang et al. 2018c in prep
Conclusions HSC detects lights of super massive galaxies to 100 kpc Super massive galaxies are not self similar - diversity of stellar envelopes Weak lensing ⇒ strong correlation between amplitudes/slopes of light profiles and dark matter halo mass References:   Huang et al. 2018a arXiv:1707.01904   Huang et al. 2018b arXiv:1803.02824   Huang et al. 2018c in prep Detailed comparison between HSC and hydro simulations - Felipe Ardila’s talk on Thursday

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