Galaxies on FIRE : Burning up the small-scale crises of Λ CDM Observed Starlight Molecular X-Rays Star Formation Cosmic evolution Shea Garrison-Kimmel (Einstein Fellow, Caltech) F RE on behalf of Phil Hopkins (Caltech) and the FIRE Collaboration Feedback In Realistic Environments
What is FIRE ? galaxy formation? Standard paradigm: • Dark matter dominates the total mass Some type of mass that only (strongly) interacts via gravity ( i.e., collisionless: no EM forces, no pressure ) • Density field is initially very smooth, with only tiny fluctuations seeded during inflation • Gravity causes these fluctuations to grow, starting with the smallest ones This is (physically) easy to simulate!
Evolution of a Milky Way-like object Diemand, Kuhlen, & Madau 2006 But this is only gravity , and we know there’s other physics important for galaxy formation
Galaxy formation Gas Gas cooling outflows feedback (e.g. supernovae) angular momentum Gas Gas
Galaxy formation Galaxy formation involves an enormous dynamic range: >> 10 6 in length
~10 10 pc ~10 7 -10 8 pc ~10 4-5 pc Hubble volume Clusters, Large-scale structure Galaxy ~10 1 -10 2 pc ~10 -2 -10 0 pc ~10 -5 pc Molecular clouds, Cores, clusters, Stars, protostellar disks Star-Forming Regions Supernovae blastwaves
~10 10 pc ~10 7 -10 8 pc ~10 4-5 pc Hubble volume Clusters, Large-scale structure Galaxy ~10 1 -10 2 pc ~10 -2 -10 0 pc ~10 -5 pc Molecular clouds, Cores, clusters, Stars, protostellar disks Star-Forming Regions Supernovae blastwaves
FIRE (tries to) model the physics driving galaxy formation cosmological collapse hydrodynamics and gas cooling star formation in self-gravitating gas not to scale! energy return from stars (feedback), based on the results of stellar evolution studies: — stellar winds — radiative feedback — supernovae types Ia and II M. Grudic+2016
What are we studying with FIRE? galactic winds and the circumgalactic medium what are the high-redshift galaxy smallest galaxies? formation (JWST) the role of cosmic rays in galaxy formation drivers of galaxy impact of baryons morphology what can we on dark matter learn from Gaia? importance of growth of magnetic fields radiation/matter supermassive interactions r-process enrichment black holes the nature of origins of how do stars form? dark matter ultra-di ff use galaxies cosmic history of distributions of the Milky Way supermassive compact objects black holes feedback formation of globular clusters gravitational wave predictions for sources (LISA) next-gen telescopes the impact of reionization on dwarf galaxy predictions
What are we studying with FIRE?
Who is FIRE? PIs at ten institutions: Phil Hopkins, Caltech Norm Murray, CITA C.A. Faucher-Giguère Andrew Wetzel Dusan Keres Northwestern UC Davis UC San Diego Robert Feldmann ETH Zurich Eliot Quataert UC Berkeley Mike Boylan-Kolchin Chris Hayward James Bullock UT Austin CCA UC Irvine
Who is FIRE? plus 35 - 45 students and postdocs
Small-scale problems What lives in Milky Way all these? lives here
Dwarf galaxies! LMC Fornax WLM M ★ =3x10 9 M ⊙ M ★ =4x10 7 M ⊙ M ★ =2x10 7 M ⊙ Pegasus Sculptor Phoenix M ★ =6x10 6 M ⊙ M ★ =4x10 6 M ⊙ M ★ =2x10 6 M ⊙ Draco Eridanus II Pictoris I Bullock & 200 pc M ★ =4x10 5 M ⊙ M ★ =6x10 4 M ⊙ M ★ =3x10 3 M ⊙ Boylan-Kolchin, 2017
Dwarf galaxies…but not enough Theory : thousands of Observations : tens of “subhalos” “satellite galaxies”
The missing satellites problem Postulate : Maybe only the biggest dark matter clumps host (detectable) galaxies?
The missing satellites problem Corollary : The known galaxies should be compatible with the biggest clumps
The central mass problem rotation velocity (km/s) ∝ enclosed mass 50 Each point is Dark matter-only Aquarius 40 simulations (Springel+2008) a separate (real) Theory satellite galaxy 30 20 Data: Milky Way sats 10 0.1 0.3 0.6 1.0 radius (kpc) rotation velocity = sqrt[G M(<r)/r] Compare dynamical (total) masses to check
The central mass problem rotation velocity (km/s) ∝ enclosed mass 50 Theory: structure around 40 Milky Way-like hosts (gravity-only Aquarius sims, Springel+2008) 30 20 Data: Milky Way sats 10 0.1 0.3 0.6 1.0 radius (kpc) rotation velocity = sqrt[G M(<r)/r] Big clumps (which are “too big to fail” to form stars) have too much central mass to host the bright galaxies
The central mass problem rotation velocity (km/s) ∝ enclosed mass 50 Theory: structure around 40 Milky Way-like hosts (gravity-only Aquarius sims, Springel+2008) 30 20 Data: Milky Way sats 10 0.1 0.3 0.6 1.0 radius (kpc) rotation velocity = sqrt[G M(<r)/r] CAVEAT: these curves are from a gravity-only sim that ignores known physics (i.e. galaxy formation)
Can known, standard model physics that aren’t included in gravity-only simulations resolve the “missing satellites” and “central mass” problems? …or do we need to invoke “new physics”?
What are we studying with FIRE? galactic winds and the circumgalactic medium what are the high-redshift galaxy smallest galaxies? formation (JWST) the role of cosmic rays in galaxy formation drivers of galaxy impact of baryons morphology what can we on dark matter learn from Gaia? importance of growth of magnetic fields radiation/matter supermassive interactions r-process enrichment black holes the nature of origins of how do stars form? dark matter ultra-di ff use galaxies cosmic history of distributions of the Milky Way supermassive compact objects black holes feedback formation of globular clusters gravitational wave predictions for sources (LISA) next-gen telescopes the impact of reionization on dwarf galaxy predictions
What are we studying with FIRE? galactic winds and the circumgalactic medium what are the high-redshift galaxy smallest galaxies? formation (JWST) the role of cosmic rays in galaxy formation drivers of galaxy impact of baryons morphology what can we on dark matter learn from Gaia? importance of growth of magnetic fields radiation/matter supermassive interactions r-process enrichment black holes the nature of origins of how do stars form? dark matter ultra-di ff use galaxies cosmic history of distributions of the Milky Way supermassive compact objects black holes feedback formation of globular clusters gravitational wave predictions for sources (LISA) next-gen telescopes the impact of reionization on dwarf galaxy predictions
Tackling small-scale problems with the FIRE simulations ELVIS on FIRE and Isolated dwarf galaxies the Latte suites at ludicrous resolution Triple Latte 2000 kpc 0.75 kpc 300 kpc
ELVIS on FIRE and the Latte suite Ten Milky Way-mass galaxies, each with a population of nearby dwarf galaxies (within ~1 Mpc of each host) Each simulation spans ~10 6 parsecs while resolving ~1 pc scales Romeo Juliet
The missing satellites problem Number of galaxies brighter than M star 30 Satellites: r <300 kpc 20 15 10 N (> M ) 5 3 2 1 10 5 10 6 10 7 10 8 10 9 stellar mass [M sun ] M [ M ] SGK+, in prep
The missing satellites problem Number of galaxies brighter than M star 30 Satellites: r <300 kpc 20 15 10 Milky Way N (> M ) 5 3 2 1 10 5 10 6 10 7 10 8 10 9 stellar mass [M sun ] M [ M ] SGK+, in prep
The missing satellites problem Number of galaxies brighter than M star 30 Satellites: r <300 kpc 20 15 Andromeda 10 Milky Way N (> M ) 5 3 2 1 10 5 10 6 10 7 10 8 10 9 stellar mass [M sun ] M [ M ] SGK+, in prep
The missing satellites problem Number of galaxies brighter than M star 30 Satellites: r <300 kpc 20 15 Andromeda 10 Milky Way N (> M ) 5 3 2 1 10 5 10 6 10 7 10 8 10 9 stellar mass [M sun ] M [ M ] SGK+, in prep
The missing satellites problem Number of galaxies brighter than M star 30 Satellites: r <300 kpc 20 15 Andromeda 10 Milky Way N (> M ) 5 3 2 1 10 5 10 6 10 7 10 8 10 9 stellar mass [M sun ] M [ M ] SGK+, in prep
No missing satellites problem! Number of galaxies brighter than M star 30 Satellites: r <300 kpc 20 15 Andromeda 10 Milky Way N (> M ) 5 3 2 1 10 5 10 6 10 7 10 8 10 9 stellar mass [M sun ] stellar mass [M sun ] M [ M ] SGK+, in prep
What about the central masses? Is the internal structure of the simulated dwarfs consistent with those observed? ELVIS on FIRE and Isolated dwarf galaxies the Latte suites at ludicrous resolution Triple Latte 2000 kpc 0.75 kpc 300 kpc
Ultra-high resolution isolated dwarf galaxies • m gas ≃ 30 M sun — equivalent to a single high mass star! • First cosmological simulations (run to z = 0) to resolve the cooling radii of individual supernovae • Density profiles resolved beyond ~30 parsecs • Target isolated dwarfs — systems in a void, far from any MW-mass galaxies Wheeler+, in prep
Internal structure of FIRE dwarfs 40 Leo T And XVI And XVIII Leo A NGC 6822 Cetus Pegasus IC 1613 WLM 30 Tucana circular velocity [km/s] 20 And XXVIII 10 m10q M =3 × 10 6 M 7 M total =8.3 × 10 9 M 5 0.1 0.3 1 3 radius [kpc]
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