Galaxies on FIRE: Burning up the small-scale crises of ΛCDM

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Eleanor Carpenter
5 years ago
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Garrison-Kimmel (Einstein Fellow, Caltech) on behalf of Phil Hopkins

1 Galaxies on FIRE: Burning up the small-scale crises of ΛCDM Observed Starlight Molecular X-Rays Star Formation Cosmic evolution Shea Garrison-Kimmel (Einstein Fellow, Caltech) on behalf of Phil Hopkins (Caltech) and the FIRE Collaboration F RE Feedback In Realistic Environments

2 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!

3 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

4 Galaxy formation Gas Gas outflows cooling feedback (e.g. supernovae) angular momentum Gas Gas

5 Galaxy formation Galaxy formation involves an enormous dynamic range: >> 10 6 in length

6 ~10 10 pc Hubble volume ~ pc ~ pc Clusters, Large-scale structure Galaxy ~10-5 pc Stars, protostellar disks ~ pc Cores, clusters, Supernovae blastwaves ~ pc Molecular clouds, Star-Forming Regions

~10 10 pc Hubble volume ~10 7-10 8 pc ~10 4-5 pc

protostellar disks ~10-2 -10 0 pc Cores, clusters,

7 ~10 10 pc Hubble volume ~ pc ~ pc Clusters, Large-scale structure Galaxy ~10-5 pc Stars, protostellar disks ~ pc Cores, clusters, Supernovae blastwaves ~ pc Molecular clouds, Star-Forming Regions

FIRE (tries to) model the physics driving galaxy formation cosmological collapse hydrodynamics and gas cooling star formation in self-gravitating gas not to scale!

8 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

9 What are we studying with FIRE? galactic winds and the circumgalactic medium what are the smallest galaxies? what can we learn from Gaia? r-process enrichment the nature of how do stars form? dark matter distributions of compact objects the role of cosmic rays in galaxy formation gravitational wave sources (LISA) importance of magnetic fields supermassive black holes feedback drivers of galaxy morphology radiation/matter interactions predictions for next-gen telescopes origins of ultra-diffuse galaxies high-redshift galaxy formation (JWST) formation of globular clusters impact of baryons on dark matter growth of supermassive black holes cosmic history of the Milky Way the impact of reionization on dwarf galaxy predictions

10 What are we studying with FIRE?

11 Who is FIRE? PIs at ten institutions: Phil Hopkins, Caltech Norm Murray, CITA Eliot Quataert UC Berkeley Dusan Keres UC San Diego C.A. Faucher-Giguère Northwestern Andrew Wetzel UC Davis Robert Feldmann ETH Zurich James Bullock UC Irvine Mike Boylan-Kolchin UT Austin Chris Hayward CCA

12 Who is FIRE? plus students and postdocs

13 Small-scale problems Milky Way lives here What lives in all these?

14 Dwarf galaxies! LMC M =3x109 M Pegasus M =6x106 M Draco M =4x105 M Fornax M =4x107 M Sculptor M =4x106 M Eridanus II M =6x104 M WLM M =2x107 M Phoenix M =2x106 M Pictoris I M =3x103 M 200 pc Bullock & Boylan-Kolchin, 2017

15 Dwarf galaxies but not enough Theory: thousands of subhalos Observations: tens of satellite galaxies

16 The missing satellites problem Postulate: Maybe only the biggest dark matter clumps host (detectable) galaxies?

17 The missing satellites problem Corollary: The known galaxies should be compatible with the biggest clumps

18 The central mass problem rotation velocity (km/s) enclosed mass Dark Each matter-only point Aquarius is simulations (Springel+2008) a separate (real) Theory satellite galaxy Data: Milky Way sats radius (kpc) rotation velocity = sqrt[g M(<r)/r] Compare dynamical (total) masses to check

19 The central mass problem rotation velocity (km/s) enclosed mass Theory: structure around Milky Way-like hosts (gravity-only Aquarius sims, Springel+2008) Data: Milky Way sats 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 40 30 20 Theory: structure around Milky Way-like hosts (gravity-only Aquarius sims, Springel+2008) Data:

20 The central mass problem rotation velocity (km/s) enclosed mass Theory: structure around Milky Way-like hosts (gravity-only Aquarius sims, Springel+2008) Data: Milky Way sats 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)

21 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?

22 What are we studying with FIRE? galactic winds and the circumgalactic medium what are the smallest galaxies? what can we learn from Gaia? r-process enrichment the nature of how do stars form? dark matter distributions of compact objects the role of cosmic rays in galaxy formation gravitational wave sources (LISA) importance of magnetic fields supermassive black holes feedback drivers of galaxy morphology radiation/matter interactions predictions for next-gen telescopes origins of ultra-diffuse galaxies high-redshift galaxy formation (JWST) formation of globular clusters impact of baryons on dark matter growth of supermassive black holes cosmic history of the Milky Way the impact of reionization on dwarf galaxy predictions

23 What are we studying with FIRE? galactic winds and the circumgalactic medium what are the smallest galaxies? what can we learn from Gaia? r-process enrichment the nature of how do stars form? dark matter distributions of compact objects the role of cosmic rays in galaxy formation gravitational wave sources (LISA) importance of magnetic fields supermassive black holes feedback drivers of galaxy morphology radiation/matter interactions predictions for next-gen telescopes origins of ultra-diffuse galaxies high-redshift galaxy formation (JWST) formation of globular clusters impact of baryons on dark matter growth of supermassive black holes cosmic history of the Milky Way the impact of reionization on dwarf galaxy predictions

24 Tackling small-scale problems with the FIRE simulations ELVIS on FIRE and the Latte suites Isolated dwarf galaxies at ludicrous resolution Triple Latte 2000 kpc 0.75 kpc 300 kpc

galaxies (within ~1 Mpc of each host) Each simulation

25 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 Juliet Romeo

26 The missing satellites problem Number of galaxies brighter than Mstar N(> M ) 30 Satellites: r < 300 kpc stellar M mass [M[Msun] ] SGK+, in prep

27 The missing satellites problem Number of galaxies brighter than Mstar N(> M ) 30 Satellites: r < 300 kpc Milky Way stellar M mass [M[Msun] ] SGK+, in prep

28 The missing satellites problem Number of galaxies brighter than Mstar N(> M ) Satellites: r < 300 kpc stellar M mass [M[Msun] ] Andromeda Milky Way SGK+, in prep

29 The missing satellites problem Number of galaxies brighter than Mstar N(> M ) Satellites: r < 300 kpc stellar M mass [M[Msun] ] Andromeda Milky Way SGK+, in prep

30 The missing satellites problem Number of galaxies brighter than Mstar N(> M ) Satellites: r < 300 kpc stellar M mass [M[Msun] ] Andromeda Milky Way SGK+, in prep

31 No missing satellites problem! Number of galaxies brighter than Mstar N(> M ) Satellites: r < 300 kpc stellar M mass [M [Msun] ] Andromeda Milky Way SGK+, in prep

32 What about the central masses? Is the internal structure of the simulated dwarfs consistent with those observed? ELVIS on FIRE and the Latte suites Isolated dwarf galaxies at ludicrous resolution Triple Latte 2000 kpc 0.75 kpc 300 kpc

33 mgas 30 Msun equivalent to a single high mass star! First cosmological simulations (run to z = 0) to resolve the cooling radii of individual supernovae Ultra-high resolution isolated dwarf galaxies Density profiles resolved beyond ~30 parsecs Target isolated dwarfs systems in a void, far from any MW-mass galaxies Wheeler+, in prep

34 Internal structure of FIRE dwarfs circular velocity [km/s] And XVI Leo T Tucana And XXVIII Leo A And XVIII m10q M = M M total = M radius [kpc] NGC 6822 Pegasus Cetus IC 1613 WLM

35 Internal structure of FIRE dwarfs circular velocity [km/s] And XVI Leo T Tucana Gravity only And XXVIII Leo A And XVIII m10q M = M M total = M radius [kpc] NGC 6822 Pegasus Cetus IC 1613 WLM

36 Internal structure of FIRE dwarfs Gravity only FIRE

37 Internal structure of FIRE dwarfs Gravity only FIRE The MW-mass hosts of ELVIS on FIRE and Latte are also free of the central mass problem

38 Feedback induced cores FIRE Gravity only Wheeler+, in prep

39 Feedback induced cores, if there s enough energy FIRE Gravity only Gravity only FIRE Wheeler+, in prep

40 What about smaller galaxies? How do we push make predictions for the ultra-faint population around the Milky Way? ELVIS on FIRE and the Latte suites Isolated dwarf galaxies at ludicrous resolution Triple Latte 2000 kpc 0.75 kpc 300 kpc

Group) 1-5 million core-hours for Latte, 10-20 million for ELVIS on FIRE mgas,star = 880 Msun 1.

41 Triple Latte: a billion particles in the Milky Way Upcoming: Triple Latte Current: ELVIS on FIRE + Latte mgas 3,500-7,070 Msun ~100 million particles in the halo (and 300 million in the Local Group) 1-5 million core-hours for Latte, million for ELVIS on FIRE mgas,star = 880 Msun 1.1 billion particles ~25 million core-hours now running (at z=2.5) F RE Feedback In Realistic Environments

42 Andrew Wetzel Caltech - Carnegie - UC Davis cosmological hydrodynamic simulations of (better >) Milky Way-mass galaxies to z = 0 Triple Latte ELVIS on FIRE (double) Latte FIRE (single Latte) Agertz&Kravtsov GARROTXA Sawala Eris CLUES Auriga HR MAGICC Mollitor Massive GASOLINE Aquarius (AREPO) Black-IIEagle NIHAO Illustris 1 billion particles Mgas = 900 Msun (better >)

43 MW-mass progenitor at z = kpc (physical) min = 10 6 M /kpc 2

44 MW-mass progenitor at z = 2.5 HST image 300 kpc (physical) 6 2 min = 10 M /kpc

45 MW-mass progenitor at z = 2.5 HST image 300 kpc (physical) 3 2 min = 10 M /kpc

Triple Latte (currently running) will provide self-consistent predictions for ultra-faint dwarfs around the MW for the first time Conclusions FIRE simulations realistically capture the evolution

46 Triple Latte (currently running) will provide self-consistent predictions for ultra-faint dwarfs around the MW for the first time Conclusions FIRE simulations realistically capture the evolution of dwarf galaxies near the MW and in the Local Group Together with ultra-high res (~30 Msun) sims of isolated dwarfs, our results indicate that baryonic physics can explain the small-scale problems

47 [this slide intentionally left blank] [the above statement is a lie]

48 Conclusions FIRE simulations realistically capture the evolution of dwarf galaxies near the MW and in the Local Group Together with ultra-high res (~30 Msun) sims of isolated dwarfs, our results indicate that baryonic physics can explain the small-scale problems Triple Latte (currently running) will provide self-consistent predictions for ultra-faint dwarfs around the MW for the first time

49 Who is FIRE? PIs at ten institutions: Phil Hopkins (Caltech) Eliot Quataert (UC Berkeley) Dusan Keres (UC San Diego) C.A. Faucher-Giguère (Northwestern) Norm Murray (CITA) James Bullock (UC Irvine) Mike Boylan-Kolchin (UT Austin) Andrew Wetzel (UC Davis) Chris Hayward (CCA) Robert Feldmann (ETH Zurich) ~30-40 graduate students and postdocs Sarah Wellon mond Fielding Paul Torrey Cameron Hummels Shea Garrison-Kimmel

50 What are we studying with FIRE? galactic winds and high-redshift g the circumgalactic medium formation (JWS the smallest galaxies impact of b what can we on dark ma learn from Gaia? drivers of galaxy morphology growth of supermas importance of black hole magnetic fields the nature of distributions of dark matter compact objects predictions for gravitation next-gen telescopes sources (L

51 What are we studying with FIRE?

52 What are we studying with FIRE? Titles Abstracts

53 Galaxy formation Gas Gas cooling angular momentum Gas Gas

54 Galaxy formation Gas Gas outflows cooling feedback (e.g. supernovae) angular momentum Gas Gas

CDM Controversies. James Bullock (UC Irvine)

CDM Controversies. James Bullock (UC Irvine) CDM Controversies James Bullock (UC Irvine) Low stellar mass: feedback can t change DM Core Cusp Tollet et al. 2015 Also: Governato+12; Penarrubia+12; Garrison-Kimmel+13, Di Cintio+14 Low stellar mass: