Theoretical Cosmology and Galaxy Formation at UMD
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1 Theoretical Cosmology and Galaxy Formation at UMD Massimo Ricotti (Associate Professor, Dept. of Astronomy) Current group members: Owen Parry (Postdoc) Sam Leithner (CTC postdoc) Emil Polisensky (PhD student) Kari Helgason (PhD student) Harley Katz (undergraduate student) Previous PhD students: KwangHo Park (Postdoc, Carnegie Mellon University) Mia Bovill (Postdoc, U of Texas, Austin)
2 Computational/Theoretical Astrophysics Main scientific interest: understanding the beginning of structure formation in the universe and the effects on the subsequent cosmic evolution. Some of the questions my research is focusing on: How small and numerous were the the first galaxies? How many survived to the present? What is the origin of today s supermassive black holes? What is the origin of globular clusters? What reionized the universe? Topics and Subtopics: 1. Galaxy Formation/Early Universe/First Stars and BHs Radiative/chemical feedback Dark matter simulations NIR background fluctuations 2. Connection to Near Field Cosmology 3. Reionization of the Intergalactic Medium Ly-alpha forest Sources of reionization: role of GCs and X-rays Primordial BHs and CMB, etc
3 Sample of past/ongoing research projects Emil Polinsesky: Testing CDM. Simulations of the Milky Way in CDM and WDM; minihalos in voids at z=0 Kari Helgason: Detecting the First Light. NIR background fluctuations, in collaboration with Alexander Kashlinsky Owen Parry: The ISM in the First Galaxies Previous students: Mia Bovill: The Quest for the Fossils of the first galaxies UT Austin, U Cattolica) KwangHo Park: Growth of the First Seed Black Holes. Simulations of accretion onto IMBH with rad. transfer Carnegie Mellon)
4 The Missing Satellites Klypin et al 1999, More et al 1999 Aquarius Simulation (Springel et al, 2008) Figure credit: Grebel There should be thousands of dwarf satellites around the Milky Way. However, as of 2005 only about 30 satellites known in LG.
5 Warm Dark Matter Cold Warmer Warmer yet Warmest
6
7 Reionization feedback on dwarf galaxy formation The reionization feedback idea is valid but fails at z<2 if the halo is highly concentrated Minihalos virialized before reionization, that evolve to z=0 in the low-density IGM, have a late phase of gas accretion and possibly star formation Do these objects exist? SFR SFR AGE AGE
8 Detecting minihalos in voids
9 Simulations of the first galaxies Feedback-regulated galaxy formation 1 Mpc box size 10 3 M sun mass res. 3D radiative transfer Run ends at redshift of reionization Ref: Ricotti, Gnedin & Shull 2002
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11 Simulating Fossils of First Galaxies The final pre-reionization output is transformed in a 1 Mpc 3 box of particles. We duplicate this box, adding perturbations to account for density variations with l > 1 Mpc. Each HR particle in the resulting N- body simulation represents a prereionization halo. Unique IDs allow us to retrieve the stellar properties at z = 0.
12 Where are the fossil Galaxies today?
13 Pre-reionization fossils and ultrafaint dsphs: a model prediction! Willman I de dirr old M31 dsph new M31 dsph old Milky Way dsph new Milky Way dsph RG05 prediction Willman I Ref: Ricotti & Gnedin 05, Bovill & Ricotti 09
14 More work with LSST We now have z=0 halos which reproduce the faintest and smallest ultrafaints! Yet undiscovered population
15 Sources of Reionization 1. Role of globular clusters (with Harley Katz, undergraduate) 2. Constraints from IR background fluctuations (Kari Helgason) 3. X-ray pre-ionization: redshifted X-ray background Accretion onto intermediate mass black holes with radiation feedback (KwangHo Park) 4. Primordial black holes
16 Bondi accretion with radiation feedback 100 M solar IMBH Park & Ricotti 2011 Gas density Ionization fraction
17 Accretion rate Park & Ricotti 2011 See also Milosavljevic et al 2008
18 Two Distinct Modes of Oscillations Mode-I n = 10 6 cm -3 Mode-II n = 10 7 cm -3
19 Moving BH + Radiative Feedback 5/21/2010
20 Modeling based on Simulations: 1. Transition from R-type to D- type ionization front 2. Isothermal bow-shock 3. Thin shell instability produce periodic accretion rate D-type R-type
21 Shell instability and periodic oscillations
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