THE COSMOLOGIAL PHYSICS OF STAR-FORMING GALAXIES
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1 THE COSMOLOGIAL PHYSICS OF STAR-FORMING GALAXIES AND THE GAMMA-RAY BACKGROUND Brian Fields University of Illinois High-Energy Impact on Cosmology, KICP, Oct
2 Collaborators Tijana Prodanovic U of Novi Sad Vasiliki Pavlidou Caltech Amy Lien U Illinois Richard Cyburt Michigan State U John Beacom Ohio State U Keith Olive U Minnesota
3 THE COSMOLOGIAL PHYSICS OF STAR-FORMING GALAXIES AND THE GAMMA-RAY BACKGROUND -Conclusions- star formation guaranteed gamma rays Fermi/GLAST near field : Milky Way spectrum: feature! calibrates extragalactic signal will detect Local Group galaxies: tests calibration (cosmic rays) star-forming galaxies imprint feature in diffuse gamma sky impact on cosmological physics star-formation gamma rays & the primordial Li problem High-Energy Impact on Cosmology, KICP, Oct
4 THE COSMOLOGIAL PHYSICS OF STAR-FORMING GALAXIES AND THE GAMMA-RAY BACKGROUND -Conclusions- star formation guaranteed gamma rays Fermi/GLAST near field : Milky Way spectrum: feature! calibrates extragalactic signal will detect Local Group galaxies: tests calibration (cosmic rays) star-forming galaxies imprint feature in diffuse gamma sky impact on cosmological physics star-formation gamma rays & the primordial Li problem High-Energy Impact on Cosmology, KICP, Oct
5 Guaranteed Gamma-Rays from Star-Forming Galaxies star formation supernova explosions supernova shocks accelerate cosmic rays Fermi/GLAST First Light Image cosmic-ray propagation in ISM ergo... pp π 0 γγ gamma-rays star formation (hadronic=pionic) gamma rays gamma-rays probe star formation cosmic-ray acceleration
6 Excessive? Hadronic Cosmic Rays: Unambiguous hadronic spectral signature: Stecker ; Dermer 1986 pp π 0 γγ symmetry about m(π 0 )/2 EGRET & Milagro Prodanovic, BDF, Beacom 2006
7 Excessive? Hadronic Cosmic Rays: Unambiguous hadronic spectral signature: Stecker ; Dermer 1986 pp π 0 γγ symmetry about pion bump EGRET & Milagro Prodanovic, BDF, Beacom 2006 m(π 0 )/2
8 Excessive? Hadronic Cosmic Rays: Unambiguous hadronic spectral signature: Stecker ; Dermer 1986 pp π 0 γγ symmetry about pion bump EGRET: a feature! EGRET & Milagro Prodanovic, BDF, Beacom 2006 m(π 0 )/2
9 Excessive? Hadronic Cosmic Rays: Unambiguous hadronic spectral signature: Stecker ; Dermer 1986 pp π 0 γγ symmetry about pion bump EGRET: a feature! EGRET & Milagro Prodanovic, BDF, Beacom 2006 m(π 0 )/2...but not pion bump: masked by GeV excess GeV excess?
10 Excessive? Hadronic Cosmic Rays: Unambiguous hadronic spectral signature: Stecker ; Dermer 1986 pp π 0 γγ symmetry about pion bump EGRET: a feature! EGRET & Milagro Prodanovic, BDF, Beacom 2006 m(π 0 )/2 GeV excess?...but not pion bump: masked by GeV excess Milagro: diffuse TeV signal inconsistent w/ local cosmic rays Unresolved point sources? TeV excess?
11 Excessive? Hadronic Cosmic Rays: Unambiguous hadronic spectral signature: Stecker ; Dermer 1986 pp π 0 γγ symmetry about pion bump EGRET: a feature! EGRET & Milagro Prodanovic, BDF, Beacom 2006 m(π 0 )/2 GeV excess?...but not pion bump: masked by GeV excess Milagro: diffuse TeV signal inconsistent w/ local cosmic rays Unresolved point sources? Puzzles cry out for Fermi/ACTs! TeV excess?
12 Gamma-Ray Tests & Calibration of Star-Formation/Supernova Observable: gamma-ray flux Laboratory: the Local Group Cosmic Rays Pavlidou & BDF 2001 F γ = EGRET Ṅγ 4πr 2 Ṅ γ = Φ p σ M gas m p only LMC detected (marginally) gamma flux consistent with Φ p R SN
13 Gamma-Ray Tests & Calibration of Star-Formation/Supernova Observable: gamma-ray flux Laboratory: the Local Group Cosmic Rays Pavlidou & BDF 2001 F γ = EGRET Ṅγ 4πr 2 Ṅ γ = Φ p σ M gas m p only LMC detected (marginally) gamma flux consistent with Fermi/GLAST Φ p R SN strong detection of LMC, SMC, M31
14 Gamma-Ray Tests & Calibration of Star-Formation/Supernova Observable: gamma-ray flux Laboratory: the Local Group Cosmic Rays Pavlidou & BDF 2001 F γ = EGRET Ṅγ 4πr 2 Ṅ γ = Φ p σ M gas m p only LMC detected (marginally) gamma flux consistent with Fermi/GLAST Φ p R SN strong detection of LMC, SMC, M31 possible detection of M33
15 Gamma-Ray Tests & Calibration of Star-Formation/Supernova Observable: gamma-ray flux Laboratory: the Local Group Cosmic Rays Pavlidou & BDF 2001 F γ = EGRET Ṅγ 4πr 2 Ṅ γ = Φ p σ M gas m p only LMC detected (marginally) gamma flux consistent with Fermi/GLAST Φ p R SN strong detection of LMC, SMC, M31 possible detection of M33 tests star-formation/gamma-ray link: supernova acceleration, confinement in spirals, dwarfs
16 Cosmic-Ray Sources Across the Star-Forming Universe Lichti, Bignami, & Paul 1978; Pavlidou & BDF 2002 Modeling the cosmic history of cosmic-ray interactions supernovae as cosmic-ray sources interstellar medium as targets
17 Cosmic-Ray Sources Across the Star-Forming Universe Lichti, Bignami, & Paul 1978; Pavlidou & BDF 2002 Modeling the cosmic history of cosmic-ray interactions supernovae as cosmic-ray sources interstellar medium as targets both fixed by cosmic star formation rate Hopkins & Beacom 2006
18 Cosmic-Ray Sources Across the Star-Forming Universe Lichti, Bignami, & Paul 1978; Pavlidou & BDF 2002 Modeling the cosmic history of cosmic-ray interactions supernovae as cosmic-ray sources interstellar medium as targets both fixed by cosmic star formation rate normalize to Milky Way CR/SN efficiency Hopkins & Beacom 2006
19 Cosmic-Ray Sources Across the Star-Forming Universe Lichti, Bignami, & Paul 1978; Pavlidou & BDF 2002 Modeling the cosmic history of cosmic-ray interactions supernovae as cosmic-ray sources interstellar medium as targets both fixed by cosmic star formation rate normalize to Milky Way CR/SN efficiency Results Pavlidou & BDF star-forming galaxies: a feature! peak ~0.5 GeV offset from MW peak: distinguishable
20 Cosmic-Ray Sources Across the Star-Forming Universe Lichti, Bignami, & Paul 1978; Pavlidou & BDF 2002 Modeling the cosmic history of cosmic-ray interactions supernovae as cosmic-ray sources interstellar medium as targets both fixed by cosmic star formation rate normalize to Milky Way CR/SN efficiency Results Pavlidou & BDF star-forming galaxies: a feature! peak ~0.5 GeV offset from MW peak: distinguishable near peak, ~30% of EGRET background (AGN)
21 Cosmic-Ray Sources Across the Star-Forming Universe Lichti, Bignami, & Paul 1978; Pavlidou & BDF 2002 Modeling the cosmic history of cosmic-ray interactions supernovae as cosmic-ray sources interstellar medium as targets both fixed by cosmic star formation rate normalize to Milky Way CR/SN efficiency Results Pavlidou & BDF star-forming galaxies: a feature! peak ~0.5 GeV offset from MW peak: distinguishable near peak, ~30% of EGRET background (AGN) GLAST: more AGN resolved galaxy peak emerges
22 Cosmic-Ray Sources Across the Star-Forming Universe Lichti, Bignami, & Paul 1978; Pavlidou & BDF 2002 Modeling the cosmic history of cosmic-ray interactions supernovae as cosmic-ray sources interstellar medium as targets both fixed by cosmic star formation rate normalize to Milky Way CR/SN efficiency Results Pavlidou & BDF star-forming galaxies: a feature! peak ~0.5 GeV offset from MW peak: distinguishable near peak, ~30% of EGRET background (AGN) GLAST: more AGN resolved galaxy peak emerges
23 Cosmic-Ray Sources Across the Star-Forming Universe Lichti, Bignami, & Paul 1978; Pavlidou & BDF 2002 Modeling the cosmic history of cosmic-ray interactions supernovae as cosmic-ray sources interstellar medium as targets both fixed by cosmic star formation rate normalize to Milky Way CR/SN efficiency Results Pavlidou & BDF star-forming galaxies: a feature! peak ~0.5 GeV offset from MW peak: distinguishable near peak, ~30% of EGRET background (AGN) GLAST: more AGN resolved galaxy peak emerges
24 Gamma Signal from Starbursts Individual starbursts: Torres, Reimer,Domingo-Santamaría, & Diegel 2004 farther than Local Group but very high star-formation rates 13 sources likely observable by GLAST Cosmic starbursts: Thomson, Quataert, & Waxman 2007 dominate star formation at z>1 Contribute ~50% of star-forming EGRB key assumption: starbursts gammas are cosmic-ray calorimeters : collisional pion production dominates energy losses
25 The Payoff: Impact on Cosmological Physics With observed signal from star-forming, cosmic-ray accelerating galaxies:
26 The Payoff: Impact on Cosmological Physics With observed signal from star-forming, cosmic-ray accelerating galaxies: measure of cosmic star-formation rate but other direct probes available Lien talk which allows gamma-rays to... Prodanovic, Pavlidou, & BDF
27 The Payoff: Impact on Cosmological Physics With observed signal from star-forming, cosmic-ray accelerating galaxies: measure of cosmic star-formation rate but other direct probes available Lien talk which allows gamma-rays to... probe supernova nonthermal energy injection into Prodanovic, Pavlidou, & BDF
28 The Payoff: Impact on Cosmological Physics With observed signal from star-forming, cosmic-ray accelerating galaxies: measure of cosmic star-formation rate but other direct probes available Lien talk which allows gamma-rays to... probe supernova nonthermal energy injection into Prodanovic, Pavlidou, & BDF cosmic-ray energy deposition: collisions vs escape nonthermal pressure in intracluster medium Pavlidou & BDF 2006
29 The Payoff: Impact on Cosmological Physics With observed signal from star-forming, cosmic-ray accelerating galaxies: measure of cosmic star-formation rate but other direct probes available Lien talk which allows gamma-rays to... probe supernova nonthermal energy injection into Prodanovic, Pavlidou, & BDF cosmic-ray energy deposition: collisions vs escape nonthermal pressure in intracluster medium Star-forming galaxy signals are foreground to exotica cosmological cosmic rays Keshet talk dark matter annihilation Pavlidou & BDF 2006
30 Fermi/GLAST Impact Extragalactic diffuse background sensitivity, angular resolution: better foreground separation intensity, spectrum probes normal galaxies AGN resolved foreground lowers AGB background contribution, galaxies stand out Local Galaxies Multiple Local Group galaxy detections tests cosmic-ray dependence on local environment (star formation) and universality of cosmic-ray confinement Milky Way better diffuse/point source separation identification of pion bump? High-Energy Impact on Cosmology, KICP, Oct
31 THE COSMOLOGIAL PHYSICS OF STAR-FORMING GALAXIES AND THE GAMMA-RAY BACKGROUND -Conclusions- star formation guaranteed gamma rays Fermi/GLAST near field : Milky Way spectrum: feature! calibrates extragalactic signal will detect Local Group galaxies: tests calibration (cosmic rays) star-forming galaxies imprint feature in diffuse gamma sky impact on cosmological physics star-formation gamma rays & the primordial Li problem High-Energy Impact on Cosmology, KICP, Oct
32 THE COSMOLOGIAL PHYSICS OF STAR-FORMING GALAXIES AND THE GAMMA-RAY BACKGROUND -Conclusions- star formation guaranteed gamma rays Fermi/GLAST near field : Milky Way spectrum: feature! calibrates extragalactic signal will detect Local Group galaxies: tests calibration (cosmic rays) star-forming galaxies imprint feature in diffuse gamma sky impact on cosmological physics star-formation gamma rays & the primordial Li problem High-Energy Impact on Cosmology, KICP, Oct
33 Paleolithography: Lithium Probes of Cosmic-Ray History Prodanovic & BDF Hadronic gamma production inevitably means lithium synthesis Observables gammas: measure mean CR fluence across universe lithium abundance: measures local CR fluence Li γ Complementary: use one to probe the other ΦCR (local) dt ΦCR (γpath) dt
34 Paleolithography: Lithium Probes of Cosmic-Ray History Prodanovic & BDF Hadronic gamma production pp π 0 γγ inevitably means lithium synthesis αα 6 Li + Observables gammas: measure mean CR fluence across universe lithium abundance: measures local CR fluence Li γ Complementary: use one to probe the other ΦCR (local) dt ΦCR (γpath) dt
35 Primordial Nucleosynthesis: The Lithium Problem Cyburt, BDF, Olive 2003, 2008
36 Predict: BBN theory: abundances vs baryon density WMAP baryons (blue) Primordial Nucleosynthesis: The Lithium Problem Cyburt, BDF, Olive 2003, 2008 BBN+CMB abundances Compare with Observations (yellow)
37 Predict: BBN theory: abundances vs baryon density WMAP baryons (blue) Primordial Nucleosynthesis: The Lithium Problem Cyburt, BDF, Olive 2003, 2008 BBN+CMB abundances Compare with Observations (yellow) Results: D agreement excellent: woo hoo!
38 Predict: BBN theory: abundances vs baryon density WMAP baryons (blue) Primordial Nucleosynthesis: The Lithium Problem Cyburt, BDF, Olive 2003, 2008 BBN+CMB abundances Compare with Observations (yellow) Results: D agreement excellent: woo hoo! 7 Li discordant: factor 4-5, 5sigma systematic errors in obs? theory? new physics?
39 Star-Forming Galaxies and the Lithium Problem Ryan, Olive, Beers, BDF, Norris 2000; Pavlidou & Fields 2006 Cosmic rays pollute primordial Li 7 Li observed = 7 Li CR + 7 Li BBN But 6 LiBeB GCR Infer true 7 Li BBN! 6,7 Li GCR How to calibrate for galactic, pre-galactic Lithium? use gamma/li dosimetry! diffuse pionic background galactic, pre-galactic(?) Li production Sharpens Li observations! But... makes WMAP Li problem worse! 14
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