1 / 19

The Population III Connection Jonathan Devor

The Population III Connection Jonathan Devor. Outline. GRBs as Cosmological Probes: Why is this interesting? Population III – A brief historical overview The primordial IMF Stars: Then and now Supernovae What can we hope to see? The road ahead.

trent
Download Presentation

The Population III Connection Jonathan Devor

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. The Population III ConnectionJonathan Devor

  2. Outline • GRBs as Cosmological Probes: Why is this interesting? • Population III – A brief historical overview • The primordial IMF • Stars: Then and now • Supernovae • What can we hope to see? • The road ahead

  3. GRBs as Cosmological Probes: Why is this interesting? • Cosmological model • Big bang nucleosynthesis • First stars (population III) • Galactic formation • Reionization epoch • Early IGM metallicity enhancement

  4. Population III – A brief historical overview • (Baade 1944) – star populations: Pop. I: Sun-like (1 - 2% metals by mass) Pop. II: Globular cluster-like (0.01 – 0.1%) Pop. III: No metals (actually < 0.001%) • (Schwarzschild et al. 1953): First model for pop. III stars (far less complex than type I stars in a modern environment)

  5. Ongoing work • 1980’s: Cosmological consequences- • Effects on CMB (SZ effect) • “Primordial” abundances of Helium • “Pregalactic metal enrichment” • Reionization epoch • Effects on early galactic formation • 1990’s: clump/star formation • 2000’s: WMAP, Swift, JWST

  6. Space Missions… • BATSE (1991-2000) = Burst and Transient Source Experiment [5-1,500 keV ] • WMAP (2003-) = Wilkinson Microwave Anisotropy Probe [22-90 GHz] • Swift (2004-) • JWST (2011-) = James Webb Space Telescope • EXIST =Energetic X-ray Imaging Survey Telescope 5-100 KeV: x10-20 better than Swift 100-600 KeV: x300 better than HEAO-A3 survey

  7. CDM at z=17 Taken from (Yoshida 2003) Taken from Swift website

  8. Primordial gas Adiabatic H2 cooling Stable point Gravity compression Taken from (Bromm 2002) Lingers at: T~200K

  9. Jean’s instability criterion

  10. Protostellar collapse • No dust, no metal – need H2 as coolent - Free electron catalyzer (feedback from UV) - 3-body channel  Clump breakup • Radiation pressure dominated (very low opacity- electron scatter) • Halo breakup Nstar ~ 1-5 (if N=1, problem getting rid of the angular momentum)

  11. Clump evolution Taken from (Omukai 1998)

  12. Growth of protostar Taken from (Omukai 2003) The accretion is effectively shut off at some critical value because of the dramatic increase in radius

  13. Pop. III supernovae • Life time:

  14. Pop. III star – remnant SPH simulation 400 pc metals fragmentation Taken from (Bromm 2003)

  15. Reionization Taken from (Wyithe 2003) Though comparable in brightness, GRB afterglows release less energy than quasars into the IGM (ionizes M of hydrogen). So they have a negligible effect on their environment (with the exception of dwarf galaxies )

  16. What can we see? With Swift, 10-25% of GRB afterglows will come from z > 5 That is, about a dozen a year! All GRBs Swift BATSE Taken from (Bromm 2002) Taken from (Lamb 2002)

  17. The road ahead – open questions • Do pop. III stars exist? Need observations!!! (Swift?) • Do their supernovae make GRBs? (quenching?) • Primordial environment • Primordial IMF / star formation history (GRB redshift distribution) • Early cosmological formation (filaments, galaxies) • “Extreme physics” (SNe, MBH)

  18. Some references • Historical: • Schwarzschild M.,”Inhomogeneous Stellar Models. III. Models with Partially Degenerate Isothermal Cores.”, 1953, Astrophysical Journal, vol. 118, p.326 • Survey papers: - Bromm V. and Larson R., “The First Stars”, 2003, astro-ph/0311019 - Bromm V., “The First Sources of Light‘, asyro-ph/0211292 - Lamb D., “Gamma-Ray Bursts as a Probe of Cosmology”, 2002, astro-ph/0210434 - Loeb A. and Barkana R.,”The reionization of the Universe by the First stars and Quasars”, Annu. Rev. Astron. Astrophys., 2001, 39:19-66 - Loeb A., “Observing the First Stars, One Star a Time”, 2003, astro-ph/0307231

  19. The Swift Song We know that gamma ray explosions happen randomly all over the sky (It's like a lottery: a ticket for each square degree) You see a FLASH! and then there's not another till about a day has gone by (But that depends upon detector sensitivity) In just a moment they spew energy worth (That's pretty fast) A value we can't even fathom on Earth (It's really vast!) But just what's giving rise to gamma ray sparked skies? Is it the death cry of a massive star or black hole birth? (Or both, or both? or both!) Chorus: Swiftly swirling, gravity twirling Neutron stars about to collide Off in a galaxy so far away Catastrophic interplay A roller coaster gamma ray ride Superbright explosion then Never to repeat again How are we supposed to know? How about a telescope rotation Swiftly onto the location Of its panchromatic afterglow?

More Related