Cococubed.com Pop III with JWST
Home Astronomy research   Software Infrastructure:      MESA      FLASH      STARLIB      MESA-Web      starkiller-astro      My instruments   White dwarf supernova:      Remnant metallicities      Colliding white dwarfs      Merging white dwarfs      Ignition conditions      Metallicity effects      Central density effects      Detonation density effects      Tracer particle burning      Subsonic burning fronts      Supersonic burning fronts      W7 profiles   Massive star supernova:      Rotating progenitors      3D evolution      26Al & 60Fe      44Ti, 60Co & 56Ni      Yields of radionuclides      Effects of 12C +12C      SN 1987A light curve      Constraints on Ni/Fe ratios      An r-process      Compact object IMF   Stars:      Neutrino HR diagram      Pulsating white dwarfs      Pop III with JWST      Monte Carlo massive stars      Neutrinos from pre-SN      Pre-SN variations      Monte Carlo white dwarfs      SAGB stars      Classical novae      He shell convection      Presolar grains      He burn on neutron stars      BBFH at 40 years   Chemical Evolution:      Iron Pseudocarbynes      Radionuclides in the 2020s      Hypatia catalog      Zone models H to Zn      Mixing ejecta      γ-rays within 100 Mpc   Thermodynamics & Networks      Stellar EOS      12C(α,γ)16O Rate      Proton-rich NSE      Reaction networks      Bayesian reaction rates   Verification Problems:      Validating an astro code      Su-Olson      Cog8      Mader      RMTV      Sedov      Noh Software instruments Presentations Illustrations YouTube: cococubed Bicycle adventures Public Outreach Education materials AAS Journals YouTube: AAS 2019 JINA R-process Workshop 2020 Digital Infrastructure 2020 MESA Marketplace 2020 MESA Summer School 2020 ASU Solar Systems 2020 ASU Energy in Everyday Life Contact: F.X.Timmes my one page vitae, full vitae, research statement, and teaching statement.	On The Observability Of Individual Population Iii Stars And Their Stellar-mass Black Hole Accretion Disks Through Cluster Caustic Transits (2018) In this article we summarize panchromatic Extragalactic Background Light data to place upper limits on the integrated near-infrared surface brightness that may come from Population III stars and possible accretion disks around their stellar-mass black holes in the epoch of First Light, broadly taken from z $\simeq$ 7 - 17. Theoretical predictions and recent near-infrared power-spectra provide tighter constraints on their sky-signal. We outline the physical properties of zero metallicity Population III stars from MESA stellar evolution models through helium-depletion, and black hole accretion disks at z $\gtrsim$ 7. We assume that second-generation non-zero metallicity stars can form at higher multiplicity, so that black hole accretion disks may be fed by Roche-lobe overflow from lower-mass companions. We use these near-infrared SB constraints to calculate the number of caustic transits behind lensing clusters that the James Webb Space Telescope and the next generation ground-based telescopes may observe for both Population III stars and their black hole accretion disks. Typical caustic magnifications can be $\mu$ $\simeq$ 10$^4$ - 10$^5$, with rise times of hours and decline times of $\lesssim$ 1 year for cluster transverse velocities of $v_T$ $\lesssim$ 1000 km/s. Microlensing by intracluster medium objects can modify transit magnifications, but lengthen visibility times. Depending on black hole masses, accretion-disk radii and feeding efficiencies, stellar-mass black hole accretion-disk caustic transits could outnumber those from Population III stars. To observe Population III caustic transits directly may require to monitor 3 - 30 lensing clusters to AB $\lesssim$ 29 mag over a decade. panchromatic backgrounds Pop III HR diagram cluster caustics and magnification map redshift space distribution