Cococubed.com Pop III with JWST
Home Astronomy research   Software Infrastructure:      MESA      FLASH      STARLIB      My codes   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:      Pop III JWST      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:      Hypatia catalog      Zone models H to Zn      Mixing ejecta      γ-rays within 100 Mpc   Thermodynamics & Networks      Stellar EOS      Reaction networks      Proton-rich NSE      Bayesian reaction rates   Verification Problems:      Validating an astro code      Su-Olson      Cog8      Mader      RMTV      Sedov      Noh Software instruments Presentations Illustrations Videos Bicycle adventures AAS Journals 2017 MESA Marketplace 2017 MESA Summer School 2017 ASU+EdX AST111x Teaching materials Education and Public Outreach Contact: F.X.Timmes my one page vitae, full vitae, research statement, and teaching statement.	Can The James Webb Space Telescope Observe Individual Population III Stars Or Their Black Hole Accretion Disks Directly Through Cluster Caustic Transits? (2017) In this paper by Windhost et al we summarize panchromatic Extragalactic Background Light data to place upper limits on the near-infrared surface brightness from Population III stars and possible accretion disks around their stellar mass black holes in the epoch of First Light, broadly taken at z $\simeq$ 7 - 17. Tighter constraints on their sky-signal come from theory and recent near-infrared power-spectrum studies. We outline the physical properties of zero metallicity Population III stars from MESA stellar evolution models through helium-depletion, and of SBH accretion disks at z $\lesssim$ 7, assuming that second-generation non-zero metallicity stars form at higher multiplicity, so that their SBH 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 that the James Webb Space Telescope may observe for both Population III stars and their SBH accretion disks behind lensing clusters. Typical caustic magnifications can be $\mu$ $\simeq$ 10$^4$ - 10$^5$, with rise times $\lesssim$ a few hours and decline times of $\sim$ a year for cluster transverse velocities $v_T$ $\lesssim$ 1000 km/s. Microlensing by intracluster medium objects can modify transit magnifications, but lengthen visibility times. Depending on SBH masses, accretion disk radii and feeding timescales, SBH accretion disks may outnumber Population III star caustic transits by $\lesssim$ 5 - 10$\times$. We present a JWST observing program to observe such events to AB $\lesssim$ 29 mag. JWST may need to monitor 10 - 100 lensing clusters during its lifetime to detect Population III objects through caustic transits directly. panchromatic backgrounds HR diagram cluster caustics and magnification map redshift space distribution