Cococubed.com Pop III with JWST

Home

Astronomy research
Software Infrastructure:
MESA
FLASH
STARLIB
MESA-Web
starkiller-astro
My instruments
White dwarf supernova:
Stable nickel production
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
Effects of 12C +12C
SN 1987A light curve
Constraints on Ni/Fe ratios
An r-process
Neutron Stars and Black Holes:
Black Hole Mass Gap
Compact object IMF
Stars:
Variable white dwarfs
Pop III with JWST
Micronovae
Neutrino HR diagram
Monte Carlo massive stars
Pre-supernovaneutrinos
Pre-supernova variations
Monte Carlo white dwarfs
SAGB stars
Nugrid Yields I
Classical novae
He shell convection
Presolar grains
He burn on neutron stars
BBFH at 40 years
Chemical Evolution:
Iron Pseudocarbynes
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
RMTV
Sedov
Noh
Software instruments
Presentations
Illustrations
Public Outreach
Education materials
2022 ASU Solar Systems Astronomy
2022 ASU Energy in Everyday Life

AAS Journals
2022 Earendel, A Highly Magnified Star
2022 TV Columbae, Micronova
2022 White Dwarfs and 12C(α,γ)16O
2022 MESA in Don't Look Up
2022 MESA Marketplace
2022 MESA Summer School
2022 MESA Classroom
2021 Bill Paxton, Tinsley Prize

Contact: F.X.Timmes
my one page vitae,
full vitae,
research statement, and
teaching statement.
A highly magnified star at redshift 6.2 (2022)

Galaxy clusters magnify background objects through strong gravitational lensing. Typical magnifications for lensed galaxies are factors of a few but can also be as high as tens or hundreds, stretching galaxies into giant arcs. Individual stars can attain even higher magnifications given fortuitous alignment with the lensing cluster. Recently, several individual stars at redshifts between approximately 1 and 1.5 have been discovered, magnified by factors of thousands, temporarily boosted by microlensing. In this
article, we report observations of a more distant and persistent magnified star at a redshift of 6.2 ± 0.1, 900 million years after the Big Bang. This star is magnified by a factor of thousands by the foreground galaxy cluster lens WHL0137-08 (redshift 0.566), as estimated by four independent lens models. Unlike previous lensed stars, the magnification and observed brightness (AB magnitude, 27.2) have remained roughly constant over 3.5 years of imaging and follow-up. The delensed absolute UV magnitude, -10 ± 2, is consistent with a star of mass greater than 50 times the mass of the Sun. Confirmation and spectral classification are forthcoming from approved observations with the James Webb Space Telescope.

 SunriseArc and Earendel Caustic curve and Earendel

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