1. . Epoch of reionization . Recombination . Peak star formation
Inflation
Astroparticle era
. Recombination
. Epoch of reionization
. Peak star formation

2. Take this to the next stage
4 claims in the NoI
first SNe
first SMBH
detect LSS change due to reionization
serendipitous transients
Take this to the next stage
Astrophysics
Simulation
Experiment design
Results and Analysis

3. ERS NoI
Just as a well publicized early goal of HST was to measure the Hubble Constant, so a well publicized early goal of JWST is to find and characterize the first stars in the Universe.
But Population III does not come with a handbook of how to do this.
JWST takes us into a discovery space of transient phenomena at AB∼27 mag of which we have no knowledge.
The community needs to know what is there, as it may affect the subsequent mission in significant ways.
SNe are the defining characteristic of Pop III. When the first SNe occur, Pop III ends, because the first metals have been injected into the IGM.
Inter alia the First Transients ERS may recognize the first supernovae by their rise time.
If this was achieved, it would open up a wealth of follow up science for the community , not fully predictable at the time of launch, but possibly among the major outcomes of the mission.

4. Astrophysics plan for May
What are the core collapse rates ?
including SLSN
What are the SNIa rates ? Jos. Vinko
What are the DCBH rates ? Dan Whalen

5. Simulation plan for May
DRAGONS Paul
STIPS Avishay and Armin Rest
ADDSTAR Jeremy
DRAGONS needs SN rates including
Can Anton get us a pre-release version of STIPS?

6. Experimental design Lifan
Will GOODS N allow us to obtain 400 sq arcmin two epochs during the ERS period ?
Are there better field choices ?
Optimize exposure time with APT including NIRSS parallel exposures
Shall we invest 10% of our time in NIRSpec ?

7. Results and Analysis
How many SNIa can we detect and what do they look like ?
SLSNe z (6,10) are transients with z dropout hosts
Do we expect to see any ?
SNe z (10,30) are K dropout transients
Can we see any in 5 years of JWST?
AGN = blue transients. Link DCBH rate with these

8. White paper issues
DCBH white paper section can be written by Lifan and Dan and Anton
Trade off between area and depth. Anton & Lifan
Include brown dwarf foreground Jeremy
Galaxies
Can we detect change in PS between z=10 and z=6?
WF survey good for finding the first red galaxies

9. White paper section on DCBH
Born starving Whalen Alvarez 2006 kicks, gas loss Ly a emitter at z 7 CR7 monolithic collapse of halo Woods 2017, Hammerle 2017 in prep GR collapse during H burning Cold flows Di Matteo 2011 ApJ Metallicity comes out solar Next step: synthetic observables AB H 18 for z=7 Rates Djikstra and Yue et al (GRB rates)

10. Whitepaper notes on SNe
SNIa section by J. Vinko
Ia rate drops to zero at z =2 w/o prompt
Peter & Joszef should write up SLSN at high z
SLSN need longer than the ERS to find
Hard to map SLSN into a specific mass  range
Peter Nugent said whatever mag gain you get from lensing is lost in drop in volume
AGN are blue according to Volker Bromm
Hummel 2012 ApJ 755 PISN rates (more references)

11. Other issues to pursue Kasen has very high SN rates
Figure of merit: million Mpc3
there are 20 Mpc3 per sq deg between z 6,7
Very high DCBH rates in Habouzit et al
Probably don’t need Ariel Goobar or Peter Nugent to do the cluster lensing simulation

12. Subaru proposal Jeremy
SSP UltraDeep (equatorial = unsuitable) SXDS (02 : 18 : 15.60,−04 : 51 : 00.00) Cosmos. (10 : 00 : 28.60,+02 : 12 : 21.00) ElaisN1 is a +50 Deep field Need a Japanese PI Kilonovae are merging NS, ejecta >0.1c, Masaomi Tanaka 1000 per Gpc3 per yr The minimum # women you can have on an ERS team is 10%

13. Other tasks suggested by A & J
WP0 set up a web page
WP1 including background
WP2
James Webb Transient Factory design
ERS learning experience for JWTF
Project Manager

14. Science and deliverables
The ERS mantra is to enable the community to play with JWST data ASP after launch
A better approach:
JWST performance is incorporated into TAO
Proposers test their observing plans with TAO
Does the planned data test the observer’s hypothesis?

15. The Theoretical Astrophysical Observatory (TAO)
Simulation database
Web form data query
Image generation
Telescope simulator
Light cone generation
SEDs + Filters
Bringing cosmological simulations and galaxy formation models to every astronomer
Opened March 2014
Registered users: 300+
Virtual universes built: 400+

16. TAO https://tao.asvo.org.au Telescope simulator Image generation
Simulation database
Web form data query
Image generation
Telescope simulator
Light cone generation
SEDs + Filters

17. > Cosmological dark matter simulations
> Galaxy formation & evolution models
> Mock survey light cones
> Mock images of galaxies
> Understand and interpret the observations

18. through NeCTAR, NCRIS and EIF funding.
The TAO project is part of the ASVO NeCTAR Virtual Laboratory, supported by
Swinburne University, Astronomy Australia Limited, and the Commonwealth Government
through NeCTAR, NCRIS and EIF funding.

19. Low redshift predictions for the distribution of cosmic gas
z=0
z=0.1
z=0.2
z=0.3
Low redshift predictions for the distribution of cosmic gas
z=1

20. High redshift predictions for the spectra of distant galaxies
z=1
z=2
z=3
z=0
z=1

21. TAO light-cone module

22. The TAO image module

23. Videogame view of ERS Scientific view of ERS
To allow the community to play with JWST data from as soon as possible after launch
Scientific view of ERS
To allow the community to conceptualize new experiments with JWST as soon as possible after launch
This is most effective if the concepts are immediately trialed on the Theoretical Astrophysical Observatory

24. Donald Trump was right…..
The Hubble Deep Field was the great achievement of HST