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Fig 2: Summary of the existing photometric selection method (Wild et al. 2014, 2016), applied to the UDS field. Left: Super-color diagram for galaxies in the UDS (grey points) from Wilkinson et al. (2021), which cleanly selects post-starbursts (PSB) from star-forming and quiescent galaxies at 0.5<z<3. Colored points show spectroscopically classified galaxies. The first super-color (SC1) describes the SED shape and is correlated with specific SFR and light-weighted age. The second super-color (SC2) describes the strength of the 4000Å/Balmer break and correlates with the fraction of the stellar mass formed during the last Gyr and metallicity. The third super-color (not shown) describes the shape of the SED around 4000Å and is used to break the degeneracy betweenthe fraction of the stellar mass formed during the last Gyr and metallicity. Inset plots show stacked optical spectra of the different spectral classes identified using the super-color method from Wild et al. (2014, 2016).Middle: Optical spectra of post-starburst (PSB) and quiescent (red) galaxies atz∼1 from [83], with post-starburst galaxies exhibiting
characteristic deep Balmer absorption lines.Right: Stellar mass vs photometric redshift distribution, showing example bins and 90% mass completeness limits (dashed lines) from Wilkinson et al. (2021).

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• Collect photometry for extragalactic deep fields, e.g. EGS. Assess usability of existing photometric catalogs, remeasure photometry as necessary.

• Modify and apply existing photometric classification code to photometry to select post-starburst, quiescent and star-forming galaxies. 

• Analyze galaxy population properties, e.g. number densities, stellar mass function and compare to literature.

• Write a paper on the newly selected galaxies, detailing the selection method and galaxy properties (e.g. number densities, stellar mass function), and present the findings at conferences.

• Publish catalogs on public facing data repositories.

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