Justin Myles

Graduate Student at Stanford University

I study observations of the large structures of the Universe -- galaxies and clusters of galaxies -- to inform an underlying cosmological model for the Universe. For an introduction to my research assuming no prior knowledge, see the following linked videos [1, 2].

My primary research interest is in experimental tests of the cosmological model with weak gravitational lensing and galaxy cluster cosmology. My work includes the redshift calibration of the Dark Energy Survey Year 3 weak lensing source galaxy catalog [3], measuring the impact of projection effects in redMaPPer clusters of galaxies [4], and measuring the X-ray luminosity of the hot gas of galaxy clusters. I have experience analyzing raw optical and X-ray photometric and spectroscopic data as well as implementing novel statistical methods to develop insights into cosmological galaxy survey datasets.

I am a DARE Fellow at Stanford University where I work at the Kavli Institute for Particle Astrophysics and Cosmology in the X-ray Astronomy and Observational Cosmology group led by Prof. Steve Allen. I also work with the Astrophysics, Cosmology, and Artificial Intelligence group led by Prof. Daniel Gruen at LMU Munich. For details on my work, feel free to get in touch.


jmyles at stanford dot edu [ PGP ]


For a full list of my publications, see ADS.

Dark Energy Survey Year 3 Results: Redshift Calibration of the Weak Lensing Source Galaxies

Dark Energy Survey Year 3 Source Galaxy Redshift Distributions
Ensemble of redshift distributions of DES weak lensing source galaxies in four tomographic bins, as inferred from galaxy photometry.

We present the derivation and validation of redshift distributions for the source galaxies used in the DES Y3 weak lensing measurements. As the first application of this method to data, we validate that the assumptions made apply to the DES Y3 weak lensing source galaxies and describe our treatment of systematic uncertainties. We construct an ensemble of redshift distributions whose variation encodes all uncertainties and combines information from galaxy color, position correlation functions, and shear ratios.

Spectroscopic Quantification of Projection Effects in the SDSS redMaPPer Galaxy Cluster Catalogue

Cluster Velocity Dispersion vs. Spectroscopic Richness
Cluster velocity dispersion as a function of spectroscopically calibrated richness. The best fitting slope implies our introduced spectroscopic richness scales with halo mass with a power-law index consistent with unity.

We present a spectroscopic quantification of projection effects in the redMaPPer Galaxy Cluster catalog. We show that a simple double-Gaussian model can be used to describe the distribution of line-of-sight velocities in the redMaPPer sample. With this model we show that projection effects are substantial, are a strong function of richness, are a stronger function of richness than recent models, and are not a strong function of luminosity. We introduce a new cluster mass proxy, a three-dimensionsal richness, which scales approximately linearly with halo mass.