Updated July 21, 2026

The work happens in San Diego, at 32.8° N.

Plot of the moment

Three panels. (a) A 512-star cluster in the x-y plane, points sized and coloured by stellar mass, with projected half-mass radii circled at t=0 and after three crossing times, and a central massive binary. (b) Binary and cluster scales against time in units of the half-mass crossing time: the half-mass and 90-percent radii expand while the binary semimajor axis drops in three discrete steps at marked encounters. (c) A four-by-four matrix of logarithmic sensitivities of endpoint observables to birth parameters, showing strong diagonal structure: cluster radii respond to the initial half-mass radius, while binary semimajor axis and eccentricity respond to their own initial values.
Jul 20What the Endpoint Remembers. A differentiable model has to earn the word. Here a 512-star cluster with a hard massive binary is evolved for three crossing times — the binary hardens, the cluster expands — and the endpoint's sensitivity to every birth parameter is obtained by differentiating straight through the adaptive timestep, agreeing with complete finite-difference reruns to three parts in a hundred thousand. The result is legible: cluster size remembers where the cluster started, the binary remembers its own orbit. That is what makes the model invertible against data rather than merely runnable. gravax →
Three panels. Left: Hertzsprung-Russell tracks for 20 to 50 solar-mass stars, coloured by evolutionary phase from main sequence through Hertzsprung gap, core helium burning, early asymptotic giant branch and helium star. Centre: current stellar mass against age, showing tracks that coincide until winds switch on near 4 to 6 megayears and then drop by different amounts under weak, fiducial and strong wind controls, each ending in a marker for eventual neutron-star or black-hole formation. Right: a heat map of the change in remnant mass across initial mass and eruptive-wind control, negligible below 40 solar masses and strongly signed above it, with an inset showing pre-supernova mass falling linearly with the wind control and its exact adjoint derivative.
Jul 20Differentiable massive-star evolution connects uncertain winds to remnant outcomes. (a) Phase-colored H–R tracks and (b) mass-loss histories for 202050M50\,M_\odot stars under weak, fiducial, and strong wind controls (dotted, solid, and dashed). The tracks coincide before wind activation and diverge as mass loss reshapes their evolution; symbols indicate eventual neutron-star or black-hole formation. (c) Wind-induced changes in remnant mass across the (MZAMS,W)(M_{\rm ZAMS},W) response surface. The inset demonstrates an exact local adjoint sensitivity of pre-supernova mass—enabling gradient-based inference through stellar evolution rather than repeated parameter sweeps. startrax →
Six panels in two columns. Top row: a simulated g-band image of a crowded cluster, first as an expected source-limited scene and then as a nominal 30-second Rubin-like exposure with sky and noise. Middle row: maps of how much information each pixel carries about the IMF slope. Bottom row: the same for the binary mass-ratio slope. The information maps are concentrated on a sparse subset of stars, and differ between the two parameters.
Jul 19Which Pixels Know the Answer. This is what differentiable codes buy you. The same truth-known cluster is rendered as an idealised scene and as a nominal 30-second Rubin-like exposure with PSF, sky, Poisson and read noise (top). Differentiating that render with respect to the population parameters gives the Fisher information carried by every individual pixel — for the IMF slope (middle) and for the binary mass-ratio slope (bottom). Note that the two are not the same pixels: different physics is constrained by different parts of the image. You cannot make this map by running a simulation forward; it exists only because the whole pipeline carries gradients. Population-to-pixel differentiation is implemented; validated detector and survey transformations, and global recovery, are proposed work. fluxax →
Three panels showing binaries raising the line-of-sight velocity dispersion, binary-blind mass estimates near three times the truth against a calibrated control and binary-aware recovery, and radial target allocations shifting between mass-first and degeneracy-first observing designs.
Jul 19The Telescope Adds Ten Pounds. Unresolved binaries inflate the observed velocity dispersion, and a binary-blind fit turns that orbital motion into 2.9 times the true cluster mass — while forecasting 4.5% precision. That is a bias 42 times its own error bar. Modelling the binaries recovers both the mass and the binary fraction, and the same machinery then says where to point the telescope next. informax →
Three panels: a synthetic cluster's natal gas surface density with an embedded stellar population, then the same stars placed without and with mass–gas coupling, coloured by spectral type from blue O stars to red M stars.
Jul 18Born Where the Gas Is. A truth-known synthetic cluster: natal gas surface density with an IMF-sampled population (left), then the same stars placed without (centre) and with (right) mass–gas coupling. With coupling on, massive O and B stars preferentially sit in dense gas — primordial mass segregation as a knob you can turn, which is what makes it testable. progenax →

On my desk

I'm writing the progenax methods paper, and I expect it out later this summer.

Confidently Wrong: Why Ignoring Binaries Biases IMF Inference at Large Sample Sizes is under review at The Astrophysical Journal — the referee report was positive. Read it on arXiv.

Nearly out the door

One masters student is finishing in August 2026.

  • Aisling AcunaBridging STARFORGE and SKIRT: A Synthetic Observation Pipeline for High-Fidelity Star Cluster Formation Simulations

Just finished

  • Surinder Singh ChhabraM.S. Computational Science — Data Science, SDSU · completed Summer 2026AstroRAG: Evidence-Aware Scientific Literature Retrieval — a multi-stage retrieval and evidence-summarisation framework for astrophysics literature discovery

Where the interesting problems are

gravax and startrax are taking most of the development effort.

  • gravaxDifferentiable collisional dynamics.In development
  • startraxFrom birth mass to stellar state and remnants.In development

Simmering

  • fluxaxPhysical states → survey observables.Far along
  • informaxWhat the data can actually recover.Far along

Teaching

It's summer — no classes, and the research runs at full tilt.

Everything I've taught is on the teaching page.

Side projects

  • SophieA schema-driven, AI-authorable platform for interactive textbooks, course sites and slides — one lesson, many accessible outputs.
  • Cosmic PlaygroundPredict. Play. Explain. — an interactive astronomy demos platform. Play with the universe; learn the physics.

Inspired by nownownow.com. Follow this page by RSS to hear when it changes. Longer-form writing is in astrobytes; the full record is on the CV.