Oxford Astrophysics will run a summer research programme for undergraduate physics students again in summer 2026. The list of available projects and links to application forms can be found below. Please ensure you meet the eligibility requirements before applying.
The selected students will work with a supervisor in the department, usually a postdoctoral researcher or lecturer, on a self-contained research project. The programme will also include lectures/seminars on current astrophysics topics, and on academic careers in astro. Students will be encouraged to take part in department life, joining researchers for coffee, discussions and seminars.
The projects run for typically 8 weeks, nominally from 29th June to 21st August. The duration may be adjusted slightly to be shorter or longer. Students will be paid as employees of the University, receiving a payment of at the Oxford living wage (subject to tax and National Insurance deductions). Students are normally expected to work full time on their project, but hours can be discussed with your supervisor. We will make sure that all computing resources needed for the selected projects are available to all selected candidates.
There are also a number of astrophysics projects available for the UNIQ+ scheme, which can be found on the UNIQ+ website -- please note that applications for UNIQ+ have different criteria and are managed separately and not by the department.
Application instructions can be found below.
Eligibility criteria
Students currently in third year of a relevant undergraduate degree or combined undergraduate masters are eligible to apply, as are students in fourth year of either a five-year Scottish masters, a five-year undergraduate masters with foundation year, or four-year Scottish Bachelor's degree. Students who already have a Bachelor's or Masters degree, or are in the final year of a Masters degree, are not eligible.
Applications are very welcome from institutes outside of Oxford.
Unfortunately, due to UK visa regulations, we are only able to accept applications from candidates who do not require a visa to work in the UK. EU students currently in the UK who have been granted Pre-Settled status are also welcome to apply along with current students in the UK on a Tier 4 visa that allows vacation employment. If you have queries about your personal circumstances, please get in touch with ashling.gordon [at] physics [dot] ox [dot] ac [dot] uk, but please be aware that unfortunately there are no exceptions to these criteria.
How to apply
To apply, submit a 1-page CV and a 1-page cover letter (in a single PDF file). As part of the form, you will be asked to rank your top 3 project choices. Applications are made through an online form (link to follow).
The 1-page cover letter should briefly mention the following, bearing in mind the one page limit:
- Your motivation for participating in the programme: Why do you want to do it? How it would benefit you?
- Your academic accomplishments to date as well as other skills relevant to research (in combination with the CV)
- Your long-term goals and any particular astrophysical interests
- Your reasons for your choice of projects
- Any extenuating circumstances, examples of adversity you have had to overcome, or lack of access or opportunities you experienced
Reference: You will also be asked to contact one academic referee who can provide a short letter in support of your application. Referees should submit their letter by filling out a google form (link to follow) before the same application deadline.
If referees do not wish to fill out a google form (for example, because they do not have a google account), they can instead email their reference, with the subject line "Reference: ApplicantSurname", to james.matthews [at] physics [dot] ox [dot] ac [dot] uk.
Deadline for applications: March 20th 2026.
Available projects
Uncovering the Causal Structure of Galaxy Formation
Supervisors: Dr Tariq Yasin, Dr Harry Desmond
Understanding how galaxies form and evolve requires disentangling complex, intertwined relationships between mass, morphology, star formation, environment, and dark matter. Traditional analyses rely on correlations, which cannot determine the direction of physical influence or identify hidden confounding processes. In this project, we will apply modern machine learning-based causal discovery techniques to large galaxy survey datasets to infer the causal structure governing galaxy formation.
Using state of the art algorithms capable of handling nonlinear relations and latent variables (e.g. [1]), we will reconstruct causal graphs linking key galaxy properties and assess which observed correlations arise from direct physical relationships rather than indirect or confounded associations. By comparing the inferred causal structures with predictions from theoretical models and simulations, we will test competing scenarios for mass growth, morphological transformation, and star formation regulation.
This project will provide the student with experience in astrophysical data analysis, machine learning, Bayesian and causal inference, and galaxy evolution theory, while contributing to the development of a new, physically informative framework for learning galaxy formation directly from data.
[1] https://arxiv.org/abs/2510.01112
Investigating the radio properties of dusty star-forming galaxies at high redshift
Supervisors: Dr Imogen Whittam, Dr Rohan Varadaraj, Prof. Matt Jarvis
Recent deep multi-wavelength surveys from both ground- and space-based facilities are revealing new populations of galaxies in the distant, high-redshift Universe. Dusty star-forming galaxies are among the most intensely star-forming systems in the Universe, yet their dust-obscured nature makes them challenging to study at optical wavelengths. Radio observations are un-obscured by dust, so provide a powerful tool for detecting and studying this dusty objects.
This project will combine data from the MIGHTEE survey - a deep survey made with the MeerKAT radio telescope (PI Jarvis) - with sub-mm observations from the SCUBA-2 instrument. The depth of the MIGHTEE radio observations allows us to detect star-forming galaxies at high redshift in the radio for the first time, providing a unique insight into the nature of these objects. In this project the student with combine the MIGHTEE and SCUBA-2 observations to detect a novel population of high-redshift dusty star-forming galaxies, and use the radio and multi-wavelength data to study their properties.
This project has the potential to lead to a journal paper.
Recommended skills: This project will involve data analysis in python, so some experience using python would be an advantage.
Testing cryogenic mechanisms for the HARMONI ELT instrument
Supervisors: Dr Edgar Castillo, Dr Miriam Cisneros, Dr Matthias Tecza
HARMONI is the first light Adaptive Optics assistecd near-IR integral field spectrograph for the ELT. It covers a large spectral range from 750nm to 2450nm with spectral resolving powers ranging from 2750 to 7000. The astronomical instrumentation group in the Astrophysics sub-department is responsible to deliver the 4 back-end spectrograph modules, and after a re-scope over the last year we are currently entering a prototyping phase in preparation for a final design review. One prototype we are developing is the disperser wheel mechanism, which allows the selection of one of 6 different wavebands. This rotary mechanism has very stringent positioning and repeatibilty requirements that can not be met with commercially available rotary stages. Our existing prototype is operational using inexpensive motion control electronics, and we are seeking a student that will implement a control system using approved observatory standard motion controllers including closed-loop position feedback, conducting mechanisms performance tests, and optimising the control algorithms to achieve the requirements. Initially these tests will all be performed with the prototype at ambient temperatures, however, depending on progress it might be possible for the student to take part in cryogenic performance tests. The student will have the opportunity to learn both hardware and software related aspects of astronomical instrumentation.
Recommended Skills: The ideal student would have experience in one of Physics or Engineering experiments, their electronic and software control, or their data analysis and presentation.
Novel probes of gas thermodynamics in cosmological weak lensing analyses
Supervisors: Dr Adrien La Posta, Prof. David Alonso
Despite the fact that baryons make up only 5% of the energy content of the Universe, understanding their distribution and thermodynamic properties is a key objective to constrain fundamental physics from current cosmological surveys. In this context, secondary signals in the cosmic microwave background, such as the thermal and kinetic Sunyaev Zel’dovich (SZ) effects, can be used as powerful tracers of the intergalactic gas. We have developed a novel approach to reconstruct the redshift evolution of the cosmic electron pressure, mapped by the thermal SZ signal, a key quantity to characterise the distribution and thermodynamics of baryonic matter. The aim of this project is to use these measurements in combination with other large-scale structure tracers (e.g. galaxy weak lensing) to jointly constrain cosmological parameters and baryon properties, following a data-driven approach
Recommended skills: Python knowledge (numpy/scipy and other standard libraries), statistics (likelihood functions, chi-squared, probability densities)
Impact of feedback and cosmology on Cosmic Infrared Background tomography
Supervisors: Dr. Sara Maleubre, Prof. David Alonso
The Cosmic Infrared Background (CIB) traces the emission of star-forming galaxies throughout all cosmic epochs. Breaking down the contribution from galaxies at different redshifts to the observed CIB maps would allow us to probe the history of star formation.
In this internship, we will measure the star formation history from simulation-based cross-correlations, reproducing the same measurements made using real CIB data. These data are complementary to direct measurements of the SFR density but giving a higher weight to more massive haloes, and thus provides additional information to constrain the physical properties of star formation. Through this analysis, we will quantify the impact of AGN and supernova feedback on this observable, as well as variations in cosmological parameters. We will then compare the results to current measurements from observations.
Recommended skills Knowledge of python (or alternative coding languages)
Characterising precursor eruptions in type IIn supernovae using the ATLAS survey
Supervisors: Dr Shubham Srivastav, Prof Stephen Smartt
Type IIn supernovae (SNe) comprise a distinct family of core-collapse supernovae that show strong signatures of interaction with circumstellar material (CSM). The progenitors of these luminous, long-lived transients are thought to be massive, luminous blue variable stars, with strong mass-loss episodes during the months to years preceding terminal explosion. However, SNe IIn are a very diverse and heterogeneous subclass, suggesting different progenitor scenarios, for instance less massive binary systems, could also play a role. SNe IIn often show precursor eruptions, i.e. lower luminosity outbursts, from months to years prior to explosion, providing a window to study the tumultuous mass-loss history and the resulting complex CSM around the progenitor.
The goal of the project is to characterise precursor eruptions in SNe IIn using a well-defined, volume-limited sample of transients observed within 100 Megaparsec observed over a 6 year span during 2017-2023 with the ATLAS survey (ATLAS100). The ATLAS100 sample contains over 1700 transients, of which 42 are SNe IIn. A majority of these IIn events have historical, pre-explosion imaging from the Pan-STARRS survey, yielding deeper constraints on precursor eruptions. The project will involve characterising the luminosity and other properties of these precursors and correlating them with the properties of the terminal explosion, with the underlying aim of connecting the precursors to the mass-loss history and therefore the nature of the underlying progenitors.
Recommended Skills: general familiarity with python and stats will be an advantage
Searching for transient, narrowband emission in the Galaxy
Supervisors: Dr Alex Andersson, Dr Steve Prabu
Astrophysical sources exhibit both broad continuum and narrow line features that provide insight into physical conditions and ongoing processes in the Universe. In particular, the line emission of neutral hydrogen (HI) at λ=21cm has a variety of uses, from measuring the hydrogen content along lines-of-sight in the Milky Way to understanding the kinematics of other galaxies. Furthermore, the 21cm line has long been proposed as a target frequency at which to search for signs of technologically advanced life in the Universe, most famously as a suggested origin of the Wow! signal. Similarly, the line emissions of the hydroxyl radical (OH) at λ~18cm probe both ends of the lives of stars, as they form in collapsing interstellar clouds and as giant stars shed their outer layers to form nebulae. Such sources are referred to as masers, analogous to terrestrial laser technology. Recently, both of these line transitions have been suggested as the sites for transient phenomena, producing the emission of high-intensity, spatially compact bursts, taking place over minutes to days. The detection of narrow and potentially variable HI or OH lines would therefore be of great utility for our understanding of coherent radiation processes and in the search for life in the Universe. The Breakthrough Listen datastreams provide unprecedented frequency resolution for discovering these signals. In this project, the researcher will perform extensive searches through the Breakthrough Listen archives in search of HI and OH signals to provide observational evidence of potential transient phenomena associated with these transitions. In particular, the uniquely high resolution capabilities of these data allow for unprecedented details to be uncovered in these maser systems.
The project will require an enthusiasm for astrophysics, SETI and good computing/data management skills. Familiarity with Python is recommended and an understanding of basic UNIX commands for remote computer usage would be advantageous.
Recommended Skills: Familiarity with Python and basic UNIX commands for remote computer usage.
Exploration of fabrication tolerance effects in Josephson-junction-based superconducting quantum parametric amplifiers
Supervisors: Dr. Michele Piscitelli, Dr. Boon Kok Tan
Superconducting parametric amplifiers, such as resonator-based Josephson Parametric Amplifiers (JPAs), are essential for near–quantum-limited, low-noise readout in quantum computing. They also play a key role in enhancing detector sensitivity in small-signal fundamental physics experiments, such as dark matter searches. These amplifiers can be realised using either high-gap superconducting films or Josephson junctions.
Traditionally, such devices have been fabricated in collaboration with external institutes using their cleanroom facilities. Our group now aims to transition fabrication in-house by leveraging our nanofabrication facilities, previously optimised for qubit chip development, to produce a series of Josephson-junction-based parametric amplifiers, including microwave-frequency JPAs. Within this broader effort, the focus of this internship project is to investigate how nanofabrication constraints impact the performance of these devices.
Josephson junctions made using current techniques will exhibit variations in their physical properties due to fabrication process non-uniformity. For instance, the insulating oxide layer used to form the junction tunnel barrier, can vary in thickness across the substrate and include localised defects. This leads to variations in design-critical junction parameters, which in turn affects the gain performance of junction-based amplifiers.
In this project, the student will learn to use and build upon existing code or commercial software for designing and simulating the performance of parametric amplifiers. Using these tools, we expect the student to study the effect of Josephson junction parameter variation on JPA device performance. They will use tolerance analysis to inform fabrication requirements and procedures, and also investigate better design specifications for current fabrication capabilities. If time allows, this work may be extended to broader bandwidth parametric amplifiers.
This project is ideal for students interested in superconducting quantum device simulation and those who enjoy developing theoretical/computational software. Students interested in experimentation will have the opportunity to test the fabricated devices using state-of-the-art cryogenic facilities and top-end laboratory equipment. Students may also be able to gain some experience with relevant nanofabrication techniques.
Recommended Skills: General coding knowledge
Measuring the varying mass-to-light ratios galaxies: Towards a deeper understanding of Dark Matter Haloes
Supervisors: Prof Matt Jarvis, Dr Tariq Yasin (with Andreea Varasteanu)
In this project the student will work with multi-wavelength imaging data to determine the mass-to-light ratio of the stellar component of galaxies in the SPARC database. SPARC is the benchmark sample that has been used to pin down the total mass in galaxies and also test for departures from the Lambda CDM model of the Universe, specifically testing predictions for modified Newtonian Dynamics.
However, we have recently found that varying mass-to-light ratios across individual galaxies and across samples of galaxies can add significant uncertainties to such studies and that this information is critical in order to measure the amount of mass in galaxies that is in the form of Dark Matter. The student will use the visible-near-infrared imaging data of subsets of the SPARC galaxies to measure this by first measuring the photometric properties of the galaxies in elliptical apertures centred on the galaxy and the by fitting the full spectral energy distribution of the galaxies’ stellar emission. The student will therefore have a chance to learn and gain experience in photometry of galaxies and how to extract key physical quantities such as stellar mass and star-formation rates. Much of which underpins current research into galaxy evolution. The project has the potential to lead to publication for the student.
The project will follow the methodology outlined in https://arxiv.org/pdf/2504.20857