robert.j.harris@durham.ac.uk

cyril.bourgenot@durham.ac.uk

james.osborn@durham.ac.uk

james.osborn@durham.ac.uk

kieran.s.obrien@durham.ac.uk

r.w.wilson@durham.ac.uk

yuan.ren@durham.ac.uk

cyril.bourgenot@durham.ac.uk

anthony.brown@durham.ac.uk

anthony.brown@durham.ac.uk

t.j.morris@durham.ac.uk

Learning how we walk

With 33 joints and 29 muscles our feet are incredibly complex, and despite having learnt to walk upright thousands of years ago, humanity still does not fully understand how we use our feet to balance. State-of-the-art gait analysis (the study of how we walk) instrumentation either treats the forces exerted by the foot on the floor as a single point (force plate) or measures the pressure exerted by different points of the foot (pressure mat/insoles). This limits the information that we can acquire on the foot-floor forces, which in turn limits our insight into how our feet interact with the floor to balance ourselves. Overcoming this this is vital to tackle the high incidence and impact of falls in our ageing society.

In your PhD, you will join our interdisciplinary team based in Durham, Newcastle and London to develop new instrumentation to revolutionise our understanding of how our feet enable us to balance and move around, impacting a diverse range of rehabilitation and sports applications. Whilst this PhD project focus on the instrumentation development and data analysis you will also as grow your expertise in movement biomechanics.

Please contact Robert Harris for further information

Opto-mechanical design optimisation of a thermal Infrared (MWIR or LWIR) instrument  

MWIR (Mid-Wave Infrared) and LWIR (Long-Wave Infrared) instruments on satellite platforms are essential tools for monitoring land and sea surface temperatures globally, providing critical data for understanding climate patterns and weather forecasting. With multispectral capabilities, they also assist in identifying and tracking greenhouse gases such as SO2, CO2 and CH4 through their thermal signatures and contribute to mapping air quality and pollutant distribution.

Working with Surrey Satellite Technology Limited (SSTL) and the Centre for Advanced Instrumentation (CfAI), this PhD project will investigate an existing or currently in-development optical payload design and optimize it for manufacturing – manufacturing is not guaranteed during the course of the PhD (subject to successful funding application). In particular, the design will be tailored for metal optics and compatibility with diamond machining technologies currently available at CfAI. The project will explore Finite Element Analysis and how optical surface displacement translates into optical aberrations. Additionally, the research may investigate emerging technologies for optics, such as additive manufacturing design and freeform surfaces. Surrey Satellite Technology Limited (SSTL) has extensive experience in designing and deploying compact, reliable infrared satellite instruments for Earth observation missions. Notably, SSTL has been involved in the design and deployment of the SATVU constellation, which provides unparalleled ground sampling at 3.5-meter resolution.

We are seeking an enthusiastic candidate with a background in optical or mechanical engineering, physics, or photonics. You will join a cutting-edge research group in optical instrumentation at the Centre for Advanced Instrumentation at Durham University and collaborate with a leading industry partner in small satellite technology. The project will benefit from our state-of-the-art space optics manufacturing capabilities, cleanrooms, and space qualification facilities. The role is primarily based at Durham University’s main campus, with additional research conducted at the NetPark Research Institute in Sedgefield, and will include temporary placements at SSTL.

Fully funded
Deadline: Open

Please contact Cyril Bourgenot for further information

Atmospheric impact assessment of space activity

As of August 2025, over 12,600 active satellites orbit Earth, doubling since 2022. Expectations are for satellite populations to rise to 20-30,000 by 2030 and as many as 100,000 by 2050. Much of this growth is derived from the expansion of so-called mega-constellations, large networks of satellites delivering communications and other services around the world. Unlike traditional missions with long operational lifespans, these constellations introduce a high-throughput cycle of satellites entering and exiting the orbital environment to maintain network integrity and upgrade technology. Currently, 1 or 2 tracked objects re-enter the Earth’s atmosphere every day, with this number set to increase significantly over the next decade. These launches and re-entries release soot and metallic particulates (e.g. aluminium oxide) into the upper atmosphere. These particles may influence climate dynamics by forming stratospheric clouds and accelerating ozone depletion, increasing UV exposure risks. Current data is sparse, relying on costly, infrequent (currently discontinued) missions (e.g. NOAA aircraft). Without long-term and scalable monitoring, climate models and policy decisions lack a reliable evidence base.

 This programme will develop proof-of-concept technology demonstrators focused on one or both of the following approaches:

1.        Develop and test a portable multi-spectral imaging/spectrographic systems capable of monitoring re-entry events in real time. These instruments will help determine the physical processes occurring during re-entry—specifically whether objects ablate, melt, or fragment, and how these behaviours vary with trajectory, composition, and structural design.

2.        Balloon-borne sample return missions to collect and characterise particulates in the upper atmosphere, providing direct evidence of their physical and chemical properties.

The specific focus will be tailored to the candidate’s background and interests, with flexibility to pursue either a single approach in depth or a comparative study across both. The project will include design, prototyping, and field validation phases.

This project is conducted in partnership with the University of Auckland, New Zealand, offering a unique opportunity to test instrumentation and collect data across both hemispheres. The collaboration supports joint field campaigns, shared access to facilities, and integration with complementary research in atmospheric science and space sustainability.

Please contact James Osborn for more information

PhD students observing a satellite from La Palma, Spain.

Monitoring and Forecasting Atmospheric Turbulence for Astronomy, Optical Communications, and Space Situational Awareness 

Atmospheric turbulence is a critical limiting factor for ground-based optical systems, affecting image resolution in astronomy, signal fidelity in free-space optical communications, and tracking accuracy in space situational awareness (SSA). This PhD project aims to develop and apply advanced turbulence monitoring and forecasting tools to support these three domains, enhancing the performance and reliability of ground-based optical systems.

Research Objectives:

1. Characterise atmospheric turbulence at key observatory and ground station sites using state-of-the-art instrumentation and data analysis techniques.
2. Develop and validate forecasting models, including data assimilation, for optical turbulence to support dynamic scheduling and adaptive system control in astronomy and communications.
3. Apply turbulence data to improve:
   1. Adaptive optics systems for large telescopes (e.g., VLT, ELT).
   2. Free-space optical communication links, including satellite-to-ground and inter-satellite systems.
   3. SSA systems for tracking and monitoring space debris and satellites.

Impact and Applications:

This project will contribute to:

1. Improving image quality and photometric precision in ground-based astronomy.
2. Enhancing the reliability and bandwidth of optical communication systems.
3. Supporting SSA efforts by refining ground-based tracking capabilities.

The student will join CfAI’s vibrant research environment, working alongside experts in adaptive optics, space instrumentation, and atmospheric physics. The project offers opportunities for international collaboration, fieldwork, and cross-sector impact.

Please contact James Osborn for more information

Top: PhD student developing and testing atmospheric optical turbulence instrumentation on La Palma, Spain.

Bottom: State of the Art turbulence forecast model developed at Durham. The colour indicates the strength of the atmospheric optical turbulence in units of the refractive index structure constant.

Developing Photon Counting Spectroscopy for Astronomy

Many of the most important discoveries in astronomy over the last decades have been driven by technological advances that have enabled researchers to open up new avenues of research. This includes advances in telescope design, such as with the upcoming Extremely Large Telescope (ELT), modes of operation such as Adaptive Optics and perhaps most importantly, through developments in the detector technologies used, such as moving from photographic plates to electronic imaging.

At Durham, we are part of a world-leading collaboration to develop and exploit Kinetic Inductance Detectors (KIDs) for optical and near-infrared astronomy. KIDs could potentially drive the next revolution in astronomy as they enable incredibly sensitive 3D spectroscopy by counting individual photons. They are made from super-conducting materials that use the kinetic inductance effect to measure the energy of a photon (to better than 10%) and its arrival time to better than 1 microsecond. By making arrays of 1000’s of such detectors, we are able to open areas of research impossible with other technologies.

One such area is the field of time domain astronomy, this growing field includes the observations of the compact binary precursors of gravitational wave sources and the transiting exoplanets, among others. These objects show variability on timescales of milliseconds to hours and you will observe this variability spectroscopically to determine the fundamental properties of such systems.

This project represents an exciting opportunity to join our team of students a post-docs and be involved in a novel instrumentation project from an early stage. We are looking for a highly motivated student to work on instrument development in the Centre for Advanced Instrumentation. No prior knowledge of KIDs is expected and all necessary training will be given. The project would suit students interested in experimental physics from a wide range of backgrounds, including astronomy, low temperature physics, optics, and superconductivity. Projects will include some observational astronomy alongside the instrument development.

Please contact Kieran O'brien for more information

Left: Microscope image (∼ 0.3 × 0.5mm) of pixels in a KID array, from Mazin Lab website. Centre and Right: photo of the KID development lab at Durham University.

Characterising atmospheric turbulence for ground based astronomy

The aim of this studentship is to develop new concepts and technology to characterise the effects of atmospheric turbulence for astronomy. The optical effects of atmospheric turbulence, known as ‘seeing’, are a major limitation for ground based optical astronomy. Seeing degrades the image resolution that can be achieved with large telescopes and adds noise to photometric
measurements.

The student will engage with the development, deployment and exploitation of site testing instrumentation for international observatories, with the goal of improving our understanding of the effects of the Earth’s atmosphere on astronomical observations.

A particular emphasis of this project will be to develop compact systems for turbulence monitoring with fixed pointing, so that they do not rely complex and expensive telescope and observatory installations for their operation.
The work will be directly applicable to current large astronomical telescopes, as well as the next generation of giant telescopes such as the 40 metre European Extremely Large Telescope in Chile. The aim is to provide data to improve the performance of large telescopes, for example through the optimisation of adaptive optics correction systems, or the forecasting of optical turbulence conditions at observatory sites. It will help them to reach their science goals, including characterising extra-solar planets, understanding the formation of galaxies, and elucidating the nature of dark matter and dark energy. Optical turbulence monitors also have wider applications, for example in the development of technology for satellite free-space optical communications.

The student will join the dynamic environment of the Centre for Advanced Instrumentation (CfAI), within the Physics Department at Durham University. The CfAI is a world leading research centre with a large and successful Astronomical Instrumentation group, including Adaptive Optics and Space Science technologies. CfAI has extensive experience in analysing atmospheric turbulence and the use of computer modelling of complex optical systems to design optical instrumentation for some of the world’s premier astronomical observatories.

Please contact Richard Wilson for more information.

Compact Terahertz Spectrometer based on Metasurfaces

Terahertz (THz) spectroscopy holds significant importance owing to the abundance of molecular and atomic fingerprint lines within this frequency range. In astronomy, THz spectroscopy provides a powerful probe of rotational and vibrational transitions of molecules, offering insights into star and planet formation as well as the physical and chemical processes in galactic and interstellar environments.

Conventional THz spectrometers typically rely on multiple free-space optical elements or moving parts, which makes them bulky and challenge to integrate into compact systems. Metasurfaces - planar optical components composed of subwavelength nanostructures, have recently emerged as a powerful new approach for controlling the polarization, phase, and amplitude of light with unprecedented flexibility. These advances open the door to the design of highly compact and versatile spectroscopic instruments.

This PhD project will focus on the development of a proof-of-concept compact THz spectrometer based on metasurfaces. The project will span scales from designing and optimizing nanophotonics to integrating and characterizing a full spectrometer system. We are seeking a motivated candidate with a strong interest in experimental physics. Applicants from broad backgrounds, including astronomy, optics, electrical engineering are encouraged to apply.

For more information, please contact: Yuan Ren

Building a High-Spectral-Resolution Spectrograph to Probe Comets and Trace the Origins of Volatiles

The processes behind the formation of planetary systems, their evolution, and their ability to support life remain some of the most profound and unresolved questions in astronomy. Investigating these phenomena is a major scientific challenge, and interplanetary objects such as comets serve as critical windows into the early stages of planetary development. Their icy cores preserve essential clues about the environments in which the first planets formed, offering valuable insights into the history of the solar system.

Isotopic ratios - the relative abundances of isotopes of a given element - are particularly powerful for probing the formation and evolutionary history of cometary materials. These ratios provide direct information about the processes and environments that shaped the early solar system and are key to tracing the origins of volatiles in comets. To quantify isotopic ratios with a strong signal, a high-resolution spectrograph in orbit is required.

This PhD project aims to explore early designs and prototypes of a VIPA-based Isotope Ratio Spectrograph (VIPAIRS): a compact, high-resolution spectrometer (R > 100,000) capable of measuring isotopic signatures for the first time. Other applications, such as probing atmospheric trace gases (e.g., O₂, CO₂), will also be investigated.

• Develop an analytical model of the VIPA spectrograph and a data reduction pipeline to extract spectral information.
• Prototype a visible/near-infrared system and validate its performance, exploiting its compactness and high resolution more effectively than currently available instrumentation.
• Investigate novel VIPA-based technology concepts, such as a multiband VIPA spectrograph using a filtered camera, a tunable VIPA, and multiple VIPA beams combined onto a single detector.
• Contribute to the design of a UV spectrograph, capable of acquiring a comprehensive dataset of isotopic ratios for H, N, C, and O in the UV spectrum in comets.

The student will join CfAI’s research environment, working alongside experts in adaptive optics, space instrumentation, and atmospheric physics. The project will involve travel between the two CfAI sites: The Ogden Centre on Durham campus and the NETPark Research Institute in Sedgefield (20 minutes by bus from Durham city).

For more information, please contact: Cyril Bourgenot 

Ultra High Energy Neutrino Astronomy with Trinity

The Trinity telescope is a new and unique approach to observing the neutrino Universe. Trinity will
indirectly observe Ultra-High-Energy (UHE) tau neutrinos by detecting the Cherenkov radiation emitted by
an upwards going air shower that appears out of the ground. This air shower is the result of a tau neutrino
skim through the Earth’s crust, interacting with matter to produce a tau particle, which decays as it comes
out of the Earth. By placing a bespoke wide-field-of-view telescope on a mountain, and pointing it below
the horizon, Trinity will observe these upwards travelling flashes of light (see Figure 1 below). Essentially,
Trinity is translating expertise in gamma-ray astronomy to UHE neutrino astronomy, which allows us to
minimise the observed background, whilst maximising the energy and angular resolution of the observations.

In your PhD, you’ll be joining the Trinity collaboration, exploiting the Trinity demonstrator telescope
to open up the UHE neutrino window to the Universe. Supervised by Dr Anthony Brown, and interacting
closing with international collaborators in the USA, the PhD post will make significant contributions to
several key operational aspects of Trinity. Your tasks will include developing new (drone-based) hardware to
calibrate Trinity, quantifying the sensitivity of Trinity and interpreting Trinity observations to place sensitive
flux limits on UHE neutrino emission from astrophysical sources.

For more information, please contact: Anthony Brown

Images outlining key aspects of the position. Top: schematic outlining key components of Trinity’s
detection technique. Middle: first data of drone-based mirror
alignment (September 2024).Bottom: photo of drone-based light source illuminating the Trinity demonstrator
telescope (for a variety of calibration requirements). 

Improving the Accuracy of Drone Based Remote Sensing with Astronomical Instrumentation

The recent advances in UAV capability has given the remote sensing community a number of exciting
possibilities. Unfortunately, in the context of plant ecology, the realization of this potential has focused on
monitoring crop health where the species of plant is known. Furthermore, this monitoring is usually restricted
to a small number of wavelengths, resulting in a noisy dataset that is not able to differentiate between plant
species or identify pathogens. As such, UAVs have not realised their full potential in UAV-based remote
sensing of plants. This unrealised potential also applies to other areas of UAV-based remote sensing such as
atmospheric content where UAV technology affords us the possibility of mapping out temporal and spatial
variations in atmospheric gas and dust content.

This PhD position will look to combine astronomical instrumentation, UAV technology and machine
learning, with a sensor-fusion approach to improve remote sensing capability. To achieve this, your tasks will
include developing new imaging capability to mount to UAVs, apply machine learning analysis to remote
sensing data sets to improve remote sensing accuracy and conduct simulations to quantify the accuracy of
the new remote sensing capability.

For more information, please contact: Anthony Brown

Top: image of UAV-based calibration system above a telescope array in Namibia. Bottom: UAV imagery of a wheat field with different pathogens

Multi-Wavelength wavefront sensing for exoplanet imaging

Most large telescopes make use of adaptive optics to overcome the blurring effects of atmospheric turbulence, allowing observations of the universe with exquisite spatial resolution. Adaptive optics observations have unlocked new science over the last two decades, enabling the characterisation of high-redshift galaxy kinematics, confirmed the existence of the super massive black hole at the center of our galaxy (winning the 2020 Nobel prize in Physics), and taking direct images of gas giants orbiting other stars. The next generation of extremely large telescopes with 30+ meter diameter primary mirrors coming online in the next decade and these telescopes all use adaptive optics. One of the driving science goals for these telescopes is to image exoplanets and characterise their surfaces and atmospheres. To meet this ambitious challenge we require research into new techniques,
technologies, and instrumentation that will enhance adaptive optics system performance beyond what is currently possible.

One of the key pieces of technology within an adaptive optics system is the wavefront sensor, which measures the
atmospheric phase aberrations several thousand times a second. The Pyramid wavefront sensor is at the heart of many highperformance adaptive optics systems, however it suffers from chromatic and non-linear effects that can affect measurements. The extremely large telescopes themselves also introduce complex wavefront aberrations that can be difficult to measure and control with existing Pyramid sensors. Recent research by Durham and collaborators has shown that by combining Pyramid wavefront sensor measurements at multiple wavelengths we can overcome many of these effects.

The goal of this project will be to develop an instrument that will provide the first on-sky demonstration of a multiwavelength Pyramid wavefront sensor. The instrument will be installed on a 2-meter diameter telescope in Asiago (Italy) where an international team of young adaptive optics researchers and students are working on the development of a new adaptive optics testbed. No experience of optical instrumentation development is required for this PhD but you will need to have an interest in experimental physics and be willing to learn a wide range of transferrable skills such as optical design, data reduction, and adaptive optics simulation development. This is a rare opportunity to undertake research and development of a new technology and test it at a telescope. A successful demonstration of this technology in the next few years could result in it being adopted for use in the next generation of planet characterising instruments.

For more information, please contact: Tim Morris

Image of the 39m Extremely Large Telescope under construction in Chile. Image ©European Southern Observatory