A theoretical framework to understand the diversity of exoplanet atmospheres with current and future observatories

The exoplanet field has been evolving at an astonishing rate: nearly two thousand planets have been detected and many more are awaiting confirmation. Astronomers have begun classifying these planets by mass, radius and orbital parameters, but these numbers tell us only part of the story as we know very little about their chemical composition. Spectroscopic observations of exoplanet atmospheres can provide this missing information, critical for understanding the origin and evolution of these distant worlds. Currently, transit spectroscopy and direct imaging spectroscopy are the most promising methods to achieve this goal. Ground and space-based observations (VLT, Keck Observatory, IRTF, Spitzer Space Telescope, HST) of exoplanets have shown the potentials of the transit method. However, the instruments used in the past ten years were not optimised for this task: the available data are mostly photometric or low resolution spectra with low signal to noise. The interpretation of these --- often sparse --- data is generally a challenge. With the arrival of new facilities (GPI, SPHERE, E-ELT, JWST), and possibly dedicated space instruments such as the Exoplanet Characterisation Observatory (EChO), many questions needed to be tackled in a more systematic way. The focus of this thesis is to provide a theoretical framework to address the question of molecular detectability in exoplanet atmospheres with current and future facilities. The atmospheric components and their spectroscopic signals depend strongly on the planetary temperature and size, therefore I have simulated a significant sample of planets out of a range of sizes and temperatures, to describe comprehensively the chemical compositions that can be expected in those exotic worlds. Such simulations were convolved through instrument simulators to assess performance and limitations of current and future facilities. While my study has been inspired by transit spectroscopy with a hypothetical EChO-like space-based instrument, the methodology and results of this thesis are applicable to observations with other instruments and techniques

Photometric stability analysis of the Exoplanet Characterisation Observatory

Photometric stability is a key requirement for time-resolved spectroscopic observations of transiting extrasolar planets. In the context of the Exoplanet Characterisation Observatory (EChO) mission design, we here present and investigate means of translating spacecraft pointing instabilities as well as temperature fluctuation of its optical chain into an overall error budget of the exoplanetary spectrum to be retrieved. Given the instrument specifications as of date, we investigate the magnitudes of these photometric instabilities in the context of simulated observations of the exoplanet HD189733b secondary eclipse.Comment: submitted to MNRA

Small bodies science with the Twinkle space telescope

© 2019 Society of PhotoOptical Instrumentation Engineers (SPIE). Twinkle is an upcoming 0.45-m space-based telescope equipped with a visible and two near-infrared spectrometers covering the spectral range 0.4 to 4.5 μm with a resolving power R 250 (λ 2.42 μm). We explore Twinkle's capabilities for small bodies science and find that, given Twinkle's sensitivity, pointing stability, and spectral range, the mission can observe a large number of small bodies. The sensitivity of Twinkle is calculated and compared to the flux from an object of a given visible magnitude. The number, and brightness, of asteroids and comets that enter Twinkle's field of regard is studied over three time periods of up to a decade. We find that, over a decade, several thousand asteroids enter Twinkle's field of regard with a brightness and nonsidereal rate that will allow Twinkle to characterize them at the instrumentation's native resolution with SNR > 100. Hundreds of comets can also be observed. Therefore, Twinkle offers researchers the opportunity to contribute significantly to the field of Solar System small bodies research

EChOSim: The Exoplanet Characterisation Observatory software simulator

EChOSim is the end-to-end time-domain simulator of the Exoplanet Characterisation Observatory (EChO) space mission. EChOSim has been developed to assess the capability EChO has to detect and characterize the atmospheres of transiting exoplanets, and through this revolutionize the knowledge we have of the Milky Way and of our place in the Galaxy. Here we discuss the details of the EChOSim implementation and describe the models used to represent the instrument and to simulate the detection. Software simulators have assumed a central role in the design of new instrumentation and in assessing the level of systematics affecting the measurements of existing experiments. Thanks to its high modularity, EChOSim can simulate basic aspects of several existing and proposed spectrometers for exoplanet transits, including instruments on the Hubble Space Telescope and Spitzer, or ground-based and balloon borne experiments. A discussion of different uses of EChOSim is given, including examples of simulations performed to assess the EChO mission

A sustainable path for space science

High-performance scientific satellites are currently the exclusive domain of government-funded agencies. The team behind the Twinkle Space Mission is developing a new class of small and sustainable science satellites that leverages recent innovations in the commercial space sector

A catalogue of bright (K <9) M dwarfs

Using the Position and Proper Motion Extended-L (PPMXL) catalogue, we have used optical and near-infrared colour cuts together with a reduced proper motion cut to find bright M dwarfs for future exoplanet transit studies. PPMXL's low proper motion uncertainties allow us to probe down to smaller proper motions than previous similar studies. We have combined unique objects found with this method to that of previous work to produce 8479 K <9 M dwarfs. Low-resolution spectroscopy was obtained of a sample of the objects found using this selection method to gain statistics on their spectral type and physical properties. Results show a spectral-type range of K7-M4V. This catalogue is the most complete collection of K <9 M dwarfs currently available and is made available here.Peer reviewe

Exoplanet spectroscopy and photometry with the Twinkle space telescope

The Twinkle space telescope has been designed for the characterisation of exoplanets and Solar System objects. Operating in a low Earth, Sun-synchronous orbit, Twinkle is equipped with a 45 cm telescope and visible (0.4 – 1 μm) and infrared (1.3 – 4.5 μm) spectrometers which can be operated simultaneously. Twinkle is a general observatory which will provide on-demand observations of a wide variety of targets within wavelength ranges that are currently not accessible using other space telescopes or accessible only to oversubscribed observatories in the short-term future. Here we explore the ability of Twinkle’s spectrometers to characterise the currently-known exoplanets. We study the spectral resolution achievable by combining multiple observations for various planetary and stellar types. We also simulate spectral retrievals for some well-known planets (HD 209458 b, GJ 3470 b and 55 Cnc e). From the exoplanets known today, we find that with a single transit or eclipse, Twinkle could probe 89 planets at low spectral resolution (R 20) in channel 1 (1.3 – 4.5 μm). With 10 observations, the atmospheres of 144 planets could be characterised with R 20. By stacking 10 transits, there are 1185 potential targets for study at R < 20 as well as 388 planets at higher resolutions. The majority of targets are found to be large gaseous planets although by stacking multiple observations smaller planets around bright stars (e.g. 55 Cnc e) could be observed with Twinkle. Photometry and low resolution spectroscopy with Twinkle will be useful to refine planetary, stellar and orbital parameters, monitor stellar activity through time and search for transit time and duration variations (TTVs and TDVs). Refinement of these parameters could be used to in the planning of observations with larger space-based observatories such as JWST and ARIEL. For planets orbiting very bright stars, Twinkle observations at higher spectral resolution will enable us to probe the chemical and thermal properties of an atmosphere. Simultaneous coverage across a wide wavelength range will reduce the degeneracies seen with Hubble and provide access to detections of a wide range molecules. There is the potential to revisit them many times over the mission lifetime to detect variations in cloud cover

Bringing pupils into the ORBYTS of research

Most scientists would consider themselves lucky to publish a research paper while still an undergraduate, but a group of pupils at Highams Park School in East London has co-authored a paper at age 18, thanks to ORBYTS. Original Research By Young Twinkle Scientists (ORBYTS) comprises the core part of EduTwinkle, the education and outreach arm of the upcoming exoplanet space mission Twinkle, led by UK scientists and engineers, and is aimed at A-level students. ORBYTS was founded in 2016 by Clara Sousa-Silva, who was splitting her time teaching at Highams Park School and working as a postdoc at University College London, via the Researchers in Schools programme. This blend of education and research inspired her to set up a scheme enabling young postdoc and PhD students from her research group at UCL, ExoMol, to perform novel research with some of her sixth-form students. ORBYTS now involves more than 30 pupils in eight schools across the UK