Ian B. Hutchinson's research while affiliated with University of Leicester and other places

... Additionally, the vibrational bands at 610 and 597 cm −1 only exhibited by AC1 among all the samples, according to the literature [35,39], can be attributed to the asymmetric deformation vibrations of free tetrahedral SO 4 2− , considering the results in Table 2, AC1 owns the highest content of sulfur content, it proves the residual SO 4 2− in AC1 structurally. Table 3 The Raman spectrum is shown in Fig. 8. Bands at 142 cm −1 , 425 cm −1 , 511 cm −1 correspond to the Si-O lattice vibrations [40,41], and the decrease of intensity in these bands indicates that the reduction in crystallinity, which is consistent with the results of XRD. And bands at 665 cm −1 and 752 cm −1 can be attributed to vibration of Si-O-Si [42] and stretching vibration of Al-O group, respectively. ...

... Therefore, its origin, form, and thermal history could greatly inform our understanding of Mars' past habitability. The paper of McHugh et al. (Raman Analysis of a Shocked Planetary Surface Analog: Implications for Habitability on Mars, University of Leicester, UK) [24] reports on the Raman analysis of a Nakhla meteorite analog (containing carbonaceous material) that was subjected to shock through projectile impact to simulate the effect of meteorite impact. The characterization was performed using the RLS Simulator, in an equivalent manner to that planned for ExoMars operations. ...

... Indeed, a great opportunity exists for new missions with widefield-of-view soft X-ray instruments designed to simultaneously observe the GRB X-ray and gamma-ray emissions from 0.3 keV to 10 MeV from the moment of the GRB trigger without any time delay, such as, e.g., THESEUS (Amati et al. 2018(Amati et al. , 2021 and HERMES (Fuschino et al. 2019;Fiore et al. 2020). ...

... The existing approaches to Raman spectroscopy for quantitative analysis can be classified into two distinct groups: Raman imaging (or point-counting; Haskin et al., 1997; and models based on spectral parameters (Demaret et al., 2021). The former is based on statistical principles of the acquired spectral data sets. ...

... Early in the mission development, it was identified that the spacecraft would not be capable of cooling the SXI focal plane to the low temperatures necessary for the use of CCDs. 7 This is a consequence of the orbital properties of the mission, which involve occasional transits through the South Atlantic Anomaly. During these repeated orbits over the course of the 3-year mission, the estimated end-of-life proton fluence for the SXI detectors is 1.55 × 10 9 p þ (60 MeV)/cm 2 . ...

... Thereafter, many lobster eye telescopes were installed on pico or nano satellites (Van Inneman et al. 2000;Hudec 2018;Su et al. 2018) or the International Space Station (Tremsin & Siegmund 1998;Fraser et al. 2002) for X-ray observations. Thanks to these successful applications, lobster eye telescopes are now considered important wide-field X-ray survey instruments for many satellites, such as the Microchannel X-ray Telescope on board the SVOM (Gotz et al. 2014), the Wide-field X-ray Telescope (WXT) on board the Einstein Probe (EP; Yuan et al. 2018), the Soft X-ray Imager (SXI) on board the SMILE (Peng et al. 2018), the LEXT on board the Gamow (Feldman et al. 2021), and the SXI on board the Theseus (Feldman et al. 2020). The point-spread function (PSF) of lobster eye telescopes (Rhea et al. 2021) is very unique, which would spread photons to a very large scale. ...

... It is worth noting that, a previous thermal test performed on a separate WXT qualification model at the 100XF shows no noticeable variations in the optical performance as the whole MA is heated uniformly all the way up to 25 degrees. Furthermore, in a thermal experiment on another qualification model of the MA carried out at the University of Leicester as a collaborative work [22], it was found that the imaging quality of the MA remains almost unchanged with a thermal gradient of ∼ 9 o C across the optic (private communication, Feldman Charlotte). The performance of the CMOS sensors onboard LEIA operated at various temperatures will be presented elsewhere (Ling et al. in preparation). ...

... Over the past decades the LE optics has been studied extensively by several groups (e.g., Wilkins et al. 1989;Chapman et al. 1991;Fraser et al. 1992Fraser et al. , 1993Kaaret et al. 1992;Peele et al. 1996;Brunton et al. 1999;Zhao et al. 2014;Collier et al. 2015;Willingale et al. 2016;Hudec et al. 2017), and conceptual designs for LE X-ray ASMs have also been proposed (e.g., Priedhorsky et al. 1996;Fraser et al. 2002). In practice, a number of realistic missions with LE ASMs have been proposed (e.g., Yuan et al. 2016;O'Brien et al. 2020). ...

... Clearly, the sample preparation processes, resulting grain size distribution, and flattening process are critical aspects of the RLS instrument performance, and they are related to the instrument mineral identification capabilities and the overall scientific performance of the instrument. Once the capabilities and performance of the RLS Engineering and Qualification Model (EQM) have been demonstrated, [17] the biggest challenge for RLS is in dealing with these uncertainties. For that reason, the RLS EQM has been comprehensively tested to demonstrate that the ALD SPDS QM sample grain distribution and flattening processes are compatible with the RLS performance requirements. ...

... In general, carbonate and sulphate are the principal components of natural minerals [51]. In this study, calcium carbonate (Aladdin, CAS: 471-34-1, AR Grade, CaCO 3 ) and sodium sulphate (Aladdin, CAS: 7757-82-6, AR Grade, Na 2 SO 4 ) were used as mineral samples to simulate mineral detection in the ions, and the 992 cm −1 peak of sodium sulphate is assigned to the symmetric stretching mode of SO 2− 4 ions. ...