ORCID Profile
0000-0001-8932-9694
Current Organisations
European Space Astronomy Centre
,
Indiana University Bloomington
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Publisher: Copernicus GmbH
Date: 23-09-2022
Abstract: & & & strong& Mars Express& /strong& & & & & With almost two decades of Mars observation behind it, Mars Express remains a dependable and highly productive mission.& & & & Recent science highlights include (1) continued mapping of subsurface reflectors beneath the south polar layered ice deposits, and associated work to explain the cause of these reflections (2) a global map of minerals on Mars with 200 m x resolution, obtained from analysis of infrared spectra (3) release of 50 m resolution Digital Elevation Models based on HRSC stereo topography for quadrangles covering an ever-increasing proportion of the global surface (4) detailed characterization of the landing sites of the ESA, NASA and Chinese rovers (5) a global climatology of ozone and water from both nadir and occultation observations and its relation to atmospheric dust (6) transient atmospheric phenomena, such as a recurrent orographic cloud feature at Arsia Mons (7) detailed investigation of the ionospheric structure, its variability, and coupling to the lower atmosphere (8) continued monitoring of both the upstream solar wind conditions and of downstream escaping ions (9) detailed study of Phobos during flybys at altitudes as low as 50 km.& & & & Spacecraft and instrument teams continue to implement new and improved observation modes. One ex le is new MARSIS instrument software which now allows raw data to be returned from much longer subsurface sounding passes, improving the search for basal reflectors beneath polar ice caps another ex le is mutual radio occultation observations between Mars Express and ExoMars Trace Gas Orbiter, potentially providing vertical profiles of ionospheric electron content with good spatial and temporal coverage.& & & & & & & & & & strong& ExoMars Trace Gas Orbiter& /strong& & & & & & TGO has now completed two full Martian years of observations.& & & & Highlights include (1) continuing non-detection of methane, with upper limits as low as 20 ppt by volume. Reconciling this continued non-detection by TGO with the background levels of several hundred ppt in Gale crater by MSL remains an enigma, stimulating further research. (2) detection of HCl, the first reported halogen-containing species in the atmosphere of Mars. (3) further detail of the transport of water to high altitudes, a critical step in the escape of water from Mars. (4) mapping of atomic hydrogen in the top 1-2 m of regolith, indicative of water ice and hydrated minerals, suggesting surprisingly high abundances of subsurface water ice in low latitude regions including one in central Valles Marineris and (5) continued acquisition of 5 m colour imagery and digital elevation models over a wide range of terrain and target types, including landing site characterization.& & & & & & & & & & strong& Future plans:& /strong& Mission extension cases for both missions have been submitted for the years 2023-2025 and 2026-2028. The extension of the observations would allow several new and optimized observation types in particular, it will allow many collaborative observation opportunities with other missions and with ground- and space-based observatories. Of particular note are joint observations with James Webb Space Telescope, for which dedicated observations of Mars are due to be conducted in 2022-2023. Science goals include mapping of the water D/H ratio, search for trace gases including methane, and mapping of thermospheric structure using 4.3 & #956 m CO2 emission the full-disk views provided by JWST are highly complementary to the vertical profiling and long temporal coverage provided by MEx and TGO.& & & & & strong& & & /strong& & &
Publisher: Copernicus GmbH
Date: 23-09-2022
DOI: 10.5194/EPSC2022-136
Abstract: & & The scientific objectives of Mars Express (MEX) and ExoMars 2016 Trace Gas Orbiter (TGO) missions are very complementary, with increasing synergies among the science teams, in particular for the study of the atmosphere. In this contribution we summarize the coordination efforts to perform joint observations by the two European satellites around Mars until 2022, and the science opportunities for the expected mission extension until 2025.& & & & Since the start of the TGO science operations in April 2018 we have executed hundreds of coordinated observations of the Martian atmosphere, first reported in [1,2] and extended here to 2022. The science data obtained during these coordinated observations provide useful input for cross-calibration of the instruments, comparison of atmospheric vertical profiles, and potential for the study of the temperature, composition, meteorology and climate of Mars.& & & & & img src=& quot & quot alt=& quot & quot width=& quot & quot height=& quot & quot /& & & & & Figure 1: & Types of coordinated observations performed:& MEX-TGO Sun Occultations (within 15min and distance & km), MEX-TGO Nadir crossings& (simultaneous, within & deg seen from Mars center), MEX Nadir over TGO Sun Occultation point (simultaneous within distance & km), and MEX-TGO Radio Occ. points (tested in 2021 and run operationally in 2022 onwards)& & & & These observations are routinely coordinated in collaboration between the Science Operations Centers (SOCs) of both missions [1, 3] and the instrument teams, in particular the spectrometers NOMAD and ACS onboard TGO [4,5] and SPICAM, OMEGA and PFS onboard MEX [6,7,8].& & & & The various types of joint observations are represented in Figure 1. First the joint solar occultations by the spectrometers SPICAM (MEX) and ACS-NOMAD (TGO) are performed quasi-simultaneously (& minutes difference), allowing the comparison of vertical profiles of the atmosphere in the same region (& km distance) both at the ingress and egress points (i.e. dusk and/or dawn terminator). Then, all spectrometers observe regularly in nadir geometry and we have so far performed hundreds of simultaneous observations of the crossing points (within ~350km, or & deg as seen from Mars) and quasi-simultaneous observations of the same location within a few minutes difference, at various distances and illumination conditions. Then with MEX we are also observing nadir in the region of the TGO solar occultation, so vertical atmospheric profiles can be complemented with wider contextual imaging and/or temperature retrievals. Finally, in 2021 we have validated the spacecraft-to-spacecraft radio occultations [9], and started routine observations in 2022 to provide useful information of the ionosphere.& & & & The authors acknowledge the contributions of the European Space Agency, Roscomos, all National Agencies, research institutions and teams involved in the success of the Mars Express and ExoMars 2016 missions. ExoMars is a space mission of the European Space Agency (ESA) and Roscosmos (Russia).& & & & References:& & & & [1] Cardesin Moinelo, A. et al: First year of coordinated science observations by Mars Express and ExoMars 2016 Trace Gas Orbiter, ICARUS 353, 2021& & & & [2] Cardesin Moinelo, A. et al: Atmospheric observations performed simultaneously in 2020-2021 by ESA& #8217 s Mars Express and Trace Gas Orbiter, European Planetary Science Congress, Vol. 15, EPSC2021-128, 2021& & & & [3] Geiger, B et al: Long Term Planning for the ExoMars Trace Gas Orbiter Mission: Opportunity Analysis and Observation Scheduling, Proceedings of SpaceOps Conference, 2018& & & & [4] Vandaele, A. C. et al: NOMAD, an Integrated Suite of Three Spectrometers for the ExoMars Trace Gas Mission: Technical Description, Science Objectives and Expected Performance, Space Sci Rev 214: 80. 2018& & & & [5] Korablev, O. et al: The Atmospheric Chemistry Suite (ACS) of Three Spectrometers for the ExoMars 2016 Trace Gas Orbiter Space Sci Rev 214: 7. 2018& & & & [6] Montmessin et al, SPICAM on Mars Express: A 10 year in-depth survey of the Martian atmosphere. Icarus, Volume 297, p. 195-216. 2017& & & & [7] Bibring, J.-P., et al., OMEGA: Observatoire pour la Min& #233 ralogie, l& #8217 Eau, les Glaces et l& #8217 Activit& #233 , ESA SP-1240, pp. 3& #8211 . 2004& & & & [8] Formisano V. et al: The Planetary Fourier Spectrometer (PFS) onboard the European Mars Express mission, Planetary and Space Science, Volume 53, Issue 10, p. 963-974. 2005& & & & [9] Svedhem H. et al: First results from the MEX & #8211 TGO Mutual Radio Occultation Experiment, European Planetary Science Congress, Vol. 15, Vol. 15, EPSC2021-719, 2021& &
Publisher: Copernicus GmbH
Date: 15-05-2023
DOI: 10.5194/EGUSPHERE-EGU23-8669
Abstract: Mars Express, ESA's first flagship for Mars exploration, will reach the momentous milestones of 20 years in space and at Mars on 2 June and 25 December this year, respectively. Its scientific record is unprecedented for a mission which was initially planned for one Martian year. Since end 2003 Mars Express has gathered a wealth of data from the subsurface, surface, atmosphere, plasma environment and moons of the red planet in a quasi-uninterrupted and routine way. Furthermore, Mars Express is currently as scientifically active and productive as at any time through its lifetime in space, thanks to several additions and improvements recently made to its spacecraft and payload capabilities (e.g., MARSIS radar new subsurface and Phobos operative modes, radio frequency occultation measurements between Mars Express and ESA& #8217 s Trace Gas Orbiter using an upgraded MELACOM communications system, plasma sounding by ASPERA during MARSIS measurements, occultation observations during egress). Mars Express is expected to maintain and even enhance its scientific return over the next few years, should the mission be extended. Technical feasibility of further mission extensions has been reviewed and confirmed. The mission is constrained by 3 lifetime-limiting elements which are the remaining gyro lifetime, remaining fuel and the battery lifetime. However, it has been demonstrated that none of those 3 constraints is likely to prevent Mars Express from continuing its routine operations until beyond 2030. Whether Mars Express is extended or not, nominal archiving is proceeding at pace and higher-level data sets being produced in collaboration with the PI teams to optimise the Mars Express archive legacy.The mission and science operations teams, together with the mission scientists, are looking forward to several additional years of scientific productivity and discoveries. Successful joint science c aigns with the CNSA Tianwen/Zhurong orbiter and rover missions, UAE& #8217 s Hope orbiter mission, and especially the upcoming MMX mission to Phobos by JAXA should contribute to further augment Mars Express& #8217 20-year success story.
Publisher: Copernicus GmbH
Date: 23-09-2022
DOI: 10.5194/EPSC2022-684
Abstract: & & The Visual Monitoring Camera (VMC) is a small camera onboard Mars Express, initially intended to provide visual confirmation of the separation of the Beagle 2 lander. In 2007, a few years after the end of its original mission, VMC was turned on again to obtain full-disk images of Mars for outreach purposes (Ormston et al., 2011). As VMC obtained more images, the scientific capabilities of the camera became evident (S& #225 nchez-Lavega et al., 2018), and finally the small camera was upgraded to be a new scientific instrument, with an agreement between the European Space Agency (ESA) and the University of the Basque Country (Spain UPV/EHU). In this work we describe the calibration and technical efforts that are allowing us to maximize the scientific output from this small camera.& & & & & img src=& quot & quot alt=& quot & quot /& & & & & Figure 1. Image of VMC before launch (left) and scheme from the Flight User Manual (right)& & & & & & & & & VMC is also called the Mars webcam, as it is similar to a typical webcam of the 2000s. The sensor has a a 640x480 pixel array, and a Field of View (FOV) of 30& #186 x40& #186 . This wide FOV, together with the elliptical orbit of Mars Express, enables full-disk observations from apocenters, which are the most common product of VMC. It is also possible to use this wide FOV to image large sections of the limb, and therefore monitor the occurrence of high altitude aerosols, as shown by S& #225 nchez-Lavega et al. (2018).& & & & & img src=& quot & quot alt=& quot & quot /& & & & & Figure 2. Full disk of Mars as seen by VMC.& & & & & & & & & & strong& Operations& /strong& & & & & Since 2018 VMC operations follow a similar routine as those used for other science instruments. The Science Ground Segment takes care of the Medium Term Planning (MTP) following the inputs from the science team. The science team performs the Short Term Planning (STP). Fig. 3 shows a typical VMC observation, which consists of a default image, followed by one to several loops of 6 images that use a set of predefined exposures. The exposure times are set to maximize the dynamic range of the final science products obtained by combining the in idual images.& & & & & img src=& quot & quot alt=& quot & quot /& & & & & Figure 3. Scheme of a typical VMC observation.& & & & & & & & & & strong& Calibration of images& /strong& & & & & The images are calibrated following the standard scheme of subtracting a dark current and iding by a flatfield image. The flat field correction is much more relevant than the dark correction in the quality of the final images after calibration. No onground calibration is known for VMC, therefore the dark current and flat-field corrections used are based only on in-flight observations. The dark was obtained by pointing VMC to the sky, specifically the area of Eridanus, where few bright stars are present.& & & & The flat-field was created using dark-corrected images of flat portions of Mars that were well and uniformly illuminated, as free as possible from large structures, and as flat as possible.& & & & Calibrated images are routinely archived at ESA& #8217 s Planetary Science Archive (PSA), as described by Ravanis et al. (2020)& & & & & img src=& quot & quot alt=& quot & quot /& & & & & Figure 4. VMC dark (left) and flat (right).& & & & & & & & & & strong& Geometry& /strong& & & & & The original documents indicate the design parameters for the orientation of VMC in the reference frame of MEX, and for the pixel resolution (iFOV). However, the accurate parameters once VMC was mounted on MEX were never measured on the ground. In addition to this, we find that the timest of images suffers a random shift of a few seconds. As a result, we have 5 free parameters: 3 Euler angles for the attitude relative to the MEX reference frame the pixel resolution (iFOV) and the shift in time from the actual timest to the labeled timest .& & & & In order to determine the attitude and iFOV of VMC relative to Mars Express, we used images showing stars. Many of these observations covered the stars of the constellation of Orion, because several suitable stars are present in that region of the sky. During these observations the spacecraft maintains a fixed attitude, therefore, the time related uncertainty is not present and only 4 free parameters remain: 3 Euler angles, and the pixel size. These parameters are shown in table 1.& & & & & img src=& quot & quot alt=& quot & quot width=& quot & quot height=& quot & quot /& & & & & Table 1. VMC geometric parameters as given by the Flight User Manual (FUM) and calibrated values.& & & & The shift in time was estimated from observations showing Phobos. The relative speed of Phobos as seen from Mars Express is high, and therefore it is possible to use its position as an accurate clock. We find that our images are usually obtained between 6 and 13 seconds before the labeled time, but we find random variations. Subtracting 10 seconds is considered a good strategy in most cases, but this uncertainty remains as a limitation.& & & & & img src=& quot & quot alt=& quot & quot /& & & & & Figure 5. VMC image showing the stars of Orion (left), and Phobos in front of Mars (right). Red circles represent the expected position before calibration. Green circles are the expected positions according to the new calibration.& & & & & & & & & & strong& Conclusions& /strong& & & & & Within the expectable limitations, the performance of this new instrument is very good and VMC is enabling novel science results and techniques (e.g. Hern& #225 ndez-Bernal et al. 2021). This is in part because VMC provides some capabilities that are not common among instruments in orbital planetary missions. Even with no on-ground calibration available, it has been possible to calibrate the camera, both photometrically and geometrically. Some hardware limitations remain, and others have been partially overcome with specially developed operational strategies.& & & & & & & & & & strong& References& /strong& & & & & Hern& #225 ndez& #8208 Bernal et al. (2021). A Long& #8208 Term Study of Mars Mesospheric Clouds Seen at Twilight Based on Mars Express VMC Images.& & & & Ormston et al. (2011) An ordinary camera in an extraordinary location: Outreach with the Mars Webcam.& & & & Ravanis et al. (2020). From engineering to science: Mars Express Visual Monitoring Camera's first science data release.& & & & S& #225 nchez-Lavega et al. (2018). Limb clouds and dust on Mars from images obtained by the Visual Monitoring Camera (VMC) onboard Mars Express.& &
Publisher: SAGE Publications
Date: 03-12-2021
DOI: 10.31124/ADVANCE.17099393
Abstract: We used descriptive statistics and a logistic regression to examine between-school inequalities in science and math curricular offerings in Year 12 (final year) in all schools in one Australian state (Victoria). Dataset contains variables about school contexts: school enrolment size, school socioeconomic composition, school sector, and school location.
Publisher: Copernicus GmbH
Date: 23-09-2022
DOI: 10.5194/EPSC2022-939
Abstract: & & & strong& Abstract& /strong& & & & & The European Space Agency& #8217 s (ESA) Mars Express (MEX) mission to Mars has been returning valuable scientific data for ~18 years.& & This data is available to the public for free via the Planetary Science Archive (PSA), which houses the raw, calibrated, and higher-level data returned by the ESA& #8217 s planetary missions, including data provided by the various MEX instrument teams.& & The High Resolution Stereo Camera (HRSC) has provided several types of datasets throughout the mission, and its images have proven popular not only among scientists but also the public for the spectacular images of the red planet.& A new version (version 4.0) of the radiometrically calibrated HRSC data has been made available which covers the entirety of the mission& #8217 s operation up to now.& & & & & & This new version utilizes an updated calibration, which is especially important for later images as it improves the adjustments for the aging of the instrument [1].& In addition to the new calibration, the data is now split into mission phases.& Previous versions of the radiometrically calibrated data incorporated all observations into a single dataset, which led to increasing lag in some access methods as the dataset continued to grow in size and number of files.& All this data and more can be accessed at the PSA at: archives.esac.esa.int sa/& & & & & & & & & & strong& Introduction& /strong& & & & & MEX was inserted into Mars orbit in December 2003, though several instrument test observations also exist from the cruise phase of the mission, prior to arrival at Mars.& Thus, this long-lived Mars mission covers 18+ years of data with its 7 instruments.& Later in the mission& #8217 s lifetime, the camera used for the Beagle 2 lander separation was reactivated and used for public outreach.& Over time, the camera began to be used for scientific observations as well, making& MEX an unusual mission in that it now has more scientific instruments in operation than it was launched with.& & & & & & & & & & strong& The PSA user interface& /strong& & & & & The ESA& #8217 s PSA uses the Planetary Data System (PDS) format developed by NASA to store the data from its various planetary missions.& In the case of MEX, the data is stored in the PDS3 format, which primarily uses ASCII files to store and describe the data. & Newer missions, from ExoMars onward use the PDS4 data standard, which uses XML files.& There are three primary ways in which to find the data.& One is the FTP area, which houses all the public data in the PSA.& Here, there are no advanced search capabilities, but it does provide access to all the supporting files and documentation for the various datasets.& When first searching for new data, users would benefit from using the Table View search interface [2].& Here the user can search using various parameters, such as mission name, target, instrument name, processing level, observation times, etc.& The Table View is also linked to the Image View, where users can view the browse images provided by the PI teams.& The Table View interface also has a section for & #8220 Free Search& #8221 , allowing one to use Contextual Query Language (CQL) to search over additional parameters.& Finally, there is also a Map View for viewing the footprints of data from those instruments where such calculations can be of some utility.& These various search methods rely in part on the metadata provided by the instrument teams in the labels associated with each of the data products, though the Map View also benefits from a homogenized approach to calculating geometrical parameters for all data across various missions.& & & & & & & & & & strong& Conclusion& /strong& & & & & The redelivery of the HRSC data provides an improved dataset with newer calibration factors applied.& This data can be freely accessed at the ESA& #8217 s PSA, at archives.esac.esa.int sa/.& There are multiple ways of browsing the HRSC and other instrument teams& #8217 data, including from other planetary missions, which will be explained in this poster.& The development of the PSA& #8217 s user interface is an ongoing project, and we welcome feedback from the community for suggestions on new ways to search this wealth of data.& Feedback and suggestions can be sent to psahelp@cosmos.esa.int.& & & & & & & & & & strong& Acknowledgements& /strong& & & & & The MEX Archive Scientist and the entire PSA team would like to extend their thanks to the HRSC team for their effort in updating previous deliveries and continuing to deliver new data from Mars to the public via ESA& #8217 s PSA.& Our thanks go also to the European taxpayers, whose contributions to the European Space Agency enable the gathering and dissemination of this scientific knowledge, and preserving it for future generations of scientists to work on.& & & & & & & & & & strong& References& /strong& & & & & [1] Gwinner, K. et al.: The High Resolution Stereo Camera (HRSC) of Mars Express and its approach to science analysis and mapping for Mars and its satellites, Planetary and Space Science, Vol. 126, pp. 93-138, 2016.& & & & [2] Besse, S., Vallat, C., Barthelemy, M., Coia, D., Costa, M., De Marchi, G., Fraga, D., Grotheer, E., Heather, D., Lim, T., Martinez, S., Arviset, C., Barbarisi, I., Docosal, R., Macfarlane, A., Rios, C., Saiz, J., and Vallejo, F.:& ESA& #8217 s Planetary Science Archive: Preserve and present reliable scientific data sets, Planetary and Space Science, Vol. 150, pp. 131-140, 2018.& &
Publisher: SAGE Publications
Date: 03-12-2021
DOI: 10.31124/ADVANCE.17099393.V1
Abstract: We used descriptive statistics and a logistic regression to examine between-school inequalities in science and math curricular offerings in Year 12 (final year) in all schools in one Australian state (Victoria). Dataset contains variables about school contexts: school enrolment size, school socioeconomic composition, school sector, and school location.
Publisher: Authorea, Inc.
Date: 30-09-2023
Publisher: Copernicus GmbH
Date: 23-09-2022
Abstract: & & Mars Express has the distinction of being one of the oldest operational spacecraft at Mars, with over 18 years since its injection into Martian orbit in December 2003. Designed for a nominal mission of one Martian year to survey the red planet, it is currently applying for its 9& sup& th& /sup& mission extension. A recent technical review has concluded that Mars Express was technically fit to continue providing excellent science return for the 2023-25 and 2026-28 extension intervals.& & & & & & & & & The spacecraft subsystems, scientific payload and ground segment are in overall good health, allowing continued smooth mission and science operations. The 3 lifetime-limiting elements of the spacecraft are the gyros, the batteries, and the fuel remaining onboard. The situation of the gyros has been improved by the successful implementation of a gyroless operations mode in May 2018 by the Mars Express teams at ESOC and ESAC. This difficult modification saved the mission and now allows an IMU duty cycle currently reduced to a monthly figure of about 3 to 4 % of the original usage. Mars Express can expect its gyro lifetime to be extended well beyond the 2025 timeframe.& & & & & & & & & Studies performed in 2019 and 2020 have shown the spacecraft batteries to be much less degraded than had previously been assumed. The findings of these studies were substantiated in subsequent eclipse seasons. A new battery power model now used operationally allows for more flexibility in science planning particularly during eclipse seasons. The longest, most challenging eclipses of the mission were passed successfully in 2021. With shorter eclipse durations in the coming years the outlook is very favourable for continuing to operate the batteries well beyond 2030.& & & & & & & & & The fuel situation remains satisfactory based on regularly actualised estimates and on a very low fuel consumption (assuming no safe modes the last one was in 2011). The estimated ~3kg of usable hydrazine (with high confidence based on the Venus Express experience) left onboard can take the spacecraft mission operations to beyond 2030 with the current load of science operations.& & & & Planning and execution of science operations have been improved by upgrades to the mission operations run from the MOC at ESOC and to the Science Ground Segment operations done at ESAC near Madrid. More flexible, rationalised and in some cases even reduced constraints are now in place which enhance the capability of the spacecraft and its payload in performing scientific observations and data taking.& & & & & & & & & Finally, new science opportunities are presenting themselves in the coming years, illustrated recently by the routine implementation of mutual radio occultations between Mars Express and the ExoMars Trace Gas Orbiter. This will greatly expand the number of atmospheric observations in the future. Automated dual-band radio science occultation observations have now been implemented at egress. The MARSIS subsurface radar is implementing two new promising modes of operation, one to investigate the subsurface at a better s ling rate and one to characterise Phobos, the largest Martian moon and future target for Japan& #8217 s MMX mission. Another proposed mission capability will be to perform active sounding of the local plasma environment using combined operation of the ASPERA particle detector and the MARSIS radar. MELACOM relay operations have increasingly taken place with regular Mars Surface Laboratory overflights and were also recently upgraded to implement CNSA& #8217 s Zhurong rover overflights and prepare for supporting the ExoMars rover mission as well as other NASA landed assets. These are only a limited set of ex les of how Mars Express keeps delivering new and exciting science return.& & & & & & & & & Interplanetary missions can operate over many years and learning how to use the technology in ways that were maybe not part of the original operational concept is an incredibly important ability. The above demonstrates that the Mars Express teams have been able throughout the mission& #8217 s many years of life to render Mars Express a better spacecraft now than at any time before, with in-flight upgrades that kept the mission flying. Those teams were able to make such changes thanks to: robust in-house control and support of the ESAC-run MAPPS planning software allowing for continuous improvement Flight Control Team with enough skill and resources to modify and fully test the flight code instrument teams with enough funding and support to allow for software updates/testing late in the mission. This might help younger and upcoming missions assemble the resources now so that they can attempt life-extending changes later.& & & & & & & & & Combining a special set of payload instruments onboard Mars Express, very resilient spacecraft and payload health and a favourable orbit configuration, this makes for a still unique mission at Mars, very much complementary to newer orbiting elements with different capabilities. ESA is getting the most out of Mars Express and will continue to do so in the coming years, contributing to and enhancing the international cooperation at Mars.& &
No related grants have been discovered for Alejandro Cardesín-Moinelo.