Jordi Ibáñez

Geociencias Barcelona

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Cătălin Popescu

ALBA Synchrotron (Spain)

L. Artús

Consejo Superior de Investigaciones Científicas

R. Cuscó

Consejo Superior de Investigaciones Científicas

Daniel Errandonea

Universitat de València

Alfonso Muñoz

Laboratoire Leprince-Ringuet

P. Rodríguez‐Hernández

Universidad de La Laguna

Robin Turnbull

Universitat de València

Akun Liang

University of Edinburgh

Robert Oliva

Geociencias Barcelona

Javier González‐Platas

Universidad de La Laguna

Cooperative Institutions

Universitat de Barcelona

Consejo Superior de Investigaciones Científicas

Geociencias Barcelona

Centre National de la Recherche Scientifique

Universitat Autònoma de Barcelona

Universitat de València

Universidad Complutense de Madrid

Universitat Politècnica de Catalunya

University of Nottingham

Institut de Nanociència i Nanotecnologia de la Universitat de Barcelona

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CSD 2162840: Experimental Crystal Structure Determination

The Cambridge Structural Database (2022)

Robin Turnbull Javier González‐Platas Akun Liang Dequan Jiang Yonggang Wang

An entry from the Inorganic Crystal Structure Database, the world’s repository for inorganic crystal structures. The entry contains experimental data from a crystal diffraction study. The deposited dataset for this entry is freely available from the joint CCDC and FIZ Karlsruhe Access Structures service and typically includes 3D coordinates, cell parameters, space group, experimental conditions and quality measures.

10.25505/fiz.icsd.cc2blm1m

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Landscape evolution of the Bolivian Amazon controlled by uplift events dated 13,000, 10,000 and 6000 cal yr BP

Quaternary Science Reviews (2025)

Umberto Lombardo Lorena Becerra‐Valdivia Geanina Butiseaca Christopher Bronk Ramsey Jordi Ibáñez

10.1016/j.quascirev.2025.109197

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LO phonon–plasmon coupled modes and carrier mobilities in heavily Se-doped Ga(As, N) thin films

Journal of Materials Science Materials in Electronics (2008)

Jordi Ibáñez Esther Alarcón‐Lladó R. Cuscó L. Artús Daivid Fowler

10.1007/s10854-008-9661-x

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High-Pressure High-Temperature Stability and Thermal Equation of State of Zircon-Type Erbium Vanadate

Inorganic Chemistry (2018)

Javier Ruiz‐Fuertes D. Martínez‐García Tomás Marqueño Daniel Errandonea Simon G. MacLeod

The zircon to scheelite phase boundary of ErVO4 has been studied by high-pressure and high-temperature powder and single-crystal X-ray diffraction. This study has allowed us to delimit the best synthesis conditions of its scheelite-type phase, determine the ambient-temperature equation of state of the zircon and scheelite-type structures, and obtain the thermal equation of state of the zircon-type polymorph. The results obtained with powder samples indicate that zircon-type ErVO4 transforms to scheelite at 8.2 GPa and 293 K and at 7.5 GPa and 693 K. The analyses yield bulk moduli K0 of 158(13) GPa for the zircon phase and 158(17) GPa for the scheelite phase, with a temperature derivative of dK0/dT = −[3.8(2)] × 10–3 GPa K–1 and a volumetric thermal expansion of α0 = [0.9(2)] × 10–5 K–1 for the zircon phase according to the Berman model. The results are compared with those of other zircon-type vanadates, raising the need for careful experiments with highly crystalline scheelite to obtain reliable bulk moduli of this phase. Finally, we have performed single-crystal diffraction experiments from 110 to 395 K, and the obtained volumetric thermal expansion (α0) for zircon-type ErVO4 in the 300–395 K range is [1.4(2)] × 10–5 K–1, in good agreement with previous data and with our experimental value given from the thermal equation of state fit within the limits of uncertainty.

Scheelite

Phase boundary

Atmospheric temperature range

10.1021/acs.inorgchem.8b01808

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Moon in-situ resources: clues from the study of Lunar achondrites in preparation for Artemis sample return missions

J. M. Trigo‐Rodríguez Esther Mas-Sanz Jordi Ibáñez Jacinto Alonso‐Azcárate

. Introduction.The Moon is no longer a goal in itself but a necessary step for the conquest of space. In this work we focus in the composition of Lunar meteorites as the only objects alongside Apollo, and Luna collected samples, that the scientific community has available to first-hand analyze the Moon. Future Artemis sample return missions will provide new samples to continue learning from our satellite. Given its proximity to our planet, our satellite is an ideal planetary body to use it as a space camp for new technology, to establish a space base, and to test space mining. The continuous depletion of Earth resources put special importance on the exploration of extraterrestrial natural resources potential and the feasibility of its exploitation. After many robotic and manned missions, the utilization of lunar resources has been studied for a long time. In-Situ Resources Utilization (ISRU) refers to the generation of materials (for construction, life support, or as propellants) from the available resources on a celestial body that otherwise, would have needed to be brought from Earth [1].2. Analitical Techniques and SamplesFor the present work, four different Lunar achondrites (Lunaites) were studied: Dhofar 1084, Jiddat al Harasis 838, Northwest Africa 2700 and 11444, and Miller Range 090031 (abbreviated in Table 1). Thin sections of each meteorite allow us a characterization of the mineralogy using SEM/EDX and optical microscopy (Fig. 1). In addition, XRD measurements on capillary powder samples of the meteorites are made using a powder diffractomer equipped with a Mo X-ray souce (λ=0.709 Å). This experimental configuration allows us to minimize preferential orientation effects as well as to significantly reduce the X-ray fluorescence signal from Fe, relative to XRD measurements performed with a standard Cu X-ray tube. Finally we perform ICP-MS and ICP-AES of the samples using a similar procedure that in our previous studies of meteorites [2]. Meteorite specimens studied so far are listed in Table 1.Table 1. Lunar meteorites under study, type, probable origin and Total Known Mass (TKM).3. DiscussionLike the Lunar rocks, Lunaites provide valuable information about the chemical and mineralogical complexity that can be found in the surface of the Moon. Despite that we don’t know exactly their origin in the Lunar surface, these relatively small rocks provide clues on the processes going on in the surface of the Moon. Among the most fascinating meteorites, JaH 838 is a mingled regolith breccia presenting mare and KREEPy clasts, together with the products of thermal processing: High-Al Si-Poor (HASP) glasses with chondritic metal grains. Another one is the complex melt breccia NWA 11444 containing a wide variety of angular fragments (gabbros and basalts) and variable amounts of flow-banded glass. Crystal fragments consist predominantly of plagioclase, pyroxene, and olivine. Finally the rock also contains a few percent of Fe,Ni metal grains probably reminiscence of the projectiles sculpting the rock (see Fig. 1).Fig. 1. A kamacite grain set into an anorthite-rich matrix of NWA 11444. 4. Conclusions.From our study and having into account our current knowledge of the chemical and mineralogical lunar resources which can be realistically used for ISRU, the following resources are considered [3,4]:Metals hosted in the lunar regolith are mostly due to the continuous impact of chondritic and metallic projectiles with the Lunar surface. As a consequence, the regolith is enriched in minerals such as pyroxene, olivine, ilmenite and native metals such as Fe and Ni. In addition, it can be found hydrated minerals and rare-Earth elements. As most metals are found in the form of oxides (as well as some pure kamacite), it makes their extraction costly energy-wise as these components tend to be chemically stable [3], but their potential use for producing spacecraft parts and in-situ repairs make them more attractive. On the other hand, the extraction of oxygen is especially interesting from a biological point of view: future missions may utilize it for the production of water and other life support processes. Water, probably to be found as ice inside permanently shadowed craters of the polar regions, could be used as rocket fuel and to support life in a Moon base. On the other hand, some regions of the Moon have been hit by carbonaceous chondritic asteroids, rich in clay minerals. These hydrous minerals contain absorbed and bound water. If heated at temperatures ∼100-150 ºC absorbed water can be released and bound water at ∼300 ºC [4]. Carbon and other organic compounds are also common in regolith-rich regions of the Moon. There is a dominant flux of CM chondrites [5] that after impact dehydrate and end up as “graphitized” clasts observed in regolith breccias [6]. Furthermore, it has been theorized of an uncertain amount of hydrocarbons could be used for the production of much complex polymers, resins and plastics [1]. Finally, solar wind volatiles become also implanted in the Lunar regolith: H, N, C and in particular the He-3 isotope, rare to find on Earth and key for future developments in nuclear fusion. ConclusionsLunar meteorites are valuable samples teaching us about the processes going on over the Moon, at the same time that provide clues on the most important minerals for mining. Many different initiatives on how to tackle Lunar resources are taking place: from 3-D printers that previously construct the necessary infrastructure for lunar mining, the utilization of autonomous robots and obviously, the mingle of different proposals according to the exploitation stage. The Lunar surface provides a lot of valuable materials, but a precise know-how is required to successfully exploit them. Then, a careful study of Lunar samples and meteorites will provide significant progress in optimizing ISRU.AcknowledgementsThe authors acknowledge financial support from the Spanish Ministry (PGC2018-097374-B-I00).References

Habitability

Achondrite

10.5194/epsc2020-714

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Strain relaxation in stacked InAs/GaAs quantum dots studied by Raman scattering

Applied Physics Letters (2003)

Jordi Ibáñez A. Patanè M. Henini L. Eaves S. Hernández

We report a Raman scattering investigation of InAs vibrational modes in multiple layers of InAs self-assembled quantum dots in a GaAs matrix. The Raman peak associated with quantum-dot phonons shows a downward frequency shift as the interlayer spacing decreases. We attribute this frequency shift to the relaxation of the elastic strain in the stacked quantum-dot layers. From the phonon frequency shift, we estimate the magnitude of the strain in the quantum dot layers, which we relate to the energy of the photoluminescence emission of the dots.

Strain (injury)

10.1063/1.1618368

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Size‐Controlled Si Nanocrystals Fabricated by Electron Beam Evaporation

physica status solidi (a) (2019)

O. Blázquez Lluís López‐Conesa J. López-Vidrier Juan Luis Frieiro Sònia Estradé

Multilayers consisting of silicon nanocrystals (Si NCs) and SiO 2 are successfully fabricated by electron beam evaporation, using pure Si and SiO 2 targets in an oxygen‐rich atmosphere for alternately depositing silicon‐rich oxide (SRO) layers and SiO 2 barriers, respectively. A post‐deposition annealing process is carried out at different temperatures in order to achieve the Si precipitation in the form of nanocrystals. The stoichiometry of the layers is determined by X‐ray photoelectron spectroscopy, which confirms the controlled silicon oxidation in order to attain SRO layers. Transmission electron microscopy and Raman‐scattering measurements confirm the presence of crystalline Si‐nanoprecipitates. Photoluminescence spectra from the Si NC samples can be deconvolved into two contributions, whose dynamics suggest that two different luminescent centers are responsible for the optical emission of the samples.

Silicon oxide

Stoichiometry

10.1002/pssa.201800619

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Raman scattering study of undoped and As-doped GaN grown with different III/V ratios

Semiconductor Science and Technology (2007)

Jordi Ibáñez David Pastor Esther Alarcón‐Lladó R. Cuscó L. Artús

We have used Raman scattering to investigate a series of undoped and As-doped GaN epilayers grown on sapphire substrates by plasma-assisted molecular beam epitaxy with different Ga-to-N ratios. We find that the frequency of the E2h phonon mode of GaN is very sensitive to the Ga-to-N ratio used to grow both types of samples, which may be attributed to strain effects arising from the different growth conditions. We observe Raman signatures corresponding to the formation of submicron cubic domains in some of the spectra of the As-doped samples. We discuss the origin of a broad band located at 232 cm−1 that appears in both the undoped and the As-doped epilayers. We speculate that this band, reported in previous Raman studies on As-doped and Bi-doped GaN, may be attributed to the formation of Ga clusters.

10.1088/0268-1242/22/10/011

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Analysis of reflectance spectra of volcanic rocks from Deception Island (Antarctica)

EGUGA (2019)

Agustín Lobo Anna Giralt Jordi Ibáñez Adelina Geyer

Source

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Micro‐photoluminescence of GaInNAs layers grown on GaAs substrates of various crystallographic orientations

Physica status solidi. C, Conferences and critical reviews/Physica status solidi. C, Current topics in solid state physics (2011)

Magdalena Latkowska R. Kudrawiec G. Sęk J. Misiewicz Jordi Ibáñez

Abstract Low temperature micro‐photoluminescence (μ‐PL) has been applied to study GaInNAs bulklike layers grown on GaAs substrates with various crystallographic orientations [(100), (111)A, (311)A, (411)A, and (511)A]. At low excitation conditions, the μ‐PL spectra show sharp PL lines of ∼100‐300 μeV widths. The density of these lines changes from sample to sample as well as from place to place within one sample. When the excitation power is increased, an additional smooth PL band appears at the higher‐energy side. This band is located ∼30‐100 meV above the band of sharp PL lines and is attributed to free exciton/carrier recombination. The sharp PL lines are attributed to the recombination of localized excitons trapped at local potential minima. These lines are not resolved in macro‐PL spectra because of their high density. (© 2011 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)

Photoluminescence excitation

10.1002/pssc.201000834

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