Analysis of the damage effect of femtosecond-laser irradiation on extreme ultraviolet Mo/Si multilayer coating

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Geo-structural map of the Laguna Blanca basin (Southern Central Andes, Catamarca, Argentina)

The Laguna Blanca basin is a rhomb-shaped basin located at the SE margin of the Puna plateau in the southern Central Andes (Catamarca, Argentina). An interactive analysis using remote sensing and field mapping enabled us to produce a geo-structural map at a 1:350,000 scale. Satellite images from multispectral sensors (ASTER and Landsat 7 ETM+) and medium resolution Digital Elevation Models (SRTM and ASTER GDEM) were used in order to recognize the structures and main lithologies, which were validated in the field and through laboratory tests (e.g. spectral analysis). The final result is a geo-structural map of the Laguna Blanca basin with a new geological unit subdivision, highlighting its tectonic origin, which appears to be related to a releasing stepover along N-S sinistral strike-slip master faults

Analysis of the damage effect of femtosecond-laser irradiation on extreme ultraviolet Mo/Si multilayer coating

Damage analysis of Mo/Si multilayer coatings exposed to fs infrared laser irradiation has been performed. The Mo/Si a-periodic multilayer samples were specifically designed with wide reflectivity bandwidth and suitable phase chirp in order to reflect attosecond pulses. After irradiation, the mirror surfacewas analyzed by using an optical microscope and a profilometer. The stoichiometry of the compounds formed at the sample surface after the irradiation was investigated using X-Ray photoemission spectroscopy. The performances of the irradiated sampleswith the reflected pulse characteristics have been derived via reflectivity and phase measurements

Developing an EUV multilayer adaptive mirror: the first results

The growing interest in the study of the extreme ultraviolet (EUV) radiation-matter interaction is feeding up the development of new technologies able to overcame some current technological limits. Adaptive optics is an established technology already widely used for wavefront correction in many applications such as astronomical telescopes, laser communications, high power laser systems, microscopy and high resolution imaging systems. Although this technology is already exploited in the EUV and X-ray range, its usage is only feasible in systems with a grazing incidence configuration. On the other hand, the development of a EUV normal incidence adaptive optics can open new interesting possibilities in many different fields ranging from free electron laser and synchrotron applications up to EUV photolithography. In this work we report the preliminary results achieved in the developing of a normal incidence EUV multilayered adaptive mirror tuned at 30.4nm. The proper functioning and potential applications of such device have been demonstrated by using a High order Harmonics Generation (HHG) source

The EUV reflectance of Mercury’s surface measured by BepiColombo/PHEBUS

International audienceOn October 9th and 10th 2021, Probing the Hermean Exosphere by UV Spectroscopy (PHEBUS) aboard BepiColombo observed the disk-integrated reflected light from the Sun by Mercury in the spectral range 90 – 160 nm at a phase angle of 70°. These observations are used to derive the EUV reflectance of the surface of Mercury in this wavelength range for the first time since the Mariner 10 observations in 1974 -1975. Our observations are in agreement with a surface of Mercury darker by a factor ∼ 0.5 – 0.6 compared to the Moon in this wavelength range, with an average reflectance of 0.3% at a phase angle of 70°. This lower reflectance of Mercury could be due to the lower abundance of FeO.The derived reflectance near 160 nm is close to the derived reflectance at 220 nm by MESSENGER/MASCS at a similar phase angle. Possible spectral variations measured between 110 and 140 nm could be attributed to SiO2 glass, but the signal to noise ratio is low and other observations, possible at several periods during the rest of the cruise, are needed to confirm this last result

Metis: The Solar Orbiter visible light and ultraviolet coronal imager

Aims. Metis is the first solar coronagraph designed for a space mission and is capable of performing simultaneous imaging of the off-limb solar corona in both visible and UV light. The observations obtained with Metis aboard the Solar Orbiter ESA-NASA observatory will enable us to diagnose, with unprecedented temporal coverage and spatial resolution, the structures and dynamics of the full corona in a square field of view (FoV) of ±2.9° in width, with an inner circular FoV at 1.6°, thus spanning the solar atmosphere from 1.7 R to about 9 R, owing to the eccentricity of the spacecraft orbit. Due to the uniqueness of the Solar Orbiter mission profile, Metis will be able to observe the solar corona from a close (0.28 AU, at the closest perihelion) vantage point, achieving increasing out-of-ecliptic views with the increase of the orbit inclination over time. Moreover, observations near perihelion, during the phase of lower rotational velocity of the solar surface relative to the spacecraft, allow longer-term studies of the off-limb coronal features, thus finally disentangling their intrinsic evolution from effects due to solar rotation. Methods. Thanks to a novel occultation design and a combination of a UV interference coating of the mirrors and a spectral bandpass filter, Metis images the solar corona simultaneously in the visible light band, between 580 and 640 nm, and in the UV H※ I Lyman-α line at 121.6 nm. The visible light channel also includes a broadband polarimeter able to observe the linearly polarised component of the K corona. The coronal images in both the UV H※ I Lyman-α and polarised visible light are obtained at high spatial resolution with a spatial scale down to about 2000 km and 15 000 km at perihelion, in the cases of the visible and UV light, respectively. A temporal resolution down to 1 s can be achieved when observing coronal fluctuations in visible light. Results. The Metis measurements, obtained from different latitudes, will allow for complete characterisation of the main physical parameters and dynamics of the electron and neutral hydrogen/proton plasma components of the corona in the region where the solar wind undergoes the acceleration process and where the onset and initial propagation of coronal mass ejections (CMEs) take place. The near-Sun multi-wavelength coronal imaging performed with Metis, combined with the unique opportunities offered by the Solar Orbiter mission, can effectively address crucial issues of solar physics such as: the origin and heating/acceleration of the fast and slow solar wind streams; the origin, acceleration, and transport of the solar energetic particles; and the transient ejection of coronal mass and its evolution in the inner heliosphere, thus significantly improving our understanding of the region connecting the Sun to the heliosphere and of the processes generating and driving the solar wind and coronal mass ejections. Conclusions. This paper presents the scientific objectives and requirements, the overall optical design of the Metis instrument, the thermo-mechanical design, and the processing and power unit; reports on the results of the campaigns dedicated to integration, alignment, and tests, and to the characterisation of the instrument performance; describes the operation concept, data handling, and software tools; and, finally, the diagnostic techniques to be applied to the data, as well as a brief description of the expected scientific products. The performance of the instrument measured during calibrations ensures that the scientific objectives of Metis can be pursued with success. © 2020 ESO