The nature of aerosols in hot exoplanet atmospheres is one of the primary vexing questions facing the exoplanet field. The complex chemistry, multiple formation pathways, and lack of easily identifiable spectral features associated with aerosols make it especially challenging to constrain their key properties. We propose a transmission spectroscopy technique to identify the primary aerosol formation mechanism for the most highly irradiated hot Jupiters (HIHJs). The technique is based on the expectation that the two key types of aerosols-photochemically generated hazes and equilibrium condensate clouds-are expected to form and persist in different regions of a highly irradiated planet's atmosphere. Haze can only be produced on the permanent daysides of tidally locked hot Jupiters, and will be carried downwind by atmospheric dynamics to the evening terminator (seen as the trailing limb during transit). Clouds can only form in cooler regions on the nightside and morning terminator of HIHJs (seen as the leading limb during transit). Because opposite limbs are expected to be impacted by different types of aerosols, ingress and egress spectra, which primarily probe opposing sides of the planet, will reveal the dominant aerosol formation mechanism. We show that the benchmark HIHJ, WASP-121b, has a transmission spectrum consistent with partial aerosol coverage and that ingress-egress spectroscopy would constrain the location and formation mechanism of those aerosols. In general, using this diagnostic we find that observations with the James Webb Space Telescope and potentially with the Hubble Space Telescope should be able to distinguish between clouds and haze for currently known HIHJs.

In this work we present a grid of LTE and non-LTE synthetic spectra of hot DA white dwarfs (WDs). In addition to its usefulness for the determination of fundamental stellar parameters of isolated WDs and in binaries, this grid will be of interest for the construction of theoretical libraries for stellar studies from integrated light. The spectral grid covers both a wide temperature and gravity range, with 17,000 K <= T-eff <= 100,000 K and 7.0 <= log g <= 9.5. The stellar models are built for pure hydrogen and the spectra cover a wavelength range from 900 angstrom to 2.5 mu m. Additionally, we derive synthetic HST/ACS, HST/WFC3, Bessel UBVRI, and SDSS magnitudes. The grid was also used to model integrated spectral energy distributions of simple stellar populations and our modeling suggests that DAs might be detectable in ultraviolet bands for populations older than similar to 8 Gyr.

We present evidence that the recently discovered, directly imaged planet HD 131399 Ab is a background star with nonzero proper motion. From new JHK1L' photometry and spectroscopy obtained with the Gemini Planet Imager, VLT/SPHERE, and Keck/NIRC2, and a reanalysis of the discovery data obtained with VLT/SPHERE, we derive colors, spectra, and astrometry for HD 131399 Ab. The broader wavelength coverage and higher data quality allow us to reinvestigate its status. Its near-infrared spectral energy distribution excludes spectral types later than L0 and is consistent with a K or M dwarf, which are the most likely candidates for a background object in this direction at the apparent magnitude observed. If it were a physically associated object, the projected velocity of HD 131399 Ab would exceed escape velocity given the mass and distance to HD 131399 A. We show that HD 131399 Ab is also not following the expected track for a stationary background star at infinite distance. Solving for the proper motion and parallax required to explain the relative motion of HD 131399 Ab, we find a proper motion of 12.3 mas yr(-1). When compared to predicted background objects drawn from a galactic model, we find this proper motion to be high but consistent with the top 4% fastest-moving background stars. From our analysis, we conclude that HD 131399 Ab is a background K or M dwarf.

No description available.

The purpose of this study was to determine the protonation sites in guanosine-5'-monophosphate (5'-GMP), and to correlate the ease of protonation with the chemical nature and composition of substituent groups. The laser Raman spectra of 5'-GMP, 7-methyl-guanosine-5'-monophosphate (m7-GMP), and 8-bromoguanosine-5'-monophosphate (8-Br-GMP) at various pH and pD values were recorded with a Spex Ramalog-6 spectrometer. Based on the spectral changes observed in these studies, the preferred order of protonation sites for 5'-GMP and 8-Br-GMP is N7, 06 and N3. In the case of m7-GMP, the preferred sites are 06 and N3. The opening of the imidazole ring in m7-GMP is observed at pH value of about 9.4. It appears that the presence of the methyl group has a stabilizing effect on the protonated (keto) species. As expected, the vibrational modes of the phosphate group are unaffected by substituents on the guanine part of 5'-GMP. The complete spectra and vibrational assignments for 5'-GMP, m7- GMP and 8-Br-GMP are presented in this thesis.

<div>Thin films with selective spectral properties have great potential for use in applications such as solar thermal absorbers, selective thermal emitters, thermal barrier coatings, and thermophotovoltaics. Understanding the dependence of their optical properties with temperature is crucial for practical applications. Relatively less-used films with high thermal stability, high refractive index, and infrared transparency, such as cerium oxide CeO2 and magnesium oxide (MgO) have not been studied extensively for high-temperature applications. In this paper, CeO2, MgO, and several multilayer samples containing these compounds will be studied their change of optical properties with increasing temperature across the visible and infrared spectrum. In this work, I introduce Spectroscopic Ellipsometry (SE) to analyze dielectric constants of films and measure its thickness at multiple incident angles in visible and near-Infrared (IR) wavelengths both at room temperature and elevated temperatures. Using ellipsometry, several single and multilayer thin films (CeO2 and other transparent materials-based) have been measured their dielectric constants and thickness at room temperature and high temperature up to 500°C using thermal control stages called INSTEC. The change of their optical properties with temperatures has been characterized using theoretical modelling. Fitting their optical properties have been observed by changing thickness of each layer and calculating the corresponding Cauchy parameters in transparent material. Finally, FTIR measurements will be used to further characterize direct emission of these films at higher temperatures. This will be performed at room temperature and high temperature up to 1400 °C.</div>

This thesis examines the preparation of thin layers of material for photovoltaic applications with focused on perovskites and determining their optical properties. Basic information about the photovoltaic panels, especially about the perovskites, and the preparation of thin layers is supplied in the theoretical section. This section includes description of optical properties and the main method of study of optical properties, spectroscopic ellipsometry. Experimental section is focused on the preparation of thin layers of perovskites FAPbBr3 and its precursors by spin-coating. Optical properties are evaluated using profilometry, UV VIS spectrometry and spectroscopic ellipsometry. The conclusion summarizes the results of this experiment with focused on comparison of ellipsometric spectrums of perovskites and its precursors.

The aim of this diploma thesis is to study to the influence of compost addition to soil humic substances extracted from blackland luvicsol. Humic substances extracted from soil and from compost were characterized by titration with potentiometrical and conductival indication, UV-VIS, FT-IR and 3D EEM fluorescential spectroscopy. Compost in amount of 124, 239 and 478 t/ha was applicated and manured into dept of 150 mm at blackland luvicsol. The main aim of thesis was the appraisal of compost influence into fluorescent attributes of soil HS and localization of fluorescent peaks at excitation emission spectrums. Next part of diploma thesis was focused on the study of spectroscopic attributes of soil HS and compost by UV-VIS and infrared spectroscopy with Fourier transformation. Humic substances were characterized by humifical index E4/E6 and transmissional vibratile spectrums. The last aim of diploma thesis were the characterization of soil HS extracts and compost by acidimetral titration. For each sample was calculated value of H+ ionts amount of substance from measured titrational curves.

The work deals with a technique of imaging spectroscopic reflectometry developed at The Institute of Physical Engineering, Brno University of Technology. The technique is well suited for characterization of samples non–uniform along their surfaces. The technique is primarily used for optical characterization of thin films. First part of the work is focused on basic physical principles of the technique and on ways in which measurement data are obtained. It contains a basic description of evaluating methods and a basic concept of an imaging spectroscopic reflectometer with a description of main parts of such a device. The main part of the work is focused on a description of two devices which were built at The Institute of Physical Engineering together with a description of some of upgrades which were implemented to these devices during their development. A description of measurements done with the two devices is also included. Last part of the work is then focused on further development of the technique. Intention of possible evolution of the technique to imaging spectroscopic ellipsometry is proposed.

This diploma thesis is devoted to systematic study of structural trans- formations of Heusler alloys by means of spectroscopic ellipsometry and magneto-optical spectroscopy. Structural transformations in these alloys are induced by different microscopic mechanisms. Obtained experimental results were confronted with theoretical calculations. This allowed the discussion of obtained results and suggestion of their interpretation. In the case of Co- Fe-Si alloys, changes in optical and magneto-optical properties with change of Co-Fe ratio were observer. This was explained by lowering of the gap for minority spins with increasing Fe concentrations. Temperature dependent optical and magneto-optical properties of Ni-Mn-Ga alloy showed the pres- ence of so-called Martensitic transformation from cubic to tetragonal phase. A study of Mn-Rh-Co-Sn alloys did not show a clear dependence of physical properties upon the concentration of Rh and Mn. This was explained by strong strain inside the samples, which distorted obtained results. 1