We report photometric measurements of selected exoplanet transits from the archive of the TOPTEC telescope, operated by our team at an observatory Horní Halže, near Klášterec nad Ohří, Czech Republic. We have compared measured geometry with catalogue geometry of selected exoplanetary systems. We have found a candidate for potential system with new non-transiting planet with the help of an archive TRESCA.
This paper informs about a construction of an all-spherical Cassegrain telescope with a two lens Volosov corrector. The entrance doublet of the Volosov corrector radically corrects the residual optical aberrations of the system and makes possible the attainment of high quality of images across the field of view of up to 2˚ within the whole visual spectral branch. One optical set of the system was manufactured in the IPP AV CR v.v.i – TOPTEC Center in Turnov in 2005. Its entrance diameter was 280 mm and focal length approximately 2450 mm.
Lead zirconate titanate (PZT) is widely used for its ferroelectric and piezoelectric properties, which are conditioned by perovskite structure. Crystallization into this desired phase is determined also by a proper stoichiometry, where the lead concentration is a crucial parameter. The crystallization process takes place during annealing under high temperatures, which is linked to heavy lead losses, so the lead has to be in excess. Therefore, this paper is devoted to the control of chemical composition of PZT thin films deposited via ion beam sputtering (IBS). A commonly used approach for IBS relies on employing a multicomponent target to obtain films with the same composition as that of the target. However, in the case of PZT it is favorable to have the ability to controllably change the chemical composition of thin films in order to acquire high perovskite content. Our study revealed that the determinative lead content in PZT layers prepared by simple and dual ion-beam deposition from a multicomponent target can be easily controlled by the power of primary ion source. At the same time, the composition is also dependent on the substrate temperature and the power of assistant ion source. Thin PZT films with more than 30 % lead excess were acquired from a stoichiometric multicomponent target (i.e. a target without any lead excess). We can therefore propose several possible sets of deposition parameters suitable for the PZT deposition via IBS to obtain high perovskite content.
Lead zirconate titanate (Pb[ZrxTi1-x]O3 ) is well-known for his excellent ferroelectric, piezoelectric and electromechanical properties. These properties are closely related to the perovskite crystal structure of PZT. A common way to achieve thin film of perovskite PZT is to anneal the layer after deposition. The high annealing temperature (600 – 700°C) limits a set of usable substrates. To grow a thin layer of perovskite PZT at reduced temperature it is necessary to add crystallization energy to the system by another way. In this article are presented some results of using ion beam sputtering system (IBS) with ion beam assistance (IBAD) to growth perovskite PZT layer at reduced temperature. This process is very complicated and the resulting layer properties are strongly influenced by deposition parameters (ions energy, chemical composition of the atmosphere in the sputtering chamber etc.). We achieved partial success when pyrochlore crystal structure of PZT was grown at reduced substrate temperature (110°C) (at this temperatures are the PZT layers usually amorphous)
We report on the development and implementation of the digital holographic tomography for the three-dimensio- nal (3D) observations of the domain patterns in the ferroelectric single crystals. Ferroelectric materials represent a group of materials, whose macroscopic dielectric, electromechanical, and elastic properties are greatly in uenced by the presence of domain patterns. Understanding the role of domain patterns on the aforementioned properties require the experimental techniques, which allow the precise 3D measurements of the spatial distribution of ferroelectric domains in the single crystal. Unfortunately, such techniques are rather limited at this time. The most frequently used piezoelectric atomic force microscopy allows 2D observations on the ferroelectric sample surface. Optical methods based on the birefringence measurements provide parameters of the domain patterns averaged over the sample volume. In this paper, we analyze the possibility that the spatial distribution of the ferroelectric domains can be obtained by means of the measurement of the wavefront deformation of the transmitted optical wave. We demonstrate that the spatial distribution of the ferroelectric domains can be determined by means of the measurement of the spatial distribution of the refractive index. Finally, it is demonstrated that the measurements of wavefront deformations generated in ferroelectric polydomain systems with small variations of the refractive index provide data, which can be further processed by means of the conventional tomographic methods.
We report on the discovery of new four variable stars in the Cassiopea constellation from the archive of the HALZ telescope, operated by the TOPTEC team at Horní Halže, near Klášterec nad Ohří, Czech Republic. The stars are catalogued as UCAC4 718-108144 (23h 04m 16.383s +53° 29’ 44.78”), UCAC4 725-101725 (23h 09m 27.87s +54° 51’ 23.27”), UCAC4 725-101699 (23h 09m 19.53s +54° 57’ 57.18”), UCAC4 722-105015 (23h 10m 42.4s +54° 14’ 33.33”). From the light curve, the stars should be a HADS – type variable (UCAC4 718-108144), an EW – type variable (UCAC4 725-101725), an EA - type variable (UCAC4 725-101699) and an ELL – type variable (UCAC4 722-105015). We registered these stars in the CzeV catalogue as new variable stars CzeV709, CzeV710, CzeV711 and CzeV715.
We report on the discovery of a new variable star during the search for new exoplanets in the Centaurus constellation from the archive of the FRAM telescope, operated by the FRAM team at Los Leones, near Malargüe, Argentina. The star is catalogued as GSC 08630-01117 (11h 36m 10s -53° 12’ 15.04”). From the light curve, the star should be an ELL-type variable. We computed the period P = 0.6311+/- 0.0002 days. The maximum is 13.07 +/- 0.02 mag and minimum is 13.22 +/-0.02 mag (in the Johnson V filter) with an amplitude of about 0.15 mag. We registered this star in the CzeV catalogue and in the VSX catalogue as new variable star CzeV603. The FRAM telescope observed several transits of known exoplanets. These observations show the ability to detect new exoplanets using the FRAM telescope.
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