SNe Ia können als Standardkerzen verwendet werden, um den Zustandsparameter der dunklen Energie w zu messen. Nachdem viele SN Ia beobachtet wurden, wird die Genauigkeit aktueller Studien durch systematische Fehler beschränkt, wobei die Flusskalibrierung (in Wellenlänge) die dominierende Fehlerquelle ist. In dieser Arbeit wird eine Möglichkeit präsentiert, das Problem mit dem “SNIFS Calibration Apparatus” (SCALA) zu lösen oder wenigstens zu verringern. Das Ziel von SCALA ist es, dass System aus Teleskop und SNIFS mit hoher Genauigkeit zu kalibrieren und diese Kalibration auf das Standardstern-Netzwerk zu übertragen und somit die Modellabhängigkeit zu unterdrücken. SCALA erzeugt 18 nahezu parallele und kolimierte monochromatische Strahlen (mit einstellbarer Wellenlänge), die Öffnungswinkel von einem Grad haben. Die Kombination dieser Strahlen leuchtet die Bildebene des UH 88, Teleskops (Universität Hawaii 88 inch Teleskop) mit einer Genauigkeit von 1% gleichmäß ig aus. SCALA wurde im Jahr 2014 installiert und ist seit 2015 im regulären Betrieb. Im in-situ Betrieb wird einer der Strahlen ständig mit einer Photodiode überwacht, die mit einer NIST-kalibrierten Photodiode kalibriert wurde. Eine zweite so kalibrierte Photodiode wird von Strahl zu Strahl bewegt, um den Helligkeitsverlauf der anderen 17 Strahlen als Funktion der Wellenlänge zu messen. Auf diese Weise sind wir in der Lage die Ausleuchtung von SCALA mit einer Genauigkeit von besser als 1% zu vermessen. Auf diese Weise kann mit der bekannten Wellenlänge des verwendeten Lichts die Transmissionskurve des SNIFS+UH 88 Systems gemessen werden. Die gemessenen systematischen Ungenauigkeiten der Messung sind kleiner als 0.7%. Der nächste Schritt besteht darin, die mit SCALA erreichte Kalibration mit einer herkömmlichen, auf Basis des Standard Stern Netzwerkes, zu vergleichen. / SNe Ia can be used as standard candles to measure the dark energy equation of state parameter, w. Having observed a good number of these objects, current studies are limited by systematic uncertainties, among which relative (color) flux calibration is dominating. This work presents a way to solve, or at least limit, the problem with the SNIFS Calibration Apparatus (SCALA). SCALA's goal is to provide high precision calibration for the “telescope+ SNIFS” system and refine the primary standard star network, to eliminate the uncertainties due to the knowledge of their models. SCALA produces 18 quasi-parallel and collimated monochromatic (and wavelength tunable) beams with opening angles of 1 degree. The combination of these beams allows us to achieve an illumination of the focal plane of the University of Hawaii 88 inches telescope (UH 88), that is flat to within 1%. SCALA was commissioned in 2014 and fully deployed in 2015. In the in-situ set up, one of the SCALA beams is constantly monitored by a photodiode (calibrated against a NIST-calibrated photodiode), which is used as flux standard to transfer the NIST-calibration to the telescope+instrument first, and the standard star spectra afterwards. We measure the overall wavelength trend of the illumination from SCALA with a precision better than 1%, by moving another of these calibrated photodiodes from beam to beam. We can hence measure relative trasmissivity curves for each SCALA beam. Therefore, we can produce throughput curves of the SNIFS+UH 88 system. The measured systematics affecting our results sum to errors smaller than 0.7%. The next step would be to compare the calibration of the system achieved with SCALA with the traditional calibration obtained by observing standard stars.

In astronomy, the Sun has an important role. It keeps the solar-system together and is thesource for life, heat, light and energy to Earth. As any other star or planet, the Sun has amagnetic field. The magnetic field of the Sun has a great impact on the Sun itself as well asits surrounding. The magnetic field shapes solar wind, causes flares and drives coronal massejections radiating towards the Earth (and other planets). The Sun's magnetic field is still notfully understood, and therefore it is useful to study other stars with properties similar to theSun. So by studying young solar-type stars, the evolution of the Sun can be more easilyunderstood. The aim of this project is to study the surface magnetic field in a youngsolar-type star, π1 UMa to see how the magnetic field is distributed and if there are anypatterns like polarity reversals. Magnetic field generates polarisation and with Stokes vector Iand V, polarisation can be described. Earlier measurements from two time-epochs (2014 and2015) of Stokes I and V have been obtained from the spectropolarimeter NARVAL. To getthe desired mean polarisation profiles of the star, a technique called least squaredeconvolution was applied which increases the signal-to-noise level. To reconstruct themagnetic topology the Zeeman-Doppler imaging technique was used. Then we obtained thesurface magnetic field maps of both measurements. No change of the polarity of magneticfield at the visible stellar pole was found. Most of the magnetic field energy was contained inthe spherical harmonic modes with angular degrees l=1-3. The star shows dominance in thetoroidal component so the study seem to agree with the previously established trend thatyounger and faster rotating stars have predominantly toroidal magnetic fields and older starswith slower rotation rate, like the Sun, have predominantly poloidal field. Looking at themagnetic field plots, the star show dominance in the azimuthal field component, and themean magnetic field strength is similar to one found in the previous study. The results of thesurface magnetic field in our study thus agrees with previous study of the same star. With thiswe can conclude that the Sun's magnetic field probably been different when it was younger, and possibly similar to the star analyzed in this study.

Nurses are expected to perform evidence-based practice (EBP) at the point of care (POC) to promote positive outcomes through the quality and safety of patient care. The struggle for nurses on the surgical digestive unit in a hospital to adopt EBP is the lack of access and knowledge to evidence-based research at the POC. The utilization of information technology is an innovated approach to providing access and knowledge for EBP at the POC to improve patient outcomes. The project was to develop a quality improvement program to improve nursing access and knowledge of EBP resources. The program was to identify the type of e-nursing resources and necessary education to provide nurses access to evidence-based resources and the knowledge to utilize these resources in nursing practice. The purpose of the doctoral project was set to identify necessary resources to develop an evidence-based program for staff nurses to access evidence-based resources and improve nursing knowledge on EBP at the POC. The use of the Stevens's star model of knowledge transformation was the framework for the project, and use of the logic model guided the structure for program evaluation. The quantitative project used a 1 group pre- and post-survey design using a convenience sample (n =10). A final statistical analysis to determine effectiveness of the educational intervention was inconclusive. Quantitative descriptive data from pre- and post-survey results were used to summarize recommendations for the future development of an EBP quality improvement project with the use of information technology tools. The further dissemination of the findings could promote new methods to implement quality improvement programs to improve the quality and safety of patient care to promote positive health outcomes.

Energy benchmarking and disclosure policies exist in several local and state governments to manage the energy consumption of existing buildings and encourage energy efficient retrofits and upgrades, yet little is known about whether these efforts have improved overall energy efficiency. The purpose of this repeated-measures study was to examine the influence of New York City's (NYC's) Benchmarking Law (LL84) on the energy performance of the city's existing commercial buildings through investigating whether the energy performance of the city's existing commercial buildings significantly improved after the implementation of this policy. The study was based on Ostrom's institutional analysis and development framework. Paired-sample t tests were performed to statistically analyze the annually disclosed energy benchmarking data for 1,072 of NYC's existing commercial buildings that were benchmarked in both 2011 and 2016. Compared to 2011, the study results revealed statistically significant improvements in the energy performance of NYC's commercial buildings by 2016. On average, their site energy use intensity (EUI) significantly reduced by 5%, source EUI significantly decreased by 10%, greenhouse gas emissions significantly dropped by 12%, and ENERGY STAR performance rating significantly improved by 5%. However, these improvements were primarily achieved in 2012, 1 year after the city's energy benchmarking data were publicly disclosed. Additional measures should be considered to maintain continuous energy savings and greenhouse gas mitigation patterns. Positive social change implications include the potential to promote energy-efficient upgrades and inspire the adoption of sustainable building concepts.

abstract: This dissertation details the development of an open source, frequency domain multiplexed (FDM) readout for large-format arrays of superconducting lumped-element kinetic inductance detectors (LEKIDs). The system architecture is designed to meet the requirements of current and next generation balloon-borne and ground-based submillimeter (sub-mm), far-infrared (FIR) and millimeter-wave (mm-wave) astronomical cameras, whose science goals will soon drive the pixel counts of sub-mm detector arrays from the kilopixel to the megapixel regime. The in-flight performance of the readout system was verified during the summer, 2018 flight of ASI's OLIMPO balloon-borne telescope, from Svalbard, Norway. This was the first flight for both LEKID detectors and their associated readout electronics. In winter 2019/2020, the system will fly on NASA's long-duration Balloon Borne Large Aperture Submillimeter Telescope (BLAST-TNG), a sub-mm polarimeter which will map the polarized thermal emission from cosmic dust at 250, 350 and 500 microns (spatial resolution of 30", 41" and 59"). It is also a core system in several upcoming ground based mm-wave instruments which will soon observe at the 50 m Large Millimeter Telescope (e.g., TolTEC, SuperSpec, MUSCAT), at Sierra Negra, Mexico. The design and verification of the FPGA firmware, software and electronics which make up the system are described in detail. Primary system requirements are derived from the science objectives of BLAST-TNG, and discussed in the context of relevant size, weight, power and cost (SWaP-C) considerations for balloon platforms. The system was used to characterize the instrumental performance of the BLAST-TNG receiver and detector arrays in the lead-up to the 2019/2020 flight attempt from McMurdo Station, Antarctica. The results of this characterization are interpreted by applying a parametric software model of a LEKID detector to the measured data in order to estimate important system parameters, including the optical efficiency, optical passbands and sensitivity. The role that magnetic fields (B-fields) play in shaping structures on various scales in the interstellar medium is one of the central areas of research which is carried out by sub-mm/FIR observatories. The Davis-Chandrasekhar-Fermi Method (DCFM) is applied to a BLASTPol 2012 map (smoothed to 5') of the inner ~1.25 deg2 of the Carina Nebula Complex (CNC, NGC 3372) in order to estimate the strength of the B-field in the plane-of-the-sky (B-pos). The resulting map contains estimates of B-pos along several thousand sightlines through the CNC. This data analysis pipeline will be used to process maps of the CNC and other science targets which will be produced during the upcoming BLAST-TNG flight. A target selection survey of five nearby external galaxies which will be mapped during the flight is also presented. / Dissertation/Thesis / Doctoral Dissertation Astrophysics 2019

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(Field trip activities in Prague focusing on the Star game reserve and their application and use in the teaching of nature science) The subject of this diploma thesis are organizational forms of teaching with a focus on excursion activities in science classes at the 2nd level of primary school and in the corresponding years of lower grammar school. The work is clearly divided into several parts. The first part deals with general information about the excursion activity as a whole. It deals with the division of individual excursions, their preparation and course. Subsequently, the possibilities of educational programs in Prague and the surrounding area are characterized, which are prepared from various institutions. Furthermore, the work specifically focuses on the Prague forest in the field of the Star game reserve, because in the last part of the text is made an educational walk connecting the history and nature of this place. An integral part of the work is a questionnaire survey dealing with the use of excursions in science teaching.

京都大学 / 0048 / 新制・課程博士 / 博士(理学) / 甲第20915号 / 理博第4367号 / 新制||理||1627(附属図書館) / 京都大学大学院理学研究科物理学・宇宙物理学専攻 / (主査)准教授 菅沼 秀夫, 教授 田中 貴浩, 教授 川合 光 / 学位規則第4条第1項該当 / Doctor of Science / Kyoto University / DFAM

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