Low-Energy Family House in Krásné Pole

Import 29/09/2010Cílem bakalářské práce je zhotovení stavební dokumentace novostavby nízkoenergetického rodinného domu. Bakalářská práce je vypracována v rozsahu potřebném pro dokumentaci pro provedení stavby. Řešení je zaměřeno na splnění požadavků pro nízkoenergetické domy a to především umístění stavby na pozemku, orientace ke světovým stranám a dispoziční řešení atd. Součástí projektu je tepelně technické posouzení domu, spolehlivostní posouzení hlavního nosného prvku stropu. Výsledkem bakalářské práce je prováděcí projekt, který se skládá z 80% Architektonicko -stavební části a z 20% specializace Pozemní Stavitelství.The aim of thesis is to design building documentation of new low-energy family house. The documentation was elaborated within the range that is needful for building construction. The solution is focused on fulfilling demands for low-energy houses e.g. location on grounds, building orientation regarding point of the compas, disposition. This work involves a heat technical examination of house, reability examination of main beam of ceiling. Content of this thesis is construction project, which is composed by 80% od architektural – construction part and 20 % of structual engineering specialization.Prezenční226 - Katedra architekturyvelmi dobř

Hydraulic losses in plastic pipeline

Práce se zabývá rešerší problematiky výpočtu třecích ztrát při proudění čisté vody v přímém potrubí z termoplastu a jejich následném porovnání s hodnotami ztrát udávaných vybranými výrobci.This work deals with the research of methods of friction loss calculations for a clean water flow in straight thermoplastic piping and their subsequential comparison with losses listed by chosen manufacturers

The dynamics of the ionized and molecular ISM in powerful obscured quasars at z>=3.5

We present an analysis of the kinematics and excitation of the warm ionized gas in two obscured, powerful quasars at z>=3.5 from the SWIRE survey, SWIRE J022513.90-043419.9 and SWIRE J022550.67-042142, based on imaging spectroscopy on the VLT. Line ratios in both targets are consistent with luminous narrow-line regions of AGN. SWIRE J022550.67-042142 has very broad (FWHM=2000 km/s), spatially compact [OIII] line emission. SWIRE J022513.90-043419.9 is spatially resolved, has complex line profiles of H-beta and [OIII], including broad wings with blueshifts of up to -1500 km/s relative to the narrow [OIII]5007 component, and widths of up to FWHM=5000 km/s. Estimating the systemic redshift from the narrow H-beta line, as is standard for AGN host galaxies, implies that a significant fraction of the molecular gas is blueshifted by up to ~ -1000 km/s relative to the systemic velocity. Thus the molecular gas could be participating in the outflow. Significant fractions of the ionized and molecular gas reach velocities greater than the escape velocity. We compare empirical and modeling constraints for different energy injection mechanisms, such as merging, star formation, and momentum-driven AGN winds. We argue that the radio source is the most likely culprit, in spite of the sources rather modest radio power of 10^25 W/Hz. Such a radio power is not uncommon for intense starburst galaxies at z~2. We discuss these results in light of the co-evolution of AGN and their host galaxy.Comment: Accepted by MNRA

Creating a 3D Face Model Using Kinect Device

Cílem této bakalářské práce je navrhnout způsob pro zvýšení rozlišení 3D modelů obličeje pořízených senzorem Kinect a toto řešení implementovat. V práci jsou popsány metody snímání 3D modelů,senzor Kinect a jeho vlastnosti v porovnání s kvalitními 3D skenery. Hlavní částí práce je popis statistického modelu založeného na PCA analýze a jeho využití při návrhu aplikace. V závěru je provedeno testování s různými vstupy a zhodnocení dosažených výsledků implementovaného programu.The main aim of this bachelor's thesis is to suggest a method for increasing the resolution of 3D face models captured by Kinect. The document describes different methods of capturing 3D models and compares the Kinect sensor with more acurate scanners. The main part of this document is dedicated to statistic model based on the PCA and its usage in the project. The last section of the paper describes testing of various models and discuss the results and another options of aplication.

Observations of Feedback from Radio-Quiet Quasars: I. Extents and Morphologies of Ionized Gas Nebulae

Black hole feedback -- the strong interaction between the energy output of supermassive black holes and their surrounding environments -- is routinely invoked to explain the absence of overly luminous galaxies, the black hole vs. bulge correlations and the similarity of black hole accretion and star formation histories. Yet direct probes of this process in action are scarce and limited to small samples of active nuclei. We present Gemini IFU observations of the distribution of ionized gas around luminous, obscured, radio-quiet (RQ) quasars at z~0.5. We detect extended ionized gas nebulae via [O III]5007 emission in every case, with a mean diameter of 28 kpc. These nebulae are nearly perfectly round. The regular morphologies of nebulae around RQ quasars are in striking contrast with lumpy or elongated nebulae seen around radio galaxies at low and high redshifts. We present the uniformly measured size-luminosity relationship of [O III] nebulae around Seyfert 2 galaxies and type 2 quasars spanning 6 orders of magnitude in luminosity and confirm the flat slope of the correlation (R ~ L^{0.25+/-0.02}). We find a universal behavior of the [O III]/H-beta ratio in our entire RQ quasar sample: it persists at a constant value (~10) in the central regions, until reaching a "break" isophotal radius ranging from 4 to 11 kpc where it starts to decrease. We propose a model of clumpy nebulae in which clouds that produce line emission transition from being ionization-bounded at small distances from the quasar to being matter-bounded in the outer parts of the nebula, which qualitatively explains the observed line ratio and surface brightness profiles. It is striking that we see such smooth and round large-scale gas nebulosities in this sample, which are inconsistent with illuminated merger debris and which we suggest may be the signature of accretion energy from the nucleus reaching gas at large scales.Comment: 44 pages, 11 figures, 3 tables. Accepted for publication in MNRA

Observations of Feedback from Radio-Quiet Quasars - II. Kinematics of Ionized Gas Nebulae

The prevalence and energetics of quasar feedback is a major unresolved problem in galaxy formation theory. In this paper, we present Gemini Integral Field Unit observations of ionized gas around eleven luminous, obscured, radio-quiet quasars at z~0.5 out to ~15 kpc from the quasar; specifically, we measure the kinematics and morphology of [O III]5007 emission. The round morphologies of the nebulae and the large line-of-sight velocity widths (with velocities containing 80% of the emission as high as 1000 km/s combined with relatively small velocity difference across them (from 90 to 520 km/s) point toward wide-angle quasi-spherical outflows. We use the observed velocity widths to estimate a median outflow velocity of 760 km/s, similar to or above the escape velocities from the host galaxies. The line-of-sight velocity dispersion declines slightly toward outer parts of the nebulae (by 3% per kpc on average). The majority of nebulae show blueshifted excesses in their line profiles across most of their extents, signifying gas outflows. For the median outflow velocity, we find a kinetic energy flow between 4x10^{44} and 3x10^{45} erg/s and mass outflow rate between 2000 and 20000 Msun/yr. These values are large enough for the observed quasar winds to have a significant impact on their host galaxies. The median rate of converting bolometric luminosity to kinetic energy of ionized gas clouds is ~2%. We report four new candidates for "super-bubbles" -- outflows that may have broken out of the denser regions of the host galaxy.Comment: 23 pages, 10 figures, 2 tables, accepted for publication in MNRA

Business Start-up for Bike&Shoulder Bag – Bishbag

Tato bakalářská práce se zaměřuje na podnikatelský záměr pro začínající společnost nabízející koženou brašnou přes rameno, která je lehce přizpůsobitelná na přední řídítka na kole. Práce je rozdělena na teoretickou a praktickou část. Práce zahrnuje teoretické poznatky z oblasti podnikání, potřebné k vypracování podnikatelského záměru. Praktická část se zaměřuje na vypracování podnikatelského start-upu pro výrobek Bishbag. Obsahuje návrh start-upu a ukazuje na možnosti realizace, marketing jako celek, distribuce, propagace, SWOT analýzu a podrobnější analýzu tohoto plánu.This bachelor thesis is focused on Business plan for a start-up company which is offering leather shoulder bag, which is easily applied to bicycle handlebar. This thesis is divided into theoretical and practical part. Bachelor thesis includes theoretical knowledge about the business, which you need to develop a business plan. The practical part focuses on developing business start-up for a product named Bishbag. It includes a proposal for start-up and pointing to the possibility of realization, marketing as a whole, distribution, promotion, SWOT analysis and more detailed analysis of this plan.

CO line emission in the halo of a radio galaxy at z=2.6

We report the detection of luminous CO(3-2) line emission in the halo of the z=2.6 radio galaxy (HzRG) TXS0828+193, which has no detected counterpart at optical to mid-infrared wavelengths implying a stellar mass < few x10^9 M_sun and relatively low star-formation rates. With the IRAM PdBI we find two CO emission line components at the same position at ~80 kpc distance from the HzRG along the axis of the radio jet, with different blueshifts of few 100 km s^-1 relative to the HzRG and a total luminosity of ~2x10^10 K km s^-1 pc^2 detected at 8 sigma significance. HzRGs have significant galaxy overdensities and extended halos of metal-enriched gas often with embedded clouds or filaments of denser material, and likely trace very massive dark-matter halos. The CO emission may be associated with a gas-rich, low-mass satellite galaxy with little on-going star formation, in contrast to all previous CO detections of galaxies at similar redshifts. Alternatively, the CO may be related to a gas cloud or filament and perhaps jet-induced gas cooling in the outer halo, somewhat in analogy with extended CO emission found in low-redshift galaxy clusters.Comment: MNRAS Letters, accepte