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In this thesis the linearity of the ATLAS track-counting luminosity measurement is studied using two different sets Monte Carlo simulated crossings of proton-proton bunches. A primary high-momentum, or hard, interaction must be chosen for the Monte Carlo simulation. The first of the two sets is simulated using Z→µµ as primary hard scatter in the bunch crossings while the second set is simulated with a single neutrino particle gun as the primary hard scatter. The luminosity can be determined by track counting from the relationship between the number of reconstructed charged particle tracks and the number of proton-proton interactions per bunch crossing in the ATLAS detector. The relationship between the two is theoretically linear but is affected by non-linear effects from the presence of fake tracks and the reduced tracking efficiency at large µ.  The linearity is studied and compared for eight different sets of track selection criteria called working points. Four of the working points were used during Run 2 of the Large Hadron Collider and four are introduced for Run 3.  It is found that the use of the physical hard scatter, Z→µµ, in the Monte Carlo generation results in the appearance of tracks at all interaction rates, to a degree that does not agree with experiment. The use of the single neutrino particle gun for the simulation of hard scatter interactions is found to be more suitable for the track counting studies. Two of the working points introduced for Run 3, called TightModHighPtStrictLumi and TightModFullEtaHighPtStrictLumi, are found to outperform the rest of the working points. / I denna uppsats studeras linjäriteten av en luminositet-mätningsmetod kallad track-counting som används vid ATLAS-detektorn. Linjäriteten studeras för två olika uppsättningar av simulerade proton-protonkollisioner. Kollisionerna produceras med hjälp av Monte Carlo-simuleringar. Den första uppsättningen simuleras användandes Z→µµ som mest högenergetisk interaktion i alla event medan den andra uppsättningen istället simuleras användandes en högenergetisk neutrinopartikel i alla event. Med hjälp av track-counting bestäms luminositeten genom förhållandet mellan antalet rekonstruerade laddade partikelspår och antalet proton-protoninteraktioner per "bunch crossing" i ATLAS-detektorn. I teorin är relationen mellan de två linjär, men track-counting metoden påverkas av icke-linjära effekter såsom falskt rekonstruerade partikelspår och minskad effektivitet vid stora µ-värden. Linjäriteten studeras och jämförs för åtta olika uppsättningar av kriterier som appliceras på partikelspåren. Linjäriteten jämförs for åtta olika uppsättningar av spårkriterier som kallas "Working points". Fyra Working points har tidigare använts under den andra körningen av "the Large Hadron Collider" medan fyra Working points är introducerade inför den tredje körningen.   Användningen av uppsättningen kollisioner som simuleras med Z→µµ som mest högenergetisk interaktion resulterar i spår vid alla µ-värden till en grad som inte överensstämmer med förväntningar. Användningen av neutrinopartikeln som mest högenergetsik interaktion vid simulering av event visar sig vara mer lämplig för studier som berör track-counting. Två av de Working points som introducerades inför den tredje körningen av "The Large Hadron Collider" visar sig prestera bättre än de andra. Dessa Working points har namnen TightModHighPtStrictLumi och TightModFullEtaHighPtStrictLumi.

Finding if color has an effect on depth perception in virtual reality (VR) is important, as it could be important for e.g. surgeons to perceive the depth correctly if they were to be trained in VR environments as a preparation for surgeries on real patients. If color has an effect on perceived depth in VR then producers of these simulations have to take their color choices into account when creating simulations. Previous research has shown that luminosity and hue can have effects on depth perception. It is also perceived that depth underestimation is prevalent in VR. Discerning if either the color of the focal object or the background is affecting the depth perception is important. Therefore finding what effect different color attributes of a focal object and background has on the depth perception in a VR environment is important. This experimental study examined this through a case study performed in a VR environment built in Unity. The tests were set up to emulate the piercing of a catheter into a plane, where the user pressed a button the moment the plane was pierced. To test different colors of the focal object, in this case a plane, the background was assigned neutral colors (white or black) and while testing the background the plane had a neutral color (white). Results from the study show that colors have a small effect, namely up to 13.2 mm error (for the yellow hue with high luminosity and high saturation), on users’ depth perception in VR. No single attribute was better than another but on the object, blue hue gave the largest error while red hue gave the smallest error. For the background, there was more variation on the data but green and blue hue gave the smallest errors and red and yellow the largest. In sum, color has differing effects on depth perception in VR depending on if the color is applied to a background or an object. Red color gave the most accurate depth perception when applied to the object. For color applied to the background, green hue with high luminosity and blue hue with low luminosity resulted in the most accurate depth perception. / Att ta reda på om färg har en påverkan på djupseende i virtuell verklighet (VR) är viktigt, eftersom det skulle vara viktigt för t.ex. kirurger att uppfatta djupet korrekt om de skulle bli tränade i VR miljöer som en förberedelse inför operationer på riktiga patienter. Om färg har en effekt på upplevd djup i VR, då måste tillverkarna av dessa simulationer ha deras färgval i åtanke när de skapar simulatorerna. Tidigare forskning har visat att ljusintensitet och kulörton kan ha en effekt på djupseende. Det har också upptäckts att djupunderskattning är allmänt förekommande i VR. Att urskilja om antingen färgen på fokusobjektet eller på bakgrunden påverkar djupseendet är viktigt. Således att hitta vilken effekt olika färg attribut av ett fokusobjekt och bakgrund har på djupseendet i en VR miljö. Studien undersökte detta genom en fallstudie i en VR miljö byggd i Unity. Testen var uppbyggda för att efterlikna en kateter som genomtränger ett plan där användaren trycker på en knapp då den trängde igenom planet. För att testa olika färger på fokusobjektet, i detta fall ett plan, blev bakgrunden tilldelad neutrala färger (vit och svart) och när bakgrunden testades var planet tilldelad en neutral färg (vit). Resultaten från studien visar att färg har en liten effekt, upp till 13.2 mm i fel (för den gula kulörtonen med hög ljusintensitet och hög mättnad), på djupseende i VR. Inget enskilt attribut var bättre än ett annat, men på objektet gav blå kulörton det största felet medan röd kulörton gav det minsta felet. För bakgrunden var det mer variation på data men grön och blå kulörton gav de minsta felen och röd och gul gav de största felen. Färgen har olika påverkan på djupseende i VR beroende på om färgen är applicerad på en bakgrund eller ett objekt. Röd färg gav det mest korrekta djupseendet när den var applicerad på objektet. För färg applicerad på bakgrund, resulterade grön kulörton med hög ljusintensitet och blå kulörton med låg ljusintensitet i det mest korrekta djupseendet.

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Theories of how galaxies form and evolve depend greatly on constraints provided by observations. However, when those observations come from different datasets, systematic offsets may occur. This causes difficulties measuring variations in parameters between filters. In this thesis I present the variation in total luminosity density with wavelength in the nearby Universe (z<0.1), produced from a consistent reanalysis of NIR and optical observations, taken from the MGC, UKIDSS and SDSS surveys. I derive luminosity distributions, best-fitting Schechter function parameterisations and total luminosity densities in ugrizYJHK, and compare the variation in luminosity density with cosmic star formation history (CSFH) and initial mass function (IMF) models. I examine the r band luminosity distribution produced using different aperture definitions, the joint luminosity- surface brightness (bivariate brightness) distribution in ugrizYJHK, comparing them to previously derived distributions, and how the total luminosity density varies with wavelength when surface brightness incompleteness is accounted for. I find the following results. (1) The total luminosity density calculated using a non-Sersic (e.g. Kron or Petrosian) aperture is underestimated by at least 15%, (2) Changing the detection threshold has a minor effect on the best-fitting Schecter parameters, but the choice of Kron or Petrosian apertures causes an offset between datasets, regardless of the filter used to define the source list, (3) The decision to use circular or elliptical apertures causes an offset in M* of 0.20 mag, and best-fitting Schechter parameters from total magnitude photometric systems have a flatter faint-end slope than Kron or Petrosian photometry, (4) There is no surface brightness distribution evolution with luminosity for luminous galaxies, but at fainter magnitudes the distribution broadens and the peak surface brightness dims. A Choloniewski function that is modified to account for this surface brightness evolution fits the bivariate-brightness distribution better than an unmodified Choloniewski function, (5) The energy density per unit interval, vf(v) derived using MGC and GAMA samples agrees within 90% confidence intervals, but does not agree with predictions using standard CSFH and IMF models. Possible improvements to the data and alterations to the theory are suggested.

Le thème des analyses présentées dans ce document est la mesure des propriétés du boson de Higgs se désintégrant dans le mode H→ZZ→4l dans l'expérience ATLAS au CERN. Le document commence par un résumé détaillé concernant la procédure d'étalonnage des électrons: l'algorithme de combinaison trace-cluster améliore la résolution en énergie (surtout pour les électrons ayant une faible énergie transverse) en exploitant les informations du cluster et de la trace dans un ajustement par maximum de vraisemblance. L'amélioration en résolution est approximativement de 18-20% pour les désintégrations du J/Ψ en di-électrons, et 3% pour Z→ee. Par la suite, la combinaison E-p est appliquée au canal H→ZZ→4l avec électrons dans l'état final permettant d’obtenir un gain modéré sur la distribution de la masse invariante (4-5%). En deuxième lieu, la masse du boson de Higgs et sa largeur sont estimées, en particulier afin de comprendre les effets apportés par l'utilisation de l'algorithme de combinaison trace-cluster. La masse a été calculée en se servant d'un ajustement à deux dimensions appliqué sur la masse invariante m4l et un score de discrimination du signal contre le bruit de fond ZZ*. Cette discrimination est obtenue en exploitant les corrélations angulaires dont les distributions sont sensibles au spin et à la parité du boson de Higgs. L’étude sur la largeur du boson est ensuite détaillée : les résultats sont basés sur une approche qui vise à contraindre cette largeur en analysant la région de haute masse m4l où le boson de Higgs se comporte comme un propagateur. La section efficace au pic de la résonance (« on-shell ») dépend de la largeur totale du boson de Higgs, ce qui n’est pas le cas pour la production dans la région de haute masse (« off-shell »). Par conséquent, des limites indirectes sur la largeur peuvent être déterminées en combinant les régions « on-shell » et « off-shell ». Une limite à 6.7 fois la largeur Higgs ΓSMH est obtenue via le canal 4l. En combinant la mesure « on-shell » avec tous les canaux de désintégration étudiés (notamment ZZ→4l, ZZ→2l2ν and WW→lνlν), les résultats aboutissent à une limite observée (attendue) sur la largeur totale de 22.7 (33.0) MeV. La dernière partie de ce travail de thèse est consacrée à l'analyse sur la largeur du boson de Higgs en quatre leptons à haute (High-Luminosity LHC) luminosité intégrée (respectivement 300 fb⁻¹ et 3000 fb⁻¹) : il s’agit d’une étude extrapolant à √s =14 TeV les techniques utilisées pour l’analyse à 8 TeV (Run 1). / The theme of the analyses presented in this Thesis is the measurement of the Higgs boson properties in the H→ZZ→4l decay channel with the ATLAS experiment at the LHC. A detailed overview on the electron calibration process is first presented. In this regard, the track-cluster combination algorithm is found to improve the energy resolution of low ET electrons by exploiting both track and cluster information into a maximum likelihood fit. The improvement in resolution is approximately 18-20% for J/Ψ dielectron decays, and of the order of 3% for Z→ee events. In addition, the E-p combination algorithm has also been applied to the H→ZZ→4l channel with electrons in the final state resulting in a non-negligible gain on the invariant mass distribution (4-5%). Secondly, the Higgs mass and its total width are evaluated in the H→ZZ→4l channel. The Higgs mass is measured in the 4l decay channel with particular interest on the beneficial effects brought by the improved electron calibration and the track-cluster combination. The mass on the full 2011 and 2012 datasets is worked out with a 2-dimensional fit on the invariant mass of the 4 lepton final state, m4l, and on a boosted decision tree (BDT)-based output conceived against the main ZZ irreducible background and constructed on variables that are sensitive to the Higgs boson spin-parity state. Regarding the Higgs width, results are based on a relatively recent approach aimed at indirectly constraining the Higgs boson width by exploiting the m4l high-mass region where the Higgs boson acts as a propagator. The Higgs production cross section in the on-shell m4l region, where the Higgs boson is a resonance, depends on the total Higgs width, whereas this is not the case for the high mass m4l (off-shell). Limits on the Higgs width can be therefore set when merging the off-shell results with the on-shell ones. A limit of ∼ 6.7 times ΓSMH is obtained in the four lepton channel. Secondly, by combining with the on-shell measurement and using all the decay channels in the analysis, i.e. ZZ→4l, ZZ→2l2ν and WW→lνlν, the results lead to an observed (expected) 95% C.L. upper limit on the Higgs boson total width of 22.7 (33.0) MeV (4.2 MeV is the Standard Model predicted Higgs width at mH=125 GeV).The last section of the thesis is devoted to the evaluation of the Higgs width at √s=14 TeV in the high luminosity scenario (High Luminosity LHC), 300 fb⁻¹ and 3000 fb⁻¹, by employing the same techniques exploited in the previous Run 1 analysis at √s=8 TeV.

This thesis is focused on the theoretical and practical introduction to the verification procedures used today for obtaining luminosity curves of lamps. The introduction acquaints readers with the photometric variables. Consequently, it is theoretically described procedure for constructing luminance curves by zonal flow and further familiarization with the near-field photometry. For the practical part was chosen several lights. These lamps were measured by luxmeter first from a very close photometric distance from lights, and then from large distance. The next step was to obtain pictures of luminaries in planes C 0 to 345 ° (with a step of 15 °) of the angle gamma from 0 to 180 ° (in steps of 5 °). The measured data were processed by zonal flow and through programs LumiDISP and Matlab. The partial result of this thesis is to verify whether it is possible to use the luminance analyzer for obtaining luminosity curves, it means, if the luminosity curve obtained through luminance analyzer will comply with the curves obtained through a luxmeter. Further work should ascertain the feasibility of acquired photographs lamps from a very close photometric distance could create luminosity curve for any location and distance from the observer to measured lamps.

Gamma-ray burst light curves are notoriously irregular, yet a significant number consists of a single fast-rising, exponentially decaying pulse. These are called single-peaked light curves. The goal of this thesis is to analyse a sample of 2710 GRBs collected by the Fermi space telescope by identifying single-peaked bursts and comparing their properties to those of the multi-peaked bursts. Furthermore, the validity of the relativistic shock breakout theory as an explanation for single-peaked, low-luminosity GRBs is investigated using a closure relation. For this investigation, the Fermi sample wascomplemented by low-luminosity GRBs observed by other instruments. A criterion for selecting single-peaked bursts was successfully developed, yielding 48% long and 79% short, single-peaked GRBs. Significant differences between the populations were found in multiple properties. In general, single-peaked GRBs appear to be weaker and more slowly varying than multi-peaked ones; however, a larger sample of GRBs with redshift measurements is needed to draw conclusions about possible intrinsic differences in energy connected to the progenitor systems. The investigation of low-luminosity GRBs’ compliance with the shock breakout closure relation showed that 64% of the low-luminosity GRBs were within a factor 5 of fulfilling the relation as opposed to only 24% of high-luminosity GRBs. It was further shown that only a small number (&lt; 5%) of Fermi GRBs without redshift measurements could be low-luminosity shock breakout GRBs according to this theory. In conclusion, while the shock breakout closure relation does hold for a greater proportion of low-luminosity GRBs than high-luminosity GRBs, there is still a large number of low-luminosity GRBs left unexplained by this theory. / Gammablixtljuskurvor är ökänt oregelbundna men en betydande andel består av en enda snabbt stigande och exponentiellt avtagande puls. Dessa kallas singelpeakade ljuskurvor. Målet med detta examensarbete är att analysera de 2710 gammablixtar som Fermirymdteleskopet har observerat genom att identifiera singelpeakade blixtar och jämföra deras egenskaper med multipeakade blixtars. Dessutom undersöks den relativistiska shockbreakoutteorin som förklaringsmodell för singelpeakade lågluminositetsgammablixtar. I denna undersökning kompletterades fermiblixtarna med lågluminositetsblixtar från andra instrument. Ett kriterium för identifikation av singelpeakade gammablixtar utvecklades och detta resulterade i 48% långa och 70% korta, singelpeakade gammablixtar. Flertalet egenskaper uppvisade signifikanta skillnader mellan populationerna. I allmänhet verkar singelpeakade gammablixtar vara svagare och variera långsammare än multipeakade. Dock behövs en större population av gammablixtar med uppmätta rödskift för att med säkerhet kunna avgöra om singelpeakade blixtar verkligen släpper ut mindre energi. Undersökningen av huruvida lågluminositetsgammablixtar kan förklaras med shockbreakoutteorin visade att 64% av lågluminositetsblixtarna uppfyllde kravet upp till en faktor fem medan bara 24% av högluminositetsblixtarna gjorde det. Vidare visades att endast ett litet antal (&lt;5%) av fermiblixtarna utan uppmätta rödskift skulle kunna vara lågluminositetsshockbreakoutblixtar enligt denna teori. Även om shockbreakoutteorin kan förklara en större andel av lågluminositetsblixtarna än högluminositetsblixtarna återstår ett stort antal oförklarade lågluminositetsblixtar.

No description available.

With energy outputs &gt;~10^51 erg in 0.1-1000 seconds, Gamma-ray Bursts (GRBs) are the most powerful events yet observed in the Universe. As such they are potential probes of the very early Universe, back to the era of re-ionisation and the first stars, but at the same time they have been observed to span a wide range in luminosity and redshift from the relatively local Universe (z~0.0085) out to z~6.29. GRBs divide into two classes based primarily on their duration as measured by T90 (the time taken to observe 90% of the total burst fluence). Long bursts (L-GRBs) have T90&gt;~2 seconds, and shorts (S-GRBs) T90&lt;~2 seconds. Though much has been learned regarding long duration GRBs since the first afterglow discovery in 1997 (including their likely association with massive core collapse supernovae), much remains unknown regarding short duration GRBs. In this work, after a brief historical introduction and review, we present analyses of the angular cross-correlation on the sky of short GRBs from the BATSE catalogue with galaxies in the local Universe sampled from the PSCz Redshift Survey and the Third Reference Catalogue of Bright Galaxies (RC3). In particular we show that 20%+/-8% (1 sigma) of all BATSE short duration bursts (localised to 10 degrees or better) show correlation with galaxy samples (morphological T-type&lt;=4) within ~112 Mpc. Our statistics thus provide evidence that a substantial fraction of BATSE short GRBs show a tendency to be associated with large scale structure on the sky traced by a variety of galaxy types. Short GRBs are believed to be produced in the final merger of compact object (neutron star-neutron star or neutron star-black hole) binaries, though other possible progenitors are known to exist. The short initial spike of a giant flare from a Soft Gamma Repeater (SGR) such as the December 27th 2004 event from SGR1806-20 would have been detectable by BATSE as a short GRB if it occurred in a galaxy within ~30-50 Mpc (assuming a distance to SGR1806-20 of 15 kpc). Using the observed luminosities and rates of Galactic SGR giant flares, as well as theoretical predictions for the rate of binary mergers, we investigate the ability of plausible Luminosity Functions (LF), singly and in combination, to reproduce our observed correlations and a cosmological S-GRB population. We find the correlations are best explained by a separate population of lower luminosity S-GRBs, with properties consistent with them being due to giant flares from extra-galactic SGRs. Overall predicted number counts are a good fit to the observed BATSE number counts, and furthermore, the wider redshift distribution is consistent with the early Swift S-GRB redshift distribution. The three closest GRBs which have been observed to date were all long duration bursts, and we have therefore also searched for cross-correlation signals between the BATSE long GRBs and local galaxies. The three nearby bursts shared several similar properties such as being under-luminous, spectrally soft and of low variability. We have therefore also investigated a subset of L-GRBs with light curve properties similar to these known nearby bursts. The whole sample is found to exhibit a correlation level consistent with zero (1 sigma upper limit=10%, equivalent to 144 bursts) out to a radius of ~155 Mpc, but a spectrally soft, low observed fluence and low variability subset shows a correlation level of 28%+/-16% (=50+/-28 bursts) within 155 Mpc. These results are consistent with low-luminosity, low-variability bursts being a separate sub-class of L-GRBs which may be much more prevalent in the local Universe than their high-luminosity, cosmologically distant counterparts. To investigate this further, we once again examined plausible luminosity functions for single and dual high and low luminosity populations, based on observed intrinsic rates from the literature. The local population was once again found only to be produced to a sufficient level (while maintaining consistency with the observed overall number counts) by a separate low luminosity population with intrinsic rates several hundred times greater than their cosmological counterparts. Constraining the models via the Swift overall redshift distribution instead of threshold-adjusted BATSE number counts showed that the dual LF models were able to produce excellent fits to the entire redshift distribution while adequately reproducing a local population. Finally, suggestions are made as to the direction future work may follow in order to build on these initial investigations, as well as to how observations with future missions and detectors such as Fermi (formerly GLAST), Advanced LIGO and LOFAR may shed further light on nearby GRBs.