SDSS-HET Survey of Kepler Eclipsing Binaries. Description of the Survey and First Results

The Kepler mission has provided a treasure trove of eclipsing binaries (EBs), observed at extremely high photometric precision, nearly continuously for several years. We are carrying out a survey of ~100 of these EBs to derive dynamical masses and radii with precisions of 3% or better. We use multiplexed near-infrared H-band spectroscopy from the Sloan Digital Sky Survey-III and -IV APOGEE instrument and optical spectroscopy from the Hobby–Eberly Telescope High-resolution Spectrograph to derive double-lined spectroscopic orbits and dynamical mass ratios (q) for the EB sample, two of which we showcase in this paper. This orbital information is combined with Kepler photometry to derive orbital inclination, dynamical masses of the system components, radii, and temperatures. These measurements are directly applicable for benchmarking stellar models that are integrating the next generation of improvements, such as the magnetic suppression of convection efficiency, updated opacity tables, and fine-tuned equations of state. We selected our EB sample to include systems with low-mass (M ≾ 0.8 M⊙) primary or secondary components, as well as many EBs expected to populate the relatively sparse parameter space below ~0.5 M⊙. In this paper, we describe our EB sample and the analytical techniques we are utilizing, and also present masses and radii for two systems that inhabit particularly underpopulated regions of mass–radius–period space: KIC 2445134 and KIC 3003991. Our joint spectroscopic and photometric analysis of KIC 2445134 (q = 0.411 ± 0.001) yields masses and radii of M_A = 1.29 ± 0.03 M⊙, M_B = 0.53 ± 0.01 M⊙, R_A = 1.42 ± 0.01 R⊙, R_B = 0.510 ± 0.004 R⊙, and a temperature ratio of T_B/T_A = 0.635 ± 0.001; our analysis of KIC 3003991 (q = 0.298 ± 0.006) yields M_A = 0.74 ± 0.04 M⊙, M_B = 0.222 ± 0.007 M⊙, R_A = 0.84 ± 0.01 R⊙, R_B = 0.250 ± 0.004 R⊙, and a temperature ratio of T_B/T_A = 0.662 ± 0.001

Heavy neutrinos on the ZZ pole

Osnovna zamisel tega dela je bila obravnavati fiziko, ki sega preko Standardnega Modela (SM) in s pomočjo računalniških simulacij ugotoviti, ali je s sedanjimi eksperimenti mogoče potrditi takšne modele. V ta namen najprej obravnavam standardni Model in interakcije v njegovem bozonskem sektorju, ki v nadaljevanju igrajo ključno vlogo pri možnosti detekcije novih delcev. Nadaljujem z vpeljavo obsežnejšega modela. Naravna pot razširitve standardnega modela je vključitev v model, ki se ponaša z večjo simetrijo. Tu se osredotočam na levo - desno simetrični model (LRSM), ki enakovredno obravnava levo in desno ročne kiralnosti. Ob vpeljavi osnovnih lastnosti tega modela predstavim tudi interakcije, nove delce ter gugalnični mehanizem tipa I, ki razloži določene nejasnosti. Magistrsko nalogo zaključim s poglavjem o računalniških simulacijah, v katerem so predstavljeni rezultati simulacij, preko katerih ugotovimo kateri procesi trenutno ostajajo v dosegu današnjih eksperimentov v fiziki visokih energij.The basic idea of this thesis was to discuss physics beyond Standard Model (SM) and to find out whether such models could be confirmed with the currently available experimental equipment via computer simulations. Firstly, I focus on Standard Model and interactions in its boson sector, which take crucial part in potentially possible detection of new particles. Secondly, I introduce a more comprehensive model. A natural way of extending the Standard Model is to integrate it into a more symmetric framework. Here, I focus on Left-Right Symmetric Model (LRSM), which treats left- and right-handed chiralities equally. After defining basic properties of the model, I revisit its interactions and new particles. Furthermore, I consider a Type I see saw mechanism, which explains some obscurities. Finally, I conclude the thesis with the chapter about computer simulations, where we find out which of the discussed processes are within reach of the potential detection by the current high energy physics experiments

Iskanje procesov gugalničnega mehanizma tipa II s pari enako nabitih leptonov v končnih stanjih z detektorjem ATLAS

A search for pair production of doubly charged Higgs bosons ((H^{pm pm})), each decaying into a pair of prompt, isolated, and highly energetic leptons with the same electric charge, is presented. The search uses a proton-proton collision data sample at a centre-of-mass energy of 13 TeV corresponding to an integrated luminosity of 139 fb(^{-1}) recorded by the ATLAS detector during Run 2 of the Large Hadron Collider (LHC). This analysis focuses on same-charge leptonic decays, (H^{pm pm} rightarrow ell^{pm} ell^{prime pm}), where (ell, ell^{prime} = e, mu, tau), in two-, three- and four-lepton channels but only considers final states, which include electrons or muons. No evidence of a signal is observed. Assuming that the branching ratios to each possible leptonic final state are equal, (mathcal{B}(H^{pm pm} rightarrow e^{pm} e^{pm} / e^{pm} mu^{pm} / mu^{pm} mu^{pm} / e^{pm} tau^{pm} / mu^{pm} tau^{pm} / tau^{pm} tau^{pm}) = 1/6), the corresponding upper limits on the pair production cross-section of doubly charged Higgs bosons are derived as a function of its mass, (m_{H^{pm pm}}), at a 95% confidence level. The limits, which are the strongest produced by the ATLAS Collaboration to date, are obtained for the left-right symmetric type-II seesaw model. Additionally, this work provides the first direct test of the Zee-Babu neutrino mass model at the LHC.V doktorskem delu je predstavljeno iskanje nastanka para dvojno nabitih Higgsovih bozonov ((H^{pm pm})), izmed katerih vsak razpade na par neposrednih, izoliranih in visokoenergijskih leptonov z enakim električnim nabojem. V analizi so uporabljeni podatki, zabeleženi z detektorjem ATLAS med drugim obratovalnim ciklom (Run 2) velikega hadronskega trkalnika (LHC), kar ustreza integrirani luminoznosti 139 fb(^{-1}). Zajeti so bili med trki protonov pri težiščni energiji 13 TeV. Analiza se osredotoča na razpade delca ((H^{pm pm})) v par leptonov z enakim nabojem, (H^{pm pm} rightarrow ell^{pm} ell^{prime pm}), pri čemer je (ell, ell^{prime} = e, mu, tau). Posebej so obravnavana končna stanja z dvema, tremi in štirimi leptoni, vendar so upoštevana le ta, ki vključujejo elektrone ali mione. Statistična obdelava podatkov ne kaže znatnih odstopanj od napovedi Standardnega modela. Ob predpostavki, da so razvejitvena razmerja v vsa možna leptonska končna stanja enaka, (mathcal{B}(H^{pm pm} rightarrow e^{pm} e^{pm} / e^{pm} mu^{pm} / mu^{pm} mu^{pm} / e^{pm} tau^{pm} / mu^{pm} tau^{pm} / tau^{pm} tau^{pm}) = 1/6), so izpeljane ustrezne zgornje meje produkcijskih sipalnih presekov dvojno nabitih Higgsovih bozonov kot funkcija njihove mase (m_{H^{pm pm}}), pri stopnji zaupanja 95 %. Meje, ki so najstrožje, kar jih je doslej objavila kolaboracija ATLAS, so določene za gugalnični mehanizem tipa II znotraj levo-desno simetričnega modela. Poleg tega je to delo prvi neposredni preizkus modela Zee-Babu na LHC

The SDSS-HET Survey of Kepler Eclipsing Binaries. Description of the Survey and First Results

The Kepler mission has provided a treasure trove of eclipsing binaries (EBs), observed at extremely high photometric precision, nearly continuously for several years. We are carrying out a survey of similar to 100 of these EBs to derive dynamical masses and radii with precisions of 3% or better. We use multiplexed near-infrared H-band spectroscopy from the Sloan Digital Sky Survey-III and -IV APOGEE instrument and optical spectroscopy from the Hobby-Eberly Telescope High-resolution Spectrograph to derive double-lined spectroscopic orbits and dynamical mass ratios (q) for the EB sample, two of which we showcase in this paper. This orbital information is combined with Kepler photometry to derive orbital inclination, dynamical masses of the system components, radii, and temperatures. These measurements are directly applicable for benchmarking stellar models that are integrating the next generation of improvements, such as the magnetic suppression of convection efficiency, updated opacity tables, and fine-tuned equations of state. We selected our EB sample to include systems with low-mass (M less than or similar to 0.8 M-circle dot) primary or secondary components, as well as many EBs expected to populate the relatively sparse parameter space below similar to 0.5 M-circle dot. In this paper, we describe our EB sample and the analytical techniques we are utilizing, and also present masses and radii for two systems that inhabit particularly underpopulated regions of mass-radius-period space: KIC 2445134 and KIC 3003991. Our joint spectroscopic and photometric analysis of KIC 2445134 (q = 0.411 +/- 0.001) yields masses and radii of M-A = 1.29 +/- 0.03 M-circle dot, M-B = 0.53 +/- 0.01 M-circle dot, R-A = 1.42 +/- 0.01 R-circle dot, R-B = 0.510 +/- 0.004 R-circle dot, and a temperature ratio of T-B/T-A = 0.635 +/- 0.001; our analysis of KIC 3003991 (q = 0.298 +/- 0.006) yields M-A = 0.74 +/- 0.04 M-circle dot, M-B = 0.222 +/- 0.007 M-circle dot, R-A = 0.84 +/- 0.01 R-circle dot, R-B = 0.250 +/- 0.004 R-circle dot, and a temperature ratio of T-B/T-A = 0.662 +/- 0.001.NASA ADAP grants [NNX13AF32G, 16-ADAP16-0201]; NSF grantNational Science Foundation (NSF) [AST 1517592]; Center for Exoplanets and Habitable Worlds; Pennsylvania State University; Eberly College of Science; Pennsylvania Space Grant Consortium; NSFNational Science Foundation (NSF) [AST 1006676, AST 1126413]; National Aeronautics and Space AdministrationNational Aeronautics & Space Administration (NASA); National Science FoundationNational Science Foundation (NSF); Alfred P..Sloan FoundationAlfred P. Sloan Foundation; U.S. Department of Energy of ScienceUnited States Department of Energy (DOE); University of Arizona; Brazilian Participation Group; Brookhaven National LaboratoryUnited States Department of Energy (DOE); University of CambridgeUniversity of Cambridge; Carnegie Mellon University; University of FloridaUniversity of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins UniversityJohns Hopkins University; Lawrence Berkeley National LaboratoryUnited States Department of Energy (DOE); Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State UniversityOhio State University; University of Portsmouth; Princeton UniversityPrinceton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of WashingtonUniversity of Washington; Yale UniversityThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at [email protected]

The SDSS-HET Survey of Kepler Eclipsing Binaries. Description of the Survey and First Results

The Kepler mission has provided a treasure trove of eclipsing binaries (EBs), observed at extremely high photometric precision, nearly continuously for several years. We are carrying out a survey of similar to 100 of these EBs to derive dynamical masses and radii with precisions of 3% or better. We use multiplexed near-infrared H-band spectroscopy from the Sloan Digital Sky Survey-III and -IV APOGEE instrument and optical spectroscopy from the Hobby-Eberly Telescope High-resolution Spectrograph to derive double-lined spectroscopic orbits and dynamical mass ratios (q) for the EB sample, two of which we showcase in this paper. This orbital information is combined with Kepler photometry to derive orbital inclination, dynamical masses of the system components, radii, and temperatures. These measurements are directly applicable for benchmarking stellar models that are integrating the next generation of improvements, such as the magnetic suppression of convection efficiency, updated opacity tables, and fine-tuned equations of state. We selected our EB sample to include systems with low-mass (M less than or similar to 0.8 M-circle dot) primary or secondary components, as well as many EBs expected to populate the relatively sparse parameter space below similar to 0.5 M-circle dot. In this paper, we describe our EB sample and the analytical techniques we are utilizing, and also present masses and radii for two systems that inhabit particularly underpopulated regions of mass-radius-period space: KIC 2445134 and KIC 3003991. Our joint spectroscopic and photometric analysis of KIC 2445134 (q = 0.411 +/- 0.001) yields masses and radii of M-A = 1.29 +/- 0.03 M-circle dot, M-B = 0.53 +/- 0.01 M-circle dot, R-A = 1.42 +/- 0.01 R-circle dot, R-B = 0.510 +/- 0.004 R-circle dot, and a temperature ratio of T-B/T-A = 0.635 +/- 0.001; our analysis of KIC 3003991 (q = 0.298 +/- 0.006) yields M-A = 0.74 +/- 0.04 M-circle dot, M-B = 0.222 +/- 0.007 M-circle dot, R-A = 0.84 +/- 0.01 R-circle dot, R-B = 0.250 +/- 0.004 R-circle dot, and a temperature ratio of T-B/T-A = 0.662 +/- 0.001.NASA ADAP grants [NNX13AF32G, 16-ADAP16-0201]; NSF grantNational Science Foundation (NSF) [AST 1517592]; Center for Exoplanets and Habitable Worlds; Pennsylvania State University; Eberly College of Science; Pennsylvania Space Grant Consortium; NSFNational Science Foundation (NSF) [AST 1006676, AST 1126413]; National Aeronautics and Space AdministrationNational Aeronautics & Space Administration (NASA); National Science FoundationNational Science Foundation (NSF); Alfred P..Sloan FoundationAlfred P. Sloan Foundation; U.S. Department of Energy of ScienceUnited States Department of Energy (DOE); University of Arizona; Brazilian Participation Group; Brookhaven National LaboratoryUnited States Department of Energy (DOE); University of CambridgeUniversity of Cambridge; Carnegie Mellon University; University of FloridaUniversity of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins UniversityJohns Hopkins University; Lawrence Berkeley National LaboratoryUnited States Department of Energy (DOE); Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State UniversityOhio State University; University of Portsmouth; Princeton UniversityPrinceton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of WashingtonUniversity of Washington; Yale UniversityThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at [email protected]