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Measurement of Associated Z+Charm Production and Search for W' Bosons in the CMS Experimented at the LHC

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UNIVERSIDAD COMPLUTENSE DE MADRID

FACULTAD DE CIENCIAS FÍSICAS
Departamento de Física Atómica, Molecular y Nuclear

TESIS DOCTORAL

Measurement of associated Z+charm production and search for W' bosons in the CMS experimented at the LHC

Medida de la producción asociada de Z+charm y búsqueda de bosones
W' en el experimento CMS del LHC

MEMORIA PARA OPTAR AL GRADO DE DOCTOR
PRESENTADA POR

Alberto Escalante del Valle

Director

Juan Alcaraz Maestre
Madrid, 2017

©Alberto Escalante del Valle, 2017

´
CENTRO DE INVESTIGACIONES ENERGETICAS

´
MEDIOAMBIENTALES Y TECNOLOGICAS

Measurement of associated Z+charm production and Search for W0 bosons in the CMS experiment at the LHC

by

Alberto Escalante del Valle

A thesis submitted in partial fulfillment for the degree of Doctor of Philosophy

in the

Universidad Complutense de Madrid
Facultad de Ciencias F´ısicas
Departamento de F´ısica At´omica, Molecular y Nuclear

Supervised by:
Dr. Juan Alcaraz Maestre
Dr. Juan Pablo Ferna´ndez Ramos

Madrid
February 2017

´
CENTRO DE INVESTIGACIONES ENERGETICAS

´
MEDIOAMBIENTALES Y TECNOLOGICAS

Medida de la producci´on asociada de
Z+charm y Bu´squeda de bosones W0 en el experimento CMS del LHC

por

Alberto Escalante del Valle

Memoria de la tesis presentada para optar al grado de Doctor en Filosof´ıa

en la

Universidad Complutense de Madrid
Facultad de Ciencias F´ısicas
Departamento de F´ısica At´omica, Molecular y Nuclear

Supervisado por:
Dr. Juan Alcaraz Maestre
Dr. Juan Pablo Ferna´ndez Ramos

Madrid
Febrero 2017

Abstract

Measurement of associated Z+charm production and
Search for W0 bosons in the CMS experiment at the LHC

by Alberto Escalante del Valle

Do we understand how elementary particles interact with each other? Are we able to predict the result of the collisions of these elementary particles at the LHC? The objective of this thesis is to investigate the validity of our current theoretical model, the Standard Model of particle physics, to explain the production of two low rate processes in proton-proton collisions at the LHC.

The first half of the thesis studies the potential production of new types of interactions, mediated by new W0 bosons, present in many extensions of the Standard Model. This is the first search of this kind at a centre of mass energy of 13 TeV in CMS and uses a dataset of 2.3 fb−1 to search for an excess in the production of events with a muon and large missing transverse energy. As a result of this study, the analysed data is found to be in agreement with predictions of the Standard Model and disfavours the production of new W0 → µν processes. This analysis alone is not able to exclude the production of all kind of W0 interactions. However, it puts strong constrains to its potential cross

0

−1

section and decay to a muon and a neutrino, σW B(W → µν) < 3 fb for W0 masses larger than 2 TeV. In the context of the Sequential Standard Model model, this result excludes WS0 SM bosons with masses smaller than 3.9 TeV.

0

The second part of the manuscript presents the first measurement in CMS of the associated production of Z bosons with charm quarks, Z + c, using 19.7 fb−1 of data collected at 8 TeV. This is a rare process in the Standard Model and its cross section in the studied fiducial region is measured to be σfid(Z + c) = 8.6 ± 0.5 (stat) ± 0.7 (syst) pb. Additionally its relative production to that of bottom quarks, Z + b, is measured to be σ(Z + c)/σ(Z + b) = 2.0 ± 0.2 (stat) ± 0.2 (syst). Both measurements are also determined differentially as a function of transverse momentum of the Z boson and of the heavy flavour jet. Finally these measurements are compared with different theoretical predictions.

Acknowledgements

¿Cu´anto tiempo se tarda en escribir una tesis doctoral? En mi caso ∼3650 d´ıas. Este documento cierra mi etapa de formaci´on como f´ısico que empec´e hace aproximadamente 10 an˜os cuando me matricul´e en Ciencias F´ısicas en la UCM con 18 an˜os. Y claro, tantos an˜os dan para muchas experiencias y para estar en deuda con mucha gente.

En primer lugar me gustar´ıa dar las gracias a todas aquellas personas que me dieron una oportunidad sin conocerme de nada, a todas aquellas personas que tuvieron abierta la puerta de su despacho para escucharme y me regalaron un minuto de su tiempo, y sobre todo a aquellas personas que fueron capaces de motivarme y sacar lo mejor de m´ı mismo. Todos ell@s saben quienes son, y por ello se merecen estar en el primer p´arrafo. Si hoy estoy aqu´ı escribiendo estas l´ıneas es gracias a todos vosotros. Muchas gracias.

Me gustar´ıa agradecer a Juan Pablo su infatigable apoyo siempre que se lo he pedido. Por poner un ejemplo, poca gente sabe que Juan Pablo se sento´ durante casi 6 meses 8 horas diarias a mi lado y me ensen˜´o a ser un f´ısico de part´ıculas en tiempo r´ecord. Durante este tiempo fue capaz de motivarme, sacar lo mejor de mi mismo y dotarme de iniciativa para no tener miedo a proponer cosas nuevas. Gracias por ensen˜arme a volar.

Juan Pablo y yo tenemos algo en comu´n, somos muy impulsivos y muchas veces necesitamos alguien que nos guie y nos ayude a a centrarnos cuando nos aceleramos. Por ello, he tenido una suerte incre´ıble de poder trabajar con Isabel Josa Mutuberr´ıa. Isabel, al margen de ser una excelente investigadora, ha tenido la paciencia de escucharme, hacerme siempre las preguntas correctas y de esta forma organizar los conceptos en mi mente. Al mismo tiempo, Isabel ha demostrado una fuerza mental sobrenatural para poder sacar adelante Z+c cuando m´as complicado parec´ıa. Muchas gracias por todo.

Muchas veces en una empresa se dice que si alguien se va, la empresa colapsa. Esto es cierto y en W’ esa persona es Begon˜a de la Cruz. Begon˜a fue capaz de coordinar W’ en tiempos de mucha presi´on y carga de trabajo. Al mismo tiempo Begon˜a me ensen˜´o a ser ambicioso y me anim´o a estudiar la resoluci´on y la escala de los muones de alto pT . Finalmente Begon˜a se aseguro´ que W’ y yo tuvi´esemos un peso y una visibilidad mayor de la que nos corresponder´ıa por el taman˜o del grupo. No todos los h´eroes llevan capa.

´
Una tesis es una marat´on y hay veces que el mayor enemigo es uno mismo. Oscar

Gonz´alez L´opez, al margen de ser el f´ısico m´as pol´emico que conozco, me ha demostrado ser un apoyo continuo tanto personal como profesional cuando ma´s lo necesitaba. Al mismo tiempo darle unas gracias enormes por haberse le´ıdo la tesis. Para los futuros
´estudiantes de doctorado del CIEMAT, no dejen de hablar y aprender con Oscar (”el

t´ıo del CERN”), no se arrepentir´an.

ii

Acknowledgements

iii
Finalmente voy a cerrar este primer grupo de agradecimientos con una persona con la cual da verdadero placer hablar de f´ısica, Juan Alcaraz. Lo que m´as me gusta de Juan es su versatilidad para explicar un concepto y recalcar su importancia en un an´alisis concreto. Muchas de sus explicaciones me han hecho abrir los ojos y han dado lugar a nuevas ideas. Me gustar´ıa agradecerle el apoyo que me di´o en cada proyecto que empec´e, por dejarme equivocarme para aprender de ello y sobre todo dejarme ser investigador durante estos u´ltimos cuatro an˜os. Gracias.

En un segundo lugar me gustar´ıa agradecer a los CMSeros que me han acompan˜ado en este viaje: Cruz, Mara, Jesu´s, Chema, Pablo, Cristina, Ignacio, Silvia, Nica, Marcos, Conchita y Marta. Gracias. In this part I would like to thank to the people at CERN that helped me during this thesis, namely: Ivan, Slava, Daniele, Petra, Caroline, Kostas, Simon, Carlo, Mar´ıa, Mauro, Luca, Shahram, Roberto, Alice... and especially to the Z0 → µµ and W0 → eν analysis teams. El primer p´arrafo va dedicado a todos vosotros.

El siguiente p´arrafo va dedicado a mis compan˜eros de despacho/aventuras en el CIEMAT. Eduino un gustazo haber debatido largo y tendido de f´ısica contigo. Me llevo un amigo. Marisma, te dejo como mam´a de CMS, cuida de los nuevos y demuestra lo que vales (¡much´ısimo!). Javismo, simplemente: crack. Daniel D., un gustazo conversar contigo y compartir experiencias. Mariano, casi tan buen portero como b´etico. Gran Manu, tu grandeza esta al nivel de tu altura (¡taponazo incluido!). Manuelinho, (hostias al teclado=ON) gran persona y mejor cantante (hostias al teclado=OFF). Diana, por tu culpa perd´ı un cal-
´cet´ın, no te lo perdonar´e jama´s. Miguel Angel y Adri´an Q., os mando todas las fuerzas

que me sobran, ¡´animo para la recta final de la tesis!. Irene, juventud y energ´ıa, ¡lo tienes todo para triunfar!. A los m´as veteranos, Bruno, Rafa, Jos´e, Jorge y Don Nacho, un placer haber compartido batallitas con ustedes. B´arbara, mi ”salvadora” en Benasque y a la par un tesoro de persona. Juanjo y Jaime, maestros de la inform´atica. Don Antonio, ahora en versi´on doctor y padrazo, enhorabuena. Finalmente Carlos, todo que intentas le pones un empen˜o envidiable: investigaci´on, deporte, debatir, salir de fiesta... Seguir´e tu ejemplo en el futuro. ¡Gracias a todos por acompan˜arme en esta aventura!

¿Qu´e hay que hacer para completar una tesis doctoral sin volverse loco? En mi caso he recargado las pilas gracias a mis compan˜eros de equipo. Quiero aprovechar este u´ltimo pa´rrafo para agradecer a todas las personas con las que he compartido vestuario durante todos estos an˜os: ESA Trainees*, Cross F´ısicas UED*, F´ısicas (Sala, Siete, Once y Rugby), Gran Potra, Ol´ımpicos FC, Melvilles*, Hors Categorie, Solteros FC**, Saint-Genis-Ferney-Crozet, La Can˜ada FC, Sons of Pitches*, CERN XV**... All MVPs.

Y en u´ltimo lugar agradecer a mi familia su apoyo durante todos estos an˜os, especialmente cuando he estado m´as lejos f´ısica y mentalmente. Soy un afortunado, GRACIAS.

Contents

Abstract

i

Acknowledgements List of Figures List of Tables

ii vii x

Abbreviations

xi

Introduction

1

1 LHC and the CMS experiment

5

58

1.1 The accelerator: Large Hadron Collider . . . . . . . . . . . . . . . . . . .

1.2 Introduction to LHC physics . . . . . . . . . . . . . . . . . . . . . . . . .
1.2.1 Parton distribution functions . . . . . . . . . . . . . . . . . . . . . 12 1.2.2 The hard interaction . . . . . . . . . . . . . . . . . . . . . . . . . . 14 1.2.3 Parton shower and hadronization . . . . . . . . . . . . . . . . . . . 16 1.2.4 13 TeV vs 8 TeV physics . . . . . . . . . . . . . . . . . . . . . . . . 18
1.3 The detector: Compact Muon Solenoid . . . . . . . . . . . . . . . . . . . . 20
1.3.1 Tracker system . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 22 1.3.2 Electromagnetic calorimeter . . . . . . . . . . . . . . . . . . . . . . 24 1.3.3 Hadronic calorimeter . . . . . . . . . . . . . . . . . . . . . . . . . . 25 1.3.4 Muon detectors . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 26

2 Search for W0 → µν bosons

28

2.1 Is the Standard Model the ultimate theory? . . . . . . . . . . . . . . . . . 28
2.1.1 New interactions and extended gauge symmetries . . . . . . . . . . 31

2.1.2 Sequential Standard Model W0 . . . . . . . . . . . . . . . . . . . . 34
2.2 Data samples and simulation . . . . . . . . . . . . . . . . . . . . . . . . . 36
2.2.1 13 TeV dataset in 2015 . . . . . . . . . . . . . . . . . . . . . . . . 36 2.2.2 Monte Carlo simulations . . . . . . . . . . . . . . . . . . . . . . . . 37
2.3 Physics objects: muons and MET . . . . . . . . . . . . . . . . . . . . . . . 41
2.3.1 Trigger . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 42 2.3.2 Primary vertex . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 44

iv

Contents

v

2.3.3 Muon reconstruction and identification . . . . . . . . . . . . . . . . 45 2.3.4 Muon pT assignment and performance . . . . . . . . . . . . . . . . 49

2.3.5 Muon momentum resolution . . . . . . . . . . . . . . . . . . . . . . 51 2.3.6 Muon momentum scale . . . . . . . . . . . . . . . . . . . . . . . . 54 2.3.7 Jets . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 59 2.3.8 MET . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 60
2.4 The W0 search: . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 62

2.4.1 Analysis pre-selection: single muon candidates . . . . . . . . . . . 62 2.4.2 Discriminant variable for the search: transverse mass . . . . . . . . 66

2.4.3 Kinematic selection . . . . . . . . . . . . . . . . . . . . . . . . . . 69 2.4.4 Final selection . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 71 2.4.5 Scrutiny of the highest MT events . . . . . . . . . . . . . . . . . . 73 2.4.6 Systematic uncertainties . . . . . . . . . . . . . . . . . . . . . . . . 75
2.5 Results and interpretation . . . . . . . . . . . . . . . . . . . . . . . . . . . 78
2.5.1 Statistical model . . . . . . . . . . . . . . . . . . . . . . . . . . . . 78 2.5.2 The upper limit . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 80

2.5.3 Constrains to the W0 production at 13 TeV . . . . . . . . . . . . . 81

2.6 Search for new W0 bosons: conclusions . . . . . . . . . . . . . . . . . . . . 86

3 Z + c cross section measurement

88

3.1 Standard model against Z + c and Z + b . . . . . . . . . . . . . . . . . . . 88

3.1.1 The charm quark PDF . . . . . . . . . . . . . . . . . . . . . . . . . 92
3.2 Data samples and simulation . . . . . . . . . . . . . . . . . . . . . . . . . 94
3.2.1 2012 8 TeV dataset . . . . . . . . . . . . . . . . . . . . . . . . . . . 94 3.2.2 Monte Carlo simulations . . . . . . . . . . . . . . . . . . . . . . . . 94

3.3 Physics objects: leptons and heavy flavour . . . . . . . . . . . . . . . . . . 96

3.3.1 Muons . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 96 3.3.2 Electrons . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 97 3.3.3 Heavy flavour tagging . . . . . . . . . . . . . . . . . . . . . . . . . 100
3.4 The Z+charm measurement . . . . . . . . . . . . . . . . . . . . . . . . . . 104
3.4.1 Z+jets selection . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 104 3.4.2 Z+heavy flavour selection . . . . . . . . . . . . . . . . . . . . . . . 106 3.4.3 W+c and eµ auxiliary samples . . . . . . . . . . . . . . . . . . . . 111

¯
3.4.4 Other background: tt, diboson and Z+light . . . . . . . . . . . . . 120

3.4.5 Signal extraction . . . . . . . . . . . . . . . . . . . . . . . . . . . . 122 3.4.6 Systematic uncertainties . . . . . . . . . . . . . . . . . . . . . . . . 126
3.5 Results and interpretation . . . . . . . . . . . . . . . . . . . . . . . . . . . 131

3.5.1 Inclusive Z+c and Z+c/Z+b cross section . . . . . . . . . . . . . . 132 3.5.2 Differential Z+c and Z+c/Z+b cross section . . . . . . . . . . . . 136
3.6 Z + c cross section measurement: conclusions . . . . . . . . . . . . . . . . 142

Summary and outlook Resumen

144 148

Contents

vi

A Summary of the Standard Model of Particle Physics

150

A.1 Local gauge invariance . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 152 A.2 Quantum Electrodynamics: QED . . . . . . . . . . . . . . . . . . . . . . . 153 A.3 Quantum Cromodynamics: QCD . . . . . . . . . . . . . . . . . . . . . . . 154 A.4 Electroweak unification . . . . . . . . . . . . . . . . . . . . . . . . . . . . 156

A.5 Spontaneous symmetry breaking and

Higgs mechanism . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 160

B Publications and technical reports Bibliography

164 166

List of Figures

1.1 Sketch of the LHC pre-accelerator chain . . . . . . . . . . . . . . . . . . .

69

√

1.2 Measured cross sections for different SM process at s = 7, 8 and 13 TeV 1.3 LHC integrated luminosity in 2012 and 2015 . . . . . . . . . . . . . . . . . 10 1.4 Mean number of interactions per bunch crossing in 2012 . . . . . . . . . . 11 1.5 Parton distribution function for different partons at different energy scales:

Q2 = 10 GeV2 and Q2 = 1000 GeV2 . . . . . . . . . . . . . . . . . . . . . 13
1.6 Example of a hard scattering process . . . . . . . . . . . . . . . . . . . . . 14

1.7 Simplified sketch of the parton shower and hadronization processes . . . . 17 1.8 Parton luminosity ratio at 13 TeV and 8 TeV from MSTW2008NLO PDF

group . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 19

1.9 Photo of CMS detector in one of the latest stages of its construction . . . 21 1.10 3-Dimensional sketch of the CMS detector . . . . . . . . . . . . . . . . . . 22 1.11 Schematic view of the CMS Tracker in the r-z plane and its different

sub-detectors . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 23

1.12 Sketch of the CMS ECAL and its sub-detectors . . . . . . . . . . . . . . . 24

1.13 Schematic layout of the CMS HCAL . . . . . . . . . . . . . . . . . . . . . 25

1.14 Sketch of the CMS Muon system and its sub-detectors . . . . . . . . . . . 26 1.15 CMS DTs and CSC muon detector during its construction . . . . . . . . . 27

2.1 Leading order Feynman diagram describing SSM W0 production at the

LHC. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 34

2.2 Sketch that shows the dominant backgrounds in the W0 search . . . . . . 37 2.3 Higher order k-factor describing the combined QCD and EW corrections for the high mass W → µν background simulation . . . . . . . . . . . . . 39
2.4 Trigger efficiencies in W0 → µν events from simulation . . . . . . . . . . . 43 2.5 Evolution of the instantaneous luminosity in 2012 at 8 TeV and 2015 at

13 TeV . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 45

2.6 Event display of the number of reconstructed vertices in a W0 → µν can-

didate event at 13 TeV . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 45

2.7 Distribution of the number of reconstructed vertices in dilepton events . . 46 2.8 Global muon reconstruction efficiency in W0 → µν simulation . . . . . . . 47 2.9 High-pT muon identification efficiency in W0 → µν simulation . . . . . . . 48 2.10 Sketch that illustrates the definition of the observable sagitta of a track . 49 2.11 Sketch of the cosmic muon two leg-reconstruction . . . . . . . . . . . . . . 52 2.12 Muon momentum resolution using cosmic muons . . . . . . . . . . . . . . 53 2.13 Academic sketch that shows the effect of a misaligned geometry in the

track reconstruction . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 54

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  • Astrophysics and Physics of Neutrino Detection

    Astrophysics and Physics of Neutrino Detection

    Astrophysics and Physics of Neutrino Detection A THESIS SUBMITTED TO THE FACULTY OF THE GRADUATE SCHOOL OF THE UNIVERSITY OF MINNESOTA BY Cheng-Hsien Li IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF Doctor of Philosophy Professor Yong-Zhong Qian, Advisor September, 2017 c Cheng-Hsien Li 2017 ALL RIGHTS RESERVED Acknowledgements This dissertation would be impossible to complete without the help and support from many people and institutions. First and foremost, I would like to express my sincere gratitude to my research advisor, Professor Yong-Zhong Qian, who has patiently guided me through this long PhD journey. I learned a lot from his insights in neutrino physics and his approaches to problems during countless hours of discussion. He always offered helpful suggestions regarding my thesis projects and how to conduct rigorous research. I would like to thank Dr. Projjwal Banerjee for guiding me on the SN1987A project presented in this thesis. He was not only a research collaborator but he is also a dear friend to me. He kindly offered advice and encouragement which helped me overcome difficulties during my PhD study. In addition, I feel grateful to have received a lot of help from then fellow graduate students, Dr. Ke-Jun Chen, Dr. Meng-Ru Wu, Dr. Zhen Yuan, Mr. Zhu Li, and Mr. Zewei Xiong, in the Nuclear Physics Group. I am also indebted to Professor Hans-Thomas Janka and Professor Tobias Fischer for generously providing supernova simulation results from their research groups upon request, Professor Huaiyu Duan for commenting on my wave-packet project, and Professor Alexander Heger for the computing resource I received in the research group.
  • Indirect Searches in the PAMELA and Fermi Era Aldo Morselli, Igor Moskalenko

    Indirect Searches in the PAMELA and Fermi Era Aldo Morselli, Igor Moskalenko

    Indirect searches in the PAMELA and Fermi era Aldo Morselli INFN, Sezione di Roma Tor Vergata Springel, Wang, Volgensberger, Ludlow, Jenkins, Helmi, Navarro, Frenk & White ‘08 New Horizons for Modern Cosmology, Dark Matter, February 9, 2009, Galileo Instiute, Firen Aldo Morselli, INFN Roma Tor Vergata 1 PAMELA: Cosmic-Ray Antiparticle Measurements: Antiprotons an example in mSUGRA 5 years simulation fd: Clumpiness factors needed to disentangle a neutralino induced component in the antiproton flux f = the dark matter fraction concentrated in clumps d = the overdensity due to a clump with respect to the local halo density A.Lionetto, A.Morselli, V.Zdravkovic JCAP09(2005)010 [astro-ph/0502406] New Horizons for Modern Cosmology, Dark Matter, February 9, 2009, Galileo Instiute, Firen Aldo Morselli, INFN Roma Tor Vergata 2 Supersymmetry introduces free parameters: In the MSSM, with Grand Unification assumptions, the masses and couplings of the SUSY particles as well as their production cross sections, are entirely described once 5 parameters are fixed: • M1/2 the mass parameter of supersymmetric partners of gauge fields (gauginos) • µ the higgs mixing parameters that appears in the neutralino and chargino mass matrices • m0 the common mass for scalar fermions at the GUT scale • A the trilinear coupling in the Higgs sector • tang β = v2 / v1 = <H2> / <H1> the ratio between the two vacuum expectation values of the Higgs fields New Horizons for Modern Cosmology, Dark Matter, February 9, 2009, Galileo Instiute, Firen Aldo Morselli, INFN Roma Tor Vergata
  • Sterile Neutrinos in 4D and 5D in Supernovæ and the Cosmo

    Sterile Neutrinos in 4D and 5D in Supernovæ and the Cosmo

    Scuola Normale Superiore Sterile Neutrinos in 4D and 5D in Supernovæ and the Cosmo Marco Cirelli Advisors Dr. Andrea Romanino Prof. Riccardo Barbieri Ph.D. Thesis Autumn 2003 A Anna Contents Preface iii Rationale 1 1 Introduction: New Particle Physics from Astrophysics and Cosmology 3 1.1 TheStandardModelandwhytogobeyond . ......... 3 1.1.1 TheHierarchyProblem . ..... 5 1.1.2 Introduction to Extra Dimensions . ......... 7 1.2 “Standard” neutrino physics and why to go beyond . .............. 11 1.2.1 “Whatisleft,whatisnext?” . ....... 13 1.2.2 Sterileneutrinos .............................. ...... 15 1.3 TheroleofSupernovæ.............................. ....... 18 1.3.1 Supernova basics and neutrino signal formation . .............. 18 1.3.2 Theenergylossconstraint. ........ 21 1.3.3 Waitingforthenextsupernova . ........ 23 1.4 TheroleoftheEarlyUniverse . ......... 27 1.4.1 Big Bang Nucleosynthesis . ....... 27 1.4.2 Large Scale Structure and Cosmic Microwave Background............. 35 2 A (4D) sterile neutrino 38 2.1 Active-sterile neutrino mixing formalism . ................ 38 2.2 Sterile effects in cosmology . .......... 41 2.2.1 Technicaldetails .............................. ...... 41 2.2.2 Results ....................................... 45 2.3 SterileeffectsinSupernovæ . .......... 48 2.3.1 Technicaldetails .............................. ...... 50 2.3.2 Results ....................................... 54 3 Neutrinos in Extra Dimensions 56 3.1 Theextradimensionalsetup. .......... 57 3.2 Cosmological safety (or irrelevance) . ............... 58 i 3.3 Supernovacoreevolution . ......... 58 3.3.1 Thefeedbackmechanisms . ...... 59 3.3.2 Details of the model of core evolution . .......... 60 3.4 Theoutcome: boundsandsignals. .......... 70 3.5 Appendix: subleading invisible channels . ............... 76 4 Conclusions 77 References 79 ii Preface During my Ph.D. course, under the guidance of Riccardo Barbieri and Andrea Romanino, I began work- ing on fascinating subjects at the intersection of High Energy Physics, Neutrino Physics, Astrophysics and Cosmology.
  • Pos (EPS-HEP2011) 098 Neutrino Mass Models at the Tev Scale

    Pos (EPS-HEP2011) 098 Neutrino Mass Models at the Tev Scale

    Neutrino mass models at the TeV scale and their PoS(EPS-HEP2011)098 tests at the LHC Alessandro Strumia∗ Dipartimento di Fisica dell’Università di Pisa and INFN, Italia National Institute of Chemical Physics and Biophysics, Ravala 10, Tallinn, Estonia E-mail: [email protected] Assuming that the new particles introduced by type-I, type-II, type-III see-saw in order to mediate neutrino masses are below a TeV, we describe their resulting manifestations at LHC. The 2011 Europhysics Conference on High Energy Physics-HEP 2011, July 21-27, 2011 Grenoble, Rhône-Alpes France ∗Speaker. c Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-ShareAlike Licence. http://pos.sissa.it/ Neutrino mass models at LHC Alessandro Strumia HH HH L H Singlet Triplet Triplet LL LL L H Figure 1: The neutrino Majorana mass operator (LH)2 can be mediated by tree level exchange of: I) a fermion singlet (‘see-saw’); II) a fermion triplet; III) a scalar triplet. PoS(EPS-HEP2011)098 1. See-saw models In the past decade we observed violations of lepton flavor in neutrinos and understood that it is due to neutrino oscillations due to neutrino masses [1]. Neutrino masses can be of Majorana type (violating also lepton number) or of Dirac type (adding to the SM a light right-handed neutrino, such that lepton number is conserved). We here stick to the most plausible scenario for neutrino masses: the see-saw models, all de- signed to give at tree level Majorana masses described by the unique dimension-5 effective operator 2 2 (LH) =2LL.
  • Jhep06(2010)036

    Jhep06(2010)036

    Published for SISSA by Springer Received: April 6, 2010 Accepted: May 25, 2010 Published: June 8, 2010 JHEP06(2010)036 Thermal production of axino dark matter Alessandro Strumia CERN, PH-TH, CH-1211, Geneva 23, Switzerland Dipartimento di Fisica dell’Universit`adi Pisa, Largo Pontecorvo 3, 56127, Pisa, Italia INFN { Sezione di Pisa, Largo Pontecorvo 3, 56127, Pisa, Italia E-mail: [email protected] Abstract: We reconsider thermal production of axinos in the early universe, adding: a) missed terms in the axino interaction; b) production via gluon decays kinematically allowed by thermal masses; c) a precise modeling of reheating. We find an axino abunance a few times larger than previous computations. Keywords: Supersymmetry Phenomenology ArXiv ePrint: 1003.5847 Open Access doi:10.1007/JHEP06(2010)036 Contents 1 Introduction1 2 Axino couplings2 3 Thermal axino production rate2 JHEP06(2010)036 4 Thermal axino abundance5 5 Conclusions6 1 Introduction The strong CP problem can be solved by the Peccei-Quinn symmetry [1], that manifests 9 at low energy as a light axion a with a decay constant f >∼ 5 10 GeV [2]. In supersym- metric models the axion a gets extended into an axion supermultiplet which also contains the scalar saxion s and the fermionic axinoa ~ [3{5]. Depending on the model of super- symmetry breaking, the axino can easily be lighter than all other sparticles, becoming the stable lightest supersymmetric particle (LSP) and consequently a Dark Matter candidate (warm axino: [6]; hot axino: [7]; cold axino: [8]; [9]). It is thereby interesting to compute its cosmological abundance.
  • KEK-PH2018 Timetable

    KEK-PH2018 Timetable

    KEK-PH2018 Timetable Tuesday, 13 February 2018 09:00 - 09:30 Registration 09:30 - 10:30 Talks Convener: Mihoko Nojiri (KEK) 09:30 Late-time magnetogenesis 30' Speaker: Kiwoon Choi (CTPU, IBS) 10:00 Lovely phase space 30' Speaker: Tom Melia (Kavli IPMU) 10:30 - 11:00 Tea Time 11:00 - 12:00 Talks Convener: Alejandro Ibarra (Technical University of Munich) 11:00 Axion coupled to hidden sector 30' Speaker: Fuminobu Takahashi (Tohoku University) 11:30 Multi-Messenger Astrophysics in the Gravitational Wave Era 30' Speaker: Kunihito Ioka (YITP, Kyoto University) 12:00 - 13:30 Lunch 13:30 - 15:30 Joint Session with Muon g-2 Workshop Convener: Bradley Lee Roberts (Boston University) Location: Kobayashi Hall, Kenkyu-honkan 13:30 Belle II overview 30' Speaker: Phillip Urquijo (University of Melbourne) 14:00 Fermilab muon g-2 experiment 30' Speaker: Sudeshna Ganguly (University of Illinois at Urbana-Champaign) 14:30 J-PARC muon g-2 experiment 30' Speaker: Takayuki Yamazaki (KEK) 15:00 New Physics and the Muon g-2 30' Speaker: Hooman Davoudiasl (Brookhaven National Laboratory) 15:30 - 15:50 Tea Time 15:50 - 17:30 Short Talks Convener: Fuminobu Takahashi (Tohoku University) 15:50 High-energy neutrinos from multi-body decaying dark matter 20' Speaker: Nagisa Hiroshima (KEK, ICRR) 16:10 Search for New physics with High multiplicity from High energy cosmic rays 20' Speaker: Yongsoo Jho (Yonsei University) 16:30 Thermal Gravitational Contribution to Dark Matter Production 20' Speaker: Yong Tang (University of Tokyo) 16:50 Enhanced Axion-Photon Coupling
  • Publications 2008- 2009

    Publications 2008- 2009

    Publications 2008- 2009 Inter-team papers – in refereed journals 1. Model-independent implications of the e+-, anti-proton cosmic ray spectra on properties of Dark Matter Marco Cirelli (Saclay, SPhT), Mario Kadastik, Martti Raidal (NICPB, Tallinn), Alessandro Strumia (Pisa U. & INFN, Pisa) . Sep 2008. 25pp. Published in Nucl.Phys.B813:1-21,2009. e-Print: arXiv:0809.2409 [hep-ph]* Cited 141 times 2. Non-linear isocurvature perturbations and non-Gaussianities David Langlois, Filippo Vernizzi, David Wands (includes UniverseNet members from Saclay + APC Paris). Sep 2008. 24pp. Published in JCAP 0812:004,2008. e-Print: arXiv:0809.4646 [astro-ph] Cited 13 times 3. The Effective Theory of Quintessence: the w<-1 Side Unveiled Paolo Creminelli, Guido D'Amico, Jorge Norena, Filippo Vernizzi (includes UniverseNet members from Saclay + ICTP Trieste). Nov 2008. 34pp. Published in JCAP 0902:018,2009. e-Print: arXiv:0811.0827 [astro-ph] Cited 8 times 4. Parameterizing the effect of dark energy perturbations on the growth of structures. Guillermo Ballesteros (Madrid, IFT & CERN), Antonio Riotto (CERN & INFN, Padua). Jul 2008. Published in Phys.Lett.B668:171-176,2008. e-Print: arXiv:0807.3343 [astro-ph]* Cited 11 times 5. Exact Spherically symmetric solutions in massive gravity. Z. Berezhiani (L'Aquila U. & Gran Sasso), D. Comelli (INFN, Ferrara), F. Nesti, L. Pilo (L'Aquila U. & Gran Sasso) . Mar 2008. 20pp. Published in JHEP 0807:130,2008. e-Print: arXiv:0803.1687 [hep-th]* Cited 10 times 6. Precision studies of the NNLO DGLAP evolution at the LHC with CANDIA. Alessandro Cafarella (Democritos Nucl. Res. Ctr.), Claudio Coriano (Salento U.
  • Grand Unification at the Electroweak Scale

    Grand Unification at the Electroweak Scale

    Large Extra Dimensions & Grand Unification at the Electroweak Scale Behrad Taghavi Department of Physics & Astronomy, Stony Brook University. ! Advisor: Dr. Patric Meade OUTLINE • Motivations • Kaluza-Klein Theory • Localization on Topological Defects • Large Extra Dimensions Paradigm • ADD Model • Hierarchy Problem • Proton Stability • Other Models (eg. UED) • References 2 MOTIVATIONS We need beyond standard model theories to answer questions like hierarchy problem, unification of all fundamental forces, etc. Most of beyond standard model theories (like String Theory, M Theory, GUTs, MSSM, etc.) predict unification of forces at the energy scale close to planck mass. Large Extra Dimensions paradigm is capable of answering most of unanswered questions in SM elegantly and also keeps high energy physics as a experiment-based field of physics. 3 KALUZA-KLEIN THEORY Kaluza–Klein theory (KK theory) is a unified field theory of gravitation and electromagnetism built around the idea of a fifth dimension beyond the usual 4 of space and time. “Kaluza-Klein” mechanism has been first introduced in the 1921 paper of “Theodor Kaluza” , which extended classical GR to 4+1 dimensions that resulted in unification of Electromagnetism and Einstein’s Gravity. In 1926, “Oskar Klein” gave Kaluza's classical 5-dimensional theory a quantum interpretation by introduction of “curled up” or “compact” dimensions. 4 KALUZA-KLEIN THEORY Assume that the world is (4+ n )-dimensional (n 1 ), but the extra ≥ dimensions are compact. If n =1 , our world is a M 4 S 1 manifold. ! ⌦ All fields are defined on this “M 4 S 1 cylinder”. ⌦ ! For a scalar field Φ ( x µ ,Z ) single-valuedness condition reads: Φ(xµ,Z)=Φ(xµ,Z+2⇡R),µ=0, 1, 2, 3.
  • Is the Resonance at 125 Gev the Higgs Boson?

    Is the Resonance at 125 Gev the Higgs Boson?

    Physics Letters B 718 (2012) 469–474 Contents lists available at SciVerse ScienceDirect Physics Letters B www.elsevier.com/locate/physletb Is the resonance at 125 GeV the Higgs boson? ∗ Pier Paolo Giardino a, Kristjan Kannike b,c, , Martti Raidal c,d,e, Alessandro Strumia a,c a Dipartimento di Fisica dell’Università di Pisa and INFN, Italy b Scuola Normale Superiore and INFN, Piazza dei Cavalieri 7, 56126 Pisa, Italy c National Institute of Chemical Physics and Biophysics, Ravala 10, Tallinn, Estonia d CERN, Theory Division, CH-1211 Geneva 23, Switzerland e Institute of Physics, University of Tartu, Estonia article info abstract Article history: The recently discovered resonance at 125 GeV has properties remarkably close to those of the Standard Received 25 July 2012 Model Higgs boson. We perform model-independent fits of all presently available data. The non-standard Received in revised form 4 October 2012 best-fits found in our previous analyses remain favored with respect to the SM fit, mainly but not only Accepted 18 October 2012 because the γγ rate remains above the SM prediction. Available online 22 October 2012 © 2012 Elsevier B.V. All rights reserved. Editor: B. Grinstein 1. Introduction study whether the Higgs boson is SM-like or is there any indication for new physics beyond the SM. The latter possibility is motivated − New searches for the Higgs boson [1–5] based on 5 fb 1 data by numerous multi-Higgs boson, supersymmetric, composite Higgs per experiment collected in 2012 by the Large Hadron Collider boson, dark matter, exotic scalar, etc., models.