The CMS Collaboration at the LHC searched for microscopic black hole signatures using 35 pb-1 of 7 TeV proton-proton collision data. No significant excess beyond standard model expectations was observed in events with high total transverse energy. Limits are set on the minimum black hole mass in the range of 3.5-4.5 TeV for various parameters in the large extra dimensions model. These are the first direct limits on black hole production at a particle collider.
The optimal cosmic_epoch_for_precision_cosmologySérgio Sacani
The document discusses the optimal epoch for precision cosmology measurements based on the number of independent Fourier modes available. It finds that the best constraints on the primordial power spectrum are accessible at redshifts around z=10 through instruments like 21-cm intensity mapping. The ability to constrain the initial cosmological conditions will deteriorate rapidly in our cosmic future as the exponential expansion erases information beyond 100 Hubble times from now.
This document summarizes a research project that involves building a toy model of particle collisions using C++ and ROOT. The model simulates collisions by sampling probability distributions measured in real collisions. It generates particles and assigns them properties like momentum and angle. It also models physical processes like jet production and elliptic flow. The goal is to study how properties of particles like jets are affected by a quark-gluon plasma and vice versa. The model allows tuning parameters to learn about collision interactions and switch physics processes on or off.
2014 NJP - Oscillatory solitons and time-resolved phase locking of two polari...Guilherme Tosi
This document summarizes time-resolved measurements of two polariton condensates formed in a semiconductor microcavity under nonresonant excitation. The measurements directly observe oscillatory behavior as dark or bright soliton-like waves form between the excitation spots. They also observe phase locking of the two initially independent condensates over time. These phenomena provide insights into the underlying dynamics of polariton-polariton interactions and propagation of polariton condensates.
A revised upper_limit_to_energy_extraction_from_a_kerr_black_holeSérgio Sacani
Uma nova simulação computacional feita pela NASA mostra que as partículas da matéria escura colidindo na extrema gravidade de um buraco negro pode produzir uma luz de raios-gamma forte e potencialmente observável. Detectando essa emissão forneceria aos astrônomos com uma nova ferramenta para entender tanto os buracos negros como a natureza da matéria escura, uma elusiva substância responsável pela maior parte da massa do universo que nem reflete, absorve ou emite luz.
Quantum chemical molecular dynamics simulations of graphene hydrogenationStephan Irle
Chemical adsorption of hydrogen atoms on graphite
surfaces has attracted considerable interest due to its
relevance for a broad range of areas including
plasma/fusion physics, gap tuning in graphene, and hydrogen storage. We adjusted the C-H repulsive potential of the spin-polarized self-consistent-charge density-functional tight-binding (sSCC-DFTB) method to reproduce
CCSD(T)-based relaxed potential energy curves for the
attack of atomic hydrogen on a center carbon atom of
pyrene and coronene at a tiny fraction of the computational
cost. Using this cheap quantum chemical potential, we performed direct on-the-fly Born-Oppenheimer
MD simulations while “shooting” H atoms with varying collision energies on a periodic graphene target
equilibrated at 300 Kelvin. We compared reaction cross sections for a) elastic collisions, b)
chemisorption reactions, c) penetration reactions in dependence of H/D/T kinetic energies, and found
remarkable differences to previously reported classical MD simulations of the same process. Using the
same potential, in simulations involving the shooting of up to 400 hydrogen atoms on the graphene sheet,
we observed the self-assembly of C4H, a novel polymer with localized aromatic hexagons, in agreement
with recent experimental findings.
This document summarizes Ryan Moodie's master's thesis on modeling the polarization behavior of photon Bose-Einstein condensates in a laser-pumped dye-filled microcavity. The model extends prior rate equation theory to include polarization by splitting photon modes into x- and y-polarized modes and introducing a molecular angular diffusion term. Numerical solutions predict multiple mode condensation and a transition from weakly to strongly polarized emission above pumping threshold. Some unusual behavior motivated further modeling, with the goal of better understanding polarization dynamics and potential hysteresis effects.
What can we learn from molecular dynamics simulations of carbon nanotube and ...Stephan Irle
The document summarizes molecular dynamics simulations of carbon nanotube and graphene growth performed by the author and collaborators. It describes how density functional tight-binding molecular dynamics simulations were used to study: [1] acetylene decomposition on iron clusters, which led to polyacetylene formation and carbon cluster attachment; [2] cap nucleation by supplying carbon atoms to an iron cluster and annealing; and [3] sidewall growth through carbon atom insertion and ring formation. The simulations provided insights into carbon nanotube growth mechanisms at an atomic scale that are difficult to observe experimentally.
Density-Functional Tight-Binding (DFTB) as fast approximate DFT method - An i...Stephan Irle
This presentation was given April 27, 2013 at Ibaraki University in Mito, Japan (Professor Seiji Mori's group). The presentation does not claim to give a complete overview of the complex field of DFTB parameterization, but rather focuses on the method's central approximations and discusses its performance in various applications.
The optimal cosmic_epoch_for_precision_cosmologySérgio Sacani
The document discusses the optimal epoch for precision cosmology measurements based on the number of independent Fourier modes available. It finds that the best constraints on the primordial power spectrum are accessible at redshifts around z=10 through instruments like 21-cm intensity mapping. The ability to constrain the initial cosmological conditions will deteriorate rapidly in our cosmic future as the exponential expansion erases information beyond 100 Hubble times from now.
This document summarizes a research project that involves building a toy model of particle collisions using C++ and ROOT. The model simulates collisions by sampling probability distributions measured in real collisions. It generates particles and assigns them properties like momentum and angle. It also models physical processes like jet production and elliptic flow. The goal is to study how properties of particles like jets are affected by a quark-gluon plasma and vice versa. The model allows tuning parameters to learn about collision interactions and switch physics processes on or off.
2014 NJP - Oscillatory solitons and time-resolved phase locking of two polari...Guilherme Tosi
This document summarizes time-resolved measurements of two polariton condensates formed in a semiconductor microcavity under nonresonant excitation. The measurements directly observe oscillatory behavior as dark or bright soliton-like waves form between the excitation spots. They also observe phase locking of the two initially independent condensates over time. These phenomena provide insights into the underlying dynamics of polariton-polariton interactions and propagation of polariton condensates.
A revised upper_limit_to_energy_extraction_from_a_kerr_black_holeSérgio Sacani
Uma nova simulação computacional feita pela NASA mostra que as partículas da matéria escura colidindo na extrema gravidade de um buraco negro pode produzir uma luz de raios-gamma forte e potencialmente observável. Detectando essa emissão forneceria aos astrônomos com uma nova ferramenta para entender tanto os buracos negros como a natureza da matéria escura, uma elusiva substância responsável pela maior parte da massa do universo que nem reflete, absorve ou emite luz.
Quantum chemical molecular dynamics simulations of graphene hydrogenationStephan Irle
Chemical adsorption of hydrogen atoms on graphite
surfaces has attracted considerable interest due to its
relevance for a broad range of areas including
plasma/fusion physics, gap tuning in graphene, and hydrogen storage. We adjusted the C-H repulsive potential of the spin-polarized self-consistent-charge density-functional tight-binding (sSCC-DFTB) method to reproduce
CCSD(T)-based relaxed potential energy curves for the
attack of atomic hydrogen on a center carbon atom of
pyrene and coronene at a tiny fraction of the computational
cost. Using this cheap quantum chemical potential, we performed direct on-the-fly Born-Oppenheimer
MD simulations while “shooting” H atoms with varying collision energies on a periodic graphene target
equilibrated at 300 Kelvin. We compared reaction cross sections for a) elastic collisions, b)
chemisorption reactions, c) penetration reactions in dependence of H/D/T kinetic energies, and found
remarkable differences to previously reported classical MD simulations of the same process. Using the
same potential, in simulations involving the shooting of up to 400 hydrogen atoms on the graphene sheet,
we observed the self-assembly of C4H, a novel polymer with localized aromatic hexagons, in agreement
with recent experimental findings.
This document summarizes Ryan Moodie's master's thesis on modeling the polarization behavior of photon Bose-Einstein condensates in a laser-pumped dye-filled microcavity. The model extends prior rate equation theory to include polarization by splitting photon modes into x- and y-polarized modes and introducing a molecular angular diffusion term. Numerical solutions predict multiple mode condensation and a transition from weakly to strongly polarized emission above pumping threshold. Some unusual behavior motivated further modeling, with the goal of better understanding polarization dynamics and potential hysteresis effects.
What can we learn from molecular dynamics simulations of carbon nanotube and ...Stephan Irle
The document summarizes molecular dynamics simulations of carbon nanotube and graphene growth performed by the author and collaborators. It describes how density functional tight-binding molecular dynamics simulations were used to study: [1] acetylene decomposition on iron clusters, which led to polyacetylene formation and carbon cluster attachment; [2] cap nucleation by supplying carbon atoms to an iron cluster and annealing; and [3] sidewall growth through carbon atom insertion and ring formation. The simulations provided insights into carbon nanotube growth mechanisms at an atomic scale that are difficult to observe experimentally.
Density-Functional Tight-Binding (DFTB) as fast approximate DFT method - An i...Stephan Irle
This presentation was given April 27, 2013 at Ibaraki University in Mito, Japan (Professor Seiji Mori's group). The presentation does not claim to give a complete overview of the complex field of DFTB parameterization, but rather focuses on the method's central approximations and discusses its performance in various applications.
Recent developments for the quantum chemical investigation of molecular syste...Stephan Irle
The structural complexity of molecular clusters increases with size due to the associated, rapidly growing configuration space. Two examples are realized in i) the transition from molecular to bulk systems, and ii) in the subsequent chemical functionalization of nanomaterials. In such systems, traditional quantum chemical approaches of investigations are hampered by the vastly increasing computational cost, even considering ever-growing supercomputer capabilities. Computationally inexpensive, yet accurate schemes such as the density-functional tight-binding (DFTB) method promise here a significant advantage.
We have recently engaged in developing novel methodologies for systems with increasing structural complexity, driven by motivation from experimental studies. In this presentation, we will briefly review a) our advances in the automatic parameterization of DFTB, and b) the Kick-fragment-based “CrazyLego” conformationally aware approach for studying molecular and ionic liquid clusters with increasing size.
This document discusses various techniques for structurally characterizing nanoparticles, including transmission electron microscopy (TEM), X-ray diffraction, and simulations. TEM can be used to obtain selected area electron diffraction patterns, high resolution TEM images, and particle assembly information. X-ray diffraction can determine particle size and distributions through peak broadening and the Scherrer equation. Both techniques along with simulations are useful for analyzing structure, orientation, defects and composition of nanoparticles.
This study measures the spatial clustering of submillimeter galaxies (SMGs) at redshifts of 1-3 using data from a submillimeter survey of galaxies in the Extended Chandra Deep Field South. The authors detect clustering between SMGs and galaxies at over 4 sigma significance. They estimate an autocorrelation length of 7.7-2.3 h-1 Mpc for SMGs, corresponding to dark matter halo masses of log(Mhalo[h-1 M⊙]) = 12.8-0.5. Based on simulations, the descendants of z=2 SMGs are expected to be massive elliptical galaxies in moderate- to high-mass groups today.
Systematic Study Multiplicity Production Nucleus – Nucleus Collisions at 4.5 ...IOSRJAP
The correlations between the multiplicity distributions and the projectile fragments, as well as the correlation between the black and grey fragments were given. We observed that the mean number of interacting projectile nucleons increases quickly as the value of heavily ionizing charged particles increase as expected but attains a more or less constant value for extreme central collisions. Finally, there is no distinct correlation between the shower particle production and the target excitation, but the average value of grey particles decreases with the increase of the number of black particles and vice versa. This correlation can also be explained by the fireball model.
Millimetre-wave emission from an intermediatemass black hole candidate in the...Sérgio Sacani
This document reports the discovery of a point-like continuum source (CO–0.40–0.22*) located near the center of a peculiar molecular cloud (CO–0.40–0.22) in the Milky Way galaxy. CO–0.40–0.22* has properties consistent with being an intermediate-mass black hole of around 105 solar masses, including its luminosity, spectrum, and ability to reproduce the kinematics of gas in simulations. This would make it one of the most promising intermediate-mass black hole candidates identified in the Milky Way to date.
The Double Chooz experiment measured the neutrino oscillation angle θ13 by observing the flux of antineutrinos produced in the Chooz nuclear power plant reactors via inverse beta decay interactions in the Double Chooz detectors. Two analyses were performed using neutron capture on gadolinium and hydrogen, giving consistent results of sin2 2θ13 = 0.109 ± 0.030 (stat) ± 0.025 (syst) and sin2 2θ13 = 0.097 ± 0.034 (stat) ± 0.034 (syst), respectively, excluding the no oscillation hypothesis at 99.8% confidence level and 2σ. The observation provides evidence for the disappearance of antineutrinos due to oscillations.
Determining a structure with electron crystallography - Overview of the paper...Joke Hadermann
The route to a solved structure (in this case Pb13Mn9O25) on the basis of precession electron diffraction, combined with HAADF-STEM, HRTEM, EELS and EDX is shown.
Summary of the paper "Solving the Structure of Li Ion Battery Materials with Precession
Electron Diffraction: Application to Li2CoPO4F"
Electron crystallography for lithium based battery materialsJoke Hadermann
This lecture was given at the IUCr (International Union of Crystallography) meeting in Madrid, 2011. Contents are focussed on the use of precession electron diffraction for functional materials, mainly lithium based battery materials, but also a perovskite was included, since a large part of the audience worked on that subject.
Solving the Structure of Li Ion Battery Materials with Precession Electron Di...Joke Hadermann
Very short summary of the paper "Solving the Structure of Li Ion Battery Materials with Precession
Electron Diffraction: Application to Li2CoPO4F", published in Chem. Mater.
Non-linear response of two dimensional crystals and layered materialsClaudio Attaccalite
Real-time simulations are a powerful tool for studying the non-linear response of solids. Second Harmonic Generation is not zero for the 1s exciton in two-dimensional hexagonal crystals like h-BN. Two-photon absorption can probe dark excitons in h-BN. Tight-binding modeling and experimental results on h-BN and MoS2 monolayers support the role of electron-hole interaction in non-linear response.
Direct space structure solution from precession electron diffraction data: Re...Joke Hadermann
The presentation shows the main points from the publication "Direct space structure solution from precession electron diffraction data: Resolving heavy and light scatterers in Pb13Mn9O25" about how thee structure of Pb13Mn9O25 was solved using transmission electron microscopy.
The current ability to test theories of gravity with black hole shadowsSérgio Sacani
Our Galactic Centre, Sagittarius A*, is believed to harbour a
supermassive black hole, as suggested by observations tracking
individual orbiting stars1,2
. Upcoming submillimetre verylong
baseline interferometry images of Sagittarius A* carried
out by the Event Horizon Telescope collaboration (EHTC)3,4
are expected to provide critical evidence for the existence of
this supermassive black hole5,6. We assess our present ability
to use EHTC images to determine whether they correspond
to a Kerr black hole as predicted by Einstein’s theory
of general relativity or to a black hole in alternative theories
of gravity. To this end, we perform general-relativistic magnetohydrodynamical
simulations and use general-relativistic
radiative-transfer calculations to generate synthetic shadow
images of a magnetized accretion flow onto a Kerr black hole.
In addition, we perform these simulations and calculations for
a dilaton black hole, which we take as a representative solution
of an alternative theory of gravity. Adopting the very-long
baseline interferometry configuration from the 2017 EHTC
campaign, we find that it could be extremely difficult to distinguish
between black holes from different theories of gravity,
thus highlighting that great caution is needed when interpreting
black hole images as tests of general relativity.
- The document discusses using 21cm forest observations to constrain properties of ultra-light dark matter particles like axions.
- 21cm forest observations can probe particle masses up to 10^-19 eV, 3 orders of magnitude higher than Lyman-alpha forest observations.
- Fisher forecast analysis suggests 21cm forest observations could probe ultra-light particle masses around 10^-20 eV and particle fraction values around 0.3.
- Ongoing work is studying effects of isocurvature fluctuations from breaking the Peccei-Quinn symmetry on 21cm forest observations.
This document describes the tight-binding method for calculating the energy diagram of nanoelectronic systems. It introduces the tight-binding method and its application to calculating the energy diagrams of polyacetylene, single-layer graphene, bilayer graphene, and multi-layer graphene. It also discusses using the tight-binding method to calculate the energy diagrams of two and four layer graphene in a constant electric field and single-layer graphene in a modulated electric field. The document provides the theoretical framework and mathematical equations for applying the tight-binding method to these different nanoscale systems.
An unindetified line_in_xray_spectra_of_the_adromeda_galaxy_and_perseus_galax...Sérgio Sacani
This document summarizes an analysis of X-ray spectra from the Andromeda galaxy and Perseus galaxy cluster observed with the XMM-Newton X-ray observatory. The analysis identified a weak unidentified line at an energy of approximately 3.5 keV in the spectra of both objects. The line strength increases towards the centers of the objects and is stronger in Perseus than in Andromeda. The line properties are consistent with originating from the decay of dark matter particles, though an instrumental or astrophysical source cannot be ruled out based on individual objects. Future detections or non-detections in additional targets could help reveal the nature of this line.
Prof Tom Trainor (University of Washington, Seattle, USA)Rene Kotze
TITLE: Two cultures in high energy nuclear physics
Since the mid eighties a community originating within the Bevalac program at the LBNL has sought to achieve formation of a color-deconfined quark-gluon plasma in heavy ion (A-A) collisions using successively higher collision energies at the AGS, SPS, RHIC and now the LHC, emphasizing a flowing dense "partonic" medium as the principal phenomenon. During much of the same period the high energy physics (HEP) community studying elementary collisions (e-e, e-p, p-p) developed the modern theory of QCD, emphasizing dijet production (fragmentation of scattered partons to observable hadrons) as the principal (calculable) phenomenon. Initially it was assumed that the QGP phenomenon in most-central A-A collisions might be distinguished from the HEP dijet phenomenon in elementary collisions. However, strong overlaps in phenomenology have revealed significant conflicts between QGP and HEP "cultures," especially at RHIC and LHC energies. In this talk I review some of the history and contrast an assortment of experimental evidence and interpretations from the two cultures with suggested conflict resolution.
The document discusses the geometry and factors involved in calculating the integrated intensity collected from single crystals, mosaic crystals, and powder samples during X-ray diffraction experiments. It describes how the integrated intensity is affected by the crystal structure, sample thickness, absorption, and factors like the Lorentz-polarization factor and multiplicity. It also discusses the differences between primary and secondary extinction effects in perfect and mosaic crystals.
1. The document discusses classical scattering theory and introduces concepts like Thomson scattering, polarization factors, and vector addition of waves when describing scattering processes.
2. It examines scattering by both single electrons and groups of electrons, defining atomic scattering factors to account for coherent scattering from whole atoms.
3. Examples and equations are provided to describe incoherent scattering processes like Compton scattering and how they contribute to the total scattering observed from materials.
Scheelite CGEW/MO for luminescence - Summary of the paperJoke Hadermann
This document summarizes a research paper that studied the incommensurate modulation and luminescence properties of CaGd2(1-x)Eu2x(MoO4)4(1-y)(WO4)4y phosphors. The researchers found that these materials exhibit incommensurate modulation of the cation ordering due to vacancies in the scheelite structure, which requires description in superspace. Replacing Mo6+ with W6+ switched the modulation from 3+2D to 3+1D, despite their similar sizes. Variations in Eu content changed luminescence intensity but not the modulation periodicity. The results contradict prior reports of simple ordered structures.
This report provides information about an Ontario Energy Board decision regarding sub-metering of electricity in rental residential properties. The decision found that existing sub-metering arrangements are unenforceable and must be unwound. It allows for sub-metering if new informed consent is obtained from tenants and energy audits are conducted. The report outlines the key elements of the decision and strategies for landlords and tenants regarding existing sub-metering agreements. It also discusses increasing fairness in sub-metering practices going forward.
Recent developments for the quantum chemical investigation of molecular syste...Stephan Irle
The structural complexity of molecular clusters increases with size due to the associated, rapidly growing configuration space. Two examples are realized in i) the transition from molecular to bulk systems, and ii) in the subsequent chemical functionalization of nanomaterials. In such systems, traditional quantum chemical approaches of investigations are hampered by the vastly increasing computational cost, even considering ever-growing supercomputer capabilities. Computationally inexpensive, yet accurate schemes such as the density-functional tight-binding (DFTB) method promise here a significant advantage.
We have recently engaged in developing novel methodologies for systems with increasing structural complexity, driven by motivation from experimental studies. In this presentation, we will briefly review a) our advances in the automatic parameterization of DFTB, and b) the Kick-fragment-based “CrazyLego” conformationally aware approach for studying molecular and ionic liquid clusters with increasing size.
This document discusses various techniques for structurally characterizing nanoparticles, including transmission electron microscopy (TEM), X-ray diffraction, and simulations. TEM can be used to obtain selected area electron diffraction patterns, high resolution TEM images, and particle assembly information. X-ray diffraction can determine particle size and distributions through peak broadening and the Scherrer equation. Both techniques along with simulations are useful for analyzing structure, orientation, defects and composition of nanoparticles.
This study measures the spatial clustering of submillimeter galaxies (SMGs) at redshifts of 1-3 using data from a submillimeter survey of galaxies in the Extended Chandra Deep Field South. The authors detect clustering between SMGs and galaxies at over 4 sigma significance. They estimate an autocorrelation length of 7.7-2.3 h-1 Mpc for SMGs, corresponding to dark matter halo masses of log(Mhalo[h-1 M⊙]) = 12.8-0.5. Based on simulations, the descendants of z=2 SMGs are expected to be massive elliptical galaxies in moderate- to high-mass groups today.
Systematic Study Multiplicity Production Nucleus – Nucleus Collisions at 4.5 ...IOSRJAP
The correlations between the multiplicity distributions and the projectile fragments, as well as the correlation between the black and grey fragments were given. We observed that the mean number of interacting projectile nucleons increases quickly as the value of heavily ionizing charged particles increase as expected but attains a more or less constant value for extreme central collisions. Finally, there is no distinct correlation between the shower particle production and the target excitation, but the average value of grey particles decreases with the increase of the number of black particles and vice versa. This correlation can also be explained by the fireball model.
Millimetre-wave emission from an intermediatemass black hole candidate in the...Sérgio Sacani
This document reports the discovery of a point-like continuum source (CO–0.40–0.22*) located near the center of a peculiar molecular cloud (CO–0.40–0.22) in the Milky Way galaxy. CO–0.40–0.22* has properties consistent with being an intermediate-mass black hole of around 105 solar masses, including its luminosity, spectrum, and ability to reproduce the kinematics of gas in simulations. This would make it one of the most promising intermediate-mass black hole candidates identified in the Milky Way to date.
The Double Chooz experiment measured the neutrino oscillation angle θ13 by observing the flux of antineutrinos produced in the Chooz nuclear power plant reactors via inverse beta decay interactions in the Double Chooz detectors. Two analyses were performed using neutron capture on gadolinium and hydrogen, giving consistent results of sin2 2θ13 = 0.109 ± 0.030 (stat) ± 0.025 (syst) and sin2 2θ13 = 0.097 ± 0.034 (stat) ± 0.034 (syst), respectively, excluding the no oscillation hypothesis at 99.8% confidence level and 2σ. The observation provides evidence for the disappearance of antineutrinos due to oscillations.
Determining a structure with electron crystallography - Overview of the paper...Joke Hadermann
The route to a solved structure (in this case Pb13Mn9O25) on the basis of precession electron diffraction, combined with HAADF-STEM, HRTEM, EELS and EDX is shown.
Summary of the paper "Solving the Structure of Li Ion Battery Materials with Precession
Electron Diffraction: Application to Li2CoPO4F"
Electron crystallography for lithium based battery materialsJoke Hadermann
This lecture was given at the IUCr (International Union of Crystallography) meeting in Madrid, 2011. Contents are focussed on the use of precession electron diffraction for functional materials, mainly lithium based battery materials, but also a perovskite was included, since a large part of the audience worked on that subject.
Solving the Structure of Li Ion Battery Materials with Precession Electron Di...Joke Hadermann
Very short summary of the paper "Solving the Structure of Li Ion Battery Materials with Precession
Electron Diffraction: Application to Li2CoPO4F", published in Chem. Mater.
Non-linear response of two dimensional crystals and layered materialsClaudio Attaccalite
Real-time simulations are a powerful tool for studying the non-linear response of solids. Second Harmonic Generation is not zero for the 1s exciton in two-dimensional hexagonal crystals like h-BN. Two-photon absorption can probe dark excitons in h-BN. Tight-binding modeling and experimental results on h-BN and MoS2 monolayers support the role of electron-hole interaction in non-linear response.
Direct space structure solution from precession electron diffraction data: Re...Joke Hadermann
The presentation shows the main points from the publication "Direct space structure solution from precession electron diffraction data: Resolving heavy and light scatterers in Pb13Mn9O25" about how thee structure of Pb13Mn9O25 was solved using transmission electron microscopy.
The current ability to test theories of gravity with black hole shadowsSérgio Sacani
Our Galactic Centre, Sagittarius A*, is believed to harbour a
supermassive black hole, as suggested by observations tracking
individual orbiting stars1,2
. Upcoming submillimetre verylong
baseline interferometry images of Sagittarius A* carried
out by the Event Horizon Telescope collaboration (EHTC)3,4
are expected to provide critical evidence for the existence of
this supermassive black hole5,6. We assess our present ability
to use EHTC images to determine whether they correspond
to a Kerr black hole as predicted by Einstein’s theory
of general relativity or to a black hole in alternative theories
of gravity. To this end, we perform general-relativistic magnetohydrodynamical
simulations and use general-relativistic
radiative-transfer calculations to generate synthetic shadow
images of a magnetized accretion flow onto a Kerr black hole.
In addition, we perform these simulations and calculations for
a dilaton black hole, which we take as a representative solution
of an alternative theory of gravity. Adopting the very-long
baseline interferometry configuration from the 2017 EHTC
campaign, we find that it could be extremely difficult to distinguish
between black holes from different theories of gravity,
thus highlighting that great caution is needed when interpreting
black hole images as tests of general relativity.
- The document discusses using 21cm forest observations to constrain properties of ultra-light dark matter particles like axions.
- 21cm forest observations can probe particle masses up to 10^-19 eV, 3 orders of magnitude higher than Lyman-alpha forest observations.
- Fisher forecast analysis suggests 21cm forest observations could probe ultra-light particle masses around 10^-20 eV and particle fraction values around 0.3.
- Ongoing work is studying effects of isocurvature fluctuations from breaking the Peccei-Quinn symmetry on 21cm forest observations.
This document describes the tight-binding method for calculating the energy diagram of nanoelectronic systems. It introduces the tight-binding method and its application to calculating the energy diagrams of polyacetylene, single-layer graphene, bilayer graphene, and multi-layer graphene. It also discusses using the tight-binding method to calculate the energy diagrams of two and four layer graphene in a constant electric field and single-layer graphene in a modulated electric field. The document provides the theoretical framework and mathematical equations for applying the tight-binding method to these different nanoscale systems.
An unindetified line_in_xray_spectra_of_the_adromeda_galaxy_and_perseus_galax...Sérgio Sacani
This document summarizes an analysis of X-ray spectra from the Andromeda galaxy and Perseus galaxy cluster observed with the XMM-Newton X-ray observatory. The analysis identified a weak unidentified line at an energy of approximately 3.5 keV in the spectra of both objects. The line strength increases towards the centers of the objects and is stronger in Perseus than in Andromeda. The line properties are consistent with originating from the decay of dark matter particles, though an instrumental or astrophysical source cannot be ruled out based on individual objects. Future detections or non-detections in additional targets could help reveal the nature of this line.
Prof Tom Trainor (University of Washington, Seattle, USA)Rene Kotze
TITLE: Two cultures in high energy nuclear physics
Since the mid eighties a community originating within the Bevalac program at the LBNL has sought to achieve formation of a color-deconfined quark-gluon plasma in heavy ion (A-A) collisions using successively higher collision energies at the AGS, SPS, RHIC and now the LHC, emphasizing a flowing dense "partonic" medium as the principal phenomenon. During much of the same period the high energy physics (HEP) community studying elementary collisions (e-e, e-p, p-p) developed the modern theory of QCD, emphasizing dijet production (fragmentation of scattered partons to observable hadrons) as the principal (calculable) phenomenon. Initially it was assumed that the QGP phenomenon in most-central A-A collisions might be distinguished from the HEP dijet phenomenon in elementary collisions. However, strong overlaps in phenomenology have revealed significant conflicts between QGP and HEP "cultures," especially at RHIC and LHC energies. In this talk I review some of the history and contrast an assortment of experimental evidence and interpretations from the two cultures with suggested conflict resolution.
The document discusses the geometry and factors involved in calculating the integrated intensity collected from single crystals, mosaic crystals, and powder samples during X-ray diffraction experiments. It describes how the integrated intensity is affected by the crystal structure, sample thickness, absorption, and factors like the Lorentz-polarization factor and multiplicity. It also discusses the differences between primary and secondary extinction effects in perfect and mosaic crystals.
1. The document discusses classical scattering theory and introduces concepts like Thomson scattering, polarization factors, and vector addition of waves when describing scattering processes.
2. It examines scattering by both single electrons and groups of electrons, defining atomic scattering factors to account for coherent scattering from whole atoms.
3. Examples and equations are provided to describe incoherent scattering processes like Compton scattering and how they contribute to the total scattering observed from materials.
Scheelite CGEW/MO for luminescence - Summary of the paperJoke Hadermann
This document summarizes a research paper that studied the incommensurate modulation and luminescence properties of CaGd2(1-x)Eu2x(MoO4)4(1-y)(WO4)4y phosphors. The researchers found that these materials exhibit incommensurate modulation of the cation ordering due to vacancies in the scheelite structure, which requires description in superspace. Replacing Mo6+ with W6+ switched the modulation from 3+2D to 3+1D, despite their similar sizes. Variations in Eu content changed luminescence intensity but not the modulation periodicity. The results contradict prior reports of simple ordered structures.
This report provides information about an Ontario Energy Board decision regarding sub-metering of electricity in rental residential properties. The decision found that existing sub-metering arrangements are unenforceable and must be unwound. It allows for sub-metering if new informed consent is obtained from tenants and energy audits are conducted. The report outlines the key elements of the decision and strategies for landlords and tenants regarding existing sub-metering agreements. It also discusses increasing fairness in sub-metering practices going forward.
La Web 1.0 permitía solo lectura de información centralizada y poco actualizada, mientras que la Web 2.0 facilita la interacción y colaboración entre usuarios a través de herramientas como blogs, wikis, redes sociales y YouTube, donde los usuarios comparten y crean contenido de forma dinámica.
Los últimos trabajos de medición y oscultación relativos al estado de la vía, en el tramo sin renovar entre Calp y Dénia, han obligado a FGV a reducir la velocidad de paso en diferentes puntos entre ambas estaciones, hasta que se acometan las renovaciones previstas, que siguen su normal ritmo de planificaciones, licitaciones, adjudicaciones y ejecución de obras. Consulte el nuevo horario.
Yiya Murano poisoned Carmen del Giorgio de Venturini and Lelia Formisano de Ayala by inviting them over for tea and biscuits laced with poison. She did so in an attempt to steal their money by promising to double their investment. However, her plan was foiled when Carmen and Lelia's daughter, Sarah, discovered their bodies and identified Yiya as the culprit. Yiya then attempted to kill Sarah before she could call the police, but was caught.
La primera plataforma de publicación de contenidos audiovisuales móvil y web, con conversión automática de formatos y funcionalidades 2.0. Podemos crear un canal de TV para móvil, o para móvil e internet, etc.
Proyecto de Expresión Oral y Escrita - Mr. MercedesSaritaLoyola72
Este documento resume el primer capítulo del libro "Mr. Mercedes" de Stephen King. Narra la historia de un hombre obsesionado que robó un Mercedes y atropelló a varias personas haciendo fila para un trabajo, matando a 8 e hiriendo a 15. Un policía retirado llamado William Hodges, que no pudo resolver el caso, recibe una carta del supuesto asesino desafiándolo. Hodges decide investigar para atraparlo y así darle sentido nuevamente a su vida.
Presentación de Fernando Moroy, director de Relaciones Institucionales de La Caixa D.T Madrid, Vicepresidente en España de la Red de Business Angels Keiretsu y Profesor de EOI
El documento describe el Sistema de Información Virtual sobre Personas Mayores, una iniciativa del Instituto de Mayores y Servicios Sociales (IMSERSO) y el Consejo Superior de Investigaciones Científicas (CSIC). El sistema proporciona información gratuita y de libre acceso dirigida al mundo académico, profesionales de servicios sociales y la sociedad en general, con contenido sobre envejecimiento, atención a la dependencia, legislación, investigación y recursos sociales. El sistema sigue estándares de accesibilidad, us
Nominations for 2016 Philippines Property Awards UnderwayKMC Savills, Inc.
Come April 7, 2016, the shape of the real estate industry in the Philippines and how has dramatically changed, will hog the spotlight when the Philippines Property Awards announce a plethora of big winners in the fourth consecutive year that Ensign Media organized the event. KMC MAG Group's Michael McCullough will be one of the judges at this year's event.
ARC International provides multimedia solutions and intellectual property to consumer electronics companies globally to improve the audio and video experience on electronic devices. In 2008, ARC grew revenues driven by higher royalty payments from new customers, but remained cautious due to economic uncertainty. ARC strengthened its portfolio through acquisitions, broadened its target markets, and restructured operations to lower costs and accelerate transition to profitability.
This document provides information on apartment rental properties in Dunwoody, Sandy Springs, Stone Mountain, and Tucker, Georgia that offer discounts to employees of local hospitals. It lists individual apartment communities with contact details and brief descriptions. It also includes instructions on how to use the directory and receive discounts by presenting a printable coupon. The directory is provided for hospital employees to search for affordable rental housing near their place of work.
Este documento proporciona información sobre las marcas comerciales y los derechos de autor relacionados con Dreamweaver y otras aplicaciones de Macromedia. También incluye enlaces a sitios web de terceros y avisos legales de Apple y Opera. El documento contiene agradecimientos al equipo que trabajó en Dreamweaver.
Este documento describe el uso de la plataforma de aprendizaje Moodle en el Departamento de Salud de la Ribera en Valencia, España. Se ha definido un procedimiento de formación e-learning y una serie de indicadores para evaluar la calidad. El procedimiento incluye fases de análisis de necesidades, diseño, desarrollo de materiales, implementación y evaluación. Los indicadores miden factores pedagógicos, organizativos y técnicos para supervisar la calidad de las acciones formativas.
This document is a resume for Nycole-Lanyse Jacques summarizing her professional experience and education. She has over 6 years of customer service experience in business administration and hospitality. Her experience includes managing customer relationships and providing excellent customer service at several restaurant and hospitality jobs. She also has experience in administrative support and has skills in Microsoft Office, data entry, and point of sale systems. She has an Associate's degree from George Mason University with credits towards a Bachelor's degree in Nursing or Government and International Politics.
The document describes an LED office light called the CLSeries that is available in 30W, 40W, and 50W models. It has a proprietary diffuser system that widens the beam angle and provides glare-free, uniform lighting. The light is lightweight and made of impact-proof, fire-retardant materials. It also has smart circuitry protection against overheating, overvoltage, and overcurrent situations. The advance light engine uses a high-efficiency MCPCB and LED chips for low heat and long lifespan.
The Lovie Awards and Google present The Lovie Talkslovieawards
Lovie Talks is our unique view into the ever-changing landscape of what's happening online, designed to provoke and inspire by highlighting some of the most innovative work and trends on the Internet
This document lists participants and the program committee for the ICT Forum 2012 & SPI Biz Conference. The conference will take place from October 2-4, 2012 in Nis, Serbia and will include sessions on managing security and business continuity, building question answering systems, intelligent search systems, mobile e-learning, social networks, Twitter support for business, electronic communication promotion, and occupational training. The conference is co-organized by the Regional Chamber of Commerce Nis and co-financed by the EU through the Bulgaria-Serbia IPA Cross-Border Programme.
Essential information on moving from Metastorm BPM to the latest OpenText MBPM platform.Organisations currently on Metastorm BPM version v7 or earlier have a limited period to move their platforms to OpenText MBPM v9 before support ends.
The distribution and_annihilation_of_dark_matter_around_black_holesSérgio Sacani
Uma nova simulação computacional feita pela NASA mostra que as partículas da matéria escura colidindo na extrema gravidade de um buraco negro pode produzir uma luz de raios-gamma forte e potencialmente observável. Detectando essa emissão forneceria aos astrônomos com uma nova ferramenta para entender tanto os buracos negros como a natureza da matéria escura, uma elusiva substância responsável pela maior parte da massa do universo que nem reflete, absorve ou emite luz.
In search of multipath interference using large moleculesGabriel O'Brien
This document summarizes an experiment that tested the quantum mechanical principle of superposition using large dye molecules. The experiment measured interference patterns when the molecules passed through single, double, and triple slits. It observed less than 1% deviation from the expected interference patterns based on quantum mechanics, providing evidence that the superposition principle applies even to massive particles like these large molecules. The experiment is one of the first to directly observe quantum interference using massive particles rather than light or single particles.
This document summarizes the use of positron annihilation techniques to study semiconductors and lattice defects. Positrons emitted from radioactive nuclei can be used to probe vacancy-type defects in materials. When a positron encounters an electron, they annihilate and emit gamma rays. By analyzing properties of the gamma rays like energy, momentum, and timing, information can be gained about the defect where annihilation occurred, allowing quantification of defect types, concentrations, and charge states in semiconductors. Common positron annihilation techniques described include positron lifetime spectroscopy and Doppler broadening spectroscopy.
This document numerically analyzes the wave function of atoms under the combined effects of an optical lattice trapping potential and a harmonic oscillator potential, as used in Bose-Einstein condensation experiments. It employs the Crank-Nicolson scheme to solve the Gross-Pitaevskii equation. The results show that the wave function distribution responds to parameters like the trapping frequencies ratio, optical lattice intensity, chemical potential, and energy. Careful adjustment of the time step and grid spacing is needed to satisfy conservation of norms and energy as required by the physical system. Distributions of the overlapping potentials for different q-factors are presented.
This document summarizes a study investigating how the temperature changes when atoms loaded into an optical lattice are adiabatically ramped from a superfluid phase to a Mott insulating phase. The researchers calculate the entropy of the single-band Bose-Hubbard model for various densities, interaction strengths, temperatures, and dimensions using quantum Monte Carlo simulations. Their results support the view that current cold atom experiments remain in the quantum regime for all lattice depths with low temperatures and minimal heating during the ramping process.
Laser Pulsing in Linear Compton ScatteringTodd Hodges
This document summarizes a method for calculating the energy spectrum of radiation produced in linear Compton scattering, accounting for the pulsed structure of the incident laser beam. The method involves performing a Lorentz transformation of the Klein-Nishina scattering cross section to calculate the emission from individual electrons in an electron beam, and then summing over all electrons to obtain the total energy spectrum. This approach allows for accurate modeling of effects of electron beam energy spread and emittance. The method is then applied to predict the photon spectrum from a proposed compact inverse Compton scattering x-ray source at Old Dominion University.
The document discusses the Compton effect, which describes the scattering of photons by charged particles like electrons. It provides the mathematical description using conservation of energy and momentum. The Compton effect leads to a shift in the wavelength of scattered photons. Practical applications of the Compton effect include Compton scatter densitometry to measure electron density, Compton scatter imaging for 3D electron density mapping, and Compton profile analysis to characterize materials.
This poster outlines searches by the CMS Collaboration for three beyond-standard-model candidates: Z' bosons from E6 and sequential standard models, and large extra dimensions. Events with two taus decaying to an electron and muon are selected to exploit the cleanest decay channel while mitigating large standard model backgrounds. No significant excesses are observed in the visible mass distribution, allowing lower mass limits to be set excluding Z' masses below 1.1-1.4 TeV and scales of large extra dimensions below 1.6-4.4 TeV depending on the model.
1) DUNE aims to resolve the matter-antimatter asymmetry by searching for neutron-antineutron oscillations, a baryon number violating process.
2) Simulations of atmospheric neutrino backgrounds that could mimic the signal are underway using GENIE to determine the viability of detecting oscillations above background levels.
3) If viable, the analysis will consider effects of cosmogenic muons and fast neutrons, with generators for neutron-antineutron interactions in argon under construction.
This document describes the ATTA (Atom Trap Trace Analysis) experiment which aims to precisely measure trace amounts of krypton isotopes in liquid xenon. ATTA uses laser cooling and trapping techniques to isolate and count individual atoms. The document outlines the ATTA system, which involves exciting atoms to a metastable state using a plasma source, slowing and collimating atoms using optical molasses and Zeeman slowing, and finally trapping atoms using magneto-optical traps. Precisely measuring krypton contamination levels in xenon is important for the larger XENON dark matter detection experiment to understand background signals and increase sensitivity to detect weakly interacting massive particles (WIMPs).
Electronic properties of nanostructured quantum dotsAlexander Decker
1. The document discusses electronic properties of nanostructured quantum dots, specifically analyzing their properties through simulation results.
2. Quantum dots confine the motion of electrons in all three dimensions, giving them discrete energy levels similar to atoms. Their small size means quantum effects are prominent.
3. The simulations show that the optical and electronic characteristics of different quantum dot nanostructures are similar for a given boundary condition.
11.electronic properties of nanostructured quantum dotsAlexander Decker
This document analyzes the electronic properties of quantum dots through simulation. It discusses how quantum dots confine the movement of electrons in three dimensions, giving them discrete energy levels similar to atoms. The size and shape of quantum dots can be engineered to control their optical and electronic properties. Simulation results showed that quantum dot characteristics were equivalent for different nanostructures under the same boundary conditions. In conclusion, the document examines how quantum dots can be used in applications like lasers, sensors, and quantum computing.
Poster of my master\'s research presented at the Physics@FOM conference at Veldhoven on 20 januari 2010. There\'s one error in the equations, can you find it?
Dark Matter Annihilation inside Large-Volume Neutrino DetectorsSérgio Sacani
New particles in theories beyond the standard model can manifest as stable relics that interact strongly with visible matter and make up a small fraction of the total dark matter abundance. Such particles represent an interesting physics target since they can evade existing bounds from direct detection due to their rapid thermalization in high-density environments. In this work we point out that their annihilation to visible matter inside large-volume neutrino telescopes can provide a new way to constrain or discover such particles. The signal is the most pronounced for relic masses in the GeV range, and can be efficiently constrained by existing Super-Kamiokande searches for dinucleon annihilation. We also provide an explicit realization of this scenario in the form of secluded dark matter coupled to a dark photon, and we show that the present method implies novel and stringent bounds on the model that are complementary to direct constraints from beam dumps, colliders, and direct detection experiments.
This document provides an overview of dimuon analyses at the LHC and discusses big data challenges. It outlines the Standard Model and motivations for new physics searches. The CMS detector is described, focusing on muon reconstruction challenges. Data selection and efficiency measurements are discussed. The analysis philosophy of searching for a narrow resonance over the Drell-Yan continuum is presented.
This document provides an introduction to lasers and their applications. It begins with recommended textbooks on the subject, then provides a chart showing the laser spectrum and examples of different laser types and their wavelengths. The remainder of the document discusses the basic components and functioning of lasers, including the gain medium that provides stimulated emission, the pump source to create population inversion, and the optical cavity formed by mirrors. It also provides brief histories of the development of masers and the first ruby laser.
This document provides an introduction to lasers and their applications. It begins with recommended textbooks on the subject, then provides a chart showing the laser spectrum and examples of different laser types and their wavelengths. The remainder of the document discusses the basic components and functioning of lasers, including the gain medium that provides stimulated emission, the pump source to create population inversion, and the optical cavity formed by mirrors. It also provides brief histories of the development of masers and the first ruby laser.
Fundamental principle of information to-energy conversion.Fausto Intilla
Abstract. - The equivalence of 1 bit of information to entropy was given by Landauer in 1961 as kln2, k the Boltzmann constant. Erasing information implies heat dissipation and the energy of 1 bit would then be (the
Landauer´s limit) kT ln 2, T being the ambient temperature. From a quantum-cosmological point of view the minimum quantum of energy in the universe corresponds today to a temperature of 10^-29 ºK, probably forming a cosmic background of a Bose condensate [1]. Then, the bit with minimum energy today in the Universe is a quantum of energy 10^-45 ergs, with an equivalent mass of 10^-66 g. Low temperature implies low energy per bit and, of course, this is the way for faster and less energy dissipating computing devices. Our conjecture is this: the possibility of a future access to the CBBC (a coupling/channeling?) would mean a huge
jump in the performance of these devices.
Precision determination of the small-x gluon from charm production at LHCbjuanrojochacon
This document discusses using LHCb data on charm production to constrain the small-x gluon and improve predictions for neutrino fluxes. LHCb data at 7 TeV, 5 TeV and 13 TeV provides stringent constraints on the small-x gluon beyond HERA. This improved gluon allows more accurate predictions for signals and backgrounds at neutrino telescopes. At a 100 TeV collider, inclusive cross sections depend directly on small-x PDFs, but using LHCb data leads to stabilized predictions with reduced uncertainties.
Similar to Search for microscopic black hole signatures at the large hadron collider (20)
SDSS1335+0728: The awakening of a ∼ 106M⊙ black hole⋆Sérgio Sacani
Context. The early-type galaxy SDSS J133519.91+072807.4 (hereafter SDSS1335+0728), which had exhibited no prior optical variations during the preceding two decades, began showing significant nuclear variability in the Zwicky Transient Facility (ZTF) alert stream from December 2019 (as ZTF19acnskyy). This variability behaviour, coupled with the host-galaxy properties, suggests that SDSS1335+0728 hosts a ∼ 106M⊙ black hole (BH) that is currently in the process of ‘turning on’. Aims. We present a multi-wavelength photometric analysis and spectroscopic follow-up performed with the aim of better understanding the origin of the nuclear variations detected in SDSS1335+0728. Methods. We used archival photometry (from WISE, 2MASS, SDSS, GALEX, eROSITA) and spectroscopic data (from SDSS and LAMOST) to study the state of SDSS1335+0728 prior to December 2019, and new observations from Swift, SOAR/Goodman, VLT/X-shooter, and Keck/LRIS taken after its turn-on to characterise its current state. We analysed the variability of SDSS1335+0728 in the X-ray/UV/optical/mid-infrared range, modelled its spectral energy distribution prior to and after December 2019, and studied the evolution of its UV/optical spectra. Results. From our multi-wavelength photometric analysis, we find that: (a) since 2021, the UV flux (from Swift/UVOT observations) is four times brighter than the flux reported by GALEX in 2004; (b) since June 2022, the mid-infrared flux has risen more than two times, and the W1−W2 WISE colour has become redder; and (c) since February 2024, the source has begun showing X-ray emission. From our spectroscopic follow-up, we see that (i) the narrow emission line ratios are now consistent with a more energetic ionising continuum; (ii) broad emission lines are not detected; and (iii) the [OIII] line increased its flux ∼ 3.6 years after the first ZTF alert, which implies a relatively compact narrow-line-emitting region. Conclusions. We conclude that the variations observed in SDSS1335+0728 could be either explained by a ∼ 106M⊙ AGN that is just turning on or by an exotic tidal disruption event (TDE). If the former is true, SDSS1335+0728 is one of the strongest cases of an AGNobserved in the process of activating. If the latter were found to be the case, it would correspond to the longest and faintest TDE ever observed (or another class of still unknown nuclear transient). Future observations of SDSS1335+0728 are crucial to further understand its behaviour. Key words. galaxies: active– accretion, accretion discs– galaxies: individual: SDSS J133519.91+072807.4
Discovery of An Apparent Red, High-Velocity Type Ia Supernova at 𝐳 = 2.9 wi...Sérgio Sacani
We present the JWST discovery of SN 2023adsy, a transient object located in a host galaxy JADES-GS
+
53.13485
−
27.82088
with a host spectroscopic redshift of
2.903
±
0.007
. The transient was identified in deep James Webb Space Telescope (JWST)/NIRCam imaging from the JWST Advanced Deep Extragalactic Survey (JADES) program. Photometric and spectroscopic followup with NIRCam and NIRSpec, respectively, confirm the redshift and yield UV-NIR light-curve, NIR color, and spectroscopic information all consistent with a Type Ia classification. Despite its classification as a likely SN Ia, SN 2023adsy is both fairly red (
�
(
�
−
�
)
∼
0.9
) despite a host galaxy with low-extinction and has a high Ca II velocity (
19
,
000
±
2
,
000
km/s) compared to the general population of SNe Ia. While these characteristics are consistent with some Ca-rich SNe Ia, particularly SN 2016hnk, SN 2023adsy is intrinsically brighter than the low-
�
Ca-rich population. Although such an object is too red for any low-
�
cosmological sample, we apply a fiducial standardization approach to SN 2023adsy and find that the SN 2023adsy luminosity distance measurement is in excellent agreement (
≲
1
�
) with
Λ
CDM. Therefore unlike low-
�
Ca-rich SNe Ia, SN 2023adsy is standardizable and gives no indication that SN Ia standardized luminosities change significantly with redshift. A larger sample of distant SNe Ia is required to determine if SN Ia population characteristics at high-
�
truly diverge from their low-
�
counterparts, and to confirm that standardized luminosities nevertheless remain constant with redshift.
Evidence of Jet Activity from the Secondary Black Hole in the OJ 287 Binary S...Sérgio Sacani
Wereport the study of a huge optical intraday flare on 2021 November 12 at 2 a.m. UT in the blazar OJ287. In the binary black hole model, it is associated with an impact of the secondary black hole on the accretion disk of the primary. Our multifrequency observing campaign was set up to search for such a signature of the impact based on a prediction made 8 yr earlier. The first I-band results of the flare have already been reported by Kishore et al. (2024). Here we combine these data with our monitoring in the R-band. There is a big change in the R–I spectral index by 1.0 ±0.1 between the normal background and the flare, suggesting a new component of radiation. The polarization variation during the rise of the flare suggests the same. The limits on the source size place it most reasonably in the jet of the secondary BH. We then ask why we have not seen this phenomenon before. We show that OJ287 was never before observed with sufficient sensitivity on the night when the flare should have happened according to the binary model. We also study the probability that this flare is just an oversized example of intraday variability using the Krakow data set of intense monitoring between 2015 and 2023. We find that the occurrence of a flare of this size and rapidity is unlikely. In machine-readable Tables 1 and 2, we give the full orbit-linked historical light curve of OJ287 as well as the dense monitoring sample of Krakow.
Candidate young stellar objects in the S-cluster: Kinematic analysis of a sub...Sérgio Sacani
Context. The observation of several L-band emission sources in the S cluster has led to a rich discussion of their nature. However, a definitive answer to the classification of the dusty objects requires an explanation for the detection of compact Doppler-shifted Brγ emission. The ionized hydrogen in combination with the observation of mid-infrared L-band continuum emission suggests that most of these sources are embedded in a dusty envelope. These embedded sources are part of the S-cluster, and their relationship to the S-stars is still under debate. To date, the question of the origin of these two populations has been vague, although all explanations favor migration processes for the individual cluster members. Aims. This work revisits the S-cluster and its dusty members orbiting the supermassive black hole SgrA* on bound Keplerian orbits from a kinematic perspective. The aim is to explore the Keplerian parameters for patterns that might imply a nonrandom distribution of the sample. Additionally, various analytical aspects are considered to address the nature of the dusty sources. Methods. Based on the photometric analysis, we estimated the individual H−K and K−L colors for the source sample and compared the results to known cluster members. The classification revealed a noticeable contrast between the S-stars and the dusty sources. To fit the flux-density distribution, we utilized the radiative transfer code HYPERION and implemented a young stellar object Class I model. We obtained the position angle from the Keplerian fit results; additionally, we analyzed the distribution of the inclinations and the longitudes of the ascending node. Results. The colors of the dusty sources suggest a stellar nature consistent with the spectral energy distribution in the near and midinfrared domains. Furthermore, the evaporation timescales of dusty and gaseous clumps in the vicinity of SgrA* are much shorter ( 2yr) than the epochs covered by the observations (≈15yr). In addition to the strong evidence for the stellar classification of the D-sources, we also find a clear disk-like pattern following the arrangements of S-stars proposed in the literature. Furthermore, we find a global intrinsic inclination for all dusty sources of 60 ± 20◦, implying a common formation process. Conclusions. The pattern of the dusty sources manifested in the distribution of the position angles, inclinations, and longitudes of the ascending node strongly suggests two different scenarios: the main-sequence stars and the dusty stellar S-cluster sources share a common formation history or migrated with a similar formation channel in the vicinity of SgrA*. Alternatively, the gravitational influence of SgrA* in combination with a massive perturber, such as a putative intermediate mass black hole in the IRS 13 cluster, forces the dusty objects and S-stars to follow a particular orbital arrangement. Key words. stars: black holes– stars: formation– Galaxy: center– galaxies: star formation
JAMES WEBB STUDY THE MASSIVE BLACK HOLE SEEDSSérgio Sacani
The pathway(s) to seeding the massive black holes (MBHs) that exist at the heart of galaxies in the present and distant Universe remains an unsolved problem. Here we categorise, describe and quantitatively discuss the formation pathways of both light and heavy seeds. We emphasise that the most recent computational models suggest that rather than a bimodal-like mass spectrum between light and heavy seeds with light at one end and heavy at the other that instead a continuum exists. Light seeds being more ubiquitous and the heavier seeds becoming less and less abundant due the rarer environmental conditions required for their formation. We therefore examine the different mechanisms that give rise to different seed mass spectrums. We show how and why the mechanisms that produce the heaviest seeds are also among the rarest events in the Universe and are hence extremely unlikely to be the seeds for the vast majority of the MBH population. We quantify, within the limits of the current large uncertainties in the seeding processes, the expected number densities of the seed mass spectrum. We argue that light seeds must be at least 103 to 105 times more numerous than heavy seeds to explain the MBH population as a whole. Based on our current understanding of the seed population this makes heavy seeds (Mseed > 103 M⊙) a significantly more likely pathway given that heavy seeds have an abundance pattern than is close to and likely in excess of 10−4 compared to light seeds. Finally, we examine the current state-of-the-art in numerical calculations and recent observations and plot a path forward for near-future advances in both domains.
Anti-Universe And Emergent Gravity and the Dark UniverseSérgio Sacani
Recent theoretical progress indicates that spacetime and gravity emerge together from the entanglement structure of an underlying microscopic theory. These ideas are best understood in Anti-de Sitter space, where they rely on the area law for entanglement entropy. The extension to de Sitter space requires taking into account the entropy and temperature associated with the cosmological horizon. Using insights from string theory, black hole physics and quantum information theory we argue that the positive dark energy leads to a thermal volume law contribution to the entropy that overtakes the area law precisely at the cosmological horizon. Due to the competition between area and volume law entanglement the microscopic de Sitter states do not thermalise at sub-Hubble scales: they exhibit memory effects in the form of an entropy displacement caused by matter. The emergent laws of gravity contain an additional ‘dark’ gravitational force describing the ‘elastic’ response due to the entropy displacement. We derive an estimate of the strength of this extra force in terms of the baryonic mass, Newton’s constant and the Hubble acceleration scale a0 = cH0, and provide evidence for the fact that this additional ‘dark gravity force’ explains the observed phenomena in galaxies and clusters currently attributed to dark matter.
The binding of cosmological structures by massless topological defectsSérgio Sacani
Assuming spherical symmetry and weak field, it is shown that if one solves the Poisson equation or the Einstein field
equations sourced by a topological defect, i.e. a singularity of a very specific form, the result is a localized gravitational
field capable of driving flat rotation (i.e. Keplerian circular orbits at a constant speed for all radii) of test masses on a thin
spherical shell without any underlying mass. Moreover, a large-scale structure which exploits this solution by assembling
concentrically a number of such topological defects can establish a flat stellar or galactic rotation curve, and can also deflect
light in the same manner as an equipotential (isothermal) sphere. Thus, the need for dark matter or modified gravity theory is
mitigated, at least in part.
EWOCS-I: The catalog of X-ray sources in Westerlund 1 from the Extended Weste...Sérgio Sacani
Context. With a mass exceeding several 104 M⊙ and a rich and dense population of massive stars, supermassive young star clusters
represent the most massive star-forming environment that is dominated by the feedback from massive stars and gravitational interactions
among stars.
Aims. In this paper we present the Extended Westerlund 1 and 2 Open Clusters Survey (EWOCS) project, which aims to investigate
the influence of the starburst environment on the formation of stars and planets, and on the evolution of both low and high mass stars.
The primary targets of this project are Westerlund 1 and 2, the closest supermassive star clusters to the Sun.
Methods. The project is based primarily on recent observations conducted with the Chandra and JWST observatories. Specifically,
the Chandra survey of Westerlund 1 consists of 36 new ACIS-I observations, nearly co-pointed, for a total exposure time of 1 Msec.
Additionally, we included 8 archival Chandra/ACIS-S observations. This paper presents the resulting catalog of X-ray sources within
and around Westerlund 1. Sources were detected by combining various existing methods, and photon extraction and source validation
were carried out using the ACIS-Extract software.
Results. The EWOCS X-ray catalog comprises 5963 validated sources out of the 9420 initially provided to ACIS-Extract, reaching a
photon flux threshold of approximately 2 × 10−8 photons cm−2
s
−1
. The X-ray sources exhibit a highly concentrated spatial distribution,
with 1075 sources located within the central 1 arcmin. We have successfully detected X-ray emissions from 126 out of the 166 known
massive stars of the cluster, and we have collected over 71 000 photons from the magnetar CXO J164710.20-455217.
The debris of the ‘last major merger’ is dynamically youngSérgio Sacani
The Milky Way’s (MW) inner stellar halo contains an [Fe/H]-rich component with highly eccentric orbits, often referred to as the
‘last major merger.’ Hypotheses for the origin of this component include Gaia-Sausage/Enceladus (GSE), where the progenitor
collided with the MW proto-disc 8–11 Gyr ago, and the Virgo Radial Merger (VRM), where the progenitor collided with the
MW disc within the last 3 Gyr. These two scenarios make different predictions about observable structure in local phase space,
because the morphology of debris depends on how long it has had to phase mix. The recently identified phase-space folds in Gaia
DR3 have positive caustic velocities, making them fundamentally different than the phase-mixed chevrons found in simulations
at late times. Roughly 20 per cent of the stars in the prograde local stellar halo are associated with the observed caustics. Based
on a simple phase-mixing model, the observed number of caustics are consistent with a merger that occurred 1–2 Gyr ago.
We also compare the observed phase-space distribution to FIRE-2 Latte simulations of GSE-like mergers, using a quantitative
measurement of phase mixing (2D causticality). The observed local phase-space distribution best matches the simulated data
1–2 Gyr after collision, and certainly not later than 3 Gyr. This is further evidence that the progenitor of the ‘last major merger’
did not collide with the MW proto-disc at early times, as is thought for the GSE, but instead collided with the MW disc within
the last few Gyr, consistent with the body of work surrounding the VRM.
Observation of Io’s Resurfacing via Plume Deposition Using Ground-based Adapt...Sérgio Sacani
Since volcanic activity was first discovered on Io from Voyager images in 1979, changes
on Io’s surface have been monitored from both spacecraft and ground-based telescopes.
Here, we present the highest spatial resolution images of Io ever obtained from a groundbased telescope. These images, acquired by the SHARK-VIS instrument on the Large
Binocular Telescope, show evidence of a major resurfacing event on Io’s trailing hemisphere. When compared to the most recent spacecraft images, the SHARK-VIS images
show that a plume deposit from a powerful eruption at Pillan Patera has covered part
of the long-lived Pele plume deposit. Although this type of resurfacing event may be common on Io, few have been detected due to the rarity of spacecraft visits and the previously low spatial resolution available from Earth-based telescopes. The SHARK-VIS instrument ushers in a new era of high resolution imaging of Io’s surface using adaptive
optics at visible wavelengths.
Earliest Galaxies in the JADES Origins Field: Luminosity Function and Cosmic ...Sérgio Sacani
We characterize the earliest galaxy population in the JADES Origins Field (JOF), the deepest
imaging field observed with JWST. We make use of the ancillary Hubble optical images (5 filters
spanning 0.4−0.9µm) and novel JWST images with 14 filters spanning 0.8−5µm, including 7 mediumband filters, and reaching total exposure times of up to 46 hours per filter. We combine all our data
at > 2.3µm to construct an ultradeep image, reaching as deep as ≈ 31.4 AB mag in the stack and
30.3-31.0 AB mag (5σ, r = 0.1” circular aperture) in individual filters. We measure photometric
redshifts and use robust selection criteria to identify a sample of eight galaxy candidates at redshifts
z = 11.5 − 15. These objects show compact half-light radii of R1/2 ∼ 50 − 200pc, stellar masses of
M⋆ ∼ 107−108M⊙, and star-formation rates of SFR ∼ 0.1−1 M⊙ yr−1
. Our search finds no candidates
at 15 < z < 20, placing upper limits at these redshifts. We develop a forward modeling approach to
infer the properties of the evolving luminosity function without binning in redshift or luminosity that
marginalizes over the photometric redshift uncertainty of our candidate galaxies and incorporates the
impact of non-detections. We find a z = 12 luminosity function in good agreement with prior results,
and that the luminosity function normalization and UV luminosity density decline by a factor of ∼ 2.5
from z = 12 to z = 14. We discuss the possible implications of our results in the context of theoretical
models for evolution of the dark matter halo mass function.
THE IMPORTANCE OF MARTIAN ATMOSPHERE SAMPLE RETURN.Sérgio Sacani
The return of a sample of near-surface atmosphere from Mars would facilitate answers to several first-order science questions surrounding the formation and evolution of the planet. One of the important aspects of terrestrial planet formation in general is the role that primary atmospheres played in influencing the chemistry and structure of the planets and their antecedents. Studies of the martian atmosphere can be used to investigate the role of a primary atmosphere in its history. Atmosphere samples would also inform our understanding of the near-surface chemistry of the planet, and ultimately the prospects for life. High-precision isotopic analyses of constituent gases are needed to address these questions, requiring that the analyses are made on returned samples rather than in situ.
Multi-source connectivity as the driver of solar wind variability in the heli...Sérgio Sacani
The ambient solar wind that flls the heliosphere originates from multiple
sources in the solar corona and is highly structured. It is often described
as high-speed, relatively homogeneous, plasma streams from coronal
holes and slow-speed, highly variable, streams whose source regions are
under debate. A key goal of ESA/NASA’s Solar Orbiter mission is to identify
solar wind sources and understand what drives the complexity seen in the
heliosphere. By combining magnetic feld modelling and spectroscopic
techniques with high-resolution observations and measurements, we show
that the solar wind variability detected in situ by Solar Orbiter in March
2022 is driven by spatio-temporal changes in the magnetic connectivity to
multiple sources in the solar atmosphere. The magnetic feld footpoints
connected to the spacecraft moved from the boundaries of a coronal hole
to one active region (12961) and then across to another region (12957). This
is refected in the in situ measurements, which show the transition from fast
to highly Alfvénic then to slow solar wind that is disrupted by the arrival of
a coronal mass ejection. Our results describe solar wind variability at 0.5 au
but are applicable to near-Earth observatories.
Gliese 12 b: A Temperate Earth-sized Planet at 12 pc Ideal for Atmospheric Tr...Sérgio Sacani
Recent discoveries of Earth-sized planets transiting nearby M dwarfs have made it possible to characterize the
atmospheres of terrestrial planets via follow-up spectroscopic observations. However, the number of such planets
receiving low insolation is still small, limiting our ability to understand the diversity of the atmospheric
composition and climates of temperate terrestrial planets. We report the discovery of an Earth-sized planet
transiting the nearby (12 pc) inactive M3.0 dwarf Gliese 12 (TOI-6251) with an orbital period (Porb) of 12.76 days.
The planet, Gliese 12 b, was initially identified as a candidate with an ambiguous Porb from TESS data. We
confirmed the transit signal and Porb using ground-based photometry with MuSCAT2 and MuSCAT3, and
validated the planetary nature of the signal using high-resolution images from Gemini/NIRI and Keck/NIRC2 as
well as radial velocity (RV) measurements from the InfraRed Doppler instrument on the Subaru 8.2 m telescope
and from CARMENES on the CAHA 3.5 m telescope. X-ray observations with XMM-Newton showed the host
star is inactive, with an X-ray-to-bolometric luminosity ratio of log 5.7 L L X bol » - . Joint analysis of the light
curves and RV measurements revealed that Gliese 12 b has a radius of 0.96 ± 0.05 R⊕,a3σ mass upper limit of
3.9 M⊕, and an equilibrium temperature of 315 ± 6 K assuming zero albedo. The transmission spectroscopy metric
(TSM) value of Gliese 12 b is close to the TSM values of the TRAPPIST-1 planets, adding Gliese 12 b to the small
list of potentially terrestrial, temperate planets amenable to atmospheric characterization with JWST.
Gliese 12 b, a temperate Earth-sized planet at 12 parsecs discovered with TES...Sérgio Sacani
We report on the discovery of Gliese 12 b, the nearest transiting temperate, Earth-sized planet found to date. Gliese 12 is a
bright (V = 12.6 mag, K = 7.8 mag) metal-poor M4V star only 12.162 ± 0.005 pc away from the Solar system with one of the
lowest stellar activity levels known for M-dwarfs. A planet candidate was detected by TESS based on only 3 transits in sectors
42, 43, and 57, with an ambiguity in the orbital period due to observational gaps. We performed follow-up transit observations
with CHEOPS and ground-based photometry with MINERVA-Australis, SPECULOOS, and Purple Mountain Observatory,
as well as further TESS observations in sector 70. We statistically validate Gliese 12 b as a planet with an orbital period of
12.76144 ± 0.00006 d and a radius of 1.0 ± 0.1 R⊕, resulting in an equilibrium temperature of ∼315 K. Gliese 12 b has excellent
future prospects for precise mass measurement, which may inform how planetary internal structure is affected by the stellar
compositional environment. Gliese 12 b also represents one of the best targets to study whether Earth-like planets orbiting cool
stars can retain their atmospheres, a crucial step to advance our understanding of habitability on Earth and across the galaxy.
The importance of continents, oceans and plate tectonics for the evolution of...Sérgio Sacani
Within the uncertainties of involved astronomical and biological parameters, the Drake Equation
typically predicts that there should be many exoplanets in our galaxy hosting active, communicative
civilizations (ACCs). These optimistic calculations are however not supported by evidence, which is
often referred to as the Fermi Paradox. Here, we elaborate on this long-standing enigma by showing
the importance of planetary tectonic style for biological evolution. We summarize growing evidence
that a prolonged transition from Mesoproterozoic active single lid tectonics (1.6 to 1.0 Ga) to modern
plate tectonics occurred in the Neoproterozoic Era (1.0 to 0.541 Ga), which dramatically accelerated
emergence and evolution of complex species. We further suggest that both continents and oceans
are required for ACCs because early evolution of simple life must happen in water but late evolution
of advanced life capable of creating technology must happen on land. We resolve the Fermi Paradox
(1) by adding two additional terms to the Drake Equation: foc
(the fraction of habitable exoplanets
with significant continents and oceans) and fpt
(the fraction of habitable exoplanets with significant
continents and oceans that have had plate tectonics operating for at least 0.5 Ga); and (2) by
demonstrating that the product of foc
and fpt
is very small (< 0.00003–0.002). We propose that the lack
of evidence for ACCs reflects the scarcity of long-lived plate tectonics and/or continents and oceans on
exoplanets with primitive life.
A Giant Impact Origin for the First Subduction on EarthSérgio Sacani
Hadean zircons provide a potential record of Earth's earliest subduction 4.3 billion years ago. Itremains enigmatic how subduction could be initiated so soon after the presumably Moon‐forming giant impact(MGI). Earlier studies found an increase in Earth's core‐mantle boundary (CMB) temperature due to theaccumulation of the impactor's core, and our recent work shows Earth's lower mantle remains largely solid, withsome of the impactor's mantle potentially surviving as the large low‐shear velocity provinces (LLSVPs). Here,we show that a hot post‐impact CMB drives the initiation of strong mantle plumes that can induce subductioninitiation ∼200 Myr after the MGI. 2D and 3D thermomechanical computations show that a high CMBtemperature is the primary factor triggering early subduction, with enrichment of heat‐producing elements inLLSVPs as another potential factor. The models link the earliest subduction to the MGI with implications forunderstanding the diverse tectonic regimes of rocky planets.
Climate extremes likely to drive land mammal extinction during next supercont...Sérgio Sacani
Mammals have dominated Earth for approximately 55 Myr thanks to their
adaptations and resilience to warming and cooling during the Cenozoic. All
life will eventually perish in a runaway greenhouse once absorbed solar
radiation exceeds the emission of thermal radiation in several billions of
years. However, conditions rendering the Earth naturally inhospitable to
mammals may develop sooner because of long-term processes linked to
plate tectonics (short-term perturbations are not considered here). In
~250 Myr, all continents will converge to form Earth’s next supercontinent,
Pangea Ultima. A natural consequence of the creation and decay of Pangea
Ultima will be extremes in pCO2 due to changes in volcanic rifting and
outgassing. Here we show that increased pCO2, solar energy (F⨀;
approximately +2.5% W m−2 greater than today) and continentality (larger
range in temperatures away from the ocean) lead to increasing warming
hostile to mammalian life. We assess their impact on mammalian
physiological limits (dry bulb, wet bulb and Humidex heat stress indicators)
as well as a planetary habitability index. Given mammals’ continued survival,
predicted background pCO2 levels of 410–816 ppm combined with increased
F⨀ will probably lead to a climate tipping point and their mass extinction.
The results also highlight how global landmass configuration, pCO2 and F⨀
play a critical role in planetary habitability.
Constraints on Neutrino Natal Kicks from Black-Hole Binary VFTS 243Sérgio Sacani
The recently reported observation of VFTS 243 is the first example of a massive black-hole binary
system with negligible binary interaction following black-hole formation. The black-hole mass (≈10M⊙)
and near-circular orbit (e ≈ 0.02) of VFTS 243 suggest that the progenitor star experienced complete
collapse, with energy-momentum being lost predominantly through neutrinos. VFTS 243 enables us to
constrain the natal kick and neutrino-emission asymmetry during black-hole formation. At 68% confidence
level, the natal kick velocity (mass decrement) is ≲10 km=s (≲1.0M⊙), with a full probability distribution
that peaks when ≈0.3M⊙ were ejected, presumably in neutrinos, and the black hole experienced a natal
kick of 4 km=s. The neutrino-emission asymmetry is ≲4%, with best fit values of ∼0–0.2%. Such a small
neutrino natal kick accompanying black-hole formation is in agreement with theoretical predictions.
Detectability of Solar Panels as a TechnosignatureSérgio Sacani
In this work, we assess the potential detectability of solar panels made of silicon on an Earth-like
exoplanet as a potential technosignature. Silicon-based photovoltaic cells have high reflectance in the
UV-VIS and in the near-IR, within the wavelength range of a space-based flagship mission concept
like the Habitable Worlds Observatory (HWO). Assuming that only solar energy is used to provide
the 2022 human energy needs with a land cover of ∼ 2.4%, and projecting the future energy demand
assuming various growth-rate scenarios, we assess the detectability with an 8 m HWO-like telescope.
Assuming the most favorable viewing orientation, and focusing on the strong absorption edge in the
ultraviolet-to-visible (0.34 − 0.52 µm), we find that several 100s of hours of observation time is needed
to reach a SNR of 5 for an Earth-like planet around a Sun-like star at 10pc, even with a solar panel
coverage of ∼ 23% land coverage of a future Earth. We discuss the necessity of concepts like Kardeshev
Type I/II civilizations and Dyson spheres, which would aim to harness vast amounts of energy. Even
with much larger populations than today, the total energy use of human civilization would be orders of
magnitude below the threshold for causing direct thermal heating or reaching the scale of a Kardashev
Type I civilization. Any extraterrrestrial civilization that likewise achieves sustainable population
levels may also find a limit on its need to expand, which suggests that a galaxy-spanning civilization
as imagined in the Fermi paradox may not exist.
Detectability of Solar Panels as a Technosignature
Search for microscopic black hole signatures at the large hadron collider
1. EUROPEAN ORGANIZATION FOR NUCLEAR RESEARCH (CERN)
CERN-PH-EP/2010-073
2010/12/16
CMS-EXO-10-017
Search for Microscopic Black Hole Signatures at the Large
Hadron Collider
arXiv:1012.3375v1 [hep-ex] 15 Dec 2010
The CMS Collaboration∗
Abstract
A search for microscopic black hole production and decay in pp collisions at a center-
of-mass energy of 7 TeV has been conducted by the CMS Collaboration at the LHC,
using a data sample corresponding to an integrated luminosity of 35 pb−1 . Events
with large total transverse energy are analyzed for the presence of multiple high-
energy jets, leptons, and photons, typical of a signal expected from a microscopic
black hole. Good agreement with the expected standard model backgrounds, domi-
nated by QCD multijet production, is observed for various final-state multiplicities.
Limits on the minimum black hole mass are set, in the range 3.5 – 4.5 TeV, for a variety
of parameters in a model with large extra dimensions, along with model-independent
limits on new physics in these final states. These are the first direct limits on black hole
production at a particle accelerator.
Submitted to Physics Letters B
∗ See Appendix A for the list of collaboration members
2.
3. 1
One of the exciting predictions of theoretical models with extra spatial dimensions and low-
scale quantum gravity is the possibility of copious production of microscopic black holes in
particle collisions at the CERN Large Hadron Collider (LHC) [1, 2]. Models with low-scale
gravity are aimed at solving the hierarchy problem, the puzzlingly large difference between
the electroweak and Planck scales.
In this Letter we focus on microscopic black hole production in a model with large, flat, ex-
tra spatial dimensions, proposed by Arkani-Hamed, Dimopoulos, and Dvali, and referred to
as the ADD model [3, 4]. This model alleviates the hierarchy problem by introducing n extra
dimensions in space, compactified on an n-dimensional torus or sphere with radius r. The mul-
tidimensional space-time is only open to the gravitational interaction, while the gauge interac-
tions are localized on the 3 + 1 space-time membrane. As a result, the gravitational coupling
is enhanced at distances smaller than r, and Newton’s law of gravitation is modified at short
distances. The “true” Planck scale in 4 + n dimensions (MD ) is consequently lowered to the
electroweak scale, much smaller than the apparent Planck scale of MPl ∼ 1016 TeV seen by a
3 + 1 space-time observer. The relationship between MD and MPl follows from Gauss’s law
and is given as MPl = 8πMD+2 r n , using the Particle Data Group (PDG) definition [5].
2 n
Such a change in space-time structure and subsequent strengthening of the gravitational field in
the ADD model could allow black hole formation in particle collisions at energies greater than
MD , rather than MPl , which is the case for a truly 4-dimensional world. Colliding particles
would collapse in a black hole if their impact parameter were smaller than the Schwarzschild
radius of a black hole with the mass MBH equal to the total energy accessible in the collision.
The Schwarzschild radius of a black hole with mass MBH embedded in 4 + n space-time can be
found by solving Einstein’s general relativity equations and is given by [6, 7]:
n +1
1
1 MBH 8Γ n+3
2
rS = √ .
πMD MD n + 2
The parton-level cross section of black hole production is derived from geometrical considera-
2
tions and is given by σ ∼ πrS [1, 2]. At LHC energies, this cross section can reach 100 pb for MD
of 1 TeV. The exact cross section cannot be calculated without knowledge of the underlying the-
ory of quantum gravity and is subject to significant uncertainty. It is commonly accepted [1, 2]
min
that the minimum black hole mass MBH cannot be smaller than MD ; although the formation
threshold can be significantly larger than this. When a black hole is formed, some fraction of
the colliding parton energy may not be trapped within the event horizon and will be emitted in
the form of gravitational shock waves, which results in energy, momentum, and angular mo-
mentum loss. This effect is particularly model-dependent for black hole masses close to MD .
In general, black holes in particle collisions are produced with non-zero angular momentum,
which also affects their properties and production cross section.
Once produced, the microscopic black holes would decay thermally via Hawking radiation
[8], democratically (with equal probabilities) to all standard model (SM) degrees of freedom.
Quarks and gluons are the dominant particles produced in the black hole evaporation (∼ 75%)
because they have a large number of color degrees of freedom. The remaining fraction is ac-
counted for by leptons, W and Z bosons, photons, and possibly Higgs bosons. Emission of
gravitons by a black hole in the bulk space is generally expected to be suppressed [9]. In
some models the evaporation is terminated earlier, when the black hole mass reaches MD ,
with the formation of a stable non-interacting and non-accreting remnant. The Hawking tem-
perature for a black hole in 4 + n space-time is given by [1, 2, 7]: TH = 4πr1 (in Planck units
n+
S
4. 2
h = c = k B = 1, where k B is the Boltzmann constant) and is typically in the range of a few
¯
hundred GeV. The lifetime for such a microscopic black hole is ∼ 10−27 s [1, 2, 7].
Here we consider semi-classical black holes, whose properties are similar to those for classical
black holes described by general relativity and whose mass is close enough to MD so that
quantum effects can not be ignored completely. There are also models [10–12] of quantum black
holes that decay before they thermalize, mainly into two-jet final states. We do not consider this
signature here, leaving it for dedicated searches in the dijet channel [13, 14].
The microscopic black holes produced at the LHC would be distinguished by high multiplicity,
democratic, and highly isotropic decays with the final-state particles carrying hundreds of GeV
of energy. Most of these particles would be reconstructed as jets of hadrons. Observation of
such spectacular signatures would provide direct information on the nature of black holes as
well as the structure and dimensionality of space-time [1]. Microscopic black hole properties
are reviewed in more detail in [15, 16].
√
The search for black holes is based on s = 7 TeV pp collision data recorded by the Compact
Muon Solenoid (CMS) detector at the LHC between March and October 2010, which corre-
spond to an integrated luminosity of 34.7 ± 3.8 pb−1 . A detailed description of the CMS ex-
periment can be found elsewhere [17]. The central feature of the CMS detector is the 3.8 T
superconducting solenoid enclosing the silicon pixel and strip tracker, the electromagnetic cal-
orimeter (ECAL), and the brass-scintillator hadronic calorimeter (HCAL). For triggering pur-
poses and to facilitate jet reconstruction, the calorimeter cells are grouped in projective towers,
of granularity ∆η × ∆φ = 0.087 × 0.087 at central rapidities and 0.175 × 0.175 in the forward
region. Here, the pseudorapidity η is defined as − ln(tan 2 ), where θ is the polar angle with
θ
respect to the direction of the counterclockwise beam, and φ is the azimuthal angle. Muons are
measured in the pseudorapidity window |η | 2.4 in gaseous detectors embedded in the steel
return yoke.
The CMS trigger system consists of two levels. The first level (L1), composed of custom hard-
ware, uses information from the calorimeters and muon detectors to select the most interesting
events for more refined selection and analysis at a rate of up to 80 kHz. The software-based
High Level Trigger (HLT) further decreases the rate to a maximum of ∼ 300 Hz for data storage.
The instantaneous luminosity is measured using information from forward hadronic calorime-
ters [18].
We use data collected with a dedicated trigger on the total jet activity, HT , where HT is defined
as the scalar sum of the transverse energies ET of the jets above a preprogrammed threshold.
At L1 this jet ET threshold was 10 GeV, and the HT threshold was 50 GeV. At HLT, the jet ET
threshold varied between 20 and 30 GeV, and the HT threshold between 100 and 200 GeV. The
trigger is fully efficient for the offline analysis selections described below. Energetic electrons
and photons are also reconstructed as jets at the trigger level and are thus included in the HT
sum.
Jets are reconstructed using energy deposits in the HCAL and ECAL, clustered using a collinear
and infrared safe anti-k T
algorithm with a distance parameter of 0.5 [19]. The jet energy reso-
lution is ∆E/E ≈ 100 %/ E [GeV] ⊕ 5 %. Jets are required to pass quality requirements to re-
move those consistent with calorimeter noise. Jet energies are corrected for the non-uniformity
and non-linearity of the calorimeter response, as derived using Monte Carlo (MC) samples and
collision data [20]. Jets are required to have ET 20 GeV before the jet-energy-scale correc-
/
tions and to have |η | 2.6. Missing transverse energy E T is reconstructed as the negative of the
vector sum of transverse energies in the individual calorimeter towers. This quantity is further
5. 3
corrected to account for muons in the event, which deposit little energy in the calorimeters, and
for the jet energy scale [21].
Electrons and photons are identified as isolated energy deposits in the ECAL, with a shape
consistent with that expected for electromagnetic showers. Photons are required to have no
matching hits in the inner pixel detector layers, while electrons are required to have a matching
track. Electrons and photons are required to have ET 20 GeV and to be reconstructed in
the fiducial volume of the barrel (|η | 1.44) or the endcap (1.56 |η | 2.4). The ECAL
has an ultimate energy resolution better than 0.5% for unconverted photons or electrons with
transverse energies above 100 GeV [22]. In 2010 collision data, for ET 20 GeV, this resolution
is better than 1% in the barrel.
Muons are required to have matched tracks in the central tracker and the muon spectrometer,
to be within |η | 2.1, be consistent with the interaction vertex to suppress backgrounds from
cosmic ray muons, be isolated from other tracks, and have transverse momentum p T above
20 GeV. The combined fit using tracks measured in the central tracker and the muon spectrom-
eter results in p T resolution between 1% and 5% for p T values up to 1 TeV.
The separation between any two objects (jet, lepton, or photon) is required to be
∆R = ∆φ2 + ∆η 2 0.3.
Black hole signal events are simulated using the parton-level BlackMax [23] generator (v2.01.03),
followed by a parton-showering fragmentation with PYTHIA [24] (v6.420), and a fast parametric
simulation of the CMS detector response [25], which has been extensively validated for signal
events using detailed detector simulation via GEANT 4 [26].
Several additional parameters govern black hole production and decay in the ADD model in
addition to MD and n. For each value of MD , we consider a range of the minimum black hole
min
masses, MBH , between MD and the kinematic limit of the LHC. We assume that no parton-
collision energy is lost in gravitational shock waves, i.e. it is all trapped within the event hori-
zon of the forming black hole. We consider both rotating and non-rotating black holes in this
analysis. Graviton radiation by the black hole is not considered. For most of the signal samples
we assume full Hawking evaporation without a stable non-interacting remnant.
The parameters used in the simulations are listed in Table 1 for a number of characteristic model
points. The MSTW2008lo68 [27] parton distribution functions (PDF) were used. In addition we
compare the BlackMax results with those of the CHARYBDIS 2 MC generator (v1.0.3) [28, 29].
The two generators yield different values of total cross section, as BlackMax introduces an
additional n-dependent factor applied on top of the geometrical cross section. The CHARYB-
DIS cross sections are a factor of 1.36, 1.59, and 1.78 smaller than those from BlackMax for
n = 2, 4, and 6, respectively. In addition, CHARYBDIS has been used to simulate black hole
evaporation resulting in a stable non-interacting remnant with mass MD (this model is not im-
plemented in BlackMax). In the generation, we use the Particle Data Group [5] definition of the
Planck scale MD . (Using another popular choice for MD from Dimopoulos and Landsberg [1]
would result in a suppression of the production cross section by a factor of 1.35, 5.21, or 9.29
for n = 2, 4, or 6, respectively.)
We employ a selection based on total transverse energy to separate black hole candidate events
from the backgrounds. The variable ST is defined as a scalar sum of the ET of the N individual
objects (jets, electrons, photons, and muons) passing the above selections. Only objects with
ET 50 GeV are included in the calculation of ST , in order to suppress the SM backgrounds
6. 4
Table 1: Monte Carlo signal points for some of the model parameters probed, corresponding
leading order cross sections (σ), and the minimum required values for the event multiplicity
(N ≥ N min ) and ST (Smin ), as well as the signal acceptance (A), the expected number of signal
T
events (nsig ), the number of observed events (ndata ) in data, the expected number of background
events (nbkg ), and the observed (σ95 ) and expected (σexp. ) limits on the signal cross section at
95
95% confidence level.
MD MBH n σ N min Smin
T A nsig ndata nbkg σ95 95
σexp.
(TeV) (TeV) (pb) (TeV) (%) (pb) (pb)
1.5 2.5 6 117.9 3 1.5 90.6 3713 203 241 ± 45 1.69 2.52
1.5 3.0 6 25.94 3 1.8 91.3 823 45 66.2 ± 22.2 0.62 1.13
1.5 3.5 6 4.97 4 2.1 88.3 153 6 12.1 ± 6.3 0.21 0.39
1.5 4.0 6 0.77 5 2.4 84.4 22.5 0 2.01 ± 1.48 0.11 0.18
1.5 4.5 6 0.09 5 2.9 80.9 2.55 0 0.46+0.54
−0.46 0.11 0.13
1.5 5.0 6 0.007 5 3.4 75.2 0.19 0 0.13+0.21
−0.13 0.12 0.13
2.0 2.5 4 28.88 3 1.7 81.4 817 82 99.7 ± 28.1 1.16 1.64
2.0 3.0 4 6.45 3 2.0 83.2 186 21 30.8 ± 14.0 0.47 0.76
2.0 3.5 4 1.26 4 2.3 77.9 34.0 3 6.12 ± 4.05 0.20 0.31
2.0 4.0 4 0.20 4 2.8 73.4 5.07 0 1.35+1.45
−1.35 0.12 0.19
2.0 4.5 4 0.02 5 3.2 64.4 0.53 0 0.21+0.31
−0.21 0.14 0.15
2.0 5.0 4 0.002 5 3.7 59.6 0.04 0 0.06+0.12
−0.06 0.15 0.15
3.0 3.0 2 0.59 3 2.4 62.1 12.8 2 7.88 ± 5.80 0.21 0.46
3.0 3.5 2 0.12 3 2.8 58.9 2.41 0 2.40+2.57
−2.40 0.15 0.28
3.0 4.0 2 0.02 4 3.2 47.3 0.32 0 0.46+0.67
−0.46 0.19 0.23
3.0 4.5 2 0.002 5 3.6 33.6 0.03 0 0.08+0.15
−0.08 0.26 0.28
3.0 5.0 2 0.0002 5 4.0 34.5 0.002 0 0.03+0.07
−0.03 0.26 0.26
7. 5
and to be insensitive to jets from pile-up, while being fully efficient for black hole decays.
Further, the missing transverse energy in the event is added to ST , if the missing transverse
/
energy value exceeds 50 GeV. Note that while E T is counted toward ST , it is not considered in
the determination of N.
The main background to black hole signals arises from QCD multijet events. Other back-
¯
grounds from direct photon, W/Z +jets, and tt production were estimated from MC simu-
lations, using the M AD G RAPH [30] leading-order parton-level event generator with CTEQ6L
PDF set [31], followed by PYTHIA [24] parton showering and full CMS detector simulation via
GEANT 4 [26]. These additional backgrounds are negligible at large values of ST and contribute
less than 1% to the total background after the final selection.
The dominant multijet background can only be estimated reliably from data. For QCD events,
ST is almost completely determined by the hard 2 → 2 parton scattering process. Further
splitting of the jets due to final-state radiation, as well as jets due to initial-state radiation – most
often nearly collinear with either incoming or outgoing partons – does not change the ST value
considerably. Consequently, the shape of the ST distribution is expected to be independent of
the event multiplicity N, as long as ST is sufficiently above the turn-on region (i.e., much higher
than N × 50 GeV).
We confirmed the assumption of the ST shape invariance of N using MC generators capable of
simulating multijet final states from either matrix elements [32] or parton showers [24]. This
shape invariance offers a direct way of extracting the expected number of background events
in the search for black hole production. The decay of black holes with a mass of a few TeV typi-
cally results in events with multiplicity of half-a-dozen objects in the final state. The conjecture
that the ST shape is independent of the multiplicity has also been checked with data using the
exclusive multiplicities of N = 2 and N = 3. Even in the presence of a signal, its contribution to
these multiplicities is expected to be small and only seen at large values of ST , so these samples
can be used for the background prediction at higher multiplicities. Moreover, since dedicated
analyses of the dijet invariant mass spectrum have been conducted [13, 14], we know that there
are no appreciable contributions from new physics to the dijet final state up to invariant masses
of about 1.5 TeV, which, for central jets, translates to a similar range of ST .
We fit the ST distributions between 600 and 1100 GeV, where no black hole signal is expected,
P (1+ x ) P1
for data events with N = 2 and N = 3 using an ansatz function P02 +P3 log(x) , which is shown
x
with the solid line in Fig. 1. To check the systematic uncertainty of the fit, we use two addi-
tional ansatz functions, ( P + P P0+ x2 )P3 and ( P +0x)P2 [13], which are shown as the upper and lower
P
1 2x 1
boundaries of the shaded band in Fig. 1. The default choice of the ansatz function was made
based on the best-fit to the ST distribution for N = 2. Additional systematic uncertainty arises
from a slight difference between the best-fit shapes for N = 2 and N = 3. Nevertheless, the fits
for these two exclusive multiplicities agree with each other within the uncertainties, demon-
strating that the shape of the ST distribution is independent of the final-state multiplicity.
The ST distributions for data events with multiplicities N ≥ 3, 4, and 5 are shown in Figs. 2a, b,
and c, respectively. The solid curves in the figures are the predicted background shapes, found
by normalizing the fits of the N = 2 and 3 ST distributions to the range ST = 1000 − 1100 GeV,
where no black hole signal contribution is expected.
Since no excess is observed above the predicted background, we set limits on the black hole
production. We assign a systematic uncertainty on the background estimate of 6% to 125% for
the ST range used in this search. This uncertainy comes from the normalization uncertainty (4 –
12%, dominated by the statistics in the normalization region) added in quadrature to the uncer-
8. 6Events / 100 GeV
Events / 100 GeV
N=2 a) N=3 b)
Data Photon+Jets Data Photon+Jets
4 Background W+Jets 4 Background W+Jets
10 ttbar 10 ttbar
Uncertainty Z+Jets Uncertainty Z+Jets
min min
MD = 1.5 TeV, M = 3.0 TeV, n = 6 MD = 1.5 TeV, M = 3.0 TeV, n = 6
BH BH
min min
3
MD = 2.0 TeV, M = 3.0 TeV, n = 4 3
MD = 2.0 TeV, M = 3.0 TeV, n = 4
BH BH
10 MD = 3.0 TeV, M min = 3.0 TeV, n = 2 10 MD = 3.0 TeV, M min = 3.0 TeV, n = 2
BH BH
2
CMS, 35 pb-1 2 CMS, 35 pb-1
10 10
s = 7 TeV s = 7 TeV
10 10
1 1
-1 -1
10 1000 1500 2000 2500 3000 10 1000 1500 2000 2500 3000
ST (GeV) ST (GeV)
Figure 1: Total transverse energy ST , for events with the multiplicities of a) N = 2, and b) N = 3
objects in the final state. Data are depicted as solid circles with error bars; the shaded band is
the background prediction obtained from data (solid line) with its uncertainty. Non-multijet
backgrounds are shown as colored histograms. Also shown is the predicted black hole signal
for three different parameter sets.
tainties arising from using various ansatz fit functions and the difference between the shapes
obtained from the N = 2 and N = 3 samples. The integrated luminosity is measured with an
uncertainty of 11% [18]. The uncertainty on the signal yield is dominated by the jet energy scale
uncertainty of ≈ 5% [20] which translates into a 5% uncertainty on the signal. An additional
2% uncertainty on the signal acceptance comes from the variation of PDFs within the CTEQ6
error set [31]. The particle identification efficiency does not affect the signal distribution, since
an electron failing the identification requirements would be classified either as a photon or a
jet; a photon failing the selection would become a jet; a rejected muon would contribute to the
/
E T . In any case the total value of ST is not affected.
We set limits on black hole production with the optimized ST and N selections by counting
events with ST Smin and N N min . We optimized the signal (S) significance in the presence
T √
of background (B) using the ratio S/ S + B for each set. The optimum choice of parameters is
listed in Table 1, as well as the predicted number of background events, the expected number
of signal events, and the observed number of events in data. Note that the background uncer-
tainty, dominated by the choice of the fitting function, is highly correlated for various working
points listed in Table 1 and also bin-to-bin for the ST distributions shown in Figs. 1 and 2.
We set upper limits on the black hole production cross section using the Bayesian method
with flat signal prior and log-normal prior for integration over the nuisance parameters (back-
ground, signal acceptance, luminosity) [5, 33]. These upper limits at the 95% confidence level
min
(CL) are shown in Fig. 3, as a function of MBH . For the three working points shown in the
figure, the observed (expected) lower limits on the black hole mass are 3.5, 4.2 and 4.5 TeV (3.2,
4.0, and 4.5 TeV), respectively.
Translating these upper limits into lower limits on the parameters of the ADD model, we can
exclude the production of black holes with minimum mass of 3.5 − 4.5 TeV for values of the
multidimensional Planck scale up to 3.5 TeV at 95% CL. These limits, shown in Fig. 4, do not
exhibit significant dependence on the details of the production and evaporation model. These
9. Events / 100 GeV 7
Events / 100 GeV
N≥ 3 a) 4
N≥ 4 b)
4 Data 10 Data
10 Background Background
Uncertainty Uncertainty
MD = 1.5 TeV, M min = 3.0 TeV, n = 6 3 min
MD = 1.5 TeV, MBH = 3.0 TeV, n = 6
3 BH 10
10 MD = 2.0 TeV, M min = 3.0 TeV, n = 4 MD = 2.0 TeV, M min = 3.0 TeV, n = 4
BH BH
MD = 3.0 TeV, M min = 3.0 TeV, n = 2 min
MD = 3.0 TeV, MBH = 3.0 TeV, n = 2
BH
2
102 10
10 10
1 1
-1
CMS, 35 pb CMS, 35 pb-1
10-1
s = 7 TeV -1
10 s = 7 TeV
1000 1500 2000 2500 3000 1000 1500 2000 2500 3000
ST (GeV) ST (GeV)
Events / 100 GeV
10
4 N≥ 5 c)
Data
Background
Uncertainty
3
10 MD = 1.5 TeV, M min = 3.0 TeV, n = 6
BH
MD = 2.0 TeV, M min = 3.0 TeV, n = 4
BH
MD = 3.0 TeV, M min = 3.0 TeV, n = 2
BH
2
10
10
1
CMS, 35 pb-1
-1
10
s = 7 TeV
1000 1500 2000 2500 3000
ST (GeV)
Figure 2: Total transverse energy ST , for events with multiplicities a) N ≥ 3, b) N ≥ 4, and c)
N ≥ 5 objects in the final state. Data are depicted as solid circles with error bars; the shaded
band is the background prediction (solid line) with its uncertainty. Also shown are black hole
signals for three different parameter sets.
10. 8
σ (pb)
102 CMS, 35 pb-1 Non-rotating Black Holes
s = 7 TeV MD = 3.0 TeV, n = 2
MD = 2.0 TeV, n = 4
MD = 1.5 TeV, n = 6
10 Theoretical Cross Section
MD = 3.0 TeV, n = 2
MD = 2.0 TeV, n = 4
MD = 1.5 TeV, n = 6
1
10-1
2.5 3 3.5 4 4.5 5
min
MBH (TeV)
Figure 3: The 95% confidence level upper limits on the black hole production cross section
(solid lines) and three theoretical predictions for the cross section (dotted lines), as a function
of the black hole mass.
Excluded MBH (TeV)
4.5
CMS, 35 pb-1
s = 7 TeV
min
n=6
4 n=4
Non-Rotating n=2
3.5 Rotating
Stable Non-Interacting Remnant
1.5 2 2.5 3 3.5
MD (TeV)
Figure 4: The 95% confidence level limits on the black hole mass as a function of the multi-
dimensional Planck scale MD for several benchmark scenarios. The area below each curve is
excluded by this search.
11. 9
are the first limits of a dedicated search for black hole production at hadron colliders.
σ(S Smin) × A (ρb)
σ(S Smin) × A (ρb)
σ(S Smin) × A (ρb)
10 a) 10 b) 10 c)
CMS, 35 pb-1 CMS, 35 pb-1 CMS, 35 pb-1
s = 7 TeV s = 7 TeV s = 7 TeV
T
T
T
N≥ 3 N≥ 4 N≥ 5
Observed σ 95 Observed σ 95 Observed σ 95
1 1 1
T
T
T
Expected σ 95
exp. Expected σ 95 Expected σ 95
exp. exp.
10-1 10-1 10-1
1500 2000 2500 3000 1500 2000 2500 3000 1500 2000 2500 3000
Smin (GeV)
T
Smin (GeV)
T
Smin (GeV)
T
Figure 5: Model-independent 95% confidence level upper limits on a signal cross section times
acceptance for counting experiments with ST Smin as a function of Smin for (a) N ≥ 3, (b)
T T
N ≥ 4, and (c) N ≥ 5. The blue (red) lines correspond to an observed (expected) limit for
nominal signal acceptance uncertainty of 5%.
Finally, we produce model-independent upper limits on the cross section times the acceptance
for new physics production in high-ST inclusive final states for N ≥ 3, 4, and 5. Figure 5 shows
95% CL upper limits from a counting experiment for ST Smin as a function of Smin , which can
T T
be used to test models of new physics that result in these final states. A few examples of such
¯
models are production of high-mass tt resonances [34] in the six-jet and lepton + jet final states,
R-parity violating gluino decay into three jets, resulting in the six-jet final state [35, 36], and
a class of models with strong dynamics, with a strongly produced resonance decaying into a
pair of resonances further decaying into two jets each, resulting in the four-jet final state [37]. In
addition, these limits can be used to constrain black hole production for additional regions of
the parameter space of the model, as well as set limits on the existence of string balls [38], which
are quantum precursors of black holes predicted in certain string models. We have checked
that for the black hole model parameters we probed with the dedicated optimized analysis, the
sensitivity of the search in terms of the excluded black hole mass range exceeds that from the
model-independent cross section limits by as little as 5 – 8%. Thus, model-independent limits
can be used efficiently to constrain the allowed parameter space in an even broader variety of
black hole models than we covered in this Letter.
To conclude, we have performed the first dedicated search for microscopic black holes at a par-
ticle accelerator and set limits on their production within a variety of models. The lower limits
on the black hole mass at 95% CL range from 3.5 to 4.5 TeV for values of the Planck scale up
to 3.5 TeV in the model with large extra dimensions in space. Additionally, we have produced
model-independent limits on the production of energetic, high-multiplicity final states, which
can be used to constrain a variety of models of new physics.
We wish to congratulate our colleagues in the CERN accelerator departments for the excellent
performance of the LHC machine. We thank the technical and administrative staff at CERN
and other CMS institutes, and acknowledge support from: FMSR (Austria); FNRS and FWO
(Belgium); CNPq, CAPES, FAPERJ, and FAPESP (Brazil); MES (Bulgaria); CERN; CAS, MoST,
and NSFC (China); COLCIENCIAS (Colombia); MSES (Croatia); RPF (Cyprus); Academy of
Sciences and NICPB (Estonia); Academy of Finland, ME, and HIP (Finland); CEA and
CNRS/IN2P3 (France); BMBF, DFG, and HGF (Germany); GSRT (Greece); OTKA and NKTH
(Hungary); DAE and DST (India); IPM (Iran); SFI (Ireland); INFN (Italy); NRF and WCU
(Korea); LAS (Lithuania); CINVESTAV, CONACYT, SEP, and UASLP-FAI (Mexico); PAEC
(Pakistan); SCSR (Poland); FCT (Portugal); JINR (Armenia, Belarus, Georgia, Ukraine,
12. 10
Uzbekistan); MST and MAE (Russia); MSTD (Serbia); MICINN and CPAN (Spain); Swiss
Funding Agencies (Switzerland); NSC (Taipei); TUBITAK and TAEK (Turkey); STFC (United
Kingdom); DOE and NSF (USA).
References
[1] S. Dimopoulos and G. Landsberg, “Black Holes at the LHC”, Phys. Rev. Lett. 87 (2001)
161602, arXiv:hep-ph/0106295. doi:10.1103/PhysRevLett.87.161602.
[2] S. Giddings and S. Thomas, “High-energy colliders as black hole factories: The end of
short distance physics”, Phys. Rev. D65 (2002) 056010, arXiv:hep-ph/0106219.
doi:10.1103/PhysRevD.65.056010.
[3] N. Arkani-Hamed, S. Dimopoulos, and G. Dvali, “The Hierarchy problem and new
dimensions at a millimeter”, Phys. Lett. B429 (1998) 263.
doi:10.1016/S0370-2693(98)00466-3.
[4] N. Arkani-Hamed, S. Dimopoulos, and G. Dvali, “Phenomenology, astrophysics and
cosmology of theories with submillimeter dimensions and TeV scale quantum gravity”,
Phys. Rev. D59 (1999) 086004. doi:10.1103/PhysRevD.59.086004.
[5] Particle Data Group Collaboration, “The Review of Particle Physics”, J. Phys. G37 (2010)
075021. doi:10.1088/0954-3899/37/7A/075021.
[6] R. Myers and M. Perry, “Black Holes in Higher Dimensional Space-Times”, Ann. Phys.
172 (1986) 304. doi:10.1016/0003-4916(86)90186-7.
[7] P. Argyres, S. Dimopoulos, and J. March-Russell, “Black holes and submillimeter
dimensions”, Phys. Lett. B441 (1998) 96. doi:10.1016/S0370-2693(98)01184-8.
[8] S. Hawking, “Particle Creation by Black Holes”, Commun. Math. Phys. 43 (1975) 199.
doi:10.1007/BF02345020.
[9] R. Emparan, G. Horowitz, and R. Myers, “Black holes radiate mainly on the brane”,
Phys. Rev. Lett. 85 (2000) 499, arXiv:hep-th/0003118.
doi:10.1103/PhysRevLett.85.499.
[10] P. Meade and L. Randall, “Black Holes and Quantum Gravity at the LHC”, JHEP 05
(2008) 003, arXiv:0708.3017. doi:10.1088/1126-6708/2008/05/003.
[11] X. Calmet, W. Gong, and S. Hsu, “Colorful quantum black holes at the LHC”, Phys. Lett.
B668 (2008) 20, arXiv:0806.4605. doi:10.1016/j.physletb.2008.08.011.
[12] D. Gingrich, “Quantum black holes with charge, colour, and spin at the LHC”, J. Phys.
G37 (2010) 105108, arXiv:0912.0826.
doi:10.1088/0954-3899/37/10/105008.
[13] CMS Collaboration, “Search for Dijet Resonances in 7 TeV pp Collisions at CMS”, Phys.
Rev. Lett. 105 (2010) 211801, arXiv:1010.0203.
doi:10.1103/PhysRevLett.105.21180.
[14] CMS Collaboration, CMS Collaboration, “Search for Quark Compositeness with the Dijet
√
Centrality Ratio in pp Collisions at s = 7 TeV”. 2010. arXiv:1010.4439.
13. 11
[15] P. Kanti, “Black holes in theories with large extra dimensions: A Review”, Int. J. Mod.
Phys. A19 (2004) 4899, arXiv:hep-ph/0402168.
doi:10.1142/S0217751X04018324.
[16] G. Landsberg, “Black Holes at Future Colliders and Beyond”, J. Phys. G32 (2006) R337,
arXiv:hep-ph/0607297. doi:10.1088/0954-3899/32/9/R02.
[17] CMS Collaboration, “The CMS experiment at the CERN LHC”, JINST 3 (2008) S08004.
doi:10.1088/1748-0221/3/08/S08004.
[18] CMS Collaboration, “Measurement of CMS Luminosity”, CMS Physics Analysis Summary
CMS-PAS-EWK-10-004 (2010).
[19] M. Cacciari, G. Salam, and G. Soyez, “The anti-k T jet clustering algorithm”, JHEP 04
(2008) 063. doi:10.1088/1126-6708/2008/04/063.
[20] CMS Collaboration, “Jet Energy Corrections determination at 7 TeV”, CMS Physics
Analysis Summary CMS-PAS-JME-10-010 (2010).
[21] CMS Collaboration, “Missing Transverse√ Energy Performance in Minimum-Bias and Jet
Events from Proton-Proton Collisions at s = 7 TeV”, CMS Physics Analysis Summary
CMS-PAS-JME-10-004 (2010).
[22] P. Adzic et al., “Energy resolution of the barrel of the CMS electromagnetic calorimeter”,
JINST 2 (2007) P04004. doi:10.1088/1748-0221/2/04/P04004.
[23] D.-C. Dai, G. Starkman, D. Stojkovic et al., “BlackMax: A black-hole event generator with
rotation, recoil, split branes, and brane tension”, Phys. Rev. D77 (2008) 076007.
doi:10.1103/PhysRevD.77.076007.
¨
[24] T. Sjostrand, S. Mrenna, and P. Skands, “PYTHIA 6.4 Physics and Manual”, JHEP 05
(2006) 026. doi:10.1088/1126-6708/2006/05/026.
[25] D. Orbaker, “Fast Simulation of the CMS Detector”, J. Phys. Conf. Ser. 219 (2010) 032053.
doi:10.1088/1742-6596/219/3/032053.
[26] GEANT 4 Collaboration, “GEANT4 – a simulation toolkit”, Nucl. Instr. and Methods
A506 (2003) 250. doi:10.1016/S0168-9002(03)01368-8.
[27] A. D. Martin, W. J. Stirling, R. S. Thorne et al., “Heavy-quark mass dependence in global
PDF analyses and 3- and 4-flavour parton distributions”, Eur. Phys. J. C70 (2010) 51,
arXiv:1007.2624. doi:10.1140/epjc/s10052-010-1462-8.
[28] C. M. Harris, P. Richardson, and B. R. Webber, “CHARYBDIS: A black hole event
generator”, JHEP 08 (2003) 033, arXiv:hep-ph/0307305.
[29] J. Frost et al., “Phenomenology of Production and Decay of Spinning Extra- Dimensional
Black Holes at Hadron Colliders”, JHEP 10 (2009) 014, arXiv:0904.0979.
doi:10.1088/1126-6708/2009/10/014.
[30] J. Alwall et al., “MadGraph/MadEvent v4: The New Web Generation”, JHEP 09 (2007)
028. doi:10.1088/1126-6708/2007/09/028.
[31] CTEQ Collaboration, “Implications of CTEQ global analysis for collider observables”,
Phys. Rev. D78 (2008) 013004. doi:10.1103/PhysRevD.78.013004.
14. 12
[32] M. Mangano, M. Moretti, F. Piccinini et al., “ALPGEN, a generator for hard multiparton
processes in hadronic collisions”, JHEP 07 (2003) 001, arXiv:hep-ph/0206293.
doi:10.1088/1126-6708/2003/07/001.
[33] I. Bertram, G. Landsberg, J. Linnemann et al., “A Recipe for the construction of
confidence limits”, technical report, 2000. FERMILAB-TM-2104.
[34] K. Agashe, A. Belyaev, T. Krupovnickas et al., “LHC Signals from Warped Extra
Dimensions”, Phys. Rev. D77 (2008) 015003. doi:10.1103/PhysRevD.77.015003.
[35] R. Chivukula, M. Golden, and E. Simmons, “Six jet signals of highly colored fermions”,
Phys. Lett. B257 (1991) 403. doi:10.1016/0370-2693(91)91915-I.
[36] R. Chivukula, M. Golden, and E. Simmons, “Multi-jet physics at hadron colliders”, Nucl.
Phys. B363 (1991) 83. doi:10.1016/0550-3213(91)90235-P.
[37] B. Dobrescu, K. Kong, and R. Mahbubani, “Massive color-octet bosons and pairs of
resonances at hadron colliders”, Phys. Lett. B670 (2008) 119,
arXiv:arXiv:0709.2378v3 [hep-ph].
doi:10.1016/j.physletb.2008.10.048.
[38] S. Dimopoulos and R. Emparan, “String balls at the LHC and beyond”, Phys. Lett. B526
(2002) 393, arXiv:hep-ph/0108060. doi:10.1016/S0370-2693(01)01525-8.
15. 13
A The CMS Collaboration
Yerevan Physics Institute, Yerevan, Armenia
V. Khachatryan, A.M. Sirunyan, A. Tumasyan
Institut fur Hochenergiephysik der OeAW, Wien, Austria
¨
¨ ¨
W. Adam, T. Bergauer, M. Dragicevic, J. Ero, C. Fabjan, M. Friedl, R. Fruhwirth, V.M. Ghete,
J. Hammer1 , S. H¨ nsel, C. Hartl, M. Hoch, N. Hormann, J. Hrubec, M. Jeitler, G. Kasieczka,
a ¨
¨
W. Kiesenhofer, M. Krammer, D. Liko, I. Mikulec, M. Pernicka, H. Rohringer, R. Schofbeck,
J. Strauss, A. Taurok, F. Teischinger, W. Waltenberger, G. Walzel, E. Widl, C.-E. Wulz
National Centre for Particle and High Energy Physics, Minsk, Belarus
V. Mossolov, N. Shumeiko, J. Suarez Gonzalez
Universiteit Antwerpen, Antwerpen, Belgium
L. Benucci, K. Cerny, E.A. De Wolf, X. Janssen, T. Maes, L. Mucibello, S. Ochesanu, B. Roland,
R. Rougny, M. Selvaggi, H. Van Haevermaet, P. Van Mechelen, N. Van Remortel
Vrije Universiteit Brussel, Brussel, Belgium
V. Adler, S. Beauceron, F. Blekman, S. Blyweert, J. D’Hondt, O. Devroede, R. Gonzalez Suarez,
A. Kalogeropoulos, J. Maes, M. Maes, S. Tavernier, W. Van Doninck, P. Van Mulders, G.P. Van
Onsem, I. Villella
Universit´ Libre de Bruxelles, Bruxelles, Belgium
e
O. Charaf, B. Clerbaux, G. De Lentdecker, V. Dero, A.P.R. Gay, G.H. Hammad, T. Hreus,
P.E. Marage, L. Thomas, C. Vander Velde, P. Vanlaer, J. Wickens
Ghent University, Ghent, Belgium
S. Costantini, M. Grunewald, B. Klein, A. Marinov, J. Mccartin, D. Ryckbosch, F. Thyssen,
M. Tytgat, L. Vanelderen, P. Verwilligen, S. Walsh, N. Zaganidis
Universit´ Catholique de Louvain, Louvain-la-Neuve, Belgium
e
S. Basegmez, G. Bruno, J. Caudron, L. Ceard, J. De Favereau De Jeneret, C. Delaere, P. Demin,
D. Favart, A. Giammanco, G. Gr´ goire, J. Hollar, V. Lemaitre, J. Liao, O. Militaru, S. Ovyn,
e
D. Pagano, A. Pin, K. Piotrzkowski, L. Quertenmont, N. Schul
Universit´ de Mons, Mons, Belgium
e
N. Beliy, T. Caebergs, E. Daubie
Centro Brasileiro de Pesquisas Fisicas, Rio de Janeiro, Brazil
G.A. Alves, D. De Jesus Damiao, M.E. Pol, M.H.G. Souza
Universidade do Estado do Rio de Janeiro, Rio de Janeiro, Brazil
W. Carvalho, E.M. Da Costa, C. De Oliveira Martins, S. Fonseca De Souza, L. Mundim,
H. Nogima, V. Oguri, W.L. Prado Da Silva, A. Santoro, S.M. Silva Do Amaral, A. Sznajder,
F. Torres Da Silva De Araujo
Instituto de Fisica Teorica, Universidade Estadual Paulista, Sao Paulo, Brazil
F.A. Dias, M.A.F. Dias, T.R. Fernandez Perez Tomei, E. M. Gregores2 , F. Marinho, S.F. Novaes,
Sandra S. Padula
Institute for Nuclear Research and Nuclear Energy, Sofia, Bulgaria
N. Darmenov1 , L. Dimitrov, V. Genchev1 , P. Iaydjiev1 , S. Piperov, M. Rodozov, S. Stoykova,
G. Sultanov, V. Tcholakov, R. Trayanov, I. Vankov
16. 14 A The CMS Collaboration
University of Sofia, Sofia, Bulgaria
M. Dyulendarova, R. Hadjiiska, V. Kozhuharov, L. Litov, E. Marinova, M. Mateev, B. Pavlov,
P. Petkov
Institute of High Energy Physics, Beijing, China
J.G. Bian, G.M. Chen, H.S. Chen, C.H. Jiang, D. Liang, S. Liang, J. Wang, J. Wang, X. Wang,
Z. Wang, M. Xu, M. Yang, J. Zang, Z. Zhang
State Key Lab. of Nucl. Phys. and Tech., Peking University, Beijing, China
Y. Ban, S. Guo, W. Li, Y. Mao, S.J. Qian, H. Teng, L. Zhang, B. Zhu
Universidad de Los Andes, Bogota, Colombia
A. Cabrera, B. Gomez Moreno, A.A. Ocampo Rios, A.F. Osorio Oliveros, J.C. Sanabria
Technical University of Split, Split, Croatia
N. Godinovic, D. Lelas, K. Lelas, R. Plestina3 , D. Polic, I. Puljak
University of Split, Split, Croatia
Z. Antunovic, M. Dzelalija
Institute Rudjer Boskovic, Zagreb, Croatia
V. Brigljevic, S. Duric, K. Kadija, S. Morovic
University of Cyprus, Nicosia, Cyprus
A. Attikis, M. Galanti, J. Mousa, C. Nicolaou, F. Ptochos, P.A. Razis, H. Rykaczewski
Academy of Scientific Research and Technology of the Arab Republic of Egypt, Egyptian
Network of High Energy Physics, Cairo, Egypt
Y. Assran4 , A. Awad
National Institute of Chemical Physics and Biophysics, Tallinn, Estonia
¨
A. Hektor, M. Kadastik, K. Kannike, M. Muntel, M. Raidal, L. Rebane
Department of Physics, University of Helsinki, Helsinki, Finland
V. Azzolini, P. Eerola
Helsinki Institute of Physics, Helsinki, Finland
a ¨
S. Czellar, J. H¨ rkonen, A. Heikkinen, V. Karim¨ ki, R. Kinnunen, J. Klem, M.J. Kortelainen,
a
e e a a¨
T. Lamp´ n, K. Lassila-Perini, S. Lehti, T. Lind´ n, P. Luukka, T. M¨ enp¨ a, E. Tuominen,
J. Tuominiemi, E. Tuovinen, D. Ungaro, L. Wendland
Lappeenranta University of Technology, Lappeenranta, Finland
K. Banzuzi, A. Korpela, T. Tuuva
Laboratoire d’Annecy-le-Vieux de Physique des Particules, IN2P3-CNRS, Annecy-le-Vieux,
France
D. Sillou
DSM/IRFU, CEA/Saclay, Gif-sur-Yvette, France
M. Besancon, S. Choudhury, M. Dejardin, D. Denegri, B. Fabbro, J.L. Faure, F. Ferri, S. Ganjour,
F.X. Gentit, A. Givernaud, P. Gras, G. Hamel de Monchenault, P. Jarry, E. Locci, J. Malcles,
M. Marionneau, L. Millischer, J. Rander, A. Rosowsky, I. Shreyber, M. Titov, P. Verrecchia
Laboratoire Leprince-Ringuet, Ecole Polytechnique, IN2P3-CNRS, Palaiseau, France
S. Baffioni, F. Beaudette, L. Bianchini, M. Bluj5 , C. Broutin, P. Busson, C. Charlot, T. Dahms,
L. Dobrzynski, R. Granier de Cassagnac, M. Haguenauer, P. Min´ , C. Mironov, C. Ochando,
e
P. Paganini, D. Sabes, R. Salerno, Y. Sirois, C. Thiebaux, B. Wyslouch6 , A. Zabi
17. 15
Institut Pluridisciplinaire Hubert Curien, Universit´ de Strasbourg, Universit´ de Haute
e e
Alsace Mulhouse, CNRS/IN2P3, Strasbourg, France
J.-L. Agram7 , J. Andrea, A. Besson, D. Bloch, D. Bodin, J.-M. Brom, M. Cardaci, E.C. Chabert,
C. Collard, E. Conte7 , F. Drouhin7 , C. Ferro, J.-C. Fontaine7 , D. Gel´ , U. Goerlach, S. Greder,
e
P. Juillot, M. Karim7 , A.-C. Le Bihan, Y. Mikami, P. Van Hove
Centre de Calcul de l’Institut National de Physique Nucleaire et de Physique des
Particules (IN2P3), Villeurbanne, France
F. Fassi, D. Mercier
Universit´ de Lyon, Universit´ Claude Bernard Lyon 1, CNRS-IN2P3, Institut de Physique
e e
Nucl´ aire de Lyon, Villeurbanne, France
e
C. Baty, N. Beaupere, M. Bedjidian, O. Bondu, G. Boudoul, D. Boumediene, H. Brun,
N. Chanon, R. Chierici, D. Contardo, P. Depasse, H. El Mamouni, A. Falkiewicz, J. Fay,
S. Gascon, B. Ille, T. Kurca, T. Le Grand, M. Lethuillier, L. Mirabito, S. Perries, V. Sordini, S. Tosi,
Y. Tschudi, P. Verdier, H. Xiao
E. Andronikashvili Institute of Physics, Academy of Science, Tbilisi, Georgia
V. Roinishvili
RWTH Aachen University, I. Physikalisches Institut, Aachen, Germany
G. Anagnostou, M. Edelhoff, L. Feld, N. Heracleous, O. Hindrichs, R. Jussen, K. Klein, J. Merz,
N. Mohr, A. Ostapchuk, A. Perieanu, F. Raupach, J. Sammet, S. Schael, D. Sprenger, H. Weber,
M. Weber, B. Wittmer
RWTH Aachen University, III. Physikalisches Institut A, Aachen, Germany
M. Ata, W. Bender, M. Erdmann, J. Frangenheim, T. Hebbeker, A. Hinzmann, K. Hoepfner,
C. Hof, T. Klimkovich, D. Klingebiel, P. Kreuzer, D. Lanske† , C. Magass, G. Masetti,
M. Merschmeyer, A. Meyer, P. Papacz, H. Pieta, H. Reithler, S.A. Schmitz, L. Sonnenschein,
J. Steggemann, D. Teyssier
RWTH Aachen University, III. Physikalisches Institut B, Aachen, Germany
¨
M. Bontenackels, M. Davids, M. Duda, G. Flugge, H. Geenen, M. Giffels, W. Haj Ahmad,
D. Heydhausen, T. Kress, Y. Kuessel, A. Linn, A. Nowack, L. Perchalla, O. Pooth, J. Rennefeld,
P. Sauerland, A. Stahl, M. Thomas, D. Tornier, M.H. Zoeller
Deutsches Elektronen-Synchrotron, Hamburg, Germany
M. Aldaya Martin, W. Behrenhoff, U. Behrens, M. Bergholz8 , K. Borras, A. Cakir, A. Campbell,
E. Castro, D. Dammann, G. Eckerlin, D. Eckstein, A. Flossdorf, G. Flucke, A. Geiser, I. Glushkov,
J. Hauk, H. Jung, M. Kasemann, I. Katkov, P. Katsas, C. Kleinwort, H. Kluge, A. Knutsson,
D. Krucker, E. Kuznetsova, W. Lange, W. Lohmann8 , R. Mankel, M. Marienfeld, I.-A. Melzer-
¨
Pellmann, A.B. Meyer, J. Mnich, A. Mussgiller, J. Olzem, A. Parenti, A. Raspereza, A. Raval,
R. Schmidt8 , T. Schoerner-Sadenius, N. Sen, M. Stein, J. Tomaszewska, D. Volyanskyy, R. Walsh,
C. Wissing
University of Hamburg, Hamburg, Germany
C. Autermann, S. Bobrovskyi, J. Draeger, H. Enderle, U. Gebbert, K. Kaschube, G. Kaussen,
R. Klanner, J. Lange, B. Mura, S. Naumann-Emme, F. Nowak, N. Pietsch, C. Sander, H. Schettler,
¨ ¨
P. Schleper, M. Schroder, T. Schum, J. Schwandt, A.K. Srivastava, H. Stadie, G. Steinbruck,
J. Thomsen, R. Wolf
Institut fur Experimentelle Kernphysik, Karlsruhe, Germany
¨
C. Barth, J. Bauer, V. Buege, T. Chwalek, W. De Boer, A. Dierlamm, G. Dirkes, M. Feindt,
J. Gruschke, C. Hackstein, F. Hartmann, S.M. Heindl, M. Heinrich, H. Held, K.H. Hoffmann,
18. 16 A The CMS Collaboration
¨
S. Honc, T. Kuhr, D. Martschei, S. Mueller, Th. Muller, M. Niegel, O. Oberst, A. Oehler, J. Ott,
T. Peiffer, D. Piparo, G. Quast, K. Rabbertz, F. Ratnikov, M. Renz, C. Saout, A. Scheurer,
P. Schieferdecker, F.-P. Schilling, G. Schott, H.J. Simonis, F.M. Stober, D. Troendle, J. Wagner-
Kuhr, M. Zeise, V. Zhukov9 , E.B. Ziebarth
Institute of Nuclear Physics ”Demokritos”, Aghia Paraskevi, Greece
G. Daskalakis, T. Geralis, S. Kesisoglou, A. Kyriakis, D. Loukas, I. Manolakos, A. Markou,
C. Markou, C. Mavrommatis, E. Ntomari, E. Petrakou
University of Athens, Athens, Greece
L. Gouskos, T.J. Mertzimekis, A. Panagiotou1
University of Io´ nnina, Io´ nnina, Greece
a a
I. Evangelou, C. Foudas, P. Kokkas, N. Manthos, I. Papadopoulos, V. Patras, F.A. Triantis
KFKI Research Institute for Particle and Nuclear Physics, Budapest, Hungary
A. Aranyi, G. Bencze, L. Boldizsar, G. Debreczeni, C. Hajdu1 , D. Horvath10 , A. Kapusi,
K. Krajczar11 , A. Laszlo, F. Sikler, G. Vesztergombi11
Institute of Nuclear Research ATOMKI, Debrecen, Hungary
N. Beni, J. Molnar, J. Palinkas, Z. Szillasi, V. Veszpremi
University of Debrecen, Debrecen, Hungary
P. Raics, Z.L. Trocsanyi, B. Ujvari
Panjab University, Chandigarh, India
S. Bansal, S.B. Beri, V. Bhatnagar, N. Dhingra, M. Jindal, M. Kaur, J.M. Kohli, M.Z. Mehta,
N. Nishu, L.K. Saini, A. Sharma, A.P. Singh, J.B. Singh, S.P. Singh
University of Delhi, Delhi, India
S. Ahuja, S. Bhattacharya, B.C. Choudhary, P. Gupta, S. Jain, S. Jain, A. Kumar, R.K. Shivpuri
Bhabha Atomic Research Centre, Mumbai, India
R.K. Choudhury, D. Dutta, S. Kailas, S.K. Kataria, A.K. Mohanty1 , L.M. Pant, P. Shukla
Tata Institute of Fundamental Research - EHEP, Mumbai, India
T. Aziz, M. Guchait12 , A. Gurtu, M. Maity13 , D. Majumder, G. Majumder, K. Mazumdar,
G.B. Mohanty, A. Saha, K. Sudhakar, N. Wickramage
Tata Institute of Fundamental Research - HECR, Mumbai, India
S. Banerjee, S. Dugad, N.K. Mondal
Institute for Studies in Theoretical Physics Mathematics (IPM), Tehran, Iran
H. Arfaei, H. Bakhshiansohi, S.M. Etesami, A. Fahim, M. Hashemi, A. Jafari, M. Khakzad,
A. Mohammadi, M. Mohammadi Najafabadi, S. Paktinat Mehdiabadi, B. Safarzadeh,
M. Zeinali
INFN Sezione di Bari a , Universit` di Bari b , Politecnico di Bari c , Bari, Italy
a
M. Abbrescia a,b , L. Barbonea,b , C. Calabriaa,b , A. Colaleoa , D. Creanzaa,c , N. De Filippisa,c ,
M. De Palmaa,b , A. Dimitrova , L. Fiorea , G. Iasellia,c , L. Lusitoa,b,1 , G. Maggia,c , M. Maggia ,
N. Mannaa,b , B. Marangellia,b , S. Mya,c , S. Nuzzoa,b , N. Pacificoa,b , G.A. Pierroa , A. Pompilia,b ,
G. Pugliesea,c , F. Romanoa,c , G. Rosellia,b , G. Selvaggia,b , L. Silvestrisa , R. Trentaduea ,
S. Tupputia,b , G. Zitoa
INFN Sezione di Bologna a , Universit` di Bologna b , Bologna, Italy
a
G. Abbiendi a , A.C. Benvenutia , D. Bonacorsia , S. Braibant-Giacomellia,b , L. Brigliadoria ,
19. 17
P. Capiluppia,b , A. Castroa,b , F.R. Cavalloa , M. Cuffiania,b , G.M. Dallavallea , F. Fabbria ,
A. Fanfania,b , D. Fasanellaa , P. Giacomellia , M. Giuntaa , S. Marcellinia , M. Meneghellia,b ,
A. Montanaria , F.L. Navarriaa,b , F. Odoricia , A. Perrottaa , F. Primaveraa , A.M. Rossia,b ,
T. Rovellia,b , G. Sirolia,b , R. Travaglinia,b
INFN Sezione di Catania a , Universit` di Catania b , Catania, Italy
a
S. Albergoa,b , G. Cappelloa,b , M. Chiorbolia,b,1 , S. Costaa,b , A. Tricomia,b , C. Tuvea
INFN Sezione di Firenze a , Universit` di Firenze b , Firenze, Italy
a
G. Barbaglia , V. Ciullia,b , C. Civininia , R. D’Alessandroa,b , E. Focardia,b , S. Frosalia,b , E. Galloa ,
C. Gentaa , P. Lenzia,b , M. Meschinia , S. Paolettia , G. Sguazzonia , A. Tropianoa,1
INFN Laboratori Nazionali di Frascati, Frascati, Italy
L. Benussi, S. Bianco, S. Colafranceschi14 , F. Fabbri, D. Piccolo
INFN Sezione di Genova, Genova, Italy
P. Fabbricatore, R. Musenich
INFN Sezione di Milano-Biccoca a , Universit` di Milano-Bicocca b , Milano, Italy
a
A. Benagliaa,b , F. De Guioa,b,1 , L. Di Matteoa,b , A. Ghezzia,b,1 , M. Malbertia,b , S. Malvezzia ,
A. Martellia,b , A. Massironia,b , D. Menascea , L. Moronia , M. Paganonia,b , D. Pedrinia ,
S. Ragazzia,b , N. Redaellia , S. Salaa , T. Tabarelli de Fatisa,b , V. Tancinia,b
INFN Sezione di Napoli a , Universit` di Napoli ”Federico II” b , Napoli, Italy
a
S. Buontempoa , C.A. Carrillo Montoyaa , A. Cimminoa,b , A. De Cosaa,b , M. De Gruttolaa,b ,
F. Fabozzia,15 , A.O.M. Iorioa , L. Listaa , M. Merolaa,b , P. Nolia,b , P. Paoluccia
INFN Sezione di Padova a , Universit` di Padova b , Universit` di Trento (Trento) c , Padova,
a a
Italy
P. Azzia , N. Bacchettaa , P. Bellana,b , D. Biselloa,b , A. Brancaa , R. Carlina,b , P. Checchiaa ,
E. Contia , M. De Mattiaa,b , T. Dorigoa , U. Dossellia , F. Fanzagoa , F. Gasparinia,b , U. Gasparinia,b ,
P. Giubilatoa,b , A. Greselea,c , S. Lacapraraa,16 , I. Lazzizzeraa,c , M. Margonia,b , M. Mazzucatoa ,
A.T. Meneguzzoa,b , L. Perrozzia,1 , N. Pozzobona,b , P. Ronchesea,b , F. Simonettoa,b , E. Torassaa ,
M. Tosia,b , S. Vaninia,b , P. Zottoa,b , G. Zumerlea,b
INFN Sezione di Pavia a , Universit` di Pavia b , Pavia, Italy
a
P. Baessoa,b , U. Berzanoa , C. Riccardia,b , P. Torrea,b , P. Vituloa,b , C. Viviania,b
INFN Sezione di Perugia a , Universit` di Perugia b , Perugia, Italy
a
M. Biasinia,b , G.M. Bileia , B. Caponeria,b , L. Fanoa,b , P. Laricciaa,b , A. Lucaronia,b,1 ,
`
G. Mantovani a,b , M. Menichellia , A. Nappia,b , A. Santocchiaa,b , L. Servolia , S. Taronia,b ,
M. Valdataa,b , R. Volpea,b,1
INFN Sezione di Pisa a , Universit` di Pisa b , Scuola Normale Superiore di Pisa c , Pisa, Italy
a
P. Azzurria,c , G. Bagliesia , J. Bernardinia,b , T. Boccalia,1 , G. Broccoloa,c , R. Castaldia ,
R.T. D’Agnoloa,c , R. Dell’Orsoa , F. Fioria,b , L. Fo` a,c , A. Giassia , A. Kraana , F. Ligabuea,c ,
a
T. Lomtadzea , L. Martinia , A. Messineoa,b , F. Pallaa , F. Palmonaria , S. Sarkara,c , G. Segneria ,
A.T. Serbana , P. Spagnoloa , R. Tenchinia , G. Tonellia,b,1 , A. Venturia,1 , P.G. Verdinia
INFN Sezione di Roma a , Universit` di Roma ”La Sapienza” b , Roma, Italy
a
L. Baronea,b , F. Cavallaria , D. Del Rea,b , E. Di Marcoa,b , M. Diemoza , D. Francia,b , M. Grassia ,
E. Longoa,b , G. Organtinia,b , A. Palmaa,b , F. Pandolfia,b,1 , R. Paramattia , S. Rahatloua,b
20. 18 A The CMS Collaboration
INFN Sezione di Torino a , Universit` di Torino b , Universit` del Piemonte Orientale (No-
a a
vara) c , Torino, Italy
N. Amapanea,b , R. Arcidiaconoa,c , S. Argiroa,b , M. Arneodoa,c , C. Biinoa , C. Bottaa,b,1 ,
N. Cartigliaa , R. Castelloa,b , M. Costaa,b , N. Demariaa , A. Grazianoa,b,1 , C. Mariottia ,
M. Maronea,b , S. Masellia , E. Migliorea,b , G. Milaa,b , V. Monacoa,b , M. Musicha,b ,
M.M. Obertinoa,c , N. Pastronea , M. Pelliccionia,b,1 , A. Romeroa,b , M. Ruspaa,c , R. Sacchia,b ,
V. Solaa,b , A. Solanoa,b , A. Staianoa , D. Trocinoa,b , A. Vilela Pereiraa,b,1
INFN Sezione di Trieste a , Universit` di Trieste b , Trieste, Italy
a
F. Ambroglinia,b , S. Belfortea , F. Cossuttia , G. Della Riccaa,b , B. Gobboa , D. Montaninoa,b ,
A. Penzoa
Kangwon National University, Chunchon, Korea
S.G. Heo
Kyungpook National University, Daegu, Korea
S. Chang, J. Chung, D.H. Kim, G.N. Kim, J.E. Kim, D.J. Kong, H. Park, D. Son, D.C. Son
Chonnam National University, Institute for Universe and Elementary Particles, Kwangju,
Korea
Zero Kim, J.Y. Kim, S. Song
Korea University, Seoul, Korea
S. Choi, B. Hong, M. Jo, H. Kim, J.H. Kim, T.J. Kim, K.S. Lee, D.H. Moon, S.K. Park, H.B. Rhee,
E. Seo, S. Shin, K.S. Sim
University of Seoul, Seoul, Korea
M. Choi, S. Kang, H. Kim, C. Park, I.C. Park, S. Park, G. Ryu
Sungkyunkwan University, Suwon, Korea
Y. Choi, Y.K. Choi, J. Goh, J. Lee, S. Lee, H. Seo, I. Yu
Vilnius University, Vilnius, Lithuania
M.J. Bilinskas, I. Grigelionis, M. Janulis, D. Martisiute, P. Petrov, T. Sabonis
Centro de Investigacion y de Estudios Avanzados del IPN, Mexico City, Mexico
H. Castilla Valdez, E. De La Cruz Burelo, R. Lopez-Fernandez, A. S´ nchez Hern´ ndez,
a a
L.M. Villasenor-Cendejas
Universidad Iberoamericana, Mexico City, Mexico
S. Carrillo Moreno, F. Vazquez Valencia
Benemerita Universidad Autonoma de Puebla, Puebla, Mexico
H.A. Salazar Ibarguen
Universidad Autonoma de San Luis Potos´, San Luis Potos´, Mexico
´ ı ı
E. Casimiro Linares, A. Morelos Pineda, M.A. Reyes-Santos
University of Auckland, Auckland, New Zealand
P. Allfrey, D. Krofcheck
University of Canterbury, Christchurch, New Zealand
P.H. Butler, R. Doesburg, H. Silverwood
National Centre for Physics, Quaid-I-Azam University, Islamabad, Pakistan
M. Ahmad, I. Ahmed, M.I. Asghar, H.R. Hoorani, W.A. Khan, T. Khurshid, S. Qazi
21. 19
Institute of Experimental Physics, Faculty of Physics, University of Warsaw, Warsaw, Poland
M. Cwiok, W. Dominik, K. Doroba, A. Kalinowski, M. Konecki, J. Krolikowski
Soltan Institute for Nuclear Studies, Warsaw, Poland
´
T. Frueboes, R. Gokieli, M. Gorski, M. Kazana, K. Nawrocki, K. Romanowska-Rybinska,
M. Szleper, G. Wrochna, P. Zalewski
Laboratorio de Instrumenta¸ ao e F´sica Experimental de Part´culas, Lisboa, Portugal
´ c˜ ı ı
N. Almeida, A. David, P. Faccioli, P.G. Ferreira Parracho, M. Gallinaro, P. Martins, P. Musella,
A. Nayak, P.Q. Ribeiro, J. Seixas, P. Silva, J. Varela1 , H.K. Wohri
¨
Joint Institute for Nuclear Research, Dubna, Russia
I. Belotelov, P. Bunin, M. Finger, M. Finger Jr., I. Golutvin, A. Kamenev, V. Karjavin, G. Kozlov,
A. Lanev, P. Moisenz, V. Palichik, V. Perelygin, S. Shmatov, V. Smirnov, A. Volodko, A. Zarubin
Petersburg Nuclear Physics Institute, Gatchina (St Petersburg), Russia
N. Bondar, V. Golovtsov, Y. Ivanov, V. Kim, P. Levchenko, V. Murzin, V. Oreshkin, I. Smirnov,
V. Sulimov, L. Uvarov, S. Vavilov, A. Vorobyev
Institute for Nuclear Research, Moscow, Russia
Yu. Andreev, S. Gninenko, N. Golubev, M. Kirsanov, N. Krasnikov, V. Matveev, A. Pashenkov,
A. Toropin, S. Troitsky
Institute for Theoretical and Experimental Physics, Moscow, Russia
V. Epshteyn, V. Gavrilov, V. Kaftanov† , M. Kossov1 , A. Krokhotin, N. Lychkovskaya,
G. Safronov, S. Semenov, V. Stolin, E. Vlasov, A. Zhokin
Moscow State University, Moscow, Russia
E. Boos, M. Dubinin17 , L. Dudko, A. Ershov, A. Gribushin, O. Kodolova, I. Lokhtin,
S. Obraztsov, S. Petrushanko, L. Sarycheva, V. Savrin, A. Snigirev
P.N. Lebedev Physical Institute, Moscow, Russia
V. Andreev, M. Azarkin, I. Dremin, M. Kirakosyan, S.V. Rusakov, A. Vinogradov
State Research Center of Russian Federation, Institute for High Energy Physics, Protvino,
Russia
I. Azhgirey, S. Bitioukov, V. Grishin1 , V. Kachanov, D. Konstantinov, A. Korablev, V. Krychkine,
V. Petrov, R. Ryutin, S. Slabospitsky, A. Sobol, L. Tourtchanovitch, S. Troshin, N. Tyurin,
A. Uzunian, A. Volkov
University of Belgrade, Faculty of Physics and Vinca Institute of Nuclear Sciences, Belgrade,
Serbia
P. Adzic18 , M. Djordjevic, D. Krpic18 , J. Milosevic
Centro de Investigaciones Energ´ ticas Medioambientales y Tecnologicas (CIEMAT),
e ´
Madrid, Spain
M. Aguilar-Benitez, J. Alcaraz Maestre, P. Arce, C. Battilana, E. Calvo, M. Cepeda, M. Cerrada,
N. Colino, B. De La Cruz, C. Diez Pardos, D. Dom´nguez V´ zquez, C. Fernandez Bedoya,
ı a
J.P. Fern´ ndez Ramos, A. Ferrando, J. Flix, M.C. Fouz, P. Garcia-Abia, O. Gonzalez Lopez,
a
S. Goy Lopez, J.M. Hernandez, M.I. Josa, G. Merino, J. Puerta Pelayo, I. Redondo, L. Romero,
J. Santaolalla, C. Willmott
Universidad Autonoma de Madrid, Madrid, Spain
´
´
C. Albajar, G. Codispoti, J.F. de Troconiz
22. 20 A The CMS Collaboration
Universidad de Oviedo, Oviedo, Spain
J. Cuevas, J. Fernandez Menendez, S. Folgueras, I. Gonzalez Caballero, L. Lloret Iglesias,
J.M. Vizan Garcia
Instituto de F´sica de Cantabria (IFCA), CSIC-Universidad de Cantabria, Santander, Spain
ı
J.A. Brochero Cifuentes, I.J. Cabrillo, A. Calderon, M. Chamizo Llatas, S.H. Chuang, J. Duarte
Campderros, M. Felcini19 , M. Fernandez, G. Gomez, J. Gonzalez Sanchez, C. Jorda, P. Lobelle
Pardo, A. Lopez Virto, J. Marco, R. Marco, C. Martinez Rivero, F. Matorras, F.J. Munoz Sanchez,
J. Piedra Gomez20 , T. Rodrigo, A. Ruiz Jimeno, L. Scodellaro, M. Sobron Sanudo, I. Vila, R. Vilar
Cortabitarte
CERN, European Organization for Nuclear Research, Geneva, Switzerland
D. Abbaneo, E. Auffray, G. Auzinger, P. Baillon, A.H. Ball, D. Barney, A.J. Bell21 , D. Benedetti,
C. Bernet3 , W. Bialas, P. Bloch, A. Bocci, S. Bolognesi, H. Breuker, G. Brona, K. Bunkowski,
T. Camporesi, E. Cano, G. Cerminara, T. Christiansen, J.A. Coarasa Perez, B. Cur´ , e
D. D’Enterria, A. De Roeck, F. Duarte Ramos, A. Elliott-Peisert, B. Frisch, W. Funk, A. Gaddi,
S. Gennai, G. Georgiou, H. Gerwig, D. Gigi, K. Gill, D. Giordano, F. Glege, R. Gomez-Reino
Garrido, M. Gouzevitch, P. Govoni, S. Gowdy, L. Guiducci, M. Hansen, J. Harvey, J. Hegeman,
B. Hegner, C. Henderson, G. Hesketh, H.F. Hoffmann, A. Honma, V. Innocente, P. Janot,
E. Karavakis, P. Lecoq, C. Leonidopoulos, C. Lourenco, A. Macpherson, T. M¨ ki, L. Malgeri,
¸ a
M. Mannelli, L. Masetti, F. Meijers, S. Mersi, E. Meschi, R. Moser, M.U. Mozer, M. Mulders,
E. Nesvold1 , M. Nguyen, T. Orimoto, L. Orsini, E. Perez, A. Petrilli, A. Pfeiffer, M. Pierini,
M. Pimi¨ , G. Polese, A. Racz, G. Rolandi22 , T. Rommerskirchen, C. Rovelli23 , M. Rovere,
a
H. Sakulin, C. Sch¨ fer, C. Schwick, I. Segoni, A. Sharma, P. Siegrist, M. Simon, P. Sphicas24 ,
a
D. Spiga, M. Spiropulu17 , F. Stockli, M. Stoye, P. Tropea, A. Tsirou, A. Tsyganov, G.I. Veres11 ,
¨
P. Vichoudis, M. Voutilainen, W.D. Zeuner
Paul Scherrer Institut, Villigen, Switzerland
W. Bertl, K. Deiters, W. Erdmann, K. Gabathuler, R. Horisberger, Q. Ingram, H.C. Kaestli,
S. Konig, D. Kotlinski, U. Langenegger, F. Meier, D. Renker, T. Rohe, J. Sibille25 ,
¨
A. Starodumov26
Institute for Particle Physics, ETH Zurich, Zurich, Switzerland
P. Bortignon, L. Caminada27 , Z. Chen, S. Cittolin, G. Dissertori, M. Dittmar, J. Eugster,
K. Freudenreich, C. Grab, A. Herv´ , W. Hintz, P. Lecomte, W. Lustermann, C. Marchica27 ,
e
P. Martinez Ruiz del Arbol, P. Meridiani, P. Milenovic28 , F. Moortgat, P. Nef, F. Nessi-Tedaldi,
L. Pape, F. Pauss, T. Punz, A. Rizzi, F.J. Ronga, M. Rossini, L. Sala, A.K. Sanchez, M.-C. Sawley,
B. Stieger, L. Tauscher† , A. Thea, K. Theofilatos, D. Treille, C. Urscheler, R. Wallny19 , M. Weber,
L. Wehrli, J. Weng
Universit¨ t Zurich, Zurich, Switzerland
a ¨
´
E. Aguilo, C. Amsler, V. Chiochia, S. De Visscher, C. Favaro, M. Ivova Rikova, B. Millan Mejias,
C. Regenfus, P. Robmann, A. Schmidt, H. Snoek, L. Wilke
National Central University, Chung-Li, Taiwan
Y.H. Chang, K.H. Chen, W.T. Chen, S. Dutta, A. Go, C.M. Kuo, S.W. Li, W. Lin, M.H. Liu,
Z.K. Liu, Y.J. Lu, J.H. Wu, S.S. Yu
National Taiwan University (NTU), Taipei, Taiwan
P. Bartalini, P. Chang, Y.H. Chang, Y.W. Chang, Y. Chao, K.F. Chen, W.-S. Hou, Y. Hsiung,
K.Y. Kao, Y.J. Lei, R.-S. Lu, J.G. Shiu, Y.M. Tzeng, M. Wang
23. 21
Cukurova University, Adana, Turkey
A. Adiguzel, M.N. Bakirci, S. Cerci29 , Z. Demir, C. Dozen, I. Dumanoglu, E. Eskut, S. Girgis,
G. Gokbulut, Y. Guler, E. Gurpinar, I. Hos, E.E. Kangal, T. Karaman, A. Kayis Topaksu, A. Nart,
G. Onengut, K. Ozdemir, S. Ozturk, A. Polatoz, K. Sogut30 , B. Tali, H. Topakli, D. Uzun,
L.N. Vergili, M. Vergili, C. Zorbilmez
Middle East Technical University, Physics Department, Ankara, Turkey
I.V. Akin, T. Aliev, S. Bilmis, M. Deniz, H. Gamsizkan, A.M. Guler, K. Ocalan, A. Ozpineci,
M. Serin, R. Sever, U.E. Surat, E. Yildirim, M. Zeyrek
Bogazici University, Istanbul, Turkey
M. Deliomeroglu, D. Demir31 , E. Gulmez, A. Halu, B. Isildak, M. Kaya32 , O. Kaya32 ,
¨
S. Ozkorucuklu33 , N. Sonmez34
National Scientific Center, Kharkov Institute of Physics and Technology, Kharkov, Ukraine
L. Levchuk
University of Bristol, Bristol, United Kingdom
P. Bell, F. Bostock, J.J. Brooke, T.L. Cheng, E. Clement, D. Cussans, R. Frazier, J. Goldstein,
M. Grimes, M. Hansen, D. Hartley, G.P. Heath, H.F. Heath, B. Huckvale, J. Jackson, L. Kreczko,
S. Metson, D.M. Newbold35 , K. Nirunpong, A. Poll, S. Senkin, V.J. Smith, S. Ward
Rutherford Appleton Laboratory, Didcot, United Kingdom
L. Basso, K.W. Bell, A. Belyaev, C. Brew, R.M. Brown, B. Camanzi, D.J.A. Cockerill,
J.A. Coughlan, K. Harder, S. Harper, B.W. Kennedy, E. Olaiya, D. Petyt, B.C. Radburn-Smith,
C.H. Shepherd-Themistocleous, I.R. Tomalin, W.J. Womersley, S.D. Worm
Imperial College, London, United Kingdom
R. Bainbridge, G. Ball, J. Ballin, R. Beuselinck, O. Buchmuller, D. Colling, N. Cripps, M. Cutajar,
G. Davies, M. Della Negra, J. Fulcher, D. Futyan, A. Guneratne Bryer, G. Hall, Z. Hatherell,
J. Hays, G. Iles, G. Karapostoli, L. Lyons, A.-M. Magnan, J. Marrouche, R. Nandi, J. Nash,
A. Nikitenko26 , A. Papageorgiou, M. Pesaresi, K. Petridis, M. Pioppi36 , D.M. Raymond,
N. Rompotis, A. Rose, M.J. Ryan, C. Seez, P. Sharp, A. Sparrow, A. Tapper, S. Tourneur,
M. Vazquez Acosta, T. Virdee, S. Wakefield, D. Wardrope, T. Whyntie
Brunel University, Uxbridge, United Kingdom
M. Barrett, M. Chadwick, J.E. Cole, P.R. Hobson, A. Khan, P. Kyberd, D. Leslie, W. Martin,
I.D. Reid, L. Teodorescu
Baylor University, Waco, USA
K. Hatakeyama
Boston University, Boston, USA
T. Bose, E. Carrera Jarrin, A. Clough, C. Fantasia, A. Heister, J. St. John, P. Lawson, D. Lazic,
J. Rohlf, D. Sperka, L. Sulak
Brown University, Providence, USA
A. Avetisyan, S. Bhattacharya, J.P. Chou, D. Cutts, A. Ferapontov, U. Heintz, S. Jabeen,
G. Kukartsev, G. Landsberg, M. Narain, D. Nguyen, M. Segala, T. Speer, K.V. Tsang
University of California, Davis, Davis, USA
M.A. Borgia, R. Breedon, M. Calderon De La Barca Sanchez, D. Cebra, S. Chauhan, M. Chertok,
J. Conway, P.T. Cox, J. Dolen, R. Erbacher, E. Friis, W. Ko, A. Kopecky, R. Lander, H. Liu,
S. Maruyama, T. Miceli, M. Nikolic, D. Pellett, J. Robles, S. Salur, T. Schwarz, M. Searle, J. Smith,
M. Squires, M. Tripathi, R. Vasquez Sierra, C. Veelken
24. 22 A The CMS Collaboration
University of California, Los Angeles, Los Angeles, USA
V. Andreev, K. Arisaka, D. Cline, R. Cousins, A. Deisher, J. Duris, S. Erhan, C. Farrell, J. Hauser,
M. Ignatenko, C. Jarvis, C. Plager, G. Rakness, P. Schlein† , J. Tucker, V. Valuev
University of California, Riverside, Riverside, USA
J. Babb, R. Clare, J. Ellison, J.W. Gary, F. Giordano, G. Hanson, G.Y. Jeng, S.C. Kao, F. Liu,
H. Liu, A. Luthra, H. Nguyen, G. Pasztor37 , A. Satpathy, B.C. Shen† , R. Stringer, J. Sturdy,
S. Sumowidagdo, R. Wilken, S. Wimpenny
University of California, San Diego, La Jolla, USA
W. Andrews, J.G. Branson, G.B. Cerati, E. Dusinberre, D. Evans, F. Golf, A. Holzner, R. Kelley,
M. Lebourgeois, J. Letts, B. Mangano, J. Muelmenstaedt, S. Padhi, C. Palmer, G. Petrucciani,
H. Pi, M. Pieri, R. Ranieri, M. Sani, V. Sharma1 , S. Simon, Y. Tu, A. Vartak, F. Wurthwein,
¨
A. Yagil
University of California, Santa Barbara, Santa Barbara, USA
D. Barge, R. Bellan, C. Campagnari, M. D’Alfonso, T. Danielson, K. Flowers, P. Geffert,
J. Incandela, C. Justus, P. Kalavase, S.A. Koay, D. Kovalskyi, V. Krutelyov, S. Lowette, N. Mccoll,
V. Pavlunin, F. Rebassoo, J. Ribnik, J. Richman, R. Rossin, D. Stuart, W. To, J.R. Vlimant
California Institute of Technology, Pasadena, USA
A. Bornheim, J. Bunn, Y. Chen, M. Gataullin, D. Kcira, V. Litvine, Y. Ma, A. Mott, H.B. Newman,
C. Rogan, V. Timciuc, P. Traczyk, J. Veverka, R. Wilkinson, Y. Yang, R.Y. Zhu
Carnegie Mellon University, Pittsburgh, USA
B. Akgun, R. Carroll, T. Ferguson, Y. Iiyama, D.W. Jang, S.Y. Jun, Y.F. Liu, M. Paulini, J. Russ,
N. Terentyev, H. Vogel, I. Vorobiev
University of Colorado at Boulder, Boulder, USA
J.P. Cumalat, M.E. Dinardo, B.R. Drell, C.J. Edelmaier, W.T. Ford, B. Heyburn, E. Luiggi Lopez,
U. Nauenberg, J.G. Smith, K. Stenson, K.A. Ulmer, S.R. Wagner, S.L. Zang
Cornell University, Ithaca, USA
L. Agostino, J. Alexander, A. Chatterjee, S. Das, N. Eggert, L.J. Fields, L.K. Gibbons, B. Heltsley,
W. Hopkins, A. Khukhunaishvili, B. Kreis, V. Kuznetsov, G. Nicolas Kaufman, J.R. Patterson,
D. Puigh, D. Riley, A. Ryd, X. Shi, W. Sun, W.D. Teo, J. Thom, J. Thompson, J. Vaughan, Y. Weng,
L. Winstrom, P. Wittich
Fairfield University, Fairfield, USA
A. Biselli, G. Cirino, D. Winn
Fermi National Accelerator Laboratory, Batavia, USA
S. Abdullin, M. Albrow, J. Anderson, G. Apollinari, M. Atac, J.A. Bakken, S. Banerjee,
L.A.T. Bauerdick, A. Beretvas, J. Berryhill, P.C. Bhat, I. Bloch, F. Borcherding, K. Burkett,
J.N. Butler, V. Chetluru, H.W.K. Cheung, F. Chlebana, S. Cihangir, M. Demarteau, D.P. Eartly,
V.D. Elvira, S. Esen, I. Fisk, J. Freeman, Y. Gao, E. Gottschalk, D. Green, K. Gunthoti, O. Gutsche,
A. Hahn, J. Hanlon, R.M. Harris, J. Hirschauer, B. Hooberman, E. James, H. Jensen, M. Johnson,
U. Joshi, R. Khatiwada, B. Kilminster, B. Klima, K. Kousouris, S. Kunori, S. Kwan, P. Limon,
R. Lipton, J. Lykken, K. Maeshima, J.M. Marraffino, D. Mason, P. McBride, T. McCauley,
T. Miao, K. Mishra, S. Mrenna, Y. Musienko38 , C. Newman-Holmes, V. O’Dell, S. Popescu39 ,
R. Pordes, O. Prokofyev, N. Saoulidou, E. Sexton-Kennedy, S. Sharma, A. Soha, W.J. Spalding,
L. Spiegel, P. Tan, L. Taylor, S. Tkaczyk, L. Uplegger, E.W. Vaandering, R. Vidal, J. Whitmore,
W. Wu, F. Yang, F. Yumiceva, J.C. Yun
25. 23
University of Florida, Gainesville, USA
D. Acosta, P. Avery, D. Bourilkov, M. Chen, G.P. Di Giovanni, D. Dobur, A. Drozdetskiy,
R.D. Field, M. Fisher, Y. Fu, I.K. Furic, J. Gartner, S. Goldberg, B. Kim, S. Klimenko,
J. Konigsberg, A. Korytov, A. Kropivnitskaya, T. Kypreos, K. Matchev, G. Mitselmakher,
L. Muniz, Y. Pakhotin, C. Prescott, R. Remington, M. Schmitt, B. Scurlock, P. Sellers,
N. Skhirtladze, D. Wang, J. Yelton, M. Zakaria
Florida International University, Miami, USA
C. Ceron, V. Gaultney, L. Kramer, L.M. Lebolo, S. Linn, P. Markowitz, G. Martinez,
J.L. Rodriguez
Florida State University, Tallahassee, USA
T. Adams, A. Askew, D. Bandurin, J. Bochenek, J. Chen, B. Diamond, S.V. Gleyzer, J. Haas,
S. Hagopian, V. Hagopian, M. Jenkins, K.F. Johnson, H. Prosper, S. Sekmen, V. Veeraraghavan
Florida Institute of Technology, Melbourne, USA
M.M. Baarmand, B. Dorney, S. Guragain, M. Hohlmann, H. Kalakhety, R. Ralich,
I. Vodopiyanov
University of Illinois at Chicago (UIC), Chicago, USA
M.R. Adams, I.M. Anghel, L. Apanasevich, Y. Bai, V.E. Bazterra, R.R. Betts, J. Callner,
R. Cavanaugh, C. Dragoiu, E.J. Garcia-Solis, C.E. Gerber, D.J. Hofman, S. Khalatyan, F. Lacroix,
C. O’Brien, C. Silvestre, A. Smoron, D. Strom, N. Varelas
The University of Iowa, Iowa City, USA
U. Akgun, E.A. Albayrak, B. Bilki, K. Cankocak40 , W. Clarida, F. Duru, C.K. Lae, E. McCliment,
J.-P. Merlo, H. Mermerkaya, A. Mestvirishvili, A. Moeller, J. Nachtman, C.R. Newsom,
E. Norbeck, J. Olson, Y. Onel, F. Ozok, S. Sen, J. Wetzel, T. Yetkin, K. Yi
Johns Hopkins University, Baltimore, USA
B.A. Barnett, B. Blumenfeld, A. Bonato, C. Eskew, D. Fehling, G. Giurgiu, A.V. Gritsan, Z.J. Guo,
G. Hu, P. Maksimovic, S. Rappoccio, M. Swartz, N.V. Tran, A. Whitbeck
The University of Kansas, Lawrence, USA
P. Baringer, A. Bean, G. Benelli, O. Grachov, M. Murray, D. Noonan, V. Radicci, S. Sanders,
J.S. Wood, V. Zhukova
Kansas State University, Manhattan, USA
T. Bolton, I. Chakaberia, A. Ivanov, M. Makouski, Y. Maravin, S. Shrestha, I. Svintradze, Z. Wan
Lawrence Livermore National Laboratory, Livermore, USA
J. Gronberg, D. Lange, D. Wright
University of Maryland, College Park, USA
A. Baden, M. Boutemeur, S.C. Eno, D. Ferencek, J.A. Gomez, N.J. Hadley, R.G. Kellogg, M. Kirn,
Y. Lu, A.C. Mignerey, K. Rossato, P. Rumerio, F. Santanastasio, A. Skuja, J. Temple, M.B. Tonjes,
S.C. Tonwar, E. Twedt
Massachusetts Institute of Technology, Cambridge, USA
B. Alver, G. Bauer, J. Bendavid, W. Busza, E. Butz, I.A. Cali, M. Chan, V. Dutta, P. Everaerts,
G. Gomez Ceballos, M. Goncharov, K.A. Hahn, P. Harris, Y. Kim, M. Klute, Y.-J. Lee, W. Li,
C. Loizides, P.D. Luckey, T. Ma, S. Nahn, C. Paus, D. Ralph, C. Roland, G. Roland, M. Rudolph,
G.S.F. Stephans, K. Sumorok, K. Sung, E.A. Wenger, S. Xie, M. Yang, Y. Yilmaz, A.S. Yoon,
M. Zanetti
26. 24 A The CMS Collaboration
University of Minnesota, Minneapolis, USA
P. Cole, S.I. Cooper, P. Cushman, B. Dahmes, A. De Benedetti, P.R. Dudero, G. Franzoni,
J. Haupt, K. Klapoetke, Y. Kubota, J. Mans, V. Rekovic, R. Rusack, M. Sasseville, A. Singovsky
University of Mississippi, University, USA
L.M. Cremaldi, R. Godang, R. Kroeger, L. Perera, R. Rahmat, D.A. Sanders, D. Summers
University of Nebraska-Lincoln, Lincoln, USA
K. Bloom, S. Bose, J. Butt, D.R. Claes, A. Dominguez, M. Eads, J. Keller, T. Kelly, I. Kravchenko,
J. Lazo-Flores, C. Lundstedt, H. Malbouisson, S. Malik, G.R. Snow
State University of New York at Buffalo, Buffalo, USA
U. Baur, A. Godshalk, I. Iashvili, S. Jain, A. Kharchilava, A. Kumar, S.P. Shipkowski, K. Smith
Northeastern University, Boston, USA
G. Alverson, E. Barberis, D. Baumgartel, O. Boeriu, M. Chasco, K. Kaadze, S. Reucroft, J. Swain,
D. Wood, J. Zhang
Northwestern University, Evanston, USA
A. Anastassov, A. Kubik, N. Odell, R.A. Ofierzynski, B. Pollack, A. Pozdnyakov, M. Schmitt,
S. Stoynev, M. Velasco, S. Won
University of Notre Dame, Notre Dame, USA
L. Antonelli, D. Berry, M. Hildreth, C. Jessop, D.J. Karmgard, J. Kolb, T. Kolberg, K. Lannon,
W. Luo, S. Lynch, N. Marinelli, D.M. Morse, T. Pearson, R. Ruchti, J. Slaunwhite, N. Valls,
J. Warchol, M. Wayne, J. Ziegler
The Ohio State University, Columbus, USA
B. Bylsma, L.S. Durkin, J. Gu, C. Hill, P. Killewald, K. Kotov, T.Y. Ling, M. Rodenburg,
G. Williams
Princeton University, Princeton, USA
N. Adam, E. Berry, P. Elmer, D. Gerbaudo, V. Halyo, P. Hebda, A. Hunt, J. Jones, E. Laird,
D. Lopes Pegna, D. Marlow, T. Medvedeva, M. Mooney, J. Olsen, P. Pirou´ , X. Quan, H. Saka,
e
D. Stickland, C. Tully, J.S. Werner, A. Zuranski
University of Puerto Rico, Mayaguez, USA
J.G. Acosta, X.T. Huang, A. Lopez, H. Mendez, S. Oliveros, J.E. Ramirez Vargas,
A. Zatserklyaniy
Purdue University, West Lafayette, USA
E. Alagoz, V.E. Barnes, G. Bolla, L. Borrello, D. Bortoletto, A. Everett, A.F. Garfinkel, Z. Gecse,
L. Gutay, Z. Hu, M. Jones, O. Koybasi, A.T. Laasanen, N. Leonardo, C. Liu, V. Maroussov,
P. Merkel, D.H. Miller, N. Neumeister, I. Shipsey, D. Silvers, A. Svyatkovskiy, H.D. Yoo,
J. Zablocki, Y. Zheng
Purdue University Calumet, Hammond, USA
P. Jindal, N. Parashar
Rice University, Houston, USA
C. Boulahouache, V. Cuplov, K.M. Ecklund, F.J.M. Geurts, J.H. Liu, B.P. Padley, R. Redjimi,
J. Roberts, J. Zabel
University of Rochester, Rochester, USA
B. Betchart, A. Bodek, Y.S. Chung, R. Covarelli, P. de Barbaro, R. Demina, Y. Eshaq, H. Flacher,
27. 25
A. Garcia-Bellido, P. Goldenzweig, Y. Gotra, J. Han, A. Harel, D.C. Miner, D. Orbaker,
G. Petrillo, D. Vishnevskiy, M. Zielinski
The Rockefeller University, New York, USA
A. Bhatti, L. Demortier, K. Goulianos, G. Lungu, C. Mesropian, M. Yan
Rutgers, the State University of New Jersey, Piscataway, USA
O. Atramentov, A. Barker, D. Duggan, Y. Gershtein, R. Gray, E. Halkiadakis, D. Hidas, D. Hits,
A. Lath, S. Panwalkar, R. Patel, A. Richards, K. Rose, S. Schnetzer, S. Somalwar, R. Stone,
S. Thomas
University of Tennessee, Knoxville, USA
G. Cerizza, M. Hollingsworth, S. Spanier, Z.C. Yang, A. York
Texas AM University, College Station, USA
J. Asaadi, R. Eusebi, J. Gilmore, A. Gurrola, T. Kamon, V. Khotilovich, R. Montalvo,
C.N. Nguyen, I. Osipenkov, J. Pivarski, A. Safonov, S. Sengupta, A. Tatarinov, D. Toback,
M. Weinberger
Texas Tech University, Lubbock, USA
N. Akchurin, C. Bardak, J. Damgov, C. Jeong, K. Kovitanggoon, S.W. Lee, P. Mane, Y. Roh,
A. Sill, I. Volobouev, R. Wigmans, E. Yazgan
Vanderbilt University, Nashville, USA
E. Appelt, E. Brownson, D. Engh, C. Florez, W. Gabella, W. Johns, P. Kurt, C. Maguire, A. Melo,
P. Sheldon, J. Velkovska
University of Virginia, Charlottesville, USA
M.W. Arenton, M. Balazs, S. Boutle, M. Buehler, S. Conetti, B. Cox, B. Francis, R. Hirosky,
A. Ledovskoy, C. Lin, C. Neu, R. Yohay
Wayne State University, Detroit, USA
S. Gollapinni, R. Harr, P.E. Karchin, P. Lamichhane, M. Mattson, C. Milst` ne, A. Sakharov
e
University of Wisconsin, Madison, USA
M. Anderson, M. Bachtis, J.N. Bellinger, D. Carlsmith, S. Dasu, J. Efron, L. Gray, K.S. Grogg,
M. Grothe, R. Hall-Wilton1 , M. Herndon, P. Klabbers, J. Klukas, A. Lanaro, C. Lazaridis,
J. Leonard, D. Lomidze, R. Loveless, A. Mohapatra, D. Reeder, I. Ross, A. Savin, W.H. Smith,
J. Swanson, M. Weinberg
†: Deceased
1: Also at CERN, European Organization for Nuclear Research, Geneva, Switzerland
2: Also at Universidade Federal do ABC, Santo Andre, Brazil
3: Also at Laboratoire Leprince-Ringuet, Ecole Polytechnique, IN2P3-CNRS, Palaiseau, France
4: Also at Suez Canal University, Suez, Egypt
5: Also at Soltan Institute for Nuclear Studies, Warsaw, Poland
6: Also at Massachusetts Institute of Technology, Cambridge, USA
7: Also at Universit´ de Haute-Alsace, Mulhouse, France
e
8: Also at Brandenburg University of Technology, Cottbus, Germany
9: Also at Moscow State University, Moscow, Russia
10: Also at Institute of Nuclear Research ATOMKI, Debrecen, Hungary
¨ ¨
11: Also at Eotvos Lor´ nd University, Budapest, Hungary
a
12: Also at Tata Institute of Fundamental Research - HECR, Mumbai, India
13: Also at University of Visva-Bharati, Santiniketan, India
28. 26 A The CMS Collaboration
14: Also at Facolt` Ingegneria Universit` di Roma ”La Sapienza”, Roma, Italy
a a
15: Also at Universit` della Basilicata, Potenza, Italy
a
16: Also at Laboratori Nazionali di Legnaro dell’ INFN, Legnaro, Italy
17: Also at California Institute of Technology, Pasadena, USA
18: Also at Faculty of Physics of University of Belgrade, Belgrade, Serbia
19: Also at University of California, Los Angeles, Los Angeles, USA
20: Also at University of Florida, Gainesville, USA
21: Also at Universit´ de Gen` ve, Geneva, Switzerland
e e
22: Also at Scuola Normale e Sezione dell’ INFN, Pisa, Italy
23: Also at INFN Sezione di Roma; Universit` di Roma ”La Sapienza”, Roma, Italy
a
24: Also at University of Athens, Athens, Greece
25: Also at The University of Kansas, Lawrence, USA
26: Also at Institute for Theoretical and Experimental Physics, Moscow, Russia
27: Also at Paul Scherrer Institut, Villigen, Switzerland
28: Also at University of Belgrade, Faculty of Physics and Vinca Institute of Nuclear Sciences,
Belgrade, Serbia
29: Also at Adiyaman University, Adiyaman, Turkey
30: Also at Mersin University, Mersin, Turkey
31: Also at Izmir Institute of Technology, Izmir, Turkey
32: Also at Kafkas University, Kars, Turkey
33: Also at Suleyman Demirel University, Isparta, Turkey
34: Also at Ege University, Izmir, Turkey
35: Also at Rutherford Appleton Laboratory, Didcot, United Kingdom
36: Also at INFN Sezione di Perugia; Universit` di Perugia, Perugia, Italy
a
37: Also at KFKI Research Institute for Particle and Nuclear Physics, Budapest, Hungary
38: Also at Institute for Nuclear Research, Moscow, Russia
39: Also at Horia Hulubei National Institute of Physics and Nuclear Engineering (IFIN-HH),
Bucharest, Romania
40: Also at Istanbul Technical University, Istanbul, Turkey