Constraining SUSY using the relic density and the Higgs boson

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Invisible Higgs Decays to Hooperons in the NMSSM

The galactic center excess of gamma ray photons can be naturally explained by light Majorana fermions in combination with a pseudoscalar mediator. The NMSSM provides exactly these ingredients. We show that for neutralinos with a significant singlino component the galactic center excess can be linked to invisible decays of the Standard-Model-like Higgs at the LHC. We find predictions for invisible Higgs branching ratios in excess of 50 percent, easily accessible at the LHC. Constraining the NMSSM through GUT-scale boundary conditions only slightly affects this expectation. Our results complement earlier NMSSM studies of the galactic center excess, which link it to heavy Higgs searches at the LHC.Comment: 23 pages, 24 figures; v2: references adde

Constraining Supersymmetry using the relic density and the Higgs boson

Recent measurements by Planck, LHC experiments, and Xenon100 have significant impact on supersymmetric models and their parameters. We first illustrate the constraints in the mSUGRA plane and then perform a detailed analysis of the general MSSM with 13 free parameters. Using SFitter, Bayesian and Profile Likelihood approaches are applied and their results compared. The allowed structures in the parameter spaces are largely defined by different mechanisms of dark matter annihilation in combination with the light Higgs mass prediction. In mSUGRA the pseudoscalar Higgs funnel and stau co-annihilation processes are still avoiding experimental pressure. In the MSSM stau co-annihilation, the light Higgs funnel, a mixed bino--higgsino region including the heavy Higgs funnel, and a large higgsino region predict the correct relic density. Volume effects and changes in the model parameters impact the extracted mSUGRA and MSSM parameter regions in the Bayesian analysis

MSSM-inflation revisited: Towards a coherent description of high-energy physics and cosmology

The aim of this paper is to highlight the challenges and potential gains surrounding a coherent description of physics from the high-energy scales of inflation down to the lower energy scales probed in particle-physics experiments. As an example, we revisit the way inflation can be realised within an effective Minimal Supersymmetric Standard Model (eMSSM), in which the $LLe$ and $udd$ flat directions are lifted by the combined effect of soft-supersymmetric-breaking masses already present in the MSSM, together with the addition of effective non-renormalizable operators. We clarify some features of the model and address the question of the one-loop Renormalization Group improvement of the inflationary potential, discussing its impact on the fine-tuning of the model. We also compare the parameter space that is compatible with current observations (in particular the amplitude, $A_{\scriptscriptstyle{\mathrm{S}}}$, and the spectral index, $n_{\scriptscriptstyle{\mathrm{S}}}$, of the primordial cosmological fluctuations) at tree level and at one loop, and discuss the role of reheating. Finally we perform combined fits of particle and cosmological observables (mainly $A_{\scriptscriptstyle{\mathrm{S}}}$, $n_{\scriptscriptstyle{\mathrm{S}}}$, the Higgs mass, and the cold-dark-matter energy density) with the one-loop inflationary potential applied to some examples of dark-matter annihilation channels (Higgs-funnel, Higgsinos and A-funnel), and discuss the status of the ensuing MSSM spectra with respect to the LHC searches.Comment: 38 pages, 7 figure

Detection chain and electronic readout of the QUBIC instrument

The Q and U Bolometric Interferometer for Cosmology (QUBIC) Technical Demonstrator (TD) aiming to shows the feasibility of the combination of interferometry and bolometric detection. The electronic readout system is based on an array of 128 NbSi Transition Edge Sensors cooled at 350mK readout with 128 SQUIDs at 1K controlled and amplified by an Application Specific Integrated Circuit at 40K. This readout design allows a 128:1 Time Domain Multiplexing. We report the design and the performance of the detection chain in this paper. The technological demonstrator unwent a campaign of test in the lab. Evaluation of the QUBIC bolometers and readout electronics includes the measurement of I-V curves, time constant and the Noise Equivalent Power. Currently the mean Noise Equivalent Power is ~ 2 x 10⁻¹⁶ W/√Hz

Detection chain and electronic readout of the QUBIC instrument

The Q and U Bolometric Interferometer for Cosmology (QUBIC) Technical Demonstrator (TD) aiming to shows the feasibility of the combination of interferometry and bolometric detection. The electronic readout system is based on an array of 128 NbSi Transition Edge Sensors cooled at 350mK readout with 128 SQUIDs at 1K controlled and amplified by an Application Specific Integrated Circuit at 40K. This readout design allows a 128:1 Time Domain Multiplexing. We report the design and the performance of the detection chain in this paper. The technological demonstrator unwent a campaign of test in the lab. Evaluation of the QUBIC bolometers and readout electronics includes the measurement of I-V curves, time constant and the Noise Equivalent Power. Currently the mean Noise Equivalent Power is ~ 2 x 10⁻¹⁶ W/√Hz

Archeops et Planck-HFI : Etudes des systématiques pour l'analyse du fond diffus cosmologique

LAL 06-54The work presented in this document is driven by the characterisation of the Archeops and Planck-HFI instruments as well as the fight against systematics in order to reconstruct the power spectrum of the temperature anisotropies of the Cosmic Microwave Background. An introduction on the physics is followed, in a first part, by the description of the calibration of the bolometers of the two instruments using pulsed sources made of carbon fibers that we have developped for measurements of optical leakages between the different cryogenic stages of the focal plane. We explain the analysis of the optical leakages of the Archeops instrument, in combination with measurements of crosstalks and time constants of the bolometers of the Planck's cryogenic qualification model. We also present an analysis of the thermal conductivity and calorific capacity of the fibers that has be done for modelling the thermal behaviour and the emission of these sources.The second part is dedicated to the analysis of systematic effects on the temperature anisotropies analysis. We describe the measurement of the beams (on the ground and in-flight), the analysis of the bolometer time constants, and the flux calibration on Jupiter data for Archeops. We show how to extract the Fourier spectrum on the circles and what we learn on the cosmic microwave background from such an analysis, which we illustrate on Archeops' data.The last chapter deals with a proposal for a full sky submillimeter survey for the measurement of the dust polarisation in the galaxy with a high spatial resolution.Les travaux présentés dans ce manuscrit ont comme fil conducteur la compréhension des détecteurs des instruments Archeops et Planck-HFI ainsi que la lutte contre les effets systématiques dans le but de reconstruire le spectre de puissance des anisotropies de température du Fond Diffus Cosmologique. Après une introduction sur la physique, nous décrivons, dans une première partie, l'étalonnage des bolomètres des deux instruments à partir de sources pulsées constituées de fibres de carbone que nous avons mises au point pour mesurer les fuites optiques entre les différents étages cryogéniques du plan focal. Nous montrons l'analyse de ces fuites optiques à partir des données d'Archeops, ainsi que les mesures de diaphonie et de constantes de temps des bolomètres du modèle cryogénique de Planck-HFI. Nous présentons également l'analyse de la conductivité thermique et de la capacité calorifique des fibres afin de modéliser le comportement thermique et l'émission de ces sources.La seconde partie est consacrée à l'étude des effets systématiques de l'analyse des anisotropies. Nous décrivons les mesures des lobes au sol et en vol, l'analyse des constantes de temps des bolomètres et l'étalonnage en flux à partir des données sur Jupiter pour Archeops. Nous montrons ensuite comment extraire les spectres de Fourier sur les cercles et comment cette dernière analyse nous renseigne sur le fond diffus, ce que nous illustrons avec les données de vol d'Archeops.Le dernier chapitre présente un projet de mission submillimétrique permettant de cartographier tout le ciel à grande résolution dans le but de mesurer la polarisation de la poussière dans la galaxie

(Some) Polarisation Aspects of the Cosmic Microwave Background

International audienceThe purpose of this document is to address the polarisation of the Cosmic Microwave Background. I will first present what it is, and why we do measure its temperature and polarisation (and focus on the cosmological aspects of this characterisation). Then I will discuss what we have learned with its polarisation and what are the next challenges

Robust constraints on tensor perturbations from cosmological data: a comparative analysis from Bayesian and frequentist perspectives

International audienceWe analyze primordial tensor perturbations using the latest cosmic microwave background and gravitational waves data, focusing on the tensor-to-scalar ratio, $r$, and the tensor spectral tilt, $n_t$. Utilizing data from Planck PR4, BICEP/Keck, and LIGO-Virgo-KAGRA, we employ both Bayesian and frequentist methods to provide robust constraints on these parameters. Our results indicate more conservative upper limits for $r$ with profile likelihoods compared to Bayesian credible intervals, highlighting the influence of prior selection and volume effects. The profile likelihood for $n_t$ shows that the current data do not provide sufficient information to derive quantitative bounds, unless extra assumptions on $r$ are used. Additionally, we conduct a 2D profile likelihood analysis of $r$ and $n_t$, indicating a closer agreement between both statistical methods for the largest values of $r$. This study not only updates our understanding of the tensor perturbations but also highlights the importance of employing both statistical methods to explore less constrained parameters, crucial for future explorations in cosmology

Cosmology with the Planck T-E correlation coefficient

International audienceTensions in cosmological parameters measurement motivate a revisit of the effects of instrumental systematics. In this article, we focus on the Pearson’s correlation coefficient of the cosmic microwave background temperature and polarization E modes RℓTE, which has the property of not being biased by multiplicative instrumental systematics. We build a RℓTE-based likelihood for the Planck data and present the first constraints on ΛCDM (Lambda cold dark matter) parameters from the correlation coefficient. Our results are compatible with parameters derived from a power-spectra-based likelihood. In particular, the value of the Hubble parameter H0 characterizing the expansion of the Universe today, 67.5±1.3  km/s/Mpc, is consistent with the ones inferred from standard cosmic microwave background analysis. We also discuss the consistency of the Planck correlation coefficient with the one computed from the most recent ACTPol power spectra