Author: "Bartalucci A" / Topic: physics - Searchworks@Jio Institute Digital Library Search Results

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147 results on '"Bartalucci A"'

1. Towards the first mean pressure profile estimate with the NIKA2 Sunyaev-Zeldovich Large Program

Author: Hanser C., Adam R., Ade P., Ajeddig H., André P., Artis E., Aussel H., Bartalucci I., Beelen A., Benoît A., Berta S., Bing L., Bourrion O., Calvo M., Catalano A., De Petris M., Désert F.-X., Doyle S., Driessen E.F.C., Ejlali G., Ferragamo A., Gomez A., Goupy J., Katsioli S., Kéruzoré F., Kramer C., Ladjelate B., Lagache G., Leclercq S., Lestrade J.-F., Macías-Pérez J.F., Madden S.C., Maury A., Mauskopf P., Mayet F., Monfardini A., Moyer-Anin A., Muñoz-Echeverría M., Paliwal A., Payerne C., Perotto L., Pisano G., Pointecouteau E., Ponthieu N., Pratt G. W., Revéret V., Rigby A.J., Ritacco A., Romero C., Roussel H., Ruppin F., Schuster K., Sievers A., and Tucker C.
Subjects: Physics, QC1-999
Abstract: High-resolution mapping of the hot gas in galaxy clusters is a key tool for cluster-based cosmological analyses. Taking advantage of the NIKA2 millimeter camera operated at the IRAM 30-m telescope, the NIKA2 SZ Large Program seeks to get a high-resolution follow-up of 38 galaxy clusters covering a wide mass range at intermediate to high redshift. The measured SZ fluxes will be essential to calibrate the SZ scaling relation and the galaxy clusters mean pressure profile, needed for the cosmological exploitation of SZ surveys. We present in this study a method to infer a mean pressure profile from cluster observations. We have designed a pipeline encompassing the map-making and the thermodynamical properties estimates from maps. We then combine all the individual fits, propagating the uncertainties on integrated quantities, such as R500 or P500, and the intrinsic scatter coming from the deviation to the standard self-similar model. We validate the proposed method on realistic LPSZ-like cluster simulations.
Published: 2024
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2. Investigating the scatter origin in CHEX-MATE galaxy cluster X-ray surface brightness profiles

Author: Bartalucci I.
Subjects: Physics, QC1-999
Abstract: We present the statistical properties and the investigation on the origin of the scatter within the spatially resolved emission measure profiles of the CHEX–MATE sample, formed by 118 galaxy clusters selected via the SZ effect. These objects cover a wide mass, MYSZ500 = [2-15]×1014M⊙, and redshift, z=[0.02, 0.6], range. They have been observed by XMM-Newton with a dedicated program that ensures an unprecedented homogeneous and high quality data. We leveraged this exceptional data set by studying the statistical properties of the surface brightness and emission measure radial profiles. We found that there is a critical scale, R~ 0.4RYSZ500, within which the most morphologically relaxed and disturbed object profiles diverge. Above that radius these differences tend to be within 20%. We complemented the CHEX–MATE clusters with a twin sample drawn from the The Three Hundred suite of cosmological simulations. Leveraging this sample, we were able for the first time to investigate separately the scatter due to projection effects and the one due to cluster-to-cluster differences. We found that projection effects have a smaller impact on the scatter compared to object-to-object differences across all scales. Building on this, we found that below 0.4RYSZ500, the scatter is of the order of 110% reflecting the wide plethora of gas distribution in cluster cores. The scatter is at its minimum, 0.56, in the intermediate range, [0.4-0.8]RYSZ500, despite their morphological status suggesting that clusters are close to the self-similar scenario within this radial range.
Published: 2024
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3. The NIKA2 Sunyaev-Zeldovich Large Program

Author: Perotto L., Adam R., Ade P., Ajeddig H., André P., Artis E., Aussel H., Barrena R., Bartalucci I., Beelen A., Benoît A., Berta S., Bing L., Bourrion O., Calvo M., Catalano A., De Petris M., Désert F.-X., Doyle S., Driessen E. F. C., Ejlali G., Ferragamo A., Gomez A., Goupy J., Hanser C., Katsioli S., Kéruzoré F., Kramer C., Ladjelate B., Lagache G., Leclercq S., Lestrade J.-F., Macías-Pérez J.F., Madden S. C., Maury A., Mauskopf P., Mayet F., Monfardini A., Moyer-Anin A., Muñoz-Echeverría M., Paliwal A., Pisano G., Pointecouteau E., Ponthieu N., Pratt G.W., Revéret V., Rigby A. J., Ritacco A., Romero C., Roussel H., Ruppin F., Schuster K., Sievers A., Tucker C., and Yepes G.
Subjects: Physics, QC1-999
Abstract: The NIKA2 camera operating at the IRAM 30-m telescope excels in high-angular resolution mapping of the thermal Sunyaev-Zel’dovich effect towards galaxy clusters at intermediate and high-redshift. As part of the NIKA2 guaranteed-time, the SZ Large Program (LPSZ) aims at tSZ-mapping a representative sample of SZ-selected galaxy clusters in the catalogues of the Planck satellite and of the Atacama Cosmology Telescope, and also observed in X-ray with XMM-Newton or Chandra. Having completed observations in January 2023, we present tSZ maps of 38 clusters spanning the targeted mass (3 < M500/1014M⊙ < 10) and redshift (0.5 < z < 0.9) range. The first in-depth studies of individual clusters highlight the potential of combining tSZ and X-ray observations at similar angular resolution for precised mass measurements under the hydrostatic assumption MHSE. These were milestones for the development of a standard data analysis pipeline to go from NIKA2 raw data to the thermodynamic properties of galaxy clusters for the upcoming LPSZ data release. Final products will include measurements of the mean pressure profile of unprecedented quality and MHSE-observable scaling relation using a distinctive SZ-selected sample, which will be key for ultimately improving the accuracy of cluster-based cosmology.
Published: 2024
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4. Estimation of the hydrostatic-to-lensing mass bias from resolved cluster masses

Author: Muñoz-Echeverría M., Macías-Pérez J.F., Pratt G.W., Pointecouteau E., Bartalucci I., De Petris M., Ferragamo A., Hanser C., Kéruzoré F., Mayet F., Moyer-Anin A., Paliwal A., Perotto L., and Yepes G.
Subjects: Physics, QC1-999
Abstract: We present a study on the bias of hydrostatic masses with respect to lensing mass estimates for a sample of 53 clusters in a redshift range between z = 0.05 and 1.07. The M500 mass for each cluster was inferred from X-ray and lensing data, without using a priori observable-mass scaling relations. Cluster masses of our reference analysis were reconstructed homogeneously and we assess the systematic dispersion of those homogeneous masses with respect to other published mass estimates. We obtain an hydrostatic-to-lensing mass bias of (1 − b) = 0.74−0.07+0.08 and no significant evidence of evolution with redshift.
Published: 2024
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5. Systematic effects on the upcoming NIKA2 LPSZ scaling relation

Author: Moyer-Anin A., Adam R., Ade P., Ajeddig H., André P., Artis E., Aussel H., Bartalucci I., Beelen A., Benoît A., Berta S., Bing L., Bourrion O., Calvo M., Catalano A., De Petris M., Désert F.-X., Doyle S., Driessen E.F.C., Ejlali G., Gomez A., Goupy J., Hanser C., Katsioli S., Kéruzoré F., Kramer C., Ladjelate B., Lagache G., Leclercq S., Lestrade J.-F., Macías-Pérez J.F., Madden S.C., Maury A., Mauskopf P., Mayet F., Monfardini A., Muñoz-Echeverría M., Paliwal A., Perotto L., Pisano G., Pointecouteau E., Ponthieu N., Pratt G.W., Revéret V., Rigby A.J., Ritacco A., Romero C., Roussel H., Ruppin F., Schuster K., Sievers A., and Tucker C.
Subjects: Physics, QC1-999
Abstract: In cluster cosmology, cluster masses are the main parameter of interest. They are needed to constrain cosmological parameters through the cluster number count. As the mass is not an observable, a scaling relation is needed to link cluster masses to the integrated Compton parameters Y, i.e. the Sunyaev-Zeldovich observable (SZ). Planck cosmological results obtained with cluster number counts are based on a scaling relation measured with clusters at low redshift (z
Published: 2024
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6. Analysis methods used and planned for VIP-2

Author: Porcelli Alessio, Bartalucci Sergio, Bertolucci Sergio, Bazzi Massimiliano, Bragadireanu Mario, Capoccia Cesidio, Cargnelli Michael, Clozza Alberto, Curceanu Catalina, De Paolis Luca, Del Grande Raffaele, Fiorini Carlo, Guaraldo Carlo, Iliescu Mihai, Laubenstein Matthias, Marton Johann, Miliucci Marco, Milotti Edoardo, Napolitano Fabrizio, Piscicchia Kristian, Scordo Alessandro, Shi Hexi, Sirghi Diana Laura, Sirghi Florin, Sgaramella Francesco, Vazquez Doce Oton, and Zmeskal Johann
Subjects: Physics, QC1-999
Abstract: VIP-2 (VIolation of Pauli exclusion principle - 2) is an underground experiment sited in the underground “Laboratori Nazionali del Gran Sasso.” It aims to investigate possible violations of the Pauli Exclusion Principle (PEP) and, in this context, Quantum Gravity models implying violations of PEP. While an upper limit of PEP violation probability is recently published, the data requires further developments of accurate analysis techniques and methods. In this contribution, we present an overview of the methodologies proposed for current and planned analysis.
Published: 2022
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7. Multi-probe analysis of the galaxy cluster CL J1226.9+3332: Hydrostatic mass and hydrostatic-to-lensing bias

Author: Muñoz-Echeverría M., Adam R., Ade P., Ajeddig H., André P., Arnaud M., Artis E., Aussel H., Bartalucci I., Beelen A., Benoît A., Berta S., Bing L., Bourrion O., Calvo M., Catalano A., De Petris M., Désert F.-X., Doyle S., Driessen E. F. C., Ferragamo A., Gomez A., Goupy J., Kéruzoré F., Kramer C., Ladjelate B., Lagache G., Leclercq S., Lestrade J.-F., Macías-Pérez J.-F., Maury A., Mauskopf P., Mayet F., Monfardini A., Paliwal A., Perotto L., Pisano G., Pointecouteau E., Ponthieu N., Pratt G. W., Revéret V., Rigby A. J., Ritacco A., Romero C., Roussel H., Ruppin F., Schuster K., Shu S., Sievers A., Tucker C., and Yepes G.
Subjects: Physics, QC1-999
Abstract: We present a multi-probe analysis of the well-known galaxy cluster CL J1226.9+3332 as a proof of concept for multi-wavelength studies within the framework of the NIKA2 Sunyaev-Zel’dovich Large Program (LPSZ). CL J1226.9+3332 is a massive and high redshift (z = 0.888) cluster that has already been observed at several wavelengths. A joint analysis of the thermal SZ (tSZ) effect at millimeter wavelength with the NIKA2 camera and in X-ray with the XMM-Newton satellite permits the reconstruction of the cluster’s thermodynamical properties and mass assuming hydrostatic equilibrium. We test the robustness of our mass estimates against different definitions of the data analysis transfer function. Using convergence maps reconstructed from the data of the CLASH program we obtain estimates of the lensing mass, which we compare to the estimated hydrostatic mass. This allows us to measure the hydrostatic-to-lensing mass bias and the associated systematic effects related to the NIKA2 measurement. We obtain M500HSE = (7:65 ± 1:03) × 1014M⊙ and M500lens = (7:35 ± 0:65) × 1014M⊙, which implies a HSE-to-lensing bias consistent with 0 within 20%.
Published: 2022
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8. The LPSZ-CLASH galaxy cluster sample: Combining lensing and hydrostatic mass estimates

Author: Muñoz-Echeverría M., Adam R., Ade P., Ajeddig H., André P., Arnaud M., Artis E., Aussel H., Bartalucci I., Beelen A., Benoît A., Berta S., Bing L., Bourrion O., Calvo M., Catalano A., De Petris M., Désert F.-X., Doyle S., Driessen E. F. C., Ferragamo A., Gomez A., Goupy J., Kéruzoré F., Kramer C., Ladjelate B., Lagache G., Leclercq S., Lestrade J.-F., Macías-Pérez J.-F., Maury A., Mauskopf P., Mayet F., Monfardini A., Paliwal A., Perotto L., Pisano G., Pointecouteau E., Ponthieu N., Pratt G. W., Revéret V., Rigby A. J., Ritacco A., Romero C., Roussel H., Ruppin F., Schuster K., Shu S., Sievers A., Tucker C., and Yepes G.
Subjects: Physics, QC1-999
Abstract: Starting from the clusters included in the NIKA sample and in the NIKA2 Sunyaev-Zel’dovich Large Program (LPSZ) we have selected a sample of six common objects with the Cluster Lensing And Supernova survey with Hubble (CLASH) lensing data. For the LPSZ clusters we have at our disposal both high-angular resolution observations of the thermal SZ with NIKA and NIKA2 and X-ray observations with XMM-Newton from which hydrostatic mass estimates can be derived. In addition, the CLASH dataset includes lensing convergence maps that can be converted into lensing estimates of the total mass of the cluster. One-dimensional mass profiles are used to derive integrated mass estimates accounting for systematic effects (data processing, modeling, etc.). Two-dimensional analysis of the maps can reveal substructures in the cluster and, therefore, inform us about the dynamical state of each system. Moreover, we are able to study the hydrostatic mass to lensing mass bias, across different morphology and a range of redshift clusters to give more insight on the hydrostatic mass bias. The analysis presented in this proceeding follows the study discussed in [20].
Published: 2022
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9. PSZ2 G091: A massive double cluster at z ~ 0.822 observed by the NIKA2 camera

Author: Artis E., Adam R., Ade P., Ajeddig H., André P., Arnaud M., Aussel H., Bartalucci I., Beelen A., Benoît A., Berta S., Bing L., Bourrion O., Calvo M., Catalano A., De Petris M., Désert F.-X., Doyle S., Driessen E. F. C., Ferragamo A., Gomez A., Goupy J., Kéruzoré F., Kramer C., Ladjelate B., Lagache G., Leclercq S., Lestrade J.-F., Macías-Pérez J.-F., Maury A., Mauskopf P., Mayet F., Monfardini A., Muñoz-Echeverría M., Paliwal A., Perotto L., Pisano G., Pointecouteau E., Ponthieu N., Pratt G. W., Revéret V., Rigby A. J., Ritacco A., Romero C., Roussel H., Ruppin F., Schuster K., Shu S., Sievers A., Tucker C., and Yepes G.
Subjects: Physics, QC1-999
Abstract: PSZ2 G091.83+26.11 is a massive galaxy cluster with M500 = 7:43 × 1014M⊙ at z = 0:822. This object exhibits a complex morphology with a clear bimodality observed in X-rays. However, it was detected and analysed in the Planck sample as a single, spherical cluster following a universal profile [1]. This model can lead to miscalculations of thermodynamical quantities, like the pressure profile. As future multiwavelength cluster experiments will detect more and more objects at higher redshifts (where we expect the fraction of merging objects to be higher), it is crucial to quantify this systematic effect. In this work, we use high-resolution observations of PSZ2 G091.83+26.11 by the NIKA2 camera to integrate the morphological characteristics of the cluster in our modelling. This is achieved by fitting a two-halo model to the SZ image and then by reconstruction of the resulting projected pressure profile. We then compare these results with the spherical assumption.
Published: 2022
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10. The NIKA2 Sunyaev-Zeldovich Large Program: Precise galaxy cluster physics for an accurate cluster-based cosmology

Author: Perotto L., Adam R., Ade P., Ajeddig H., André P., Arnaud M., Artis E., Aussel H., Bartalucci I., Beelen A., Benoît A., Berta S., Bing L., Bourrion O., Calvo M., Catalano A., De Petris M., Désert F.-X., Doyle S., Driessen E. F. C., Ferragamo A., Gomez A., Goupy J., Kéruzoré F., Kramer C., Ladjelate B., Lagache G., Leclercq S., Lestrade J.-F., Macías-Pérez J.-F., Maury A., Mauskopf P., Mayet F., Monfardini A., Muñoz-Echeverría M., Paliwal A., Pisano G., Pointecouteau E., Ponthieu N., Pratt G.W., Revéret V., Rigby A. J., Ritacco A., Romero C., Roussel H., Ruppin F., Schuster K., Shu S., Sievers A., Tucker C., and Yepes G.
Subjects: Physics, QC1-999
Abstract: The NIKA2 Guaranteed-Time SZ Large Program (LPSZ) is dedicated to the high-angular resolution SZ mapping of a representative sample of 45 SZ-selected galaxy clusters drawn from the catalogues of the Planck satellite, or of the Atacama Cosmology Telescope. The LPSZ sample spans a mass range from 3 to 11 × 1014M⊙ and a redshift range from 0:5 to 0:9, extending to higher redshift and lower mass the previous samples dedicated to the cluster mass calibration and universal properties estimation. The main goals of the LPSZ are the measurement of the average radial profile of the ICM pressure up to R500 by combining NIKA2 with Planck or ACT data, and the estimation of the scaling law between the SZ observable and the mass using NIKA2, XMM-Newton and Planck/ACT data. Furthermore, combining LPSZ data with existing or forthcoming public data in lensing, optical/NIR or radio domains, we will build a consistent picture of the cluster physics and further gain knowledge on the mass estimate as a function of the cluster morphology and dynamical state. We give an overview of the LPSZ, present recent results and discuss the future implication for cosmology with galaxy clusters.
Published: 2022
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11. VIP-2 —High-Sensitivity Tests on the Pauli Exclusion Principle for Electrons

Author: Kristian Piscicchia, Johann Marton, Sergio Bartalucci, Massimiliano Bazzi, Sergio Bertolucci, Mario Bragadireanu, Michael Cargnelli, Alberto Clozza, Raffaele Del Grande, Luca De Paolis, Carlo Fiorini, Carlo Guaraldo, Mihail Iliescu, Matthias Laubenstein, Marco Miliucci, Edoardo Milotti, Fabrizio Napolitano, Andreas Pichler, Alessandro Scordo, Hexi Shi, Diana Laura Sirghi, Florin Sirghi, Laura Sperandio, Oton Vazquez Doce, Johann Zmeskal, and Catalina Curceanu
Subjects: Pauli Principle violation, X-ray spectroscopy, underground experiment, Science, Astrophysics, QB460-466, Physics, QC1-999
Abstract: The VIP collaboration is performing high sensitivity tests of the Pauli Exclusion Principle for electrons in the extremely low cosmic background environment of the underground Gran Sasso National Laboratory INFN (Italy). In particular, the VIP-2 Open Systems experiment was conceived to put strong constraints on those Pauli Exclusion Principle violation models which respect the so-called Messiah–Greenberg superselection rule. The experimental technique consists of introducing a direct current in a copper conductor, and searching for the X-rays emission coming from a forbidden atomic transition from the L shell to the K shell of copper when the K shell is already occupied by two electrons. The analysis of the first three months of collected data (in 2018) is presented. The obtained result represents the best bound on the Pauli Exclusion Principle violation probability which fulfills the Messiah–Greenberg rule.
Published: 2020
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12. A low-mass galaxy cluster as a test-case study for the NIKA2 SZ Large Program

Author: Kéruzoré F., Adam R., Ade P., André P., Andrianasolo A., Arnaud M., Aussel H., Bartalucci I., Beelen A., Benoît A., Bideaud A., Bourrion O., Calvo M., Catalano A., Comis B., De Petris M., Désert F.-X., Doyle S., Driessen E.F.C., Gomez A., Goupy J., Kramer C., Ladjelate B., Lagache G., Leclercq S., Lestrade J.-F., Macías-Pérez J.F., Mauskopf P., Mayet F., Monfardini A., Perotto L., Pisano G., Pointecouteau E., Ponthieu N., Pratt G.W., Revéret V., Ritacco A., Romero C., Roussel H., Ruppin F., Schuster K., Shu S., Sievers A., Tucker C., and Zylka R.
Subjects: Physics, QC1-999
Abstract: High-resolution mapping of the hot gas in galaxy clusters is a key tool for cluster-based cosmological analyses. Taking advantage of the NIKA2 millimeter camera operated at the IRAM 30-m telescope, the NIKA2 SZ Large Program seeks to get a high-resolution follow-up of 45 galaxy clusters covering a wide mass range at high redshift in order to re-calibrate some of the tools needed for the cosmological exploitation of SZ surveys. We present the second cluster analysis of this program, targeting one of the faintest sources of the sample in order to tackle the difficulties in data reduction for such faint, low-SNR clusters. In this study, the main challenge is the precise estimation of the contamination by sub-millimetric point sources, which greatly affects the tSZ map of the cluster. We account for this contamination by performing a joint fit of the SZ signal and of the flux density of the compact sources. A prior knowledge of these fluxes is given by the adjustment of the SED of each source using data from both NIKA2 and the Herschel satellite. The first results are very promising and demonstrate the possibility to estimate thermodynamic properties with NIKA2, even in a compact cluster heavily contaminated by point sources.
Published: 2020
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13. Cluster cosmology with the NIKA2 SZ Large Program

Author: Mayet F., Adam R., Ade P., André P., Andrianasolo A., Arnaud M., Aussel H., Bartalucci I., Beelen A., Benoît A., Bideaud A., Bourrion O., Calvo M., Catalano A., Comis B., De Petris M., Désert F.-X., Doyle S., Driessen E.F.C., Gomez A., Goupy J., Kéruzoré F., Kramer C., Ladjelate B., Lagache G., Leclercq S., Lestrade J.-F., Macías-Pérez J.F., Mauskopf P., Monfardini A., Perotto L., Pisano G., Pointecouteau E., Ponthieu N., Pratt G.W., Revéret V., Ritacco A., Romero C., Roussel H., Ruppin F., Schuster K., Shu S., Sievers A., Tucker C., and Zylka R.
Subjects: Physics, QC1-999
Abstract: The main limiting factor of cosmological analyses based on thermal Sunyaev-Zel’dovich (SZ) cluster statistics comes from the bias and systematic uncertainties that affect the estimates of the mass of galaxy clusters. High-angular resolution SZ observations at high redshift are needed to study a potential redshift or morphology dependence of both the mean pressure profile and of the mass-observable scaling relation used in SZ cosmological analyses. The NIKA2 camera is a new generation continuum instrument installed at the IRAM 30-m telescope. With a large field of view, a high angular resolution and a high-sensitivity, the NIKA2 camera has unique SZ mapping capabilities. In this paper, we present the NIKA2 SZ large program, aiming at observing a large sample of clusters at redshifts between 0.5 and 0.9, and the characterization of the first cluster oberved with NIKA2.
Published: 2020
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14. NIKA: a mm camera for Sunyaev-Zel’dovich science in clusters of galaxies

Author: Macías-Pérez J.F., Adam R., Ade P., André P., Andrianasolo A., Aussel H., Arnaud M., Bartalucci I., Beelen A., Benoît A., Bideaud A., Bourrion O., Calvo M., Catalano A., Comis B., De Petris M., Désert F.-X., Doyle S., Driessen E.F.C., Gomez A., Goupy J., Kéruzoré F., Kramer C., Ladjelate B., Lagache G., Leclercq S., Lestrade J.-F., Mauskopf P., Mayet F., Monfardini A., Perotto L., Pisano G., Pointecouteau E., Ponthieu N., Pratt G.W., Revéret V., Ritacco A., Romero C., Roussel H., Ruppin F., Schuster K., Shu S., Sievers A., Tucker C., and Zylka R.
Subjects: Physics, QC1-999
Abstract: Clusters of galaxies, the largest bound objects in the Universe, constitute a cosmological probe of choice, which is sensitive to both dark matter and dark energy. Within this framework, the Sunyaev-Zel’dovich (SZ) effect has opened a new window for the detection of clusters of galaxies and for the characterization of their physical properties such as mass, pressure and temperature. NIKA, a KID-based dual band camera installed at the IRAM 30-m telescope, was particularly well adapted in terms of frequency, angular resolution, field-of-view and sensitivity, for the mapping of the thermal and kinetic SZ effect in high-redshift clusters. In this paper, we present the NIKA cluster sample and a review of the main results obtained via the measurement of the SZ effect on those clusters: reconstruction of the cluster radial pressure profile, mass, temperature and velocity.
Published: 2020
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15. Mapping the gas thermodynamic properties of the massive cluster merger MOO J1142+1527 at z = 1.2

Author: Ruppin F., Adam R., Ade P., André P., Andrianasolo A., Arnaud M., Aussel H., Bartalucci I., Bautz M.W., Beelen A., Benoît A., Bideaud A., Bourrion O., Brodwin M., Calvo M., Catalano A., Comis B., Decker B., De Petris M., Désert F.-X., Doyle S., Driessen E. F. C., Eisenhardt P. R. M., Gomez A., Gonzalez A. H., Goupy J., Kéruzoré F., Kramer C., Ladjelate B., Lagache G., Leclercq S., Lestrade J.-F., Macías-Pérez J.F., Mauskopf P., Mayet F., McDonald M., Monfardini A., Moravec E., Perotto L., Pisano G., Pointecouteau E., Ponthieu N., Pratt G. W., Revéret V., Ritacco A., Romero C., Roussel H., Schuster K., Shu S., Sievers A., Stanford S. A., Stern D., Tucker C., and Zylka R.
Subjects: Physics, QC1-999
Abstract: We present the results of the analysis of the very massive cluster MOO J1142+1527 at a redshift z = 1.2 based on high angular resolution NIKA2 Sunyaev-Zel’dovich (SZ) and Chandra X-ray data. This multi-wavelength analysis enables us to estimate the shape of the temperature profile with unprecedented precision at this redshift and to obtain a map of the gas entropy distribution averaged along the line of sight. The comparison between the cluster morphological properties observed in the NIKA2 and Chandra maps together with the analysis of the entropy map allows us to conclude that MOOJ1142+1527 is an on-going merger hosting a cool-core at the position of the X-ray peak. This work demonstrates how the addition of spatially-resolved SZ observations to low signal-to-noise X-ray data can bring valuable insights on the intracluster medium thermodynamic properties at z > 1.
Published: 2020
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16. The Cluster HEritage project with XMM-Newton: Mass Assembly and Thermodynamics at the Endpoint of structure formation. I. Programme overview

Author: Alina Streblyanska, Raphael Gavazzi, I. Bartalucci, Mathilde Jauzac, P. S. Corasaniti, Paolo Tozzi, R. F. J. van der Burg, Jack Sayers, Mario Nonino, Dominique Eckert, Franco Vazza, M. Rossetti, S. Molendi, Christine Jones, A. Saro, Stefano Ettori, E. Rasia, A. Ferragamo, Nicolas Clerc, Jean-Baptiste Melin, Jose Alberto Rubino-Martin, Barbara Sartoris, Nobuhiro Okabe, R. T. Duffy, A. Iqbal, Sandrine Pires, F. Andrade-Santos, S. De Grandi, Rossella Cassano, F. Gastaldello, G. Schellenberger, Gustavo Yepes, Annalisa Bonafede, R. Barrena, Mauro Sereno, M. De Petris, Keiichi Umetsu, Etienne Pointecouteau, Paula Tarrío, Hervé Bourdin, Jean-Charles Cuillandre, Klaus Dolag, Chris P. Haines, Pasquale Mazzotta, S. Zarattini, Mario Radovich, Stefano Borgani, L. Salvati, Tiziana Venturi, M. Arnaud, Florian Kéruzoré, Simona Ghizzardi, David J. Barnes, Megan Donahue, Massimo Gaspari, S. Paltani, G. W. Pratt, Myriam Gitti, A. M. C. LeBrun, L. Perotto, S. Burkutean, F. Mayet, Scott T. Kay, Melanie Johnston-Hollitt, Lorenzo Lovisari, Herve Aussel, S. Maurogordato, Ben J Maughan, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), Istituto Nazionale di Astrofisica (INAF), University of Geneva [Switzerland], INAF-IASF Milano, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université de Genève = University of Geneva (UNIGE), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), Arnaud, M., Ettori, S., Pratt, G. W., Rossetti, M., Eckert, D., Gastaldello, F., Gavazzi, R., Kay, S. T., Lovisari, L., Maughan, B. J., Pointecouteau, E., Sereno, M., Bartalucci, I., Bonafede, A., Bourdin, H., Cassano, R., Duffy, R. T., Iqbal, A., Maurogordato, S., Rasia, E., Sayers, J., Andrade-Santos, F., Aussel, H., Barnes, D. J., Barrena, R., Borgani, S., Burkutean, S., Clerc, N., Corasaniti, P. -S., Cuillandre, J. -C., De Grandi, S., De Petris, M., Dolag, K., Donahue, M., Ferragamo, A., Gaspari, M., Ghizzardi, S., Gitti, M., Haines, C. P., Jauzac, M., Johnston-Hollitt, M., Jones, C., Keruzore, F., Lebrun, A. M. C., Mayet, F., Mazzotta, P., Melin, J. -B., Molendi, S., Nonino, M., Okabe, N., Paltani, S., Perotto, L., Pires, S., Radovich, M., Rubino-Martin, J. -A., Salvati, L., Saro, A., Sartoris, B., Schellenberger, G., Streblyanska, A., Tarrio, P., Tozzi, P., Umetsu, K., Van Der Burg, R. F. J., Vazza, F., Venturi, T., Yepes, G., Zarattini, S., Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), UAM.Departamento de Física Teórica, COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Arnaud M., Ettori S., Pratt G.W., Rossetti M., Eckert D., Gastaldello F., Gavazzi R., Kay S.T., Lovisari L., Maughan B.J., Pointecouteau E., Sereno M., Bartalucci I., Bonafede A., Bourdin H., Cassano R., Duffy R.T., Iqbal A., Maurogordato S., Rasia E., Sayers J., Andrade-Santos F., Aussel H., Barnes D.J., Barrena R., Borgani S., Burkutean S., Clerc N., Corasaniti P.-S., Cuillandre J.-C., De Grandi S., De Petris M., Dolag K., Donahue M., Ferragamo A., Gaspari M., Ghizzardi S., Gitti M., Haines C.P., Jauzac M., Johnston-Hollitt M., Jones C., Keruzore F., Lebrun A.M.C., Mayet F., Mazzotta P., Melin J.-B., Molendi S., Nonino M., Okabe N., Paltani S., Perotto L., Pires S., Radovich M., Rubino-Martin J.-A., Salvati L., Saro A., Sartoris B., Schellenberger G., Streblyanska A., Tarrio P., Tozzi P., Umetsu K., Van Der Burg R.F.J., Vazza F., Venturi T., Yepes G., and Zarattini S.
Subjects: Structure formation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, Dark matter, Population, Thermodynamics, FOS: Physical sciences, observation [Cosmology], Astrophysics, clusters: intracluster medium [Galaxies], Astrophysics::Cosmology and Extragalactic Astrophysics, clusters: general [Galaxies], Cosmology: observation, 01 natural sciences, Observations [Cosmology], law.invention, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, law, 0103 physical sciences, Cluster (physics), Planck, education, 010303 astronomy & astrophysics, Galaxy cluster, Physics, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Settore FIS/05, 010308 nuclear & particles physics, Cosmology: observations, Física, Galaxies: clusters: general, Galaxies: clusters: intracluster medium, Astronomy and Astrophysics, Astronomía, Dark matter halo, [SDU]Sciences of the Universe [physics], Space and Planetary Science, symbols, Hydrostatic equilibrium, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Cluster HEritage project with XMM-Newton - Mass Assembly and Thermodynamics at the Endpoint of structure formation (CHEX-MATE) is a three mega-second Multi-Year Heritage Programme to obtain X-ray observations of a minimally-biased, signal-to-noise limited sample of 118 galaxy clusters detected by Planck through the Sunyaev-Zeldovich effect. The programme, described in detail in this paper, aims to study the ultimate products of structure formation in time and mass. It is composed of a census of the most recent objects to have formed (Tier-1: 0.05 < z < 0.2; 2 x 10e14 M_sun < M_500 < 9 x 10e14 M_sun), together with a sample of the highest-mass objects in the Universe (Tier-2: z < 0.6; M_500 > 7.25 x 10e14 M_sun). The programme will yield an accurate vision of the statistical properties of the underlying population, measure how the gas properties are shaped by collapse into the dark matter halo, uncover the provenance of non-gravitational heating, and resolve the major uncertainties in mass determination that limit the use of clusters for cosmological parameter estimation. We will acquire X-ray exposures of uniform depth, designed to obtain individual mass measurements accurate to 15-20% under the hydrostatic assumption. We present the project motivations, describe the programme definition, and detail the ongoing multi-wavelength observational (lensing, SZ, radio) and theoretical effort that is being deployed in support of the project., 27 pages, 11 figures; A&A, in press
Published: 2021

17. High Precision Test of the Pauli Exclusion Principle for Electrons

Author: Kristian Piscicchia, Aidin Amirkhani, Sergio Bartalucci, Sergio Bertolucci, Massimiliano Bazzi, Mario Bragadireanu, Michael Cargnelli, Alberto Clozza, Catalina Curceanu, Raffaele Del Grande, Luca De Paolis, Jean-Pierre Egger, Carlo Fiorini, Carlo Guaraldo, Mihail Iliescu, Matthias Laubenstein, Johann Marton, Marco Miliucci, Edoardo Milotti, Andreas Pichler, Dorel Pietreanu, Alessandro Scordo, Hexi Shi, Diana Laura Sirghi, Florin Sirghi, Laura Sperandio, Oton Vazquez Doce, and Johann Zmeskal
Subjects: Pauli exclusion principle, quantum foundations, X-ray spectroscopy, underground experiment, Physics, QC1-999
Abstract: The VIP-2 experiment aims to perform high precision tests of the Pauli Exclusion Principle for electrons. The method consists in circulating a continuous current in a copper strip, searching for the X radiation emission due to a prohibited transition (from the 2p level to the 1s level of copper when this is already occupied by two electrons). VIP already set the best limit on the PEP violation probability for electrons 1 2 β 2 < 4.7 × 10 − 29 , the goal of the upgraded VIP-2 (VIolation of the Pauli Exclusion Principle-2) experiment is to improve this result of two orders of magnitude at least. The experimental apparatus and the results of the analysis of a first set of collected data will be presented.
Published: 2019
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18. On the Importance of Electron Diffusion in a Bulk-Matter Test of the Pauli Exclusion Principle

Author: Edoardo Milotti, Sergio Bartalucci, Sergio Bertolucci, Massimiliano Bazzi, Mario Bragadireanu, Michael Cargnelli, Alberto Clozza, Catalina Curceanu, Luca De Paolis, Jean-Pierre Egger, Carlo Guaraldo, Mihail Iliescu, Matthias Laubenstein, Johann Marton, Marco Miliucci, Andreas Pichler, Dorel Pietreanu, Kristian Piscicchia, Alessandro Scordo, Hexi Shi, Diana Laura Sirghi, Florin Sirghi, Laura Sperandio, Oton Vázquez Doce, Eberhard Widmann, and Johann Zmeskal
Subjects: Pauli exclusion principle, X-rays, diffusion processes, fundamental symmetries, Science, Astrophysics, QB460-466, Physics, QC1-999
Abstract: The VIolation of Pauli (VIP) experiment (and its upgraded version, VIP-2) uses the Ramberg and Snow (RS) method (Phys. Lett. B 1990, 238, 438) to search for violations of the Pauli exclusion principle in the Gran Sasso underground laboratory. The RS method consists of feeding a copper conductor with a high direct current, so that the large number of newly-injected conduction electrons can interact with the copper atoms and possibly cascade electromagnetically to an already occupied atomic ground state if their wavefunction has the wrong symmetry with respect to the atomic electrons, emitting characteristic X-rays as they do so. In their original data analysis, RS considered a very simple path for each electron, which is sure to return a bound, albeit a very weak one, because it ignores the meandering random walks of the electrons as they move from the entrance to the exit of the copper sample. These complex walks bring the electrons close to many more atoms than in the RS calculation. Here, we consider the full description of these walks and show that this leads to a nontrivial and nonlinear X-ray emission rate. Finally, we obtain an improved bound, which sets much tighter constraints on the violation of the Pauli exclusion principle for electrons.
Published: 2018
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19. Search for the violation of Pauli Exclusion Principle at LNGS

Author: Shi H., Bartalucci S., Bazzi M., Bertolucci S., Bragadireanu A.M., Cargnelli M., Clozza A., Curceanu C., De Paolis L., Di Matteo S., Egger J.-P., Guaraldo C., Iliescu M., Marton J., Laubenstein M., Milotti E., Pichler A., Pietreanu D., Piscicchia K., Scordo A., Sirghi D.L., Sirghi F., Sperandio L., Vazquez Doce O., Widmann E., and Zmeskal J.
Subjects: Physics, QC1-999
Abstract: In the VIP (VIolation of Pauli exclusion principle) and its follow-up VIP- 2 experiments at the Laboratori Nazionali del Gran Sasso, we test the validity of the Pauli Exclusion Principle, by searching for x-rays from copper atomic transitions from a 2p orbit electron to the ground state which is already occupied by two electrons. Such transitions are prohibited by the Pauli Exclusion Principle. The physics run of the VIP-2 experiment started in late 2016 and will collect data for three years. From the first data taking period of two months we have obtained a new limit better than the VIP result from three years of running. In this article we present the published first physics result from the VIP-2 experiment and discuss about the future perspectives.
Published: 2018
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20. Chandra observations of the Planck Early Sunyaev-Zeldovich sample

Author: I. Bartalucci, Monique Arnaud, Alexey Vikhlinin, Felipe Andrade-Santos, Christine Jones, Stephen S. Murray, Reinout J. van Weeren, Lorenzo Lovisari, Jean-Baptiste Melin, Pasquale Mazzotta, William R. Forman, Ralph P. Kraft, Gabriel W. Pratt, Laurence P. David, Stefano Borgani, Etienne Pointecouteau, Simona Giacintucci, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Andrade-Santos, Felipe, Pratt, Gabriel W., Melin, Jean-Baptiste, Arnaud, Monique, Jones, Christine, Forman, William R., Pointecouteau, Etienne, Bartalucci, Iacopo, Vikhlinin, Alexey, Murray, Stephen S., Mazzotta, Pasquale, Borgani, Stefano, Lovisari, Lorenzo, van Weeren, Reinout J., Kraft, Ralph P., David, Laurence P., and Giacintucci, Simona
Subjects: 010504 meteorology & atmospheric sciences, Astrophysics - cosmology and nongalactic astrophysics, Galaxy clusters, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 584, 858, 1654, 01 natural sciences, Astrophysics - high energy astrophysical phenomena, symbols.namesake, Intracluster medium, 0103 physical sciences, Astrophysics - Cosmology and Nongalactic Astrophysic, Planck, 010303 astronomy & astrophysics, Galaxy cluster, Sunyaev-Zeldovich effect, 0105 earth and related environmental sciences, Physics, Settore FIS/05, 584, 858, 1654, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astronomy and Astrophysics, Sample (graphics), Space and Planetary Science, symbols, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Using Chandra observations, we derive the Y-X proxy and associated total mass measurement, M-500(YX), for 147 clusters with z < 0.35 from the Planck early Sunyaev-Zeldovich catalog, and for 80 clusters with z < 0.22 from an X-ray flux-limited sample. We reextract the Planck YSZ measurements and obtain the corresponding mass proxy, M-500(SZ), from the full Planck mission maps, minimizing Malmquist bias due to observational scatter. The masses reextracted using the more precise X-ray position and characteristic size agree with the published PSZ2 values, but yield a significant reduction in the scatter (by a factor of two) in the M-500(SZ) - M-500(YX) relation. The slope is 0.93 +/- 0.03, and the median ratio, M-500(SZ)/M-500(YX) = 0.91 +/- 0.01, is within the expectations from known X-ray calibration systematics. Y-SZ/Y-X is 0.88 +/- 0.02, in good agreement with predictions from cluster structure, and implying a low level of clumpiness. In agreement with the findings of the Planck Collaboration, the slope of the Y-SZ-D-A(-2) Y-X flux relation is significantly less than unity (0.89 +/- 0.01). Using extensive simulations, we show that this result is not due to selection effects, intrinsic scatter, or covariance between quantities. We demonstrate analytically that changing the Y-SZ-Y-X relation from apparent flux to intrinsic properties results in a best-fit slope that is closer to unity and increases the dispersion about the relation. The redistribution resulting from this transformation implies that the best-fit parameters of the M-500(SZ) - M-500(YX) relation will be sample- dependent.
Published: 2021

21. Ultra-Steep Spectrum Radio 'Jellyfish' Uncovered in Abell 2877

Author: Denis Wittor, Franco Vazza, Melanie Johnston-Hollitt, Torrance Hodgson, I. Bartalucci, Benjamin McKinley, Hodgson T., Bartalucci I., Johnston-Hollitt M., McKinley B., Vazza F., and Wittor D.
Subjects: Jellyfish, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Plasma physic, Astrophysics - Astrophysics of Galaxie, Intracluster medium, biology.animal, 0103 physical sciences, Radio astronomy, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Physics, Spectral index, biology, 010308 nuclear & particles physics, Spectrum (functional analysis), Astronomy and Astrophysics, Plasma, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We report on the discovery of a mysterious ultra-steep spectrum (USS) synchrotron source in the galaxy cluster Abell 2877. We have observed the source with the Murchison Widefield Array at five frequencies across 72-231 MHz and have found the source to exhibit strong spectral curvature over this range as well the steepest known spectra of a synchrotron cluster source, with a spectral index across the central three frequency bands of $\alpha = -5.97^{+0.40}_{-0.48}$. Higher frequency radio observations, including a deep observation with the Australia Telescope Compact Array, fail to detect any of the extended diffuse emission. The source is approximately 370 kpc wide and bears an uncanny resemblance to a jellyfish with two peaks of emission and long tentacles descending south towards the cluster centre. Whilst the `USS Jellyfish' defies easy classification, we here propose that the phenomenon is caused by the reacceleration and compression of multiple aged electron populations from historic active galactic nucleus (AGN) activity, so-called `radio phoenix', by an as yet undetected weak cluster-scale mechanism. The USS Jellyfish adds to a growing number of radio phoenix in cool-core clusters with unknown reacceleration mechanisms; as the first example of a polyphoenix, however, this implies the mechanism is on the scale of the cluster itself. Indeed, we show that in simulations, emission akin to the USS Jellyfish can be produced as a short-lived, transient phase in the evolution of multiple interacting AGN remnants when subject to weak external shocks., Comment: Accepted for publication in The Astrophysical Journal
Published: 2021
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22. Iron in x-cop: Tracing enrichment in cluster outskirts with high accuracy abundance profiles

Author: Mariachiara Rossetti, Silvano Molendi, Stefano Ettori, Dominique Eckert, I. Bartalucci, Elena Rasia, Sabrina De Grandi, Remco F. J. van der Burg, Veronica Biffi, Vittorio Ghirardini, Fabio Gastaldello, Simona Ghizzardi, Massimo Gaspari, Stefano Borgani, Ghizzardi, S., Molendi, S., Van Der Burg, R., De Grandi, S., Bartalucci, I., Gastaldello, F., Rossetti, M., Biffi, V., Borgani, S., Eckert, D., Ettori, S., Gaspari, M., Ghirardini, V., and Rasia, E.
Subjects: Systematic error, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, FOS: Physical sciences, clusters: intracluster medium [Galaxies], Astrophysics, clusters: general [Galaxies], Tracing, 01 natural sciences, Abundance (ecology), 0103 physical sciences, Cluster (physics), Range (statistics), 010303 astronomy & astrophysics, Physics, Galaxies: clusters: general, Galaxies: clusters: intracluster medium, X-rays: galaxies: clusters, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: clusters [X-rays], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the first metal abundance profiles for a representative sample of massive clusters. Our measures extend to $R_{500}$ and are corrected for a systematic error plaguing previous outskirt estimates. Our profiles flatten out at large radii, admittedly not a new result, however the radial range and representative nature of our sample extends its import well beyond previous findings. We find no evidence of segregation between cool-core and non-cool-core systems beyond $\sim 0.3 R_{500}$, implying that, as was found for thermodynamic properties (Ghirardini et al, 2019), the physical state of the core does not affect global cluster properties. Our mean abundance within $R_{500}$ shows a very modest scatter, $< $15%, suggesting the enrichment process must be quite similar in all these massive systems. This is a new finding and has significant implications on feedback processes. Together with results from thermodynamic properties presented in a previous X-COP paper, it affords a coherent picture where feedback effects do not vary significantly from one system to another. By combing ICM with stellar measurements we have found the amount of Fe diffused in the ICM to be about ten times higher than that locked in stars. Although our estimates suggest, with some strength, that the measured iron mass in clusters is well in excess of the predicted one, systematic errors prevent us from making a definitive statement. Further advancements will only be possible when systematic uncertainties, principally those associated to stellar masses, both within and beyond $R_{500}$, can be reduced., 23 pages, 23 figures; submitted to A&A
Published: 2021

23. The LPSZ-CLASH galaxy cluster sample: combining lensing and hydrostatic mass estimates

Author: Muñoz-Echeverría M., Adam R., Ade P., Ajeddig H., André P., Arnaud M., Artis E., Aussel H., Bartalucci I., Beelen A., Benoît A., Berta S., Bing L., Bourrion O., Calvo M., Catalano A., De Petris M., Désert F.-X., Doyle S., Driessen E. F. C., Ferragamo A., Gomez A., Goupy J., Kéruzoré F., Kramer C., Ladjelate B., Lagache G., Leclercq S., Lestrade J.-F., Macías-Pérez J.-F., Maury A., Mauskopf P., Mayet F., Monfardini A., Paliwal A., Perotto L., Pisano G., Pointecouteau E., Ponthieu N., Pratt G. W., Revéret V., Rigby A. J., Ritacco A., Romero C., Roussel H., Ruppin F., Schuster K., Shu S., Sievers A., Tucker C., Yepes G., Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut Néel (NEEL), Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Instituto de RadioAstronomía Milimétrica (IRAM), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de physique de l'ENS - ENS Paris (LPENS), Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Hélium : du fondamental aux applications (NEEL - HELFA), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Cryogénie (NEEL - Cryo), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), clusters of galaxies, gravitational lensing, Sunyaev-Zel'dovich effect, Physics, QC1-999, gravitational lensing, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, clusters of galaxies, 0103 physical sciences, Sunyaev-Zel'dovich effect, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010306 general physics, 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Starting from the clusters included in the NIKA sample and in the NIKA2 Sunyaev-Zel'dovich Large Program (LPSZ) we have selected a sample of six common objects with the Cluster Lensing And Supernova survey with Hubble (CLASH) lensing data. For the LPSZ clusters we have at our disposal both high-angular resolution observations of the thermal SZ with NIKA and NIKA2 and X-ray observations with XMM-Newton from which hydrostatic mass estimates can be derived. In addition, the CLASH dataset includes lensing convergence maps that can be converted into lensing estimates of the total mass of the cluster. One-dimensional mass profiles are used to derive integrated mass estimates accounting for systematic effects (data processing, modeling, etc.). Two-dimensional analysis of the maps can reveal substructures in the cluster and, therefore, inform us about the dynamical state of each system. Moreover, we are able to study the hydrostatic mass to lensing mass bias, across different morphology and a range of redshift clusters to give more insight on the hydrostatic mass bias. The analysis presented in this proceeding follows the study discussed in Ferragamo et al. 2021., To appear in the Proceedings of the International Conference entitled "mm Universe @ NIKA2", Rome (Italy), June 2021, EPJ Web of conferences
Published: 2021

24. Search for a remnant violation of the Pauli exclusion principle in a Roman lead target

Author: Matthias Laubenstein, Marco Miliucci, Diana Sirghi, Michael Cargnelli, Massimiliano Bazzi, Dorel Pietreanu, Johann Marton, Luca DeÂ Paolis, C. Guaraldo, Florin Sirghi, Mario Bragadireanu, Edoardo Milotti, Catalina Curceanu, Kristian Piscicchia, Laura Sperandio, Raffaele Del Grande, Oton VazquezÂ Doce, Sergio Bertolucci, Johann Zmeskal, Carlo Fiorini, A. Amirkhani, Sergio Bartalucci, Hexi Shi, Alessandro Scordo, A. Pichler, M. Iliescu, Alberto Clozza, J. P. Egger, Piscicchia, K., Milotti, E., Amirkhani, A., Bartalucci, S., Bertolucci, S., Bazzi, M., Bragadireanu, M., Cargnelli, M., Clozza, A., Del Grande, R., Depaolis, L., Egger, J. -P., Fiorini, C., Guaraldo, C., Iliescu, M., Laubenstein, M., Marton, J., Miliucci, M., Pichler, A., Pietreanu, D., Scordo, A., Shi, H., Sirghi, D. L., Sirghi, F., Sperandio, L., Vazquezdoce, O., Zmeskal, J., and Curceanu, C.
Subjects: Particle physics, Physics and Astronomy (miscellaneous), Cosmic ray, lcsh:Astrophysics, 02 engineering and technology, Electron, 01 natural sciences, Quantum mechanics, Tests of fundamental symmetries, Orders of magnitude (bit rate), X-ray, symbols.namesake, Lead (geology), Pauli exclusion principle, X-rays, 0103 physical sciences, lcsh:QB460-466, 0202 electrical engineering, electronic engineering, information engineering, Tests of fundamental symmetrie, lcsh:Nuclear and particle physics. Atomic energy. Radioactivity, Engineering (miscellaneous), Physics, 010308 nuclear & particles physics, Spin-statistics connection, symbols, lcsh:QC770-798, 020201 artificial intelligence & image processing, National laboratory
Abstract: In this paper we report on the results of two analyses of the data taken with a dedicated VIP-Lead experiment at the Gran Sasso National Laboratory of the INFN. We use measurements taken in an environment that is especially well screened from cosmic rays, with a metal target made of “Roman lead” which is characterised by a low level of intrinsic radioactivity. The analyses lead to an improvement, on the upper bounds of the Pauli Exclusion Principle violation for electrons, which is more than one (four) orders of magnitude, when the electron-atom interactions are described in terms of scatterings (or close encounters) respectively.
Published: 2020
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25. New Concepts in Tests of the Pauli Exclusion Principle in Bulk Matter

Author: J.-P. Egger, Marco Miliucci, Florin Sirghi, Mario Bragadireanu, C. Guaraldo, Sergio Bartalucci, R. Del Grande, L. De Paolis, Hexi Shi, Johann Marton, O. Vazquez Doce, M. Iliescu, Matthias Laubenstein, J. Zmeskal, Diana Sirghi, D. Pietreanu, M. Bazzi, Carlo Fiorini, Alberto Clozza, S. Bertolucci, Edoardo Milotti, A. Pichler, Alessandro Scordo, Catalina Curceanu, K. Piscicchia, Laura Sperandio, A. Amirkhani, Michael Cargnelli, Milotti, E., Piscicchia, K., Amirkhani, A., Bartalucci, S., Bertolucci, S., Bazzi, M., Bragadireanu, M., Cargnelli, M., Clozza, A., Del Grande, R., De Paolis, L., Egger, J. -P., Fiorini, C., Guaraldo, C., Iliescu, M., Laubenstein, M., Marton, J., Miliucci, M., Pichler, A., Pietreanu, D., Scordo, A., Shi, H., Sirghi, D. L., Sirghi, F., Sperandio, L., Vazquez Doce, O., Zmeskal, J., and Curceanu, C.
Subjects: Physics, electron diffusion, 010308 nuclear & particles physics, quantum mechanics, General Physics and Astronomy, experimental tests, quantum mechanic, 01 natural sciences, Theoretical physics, symbols.namesake, Pauli exclusion principle, electron capture, experimental test, 0103 physical sciences, symbols
Abstract: The standard scheme of several tests of the Pauli Exclusion Principle in bulk matter — both in the experiment and in the subsequent data analysis — has long been based on the seminal paper by E. Ramberg, G.A. Snow [Phys. Lett. B 238, 438 (1990)]. The ideas exposed in that paper are so simple and immediate that they have long gone unchallenged. However, while some of the underlying approximations are still valid, other parts of the article must be reconsidered. Here, we discuss some new concepts thatare related to the motion of the electrons in the test metal (the “target” of the experiment) and which have been recently studied in the framework of the VIP-2 Collaboration.
Published: 2020

26. The key role of the Silicon Drift Detectors in testing the Pauli Exclusion Principle for electrons: the VIP-2 experiment

Author: Marco Miliucci, Johann Zmeskal, Sergio Bartalucci, Hexi Shi, Alessandro Scordo, Florin Sirghi, Mario Bragadireanu, J.-P. Egger, D. Pietreanu, S. Bertolucci, Matthias Laubenstein, A. Pichler, K. Piscicchia, Edoardo Milotti, T. Mazzocchi, Johann Marton, A. Amirkhani, Alberto Clozza, Laura Sperandio, M. Bazzi, R. Del Grande, L. De Paolis, Diana Sirghi, C. Guaraldo, Catalina Curceanu, Michael Cargnelli, Carlo Fiorini, M. Veith, M. Iliescu, O. Vazquez Doce, Paolis, L De, Amirkhani, A, Bartalucci, S, Bertolucci, S, Bazzi, M, Bragadireanu, M, Cargnelli, M, Clozza, A, Curceanu, C, Grande, R Del, Egger, J P, Fiorini, C, Guaraldo, C, Iliescu, M, Laubenstein, M, Marton, J, Mazzocchi, T, Miliucci, M, Milotti, E, Pichler, A, Pietreanu, D, Piscicchia, K, Scordo, A, Shi, H, Sirghi, D L, Sirghi, F, Sperandio, L, Vazquez Doce, O, Veith, M, and Zmeskal, J
Subjects: Physics, Paper, History, Silicon, 010308 nuclear & particles physics, Detector, chemistry.chemical_element, Electron, 01 natural sciences, Quantum mechanic, Quantum mechanics, Experimental tests, Spin-statistics connection, Computer Science Applications, Education, ddc, symbols.namesake, Pauli exclusion principle, chemistry, 0103 physical sciences, symbols, Key (cryptography), 010306 general physics
Abstract: The VIP experiment performed an accurate investigation of the Pauli Exclusion Principle for electrons. The apparatus was installed in the Gran Sasso Laboratories of the National Institute of Nuclear Physic in Italy, an underground environment with an extremely low cosmic background. The aim of the experiment was to test the Pauli Exclusion Principle for electrons in a copper target circulated by a Direct Current (DC) current, searching for X-rays emission due to an atomic transition forbidden by Pauli exclusion principle, from the L shell to the K shell of copper when the K shell is already occupied by two electrons. VIP set an upper limit on the Pauli exclusion principle violation probability 1/2β 2 –29. The goal of the upgraded VIP-2 experiment, presently in data taking at Gran Sasso Laboratories, is to improve this limit by two orders of magnitude. The VIP-2 experimental apparatus, in which the Silicon Drift Detectors have the key role of X-ray detectors, and preliminary results are presented.
Published: 2020

27. Testing the Pauli Exclusion Principle in the Cosmic Silence

Author: Florin Sirghi, Michael Cargnelli, Matthias Laubenstein, M. Bazzi, M. Iliescu, J.-P. Egger, Hexi Shi, Alberto Clozza, L. De Paolis, Diana Sirghi, Carlo Fiorini, C. Guaraldo, Mario Bragadireanu, Marco Miliucci, O. Vazquez Doce, Edoardo Milotti, J. Zmeskal, Sergio Bartalucci, Laura Sperandio, D. Pietreanu, Alessandro Scordo, K. Piscicchia, S. Bertolucci, A. Pichler, Catalina Curceanu, R. Del Grande, A. Amirkhani, Johann Marton, Piscicchia, K., Pichler, A., Amirkhani, A., Bartalucci, S., Bertolucci, S., Bazzi, M., Bragadireanu, M., Cargnelli, M., Clozza, A., Del Grande, R., De Paolis, L., Egger, J., Fiorini, C., Guaraldo, C., Iliescu, M., Laubenstein, M., Marton, J., Miliucci, M., Milotti, E., Pietreanu, D., Scordo, A., Shi, H., Sirghi, D. L., Sirghi, F., Sperandio, L., Vazquez Doce, O., Zmeskal, J., and Curceanu, C.
Subjects: Physics, COSMIC cancer database, 010308 nuclear & particles physics, quantum mechanics, General Physics and Astronomy, experimental tests, quantum mechanic, X-ray detectors, 01 natural sciences, Silence, symbols.namesake, Theoretical physics, Pauli exclusion principle, experimental test, 0103 physical sciences, symbols
Abstract: The VIP Collaboration is performing high precision tests of the Pauli Exclusion Principle for electrons in the extremely low cosmic background environment of the Underground Gran Sasso Laboratories of INFN (Italy). The experimental technique consists in introducing a DC current in a copper conductor, searching for Kα PEP-forbidden atomic transitions when the K shell is already occupied by two electrons. VIP set an upper limit on the PEP-violation probability (½) x β^2 < 4.7 × 10^−29. The aim of the upgraded VIP-2 experiment is to improve this result at least by two orders of magnitude. The improved experimental setup and the results of a preliminary data analysis, corresponding to the the first run of the VIP-2 data taking (2016–2017), will be presented.
Published: 2020
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28. VIP-2 - Testing spin-statistics for electrons with high sensitivity

Author: D. Pietreanu, S. Bertolucci, Michael Cargnelli, Florin Sirghi, J.-P. Egger, O. Vazquez-Doce, Matthias Laubenstein, A. Pichler, Johann Zmeskal, Johann Marton, Diana Sirghi, A. Amirkahani, Sergio Bartalucci, M. Bazzi, Hexi Shi, K. Piscicchia, Edoardo Milotti, Alberto Clozza, C. Guaraldo, L. De Paolis, M. Iliescu, Laura Sperandio, Alessandro Scordo, Catalina Curceanu, Mario Bragadireanu, Marton, J., Amirkahani, A., Bartalucci, S., Bazzi, M., Bertolucci, S., Bragadireanu, M., Cargnelli, M., Clozza, A., Curceanu, C., De Paolis, L., Egger, J. -P., Guaraldo, C., Iliescu, M., Laubenstein, M., Milotti, E., Pichler, A., Pietreanu, D., Piscicchia, K., Scordo, A., Shi, H., Sirghi, D., Sirghi, F., Sperandio, L., Vazquez-Doce, O., and Zmeskal, J.
Subjects: Paper, Physics, History, Pauli principle, quantum mechanics, experimental test, quantum mechanic, Electron, 01 natural sciences, ddc, 010305 fluids & plasmas, Computer Science Applications, Education, 0103 physical sciences, Sensitivity (control systems), Atomic physics, 010306 general physics, Spin-½
Abstract: The VIP-2 (VIolation of the Pauli Exclusion Principle) experiment conducted at the Gran Sasso underground laboratory (LNGS) of INFN is searching for possible tiny violations of standard quantum mechanics in copper atoms with extremely high sensitivity. We investigate atomic transitions with precision X-ray spectroscopy in order to test the Pauli Exclusion Principle (PEP) and therefore the spin-statistics theorem. We present the experimental method for the search for "anomalous" (i.e. Pauli-forbidden) X-ray transitions in copper atoms, produced by "new" electrons, which could have a tiny probability to undergo a Pauli-forbidden transition to the 1s ground state already occupied by two electrons. We describe the VIP-2 experimental setup and its recent optimisations. Presently VIP-2 is taking data at LNGS. The goal of VIP-2 is to test PEP for electrons with unprecedented accuracy, down to a limit in the probability that PEP is violated at the level of 10-31 (and using a more elaborate analysis even 10-40). We present current experimental results.
Published: 2020
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29. Multi-probe analysis of the galaxy cluster CL J1226.9+3332: hydrostatic mass and hydrostatic-to-lensing bias

Author: M. Muñoz-Echeverría, R. Adam, P. Ade, H. Ajeddig, P. André, M. Arnaud, E. Artis, H. Aussel, I. Bartalucci, A. Beelen, A. Benoît, S. Berta, L. Bing, O. Bourrion, M. Calvo, A. Catalano, M. De Petris, F.-X. Désert, S. Doyle, E. F. C. Driessen, A. Ferragamo, A. Gomez, J. Goupy, F. Kéruzoré, C. Kramer, B. Ladjelate, G. Lagache, S. Leclercq, J.-F. Lestrade, J.-F. Macías-Pérez, A. Maury, P. Mauskopf, F. Mayet, A. Monfardini, A. Paliwal, L. Perotto, G. Pisano, E. Pointecouteau, N. Ponthieu, G. W. Pratt, V. Revéret, A. J. Rigby, A. Ritacco, C. Romero, H. Roussel, F. Ruppin, K. Schuster, S. Shu, A. Sievers, C. Tucker, G. Yepes, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut Néel (NEEL), Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Instituto de RadioAstronomía Milimétrica (IRAM), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de physique de l'ENS - ENS Paris (LPENS), Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Hélium : du fondamental aux applications (NEEL - HELFA), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Cryogénie (NEEL - Cryo), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Physics, QC1-999, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, CMB, 01 natural sciences, clusters of galaxies, clusters of galaxies, CMB, Sunyaev-Zel'dovich effect, 0103 physical sciences, Sunyaev-Zel'dovich effect, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a multi-probe analysis of the well-known galaxy cluster CL J1226.9+3332 as a proof of concept for multi-wavelength studies within the framework of the NIKA2 Sunyaev-Zeldovich Large Program (LPSZ). CL J1226.9+3332 is a massive and high redshift (z = 0.888) cluster that has already been observed at several wavelengths. A joint analysis of the thermal SZ (tSZ) effect at millimeter wavelength with the NIKA2 camera and in X-ray with the XMM-Newton satellite permits the reconstruction of the cluster thermodynamical properties and mass assuming hydrostatic equilibrium. We test the robustness of our mass estimates against different definitions of the data analysis transfer function. Using convergence maps reconstructed from the data of the CLASH program we obtain estimates of the lensing mass, which we compare to the estimated hydrostatic mass. This allows us to measure the hydrostatic-to-lensing mass bias and the associated systematic effects related to the NIKA2 measurement. We obtain M500HSE = (7.65 +- 1.03) 1014 Msun and M500lens = (7.35 +- 0.65) 1014 Msun, which implies a HSE-to-lensing bias consistent with 0 within 20 percent., Comment: To appear in the Proceedings of the International Conference entitled mm Universe @ NIKA2, Rome (Italy), June 2021, EPJ Web of conferences
Published: 2021
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30. Low-frequency integrated radio spectra of diffuse, steep-spectrum sources in galaxy clusters: palaeontology with the MWA and ASKAP

Author: Melanie Johnston-Hollitt, I. Bartalucci, and S. W. Duchesne
Subjects: Physics, Spectral index, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Radio galaxy, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Murchison Widefield Array, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Low frequency, Spectral line, Space and Planetary Science, Sky, Halo, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, media_common
Abstract: Galaxy clusters have been found to host a range of diffuse, non-thermal emission components, generally with steep, power law spectra. In this work we report on the detection and follow-up of radio halos, relics, remnant radio galaxies, and other fossil radio plasmas in Southern Sky galaxy clusters using the Murchison Widefield Array and the Australian Square Kilometre Array Pathfinder. We make use of the frequency coverage between the two radio interferometers - from 88 to $\sim 900$ MHz - to characterise the integrated spectra of these sources within this frequency range. Highlights from the sample include the detection of a double relic system in Abell 3186, a mini-halo in RXC J0137.2-0912, a candidate halo and relic in Abell 3399, and a complex multi-episodic head-tail radio galaxy in Abell 3164. We compare this selection of sources and candidates to the literature sample, finding sources consistent with established radio power-cluster mass scaling relations. Finally, we use the low-frequency integrated spectral index, $\alpha$ ($S_\nu \propto \nu^\alpha$), of the detected sample of cluster remnants and fossil sources to compare with samples of known halos, relics, remnants and fossils to investigate a possible link between their electron populations. We find the distributions of $\alpha$ to be consistent with relic and halo emission generated by seed electrons that originated in fossil or remnant sources. However, the present sample sizes are insufficient to rule out other scenarios., Comment: 30 pages, 108 individual PDF figures. Accepted for publication in PASA. Images and catalogue available at https://dx.doi.org/10.26185/611f33b774e96
Published: 2021
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31. Exploiting NIKA2/XMM-Newton imaging synergy for intermediate-mass high-z galaxy clusters within the NIKA2 SZ large program: Observations of ACT-CL J0215.4+0030 at z ∼ 0.9

Author: J.-F. Lestrade, C. Kramer, Bilal Ladjelate, L. Perotto, G. Lagache, S. Leclercq, K. F. Schuster, Albrecht Sievers, F. Mayet, Aurélien Benoit, Martino Calvo, Alessandro Monfardini, I. Bartalucci, Florian Ruppin, O. Bourrion, Giampaolo Pisano, V. Revéret, R. Adam, A. Beelen, M. Arnaud, G. W. Pratt, Shibo Shu, Pascale Andre, A. Andrianasolo, J. Goupy, P. A. R. Ade, Alicia Gomez, F.-X. Désert, N. Ponthieu, Florian Kéruzoré, A. Ritacco, C. Romero, Etienne Pointecouteau, J. F. Macías-Pérez, H. Aussel, Carole Tucker, S. Berta, P. D. Mauskopf, A. Catalano, H. Roussel, Simon Doyle, E. F. C. Driessen, M. De Petris, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Université Paris-Saclay, Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Cardiff University, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Hélium : du fondamental aux applications (NEEL - HELFA), Institut Néel (NEEL), Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Cryogénie (NEEL - Cryo), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Instituto de RadioAstronomía Milimétrica (IRAM), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), University of Pennsylvania, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Massachusetts Institute of Technology (MIT), NASA Goddard Space Flight Center (GSFC), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), LVMH Recherche Parfums et Cosmétiques, Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Hélium : du fondamental aux applications (HELFA), Cryogénie (Cryo), Bordeaux Sciences Agro [Gradignan], Ecole Nationale Supérieure des Sciences Agronomiques de Bordeaux-Aquitaine (Bordeaux Sciences Agro), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)
Subjects: Cosmology: observations, Galaxies: clusters: individual: ACT-CL J0215.4+0030, Galaxies: clusters: intracluster medium, Techniques: high angular resolution, Physics, galaxies: clusters: individual: ACT-CL J0215.4+0030, galaxies: clusters: intracluster medium, 010308 nuclear & particles physics, techniques: high angular resolution, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Galaxy, Redshift, law.invention, Space and Planetary Science, Angular diameter, law, Intracluster medium, cosmology: observations, 0103 physical sciences, Cluster (physics), Cluster sampling, Hydrostatic equilibrium, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Galaxy cluster
Abstract: High-resolution mapping of the intracluster medium (ICM) up to high redshift and down to low masses is crucial to derive accurate mass estimates of the galaxy cluster and to understand the systematic eects aecting cosmological studies based on galaxy clusters. We present a spatially resolved Sunyaev-Zel'dovich (SZ)/X-ray analysis of ACT-CL J0215.4+0030, a high-redshift (z = 0:865) galaxy cluster of intermediate mass (M500 ' 3:5 1014 M) observed as part of the ongoing NIKA2 SZ large program, which is a follow-up of a representative sample of objects at 0:5 z 0:9. In addition to the faintness and small angular size induced by its mass and redshift, the cluster is contaminated by point sources that significantly aect the SZ signal. This is therefore an interesting case study for the most challenging sources of the NIKA2 cluster sample. We present the NIKA2 observations of this cluster and the resulting data.We identified the point sources that aect the NIKA2 maps of the cluster as submillimeter galaxies with counterparts in catalogs of sources constructed by the SPIRE instrument on board the Herschel observatory. We reconstructed the ICM pressure profile by performing a joint analysis of the SZ signal and of the point-source component in the NIKA2 150 GHz map. This cluster is a very weak source that lies below the selection limit of the Planck catalog. Nonetheless, we obtained high-quality estimates of the ICM thermodynamical properties with NIKA2. We compared the pressure profile extracted from the NIKA2 map to the pressure profile obtained from X-ray data alone by deprojecting the public XMM-Newton observations of the cluster.We combined the NIKA2 pressure profile with the X-ray deprojected density to extract detailed information on the ICM. The radial distribution of its thermodynamic properties (the pressure, temperature and entropy) indicate that the cluster has a highly disturbed core. We also computed the hydrostatic mass of the cluster, which is compatible with estimations from SZ and X-ray scaling relations. We conclude that the NIKA2 SZ large program can deliver quality information on the thermodynamics of the ICM even for one of its faintest clusters after a careful treatment of the contamination by point sources., With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737)
Published: 2020

32. High Precision Test of the Pauli Exclusion Principle for Electrons

Author: Matthias Laubenstein, M. Iliescu, Laura Sperandio, Johann Marton, Hexi Shi, Sergio Bartalucci, Michael Cargnelli, A. Pichler, Marco Miliucci, J. P. Egger, Dorel Pietreanu, Alberto Clozza, Diana Sirghi, Carlo Fiorini, Kristian Piscicchia, Florin Sirghi, Sergio Bertolucci, Raffaele Del Grande, Massimiliano Bazzi, Mario Bragadireanu, Alessandro Scordo, Luca De Paolis, Oton Vazquez Doce, Johann Zmeskal, Catalina Curceanu, A. Amirkhani, C. Guaraldo, Edoardo Milotti, Piscicchia, Kristian, Amirkhani, Aidin, Bartalucci, Sergio, Bertolucci, Sergio, Bazzi, Massimiliano, Bragadireanu, Mario, Cargnelli, Michael, Clozza, Alberto, Curceanu, Catalina, Del Grande, Raffaele, De Paolis, Luca, Egger, Jean-Pierre, Fiorini, Carlo, Guaraldo, Carlo, Iliescu, Mihail, Laubenstein, Matthia, Marton, Johann, Miliucci, Marco, Milotti, Edoardo, Pichler, Andrea, Pietreanu, Dorel, Scordo, Alessandro, Shi, Hexi, Sirghi, Diana Laura, Sirghi, Florin, Sperandio, Laura, Doce, Oton Vazquez, and Zmeskal, Johann
Subjects: quantum foundation, Particle physics, 02 engineering and technology, Electron, 01 natural sciences, 010305 fluids & plasmas, Pauli exclusion principle, symbols.namesake, Radiation emission, 0103 physical sciences, 0202 electrical engineering, electronic engineering, information engineering, Limit (mathematics), Physics, Condensed Matter Physics, lcsh:QC1-999, quantum foundations, Electronic, Optical and Magnetic Materials, underground experiment, symbols, X-ray spectroscopy, 020201 artificial intelligence & image processing, Continuous current, Order of magnitude, lcsh:Physics
Abstract: The VIP-2 experiment aims to perform high precision tests of the Pauli Exclusion Principle for electrons. The method consists in circulating a continuous current in a copper strip, searching for the X radiation emission due to a prohibited transition (from the 2p level to the 1s level of copper when this is already occupied by two electrons). VIP already set the best limit on the PEP violation probability for electrons 1 2 &beta, 2 &lt, 4.7 &times, 10 &minus, 29 , the goal of the upgraded VIP-2 (VIolation of the Pauli Exclusion Principle-2) experiment is to improve this result of two orders of magnitude at least. The experimental apparatus and the results of the analysis of a first set of collected data will be presented.
Published: 2019
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33. VIP2 in LNGS - Testing the Pauli Exclusion Principle for electrons with high sensitivity

Author: Johann Zmeskal, C. Guaraldo, Matthias Laubenstein, Sergio Bartalucci, Johann Marton, Kristian Piscicchia, A. Pichler, Hexi Shi, A. Amirkhani, M. Milucci, Carlo Fiorini, M. Iliescu, J.-P. Egger, M. Bragadireanu, Alberto Clozza, Michael Cargnelli, Massimiliano Bazzi, L. De Paolis, O. Vazquez-Doce, D. L. Sirghi, Dorel Pietreanu, Sergio Bertolucci, Alessandro Scordo, R. Del Grande, Edoardo Milotti, Laura Sperandio, Catalina Curceanu, Florin Sirghi, Marton, J., Pichler, A., Amirkhani, A., Bartalucci, S., Bazzi, M., Bertolucci, S., Bragadireanu, M., Cargnelli, M., Clozza, A., Curceanu, C., Del Grande, R., De Paolis, L., Egger, J. -P., Fiorini, C., Guaraldo, C., Iliescu, M., Laubenstein, M., Milotti, E., Milucci, M., Pietreanu, D., Piscicchia, K., Scordo, A., Shi, H., Sirghi, D., Sirghi, F., Sperandio, L., Vazquez-Doce, O., and Zmeskal, J.
Subjects: Paper, History, Particle physics, Physics - Instrumentation and Detectors, FOS: Physical sciences, quantum mechanic, Electron, 01 natural sciences, spin-statistics, Education, X-ray, symbols.namesake, Pauli exclusion principle, 0103 physical sciences, X-rays, Sensitivity (control systems), Limit (mathematics), 010306 general physics, Spectroscopy, fundamental symmetrie, Physics, Quantum Physics, 010308 nuclear & particles physics, quantum mechanics, Instrumentation and Detectors (physics.ins-det), Computer Science Applications, ddc, atomic transitions, fundamental symmetries, Underground laboratory, symbols, atomic transition, High Energy Physics::Experiment, Quantum Physics (quant-ph), Ground state
Abstract: The VIP2 (VIolation of the Pauli Exclusion Principle) experiment at the Gran Sasso underground laboratory (LNGS) is searching for possible violations of standard quantum mechanics predictions in atoms at very high sensitivity. We investigate atomic transitions with precision X-ray spectroscopy in order to test the Pauli Exclusion Principle (PEP) and therefore the related spin-statistics theorem. We will present our experimental method for the search for "anomalous" (i.e. Pauli-forbidden) X-ray transitions in copper atoms, produced by "new" electrons, which could have tiny probability to undergo Pauli-forbidden transition to the ground state already occupied by two electrons. We will describe the VIP2 experimental setup, which is taking data at LNGS presently. The goal of VIP2 is to test the PEP for electrons with unprecedented accuracy, down to a limit in the probability that PEP is violated at the level of 10$^{-31}$. We will present current experimental results and discuss implications of a possible violation., Comment: Proceedings of DICE 2018 Conference
Published: 2019

34. A low-mass galaxy cluster as a test-case study for the NIKA2 SZ Large Program

Author: Guilaine Lagache, A. Andrianasolo, Peter A. R. Ade, F. Mayet, Monique Arnaud, V. Revéret, R. Adam, Simon Doyle, Carsten Kramer, Carole Tucker, L. Perotto, Alessandro Monfardini, J.-F. Lestrade, Charles Romero, Giampaolo Pisano, P. Mauskopf, Florian Ruppin, Shibo Shu, Etienne Pointecouteau, Florian Kéruzoré, Samuel Leclercq, F.-X. Désert, Barbara Comis, Ph. André, A. Sievers, I. Bartalucci, Aurelien Bideaud, Ana Gómez, A. Ritacco, K. F. Schuster, G. W. Pratt, Alain Benoit, Herve Aussel, Bilal Ladjelate, Nicolas Ponthieu, R. Zylka, A. Catalano, Helene Roussel, M. De Petris, E. F. C. Driessen, Martino Calvo, Johannes Goupy, Alexandre Beelen, O. Bourrion, J. F. Macías-Pérez, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut Néel (NEEL), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Instituto de RadioAstronomía Milimétrica (IRAM), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Hélium : du fondamental aux applications (NEEL - HELFA), Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Cryogénie (NEEL - Cryo), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), and Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), QC1-999, satellite, clusters of galaxies, CMB, Sunyaev-Zel'dovich effect, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, Telescope, law, gas, 0103 physical sciences, Cluster (physics), thermodynamical, flux: density, 010306 general physics, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Physics, redshift: high, Redshift, Automatic Keywords, galaxy: cluster, Satellite, Millimeter, Low Mass, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Data reduction, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: High-resolution mapping of the hot gas in galaxy clusters is a key tool for cluster-based cosmological analyses. Taking advantage of the NIKA2 millimeter camera operated at the IRAM 30-m telescope, the NIKA2 SZ Large Program seeks to get a high-resolution follow-up of 45 galaxy clusters covering a wide mass range at high redshift in order to re-calibrate some of the tools needed for the cosmological exploitation of SZ surveys. We present the second cluster analysis of this program, targeting one of the faintest sources of the sample in order to tackle the difficulties in data reduction for such faint, low-SNR clusters. In this study, the main challenge is the precise estimation of the contamination by sub-millimetric point sources, which greatly affects the tSZ map of the cluster. We account for this contamination by performing a joint fit of the SZ signal and of the flux density of the compact sources. A prior knowledge of these fluxes is given by the adjustment of the SED of each source using data from both NIKA2 and the \textit{Herschel} satellite. The first results are very promising and demonstrate the possibility to estimate thermodynamic properties with NIKA2, even in a compact cluster heavily contaminated by point sources., 7 pages, to appear in the proceedings of the international conference entitled mm Universe @ NIKA2, Grenoble (France), June 2019, EPJ Web of conferences
Published: 2020

35. Unveiling the merger dynamics of the most massive MaDCoWS cluster at $z = 1.2$ from a multi-wavelength mapping of its intracluster medium properties

Author: P. A. R. Ade, N. Ponthieu, Marshall W. Bautz, A. Catalano, Pascale Andre, E. Pointecouteau, Anthony H. Gonzalez, J. Goupy, S. Leclercq, G. Lagache, Alessandro Monfardini, G. W. Pratt, D. Stern, Alicia Gomez, P. D. Mauskopf, J.-F. Lestrade, I. Bartalucci, A. Beelen, S. A. Stanford, Peter Eisenhardt, Mark Brodwin, Simon Doyle, A. Andrianasolo, Aurélien Benoit, L. Perotto, A. Ritacco, Mike McDonald, K. F. Schuster, Florian Ruppin, F. Mayet, Carole Tucker, C. Kramer, G. Pisano, V. Revéret, B. Decker, Manuel Calvo, M. Arnaud, R. Zylka, B. Comis, A. Bideaud, O. Bourrion, J. F. Macías-Pérez, R. Adam, H. Aussel, Albrecht Sievers, F.-X. Désert, Bilal Ladjelate, H. Roussel, C. Romero, Florian Kéruzoré, Emily Moravec, M. De Petris, E. F. C. Driessen, Shibo Shu, Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut Néel (NEEL), Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Instituto de RadioAstronomía Milimétrica (IRAM), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Hélium : du fondamental aux applications (NEEL - HELFA), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Cryogénie (NEEL - Cryo), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Brodwin, M. [0000-0002-4208-798X], Ade, P. [0000-0002-5127-0401], González, A. H. [0000-0002-0933-8601], Moravec, E. [0000-0001-9793-5416], Romero, C. [0000-0001-5725-0359], Stern, D. [0000-0003-2686-9241], LabEx FOCUS, Agence Nationale de la Recherche (ANR), European Research Council (ERC), National Aeronautics & Space Administration (NASA), Ministerio de Economía y Competitividad (MINECO), Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, and European Commission (EC)
Subjects: X ray astronomy, Structure formation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Galaxy clusters, Sunyaev-Zeldovich effect, X-ray astronomy, High-redshift galaxy clusters, Intracluster medium, Cool cores, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Sunyaev Zeldovich effect, law.invention, law, 0103 physical sciences, Cluster (physics), High redshift galaxy clsuters, 010303 astronomy & astrophysics, Galaxy cluster, 0105 earth and related environmental sciences, Physics, Line-of-sight, Astronomy and Astrophysics, Redshift, Galaxy, Space and Planetary Science, Galaxy clsuters, Hydrostatic equilibrium, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The characterization of the Intracluster Medium (ICM) properties of high-redshift galaxy clusters is fundamental to our understanding of large-scale structure formation processes. We present the results of a multiwavelength analysis of the very massive cluster MOO J1142+1527 at a redshift z = 1.2 discovered as part of the Massive and Distant Clusters of WISE Survey. This analysis is based on high angular resolution Chandra X-ray and NIKA2 Sunyaev-Zel'dovich (SZ) data. The cluster thermodynamic radial profiles have been obtained with unprecedented precision at this redshift and up to 0.7R , thanks to the combination of high-resolution X-ray and SZ data. The comparison between the galaxy distribution mapped in infrared by Spitzer and the morphological properties of the ICM derived from the combined analysis of the Chandra and NIKA2 data leads us to the conclusion that the cluster is an ongoing merger. We have estimated a systematic uncertainty on the cluster total mass that characterizes both the impact of the observed deviations from spherical symmetry and of the core dynamics on the mass profile. We further combine the X-ray and SZ data at the pixel level to obtain maps of the temperature and entropy distributions. We find a relatively low-entropy core at the position of the X-ray peak and high-temperature regions located on its south and west sides. This work demonstrates that the addition of spatially resolved SZ observations to low signal-to-noise X-ray data brings a high information gain on the characterization of the evolution of ICM thermodynamic properties at z > 1., With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737)
Published: 2020

36. Cluster cosmology with the NIKA2 SZ Large Program

Author: Pascal André, Samuel Leclercq, M. De Petris, Herve Aussel, Shibo Shu, Helene Roussel, F. Mayet, Bilal Ladjelate, I. Bartalucci, A. Sievers, Charles Romero, V. Revéret, Aurelien Bideaud, G. W. Pratt, Carole Tucker, Etienne Pointecouteau, Alain Benoit, Barbara Comis, Alexandre Beelen, Philip Daniel Mauskopf, O. Bourrion, J. F. Macías-Pérez, Monique Arnaud, Florian Kéruzoré, Nicolas Ponthieu, Johannes Goupy, Martino Calvo, A. Catalano, J.-F. Lestrade, Alessandro Monfardini, E. F. C. Driessen, Simon Doyle, Giampaolo Pisano, K. F. Schuster, Francois-Xavier Désert, Guilaine Lagache, R. Zylka, Florian Ruppin, Peter A. R. Ade, Ana Gómez, A. Ritacco, A. Andrianasolo, R. Adam, Carsten Kramer, L. Perotto, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut Néel (NEEL), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Instituto de RadioAstronomía Milimétrica (IRAM), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Hélium : du fondamental aux applications (NEEL - HELFA), Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Cryogénie (NEEL - Cryo), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), and Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), QC1-999, Continuum (design consultancy), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, CMB, 01 natural sciences, Cosmology, law.invention, clusters of galaxies, Telescope, clusters of galaxies, CMB, Sunyaev-Zel'dovich effect, law, 0103 physical sciences, Cluster (physics), Angular resolution, 010303 astronomy & astrophysics, Scaling, Galaxy cluster, Physics, 010308 nuclear & particles physics, Redshift, Sunyaev-Zel'dovich effect, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The main limiting factor of cosmological analyses based on thermal Sunyaev-Zel'dovich (SZ) cluster statistics comes from the bias and systematic uncertainties that affect the estimates of the mass of galaxy clusters. High-angular resolution SZ observations at high redshift are needed to study a potential redshift or morphology dependence of both the mean pressure profile and of the mass-observable scaling relation used in SZ cosmological analyses. The NIKA2 camera is a new generation continuum instrument installed at the IRAM 30-m telescope. With a large field of view, a high angular resolution and a high-sensitivity, the NIKA2 camera has unique SZ mapping capabilities. In this paper, we present the NIKA2 SZ large program, aiming at observing a large sample of clusters at redshifts between 0.5 and 0.9, and the characterization of the first cluster oberved with NIKA2., Comment: to appear in the proceedings of the international conference entitled mm Universe @ NIKA2, Grenoble (France), June 2019, EPJ Web of conferences
Published: 2020

37. Analysis of the unconcentrated background of the EPIC-pn camera on board XMM-Newton

Author: David Salvetti, Simona Ghizzardi, Andrea Tiengo, Mariachiara Rossetti, Fabio Gastaldello, Patrick Kühl, Andrea De Luca, I. Bartalucci, Paolo Esposito, Silvano Molendi, and Martino Marelli
Subjects: Photon, 010504 meteorology & atmospheric sciences, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, X-ray detector, FOS: Physical sciences, Cosmic ray, Astrophysics, 01 natural sciences, law.invention, Telescope, law, 0103 physical sciences, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 0105 earth and related environmental sciences, media_common, Astroparticle physics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), X-ray astronomy, Detector, Astronomy and Astrophysics, 3. Good health, 13. Climate action, Space and Planetary Science, Sky, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Our understanding of the background of the EPIC/pn camera onboard XMM-Newton is incomplete. This affects the study of extended sources and can influence the predictions of the background of future X-ray missions. We provide new results based on the analysis of the largest data set ever used. We focus on the unconcentrated component of the EPIC/pn background - supposedly related to cosmic rays interacting with the telescope. We find that the out-field of view region of the pn detector is actually exposed to the sky. After cleaning from the sky contamination, the unconcentrated background does not show significant spatial variations and its time behaviour is anti-correlated with the solar cycle. We find a very tight, linear correlation between unconcentrated backgrounds detected in the EPIC/pn and MOS2 cameras: this permits the correct evaluation of the pn unconcentrated background of each exposure on the basis of MOS2 data, avoiding the use (as usual) of the contaminated pn regions. We find a tight, linear correlation between the pn unconcentrated background and the proton flux in the 630-970 MeV energy band measured by SOHO/EPHIN. Through this relationship we quantify the contribution of cosmic ray interactions to the pn unconcentrated background and we find a second source which contributes to the pn unconcentrated background for a significant fraction (30%-70%), that does not vary with time and is roughly isotropic. Hard X-ray photons of the CXB satisfy all the known properties of this new component. Our findings provide an important observational confirmation of simulation results on ATHENA., Comment: 21 pages, 14 figures, 2 tables; accepted by the Astrophysical Journal
Published: 2020
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38. PSZ2 G091: A massive double cluster atz~ 0.822 observed by the NIKA2 camera

Author: Artis E., Adam R., Ade P., Ajeddig H., André P., Arnaud M., Aussel H., Bartalucci I., Beelen A., Benoît A., Berta S., Bing L., Bourrion O., Calvo M., Catalano A., De Petris M., Désert F.-X., Doyle S., Driessen E. F. C., Ferragamo A., Gomez A., Goupy J., Kéruzoré F., Kramer C., Ladjelate B., Lagache G., Leclercq S., Lestrade J.-F., Macías-Pérez J.-F., Maury A., Mauskopf P., Mayet F., Monfardini A., Muñoz-Echeverría M., Paliwal A., Perotto L., Pisano G., Pointecouteau E., Ponthieu N., Pratt G. W., Revéret V., Rigby A. J., Ritacco A., Romero C., Roussel H., Ruppin F., Schuster K., Shu S., Sievers A., Tucker C., Yepes G., Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Hélium : du fondamental aux applications (NEEL - HELFA), Institut Néel (NEEL), Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Cryogénie (NEEL - Cryo), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Instituto de RadioAstronomía Milimétrica (IRAM), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Physics, QC1-999, FOS: Physical sciences, CMB, 01 natural sciences, clusters of galaxies, clusters of galaxies, CMB, Sunyaev-Zel'dovich effect, 0103 physical sciences, Sunyaev-Zel'dovich effect, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: PSZ2 G091.83+26.11 is a massive galaxy cluster with M500 = 7.43 x 10^14 Msun at z = 0.822. This object exhibits a complex morphology with a clear bimodality observed in X-rays. However, it was detected and analysed in the Planck sample as a single, spherical cluster following a universal profile [1]. This model can lead to miscalculations of thermodynamical quantities, like the pressure profile. As future multiwavelength cluster experiments will detect more and more objects at higher redshifts (where we expect the fraction of merging objects to be higher), it is crucial to quantify this systematic effect. In this work, we use high-resolution observations of PSZ2 G091.83+26.11 by the NIKA2 camera to integrate the morphological characteristics of the cluster in our modelling. This is achieved by fitting a two-halo model to the SZ image and then by reconstruction of the resulting projected pressure profile. We then compare these results with the spherical assumption., Comment: "To appear in the Proceedings of the International Conference entitled "mm Universe @ NIKA2", Rome (Italy), June 2021, EPJ Web of conferences."
Published: 2022

39. Experimental search for the violation of Pauli exclusion principle

Author: S. Bertolucci, A. Pichler, A. M. Bragadireanu, Diana Sirghi, Sergio Bartalucci, S. Di Matteo, L. De Paolis, O. Vazquez Doce, J.-P. Egger, Johann Marton, D. Pietreanu, Edoardo Milotti, M. Bazzi, C. Guaraldo, Florin Sirghi, Johann Zmeskal, Marco Miliucci, Hexi Shi, Laura Sperandio, Matthias Laubenstein, Alessandro Scordo, K. Piscicchia, E. Widmann, Hebatalla Elnaggar, Alberto Clozza, M. Iliescu, Catalina Curceanu, Michael Cargnelli, Shi, H., Milotti, E., Bartalucci, S., Bazzi, M., Bertolucci, S., Bragadireanu, A. M., Cargnelli, M., Clozza, A., De Paolis, L., Di Matteo, S., Egger, J. -P., Elnaggar, H., Guaraldo, C., Iliescu, M., Laubenstein, M., Marton, J., Miliucci, M., Pichler, A., Pietreanu, D., Piscicchia, K., Scordo, A., Sirghi, D. L., Sirghi, F., Sperandio, L., Vazquez Doce, O., Widmann, E., Zmeskal, J., and Curceanu, C.
Subjects: Systematic error, Particle physics, Physics and Astronomy (miscellaneous), Regular Article - Experimental Physics, Electron, 01 natural sciences, Fundamental symmetries, X-ray, symbols.namesake, Pauli exclusion principle, X-rays, 0103 physical sciences, Atom, Limit (mathematics), Fundamental symmetrie, 010306 general physics, Wave function, Engineering (miscellaneous), Physics, 010308 nuclear & particles physics, Background data, Quantum field theory, symbols, Ground state
Abstract: The VIolation of Pauli exclusion principle -2 experiment, or VIP-2 experiment, at the Laboratori Nazionali del Gran Sasso searches for X-rays from copper atomic transitions that are prohibited by the Pauli exclusion principle. Candidate direct violation events come from the transition of a 2p electron to the ground state that is already occupied by two electrons. From the first data taking campaign in 2016 of VIP-2 experiment, we determined a best upper limit of \documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$3.4~\times ~10^{-29}$$\end{document}3.4×10-29 for the probability that such a violation exists. Significant improvement in the control of the experimental systematics was also achieved, although not explicitly reflected in the improved upper limit. By introducing a simultaneous spectral fit of the signal and background data in the analysis, we succeeded in taking into account systematic errors that could not be evaluated previously in this type of measurements.
Published: 2018

40. On the Importance of Electron Diffusion in a Bulk-Matter Test of the Pauli Exclusion Principle

Author: Hexi Shi, M. Cargnelli, Luca De Paolis, K. Piscicchia, Alberto Clozza, Sergio Bartalucci, Marco Miliucci, Florin Sirghi, J. P. Egger, Matthias Laubenstein, Edoardo Milotti, D. Pietreanu, Johann Zmeskal, A. Pichler, Oton Vazquez Doce, Sergio Bertolucci, Laura Sperandio, Alessandro Scordo, Eberhard Widmann, Diana Sirghi, M. Iliescu, C. Guaraldo, Catalina Curceanu, J. Marton, Mario Bragadireanu, Massimiliano Bazzi, Milotti, Edoardo, Bartalucci, Sergio, Bertolucci, Sergio, Bazzi, Massimiliano, Bragadireanu, Mario, Cargnelli, Michael, Clozza, Alberto, Curceanu, Catalina, De Paolis, Luca, Egger, Jean-Pierre, Guaraldo, Carlo, Iliescu, Mihail, Laubenstein, Matthia, Marton, Johann, Miliucci, Marco, Pichler, Andrea, Pietreanu, Dorel, Piscicchia, Kristian, Scordo, Alessandro, Shi, Hexi, Sirghi, Diana, Sirghi, Florin, Sperandio, Laura, Vázquez Doce, Oton, Widmann, Eberhard, and Zmeskal, Johann
Subjects: General Physics and Astronomy, lcsh:Astrophysics, Electron, 01 natural sciences, Article, X-ray, Pauli exclusion principle, symbols.namesake, Quantum mechanics, lcsh:QB460-466, 0103 physical sciences, Atom, X-rays, lcsh:Science, 010306 general physics, Wave function, Physics, diffusion processes, fundamental symmetries, 010308 nuclear & particles physics, Thermal conduction, Random walk, lcsh:QC1-999, Symmetry (physics), symbols, lcsh:Q, diffusion processe, Ground state, lcsh:Physics
Abstract: The VIolation of Pauli (VIP) experiment (and its upgraded version, VIP-2) uses the Ramberg and Snow (RS) method (Phys. Lett. B 1990, 238, 438) to search for violations of the Pauli exclusion principle in the Gran Sasso underground laboratory. The RS method consists of feeding a copper conductor with a high direct current, so that the large number of newly-injected conduction electrons can interact with the copper atoms and possibly cascade electromagnetically to an already occupied atomic ground state if their wavefunction has the wrong symmetry with respect to the atomic electrons, emitting characteristic X-rays as they do so. In their original data analysis, RS considered a very simple path for each electron, which is sure to return a bound, albeit a very weak one, because it ignores the meandering random walks of the electrons as they move from the entrance to the exit of the copper sample. These complex walks bring the electrons close to many more atoms than in the RS calculation. Here, we consider the full description of these walks and show that this leads to a nontrivial and nonlinear X-ray emission rate. Finally, we obtain an improved bound, which sets much tighter constraints on the violation of the Pauli exclusion principle for electrons.
Published: 2018

41. Detector setup of the VIP2 underground experiment at LNGS

Author: S. Di Matteo, Johann Marton, Florin Sirghi, M. Bazzi, Sergio Bartalucci, Matthias Laubenstein, L. De Paolis, Alessandro Scordo, Catalina Curceanu, A. M. Bragadireanu, Michael Cargnelli, Dorel Pietreanu, Edoardo Milotti, Marco Miliucci, Hexi Shi, Johann Zmeskal, D. L. Sirghi, Sergio Bertolucci, A. Pichler, Laura Sperandio, O. Vazquez Doce, E. Widmann, Hebatalla Elnaggar, Alberto Clozza, M. Iliescu, J.-P. Egger, K. Piscicchia, C. Guaraldo, Marton, J., Pichler, A., Shi, H., Milotti, E., Bartalucci, S., Bazzi, M., Bertolucci, S., Bragadireanu, A. M., Cargnelli, M., Clozza, A., Curceanu, C., De Paolis, L., Di Matteo, S., Egger, J. -P., Elnaggar, H., Guaraldo, C., Iliescu, M., Laubenstein, M., Miliucci, M., Pietreanu, D., Piscicchia, K., Scordo, A., Sirghi, D. L., Sirghi, F., Sperandio, L., Vazquez Doce, O., Widmann, E., Zmeskal, J., Stefan Meyer Institut für subatomare Physik (SMI), Osterreichische Akademie der Wissenschaften (ÖAW), Dipartimento di Fisica [Trieste], Università degli studi di Trieste = University of Trieste, Istituto Nazionale di Fisica Nucleare, Sezione di Milano (INFN), Istituto Nazionale di Fisica Nucleare (INFN), Dipartimento di Fisica e Astronomia [Bologna], Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Institut de Physique de Rennes (IPR), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Université de Neuchâtel (UNINE), Utrecht University [Utrecht], Foundational Questions Institute, FQXiAustrian Science Fund, FWF P 30635-N36, W 1252-N27John Templeton Foundation, JTF 58158Museo Storico della Fisica e Centro Studi e Ricerche Enrico Fermi, Centro Fermi, Università degli studi di Trieste, Université de Rennes 1 (UR1), and Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Nuclear and High Energy Physics, Physics - Instrumentation and Detectors, Silicon, 29.40.Gx, Physics::Instrumentation and Detectors, 29.40.Cs, FOS: Physical sciences, chemistry.chemical_element, Cosmic ray, 02 engineering and technology, Scintillator, 01 natural sciences, 7. Clean energy, SDD, 010305 fluids & plasmas, symbols.namesake, Pauli exclusion principle, Optics, Silicon photomultiplier, 0103 physical sciences, 0202 electrical engineering, electronic engineering, information engineering, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Underground experiment, Instrumentation, Nuclear and High Energy Physic, Physics, [PHYS]Physics [physics], Quantum Physics, business.industry, Detector, Instrumentation and Detectors (physics.ins-det), [PHYS.PHYS.PHYS-GEN-PH]Physics [physics]/Physics [physics]/General Physics [physics.gen-ph], SDDs, chemistry, X-ray spectroscopy, Electromagnetic shielding, symbols, 020201 artificial intelligence & image processing, Quantum Physics (quant-ph), business, Energy (signal processing)
Abstract: International audience; The VIP2 experiment tests the Pauli Exclusion Principle with high sensitivity, by searching for Pauli-forbidden atomic transitions from the 2p to the 1s shell in copper at about 8keV. The transition energy of Pauli-forbidden Kα X-rays is shifted by about 300 eV with respect to the normal allowed Kα line. This energy difference can be resolved using Silicon Drift Detectors. The data for this experiment is taken in the Gran Sasso underground laboratory (LNGS), which provides shielding from cosmic radiation. An overview of the detection system of the VIP2 experiment will be given. This includes the Silicon Drift Detectors used as X-ray detectors which provide an energy resolution of around 150 eV at 6 keV and timing information for active shielding. Furthermore, the low maintenance requirement makes them excellent X-ray detectors for the use in an underground laboratory. The VIP2 setup will be discussed which consists of a high current target system and a passive as well as an active shielding system using plastic scintillators read out by Silicon Photomultipliers. © 2018 Elsevier B.V.
Published: 2018

42. Underground Test of Quantum Mechanics: The VIP2 Experiment

Author: Sergio Bartalucci, J.-P. Egger, Mario Bragadireanu, L. De Paolis, Matthias Laubenstein, Angelo Bassi, Florin Sirghi, Alessandro Scordo, Hexi Shi, Edoardo Milotti, Johann Marton, A. Pichler, M. Bazzi, Alberto Clozza, C. Guaraldo, Laura Sperandio, Sandro Donadi, Sergio Bertolucci, E. Widmann, Carolina Berucci, Diana Sirghi, K. Piscicchia, Catalina Curceanu, J. Zmeskal, S. Di Matteo, M. Iliescu, D. Pietreanu, Michael Cargnelli, O. Vazquez-Doce, Andrei Khrennikov, Bourama Toni, Marton, Johann, Bartalucci, S., Bassi, A., Bazzi, M., Bertolucci, S., Berucci, C., Bragadireanu, M., Cargnelli, M., Clozza, A., Curceanu, C., De Paolis, L., Di Matteo, S., Donadi, S., Egger, J. -P., Guaraldo, C., Iliescu, M., Laubenstein, M., Milotti, E., Pichler, A., Pietreanu, D., Piscicchia, K., Scordo, A., Shi, H., Sirghi, D., Sirghi, F., Sperandio, L., Vazquez-Doce, O., Widmann, E., and Zmeskal, J.
Subjects: Physics - Instrumentation and Detectors, Pauli Exclusion Principle, Quantum Mechanics, Symmetries in Physics, FOS: Physical sciences, Electron, 01 natural sciences, symbols.namesake, Pauli exclusion principle, quant-ph, Quantum mechanics, 0103 physical sciences, Atom, Circulating current, Detectors and Experimental Techniques, 010306 general physics, physics.ins-det, General Theoretical Physics, Physics, Quantum Physics, 010308 nuclear & particles physics, Instrumentation and Detectors (physics.ins-det), Quantum Mechanic, Underground laboratory, symbols, Quantum Physics (quant-ph), Wave function collapse
Abstract: We are experimentally investigating possible violations of standard quantum mechanics predictions in the Gran Sasso underground laboratory in Italy. We test with high precision the Pauli exclusion principle and the collapse of the wave function (collapse models). We present our method of searching for possible small violations of the Pauli exclusion principle (PEP) for electrons, through the search for anomalous X-ray transitions in copper atoms, produced by fresh electrons (brought inside the copper bar by circulating current) which could have a non-zero probability to undergo Pauli-forbidden transition to the 1s level already occupied by two electrons, and we describe the VIP2 (Violation of PEP) experiment under data taking at the Gran Sasso underground laboratories. In this paper the new VIP2 setup installed in the Gran Sasso underground laboratory will be presented. The goal of VIP2 is to test the PEP for electrons with unprecedented accuracy, down to a limit in the probability that PEP is violated at the level of 10−31. We show preliminary experimental results and discuss implications of a possible violation.
Published: 2018

43. High precision test of the Pauli Exclusion Principle for electrons

Author: Hexi Shi, M. Veith, R. Del Grande, L. De Paolis, Matthias Laubenstein, Florin Sirghi, J.-P. Egger, Sergio Bartalucci, O. Vazquez Doce, C. Guaraldo, Marco Miliucci, Edoardo Milotti, Mario Bragadireanu, D. Laura Sirghi, Dorel Pietreanu, K. Piscicchia, T. Mazzocchi, Alberto Clozza, Michael Cargnelli, Laura Sperandio, Johann Zmeskal, A. Amirkhani, Sergio Bertolucci, Johann Marton, M. Bazzi, A. Pichler, Catalina Curceanu, M. Iliescu, Alessandro Scordo, and Carlo Fiorini
Subjects: Physics, Paper, History, COSMIC cancer database, 010308 nuclear & particles physics, Electron shell, Electron, Copper conductor, engineering.material, 01 natural sciences, Computer Science Applications, Education, L-shell, ddc, Nuclear physics, symbols.namesake, Pauli exclusion principle, 0103 physical sciences, symbols, engineering, Limit (mathematics), 010306 general physics, Order of magnitude
Abstract: The VIP collaboration is performing high precision tests of the Pauli Exclusion Principle for electrons in the extremely low cosmic background environment of the Underground Gran Sasso Laboratories of INFN (Italy). The experimental technique consists in introducing a DC current in a copper conductor, searching for the X-rays emission due to a PEP-forbidden atomic transition from the L shell to the K shell of copper when the K shell is already occupied by two electrons. VIP set un upper limit on the PEP violation probability 1 2 β 2 < 4.7 × 10 − 29 , the aim of the upgraded VIP-2 experiment is to improve this result by two orders of magnitude at least. The experimental setup and the results of preliminary data analyses will be presented.
Published: 2019

44. The Most Massive galaxy Clusters (M2C) across cosmic time: link between radial total mass distribution and dynamical state

Author: I. Bartalucci, G. W. Pratt, Monique Arnaud, Lorenzo Lovisari, J. Démoclès, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, CNES, European Project: 340519,EC:FP7:ERC,ERC-2013-ADG,M2C(2014), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), and Harvard University-Smithsonian Institution
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), galaxies: clusters: intracluster medium, Dark matter, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, dark matter, law.invention, law, 0103 physical sciences, Cluster (physics), education, 010303 astronomy & astrophysics, Galaxy cluster, Physics, education.field_of_study, Mass distribution, 010308 nuclear & particles physics, Astronomy and Astrophysics, State (functional analysis), Redshift, Space and Planetary Science, X-rays: galaxies: clusters, Hydrostatic equilibrium, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We study the dynamical state and the integrated total mass profiles of 75 massive (M500 > 5 e+14 M_sun) SZ-selected clusters at 0.080.9. Using XMM imaging observations, we characterise the dynamical state with the centroid shift, the concentration, and their combination, M, which simultaneously probes the core and the large scale gas morphology. Using spatially-resolved spectroscopy and assuming hydrostatic equilibrium, we derive the total integrated mass profiles. The mass profile shape is quantified by the sparsity, the ratio of M500 to M2500, the masses at density contrast 500 and 2500, respectively. We study the correlations between the various parameters and their dependence on redshift. We confirm that SZ-selected samples, thought to reflect most closely the underlying cluster population, are dominated by disturbed and non-cool core objects at all z. There is no significant evolution or mass dependence of either the cool core fraction or the centroid shift parameter. The M parameter evolves slightly with z, having a correlation coefficient of rho= -0.2 $\pm$ 0.1 and a null hypothesis p-value of 0.01. In the high mass regime considered here, the sparsity evolves minimally with redshift, increasing by 10% between z0.55, an effect significant at less than 2 sigma. In contrast, the dependence of the sparsity on dynamical state is much stronger, increasing by a factor of $\sim$60% from the 1/3 most relaxed to the 1/3 most disturbed objects, an effect significant at more than 3 sigma. This is the first observational evidence that the shape of the integrated total mass profile in massive clusters is principally governed by the dynamical state, and is only mildly dependent on redshift. We discuss the consequences for the comparison between observations and theoretical predictions., Comment: Accepted for publication in Astronomy & Astrophysics
Published: 2019

45. Mapping the gas thermodynamic properties of the massive cluster merger MOO J1142$+$1527 at z = 1.2

Author: Peter A. R. Ade, Pascal André, Johannes Goupy, I. Bartalucci, Alessandro Monfardini, A. Andrianasolo, Monique Arnaud, Giampaolo Pisano, Mark W. Bautz, Samuel Leclercq, Carole Tucker, Michael McDonald, R. Zylka, Charles Romero, V. Revéret, Alexandre Beelen, Guilaine Lagache, O. Bourrion, J. F. Macías-Pérez, A. Sievers, Anthony H. Gonzalez, Simon Doyle, Ana Gómez, G. W. Pratt, Mark Brodwin, A. Ritacco, Herve Aussel, Florian Kéruzoré, Florian Ruppin, Shibo Shu, F. Mayet, K. F. Schuster, Bilal Ladjelate, Alain Benoit, Aurelien Bideaud, R. Adam, B. Decker, Carsten Kramer, Francois-Xavier Désert, Etienne Pointecouteau, L. Perotto, Nicolas Ponthieu, Barbara Comis, A. Catalano, Philip Daniel Mauskopf, Peter Eisenhardt, Martino Calvo, J.-F. Lestrade, Helene Roussel, Emily Moravec, Daniel Stern, M. De Petris, E. F. C. Driessen, Spencer A. Stanford, Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut Néel (NEEL), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Instituto de RadioAstronomía Milimétrica (IRAM), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Hélium : du fondamental aux applications (NEEL - HELFA), Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Cryogénie (NEEL - Cryo), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères (LERMA (UMR_8112)), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), HEP, INSPIRE, Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology [2007-2019] (Grenoble INP [2007-2019])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Biologie cellulaire des infections virales – Cell biology of viral infection, Centre International de Recherche en Infectiologie - UMR (CIRI), Institut National de la Santé et de la Recherche Médicale (INSERM)-École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National de la Santé et de la Recherche Médicale (INSERM)-École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble [2020-....] (OSUG [2020-....]), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes [2020-....] (UGA [2020-....])-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes [2020-....] (UGA [2020-....]), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Work (thermodynamics), Cosmology and Nongalactic Astrophysics (astro-ph.CO), QC1-999, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, CMB, 01 natural sciences, clusters of galaxies, Entropy (classical thermodynamics), clusters of galaxies, CMB, Sunyaev-Zel'dovich effect, Position (vector), Intracluster medium, 0103 physical sciences, Cluster (physics), Angular resolution, 010303 astronomy & astrophysics, Physics, Line-of-sight, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Redshift, Sunyaev-Zel'dovich effect, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the results of the analysis of the very massive cluster MOO J1142$+$1527 at a redshift $z = 1.2$ based on high angular resolution NIKA2 Sunyaev-Zel'dovich (SZ) and $Chandra$ X-ray data. This multi-wavelength analysis enables us to estimate the shape of the temperature profile with unprecedented precision at this redshift and to obtain a map of the gas entropy distribution averaged along the line of sight. The comparison between the cluster morphological properties observed in the NIKA2 and $Chandra$ maps together with the analysis of the entropy map allows us to conclude that MOO J1142$+$1527 is an on-going merger hosting a cool-core at the position of the X-ray peak. This work demonstrates how the addition of spatially-resolved SZ observations to low signal-to-noise X-ray data can bring valuable insights on the intracluster medium thermodynamic properties at $z>1$., to appear in the proceedings of the international conference entitled mm Universe @ NIKA2, Grenoble (France), June 2019, EPJ Web of conferences
Published: 2019

46. A Two-arm Slot Sinuous Antenna with Improved Polarization Stability

Author: Stefano Maddio, Lorenzo Bartalucci, Monica Righini, Giuseppe Pelosi, Luca Scorrano, and Stefano Selleri
Subjects: Physics, Polarization plane, business.industry, Linear polarization, Bandwidth (signal processing), Astrophysics::Instrumentation and Methods for Astrophysics, Ultra-wideband, Input impedance, Polarization (waves), Dipole, Optics, business, Logarithmic spiral, Computer Science::Information Theory
Abstract: Sinuous antennas are among the most interesting ultra wide band antennas due to they excellent input impedance behavior over extremely large bandwidth. In two-arms configuration, either dipole or slot, they present a linearly polarized field, as opposed to the circularly polarized field of logarithmic spiral antennas. Yet polarization stability of sinuous antenna is at an issue as the polarization plane oscillates in frequency. In this contribution an improved geometry for the sinuous antenna is proposed, aimed at enhancing polarization stability.
Published: 2019

47. Correlated states and nuclear reactions: An experimental test with low energy beams

Author: M. V. Vysotskyy, Vladimir I. Vysotskii, and Sergio Bartalucci
Subjects: Quantum optics, Nuclear reaction, Physics, Nuclear and High Energy Physics, Physics and Astronomy (miscellaneous), Proton, 010308 nuclear & particles physics, Nuclear Theory, Surfaces and Interfaces, Electron, 01 natural sciences, Nuclear physics, 0103 physical sciences, Nuclear astrophysics, Nuclear fusion, Coherent states, lcsh:QC770-798, lcsh:Nuclear and particle physics. Atomic energy. Radioactivity, 010306 general physics, Nucleon, Nuclear Experiment
Abstract: An experimental program is described in this paper, aiming at detecting the formation of correlated coherent states (CCSs) in thin surface layers of crystals when bombarded by a very low energy proton or deuteron beam. CCSs are a generalization of ``nonclassical'' states of light, such as coherent and squeezed states, whose existence has been demonstrated long ago, giving rise to the remarkable development of quantum optics. In other fields, ranging from condensed matter physics to cosmology, such states have been intensively studied, but a clear signature of their existence is still lacking. This may be a clue to several unexplained phenomena, including the strong enhancement of nuclear fusion reaction rates in some crystal lattices, which have been reported on by several experiments and cannot be accounted for by electron screening only. Such an investigation is extremely relevant to nuclear astrophysics studies, few-body nucleon systems, and nucleon nucleon-interaction problems and, in particular, to energy-related nuclear fusion studies.
Published: 2019

48. High density of active galactic nuclei in the outskirts of distant galaxy clusters

Author: Elias Koulouridis, I. Bartalucci, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), and Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112))
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Active galactic nucleus, galaxies: active, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, symbols.namesake, 0103 physical sciences, Cluster (physics), galaxies: interactions, Planck, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Radius, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, South Pole Telescope, Space and Planetary Science, galaxies: clusters: general, Astrophysics of Galaxies (astro-ph.GA), X-rays: galaxies: clusters, symbols, large-scale structure of Universe, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a study of the distribution of X-ray detected active galactic nuclei (AGN) in the five most massive, $M_{500}^{SZ}>10^{14} M_{\odot}$ , and distant, z$\sim$1, galaxy clusters in the \textit{Planck} and South Pole Telescope (SPT)\textit{} surveys. The spatial and thermodynamic individual properties of each cluster have been defined with unprecedented accuracy at this redshift using deep X-ray observations. This is an essential property of our sample in order to precisely determine the $R_{500}^{Y_{\textrm x}}$ radius of the clusters. For our purposes, we computed the X-ray point-like source surface density in 0.5$R_{500}^{Y_{\textrm x}}$ wide annuli up to a clustercentric distance of 4$R_{500}^{Y_{\textrm x}}$, statistically subtracting the background and accounting for the respective average density of optical galaxies. We found a significant excess of X-ray point sources between 2 and 2.5$R_{500}^{Y_{\textrm x}}$ at the 99.9\% confidence level. The results clearly display for the first time strong observational evidence of AGN triggering in the outskirts of high-redshift massive clusters with such a high statistical significance. We argue that the particular conditions at this distance from the cluster centre increase the galaxy merging rate, which is probably the dominant mechanism of AGN triggering in the outskirts of massive clusters., Letter to the editor, accepted in A&A
Published: 2019

49. High Sensitivity Quantum Mechanics Tests in the Cosmic Silence

Author: M. Iliescu, Matthias Laubenstein, Florin Sirghi, K. Piscicchia, Johann Marton, Carlo Fiorini, J.-P. Egger, D. Laura Sirghi, Sergio Bartalucci, C. Guaraldo, A. Amirkhani, Hexi Shi, Alessandro Scordo, O. Vazquez Doce, M. Bazzi, Alberto Clozza, J. Zmeskal, S. Bertolucci, A. Pichler, L. De Paolis, Marco Miliucci, Catalina Curceanu, Edoardo Milotti, Laura Sperandio, D. Pietreanu, Michael Cargnelli, Mario Bragadireanu, and R. Del Grande
Subjects: Silence, Physics, COSMIC cancer database, Quantum mechanics, General Physics and Astronomy, Sensitivity (control systems)
Published: 2021

50. VIP2 at Gran Sasso - Test of the validity of the spin statistics theorem for electrons with X-ray spectroscopy

Author: C. Berucci, Dorel Pietreanu, Johann Zmeskal, Matthias Laubenstein, Massimiliano Bazzi, Sergio Bartalucci, M. Bragadireanu, Eberhard Widmann, Catalina Curceanu, D. L. Sirghi, Hexi Shi, L. De Paolis, M. Iliescu, Alessandro Scordo, J.-P. Egger, Sergio Bertolucci, Florin Sirghi, S. Di Matteo, Michael Cargnelli, O. Vazquez-Doce, Kristian Piscicchia, Alberto Clozza, C. Guaraldo, Edoardo Milotti, Laura Sperandio, Johann Marton, A. Pichler, Stefan Meyer Institut für subatomare Physik (SMI), Laboratori Nazionali di Frascati (LNF), Istituto Nazionale di Fisica Nucleare (INFN), Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Université de Neuchâtel (UNINE), Laboratori Nazionali del Gran Sasso (LNGS), Università degli studi di Trieste, Horia Hulubei National Institute for Physics and Nuclear Engineering, Technische Universität Munchen - Université Technique de Munich [Munich, Allemagne] (TUM), Foundational Questions Institute, FQXiAustrian Science Fund, FWF: P25529-N20, W1252-N27John Templeton Foundation, JTF: 58158CA 15220, Clark K.Jillings C.Kraus C.Saffin J.Scorza S., Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Università degli studi di Trieste = University of Trieste, Marton, J., Pichler, A., Bartalucci, S., Bazzi, M., Bertolucci, S., Berucci, C., Bragadireanu, M., Cargnelli, M., Clozza, A., Curceanu, C., Paolis, L. D., Matteo, S. D., Egger, J. -P., Guaraldo, C., Iliescu, M., Laubenstein, M., Milotti, E., Pietreanu, D., Piscicchia, K., Scordo, A., Shi, H., Sirghi, D., Sirghi, F., Sperandio, L., Vazquez-Doce, O., Widmann, E., and Zmeskal, J.
Subjects: electron, History, Physics - Instrumentation and Detectors, experimental methods, Underground laboratory, X-ray: irradiation, High-precision, Electron, 01 natural sciences, wave function: collapse, Limit (mathematics), Wave function, Wave functions, Physics, [PHYS]Physics [physics], Quantum Physics, symmetry: violation, quantum mechanics, Spin–statistics theorem, Instrumentation and Detectors (physics.ins-det), Pauli principle, Computer Science Applications, symbols, Ground state, Particle physics, spin: statistics, FOS: Physical sciences, Electrons, Education, Pauli exclusion principle, symbols.namesake, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Pauli, 010306 general physics, X-ray spectroscopy, Forbidden transitions, quantum physics, experimental tests, 010308 nuclear & particles physics, X ray spectroscopy, Spin statistics theorems, deep underground detector, [PHYS.PHYS.PHYS-GEN-PH]Physics [physics]/Physics [physics]/General Physics [physics.gen-ph], quantum physic, Gran Sasso, copper: target, X ray transitions, High Energy Physics::Experiment, Wave function collapse, Circulating current, Quantum Physics (quant-ph), Copper
Abstract: In the VIP2 (VIolation of the Pauli Exlusion Principle) experiment at the Gran Sasso underground laboratory (LNGS) we are searching for possible violations of standard quantum mechanics predictions. With high precision we investigate the Pauli Exclusion Principle and the collapse of the wave function (collapse models). We will present our experimental method of searching for possible small violations of the Pauli Exclusion Principle for electrons, via the search for "anomalous" X-ray transitions in copper atoms, produced by "new" electrons (brought inside a copper bar by circulating current) which could have the probability to undergo Pauli-forbidden transition to the ground state (1 s level) already occupied by two electrons. We will describe the concept of the VIP2 experiment taking data at LNGS presently. The goal of VIP2 is to test the PEP for electrons with unprecedented accuracy, down to a limit in the probability that PEP is violated at the level of 10$^{-31}$. We will show preliminary experimental results obtained at LNGS and discuss implications of a possible violation., Comment: Proceedings TAUP 2017
Published: 2017

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