66 research outputs found

    DEMNUni: cross-correlating the nonlinear ISWRS effect with CMB-lensing and galaxies in the presence of massive neutrinos

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    We present a novel analytical approach to study the cross-correlations between the Integrated Sachs Wolfe--Rees Sciama (ISWRS) effects and large-scale structure tracers in the presence of massive neutrinos. Our method has been validated against large N-body simulations with a massive neutrino particle component, namely the DEMNUni suite. We investigate the impact of different neutrino masses on the cross-correlations between ISWRS and both Cosmic Microwave Background (CMB) lensing and galaxies. We show that the position of the sign inversion due to nonlinear effects is strongly related to the neutrino mass. While such nonlinear cross-correlation signals may not be able alone to constrain the neutrino mass, our approach paves the way for future studies to detect the amplitude of these cross-spectra on small scales, and to explore the combined impact of dark energy and neutrino mass from future galaxy surveys and CMB experiments.Comment: 31 pages , 15 fig

    DEMNUni: The imprint of massive neutrinos on the cross-correlation between cosmic voids and CMB lensing

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    International audienceCosmic voids are a powerful probe of cosmology and are one of the core observables of upcoming galaxy surveys. The cross-correlations between voids and other large-scale structure tracers such as galaxy clustering and galaxy lensing have been shown to be very sensitive probes of cosmology and among the most promising to probe the nature of gravity and the neutrino mass. However, recent measurements of the void imprint on the lensed Cosmic Microwave Background (CMB) have been shown to be in tension with expectations based on LCDM simulations, hinting to a possibility of non-standard cosmological signatures due to massive neutrinos. In this work we use the DEMNUni cosmological simulations with massive neutrino cosmologies to study the neutrino impact on voids selected in photometric surveys, e.g. via Luminous Red Galaxies, as well as on the void- CMB lensing cross-correlation. We show how the void properties observed in this way (size function, profiles) are affected by the presence of massive neutrinos compared to the neutrino massless case, and show how these can vary as a function of the selection method of the void sample. We comment on the possibility for massive neutrinos to be the source of the aforementioned tension. Finally, we identify the most promising setup to detect signatures of massive neutrinos in the voids-CMB lensing cross-correlation and define a new quantity useful to distinguish among different neutrino masses by comparing future observations against predictions from simulations including massive neutrinos

    DEMNUni: The imprint of massive neutrinos on the cross-correlation between cosmic voids and CMB lensing

    No full text
    International audienceCosmic voids are a powerful probe of cosmology and are one of the core observables of upcoming galaxy surveys. The cross-correlations between voids and other large-scale structure tracers such as galaxy clustering and galaxy lensing have been shown to be very sensitive probes of cosmology and among the most promising to probe the nature of gravity and the neutrino mass. However, recent measurements of the void imprint on the lensed Cosmic Microwave Background (CMB) have been shown to be in tension with expectations based on LCDM simulations, hinting to a possibility of non-standard cosmological signatures due to massive neutrinos. In this work we use the DEMNUni cosmological simulations with massive neutrino cosmologies to study the neutrino impact on voids selected in photometric surveys, e.g. via Luminous Red Galaxies, as well as on the void- CMB lensing cross-correlation. We show how the void properties observed in this way (size function, profiles) are affected by the presence of massive neutrinos compared to the neutrino massless case, and show how these can vary as a function of the selection method of the void sample. We comment on the possibility for massive neutrinos to be the source of the aforementioned tension. Finally, we identify the most promising setup to detect signatures of massive neutrinos in the voids-CMB lensing cross-correlation and define a new quantity useful to distinguish among different neutrino masses by comparing future observations against predictions from simulations including massive neutrinos

    Open Day presso l’INAF IASF di Milano Report delle prime tre edizioni (2019, 2020, 2022)

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    Nel 2019, l’Istituto di Astrofisica Spaziale e Fisica cosmica di Milano (IASF), una delle due sedi di Milano dell’INAF (Istituto Nazionale di Astrofisica), ha inaugurato il proprio Open Day, una giornata dedicata agli studenti universitari. Il personale dello IASF ha aperto le porte agli studenti interessati a svolgere un progetto di ricerca presso la propria sede o, in generale, a scoprire una realtà professionale dedicata allo studio dell’Universo. Gli incontri si sono divisi in due parti: nella prima sono stati presentati l’Istituto, la sua storia, le attività di ricerca in corso e le Tesi a disposizione (triennali e magistrali), mentre nella seconda si ù aperta una discussione libera tra i presenti durante una merenda offerta dallo IASF-Milano. Le tre edizioni svolte finora (2019, 2020 e 2022) hanno visto una buona partecipazione (circa 25-40 presenze all’anno) e hanno permesso di avvicinare ulteriormente lo IASF-Milano alle Università del territorio, dando ai partecipanti una percezione di disponibilità e accessibilità della ricerca e del personale dello IASF. Dopo una pausa dovuta alla pandemia (anno 2021), lo IASF-Milano ha riaperto le porte nel 2022 in quella che ci auguriamo possa diventare una lunga tradizione

    DEMNUni: The imprint of massive neutrinos on the cross-correlation between cosmic voids and CMB lensing

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    Cosmic voids are a powerful probe of cosmology and are one of the core observables of upcoming galaxy surveys. The cross-correlations between voids and other large-scale structure tracers such as galaxy clustering and galaxy lensing have been shown to be very sensitive probes of cosmology and among the most promising to probe the nature of gravity and the neutrino mass. However, recent measurements of the void imprint on the lensed Cosmic Microwave Background (CMB) have been shown to be in tension with expectations based on LCDM simulations, hinting to a possibility of non-standard cosmological signatures due to massive neutrinos. In this work we use the DEMNUni cosmological simulations with massive neutrino cosmologies to study the neutrino impact on voids selected in photometric surveys, e.g. via Luminous Red Galaxies, as well as on the void- CMB lensing cross-correlation. We show how the void properties observed in this way (size function, profiles) are affected by the presence of massive neutrinos compared to the neutrino massless case, and show how these can vary as a function of the selection method of the void sample. We comment on the possibility for massive neutrinos to be the source of the aforementioned tension. Finally, we identify the most promising setup to detect signatures of massive neutrinos in the voids-CMB lensing cross-correlation and define a new quantity useful to distinguish among different neutrino masses by comparing future observations against predictions from simulations including massive neutrinos.Comment: 34 pages, 15 figure

    COVMOS: a new Monte Carlo approach for galaxy clustering analysis

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    We validate the COVMOS method introduced in Baratta et al. (2019) allowing for the fast simulation of catalogues of different cosmological field tracers (e.g. dark matter particles, halos, galaxies, etc.). The power spectrum and one-point probability distribution function of the underlying tracer density field are set as inputs of the method and are arbitrarily chosen by the user. In order to evaluate the validity domain of COVMOS at the level of the produced two-point statistics covariance matrix, we choose to target these two input statistical quantities from realistic NN-body simulation outputs. In particular, we perform this cloning procedure in a Λ\LambdaCDM and in a massive neutrino cosmologies, for five redshifts in the range z∈[0,2]z\in[0,2]. First, we validate the output real-space two-point statistics (both in configuration and Fourier space) estimated over 5,0005,000 COVMOS realisations per redshift and per cosmology, with a volume of 1 [Gpc/h]31\ [\mathrm{Gpc}/h]^3 and 10810^8 particles each. Such a validation is performed against the corresponding NN-body measurements, estimated from 50 simulations. We find the method to be valid up to k∌0.2h/k\sim 0.2h/Mpc for the power spectrum and down to r ∌20r~\sim 20 Mpc/h/h for the correlation function. Then, we extend the method by proposing a new modelling of the peculiar velocity distribution, aiming at reproducing the redshift-space distortions both in the linear and mildly non-linear regimes. After validating this prescription, we finally compare and validate the produced redshift-space two-point statistics covariance matrices in the same range of scales. We release on a public repository the Python code associated with this method, allowing the production of tens of thousands of realisations in record time. COVMOS is intended for any user involved in large galaxy-survey science requiring a large number of mock realisations

    Cosmology with the Laser Interferometer Space Antenna

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    The Laser Interferometer Space Antenna (LISA) has two scientific objectives of cosmological focus: to probe the expansion rate of the universe, and to understand stochastic gravitational-wave backgrounds and their implications for early universe and particle physics, from the MeV to the Planck scale. However, the range of potential cosmological applications of gravitational wave observations extends well beyond these two objectives. This publication presents a summary of the state of the art in LISA cosmology, theory and methods, and identifies new opportunities to use gravitational wave observations by LISA to probe the universe

    Euclid preparation XIII. Forecasts for galaxy morphology with the Euclid Survey using deep generative models

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    We present a machine learning framework to simulate realistic galaxies for the Euclid Survey, producing more complex and realistic galaxies than the analytical simulations currently used in Euclid. The proposed method combines a control on galaxy shape parameters offered by analytic models with realistic surface brightness distributions learned from real Hubble Space Telescope observations by deep generative models. We simulate a galaxy field of 0.4 deg2 as it will be seen by the Euclid visible imager VIS, and we show that galaxy structural parameters are recovered to an accuracy similar to that for pure analytic SĂ©rsic profiles. Based on these simulations, we estimate that the Euclid Wide Survey (EWS) will be able to resolve the internal morphological structure of galaxies down to a surface brightness of 22.5 mag arcsec−2, and the Euclid Deep Survey (EDS) down to 24.9 mag arcsec−2. This corresponds to approximately 250 million galaxies at the end of the mission and a 50% complete sample for stellar masses above 1010.6 M⊙ (resp. 109.6 M⊙) at a redshift z ∌ 0.5 for the EWS (resp. EDS). The approach presented in this work can contribute to improving the preparation of future high-precision cosmological imaging surveys by allowing simulations to incorporate more realistic galaxies

    Cosmology with the Laser Interferometer Space Antenna

    No full text
    The Laser Interferometer Space Antenna (LISA) has two scientific objectives of cosmological focus: to probe the expansion rate of the universe, and to understand stochastic gravitational-wave backgrounds and their implications for early universe and particle physics, from the MeV to the Planck scale. However, the range of potential cosmological applications of gravitational wave observations extends well beyond these two objectives. This publication presents a summary of the state of the art in LISA cosmology, theory and methods, and identifies new opportunities to use gravitational wave observations by LISA to probe the universe

    COVMOS: a new Monte Carlo approach for galaxy clustering analysis

    No full text
    We validate the COVMOS method introduced in Baratta et al. (2019) allowing for the fast simulation of catalogues of different cosmological field tracers (e.g. dark matter particles, halos, galaxies, etc.). The power spectrum and one-point probability distribution function of the underlying tracer density field are set as inputs of the method and are arbitrarily chosen by the user. In order to evaluate the validity domain of COVMOS at the level of the produced two-point statistics covariance matrix, we choose to target these two input statistical quantities from realistic NN-body simulation outputs. In particular, we perform this cloning procedure in a Λ\LambdaCDM and in a massive neutrino cosmologies, for five redshifts in the range z∈[0,2]z\in[0,2]. First, we validate the output real-space two-point statistics (both in configuration and Fourier space) estimated over 5,0005,000 COVMOS realisations per redshift and per cosmology, with a volume of 1 [Gpc/h]31\ [\mathrm{Gpc}/h]^3 and 10810^8 particles each. Such a validation is performed against the corresponding NN-body measurements, estimated from 50 simulations. We find the method to be valid up to k∌0.2h/k\sim 0.2h/Mpc for the power spectrum and down to r ∌20r~\sim 20 Mpc/h/h for the correlation function. Then, we extend the method by proposing a new modelling of the peculiar velocity distribution, aiming at reproducing the redshift-space distortions both in the linear and mildly non-linear regimes. After validating this prescription, we finally compare and validate the produced redshift-space two-point statistics covariance matrices in the same range of scales. We release on a public repository the Python code associated with this method, allowing the production of tens of thousands of realisations in record time. COVMOS is intended for any user involved in large galaxy-survey science requiring a large number of mock realisations
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