We propose to advance the knowledge of Standard Cosmological model, both from the theoretical and from the observational point of view, by making use of the most recent cosmological data, and by planning/performing new campaigns of observations with state-of-the-art instrumentation and detectors. We aim to contribute to the study of the very early Universe through observations of Cosmic Microwave Background (CMB) polarization and spectral distortions. In addition, we will contribute to the tests for the presence of Baryonic Dark Matter in filamentary structures across the network of nonlinear structures in the universe, known as the Cosmic Web, through observations of the CMB distortion due to scattering off electrons in the hot Intra Cluster Medium (ICM) of Galaxy clusters and surrounding medium (Sunyaev Zel¿dovich effect). These objectives will be pursued through the analysis of existing data and the exploitation of experiments we are currently developing as leaders or co-leaders, like: LSPE, QUBIC, COSMO, OLIMPO, MISTRAL. In addition, we are leading observational efforts through regular submission of requests for observation time at the Sardinia Radio Telescope (SRT) and the Green Bank Telescope (GBT).
The uniqueness of this project stands in several "first-time" characteristics.
-CMB polarization:
B-modes detection is a difficult task. Nevertheless, with the Winter flight planned for LSPE/SWIPE, and the large sky coverage it aims to achieve, we are confident that its results will be uniquely competitive in the field. This, in conjunction with the capability of QUBIC to reject the systematics, makes the two experiments fully synergic and orthogonal.
-CMB spectral distortions:
the effort towards the finalization of the COSMO instrument design, observing/calibration strategy and data analysis marks a unique step forward in the direction of the long-standing issue of the detection of spectral distortions in the CMB spectrum. We expect this effort to pave the way to larger and even more ambitious projects which are still missing to-date, to exploit this significant aspect of the CMB properties to probe the history of the early universe.
-MISTRAL SZ catalog:
MISTRAL is a unique experiment. Only NIKA2 at IRAM and MUSTANG2 at the GBT have similar characteristics. With 12 arcsec resolution and 4 arcmin of F.O.V., it can advance the knowledge of the structure formation, the physics of Galaxy Clusters, and the knowledge of the filamentary structure of the Cosmic Web. We are in charge of the camera development and we will submit a legacy large project for the commissioning and the first exploitation of the camera itself. By the end of this project, a baseline design of a potential spectroscopic upgrade will also inform the preparation of the next iteration of this receiver.
-Unveiling the cosmic web:
The (already performed) MUSTANG2/GBT observations on the bridge connecting the clusters Abell401 and Abell399 are unique since they could yield, for the first time with high signal-to-noise, a detection of the filamentary structure between two clusters of galaxies as tracked by the warm-hot gas. Data analysis is ongoing and we started a joint analysis with colleagues from the Atacama Cosmology Telescope (Mark Devlin from UPenn). This joint analysis features a first-time multi-scale approach, which allows us to detect the fine structure of the filament with the MUSTANG2/GBT and the large structures with the ACT.
-M31 observations with the SRT:
Andromeda represents a unique laboratory to study effects and emissions arising from extragalactic sources as well as to understand the astrophysics of our Galaxy using an external point of view. Besides filling the gap at microwave frequencies at arcminute angular resolution, these observations will allow:
-To fully characterize AME in the galaxy, at high angular resolution;
-To measure the magnetic fields through polarization measurements in the C-band and K-band (Rotation Measure);
-To search and measure methanol and water MASERs;
-To fully characterize thermal and non-thermal emission, measure the galaxy morphology and monitor the Star Formation Rate (this was already started in the C-band and can be fully exploited with K-band observations);
-Possibly, to detect Radio Recombination Lines from the galaxy.