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There exists a well known relation between the mass of the supermassive black hole (SMBH) in the center of galaxies and their bulge mass or central velocity dispersion. This suggests a co-evolution between SMBH and their galaxy hosts. Our aim is to study this relation specifically for radio loud galaxies, and as a function of redshift \\(z\\). We selected a sample of radio-galaxies and AGN by cross-matching the low radio frequency sources from VLA FIRST with spectroscopically confirmed sources from wide field surveys including SDSS DR14 ugriz and DES DR2 grzY in optical, WISE in infrared, and the Galaxy And Mass Assembly (GAMA) spectroscopic survey. Keeping only high signal to noise (S/N) sources in WISE magnitudes, and those with broad emission lines, we selected a sub sample of 42 radio sources, all with infrared-to-optical counterparts, for which we characterized the stellar, star formation, and black hole properties. We estimated the central SMBH mass, the stellar mass \\(M_\\), the Eddington ratio \\(\\) and the jet power, \\(Q_ jet\\). The relation between SMBH mass, \\(M_\\), \\(\\) and \\(z\\) are put into context by comparing them with scaling relations (\\(M_ BH\\)--\\(M_\\), \\(M_ BH/M_\\)--\\(z\\), \\(M_ BH\\)--\\(Q_ jet\\) and \\(Q_ jet\\)--\\(\\)) from the literature. An evolutionary scenario where radio-mode AGN feedback (or the cluster environments) regulate the accretion onto the SMBHs and the stellar mass assembly of the radio sources is discussed, which may explain the observed phenomenology, and in particular the presence of radio sources with high \\(M_ BH/M_\\) ratios. This pilot study represents a benchmark for future ones using wide field surveys such as Euclid and the Vera Rubin telescope.

Today, the brightest cluster galaxies (BCGs) are passive and very massive galaxies at the center of their clusters, and they still accrete mass through swallowing companions and gas from cooling flows. However their formation history is not well known. We report CO(4\\(\\)3) and continuum map observations of the SpARCS1049+56 BCG at \\(z=1.709\\), one of the most distant known BCGs. Our observations yield \\(M_ H_2<1.110^10M_\\) for the BCG; while in CO(4\\(\\)3), we detect two gas-rich companions at the northeast and southeast of the BCG, within 20 kpc, with \\(L^_ CO(43)=(5.80.6)10^9\\) K km s\\(^-1\\) pc\\(^2\\) and \\((7.40.7)10^9\\) K km s\\(^-1\\) pc\\(^2\\), respectively. The northern companion is associated with a pair of merging cluster galaxies, while the southern one shows a southern tail in CO(4\\(\\)3), which was also detected in continuum, and we suggest it to be the most distant jellyfish galaxy for which ram pressure stripping is effectively able to strip off its dense molecular gas. This study probes the presence of rare gas-rich systems in the very central region of a distant cluster core, which will potentially merge into the BCG itself. Currently, we may thus be seeing the reversal of the star formation versus density relation at play in the distant universe. This is the first time the assembly of high-\\(z\\) progenitors of our local BCGs can be studied in such great detail.

Brightest cluster galaxies (BCG) are today passive and very massive galaxies at the center of their clusters, still accreting mass through swallowing companions, and flows of cold gas, regulated by radio-mode active galactic nucleus (AGN) feedback. However, their formation history is still a matter of debate. We report new results based on millimeter observations performed with the Northern Extended Millimeter Array (NOEMA) interferometer, mapping the cold molecular gas (CO) that feeds the star formation of distant BCGs. We selected three among the strongest cool-core BCGs at intermediate redshifts (\\(z0.4\\)), namely RX 1532, MACS 1447, and CHIPS 1911. Previous unresolved millimeter observations and multi-wavelength analysis showed that they are among the most star forming (\\( SFR100~ M_/ yr\\)) and gas rich (\\(M_H_210^11~M_\\)) BCGs at intermediate redshifts. The selected BCGs are thus caught in a phase of rapid mass assembly, which makes them ideal targets for high-resolution observations of their molecular gas. By combining NOEMA intensity and velocity maps with archival images from the Hubble Space Telescope, we detect in-situ star formation, filaments of accreting cold gas likely regulated by AGN feedback, disturbed morphology associated with tidal tails of molecular gas, as well as gas compression and tails originated from stripping of gas. While effective condensation of the intra-cluster medium is required to explain the large molecular gas reservoirs, the BCGs exhibit a broad variety of environment-driven mechanisms responsible for the processing of their cold gas: flows of cooling gas (RX 1532), ram pressure or sloshing of the intra-cluster medium (MACS 1447), and galactic tides (CHIPS 1911). This study thus sheds new insights on the physical mechanisms responsible for the mass assembly of galaxies hosting AGN at the center of clusters.

Context. Galaxy clusters provide key insights into cosmic structure formation, galaxy formation and are essential for cosmological studies. Aims. We present a catalog of galaxy clusters detected in the Kilo-Degree Survey (KiDS-DR4) optimized for cosmological analyses and investigations of cluster properties. Each detection includes probabilistic membership assignments for the KiDS-DR4 galaxies within the magnitude range \\(153.5\\). The sample is highly homogeneous across the entire survey thanks to the restrictive galaxy selection criteria we adopted. Spectroscopic data from the GAMA survey were used to calibrate the clusters photometric redshift and assess their uncertainties. We introduced algorithmic enhancements to AMICO to mitigate border effects among neighbor tiles. Quality flags are also provided for each cluster detection. The sample purity and completeness assessments have been estimated using the SinFoniA data driven approach, thus avoiding strong assumptions embedded in numerical simulations. We introduced a blinding scheme of the selection function meant to support the cosmological analyses. Results. Our cluster sample includes 321 cross-matches with the X-ray eRASS1 \"primary\" sample and 235 matches with the ACT-DR5 cluster sample. We derived a mass-proxy scaling relation based on intrinsic richness, \\(_*\\), using masses from the eRASS1 catalog. Conclusions. The KiDS-DR4 cluster catalog provides a valuable data set for investigating galaxy cluster properties and contributes to cosmological studies by offering a large, well-characterized cluster sample.

There is controversy whether dusty starbursts selected at submillimeter wavelengths can trace galaxy overdensities. We perform the first systematic search for protoclusters around a homogeneously selected sample of 12 spectroscopically confirmed submillimeter galaxies (SMGs) at \\(z1.2-5.3\\) in the GOODS-N field. We applied the Poisson Probability Method (PPM) to search for Mpc scale overdensities around these SMGs using three photometric redshift catalogs. We detect galaxy overdensities for 11 out of the 12 SMGs (\\(92\\%8\\)\\%), distributed over eight protoclusters. We confirm three previously discovered protoclusters, and we detect five new ones around the SMGs SMMJ123634 (\\(z=1.225\\)), ID.19 (\\(z=2.047\\)), SMMJ123607 (\\(z=2.487\\)), SMMJ123606 (\\(z=2.505\\)), and GN10 (\\(z=5.303\\)). A wavelet-based analysis shows that the SMGs live in protocluster cores with a complex morphology (compact, filamentary, or clumpy) and an average size of \\((0.4-1)\\)Mpc. By comparing the PPM results obtained using independently the three redshift catalogs, we possibly witness a transitioning phase at \\(z4\\) for the galaxy populations. While \\(z4\\) protoclusters appear to be populated by dusty galaxies, those at highest redshifts \\(z5\\) are detected as overdensities of Lyman\\(\\) emitters or Lyman break galaxies. We also find a good correlation between the molecular (H\\(_2\\)) gas mass of the SMG and the overdensity significance. To explain the overall phenomenology, we suggest that galaxy interactions in dense environments likely triggered the starburst and gas-rich phase of the SMGs. Altogether, we support the scenario that SMGs are excellent tracers of distant protoclusters. Those presented in this work are excellent targets for the ıt James Webb Space Telescope. Surveys with forthcoming facilities (e.g., ıt Euclid, LSST) can be tuned to detect even larger samples of distant protoclusters.

The stellar mass assembly of brightest cluster galaxies (BCGs) is still debated. We have observed in CO with the IRAM-30m two star forming BCGs belonging to SpARCS clusters, 3C 244.1 (\\(z=0.4\\)) and SDSS J161112.65+550823.5 (\\(z=0.9\\)), and compared their molecular gas and star formation properties with those of a compilation of \\(100\\) distant cluster galaxies, including nine additional distant BCGs at \\(z0.4-3.5\\). We have set robust upper limits of \\(M_ H_2<1.010^10~M_\\) and \\(<2.810^10~M_\\) to their molecular gas content, respectively, as well as to the molecular gas to stellar mass ratio \\(M( H_2)/M_0.2\\) and depletion time \\(_ dep40\\) Myr of the two targeted BCGs. They are thus among the distant cluster galaxies with the lowest gas fractions and shortest depletion times. The majority, \\(64\\%15\\%\\) and \\(73\\%18\\%\\), of the 11 BCGs with observations in CO have lower \\(M( H_2)/M_\\) and \\(_ dep\\), respectively, than those estimated for main sequence galaxies. Statistical analysis tentatively suggests that the values of \\(M( H_2)/M_\\) and \\(_ dep\\) for the 11 BCGs deviates, with a significance of \\(2\\), from those of the comparison sample of cluster galaxies. A morphological analysis for a subsample of seven BCGs with archival HST observations reveals that \\(71\\%17\\%\\) of the BCGs are compact or show star-forming substructures/components. Our results suggest a scenario where distant star forming BCGs assemble a significant fraction \\(16\\%\\) of their stellar mass in the relatively short timescale \\(_ dep\\), while environmental mechanisms might prevent the replenishment of gas feeding the star formation. We speculate that compact components favor the rapid exhaustion of molecular gas and help to quench the BCGs. Distant star forming BCGs are excellent targets for ALMA and JWST.

Since the start of operations in 2011, the VLT Survey Telescope (VST) has been one of the most efficient wide-field imagers in the optical bands. However, in the next years the Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST) will be a game-changer in this field. Hence, the timing is appropriate for specializing the VST with additions that can make it unique in well-defined scientific cases. VSTPOL is a project that aims to provide the addition of wide-field polarimetric capabilities to the VST telescope, making it the first large survey telescope for linear optical polarimetry. Actually, while there are quite a number of optical telescopes, the telescopes providing polarimetric instrumentation are just a few. The number of relatively large mirror polarimetric telescopes is small, although they would be specifically needed e.g. to support many science cases of the Cherenkov Telescope Array (CTA) that, in the southern hemisphere, is co-located with the VST. The VST telescope is equipped with a single instrument, the OmegaCAM wide-field imaging camera operating in the visible bands with a field of view of 1\\(^1^\\). The polarimetric mode will be implemented through the insertion of a large rotatable polarizer installed on the field-corrector optics, which will be exchangeable with the non-polarimetric corrector optics. The limiting polarimetric systematic errors due to variable atmospheric conditions and instrumental polarization can be corrected down to a level of \\(10^-3\\) by leveraging the large amount of unpolarized stars within each field-of-view. By the user point of view, VSTPOL will be an additional mode for the VST wide-field imaging camera.

In this work we account for this skewness in parameter inference by modelling the likelihood through an Edgeworth expansion which involves the complete skewness tensor, composed of 1-point, 2-point, and 3-point correlators. To simplify the calculations of this expansion we perform a change of basis which reduces the precision matrix to the identity. In this basis, the off-diagonal elements of the skewness tensor are consistent with zero, while the amplitude of its diagonal match the level expected for a Gaussian underlying field. We perform parameter inference with this likelihood model and find that including only the diagonal part of the skewness is sufficient, while incorporating the full skewness tensor injects noise without improving accuracy. Despite the estimated excess skewness in the original basis, the cosmological constraints remain effectively unchanged when adopting a Gaussian likelihood or considering the more complete Edgeworth expansion, with variations in the figure of merit of cosmological parameters between the two cases below \\(5\\%\\). This result remains unchanged against variations of the survey volume and geometry, scale-cut, and 2-point statistic (power spectrum or correlation function). Using \\(10\\, 000\\) cloned large mocks based on realistic galaxy catalogues with characteristics close to future data, we find no detectable excess skewness on intermediate scales, due to the level of shot noise expected for the spectroscopic sample. We conclude that the Gaussian likelihood assumption is robust for 2-point statistics analyses in both Fourier and configuration space.