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Italy is frequently hit and damaged by landslides, resulting in substantial and widespread disruptions. In particular, slope failures have a high impact on the population, communication infrastructure, and economic and productive sectors. The hazard posed by landslides requires adequate responses for landslide risk mitigation, with special attention to the risk to the population. In 2006 the Italian Department of Civil Protection, an office of the Prime Minister, commissioned the Research Institute for Geo-Hydrological Protection (Istituto di Ricerca per la Protezione Idrogeologica), a research institute of the Italian National Research Council, to carry out operational forecasting of rainfall-induced landslides. Collecting landslide information in a catalogue is a preliminary action toward landslide forecasting. The use of spatially and temporally inaccurate landslide catalogues results in uncertain and unreliable operational landslide forecasting. Consequently, accurate catalogues are needed to reduce the uncertainties, which are to some extent unavoidable. To this end, over the last 15 years many researchers have been involved in compiling a catalogue called ITALICA (ITAlian rainfall-induced LandslIdes CAtalogue), which currently lists 6312 records with information on rainfall-induced landslides that occurred over the Italian territory between January 1996 and December 2021. Overall, more than one-third of the catalogue has very high geographic accuracy (less than 1 km2) and hourly temporal resolution. In contrast, less than 2 % of the catalogue has low and very low geographical accuracy and daily temporal resolution. This makes ITALICA the largest catalogue of rainfall-induced landslides accurately located in space and time available in Italy. Without this high level of accuracy, the precipitation responsible for the initiation of landslides cannot be reliably reconstructed, thus making the prediction of landslide occurrence ineffective. ITALICA can be accessed at https://doi.org/10.5281/zenodo.8009366 (Brunetti et al., 2023). ITALICA's information on rainfall-induced landslides in Italy places a special emphasis on their spatial and temporal locations, making the catalogue especially suitable for defining the rainfall conditions capable of triggering future landslides in the Italian territory. This information is fundamental for decision-making in landslide risk management.

In Italy, rainfall represents the most common triggering factor for landslides; thus, many Italian Regional Departments of Civil Protection are setting up warning systems based on rainfall recordings. Common methods are mainly based on empirical relationships that provide the rainfall thresholds above which the occurrence of landslide phenomena is likely to be expected. In recent years, the use of machine learning approaches has gained popularity in landslide susceptibility analysis and prediction. To support the operational early warning system of Liguria Civil Protection Department for landslides hazard, we propose the implementation of a polynomial Kernel regularized least squares regression (KRLS) algorithm, for predicting the daily occurrence of shallow landslides in the five Alert Zones in Liguria (North Western Italy). The model provides an estimate of the number of landslides associated with the set of three different hydrological features, also used for the Hydrological Assessment procedure: the soil moisture, the accumulated precipitation over 12 h and the precipitation peak over 3 h. Results of the model are converted to an Alert Scenario of landslide occurrence, based on the magnitude of the expected event and identified according to the National and Regional legislation (Regional Civil Protection guidelines D.G.R. n. 1116, 23/12/2020). The performance of the predictive model (e.g. accuracy of 93%) is deemed satisfactory and the methodology is considered a valuable support to the operational early warning system of Liguria Civil Protection Department. The choice of predictive variables allows, in future development, the values obtained from historical data to be replaced by those obtained from meteorological forecast models, introducing the use of the developed model in the operational forecasting chain.

Derelict mining districts represent anthropogenically influenced landscapes that are often characterized by important geological, ecological, environmental, industrial, cultural, and archeological values. Nevertheless, after mining activities cease, several environmental problems are left behind, associated with soil and water pollution, hydrogeological instability, subsidence, ecosystem damages, and landscape degradation or devastation. In this article we present a case study focused on a sulfide mining district (Petronio and Gromolo valleys, Genova) located on the ophiolitic sequences of the Northern Apennines (Eastern Liguria, Italy), with the aim of applying a GIS (Geographic Information System)-based model for the complete census of derelict mines and for the assessment of their geoheritage and geotourist values, potential risks, and environmental impact. All information has been integrated to produce a multicriteria approach for the evaluation of hazards and/or critical issues and geoheritage values. Based on the results obtained in this pilot area, an integrated cultural and touristic route has been proposed, which combines several points of interest (POIs) chosen within an area of about 8 km2.

Abstract Aims The last released European guidelines on the management of heart failure (HF) recommend in patients with chronic HF with reduced ejection fraction (HFrEF) a pharmacological approach based on four fundamental drugs to be rapidly implemented and then uptitrated to modify disease progression. The aim of the Optimization of Therapy in the Italian Management of Heart Failure (OPTIMA-HF) registry is to collect data on chronic HF outpatients in different settings of care. In the present analysis, we report the first analysis of the OPTIMA-HF registry, focusing on the real-life use of guideline-directed medical therapy in patients affected by HFrEF. Methods OPTIMA-HF is an observational, cross-sectional, multicentre, real-life Italian registry conducted in two different clinical settings: HF outpatients' clinics of Italian hospitals and community HF outpatients' services. The study comprises a T0 phase—retrospective data collection, in which data of consecutive HF outpatients seen between January and October 2022 were collected; an educational activity phase; and a T1 phase—prospective data collection, in which data of consecutive HF outpatients seen between September 2023 and November 2023 were collected. In the present analysis, we describe the T0 phase focusing on HFrEF drug prescription rates, types, doses, combination therapy, the presence of contraindications and reasons of non-optimized treatment. Results Twenty-nine centres enrolled 2110 HF patients, of which 1390 (65.9%) had HFrEF [69.5 ± 11.9 years, 76.2% males, 4.1 years since HF diagnosis, median ejection fraction (EF) 33%]. Among HFrEF patients, 89.1% were on treatment with renin–angiotensin–aldosterone system inhibitor (RAASi)/angiotensin receptor neprilysin inhibitor (ARNI) (72% ARNI and 17.1% RAASi), 95.1% with beta-blockers, 75.8% with mineralocorticoid receptor antagonists (MRA) and 63.2% with sodium/glucose cotransporter 2 inhibitors (SGLT2i). Despite high prescription rates, a non-negligible number of patients with no contraindications were not treated with each specific drug. Patients taking all four drug classes, as recommended by guidelines, were mere 46.9%. Regarding doses, a still low number of patients on RAASi/ARNI and beta-blockers were treated with a dose ≥50% of the target doses recommended by the European guidelines. Conclusions The OPTIMA-HF registry reported that HFrEF fundamental drugs are prescribed in most Italian patients; however, <50% of patients receive optimal combination therapy, and still not a satisfying number of patients receive target doses. Strategies to improve implementation of guideline-directed medical therapy are needed to improve HF prognosis.

We present a systematic search for broad-line active galactic nuclei (AGNs) in the ALPINE-CRISTAL-JWST sample of 18 star-forming galaxies (\\(M_\\star>10^{9.5}~M_{\\odot}\\)) at redshifts \\(z=4.4-5.7\\). Using JWST/NIRSpec IFU, we identify 7 AGN candidates through the detection of broad \\Ha\\ emission lines from 33 aperture spectra centred on photometric peaks. These candidates include one highly robust AGN detection with FWHM \\(\\sim\\) 2800 \\kms\\ and six showing broad components with FWHM \\(\\sim 600-1600\\) \\kms, with two in a merger system. We highlight that only broad-line detection is effective since these candidates uniformly lie within narrow emission-line ratio diagnostic diagrams where star-forming galaxies and AGNs overlap. The broad-line AGN fraction ranges from 5.9\\% to 33\\%, depending on the robustness of the candidates. Assuming that the majority are AGNs, the relatively high AGN fraction is likely due to targeting high-mass galaxies, where simulations demonstrate that broad-line detection is more feasible. Their black hole masses range from \\(10^6\\) to \\(10^{7.5}~M_{\\odot}\\) with \\(0.1 \\lesssim L_{\\rm bol}/L_{\\rm Edd}\\lesssim 1\\). Counter to previous JWST studies at high redshift that found overmassive black holes relative to their host galaxies, our candidates lie close to or below the local \\(M_{\\rm BH}-M_\\star\\) scaling relations, thus demonstrating the effect of selection biases. This study provides new insights into AGN-host galaxy co-evolution at high redshift by identifying faint broad-line AGNs in galaxy samples, highlighting the importance of considering mass-dependent selection biases and the likelihood of a large population of AGNs being undermassive and just now being tapped by JWST.

We present the morphological parameters and global properties of dust-obscured star formation in typical star-forming galaxies at z=4-6. Among 26 galaxies composed of 20 galaxies observed by the Cycle-8 ALMA Large Program, CRISTAL, and six galaxies from archival data, we have individually detected rest-frame 158\\(\\mu\\)m dust continuum emission from 19 galaxies, nine of which are reported for the first time. The derived far-infrared luminosities are in the range \\(\\log_{10} L_{\\rm IR}\\,[L_{\\odot}]=\\)10.9-12.4, an order of magnitude lower than previously detected massive dusty star-forming galaxies (DSFGs). The average relationship between the fraction of dust-obscured star formation (\\(f_{\\rm obs}\\)) and the stellar mass is consistent with previous results at z=4-6 in a mass range of \\(\\log_{10} M_{\\ast}\\,[M_{\\odot}]\\sim\\)9.5-11.0 and show potential evolution from z=6-9. The individual \\(f_{\\rm obs}\\) exhibits a significant diversity, and it shows a correlation with the spatial offset between the dust and the UV continuum, suggesting the inhomogeneous dust reddening may cause the source-to-source scatter in \\(f_{\\rm obs}\\). The effective radii of the dust emission are on average \\(\\sim\\)1.5 kpc and are \\(\\sim2\\) times more extended than the rest-frame UV. The infrared surface densities of these galaxies (\\(\\Sigma_{\\rm IR}\\sim2.0\\times10^{10}\\,L_{\\odot}\\,{\\rm kpc}^{-2}\\)) are one order of magnitude lower than those of DSFGs that host compact central starbursts. On the basis of the comparable contribution of dust-obscured and dust-unobscured star formation along with their similar spatial extent, we suggest that typical star-forming galaxies at z=4-6 form stars throughout the entirety of their disks.

We present a detailed analysis of J154506, a strongly lensed submillimeter galaxy behind the Lupus-I molecular cloud, and characterisation of its physical properties using a combination of new and archival data, including VLT/MUSE and FORS2 optical data. We identify two high-significance (SNR>5) emission lines at 97.0 and 145.5 GHz, corresponding to CO(4-3) and CO(6-5), respectively, in the spectral scans from the Atacama Compact Array and the Large Millimetre Telescope and the [CII] 158~\\(\\mu\\)m fine-structure line at 400~GHz using the Atacama Pathfinder Experiment. These detections yield a spectroscopic redshift of \\(z_{\\rm{spec}}=3.7515\\pm0.0005\\). We also report the detection of [CI], HCN(4-3), and two H\\(_2\\rm{O}^+\\) transitions, further confirming the redshift and providing insights into J154506's physical properties. By modeling sub-arcsecond resolution (0.75) ALMA Band 6 and 7 continuum data in the uv-plane, we derive an average magnification factor of \\(6.0\\pm0.4\\) and our analysis reveals a relatively cold dust (38K) in a starburst (\\(\\sim900~\\rm{M}_{\\odot}yr^{-1}\\)) galaxy with a high intrinsic dust mass (\\(\\sim2.5\\times10^{9}~\\rm{M}_{\\odot}\\)) and infrared (IR) luminosity (\\(\\sim6\\times10^{12}~\\rm{L}_{\\odot}\\)). The non-local thermodynamic equilibrium radiative transfer modelling of the joint dust SED and CO line excitation suggests the dust continuum emission is primarily associated with relatively diffuse regions with molecular gas densities of \\(10^2-10^4\\rm{cm}^{-3}\\), rather than compact, high-pressure environments typical of extreme starbursts or AGNs. This is supported by the close-to-unity ratio between the dust and gas kinetic temperatures, which argues against highly energetic heating mechanisms. The CO excitation ladder peaks close to CO(5-4) and is dominated by slightly denser molecular gas.

Following the detection of a radio-loud Active Galactic Nucleus (AGN) in the z=4.3 protocluster SPT2349-56, we have obtained additional observations with MeerKAT in S-band (2.4 GHz) with the aim of further characterizing radio emission from amongst the ~30 submillimeter (submm) galaxies (SMGs) identified in the structure. We newly identify three of the protocluster SMGs individually at 2.4GHz as having a radio-excess, two of which are now known to be X-ray luminous AGN. Two additional members are also detected with radio emission consistent with their star formation rate (SFR). Archival MeerKAT UHF (816 MHz) observations further constrain luminosities and radio spectral indices of these five galaxies. The Australia Telescope Compact Array (ATCA) is used to detect and resolve the central two sources at 5.5 and 9.0 GHz finding elongated, jet-like morphologies. The excess radio luminosities range from L1.4,rest = (1-20)x10^25 W/Hz, ~10-100x higher than expected from the SFRs, assuming the usual far-infrared-radio correlation. Of the known cluster members, only the SMG `N1' shows signs of AGN in any other diagnostics, namely a large and compact excess in CO(11-10) line emission. We compare these results to field samples of radio sources and SMGs. The overdensity of radio-loud AGN in the compact core region of the cluster may be providing significant heating to the recently discovered nascent intra-cluster medium (ICM) in SPT2349-56.

There is a broad consensus from theory that stellar feedback in galaxies at high redshifts is essential to their evolution, alongside conflicting evidence in the observational literature about its prevalence and efficacy. To this end, we utilize deep, high-resolution [CII] emission line data taken as part of the [CII] resolved ISM in star-forming galaxies with ALMA (CRISTAL) survey. Excluding sources with kinematic evidence for gravitational interactions, we perform a rigorous stacking analysis of the remaining 15 galaxies to search for broad emission features that are too weak to detect in the individual spectra, finding only weak evidence that a broad component is needed to explain the composite spectrum. Additionally, such evidence is mostly driven by CRISTAL-02, which is already known to exhibit strong outflows in multiple ISM phases. Interpreting modest residuals in the stack at \\(v\\sim300\\)kms\\(^{-1}\\) as an outflow, we derive a mass outflow rate of \\(\\dot{M}_{\\rm out}=26\\pm11\\)M\\(_\\odot\\)yr\\(^{-1}\\) and a cold outflow mass-loading factor of \\(\\eta_m=0.49\\pm0.20\\). This result holds for the subsample with the highest star-formation rate surface density \\((\\Sigma_{\\rm{SFR}}>1.93\\)M\\(_\\odot\\)yr\\(^{-1}\\)kpc\\(^{-2}\\)) but no such broad component is present in the composite of the lower-star-formation rate density subsample. Our results imply that the process of star-formation-driven feedback may already be in place in typical galaxies at \\(z=5\\), but on average not strong enough to completely quench ongoing star formation.

Characterizing dust attenuation is crucial for revealing the intrinsic physical properties of galaxies. We present an analysis of dust attenuation in 18 spectroscopically confirmed star-forming main-sequence galaxies at \\(z = 4.4-5.7\\) observed with JWST/NIRSpec IFU and NIRCam, selected from the ALPINE and CRISTAL ALMA large programs. We fit the emission line fluxes from NIRSpec and the broad-band photometry from NIRCam with Prospector, using both spatially integrated emission and \\(\\sim0.6\\) kpc pixel-by-pixel measurements. We derive the stellar-to-nebular dust attenuation ratio (\\(f=E(B-V)_{\\mathrm{star}}/E(B-V)_{\\mathrm{neb}}\\)) from the SED fits and the Balmer decrement with H\\(\\alpha\\) and H\\(\\beta\\). Although individual galaxies show large scatter, the best-fit value is \\(f = 0.51^{+0.04}_{-0.03}\\), slightly higher than that measured for local starburst galaxies. We find weak correlations of \\(f\\) with galaxy properties, increasing with higher specific star-formation rates, younger stellar ages, and more recent star-formation. For the range of \\(E(B-V)_{\\mathrm{star}} = 0.009-0.15\\) mag for in our sample, assuming \\(f = 1\\) (often adopted in high-redshift studies) instead of \\(f = 0.51\\) underestimate line luminosities and ionizing photon production efficiency \\(\\xi_\\text{ion}\\) by \\(\\sim3-36\\%\\) and \\(\\sim4-46\\%\\), respectively. We also find that the total stellar masses estimated from spatially-integrated SED fits with a delayed-\\(\\tau\\) star-formation histories are systematically smaller than the sum of pixel-by-pixel SED fits, with a median offset of \\(\\sim 0.26\\) dex, likely because the integrated fits are biased toward luminous young stellar populations.