2026-04-17T18:37:14Zivo://CDS.VizieR/J/A+A/665/A1552025-06-13T15:25:00ZJ.A_AIVOAAGES HI sources in Abell 1367 fieldMany galaxy properties are known to correlate with the environment in which the galaxies are embedded. Their cold, neutral gas content, usually assessed through 21cm HI observations, is related to many other galaxy properties as it is the underlying fuel for star formation. With its high sensitivity and broad sky coverage the blind Arecibo Galaxy Environment Survey (AGES) survey brings significant improvement to the census of HI properties of galaxies in a wide range of environments, from voids to the core of a massive cluster. Here we present an HI census over a volume of ~44000Mpc^3^ towards the merging cluster Abell 1367 and extending well beyond. Our aim is to measure the effects different environments have on the HI content of their constituent galaxies. We use AGES- a deep, blind, HI survey, with the Arecibo radio telescope, 20 square degrees on the sky, centred on the merging cluster Abell 1367 mapping the large-scale structure (LSS) surrounding the cluster out to cz=20000km/s. The survey is sensitive down to a column density of N_HI_=1.5x10^17^cm^-2^ for emission filling the beam and a line width of 10km/s. As an approximate mass sensitivity limit, a member of A1367 (at a distance of 92Mpc), containing M_HI_=2.7x10^8^M_{sun}_ distributed over a top-hat profile of 50km/s width would be detected at 4{sigma}. The results are analysed in combination with optical spectroscopy data from SDSS which we use to estimate the local galaxy density based on the Voronoi-Delaunay method. We present the results of the complete AGES survey of the A1367 field. In total we detect 457 HI sources, 213 of which are detected for the first time by the AGES survey, 134 of which are presented in this article for the first time. 225 of the detections are in the cluster and 232 in the remaining volume surveyed. Here we present the full catalogue of HI detections and their basic properties, including optical ones. In this article we concentrate on the difference between the cluster and the foreground and background LSS. We reveal a lack of correlation of HI detected fraction with local galaxy density when the cluster and the rest of the surveyed volume are analysed separately. On the other hand the HI detected fraction in the cluster is approximately half that found outside the cluster.galaxy-clustersh-i-line-emissiongalactic-and-extragalactic-astronomyinterstellar-mediumhttps://dc.g-vo.org/rr/q/lp/custom/CDS.VizieR/J/A+A/665/A155http://doi.org/10.26093/cds/vizier.36650155https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/665/A1552022A&A...665A.155Dhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/665/A155Cone search capability for table J/A+A/665/A155/tablea1 (Full catalogue of HI detections and their basic properties)Deshev B.Taylor R.Minchin R.Scott T.C.Brinks E.CDS2022https://cds.unistra.fr/vizier-org/licences_vizier.htmlCDS support team <cds-question@unistra.fr>DatasetAstroObjectsastronomy