Towards a FAIR understanding of compact group evolution: A case study of HCG16

Contributions to the XIV.0 Scientific Meeting (virtual) of the Spanish Astronomical Society, held 13-15 July 2020, online at https://www.sea-astronomia.es/reunion-cientifica-2020, id.52With funding from the Spanish government through the Severo Ochoa Centre of Excellence’accreditation SEV-2017-070

Towards a FAIR understanding of compact group evolution: A case study of HCG16

The 2019 SKA Science Meeting, entitled “New Science enabled by New Technologies in the SKA Era”, held at Alderley Park in Alderley Edge (UK) on April 8th to 12th, 2019

Evolution of compact groups from intermediate to final stages. A case study of the H

Hickson Compact Group (HCG) 16 is a prototypical compact group of galaxies in an intermediate stage of the previously proposed evolutionary sequence, where its galaxies are losing gas to the intra-group medium (IGrM). The group hosts galaxies that are H I-normal, H I-poor, and centrally active with both AGNs and starbursts, in addition to a likely new member and a H I tidal feature of similar to 160 kpc in length. Despite being a well-studied group at all wavelengths, no previous study of HCG16 has focused on its extraordinary H I component. Aims. The characteristics of HCG16 make it an ideal case study for exploring which processes are likely to dominate the late stages of evolution in compact groups, and ultimately determine their end states. In order to build a coherent picture of the evolution of this group we make use of the multi-wavelength data available, but focus particularly on H I as a tracer of interactions and evolutionary phase. Methods. We reprocess archival VLA L-band observations of HCG16 using the multi-scale CLEAN algorithm to accurately recover diffuse features. Tidal features and galaxies are separated in three dimensions using the SlicerAstro package. The H I deficiency of the separated galaxies is assessed against the benchmark of recent scaling relations of isolated galaxies. This work has been performed with particular attention to reproducibility and is accompanied by a complete workflow to reproduce all the final data products, figures, and results. Results. Despite the clear disruption of the H I component of HCG16 we find that it is not globally H I deficient, even though HCG16a and b have lost the majority of their H I and almost 50% of the group's H I is in the IGrM. The H I content of HCG16d shows highly disturbed kinematics, with only a marginal velocity gradient that is almost perpendicular to its optical major axis. The tail of similar to 160 kpc in length extending towards the southeast appears to be part of an even larger structure which spatially and kinematically connects NGC848 to the northwest corner of the group. Conclusions. This study indicates that in the recent past (similar to 1 Gyr) galaxies HCG16a and b likely underwent major interactions that unbound gas without triggering significant star formation. This gas was then swept away by a close, high-speed encounter with NGC848. The starburst events HCG16c and d, likely initiated by their mutual interaction, triggered galactic winds which, in the case of HCG16d, appear to have disrupted its H I reservoir. The tidal features still connected to all these galaxies indicate that more H I will soon be lost to the IGrM, while that which remains in the discs will likely be consumed by star-formation episodes triggered by their ongoing interaction. This is expected to result in a collection of gas-poor galaxies embedded in a diffuse H I structure, which will gradually (over several Gyr) be evaporated by the UV background, resembling the final stage of the evolutionary model of compact groups.MGJ is supported by a Juan de la Cierva formacion fellowship. We also acknowledge support from the grants AYA2015-65973-C3-1-R and RTI2018-096228-B-C31 (MINECO/FEDER, UE). This work has been supported by the Spanish Science Ministry >Centro de Excelencia Severo Ochoa> program under grant SEV-2017-0709. MGJ wishes to thank B. Koribalski, K. Lee-Waddell, and S. Cazzoli for helpful discussions. We also thank the referee for his thorough comments which helped to improve this paper. This project used archival data from the VLA. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This project used data obtained with the Dark Energy Camera (DECam), which was constructed by the Dark Energy Survey (DES) collaboration (full acknowledgement at legacysurvey.org/acknowledgment). This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We also acknowledge the use of the HyperLeda database (Makarov et al. 2014). This research made use of APLpy, an open-source plotting package for Python (Robitaille & Bressert 2012; Robitaille 2019), astropy (Astropy Collaboration 2013, 2018), Aladin (Bonnarel et al. 2000), mayavi (Ramachandran & Varoquaux 2011), and SAOImageDS9 (Joye & Mandel 2003)

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