Browsing by Author "Verheijen, M A W"

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    Insights from spectral stacking on the Hi content of cluster galaxies in various environments: a tale of two clusters
    (2021) Healy, Julia Lynn; Verheijen, M A W; Blyth, S-L; van der Hulst, J M; Kraan-Korteweg, R C
    The environment in which a galaxy resides has long been known to have an impact on how the galaxy evolves. The denser the environment, the stronger the influence. Clusters of galaxies, which are some of the densest known cosmic environments, provide a unique opportunity to study the ongoing environmental processes influencing galaxy evolution. Optical studies have shown that galaxy clusters are typically home to a higher fraction of older elliptical, bulgedominated galaxies than the field which has a higher fraction of younger, disk-dominated galaxies. Which environmental processes are the cause of this morphology-density relation is still unknown. The dominant processes at play in the cluster environment tend to strongly impact the neutral hydrogen (H i) gas disks of galaxies. The H i disk often extends far out beyond the stellar disk making it susceptible to environmental processes before the stellar component of the galaxy is affected, and thus a useful tracer of the environment-driven galaxy evolution. In this thesis I study how the ongoing environmental processes in two galaxy clusters, the Coma cluster and Abell 2626, affect the average H i content of galaxies of different morphologies in different local environments or substructure. In the analysis of both clusters, I primarily use the H i stacking technique which uses the optical position and redshift information to extract global H i profiles of galaxies that are not necessarily directly detected in H i. The global profiles are aligned using the redshifts, and co-added to create an average H i spectrum with improved signal-to-noise statistics. Using yet-to-be published H i observations of the Coma cluster from the Westerbork Synthesis Radio Telescope, in combination with a new compilation of redshifts across the cluster, I explore the average H i content of galaxies located in different substructures within the cluster compared to cluster galaxies not associated with any substructure. While no conclusions can be made about which environment in Coma has a more dominant effect on the H i content, the analysis showed that there was a clear bimodality in the H i content of the cluster galaxies: either the galaxies were detected in H i, or the H i masses were well below the detection threshold. Where galaxies were not directly detected, they were found to be at least 10–50 times more H i deficient than field galaxies of the same type. Unlike the Coma cluster, Abell 2626 has not been as well studied, and so little is known about this cluster and its environs. In the second part of the thesis, I present new radio and optical observations of the cluster. Abell 2626 was observed by MeerKAT as part of the first open call for proposals. These observations have yielded H i data for Abell 2626 at the same H i mass sensitivity as the Westerbork observations of the Coma cluster, which is 2.5 times more nearby. Using the multi-object spectrograph, Hectospec, on the MMT telescope, we have created a spectroscopic catalogue of the Abell 2626 field that matches the MeerKAT observations and is 70% complete at r = 19.1 mag. The new spectroscopic catalogue around Abell 2626 enabled the characterisation of both the large scale structure in front of and behind the cluster, as well as the identification of substructure associated with the cluster. I am also able to determine that Abell 2626 is a rich cluster, comparable to the similarly sized Virgo cluster. I explore how the average H i content of galaxies of different luminosity, colour, and morphology change across the different local environments and substructure within the cluster. I find that late-type cluster galaxies located in substructures contain on average more H i than the late-type cluster galaxies not in substructures. I postulate that this suggests that the group environment protects the late-type galaxies from gas stripping mechanisms dominant in the global cluster environment. The H i stacking analysis shows that while Abell 2626 is not as H i deficient as the more massive Coma cluster, the Abell 2626 cluster galaxies do show a radial trend in the H i deficiencies as is observed in other clusters.
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    A Westerbork blind HI imaging survey of the Perseus-Pisces filament in the Zone of Avoidance
    (2017) Ramatsoku, Mpati Analicia; Kraan-Korteweg, Renée C; Verheijen, M A W; De Blok, W J G
    In this thesis we study a structure associated with the Perseus-Pisces Supercluster (PPS; cz ~ 6000 km s⁻¹), where it crosses the Zone of Avoidance (ZoA) at the Galactic longitude of ℓ ≈ 160ᵒ. This largely unexplored region contains the X-ray emitting 3C 129 cluster which hosts two strong radio sources with bent morphologies, thus indicative of a rich intra-cluster medium (ICM). Due to its low Galactic latitude of b = 0.27, where Galactic extinction is severe at optical wavelengths (AB = 1.8 − 8.0), the details of its galaxy population and dynamics had not been investigated in detail before. Additionally, the diverse and dynamic cosmic environments of the PPS with the embedded galaxy cluster make this region an ideal laboratory to study the effects on these environments on the galaxy properties and galaxy transformation processes therein. We used the Westerbork Synthesis Radio Telescope (WSRT) to blindly map this ZoA crossing of the PPS in the 21 cm HI-wavelength. This was conducted through 35 individual pointings observed for a total of 420 hours, covering a large area of about 9.6 sq.deg and a velocity range of approximately cz ~ 2000− 16000 km s⁻¹, thus mapping the immediate surrounding regions to enable investigations of the various cosmic environmental effects on the HI properties of galaxies. With the resulting spectral line data cubes of an angular resolution of 23" x 16" and a velocity resolution of 16.5 km s⁻¹ with a rms sensitivity of ~ 0.4 mJy/beam, we detect 211 galaxies within the entire surveyed volume. These new HI detections reveal a total of four distinct overdensities. Of these overdensities, the two major ones are located at the distance of the PPS at cz ~ 4000 − 8000 km s⁻¹ and behind it at cz ~ 8000 − 12000 km s−1. The galaxy overdensity associated with the PPS is used to demonstrate how this supercluster connects across the ZoA and confirms earlier indications of a filamentary connection between Perseus, Pisces and the A569 clusters through this region of the sky. Galaxies in the background of the PPS seem to be part of the CID15 structure that had been earlier predicted in the reconstructed density and velocity maps from the 2MASS Redshift Survey. We carry out a detailed census of the galaxy population in the 3C129 cluster by combining the HI-data of the gas-rich galaxies with the near-infrared (NIR) images of the gas-poor galaxies. The NIR galaxies are identified from the high resolution (0.2"/pix, seeing ~0.8") images of the UKIDSS Galactic Plane Survey. We obtain photometry in the J,H and K bands for about 9700 galaxies identified in the NIR images within the WSRT HI surveyed area. These measurements are used to derive the red-sequence of this cluster through the (J − K) vs K colour-magnitude diagram to identify the gas-poor cluster member candidates. Within the spatial extent of the cluster of radius ~ 1.7 Mpc, a total of 261 galaxies are identified as cluster members, with 23 detected in HI. An assessment of the morphologies of these galaxy members reveals a clear morphological segregation, with E and E/S0 galaxies dominating the inner regions of the 3C129 cluster and the late-type spirals found in the cluster outskirts. We also examine the richness of the cluster by comparing it to two well-known clusters at similar redshifts. One being a massive cluster in the Great Attractor region, namely the Norma cluster, also located in the ZoA but in the South, and the other being the Coma cluster. The comparison shows that the 3C129 cluster is quite rich as was suspected. The galaxy density in the core of the 3C129 cluster is similar to that in the Norma cluster and slightly less than in the Coma cluster. Furthermore, an assessment of the spatial distribution of galaxies in the core shows a slight asymmetry aligned with the irregular distribution of the X-ray emission, thus consistent with the results from the X-ray analysis which surmised that the 3C129 cluster seems to have undergone a merger and has not yet reached a dynamically relaxed state. In support of this we find a large substructure dominated by gas-rich galaxies North of the main cluster at a slightly higher recession velocity which could be falling into the cluster. All these findings seem to support a scenario where the 3C129 cluster is still growing through accretion of galaxies from the PPS filament. The wealth of HI data allows an analysis of the environmental effects on the galaxy properties within the WSRT surveyed volume. We first characterise the cosmic environments found within the two major overdensities as outlined by the HI-detected galaxies. This is conducted by perfoming tests to search for substructures. A total of four distinct substructures are found within the PPS ZoA overdensity (cz ~ 4000 − 8000 km s−1 ) and three in the background galaxy overdensity (cz ~ 8000 − 12000 km s−1). Our analysis of the HI properties of galaxies in these varying cosmic environments shows that highly disturbed HI-disks are found in larger and tightly bound groups, due to the higher incidence of tidal interactions between the galaxies. Furthermore, an indication of HI-gas deficiency is found in the core of the 3C129 cluster. We assess the cause of this deficiency through models of the ICM of the 3C129 cluster and find ram-pressure stripping to be the dominant gas removal process in this region. Additionally, highly HI-gas deficient galaxies are also found in the cluster outskirts. Most of these galaxies are located within galaxy groups where galaxy-galaxy interactions and mergers are prevalent, thus highlighting the importance of these processes in removing gas from galaxies in groups.