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11 results on '"Bilton, Lawrence E."'

1. The Merging Galaxy Cluster Environment Affects the Morphology of Radio-AGN

Author

Rickel, Mary, Moravec, Emily, Gordon, Yjan A., Hardcastle, Martin J., Pierce, Jonathon C. S., Bilton, Lawrence E., and Roberts, Ian D.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

It has previously been found that the galaxy cluster environment can affect the fueling and evolution of Active Galactic Nuclei (AGN). This work examines the effect of the merging cluster environment on the properties of radio-AGN by comparing the radio morphology of cluster members in a sample of four merging and eight relaxed galaxy clusters at low redshift (z<0.2). Using 144-MHz data from the LOFAR Two-metre Sky Survey (LoTSS) and Zooniverse, we classify the radio morphology of the radio-detected cluster members using the following morphology classes: compact, compact extended, extended, jetted, and disturbed. We find that the merging cluster environment has a statistically significant, higher population proportion of disturbed (bent and head tail) sources, indicating that the merging environment can affect the morphology of cluster radio-AGN. We also investigate the number of AGN that are detected in the radio data only, and the number that are detected in both the radio and optical data in mergers and non-mergers. We find that the merging cluster environment has a higher population proportion of AGN that are identified only as radio-AGN compared to AGN that are identified as both radio and optical AGN. Overall, we find that the merging environment affects certain radio-AGN (disturbed and only radio identified AGN), but not all., Comment: Accepted for publication in the Astrophysical Journal. Table 4 is included as FITS and CSV as an ancillary file and is named `RickelMoravec+25_table4`; corresponding README is also provided. Rickel and Moravec are co-first authors. 20 pages and 3 figures

Published
2025

2. CHANCES, The Chilean Cluster Galaxy Evolution Survey: selection and initial characterization of clusters and superclusters

Author

Sifón, Cristóbal, Finoguenov, Alexis, Haines, Christopher P., Jaffé, Yara, Amrutha, B. M., Demarco, Ricardo, Lima, E. V. R., Lima-Dias, Ciria, Méndez-Hernández, Hugo, Merluzzi, Paola, Monachesi, Antonela, Teixeira, Gabriel S. M., Tejos, Nicolas, Araya-Araya, Pablo, Argudo-Fernández, Maria, Baier-Soto, Raúl, Bilton, Lawrence E., Bom, C. R., Calderón, Juan Pablo, Cassarà, Letizia P., Comparat, Johan, Courtois, H. M., D'Ago, Giuseppe, Dupuy, Alexandra, Fritz, Alexander, Haack, Rodrigo F., Herpich, Fabio R., Ibar, E., Kuchner, Ulrike, Lopes, Amanda R., Lopez, Sebastian, Lösch, Elismar, McGee, Sean, de Oliveira, C. Mendes, Morelli, Lorenzo, Moretti, Alessia, Pallero, Diego, Piraino-Cerda, Franco, Pompei, Emanuela, Rescigno, U., Smith, Rory, Castelli, Analía V. Smith, Sodré Jr, Laerte, and Tempel, Elmo

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

CHANCES, the CHileAN Cluster galaxy Evolution Survey, will study the evolution of galaxies in and around ${\sim}$150 massive galaxy clusters, from the local universe out to z=0.45. CHANCES will use the new 4MOST Spectroscopic Survey Facility on the VISTA 4m telescope to obtain spectra for ${\sim}$500,000 galaxies with magnitudes $r_\mathrm{AB} < 20.5$, providing comprehensive spectroscopic coverage of each cluster out to $5r_{200}$. Its wide and deep scope will trace massive and dwarf galaxies from the surrounding filaments and groups to the cores of galaxy clusters, enabling the study of galaxy pre-processing and the role of the evolving environment on galaxy evolution. In this paper we present and characterize the sample of clusters and superclusters to be targeted by CHANCES. We used literature catalogues based on X-ray emission and Sunyaev-Zel'dovich effect to define the cluster sample in a homogeneous way, with attention to cluster mass and redshift, as well as the availability of ancillary data. We calibrated literature mass estimates from various surveys against each other and provide an initial mass estimate for each cluster, which we used to define the radial extent of the 4MOST coverage. We also present an initial assessment of the structure surrounding these clusters based on the redMaPPer red-sequence algorithm as a preview of some of the science CHANCES will enable., Comment: 11 pages, 9 figures, plus references and appendix containing catalog tables, submitted to A&A

Published
2024

3. Constraining the duration of ram pressure stripping features in the optical from the direction of jellyfish galaxy tails

Author

Salinas, Vicente, Jaffé, Yara L., Smith, Rory, Shinn, Jong-Ho, Crossett, Jacob P., Gullieuszik, Marco, González-Torà, Gemma, Piraino-Cerda, Franco, Poggianti, Bianca, Vulcani, Benedetta, Biviano, Andrea, Lourenço, Ana C. C., Bilton, Lawrence E., Kelkar, Kshitija, and Calderón-Castillo, Paula

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Ram pressure stripping is perhaps the most efficient mechanism for removing gas and quenching galaxies in dense environments as they move through the intergalactic medium. Extreme examples of on-going ram pressure stripping are known as jellyfish galaxies, characterized by a tail of stripped material that can be directly observed in multiple wavelengths. Using the largest homogeneous broad-band optical jellyfish candidate sample in local clusters known to date, we measure the angle between the direction of the tails visible in the galaxies, and the direction towards the host cluster center. We find that $33\%$ of the galaxy tails point away from the cluster center, $18\%$ point towards the cluster center, and $49\%$ point elsewhere. Moreover, we find stronger signatures of ram pressure stripping happening on galaxies with a tail pointing away and towards the cluster center, and larger velocity dispersion profiles for galaxies with tails pointing away. These results are consistent with a scenario where ram pressure stripping has a stronger effect for galaxies following radial orbits on first infall. The results also suggest that in many cases, radially infalling galaxies are able to retain their tails after pericenter and continue to experience significant on-going ram pressure stripping. We further constrain the lifespan of the optical tails from the moment they first appear to the moment they disappear, by comparing the observed tail directions with matched N-body simulations through Bayesian parameter estimation. We obtain that galaxy tails appear for the first time at $\sim 1.16$ R$_{200}$ and disappear $\sim660$ Myr after pericenter., Comment: 19 pages, 17 figures

Published
2024
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4. Project ThaiPASS: International Outreach Blending Astronomy and Python

Author

Keegans, James D., Stancliffe, Richard J., Bilton, Lawrence E., Cashmore, Claire R., Gibson, Brad K., Kristensen, Mikkel T., Lawson, Thomas V., Pignatari, Marco, Vaezzadeh, Iraj, Côté, Benoit, and Chongchitnan, Siri

Subjects
Physics - Physics Education
Abstract

$\textit{Thailand-UK Python+Astronomy Summer School}$ (ThaiPASS), a collaborative project comprising UK and Thai institutions and assess its impact and possible application to schools in the United Kingdom. Since its inception in 2018, the annual ThaiPASS have trained around 60 Thai high-school students in basic data handling skills using Python in the context of various astronomy topics, using current research from the teaching team. Our impact assessment of the 5 day summer schools show an overwhelmingly positive response from students in both years, with over $80\%$ of students scoring the activities above average in all activities but one. We use this data to suggest possible future improvements. We also discuss how ThaiPASS may inspire further outreach and engagement activities within the UK and beyond., Comment: Accepted for publication into Physics Education; 21 pages, 5 figures and 3 tables

Published
2021
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5. The Impact of Disturbed Galaxy Clusters on the Kinematics of Active Galactic Nuclei

Author

Bilton, Lawrence E., Pimbblet, Kevin A., and Gordon, Yjan A.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We produce a kinematic analysis of AGN-hosting cluster galaxies from a sample 33 galaxy clusters selected using the X-ray Clusters Database (BAX) and populated with galaxies from the Sloan Digital Sky Survey (SDSS) Data Release 8 (DR8). The 33 galaxy clusters are delimited by their relative intensity of member galaxy substructuring as a proxy to core merging to derive two smaller sub-samples of 8 dynamically active (merging) and 25 dynamically relaxed (non-merging) states. The AGN were selected for each cluster sub-sample by employing the WHAN diagram to the strict criteria of log$_{10}$([NII]/H$\alpha$)$\geq-0.32$ and EW$_{\mathrm{H}\alpha}$ $\geq$ 6{\AA}, providing pools of 70 merging and 225 non-merging AGN sub-populations. By co-adding the clusters to their respective dynamical states to improve the signal-to-noise of our AGN sub-populations we find that merging galaxy clusters on average host kinematically active AGN between 0-1.5 $r_{200}$ as $r_{200}\rightarrow0$, where their velocity dispersion profile (VDP) presents a significant deviation from the non-AGN sub-population VDP by $\gtrsim3\sigma$. This result is indicative that the AGN-hosting cluster galaxies have recently coalesced onto a common potential. Further analysis of the composite distributions illustrate non-merging AGN-hosting sub-populations have, on average, already been accreted and predominantly lie within backsplash regions of the projected phase-space. This suggests merging cluster dynamical states hold relatively younger AGN sub-populations kinematically compared with those found in non-merging cluster dynamical states., Comment: Accepted for publication in the Monthly Notices of the Royal Astronomical Society; 14 pages, 6 figures

Published
2020
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6. The Rotational Profiles of Cluster Galaxies

Author

Bilton, Lawrence E., Hunt, Matthew, Pimbblet, Kevin A., and Roediger, Elke

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We compile two samples of cluster galaxies with complimentary hydrodynamic and N-body analysis using FLASH code to ascertain how their differing populations drive their rotational profiles and to better understand their dynamical histories. We select our main cluster sample from the X-ray Galaxy Clusters Database (BAX), which are populated with Sloan Digital Sky Survey (SDSS) galaxies. The BAX clusters are tested for the presence of sub-structures, acting as proxies for core mergers, culminating in sub-samples of 8 merging and 25 non-merging galaxy clusters. An additional sample of 12 galaxy clusters with known dumbbell components is procured using galaxy data from the NASA/IPAC Extragalactic Database (NED) to compare against more extreme environments. BAX clusters of each sample are stacked onto a common RA-DEC space to produce rotational profiles within the range of $0.0 - 2.5$ $r_{200}$. Merging stacks possess stronger core rotation at $\lesssim 0.5 r_{200}$ primarily contributed by a red galaxy sub-population from relaxing core mergers, this is alongside high rotational velocities from blue galaxy sub-populations, until, they mix and homogenise with the red sub-populations at $\sim r_{200}$, indicative of an infalling blue galaxy sub-population with interactive mixing between both sub-populations at $\gtrsim r_{200}$. FLASH code is utilised to simulate the merger phase between two originally independent clusters and test the evolution of their rotational profiles. Comparisons with the dumbbell clusters leads to the inference that the peculiar core rotations of some dumbbell clusters are the result of the linear motions of core galaxies relaxing onto the potential during post second infall., Comment: Accepted for publication in the Monthly Notices of the Royal Astronomical Society; 18 pages, 15 figures and 3 tables

Published
2019
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7. The Kinematics of Cluster Galaxies via Velocity Dispersion Profiles

Author

Bilton, Lawrence E. and Pimbblet, Kevin A.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present an analysis of the kinematics of a sample of 14 galaxy clusters via velocity dispersion profiles (VDPs), compiled using cluster parameters defined within the X-Ray Galaxy Clusters Database (BAX) cross-matched with data from the Sloan Digital Sky Survey (SDSS). We determine the presence of substructure in the clusters from the sample as a proxy for recent core mergers, resulting in 4 merging and 10 non-merging clusters to allow for comparison between their respective dynamical states. We create VDPs for our samples and divide them by mass, colour and morphology to assess how their kinematics respond to the environment. To improve the signal-to-noise ratio our galaxy clusters are normalised and co-added to a projected cluster radius at $0.0 - 2.5$ $r_{200}$. We find merging cluster environments possess an abundance of a kinematically-active (rising VDP) mix of red and blue elliptical galaxies, which is indicative of infalling substructures responsible for pre-processing galaxies. Comparatively, in non-merging cluster environments galaxies generally decline in kinematic activity as a function of increasing radius, with bluer galaxies possessing the highest velocities, likely as a result of fast infalling field galaxies. However, the variance in kinematic activity between blue and red cluster galaxies across merging and non-merging cluster environments suggests galaxies exhibit differing modes of galaxy accretion onto a cluster potential as a function of the presence of a core merger., Comment: Accepted for publication in the Monthly Notices of the Royal Astronomical Society; 16 pages, 7 figures

Published
2018
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8. The Motions of Galaxies within Large-Scale Structures

Author

Bilton, Lawrence E., Pimbblet, Kevin A., and Roediger, Elke

Subjects
Large-Scale Structure, Galaxy Clusters, Astronomy, Active Galactic Nuclei, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Kinematics and Dynamics
Abstract

Galaxy clusters represent one of the largest-scale structures in the Universe, with their environments of varying density being ideal for inducing an increase in activity of the cluster galaxy members and the pervading Intracluster Medium (ICM) between them. However the precise drivers, thereby the inferred consequences, of differing states of galaxy cluster activity have not been adequately disentangled. If one can procure a sufficient dichotomic sample of cluster galaxies of differing sub-populations from relaxed and unrelaxed galaxy cluster dynamical states, one could analyse how these sub-populations `move' as a function of both radius and dynamical state. Specifically, using velocity dispersion profiles (VDPs) that weight against cluster galaxies across all radii with a Gaussian window function, one can determine how cluster galaxies of properties that pertain to galaxy evolutionary indicators respond to the cluster environment as a function of the clustocentric radius. In addition, analysing the rotational profiles of these sub-populations as a function of the clustocentric radius can help identify where the bulk of the kinetic energy lies. In view of these points, we have pooled data of galaxies from the Sloan Digital Sky Survey (SDSS) two composite galaxy clusters are assembled into unrelaxed and relaxed states, which are compared with one another through splitting their cluster galaxy populations by their evolutionary proxies (i.e. morphology, colour, mass and AGN), thus analysing their resultant VDPs and rotational profiles. It is therefore found that unrelaxed galaxy clusters possess increased interaction between cluster galaxies as the radius increases, driven by blue and red elliptical galaxies, suggesting an induction of activity by pre-processed groups. AGN-hosting cluster galaxy sub-populations within these unrelaxed environs however present increased activity as \(R\rightarrow0\), indicating these are recent infallers, potentially triggered due to interactions with the ICM. Rotational profiles of unrelaxed clusters build upon the VDPs, showing significant bulk rotation of cluster galaxies with prominent core rotation driven by redder sub-populations., 176 Pages, 45 Figures and 7 Tables, {"references": ["Abadi M. G., Moore B., Bower R. G., 1999, MNRAS, 308, 947", "Abazajian K. N., et al., 2009, ApJS, 182, 543", "Abdullah M. H., Ali G. B., Ismail H. A., Rassem M. A., 2011, MNRAS, 416, 2027", "Abell G. O., 1958, ApJS, 3, 211", "Abell G. O., 1959, Leaflet of the Astronomical Society of the Pacific, 8, 121", "Aghamousa A., et al., 2016, arXiv e-prints, p. arXiv:1611.00036", "Agulli I., Aguerri J. A. 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