About Me

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Publications

Journals

  • The metallicity and elemental abundance maps of kinematically atypical galaxies for constraining minor merger and accretion histories
    Taylor, P., Kobayashi, C., Federrath, C. 2019, MNRAS, 485, 3215
    [ADS] [arXiv]
  • The impact of black hole seeding in cosmological simulations
    Wang, E.X., Taylor, P., Federrath, C., Kobayashi, C. 2019, MNRAS, 483, 4640
    [ADS] [arXiv]
  • On the [α/Fe]-[Fe/H] relations in early-type galaxies
    Vincenzo, F., Kobayashi, C., Taylor, P.. 2018, MNRAS, 480L, 38
    [ADS] [arXiv]
  • The origin of kinematically distinct cores and misaligned gas discs in galaxies from cosmological simulations
    Taylor, P., Federrath, C., Kobayashi, C. 2018, MNRAS, 479, 141
    [ADS] [arXiv]
  • The metallicity and elemental abundance gradients of simulated galaxies and their environmental dependence
    Taylor, P. and Kobayashi, C. 2017, MNRAS, 471, 3856
    [ADS] [arXiv]
  • Star formation in simulated galaxies: understanding the transition to quiescence at 3 × 1010M
    Taylor, P., Federrath, C., Kobayashi, C. 2017, MNRAS, 469, 4249
    [ADS] [arXiv]
  • Time evolution of galaxy scaling relations in cosmological simulations
    Taylor, P., Kobayashi, C. 2016, MNRAS, 463, 2465
    [ADS] [arXiv]
  • Radial Distribution of ISM Gas-phase Metallicity in CLASH Clusters at z ~ 0.35: A New Outlook on Environmental Impact on Galaxy Evolution
    Gupta, A., Yuan, T., Tran, K.H., Martizzi, D., Taylor, P., Kewley, L.J. 2016, ApJ, 831, 104
    [ADS] [arXiv]
  • Quantifying AGN-driven metal-enhanced outflows in chemodynamical simulations
    Taylor, P., Kobayashi, C. 2015, MNRAS, 452L, 59
    [ADS] [arXiv]
  • The effects of AGN feedback on present-day galaxy properties in cosmological simulations
    Taylor, P., Kobayashi, C. 2015, MNRAS, 448, 1835
    [ADS] [arXiv]
  • The Absence of an Environmental Dependence in the Mass-Metallicity Relation at z = 2
    Kacprazk, G.G., Yuan, T., Nanayakkara, T., Kobayashi, C., Tran, K.H., Kewley, L.J., Glazebrook, K., Spitler, L., Taylor, P., Cowley, M., Labbe, I., Straatman, C., Tomczak, A. 2015, ApJ, 802L, 26
    [ADS] [arXiv]
  • Seeding black holes in cosmological simulations
    Taylor, P., Kobayashi, C. 2014, MNRAS, 442, 2751
    [ADS] [arXiv]

Proceedings

  • First Detection of a Cluster-scale Gradient in the ISM metallicity of the Star-forming Galaxies
    Gupta, A., Yuan, T., Tran, K.H., Martizzi, D., Taylor, P., Kewley, L.J. 2017, AAS, 22932104
    [ADS]
  • Metallicities in cosmological simulations with AGN feedback
    Kobayashi, C., Taylor, P. 2016, IAUS, 319, 60
    [ADS]
  • Modeling abundances in galaxies
    Kobayashi, C., Taylor, P. 2016, IAUFM, 29, 246
    [ADS]

Movies

Evolution of Gas Metallicity in the IGM

The video below shows the evolution of gas-phase metallicity in the inter-galactic medium (IGM) in the vicinity of the most massive simulated galaxy. This galaxy is followed from z=5 to the present day. Enriched gas (red & white) forms in stars inside galaxies, and pollutes the IGM due to stellar and, later, AGN feedback. The video is 10 × 5.625 comoving Mpc, and the colour scale ranges from [O/H] ≤ -5 (purple & blue) to [O/H] ≥ -1 (red and white).


Evolution of Gas Temperature in the IGM

The video below shows the evolution of gas temperature in the IGM in the vicinity of the most massive simulated galaxy. This galaxy is followed from z=5 to the present day. Gas is heated by spernovae, as well as AGN feedback at late times. Only AGN feedback is powerful enough to produce the large-scale outflows seen towards the end of the video. The video is 10 × 5.625 comoving Mpc, and the colour scale ranges from T ≤ 5×103K (purple & blue) to T ≥ 108K (red and white).


Technical details

These videos were produced with a custom-written rendering code. Each gas particle was smoothed using a Gaussian kernel whose width depended on the smoothing length of the particle in the simulation. In each pixel, a ray (initially black) is traced from infinity to the near plane of the viewing frustum, and its value updated depending on the value of the physical property of interest of each smoothed particle it intercepts. The opacity of the gas is also taken into account, with denser gas being more opaque; this produces the shadow-like features seen in the videos. Finally, the total opacity along each ray is used to generate a transparency map (alpha channel) that is applied to the final image. The individual frames were converted into a video using ffmpeg.

Contact

Dr Philip Taylor
Research School of Astronomy & Astrophysics
The Australian National University
Canberra, ACT 2611, Australia

philip.1.taylor@anu.edu.au

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