ORCID Profile
0000-0002-1052-0611
Current Organisations
International Centre for Radio Astronomy Research
,
University of Western Australia
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Publisher: SPIE
Date: 12-07-2008
DOI: 10.1117/12.790496
Publisher: Elsevier BV
Date: 2022
Publisher: SPIE
Date: 16-07-2010
DOI: 10.1117/12.856703
Publisher: Oxford University Press (OUP)
Date: 23-11-2016
Publisher: Oxford University Press (OUP)
Date: 02-09-2019
Abstract: We combine the shark semi-analytic model of galaxy formation with the prospect software tool for spectral energy distribution (SED) generation to study the multiwavelength emission of galaxies from the far-ultraviolet (FUV) to the far-infrared (FIR) at 0 ≤ z ≤ 10. We produce a physical model for the attenuation of galaxies across cosmic time by combining a local Universe empirical relation to compute the dust mass of galaxies from their gas metallicity and mass, attenuation curves derived from radiative transfer calculations of galaxies in the eagle hydrodynamic simulation suite, and the properties of shark galaxies. We are able to produce a wide range of galaxies, from the z = 8 star-forming galaxies with almost no extinction, z = 2 submillimetre galaxies, down to the normal star-forming and red-sequence galaxies at z = 0. Quantitatively, we find that shark reproduces the observed (i) z = 0 FUV-to-FIR, (ii) 0 ≤ z ≤ 3 rest-frame K-band, and (iii) 0 ≤ z ≤ 10 rest-frame FUV luminosity functions, (iv) z ≤ 8 UV slopes, (v) the FUV-to-FIR number counts (including the widely disputed 850 μm), (vi) redshift distribution of bright $850\\, \\mu$m galaxies, and (vii) the integrated cosmic SED from z = 0 to 1 to an unprecedented level. This is achieved without the need to invoke changes in the stellar initial mass function, dust-to-metal mass ratio, or metal enrichment time-scales. Our model predicts star formation in galaxy discs to dominate in the FUV-to-optical, while bulges dominate at the NIR at all redshifts. The FIR sees a strong evolution in which discs dominate at z ≤ 1 and starbursts (triggered by both galaxy mergers and disc instabilities, in an even mix) dominate at higher redshifts, even out to z = 10.
Publisher: Cambridge University Press (CUP)
Date: 2019
DOI: 10.1017/PASA.2019.18
Abstract: We present T ree F rog , a massively parallel halo merger tree builder that is capable comparing different halo catalogues and producing halo merger trees. The code is written in c++11, use the MPI and OpenMP API’s for parallelisation, and includes python tools to read/manipulate the data products produced. The code correlates binding energy sorted particle ID lists between halo catalogues, determining optimal descendant rogenitor matches using multiple snapshots, a merit function that maximises the number of shared particles using pseudo-radial moments, and a scheme for correcting halo merger tree pathologies. Focusing on VELOCI raptor catalogues for this work, we demonstrate how searching multiple snapshots spanning a dynamical time significantly reduces the number of stranded halos, those lacking a descendant or a progenitor, critically correcting poorly resolved halos. We present a new merit function that improves the distinction between primary and secondary progenitors, reducing tree pathologies. We find FOF accretion rates and merger rates show similar mass ratio dependence. The model merger rates from Poole, et al. [2017, 472, 3659] agree with the measured net growth of halos through mergers.
Publisher: SPIE
Date: 16-07-2010
DOI: 10.1117/12.857832
Publisher: Cambridge University Press (CUP)
Date: 2019
DOI: 10.1017/PASA.2019.12
Abstract: We present VELOCI raptor , a massively parallel galaxy/(sub)halo finder that is also capable of robustly identifying tidally disrupted objects and separate stellar halos from galaxies. The code is written in C++11, use the Message Passing Interface (MPI) and OpenMP Application Programming Interface (API) for parallelisation, and includes python tools to read/manipulate the data products produced. We demonstrate the power of the VELOCI raptor (sub)halo finder, showing how it can identify subhalos deep within the host that have negligible density contrasts to their parent halo. We find a subhalo mass-radial distance dependence: large subhalos with mass ratios of ≳10 −2 are more common in the central regions than smaller subhalos, a result of dynamical friction and low tidal mass loss rates. This dependence is completely absent in (sub)halo finders in common use, which generally search for substructure in configuration space, yet is present in codes that track particles belonging to halos as they fall into other halos, such as hbt +. VELOCI raptor largely reproduces the dependence seen without tracking, finding a similar radial dependence to hbt + in well-resolved halos from our limited resolution fiducial simulation.
Publisher: EDP Sciences
Date: 19-06-2012
Publisher: IEEE
Date: 11-2020
Publisher: SPIE
Date: 24-09-2012
DOI: 10.1117/12.925678
Publisher: Oxford University Press (OUP)
Date: 21-09-2020
Abstract: We thoroughly explore the properties of (sub)-millimetre (mm) selected galaxies (SMGs) in the shark semi-analytic model of galaxy formation. Compared to observations, the predicted number counts at wavelengths (λ) 0.6–2 mm and redshift distributions at 0.1–2 mm, agree well. At the bright end (≳1 mJy), shark galaxies are a mix of mergers and disc instabilities. These galaxies display a stacked far-ultraviolet (FUV)-to-far-infrared (FIR) spectrum that agrees well with observations. We predict that current optical/NIR surveys are deep enough to detect bright (& mJy) λ = 0.85–2 mm-selected galaxies at z ≲ 5, but too shallow to detect counterparts at higher redshift. A James Webb Space Telescope 10 000s survey should detect all counterparts for galaxies with S0.85mm ≳ 0.01 mJy. We predict SMG’s disks contribute significantly (negligibly) to the rest-frame UV (IR). We investigate the 0 ≤ z ≤ 6 evolution of the intrinsic properties of & mJy λ = 0.85–2 mm-selected galaxies finding their: (i) stellar masses are $\\gt 10^{10.2}\\rm \\, M_{\\odot }$, with the 2 mm ones tracing the most massive galaxies ($\\gt 10^{11}\\rm \\, M_{\\odot }$) (ii) specific star formation rates (SFR) are mildly (≈3–10 times) above the main sequence (MS) (iii) host halo masses are $\\gtrsim 10^{12.3}\\, \\rm M_{\\odot }$, with 2 mm galaxies tracing the most massive haloes (protoclusters) (iv) SMGs have lower dust masses ($\\approx 10^{8}\\, \\rm M_{\\odot }$), higher dust temperatures (≈40–45 K) and higher rest-frame V-band attenuation (& .5) than MS galaxies (v) sizes decrease with redshift, from 4 kpc at z = 1 to ≲1 kpc at z = 4 and (vi) the carbon monoxide line spectra of S0.85mm ≳ 1 mJy sources peak at 4 → 3. Finally, we study the contribution of SMGs to the molecular gas and cosmic SFR density at 0 ≤ z ≤ 10, finding that & mJy sources make a negligible contribution at z ≳ 3 and 5, respectively, suggesting current observations have unveiled the majority of the SF at 0 ≤ z ≤ 10.
Publisher: SPIE
Date: 16-07-2010
DOI: 10.1117/12.857064
Publisher: ACM
Date: 11-06-2018
Publisher: EDP Sciences
Date: 04-2013
Publisher: Cambridge University Press (CUP)
Date: 2023
DOI: 10.1017/PASA.2023.47
Publisher: Elsevier BV
Date: 07-2017
Publisher: Oxford University Press (OUP)
Date: 06-09-2018
Location: Australia
No related grants have been discovered for Rodrigo Tobar.