Defending Life

Jönsson, Rita B

doi:10.1111/j.1365-3083.2007.01990.x

Cited by 97 publications

(141 citation statements)

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“…We follow the hydrodynamic evolution of galaxy mergers of varying mass and mass ratios using the N ‐body plus smoothed particle hydrodynamics (SPH) code gadget3 (Springel 2005). The synthetic photometric properties of the simulations are then calculated using the 3D adaptive mesh Monte Carlo polychromatic radiative transfer code, sunrise (Jonsson 2006). Our goal throughout is to utilize physical parameter input to the models directly constrained by observations of SMGs where possible, and from local ultraluminous infrared galaxies (ULIRGs) or the Milky Way Galaxy when data from SMGs may not be available.…”

Section: Methodsmentioning

confidence: 99%

The formation of high-redshift submillimetre galaxies

Narayanan

Hayward

Cox

et al. 2010

Monthly Notices of the Royal Astronomical Society

181

248

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We describe a model for the formation of z∼ 2 submillimetre galaxies (SMGs) which simultaneously accounts for both average and bright SMGs while providing a reasonable match to their mean observed spectral energy distributions (SEDs). By coupling hydrodynamic simulations of galaxy mergers with the high‐resolution 3D polychromatic radiative transfer code sunrise, we find that a mass sequence of merger models which use observational constraints as physical input naturally yield objects which exhibit black hole, bulge and H2 gas masses similar to those observed in SMGs. The dominant drivers behind the 850 μm flux are the masses of the merging galaxies and the stellar birth cloud covering fraction. The most luminous (S850≳ 15 mJy) sources are recovered by ∼1013 M⊙ 1:1 major mergers with a birth cloud covering fraction close to unity, whereas more average SMGs (S850∼ 5–7 mJy) may be formed in lower mass haloes (∼5 × 1012 M⊙). These models demonstrate the need for high spatial resolution hydrodynamic and radiative transfer simulations in matching both the most luminous sources as well as the full SEDs of SMGs. While these models suggest a natural formation mechanism for SMGs, they do not attempt to match cosmological statistics of galaxy populations; future efforts along this line will help ascertain the robustness of these models.

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Section: Methodsmentioning

confidence: 99%

The formation of high-redshift submillimetre galaxies

Narayanan

Hayward

Cox

et al. 2010

Monthly Notices of the Royal Astronomical Society

181

248

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“…sunrise is a parallel code which performs full Monte Carlo radiative transfer calculations using an adaptive‐mesh refinement grid (Jonsson 2006; Jonsson et al 2006). This code was developed to calculate the effects of dust on the emission from the gadget N ‐body/SPH simulations.…”

Section: Galaxy Merger Simulationsmentioning

confidence: 99%

“…sunrise can model arbitrary geometries of emitting and absorbing/scattering material with a large spatial dynamical range and efficiently generate images of the emerging radiation viewed from arbitrary points in space. We use sunrise v2 for these simulations (Jonsson 2006). Given a particular simulation geometry and viewing angle, sunrise v2 performs the Monte Carlo radiative transfer calculation for 20 wavelengths from the far‐ultraviolet (FUV) to the mid‐infrared and interpolates a resulting spectral energy distribution of 510 wavelengths including the effects of absorption and scattering.…”

Section: Galaxy Merger Simulationsmentioning

confidence: 99%

Galaxy merger morphologies and time-scales from simulations of equal-mass gas-rich disc mergers

Lotz

Jönsson

Cox

et al. 2008

Monthly Notices of the Royal Astronomical Society

409

592

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A key obstacle to understanding the galaxy merger rate and its role in galaxy evolution is the difficulty in constraining the merger properties and time‐scales from instantaneous snapshots of the real Universe. The most common way to identify galaxy mergers is by morphology, yet current theoretical calculations of the time‐scales for galaxy disturbances are quite crude. We present a morphological analysis of a large suite of gadgetN‐body/hydrodynamical equal‐mass gas‐rich disc galaxy mergers which have been processed through the Monte Carlo radiative transfer code sunrise. With the resulting images, we examine the dependence of quantitative morphology (G, M20, C, A) in the SDSS g band on merger stage, dust, viewing angle, orbital parameters, gas properties, supernova feedback and total mass. We find that mergers appear most disturbed in G−M20 and asymmetry at the first pass and at the final coalescence of their nuclei, but can have normal quantitative morphologies at other merger stages. The merger observability time‐scales depend on the method used to identify the merger as well as the gas fraction, pericentric distance and relative orientation of the merging galaxies. Enhanced star formation peaks after and lasts significantly longer than strong morphological disturbances. Despite their massive bulges, the majority of merger remnants appear disc‐like and dusty in g‐band light because of the presence of a low‐mass star‐forming disc.

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“…We used sunrise (Jonsson 2006), a Monte Carlo radiative transfer code, to generate a posteriori, mock images of the simulations, incorporating the effects of dust attenuation and spanning a range of viewing angles from edge‐ to face‐on perspectives, as listed in Table 1.…”

Section: Simulated Galaxy Samplementioning

confidence: 99%

Advanced morphological galaxy classification: a comparison of observed and simulated galaxies

Hambleton¹,

Gibson

Stinson

et al. 2011

Monthly Notices of the Royal Astronomical Society

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Encoded within the morphological structure of galaxies are clues related to their formation and evolutionary history. Recent advances pertaining to the statistics of galaxy morphology include sophisticated measures of concentration (C), asymmetry (A) and clumpiness (S). In this study, these three parameters (CAS) have been applied to a suite of simulated galaxies and compared with observational results inferred from a sample of nearby galaxies. The simulations span a range of late‐type systems, with masses between ∼1010 and ∼1012 M⊙, and employ star formation density thresholds between 0.1 and 100 cm−3. We have found that the simulated galaxies possess comparable concentrations to their observed counterparts. However, the results of the CAS analysis revealed that the simulated galaxies are generally more asymmetric, and that the range of clumpiness values extends beyond the range of those observed. Strong correlations were obtained between the three CAS parameters and colour (B − V), consistent with observed galaxies. Furthermore, the simulated galaxies possess strong links between their CAS parameters and Hubble type, mostly in‐line with their observed counterparts.

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Defending Life

Abstract: Defending LifeThe nature of host-parasite relations Elling Ulvestad 2007, XIX, 241 pp., Hardcover ISBN: 978-1-4020-5675-8 Springer (http://www.springer.com)

Cited by 97 publications

References 0 publications

The formation of high-redshift submillimetre galaxies

The formation of high-redshift submillimetre galaxies

Galaxy merger morphologies and time-scales from simulations of equal-mass gas-rich disc mergers

Advanced morphological galaxy classification: a comparison of observed and simulated galaxies

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