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Cox, Lloyd; Ottmann, Goetz; Jacobsen, Michael Hviid; Lowish, Susan; Beilharz, Peter

doi:10.1177/0725513604042661

Cited by 2 publications

(4 citation statements)

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“…The galaxy simulations used in this work have been described in detail in earlier papers (Cox 2004;Jonsson 2004;Cox et al 2006Cox et al , 2008Jonsson et al 2006;Lotz et al 2008;Rocha et al 2008), but a brief overview will be given here for context. The simulations are of seven different spiral galaxy models run with the GADGET SPH code, including star formation and feedback (Springel, Yoshida & White 2001;Springel 2005).…”

Section: Galaxy Simulationsmentioning

confidence: 99%

High-resolution panchromatic spectral models of galaxies including photoionization and dust

Jönsson

Groves

Cox

2010

Monthly Notices of the Royal Astronomical Society

241

322

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An updated version of the dust radiation‐transfer code sunrise, including models for star‐forming regions and a self‐consistent calculation of the spatially dependent dust and PAH emission, is presented. Given a hydrodynamic simulation of a galaxy, this model can calculate a realistic 2D ultraviolet–submillimetre spectral energy distribution of the galaxy, including emission lines from H ii regions, from any viewpoint. To model the emission from star‐forming regions, the mappingsiii photoionization code is used. The high wavelength resolution (∼1000 wavelengths) is made possible by the polychromatic Monte Carlo algorithm employed by sunrise. From the 2D spectral energy distributions (SEDs), images in any filter bands or integrated galaxy SEDs can be created. Using a suite of hydrodynamic simulations of disc galaxies, the output broad‐band images and SEDs are compared with observed galaxies from the multiwavelength SINGS and SLUGS galaxy surveys. Overall, the output SEDs show a good match with observed galaxies in colours ranging from far‐UV to submillimetre wavelengths. The only possible exception is the 160/850 μm colour, which the simulations underestimate by a factor of ∼5 compared to the SINGS sample. However, the simulations here agree with the SLUGS galaxies, which consistently have significantly larger amounts of cold dust than the SINGS galaxies. The sunrise model can be used to generate simulated observations of arbitrary hydrodynamic galaxy simulations. In this way, predictions of galaxy formation theories can be directly tested against observations of galaxies.

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Section: Galaxy Simulationsmentioning

confidence: 99%

High-resolution panchromatic spectral models of galaxies including photoionization and dust

Jönsson

Groves

Cox

2010

Monthly Notices of the Royal Astronomical Society

241

322

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“…The morphology of ARP 24 indicates that it may formed in a minor merger scenario (interaction between a gas-rich late-type spiral and a small companion) or from cosmological accretion of gas on galactic disks (Bournaud et al 2005). Shaping/reshaping of galaxies is the biggest effect generally attribute to mergers (Cox 2004). The tidal stripping of a satellite can produce features such as long tails, and the accretion introduces new stellar populations into the galactic disk (Walker et al 1996), i.e., promotes a high SFR (e.g., Mihos & Hernquist 1994; see also Cox 2004) in ARP 24.…”

Section: Possible Formation Scenarios Of the Yscs In Arp 24mentioning

confidence: 99%

“…Shaping/reshaping of galaxies is the biggest effect generally attribute to mergers (Cox 2004). The tidal stripping of a satellite can produce features such as long tails, and the accretion introduces new stellar populations into the galactic disk (Walker et al 1996), i.e., promotes a high SFR (e.g., Mihos & Hernquist 1994; see also Cox 2004) in ARP 24. The YSCs may form as a consequence of the high SFR per unit area in the galaxy (Larsen & Richtler 2000).…”

Section: Possible Formation Scenarios Of the Yscs In Arp 24mentioning

confidence: 99%

“…The existence of a large amount of young (A-type) stars in the nucleus of ARP 24 (see §3.3) may also be related to the age of interaction in this system. However, such a formation scenario still remains speculative, and needs to be confirmed by hydrodynamical modeling (e.g., Struck et al 2005) and numerical simulations of star formation in galaxy mergers (e.g., Struck & Smith 2003;Cox 2004).…”

Section: Possible Formation Scenarios Of the Yscs In Arp 24mentioning

confidence: 99%

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Multiwavelength Study of Young Massive Star Clusters in the Interacting Galaxy Arp 24

Cao

2007

Astron J

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We made a multi-wavelength study of young massive star clusters (YSCs) in the interacting galaxy ARP 24, using the optical and ultraviolet images from Hubble Space Telescope (HST), Sloan Digital Sky Survey, and Galaxy Evolution Explorer; the mid-infrared images from Spitzer Space Telescope; and the narrowband Hα image and optical spectra from the NAOC 2.16 m telescope. Based on the HST images, we found that the brightest infrared knot in ARP 24 is associated with a complex of five young massive star clusters, within a region of ∼ 0.95 ′′ radius (127pc) in size. The ages and masses of the star clusters in this complex and other regions were estimated using HST broadband photometries and the Starburst99 synthesis models. The star clusters in this complex are very young (within ages of ∼ 3-5 Myr) and massive (masses of ∼10 5 M ⊙ ). The ionization parameter and metallicity of the complex were estimated using the emission line ratios, and the star formation rates were calculated using monochromatic 24µm, FUV, and Hα line luminosities. We speculate that ARP 24 may formed by a retrograde fly-by encounter indicated by its one-armed appearance and fanlike structure, and the formation of the YSCs in this galaxy is triggered by the interaction. The clusters in the YSC complex may formed in a single giant molecular cloud simultaneously. From the ultraviolet to mid-infrared spectral energy distributions, we found that the region of the YSC complex is relatively bluer in optical and has higher 24µm dust emission relative to the starlight and 8µm emission. This warm infrared color may due to strong UV radiation field or other mechanisms (e.g., shocks) within this region which may destroy the Polycyclic Aromatic Hydrocarbons and enhance the small grain emission at 24µm.

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Reviews

Cited by 2 publications

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High-resolution panchromatic spectral models of galaxies including photoionization and dust

High-resolution panchromatic spectral models of galaxies including photoionization and dust

Multiwavelength Study of Young Massive Star Clusters in the Interacting Galaxy Arp 24

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