Frank, S. and Rasera, Y. and Vibert, D. and Milliard, B. and Popping, A. and Blaizot, J. and Courty, S. and Deharveng, J.-M. and Péroux, C. and Teyssier, R. and Martin, C. D. (2012) Observable signatures of the low-z circumgalactic and intergalactic media: ultraviolet line emission in simulations. Monthly Notices of the Royal Astronomical Society, 420 (2). pp. 1731-1753. ISSN 0035-8711 http://resolver.caltech.edu/CaltechAUTHORS:20120228-065354763
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We present for the first time predictions for ultraviolet (UV) line emission of intergalactic and circumgalactic gas from Adaptive Mesh Resolution (AMR) large-scale structure simulations at redshifts 0.3 < z < 1.2, with a specific emphasis on its observability with current and near-future UV instrumentation. In the three UV transitions of interest (Lyα, O vi and C iv), there is a clear bimodality in the type of emitting objects: the overwhelming majority of the flux stems from discrete, compact sources, while a much larger fraction of the volume is filled by more tenuous gas. We characterize both object types with regard to their number densities, physical sizes and shapes, brightnesses and luminosities, velocity structures, masses, temperatures, ionization states, and metal content. Degrading our AMR grids to characteristic resolutions offered by available (such as FIREBall) or foreseeable instrumentation allows us to assess which inferences can be drawn from currently possible observations, and to set foundations to prepare observing strategies for future missions. In general, the faint emission of the intergalactic medium (IGM) and filamentary structure remains beyond the capabilities of instruments with only short-duration exposure potential (i.e. stratospheric balloons), even for the most optimistic assumption for Lyα, while the yet fainter metal line transitions (O vi and C iv) for these structures will actually remain challenging for long-duration exposures (i.e. space-based telescopes), mostly due to their low metallicities pushing them more than three orders of magnitudes in brightness below the Lyα radiation. For the bright, circumgalactic medium, the situation is much more promising, and it is foreseeable that in the near future we will not only just detect such sources, but also the combination of all three lines in addition to velocity information will yield valuable insight into the physical processes at hand, illuminating (and discriminating between) important mechanisms during the formation of galaxies and their backreaction on to the IGM from whence they formed.
|Additional Information:||© 2012 The Authors. Monthly Notices of the Royal Astronomical Society © 2012 RAS. Accepted 2011 November 8. Received 2011 November 8; in original form 2011 September 14. Article first published online: 13 Jan 2012. This work has been funded within the BINGO! project by ANR under the allocation ANR-08-BLAN-0316-01. Access to the HPC resources of CINES was granted and funded under the allocation 2010-x2010042191 made by Grand Equipement National de Calcul Intensif (GENCI).|
|Subject Keywords:||methods: numerical; intergalactic medium; galaxies: structure; ultraviolet: galaxies; ultraviolet: general|
|Official Citation:||Frank, S., Rasera, Y., Vibert, D., Milliard, B., Popping, A., Blaizot, J., Courty, S., Deharveng, J.-M., Péroux, C., Teyssier, R. and Martin, C. D. (2012), Observable signatures of the low-z circumgalactic and intergalactic media: ultraviolet line emission in simulations. Monthly Notices of the Royal Astronomical Society, 420: 1731–1753. doi: 10.1111/j.1365-2966.2011.20172.x|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Ruth Sustaita|
|Deposited On:||28 Feb 2012 15:21|
|Last Modified:||28 Feb 2012 15:21|
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