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clues to a better picture of how galaxies form." The reason of course is that nearby galaxies can be studied in far greater detail than those that lie at the edge of the Cosmos and importantly that in general cosmological surveys cover such small areas of sky that they in fact do not sample the local population at all. Observations of
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Peebles and Nusser stress the importance of nearby galaxies if one is to understand the detailed processes of galaxy evolution and hence develop a complete model of how galaxies change with time. They specifically say that "âĶ.nearby galaxies offer rich and still far from completely explored
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once the final data becomes available in late 2013 and the intersection of this sample with the WH sample is the WHP sample. The WH sample consists of 80 early type galaxies (T< 0) and 533 late types, 70 of which may be described as star forming irregulars/dwarfs. Also, within the WH sample, 94
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data to define a near infrared selected sample. As many galaxy properties correlate first with stellar mass, the near infrared, where for most galaxies the bulk of the stellar radiation emerges, provides the best available choice for galaxy selection. There are 3045 galaxies with a WISE 3.4Ξm
188:>1 arc min (â12 kpc at 40 Mpc) â the W sample. Currently within the Herschel archive there are 613 observations of galaxies from this W sample. The intersection of these two samples will be referred to as the WH sample. A similar selection will be carried out for galaxies detected by
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is broadly correct. Although there is good agreement over large spatial scales there are some challenging disagreements between theory and observation when one looks over smaller scales and particularly at the properties of nearby galaxies. The distributions of galaxy
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and size, their locations within larger scale structures in the
Universe and their star formation histories as a function of galactic mass are all examples of disparity with the currently favoured model. In a recent
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To achieve the objectives set out above a representative sample of galaxies for study was defined. The
Herschel data alone does not provide a large completely sampled region of sky, but it is possible to use the
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Interpret the galaxy SEDs using radiative transfer and full SED models, to derive stellar, gas and dust properties, star formation rates and histories as a function of morphological type.
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Develop a dust evolution model that is consistent with the SEDs of galaxies of different morphological types and determine the primary sources and sinks for cosmic dust.
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databases. This data will be combined with other available data from both ground-based and space-based telescopes to make the most extensive and intensive study of
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for exploitation of space science and exploration data. It is a collaboration of six
European institutes with a primary goal of exploiting existing data in the
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The DustPedia project aims at addressing five specific but quite broad science issues that have a direct bearing on current evolutionary models of galaxies:
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197:> 5 arc min and so are resolved in the Herschel bands and lend themselves to full radiative transfer and infrared/mm SED modelling.
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Derive dust mass functions to the lowest-possible luminosities and masses and to compare these with cosmological surveys and the
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Determine how the dust NIR-mm/radio SED evolves throughout the
Universe and how this is related to the underlying dust properties
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A collage of the DustPedia galaxies as seen by the
Spectral and Photometric Imaging Receiver (SPIRE) instrument aboard Herschel.
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models of galaxy and larger scale structure formation. This has led to the wide spread belief that the current
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Peebles; et al. (2010). "Nearby galaxies as pointers to a better theory of cosmic evolution".
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rate, growth of the metal abundance, loss of metals in galactic winds, physical processes in the
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Please help update this article to reflect recent events or newly available information.
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Many observations of galaxies over large look back times correspond very well with
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address many aspects of the current galaxy evolutionary model i.e.
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etc. and so offer the potential for a much better understanding.
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Frenk; et al. (2012). "Dark matter and cosmic structure".
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detection (SN > 3) within 3000 km s (â40 Mpc) of the
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