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  • Cambridge University Press (CUP)  (3)
  • 1
    Online Resource
    Online Resource
    The far-infrared view of M87 as seen by the Herschel Space Observatory
    Cambridge University Press (CUP) ; 2010
    In:  Proceedings of the International Astronomical Union Vol. 6, No. S275 ( 2010-09), p. 145-149
    Details
    In: Proceedings of the International Astronomical Union, Cambridge University Press (CUP), Vol. 6, No. S275 ( 2010-09), p. 145-149
    Abstract: The origin of the far-infrared emission from the nearby radio galaxy M87 remains a matter of debate. Some studies find evidence of a far-infrared excess due to thermal dust emission, whereas others propose that the far-infrared emission can be explained by synchrotron emission without the need for an additional dust emission component. We observed M87 with PACS and SPIRE as part of the Herschel Virgo Cluster Survey (HeViCS). We compare the new Herschel data with a synchrotron model based on infrared, submm and radio data to investigate the origin of the far-infrared emission. We find that both the integrated SED and the Herschel surface brightness maps are adequately explained by synchrotron emission. At odds with previous claims, we find no evidence of a diffuse dust component in M87.
    Type of Medium: Online Resource
    ISSN: 1743-9213 , 1743-9221
    URL: Article
    DOI: 10.1017/S1743921310015838
    Language: English
    Publisher: Cambridge University Press (CUP)
    Publication Date: 2010
    detail.hit.zdb_id: 2170724-8
    SSG: 16,12
    Location Call Number Limitation Availability
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  • 2
    Online Resource
    Online Resource
    The cool and warm molecular gas in M82 with Herschel -SPIRE
    Cambridge University Press (CUP) ; 2012
    In:  Proceedings of the International Astronomical Union Vol. 10, No. H16 ( 2012-08), p. 618-618
    Details
    In: Proceedings of the International Astronomical Union, Cambridge University Press (CUP), Vol. 10, No. H16 ( 2012-08), p. 618-618
    Abstract: We present Herschel -SPIRE imaging spectroscopy (194-671 μm) of the bright starburst galaxy M82. We use RADEX and a Bayesian Likelihood Analysis to simultaneously model the temperature, density, column density, and filling factor of both the cool and warm components of molecular gas traced by the entire CO ladder up to J=13-12. The high-J lines observed by SPIRE trace much warmer gas (~500 K) than those observable from the ground. The addition of 13 CO (and [C I]) is new and indicates that [C I] may be tracing different gas than 12 CO. At such a high temperature, cooling is dominated by molecular hydrogen; we conclude with a discussion on the possible excitation processes in this warm component. Photon-dominated region (PDR) models require significantly higher densities than those indicated by our Bayesian likelihood analysis in order to explain the high-J CO line ratios, though cosmic-ray enhanced PDR models can do a better job reproducing the emission at lower densities. Shocks and turbulent heating are likely required to explain the bright high-J emission.
    Type of Medium: Online Resource
    ISSN: 1743-9213 , 1743-9221
    URL: Article
    DOI: 10.1017/S1743921314012472
    Language: English
    Publisher: Cambridge University Press (CUP)
    Publication Date: 2012
    detail.hit.zdb_id: 2170724-8
    SSG: 16,12
    Location Call Number Limitation Availability
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    Online Resource
  • 3
    Online Resource
    Online Resource
    Variations in the 24 μm morphologies of nearby galaxies
    Cambridge University Press (CUP) ; 2007
    In:  Proceedings of the International Astronomical Union Vol. 3, No. S245 ( 2007-07), p. 121-124
    Details
    In: Proceedings of the International Astronomical Union, Cambridge University Press (CUP), Vol. 3, No. S245 ( 2007-07), p. 121-124
    Abstract: To study the distribution of star formation and dust emission within nearby galaxies, we measured five morphological parameters in the 24 μm wave band for 73 galaxies observed as part of the Spitzer Infrared Nearby Galaxies Survey. The morphological parameters demonstrate strong variations along the Hubble sequence, including statistically significant differences between S0/a-Sab and Sc-Sd galaxies. Early-type spiral galaxies are generally found to be compact, centralized, symmetric sources in the 24 μm band, whereas late-type spiral galaxies are generally found to be extended, asymmetric 24 μm sources. These results suggest that processes that increase the real or apparent sizes of galaxies' bulges also lead to more centralized 24 μm emission.
    Type of Medium: Online Resource
    ISSN: 1743-9213 , 1743-9221
    URL: Article
    DOI: 10.1017/S1743921308017432
    Language: English
    Publisher: Cambridge University Press (CUP)
    Publication Date: 2007
    detail.hit.zdb_id: 2170724-8
    SSG: 16,12
    Location Call Number Limitation Availability
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    Online Resource
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