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The Millennium Galaxy Catalogue: the severe attenuation of bulge flux by dusty spiral discs

Published online by Cambridge University Press:  01 July 2007

Simon P. Driver
Simon P. Driver
Affiliation:
School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews, KY16 8XB, Fife, U.K. email: spd3@st-and.ac.uk
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Abstract

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Using the Millennium Galaxy Catalogue we quantify the dependency of the disc and bulge luminosity functions on galaxy inclination. Using a contemporary dust model we show that our results are consistent with galaxy discs being optically thick in their central regions (). As a consequence the measured B-band fluxes of bulges can be severely attenuated by 50% to 95% depending on disc inclination. We argue that a galaxy's optical appearance can be radically transformed by simply removing the dust, e.g. during cluster infall, with mid-type galaxies becoming earlier, redder, and more luminous. Finally we derive the mean photon escape fraction from the integrated galaxy population over the 0.1 μm to 2.1 μm range, and use this to show that the energy of starlight absorbed by dust (in our model) is in close agreement with the total far-IR emission.

Keywords

galaxies: bulgesgalaxies: evolutiongalaxies: formationgalaxies: fundamental parametersgalaxies: luminosity functionmass function
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S245: Formation and Evolution of Galaxy Bulges , July 2007 , pp. 403 - 406
Copyright
Copyright © International Astronomical Union 2008

References

Allen, P. D. et al. 2006, MNRAS 371, 2CrossRefGoogle Scholar
Burstein, D., Haynes, M., & Faber, S. 1991, Nature 353, 515CrossRefGoogle Scholar
Byun, Y. I., Freeman, K. C., & Kylafis, N. D. 1993, ApJ 432, 114CrossRefGoogle Scholar
Disney, M. J., Davies, J. I., & Phillipps, S.MNRAS 239, 939CrossRefGoogle Scholar
Driver, S. P. et al. 2005, MNRAS 360, 81CrossRefGoogle Scholar
Driver, S. P. et al. 2007, MNRAS 379, 1022CrossRefGoogle Scholar
Gonzalez, R. et al. 1998, ApJ 506, 152CrossRefGoogle Scholar
Liske, J. et al. 2003, MNRAS 344, 307CrossRefGoogle Scholar
Möllenhoff, C., Popescu, C. C., & Tuffs, R. J. 2006, ApJ 456, 941Google Scholar
Popescu, C. C. et al. 2000, ApJ 362, 138Google Scholar
Pierini, D. et al. 2003, ApJ 617, 1022CrossRefGoogle Scholar
Tuffs, R. J. et al. 2004, ApJ 419, 821Google Scholar
Valentijn, E. A. 1990, Nature 346, 153CrossRefGoogle Scholar
White, R. E. (III), Keel, W. C., & Conselice, C. J. 2000, ApJ 542, 761CrossRefGoogle Scholar