Paper

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  • Kaviraj et al.
  • http://arxiv.org/abs/0711.1493
  • Simulations on how minor mergers can explain the variation in UV-fluxes of ellipticals.
  • They say they cannot “rule out” gas accretion, but I wonder where the dividing line goes between a gas-rich dwarf being eaten and infall of gas.

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  • Grillo et al.
  • http://arxiv.org/abs/0711.0882
  • Combining gravitational lensing and galaxy dynamics (velocity dispersion as a funciton of radius in ellipticals) as a new and independant (!) method of measuring the geometry of the universe.
  • Way cool, if it ever gets on par in accuracy with the other methods.

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  • Malbon et al.
  • http://arxiv.org/abs/astro-ph/0607424
  • Black Hole – bulge mass relation
  • They find that the direct accretion of cold gas during starbursts is an important growth mechanism for lower mass black holes and at high redshift. On the other hand, the re-assembly of pre-existing black hole mass into larger units via merging dominates the growth of more massive black holes at low redshift.
  • As redshift decreases, progressively less massive black holes have the highest fractional growth rates, in line with recent claims of “downsizing” in quasar activity.

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  • Chilingarian et al.
  • http://arxiv.org/abs/0711.0412
  • short conference article introducing a java-client for euro3D datacubes (IFU-spectroscopy)
  • One day we all want to have everyones data easily accessible over a common interface. We aren’t there yet, but it’s good to know that people work on it.

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  • Hopkins et al.
  • http://arxiv.org/abs/astro-ph/0204528
  • star-formation rates of 50 well known, local Blue Compact Dwarf (BCD) galaxies based on their 1.4 GHz and 60 $\mu$m luminosities
  • Mk600, SBS0335-052, IZw18, UM461, UM462, Mk930

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  • Dowell et al.
  • http://arxiv.org/abs/astro-ph/0611586
  • SSCs in nearby spirals and irregulars from SDSS
  • SDSS colors plus spectral evolutionary modelling to determine cluster ages and mass.
  • They find a steeper slope for the mass function (at high masses) in irregulars as compared to spirals.
  • I wonder how reliable the masses are from this method. It’s a tricky business and dynamical cluster masses would be nicer.

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