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Date and Time of the Query: 2019-06-20 T14:11:09 PDT
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For refcode 2000MNRAS.313..800D:
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Copyright by Royal Astronomical Society. 2000MNRAS.313..800D Tracing the vertical composition of disc galaxies through colour gradients Richard de Grijs and Reynier F. Peletier Accepted 1999 November 25. Received 1999 November 25; in original form 1999 August 16 ABSTRACT Optical observations of a statistically complete sample of edge-on disc- dominated galaxies are used to study the intrinsic vertical colour gradients in the galactic discs, in order to constrain the effects of population gradients, residual dust extinction and gradients in the metal abundance of the galaxies. For the majority of our sample galaxies, the colours and colour gradients in the range 1.0h_z_ <= |z| <= 3.0h_z_ most likely reflect the intrinsic galactic properties (where h_z_ is the vertical scaleheight). It appears that the intrinsic vertical colour gradients are either non- existent, or small and relatively constant as a function of position along the major axes of the galaxies. On average, the earlier-type galaxies exhibit smaller vertical (B-I) gradients than the later types; our results are consistent with the absence of any vertical colour gradient in the discs of the early-type sample galaxies. In most galaxies small-scale variations in the magnitude and even the direction of the vertical gradient are observed: at larger galactocentric distances they generally display redder colours with increasing z height, whereas the opposite is often observed in and near the galactic centres. For a significant fraction of our sample galaxies another mechanism in addition to the effects of stellar population gradients is required to explain the magnitude of the observed gradients. The non-zero colour gradients in a significant fraction of our sample galaxies are likely to be (at least) partially due to residual dust extinction at these z heights, as is also evidenced from the sometimes significant differences between the vertical colour gradients measured on either side of the galactic planes. We suggest that initial vertical metallicity gradients, if any, have probably not been accentuated by accretion or merging events over the lifetimes of our sample galaxies. On the other hand, they may have weakened any existing vertical metallicity gradients, although they also may have left the existing correlations unchanged. Keywords: galaxies: abundances - galaxies: fundamental parameters - galaxies: photometry - galaxies: spiral
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