Spectral clump

Abstract. High resolution spectral data of red clump stars towards the NGP have been obtained with the spectrograph Elodie at OHP stars. Nearby Hipparcos red clump stars were also observed. We determine the thin and thick properties kinematics and chemical abundances in the solar neighbourhood. We estimate the surface mass density of the galactic disk, we also determine the thin and thick disk chemical properties. 

Cytology, that is, the visual inspection of exfoliated cells, is most commonly carried out for smears of cells, which are deposited ( smeared ) directly from brushes, spatulas or other exfoliation devices onto microscope slides. Such smears are unsuitable for spectral analysis, since they contain clumps of cells, cellular debris, erythrocytes and other contamination. However, better methods of cell slide preparations have been introduced into cytology, among them the ThinPrep methods developed by Cytyc, Inc. (see ref. 7), and spin centrifugation deposition techniques. These methods are very good for real exfoliated cell samples,7 since they permit the purification of the cell exfoliate, enrichment in the cells desired for analysis and produce good monolayers for visual cell inspection. 

The correlation analyses of toner particle size and size distribution parameters and image quality characteristics of toner deposits as measured by the spectral dependence of contrast transfer function and noise show high coefficients of correlation Specifically the Wiener spectrum data appear to yield the weight geometric mean and standard deviation of the toner population in this study. Therefore the Wiener spectrum may be another analytical tool in characterizing particle populations. It must be pointed out that the analysis reported here is mainly empirical. Further work is needed to refine the models and to examine the limits of applicability of these tests. Factors such as particle clumping, non-uniform depositions and optical limitations are specific areas for examination. 

The spectrum is parametrized by the numerical values of the M + 1 multipliers X,. In principle, their values are determined by the values of the Fourier transform C(t) at the times t r = 0, 1,. .., M, / = 0. The separation of time scales in the exploration of phase space is equivalent to a specification of times t, such that the later times differ by an order of magnitude or more from the earlier ones. Times which are comparable will correspond to the spectral structure at a given level of resolution. If the times fall into three distinct groups (early, intermediate, and late) then the resulting spectrum will have three levels of clumps as in Fig. 4. 

It is interesting to note in passing that frogs, octupi and some other animals use the spectral flattening effect to change their appearance. They appear dark when pigmented cells in their skin spread out to cover the surface more or less uniformly, and pale when the cells clump together. 

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