Einfluss psychosozialer Faktoren auf das Krankheitsgeschehen der Interstitiellen Cystitis

Die vorliegende Arbeit beschäftigt sich mit der Frage, inwieweit psychosoziale Belastungsfaktoren in Kindheit und Erwachsenenalter Einfluss auf Krankheitsentstehung und Verlauf der interstitiellen Cystitis (IC) haben. Als Testinstrumente fanden die MSBA (Mainzer Strukturierte Biographische Anamnese), das BSI (Brief Symptom Inventory) sowie ein IC-spezifischer Symptom- und Problem-Fragebogen Anwendung. Es erfolgte eine deskriptive Auswertung der Daten. An der Studie nahmen 30 Patienten teil, deren Symptomatik und Befunde die aktuellen Diagnosekriterien der IC erfüllen. Es zeigte sich ein erhöhtes Vorkommen wichtiger Kindheitsbelastungsfaktoren. Dazu zählen eine schlechte emotionale Bindung zu den Eltern bei mangelndem Geborgenheitsgefühl im Elternhaus, eine chronische Erkrankung eines Elternteils und körperliche Misshandlung. Sexueller Missbrauch spielte bei dieser Patientengruppe so gut wie keine Rolle. im Gesamtscore der Kindheitsbelastungsfaktoren liegen IC-Patienten ebenfalls weit über publizierten Durchschnittswerten für Stichproben gesunder Probanden. Zwischen Kindheitsbelastungsscore und klinischer IC-Symptomatik ergab sich keine signifikante Korrelation. Die aktuelle Sozialanamnese zeigte kein gehäuftes Vorkommen relevanter psychosozialer Belastungsfaktoren in den einzelnen Lebensbereichen. Die Lebensqualität ist durch die Krankheitssymptomatik stark eingeschränkt. Eine depressive Symptomatik gehörte in der Regel zum Krankheitsbild. Das BSI zeigte insgesamt erhöhte Werte für die subjektive Beeinträchtigung nahezu aller erfragten physischen und psychischen Symptome, insbesondere jedoch für Skalen Somatisierung, Ängstlichkeit und Phobische Angst. Zwischen Kindheitsbelastungsscore und Gesamtwert im BSI besteht ebenfalls keine signifikante Korrelation. Die Ergebnisse der Studie sprechen für eine psychosomatische Mitbeteiligung in der wahrscheinlich multifaktoriellen Genese der Interstitiellen Cystitis.The present study explores the influence of psychosocial adversities in childhood and adulthood in etiology and progress of the interstitial cystitis (IC). A systematic survey of the childhood risk factors was carried out using a specially developed, structered Interview for pain patients (MSBA-Mainzer Strukturierte Biographische Anamnese). Additionally the Brief Symptom Inventory (BSI) as well as a special IC-symptom and problem score was used. Essentially a descriptive evaluation was performed. Thirty IC-patients who fulfilled the contemporary diagnosing criterias (NIH-guidelines) participated in the study. The investigation showed higher values for relevant childhood adversities in IC-patients. A poor emotional relationship with both parents, low feeling of security in the parental home, chronic diseases of the parents and physical maltreatment were frequently reported. Sexual abuse did not play an important role in this IC group. In the cumulative adverse childhood experience score the IC-patients showed a relevant higher level than publicated datas of healthy control groups. There was no significant correlation between cumulative adverse childhood experience score and severity of clinical IC-symptoms. The contemporary social history did not show relevant psychosocial adversities in several spheres of life. The quality of life is extremely reduced because of pain and the urinary symptoms. Depression had a high incidence in this patient group. The BSI showed higher levels in almost all questioned symptom scales, especially in the dimensions somatization, anxiety and phobic anxiety. There is also no significant correlation between cumulative adverse childhood experience score and sum value in the BSI (GSI). The results of this study argue for psychosomatic participation in the probable multifactorial etiology of Interstitial Cystitis

The Concentration-Density Relation of Galaxies in Las Campanas Redshift Survey

We report the results of the evaluation of the ``concentration-density'' relation of galaxies in the local universe, taking advantage of the very large and homogeneous data set available from the Las Campanas Redshift Survey (Shectman et al. 1996). This data set consists of galaxies inhabiting the entire range of galactic environments, from the sparsest field to the densest clusters, thus allowing us to study environmental variations without combining multiple data sets with inhomogeneous characteristics. Concentration is quantified by the automatically-measured concentration index $C$, which is a good measure of a galaxy's bulge-to-disk ratio. The environment of the sample galaxies is characterized both by the three-space local galaxy density and by membership in groups and clusters. We find that the distribution of C in galaxy populations varies both with local density and with cluster/group membership: the fraction of centrally-concentrated galaxies increases with local galaxy density, and is higher in clusters than in the field. A comparison of the concentration-local density relation in clusters and the field shows that the two connect rather smoothly at the intermediate density regime, implying that the apparent cluster/field difference is only a manifestation of the variation with the local density. We conclude that the structure of galaxies is predominantly influenced by the local density and not by the broader environments characterized by cluster/field memberships.Comment: 11 pages, 4 figures, ApJ in press, uses psfig.st

The Evolution of galaxies in clusters. 5. A Study of populations since Z approximately equal to 0.5

The evolution of the colors of cluster galaxies since redshift of about 0.5 is studied using photometry of 33 clusters. In each cluster, those galaxies brighter than M(v) = -20 which are within the circular area containing the inner 30 percent of the total cluster population are selected. From the distribution of these galaxies in the color-magnitude plane, the fraction of galaxies whose rest-frame B-V colors are at least 0.2 mag bluer than the ridge line of the early-type galaxies at that magnitude is determined. It is found that low-redshift compact clusters form a very homogeneous group of objects with cores essentially devoid of blue galaxies. At redshifts greater than 0.1, compact clusters have significant numbers of blue galaxies, the fraction increasing with redshift. The colors of spiral galaxies in the cores of nearby clusters tend to be redder than those of spirals in the fiel

The Luminosity Function of Galaxies in the Las Campanas Redshift Survey

We present the $R$-band luminosity function for a sample of 18678 galaxies, with average redshift $z = 0.1$, from the Las Campanas Redshift Survey. The luminosity function may be fit by a Schechter function with $M^* = -20.29 \pm 0.02 + 5 \log h$, $\alpha = -0.70 \pm 0.05$, and $\phi^* = 0.019 \pm 0.001 \ h^3$~Mpc$^{-3}$, for absolute magnitudes$-23.0 \leq M - 5 \log h \leq -17.5$. We compare our luminosity function to that from other redshift surveys; in particular our normalization is consistent with that of the Stromlo-APM survey, and is therefore a factor of two below that implied by the$b_J \approx 20$bright galaxy counts. Our normalization thus indicates that much more evolution is needed to match the faint galaxy count data, compared to minimal evolution models which normalize at$b_J \approx 20$. Also, we show that our faint-end slope$\alpha = -0.7$, though ``shallower'' than typical previous values$\alpha = -1$, results primarily from fitting the detailed shape of the LCRS luminosity function, rather than from any absence of intrinsically faint galaxies from our survey. Finally, using [OII] 3727 equivalent width$W_{\lambda} = 5$~\AA \ as the dividing line, we find significant differences in the luminosity functions of emission and non-emission galaxies, particularly in their$\alpha$values. Emission galaxies have Schechter parameters$M^* = -20.03 \pm 0.03 + 5 \log h$and$\alpha = -0.9 \pm 0.1$, while non-emission galaxies are described by$M^* = -20.22 \pm 0.02 + 5 \log h$and$\alpha = -0.3 \pm 0.1$. (abridged abstract)Comment: 41 pages, including 13 postscript figures, uses AASTEX v4.0 style files. Important clarification of R-band definition, plus correction of luminosity densities and updated references. Main conclusions unchanged. Final version to appear in Ap