M_1 - M* Correlation in Galaxy Clusters
| dc.creator | Trevese, D. | |
| dc.creator | Cirimele, G. | |
| dc.creator | Appodia, B. | |
| dc.date | 1994-07-15 | |
| dc.date.accessioned | 2026-07-07T02:19:17Z | |
| dc.date.available | 2026-07-07T02:19:17Z | |
| dc.description | Photographic F band photometry of a sample of 36 Abell clusters has been used to study the relation between the magnitude $M_1$ of the brightest cluster member and the Schechter function parameter $M^*$. Clusters appear segregated in the $M_1$-$M^*$ plane according to their Rood \& Sastry class. We prove on a statistical basis that on average, going from early to late RS classes, $M_1$ becomes brighter while $M^*$ becomes fainter. The result agrees with the predictions of galactic cannibalism models, never confirmed by previous analyses. | |
| dc.description | 4 pages, postscript with 3 figures, in press : proc. XXIXth Rencontres de Moriond "Clusters of Galaxies" | |
| dc.identifier | https://arxiv.org/abs/astro-ph/9407047 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/9407047 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/9806 | |
| dc.subject | Astrophysics | |
| dc.title | M_1 - M* Correlation in Galaxy Clusters | |
| dc.type | text |