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Morphological number-count and redshift distributions to I < 26 from the Hubble Deep Field: Implications for the evolution of Ellipticals, Spirals and Irregulars | | S. P. Driver
; A. Fernandez-Soto
; W. J. Couch
; S. C. Odewahn
; R. A. Windhorst
; S. Phillipps
; K. Lanzetta
; A. Yahil
; | | Date: |
8 Feb 1998 | | Subject: | astro-ph | | Affiliation: | UNSW), A. Fernandez-Soto (UNSW), W. J. Couch (UNSW), S. C. Odewahn (CalTech), R. A. Windhorst (ASU), S. Phillipps (U. Bristol), K. Lanzetta (Stony-Brook), A. Yahil (Stony-Brook | | Abstract: | We combine the photometric redshift data of Fernandez-Soto et al. (1997) with the morphological data of Odewahn et al. (1996) for all galaxies with I < 26.0 detected in the Hubble Deep Field. From this combined catalog we generate the morphological galaxy number-counts and corresponding redshift distributions and compare these to the predictions of high normalization zero- and passive- evolution models. From this comparison we conclude the following: (1) E/S0s are seen in numbers and over a redshift range consistent with zero- or minimal passive- evolution to I = 24. Beyond this limit fewer E/S0s are observed than predicted implying a net negative evolutionary process --- luminosity dimming, disassembly or masking by dust --- at I > 24. (2) Spiral galaxies are present in numbers consistent with zero- evolution predictions to I = 22. Beyond this magnitude some net- positive evolution is required. Although the number-counts are consistent with the passive-evolution predictions to I=26.0 the redshift distributions favor number AND luminosity evolution. (3) There is no obvious explanation for the late-type/irregular class and this category requires further subdivision. While a small fraction of the population lies at low redshift (i.e. true irregulars), the majority lie at redshifts, 1 < z < 3. At z > 1.5 mergers are frequent and, taken in conjunction with the absence of normal spirals at z > 2, the logical inference is that they represent the progenitors of normal spirals forming via hierarchical merging. | | Source: | arXiv, astro-ph/9802092 | | Services: | Forum | Review | PDF | Favorites | |
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