HST-NICMOS Observations of M31's Metal Rich Globular Clusters and Their Surrounding Fields: I. Techniques
We have obtained HST-NICMOS observations of five of M31's most metal rich globular clusters. These data allow photometry of individual stars in the clusters and their surrounding fields. However, to achieve our goals -- obtain accurate luminosity functions to compare with their Galactic counter...
| Main Authors: | , , , , , , , , |
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| Format: | Journal article |
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2000
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| _version_ | 1797075111814103040 |
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| author | Stephens, A Frogel, J Freedman, W Gallart, C Jablonka, P Ortolani, S Renzini, A Rich, R Davies, R |
| author_facet | Stephens, A Frogel, J Freedman, W Gallart, C Jablonka, P Ortolani, S Renzini, A Rich, R Davies, R |
| author_sort | Stephens, A |
| collection | OXFORD |
| description | We have obtained HST-NICMOS observations of five of M31's most metal rich globular clusters. These data allow photometry of individual stars in the clusters and their surrounding fields. However, to achieve our goals -- obtain accurate luminosity functions to compare with their Galactic counterparts, determine metallicities from the slope of the giant branch, identify long period variables, and estimate ages from the AGB tip luminosity, we must be able to disentangle the true properties of the population from the observational effects associated with measurements made in very crowded fields. In this paper we present a careful analysis of photometry in crowded regions, and show how image blending affects the results and interpretation of such data. Although this analysis is specifically for our NICMOS observations in M31, the techniques we develop can be applied to any imaging data taken in crowded fields; we show how the effects of image blending will even limit NGST. We use three different techniques to analyze the effects of crowding on our data, including the insertion of artificial stars (traditional completeness tests) and the creation of completely artificial clusters. They are used to derive threshold- and critical-blending radii for each cluster, which determine how close to the cluster center reliable photometry can be achieved. The simulations also allow us to quantify and correct for the effects of blending on the slope and width of the RGB at different surface brightness levels. |
| first_indexed | 2024-03-06T23:45:41Z |
| format | Journal article |
| id | oxford-uuid:70ce1cac-3f05-43b5-98d5-aed43733d5c0 |
| institution | University of Oxford |
| last_indexed | 2024-03-06T23:45:41Z |
| publishDate | 2000 |
| record_format | dspace |
| spelling | oxford-uuid:70ce1cac-3f05-43b5-98d5-aed43733d5c02022-03-26T19:39:40ZHST-NICMOS Observations of M31's Metal Rich Globular Clusters and Their Surrounding Fields: I. TechniquesJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:70ce1cac-3f05-43b5-98d5-aed43733d5c0Symplectic Elements at Oxford2000Stephens, AFrogel, JFreedman, WGallart, CJablonka, POrtolani, SRenzini, ARich, RDavies, RWe have obtained HST-NICMOS observations of five of M31's most metal rich globular clusters. These data allow photometry of individual stars in the clusters and their surrounding fields. However, to achieve our goals -- obtain accurate luminosity functions to compare with their Galactic counterparts, determine metallicities from the slope of the giant branch, identify long period variables, and estimate ages from the AGB tip luminosity, we must be able to disentangle the true properties of the population from the observational effects associated with measurements made in very crowded fields. In this paper we present a careful analysis of photometry in crowded regions, and show how image blending affects the results and interpretation of such data. Although this analysis is specifically for our NICMOS observations in M31, the techniques we develop can be applied to any imaging data taken in crowded fields; we show how the effects of image blending will even limit NGST. We use three different techniques to analyze the effects of crowding on our data, including the insertion of artificial stars (traditional completeness tests) and the creation of completely artificial clusters. They are used to derive threshold- and critical-blending radii for each cluster, which determine how close to the cluster center reliable photometry can be achieved. The simulations also allow us to quantify and correct for the effects of blending on the slope and width of the RGB at different surface brightness levels. |
| spellingShingle | Stephens, A Frogel, J Freedman, W Gallart, C Jablonka, P Ortolani, S Renzini, A Rich, R Davies, R HST-NICMOS Observations of M31's Metal Rich Globular Clusters and Their Surrounding Fields: I. Techniques |
| title | HST-NICMOS Observations of M31's Metal Rich Globular Clusters and Their
Surrounding Fields: I. Techniques |
| title_full | HST-NICMOS Observations of M31's Metal Rich Globular Clusters and Their
Surrounding Fields: I. Techniques |
| title_fullStr | HST-NICMOS Observations of M31's Metal Rich Globular Clusters and Their
Surrounding Fields: I. Techniques |
| title_full_unstemmed | HST-NICMOS Observations of M31's Metal Rich Globular Clusters and Their
Surrounding Fields: I. Techniques |
| title_short | HST-NICMOS Observations of M31's Metal Rich Globular Clusters and Their
Surrounding Fields: I. Techniques |
| title_sort | hst nicmos observations of m31 s metal rich globular clusters and their surrounding fields i techniques |
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