Measuring the GC luminosity function up to z ~ 0.2

Details Measuring the GC luminosity function up to z ~ 0.2 Measuring the GC luminosity function up to z ~ 0.2

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010iaus..266..351a&link_type=abstract

Star clusters: basic galactic building blocks throughout time and space, Proceedings of the International Astronomical Union, IA

Mathematics

Logic

Techniques: Photometric, Globular Clusters: General, Galaxies: Star Clusters

Scientific paper

Globular clusters (GCs) are stellar systems (~106 M&sun;) with very regular symmetry, single age, and single metallicity. Spectroscopic studies have revealed very old ages, suggesting that GCs were formed in the earliest stages of galaxy formation and assembly. The aim of this work is to find out how far we can measure the GC luminosity function, specific frequency, and radial distribution, applying the surface-brightness-fluctuations (SBF) technique to deep ACS images. To this end, we apply the effects caused by higher redshift to HST/ACS images (in two optical bands, F606W and F814W) of M87, an elliptical galaxy with a very well-studied GC system. The effects involved are: (i) evolution, (ii) inverse k correction, (iii) binning of the image to smaller angular size, (iv) cosmological dimming of surface brightness, and (v) noise addition to account for different exposure times. After processing the images we detect the brightest GCs through direct photometry (e.g., with SExtractor), whereas the unresolved clusters are measured through SBFs. The above treatment is repeated for z=0.05, 0.1, 0.14, and 0.18, and the results are compared to the measurements at z=0 to estimate biases and incompleteness.

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