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ALHAMBRA survey: morphological classification

Published online by Cambridge University Press:  05 March 2015

M. Pović
Affiliation:
Instituto de Astrofísica de Andalucía (IAA-CSIC), Granada, Spain email: mpovic@iaa.es
M. Huertas-Company
Affiliation:
GEPI, Paris Observatory, Paris, France
I. Márquez
Affiliation:
Instituto de Astrofísica de Andalucía (IAA-CSIC), Granada, Spain email: mpovic@iaa.es
J. Masegosa
Affiliation:
Instituto de Astrofísica de Andalucía (IAA-CSIC), Granada, Spain email: mpovic@iaa.es
J. A. López Aguerri
Affiliation:
Instituto de Astrofísica de Canarias (IAC), La Laguna, Tenerife, Spain
C. Husillos
Affiliation:
Instituto de Astrofísica de Andalucía (IAA-CSIC), Granada, Spain email: mpovic@iaa.es
A. Molino
Affiliation:
Instituto de Astrofísica de Andalucía (IAA-CSIC), Granada, Spain email: mpovic@iaa.es
D. Cristóbal-Hornillos
Affiliation:
Centro de Estudios de Física del Cosmos de Aragón (CEFCA), Teruel, Spain
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Abstract

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The Advanced Large Homogeneous Area Medium Band Redshift Astronomical (ALHAMBRA) survey is a photometric survey designed to study systematically cosmic evolution and cosmic variance (Moles et al.2008). It employs 20 continuous medium-band filters (3500 - 9700 Å), plus JHK near-infrared (NIR) bands, which enable measurements of photometric redshifts with good accuracy. ALHAMBRA covers > 4 deg2 in eight discontinuous regions (~ 0.5 deg2 per region), of theseseven fields overlap with other extragalactic, multiwavelength surveys (DEEP2, SDSS, COSMOS, HDF-N, Groth, ELAIS-N1). We detect > 600.000 sources, reaching the depth of R(AB) ~ 25.0, and photometric accuracy of 2-4% (Husillos et al., in prep.). Photometric redshifts are measured using the Bayesian Photometric Redshift (BPZ) code (Benítez et al.2000), reaching one of the best accuracies up to date of δz/z ≤ 1.2% (Molino et al., in prep.).

To deal with the morphological classification of galaxies in the ALHAMBRA survey (Pović et al., in prep.), we used the galaxy Support Vector Machine code (galSVM; Huertas-Company 2008, 2009), one of the new non-parametric methods for morphological classification, specially useful when dealing with low resolution and high-redshift data. To test the accuracy of our morphological classification we used a sample of 3000 local, visually classified galaxies (Nair & Abraham 2010), moving them to conditions typical of our ALHAMBRA data (taking into account the background, redshift and magnitude distributions, etc.), and measuring their morphology using galSVM. Finally, we measured the morphology of ALHAMBRA galaxies, obtaining for each source seven morphological parameters (two concentration indexes, asymmetry, Gini, M20 moment of light, smoothness, and elongation), probability if the source belongs to early- or late-type, and its error. Comparing ALHAMBRA morph COSMOS/ACS morphology (obtained with the same method) we expect to have qualitative separation in two main morphological types for ~ 20.000 sources in 8 ALHAMBRA fields. For early-type galaxies we expect to recover ~ 70% and 30-40% up to magnitudes 20.0 and 21.5, respectively, having the contamination of late-types of < 7%. For late-type galaxies, we expect to recover ~ 70%, 60 - 70%, and ~ 30% of sources up to magnitudes 22.0, 22.5, and 23.0, respectively, having the contamination of early-types of ≤ 10%. These data will be used to study the evolution of active and non-active galaxies respect to morphology and morphological properties of galaxies in groups and clusters.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2015 

References

Benítez, N., et al. 2000, ApJ, 536, 571Google Scholar
Huertas-Company, M., et al. 2008, A&A, 478, 971Google Scholar
Moles, M., et al. 2008, AJ, 136, 1325CrossRefGoogle Scholar
Nair, P. & Abraham, R., 2010, ApJS, 186, 427Google Scholar