2024-03-28T13:27:26Zhttp://digital.csic.es/dspace-oai/requestoai:digital.csic.es:10261/1341042021-10-28T15:40:39Zcom_10261_97com_10261_4com_10261_45com_10261_37col_10261_350col_10261_298col_10261_290
The impact from survey depth and resolution on the morphological classification of galaxies
Pović, Mirjana
Márquez, Isabel
Masegosa, Josefa
Perea, Jaime
Olmo, Ascensión del
Aguerri, J.A.L.
Ascaso, Begoña
Jiménez-Teja, Y.
López-Sanjuan, C.
Molino, Alberto
Pérez-García, Ana M.
Viironen, Kerttu
Husillos, César
Cristóbal-Hornillos, David
Benítez, Narciso
Alfaro, Emilio J.
Aparicio Villegas, Teresa
Broadhurst, T.
Cabrera-Caño, Jesús
Castander, Francisco J.
Cepa, Jordi
Cerviño, Miguel
Fernández-Soto, Alberto
González Delgado, Rosa M.
Infante, Leopoldo
Martínez, Vicente J.
Moles, Mariano
Prada, Francisco
Quintana, José María
Consejo Superior de Investigaciones Científicas (España)
European Commission
Junta de Andalucía
Ministerio de Economía y Competitividad (España)
Galaxies: fundamental parameters
Surveys
We consistently analyse for the first time the impact of survey depth and spatial resolution on the most used morphological parameters for classifying galaxies through non-parametric methods: Abraham and Conselice-Bershady concentration indices, Gini, M20moment of light, asymmetry, and smoothness. Three different non-local data sets are used, Advanced Large Homogeneous Area Medium Band Redshift Astronomical (ALHAMBRA) and Subaru/XMMNewton Deep Survey (SXDS, examples of deep ground-based surveys), and Cosmos Evolution Survey (COSMOS, deep space-based survey). We used a sample of 3000 local, visually classified galaxies, measuring their morphological parameters at their real redshifts (z ~ 0). Then we simulated them to match the redshift and magnitude distributions of galaxies in the non-local surveys. The comparisons of the two sets allow us to put constraints on the use of each parameter for morphological classification and evaluate the effectiveness of the commonly used morphological diagnostic diagrams. All analysed parameters suffer from biases related to spatial resolution and depth, the impact of the former being much stronger. When including asymmetry and smoothness in classification diagrams, the noise effects must be taken into account carefully, especially for ground-based surveys. M20 is significantly affected, changing both the shape and range of its distribution at all brightness levels. We suggest that diagnostic diagrams based on 2-3 parameters should be avoided when classifying galaxies in ground-based surveys, independently of their brightness; for COSMOS they should be avoided for galaxies fainter than F814 = 23.0. These results can be applied directly to surveys similar to ALHAMBRA, SXDS and COSMOS, and also can serve as an upper/lower limit for shallower/deeper ones.
MP acknowledge financial support from JAE-Doc programme of the Spanish National Research Council (CSIC), co-funded by the European Social Fund. This research was supported by the Junta de Andalucia through project TIC114, and the Spanish Ministry of Economy and Competitiveness (MINECO) through projects AYA2010-15169, AYA2013-42227-P, and AYA2013-43188-P.
Peer Reviewed
2016-06-27T11:32:02Z
2016-06-27T11:32:02Z
2015
2016-06-27T11:32:05Z
artículo
http://purl.org/coar/resource_type/c_6501
doi: 10.1093/mnras/stv1663
issn: 1365-2966
Monthly Notices of the Royal Astronomical Society 453: 1644-1668 (2015)
http://hdl.handle.net/10261/134104
10.1093/mnras/stv1663
http://dx.doi.org/10.13039/501100003339
http://dx.doi.org/10.13039/501100000780
http://dx.doi.org/10.13039/501100003329
http://dx.doi.org/10.13039/501100011011
#PLACEHOLDER_PARENT_METADATA_VALUE#
#PLACEHOLDER_PARENT_METADATA_VALUE#
info:eu-repo/grantAgreement/MINECO/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/AYA2013-42227-P
info:eu-repo/grantAgreement/MINECO/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/AYA2013-43188-P
Publisher's version
https://doi.org/10.1093/mnras/stv1663
Sí
open
Oxford University Press