2013A&A...553L...7I
Aperture corrections for disk galaxy properties derived from the CALIFA survey. Balmer emission lines in spiral galaxies
Iglesias-Páramo, J. ( Instituto de Astrofísica de Andalucía - CSIC, 18008, Granada, Spain ; Centro Astronómico Hispano Alemán, 04004, Almería, Spain ); Vílchez, J. M. ( Instituto de Astrofísica de Andalucía - CSIC, 18008, Granada, Spain ); Galbany, L. ( CENTRA Centro Multidisciplinar de Astrofísica, Instituto Superior Técnico, Av. Rovisco Pais 1, 1049-001, Lisbon, Portugal ); Sánchez, S. F. ( Instituto de Astrofísica de Andalucía - CSIC, 18008, Granada, Spain; Centro Astronómico Hispano Alemán, 04004, Almería, Spain ); Rosales-Ortega, F. F. ( Instituto Nacional de Astrofísica, Óptica y Electrónica, Luis E. Erro 1, 72840, Tonantzintla, Puebla, Mexico ); Mast, D. ( Centro Astronómico Hispano Alemán, 04004, Almería, Spain ); García-Benito, R. ( Instituto de Astrofísica de Andalucía - CSIC, 18008, Granada, Spain ); Husemann, B. ( Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482, Potsdam, Germany ); Aguerri, J. A. L. ( Instituto de Astrofísica de Canarias, vía Láctea s/n, La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain ); Alves, J. ( University of Vienna, Department of Astrophysics, Türkenschanzstr. 17, 1180, Vienna, Austria ); Bekeraité, S. ( Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482, Potsdam, Germany ); Bland-Hawthorn, J. ( Sydney Institute for Astronomy, School of Physics A28, University of Sydney, NSW, 2006, Australia ); Catalán-Torrecilla, C. ( Departamento de Astrofísica y CC. de la Atmósfera, Universidad Complutense de Madrid, 28040, Madrid, Spain ); de Amorim, A. L. ( Instituto de Astrofísica de Andalucía - CSIC, 18008, Granada, Spain; Departamento de Física, Universidade Federal de Santa Catarina, PO Box 476, 88040-900, Florianpolis, SC, Brazil ); de Lorenzo-Cáceres, A. ( Instituto de Astrofísica de Canarias, vía Láctea s/n, La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain ); Ellis, S. ( Australian Astronomical Observatory, 105 Delhi Rd., North Ryde, NSW, 1670, Australia ); Falcón-Barroso, J. ( Instituto de Astrofísica de Canarias, vía Láctea s/n, La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain ); Flores, H. ( GEPI, Observatoire de Paris, CNRS-UMR8111, Univ. Paris-Diderot, 5 place Janssen, 92195, Meudon, France ); Florido, E. ( Departamento de Física Teórica y del Cosmos, University of Granada, Facultad de Ciencias (Edificio Mecenas), 18071, Granada, Spain; Instituto Carlos I de Física Teórica y Computación, 18071, Granada, Spain ); Gallazzi, A. ( Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Mariesvej 30, 2100, Copenhagen, Denmark; INAF-Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, 50125, Firenze, Italy ); Gomes, J. M. ( Centro de Astrofísica and Faculdade de Ciências, Universidade do Porto, Rua das Estrelas, 4150-762, Porto, Portugal ); González Delgado, R. M. ( Instituto de Astrofísica de Andalucía - CSIC, 18008, Granada, Spain ); Haines, T. ( Department of Physics and Astronomy, University of Missouri Kansas City, Kansas City, MO, 64110, USA ); Hernández-Fernández, J. D. ( Departamento de Astronomia do Instituto de Astronomia, Geofísica e Ciências Atmosféricas da USP, Rua do Matão 1226, Cidade Universitária, 05508-090, São Paulo, Brasil ); Kehrig, C. ( Instituto de Astrofísica de Andalucía - CSIC, 18008, Granada, Spain ); López-Sánchez, A. R. ( Australian Astronomical Observatory, 105 Delhi Rd., North Ryde, NSW, 1670, Australia; Department of Physics and Astronomy, Macquarie University, NSW, 2109, Australia ); Lyubenova, M. ( Max-Planck-Institut für Astronomie, Königstuhl 17, 69117, Heidelberg, Germany ); Marino, R. A. ( CEI Campus Moncloa, UCM-UPM, Departamento de Astrofísica y CC. de la Atmósfera, Facultad de CC. Físicas, Universidad Complutense de Madrid, Avda. Complutense s/n, 28040, Madrid, Spain ); Mollá, M. ( Departamento de Investigación Básica, CIEMAT, Avda. Complutense 22, 28040, Madrid, Spain ); Monreal-Ibero, A. ( Instituto de Astrofísica de Andalucía - CSIC, 18008, Granada, Spain ); Mourão, A. ( CENTRA Centro Multidisciplinar de Astrofísica, Instituto Superior Técnico, Av. Rovisco Pais 1, 1049-001, Lisbon, Portugal ); Papaderos, P. ( Centro de Astrofísica and Faculdade de Ciências, Universidade do Porto, Rua das Estrelas, 4150-762, Porto, Portugal ); Rodrigues, M. ( European Southern Observatory, Alonso de Cordova 3107, Casilla 19001, Vitacura, Santiago, Chile ); Sánchez-Blázquez, P. ( Departamento de Física Teórica, Universidad Autónoma de Madrid, 28049, Madrid, Spain ); Spekkens, K. ( Department ofPhysics, Royal Military College of Canada, PO Box 17000, Station Forces, Kingston, Ontario, K7K 7B4, Canada ); Stanishev, V. ( CENTRA Centro Multidisciplinar de Astrofísica, Instituto Superior Técnico, Av. Rovisco Pais 1, 1049-001, Lisbon, Portugal ); van de Ven, G. ( Max-Planck-Institut für Astronomie, Königstuhl 17, 69117, Heidelberg, Germany ); Walcher, C. J. ( Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482, Potsdam, Germany ); Wisotzki, L. ( Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482, Potsdam, Germany ); Zibetti, S. ( INAF-Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, 50125, Firenze, Italy ); Ziegler, B. ( University of Vienna, Department of Astrophysics, Türkenschanzstr. 17, 1180, Vienna, Austria ) and 31 coauthors show affiliations
Astronomy & Astrophysics, Volume 553, id.L7, 5 pp.
Published in May 2013
This work investigates the effect of the aperture size on derived galaxy properties for which we have spatially-resolved optical spectra. We focus on some indicators of star formation activity and dust attenuation for spiral galaxies that have been widely used in previous work on galaxy evolution. We investigated 104 spiral galaxies from the CALIFA survey for which 2D spectroscopy with complete spatial coverage is available. From the 3D cubes we derived growth curves of the most conspicuous Balmer emission lines (Hα, Hβ) for circular apertures of different radii centered at the galaxy's nucleus after removing the underlying stellar continuum. We find that the Hα flux (f(Hα)) growth curve follows a well-defined sequence with aperture radius that shows a low dispersion around the median value. From this analysis, we derived aperture corrections for galaxies in different magnitude and redshift intervals. Once stellar absorption is properly accounted for, the f(Hα)/f(Hβ) ratio growth curve shows a smooth decline, pointing toward the absence of differential dust attenuation as a function of radius. Aperture corrections as a function of the radius are provided in the interval [0.3, 2.5]R50. Finally, the Hα equivalent-width (EW(Hα)) growth curve increases with the size of the aperture and shows a very high dispersion for small apertures. This prevents us from using reliable aperture corrections for this quantity. In addition, this result suggests that separating star-forming and quiescent galaxies based on observed EW(Hα) through small apertures will probably result in low EW(Hα) star-forming galaxies begin classified as quiescent.
Keywords:
Free Keywords: Astrophysics - Cosmology and Extragalactic Astrophysics; galaxies: ISM; galaxies: evolution; surveys; techniques: spectroscopic
Astronomy: galaxies: ISM; galaxies: evolution; surveys; techniques: spectroscopic
arXiv: Astrophysics - Cosmology and Extragalactic Astrophysics
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