RT Journal Article
T1 Spatial analysis of the Hα emission in the local star-forming UCM galaxies
A1 Pérez González, Pablo Guillermo
A1 Zamorano Calvo, Jaime
A1 Gallego Maestro, Jesús
A1 Aragón Salamanca, A.
A1 Gil de Paz, Armando
AB We present a photometric study of the Halpha emission in the Universidad Complutense de Madrid (UCM) Survey galaxies. This work complements our previously published spectroscopic data. We study the location of the star-forming knots, their intensity and concentration, and the relationship of these properties with those of the host galaxy. We also estimate that the amount of Halpha emission that arises from the diffuse ionized gas is about 15% - 30% of the total Hα flux for a typical UCM galaxy. This percentage seems to be independent of the Hubble type. Conversely, we find that an "average'' UCM galaxy harbors a star formation event with 30% of its Hα luminosity arising from a nuclear component. The implications of these results for higher redshift studies are discussed, including the effects of galaxy size and the depth of the observations. A correlation between the star formation rate and the Balmer decrement is observed, but such correlation breaks down for large values of the extinction. Finally, we recalculate the Hα luminosity function and star formation rate density of the local universe using the new imaging data. Our results point out that, on average, spectroscopic observations detected about one-third of the total emission-line flux of a typical UCM galaxy. The new values obtained for the Halpha luminosity density and the star formation rate density of the local universe are 10^39.3±0.2 ergs s^-1 Mpc^-3 and ρ(SFR) = 0.016_-0.004^+0.007) M_⨀ yr-1 Mpc^-3 (H_0 = 50 km s^-1) Mpc^-1, Ω_M) = 1.0, Λ = 0). The corresponding values for the "concordance cosmology (H_0 = 70 km s^-1 Mpc^-1, Ω_M) = 0.3, Λ = 0.7) are 10^39.5±0.2 ergs s^-1 Mpc-3) and ρ_SFR = 0.029_-0.005^+0.008 M_⨀ yr^-1 Mpc^-3.
PB American Astronomical Society
SN 0004-637X
YR 2003
FD 2003-07-10
LK https://hdl.handle.net/20.500.14352/51637
UL https://hdl.handle.net/20.500.14352/51637
LA eng
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NO © 2003. The American Astronomical Society. P. G. P.-G. wishes to acknowledge the Spanish Ministry of Education and Culture for a Formación de Profesorado Universitario fellowship. A. A.-S. acknowledges generous financial support from the Royal Society. A. G. d. P. acknowledges financial support from NASA through a Long Term Space Astrophysics grant to B. F. Madore. Valuable discussion with Almudena Zurita is acknowledged. We are grateful to the anonymous referee for her/his helpful comments and suggestions. The present work was supported by the Spanish Programa Nacional de Astronomía y Astrofísica under grant AYA 2000-1790.
NO Ministerio de Educación, Cultura y Deporte (MECD), España
NO Royal Society, Reino Unido
NO National Aeronautics and Space Administration (NASA)
NO Plan Nacional de Astronomía y Astrofísica (MICINN), España
DS Docta Complutense
RD 15 may 2024