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Título:
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H? emitting galaxies and the star formation rate density at z ? 0.24
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Autores:
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Pascual, S. ;
Gallego Maestro, Jesús ;
Aragón Salamanca, A. ;
Zamorano Calvo, Jaime
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Tipo de documento:
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texto impreso
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Editorial:
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EDP Sciencies, 2001-12
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Dimensiones:
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application/pdf
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Nota general:
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info:eu-repo/semantics/openAccess
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Idiomas:
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Palabras clave:
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Estado = Publicado
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Materia = Ciencias: Física: Astrofísica
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Materia = Ciencias: Física: Astronomía
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Tipo = Artículo
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Resumen:
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We have carried out a survey searching for H? emitting galaxies at z ? 0.24 using a narrow band filter tuned with the redshifted line. The total sky area covered was 0.19 square degrees within the redshift range 0.228 to 0.255 in a set of four fields in the ELAIS-N1 zone. This corresponds to a volume of 9.8 x 10^3 Mpc^3 and a look-back time of 3.6 Gyr when H_0 = 50 km s^-1 Mpc^-1 and q_0 = 0.5 are assumed. A total of 52 objects are selected as candidates for a broad band limiting magnitude of I ~ 22.9, plus 16 detected only in the narrow band image for a narrow band limiting magnitude for object detection of 21.0. The threshold detection corresponds to about 20 Å equivalent width with an uncertainty of ~± 10 Å. Point-like objects (15) were excluded from our analysis using CLASS STAR parameter from SExtractor. The contamination from other emission lines such as [O II] ? 3727, H _ ? and [O III] ? ? 4959, 5007 at redshifts 1.2, 0.66 and 0.61 respectively is estimated, and found to be negligible at the flux limits of our sample. We find an extinction-corrected H_ ? luminosity density of (5.4 ± 1.1) x 10^39 erg s^-1 Mpc^-3. This uncertainty takes into account the photometric and Poissonian errors only. Assuming a constant relation between the H_? luminosity and star formation rate, the SFR density in the covered volume is (0.043 ± 0.009) M_? yr^-1 Mpc^-3. This translates to (0.037 ± 0.009) M¬_? yr^-1 Mpc^-3 when the total density is corrected for the AGN contribution as estimated in the local Universe. This value is a factor ~4 higher than the local SFR density. This result needs to be confirmed by future spectroscopic follow-up observations.
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En línea:
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https://eprints.ucm.es/34317/1/jesusgallego88libre.pdf
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