Star formation rates and stellar masses of Hα selected star-forming galaxies at z=0.84: a quantification of the downsizing
In this work we analyze the physical properties of a sample of 153 star-forming galaxies at z ~ 0.84, selected by their Hα flux with a narrowband filter. B-band luminosities of the objects are higher than those of local star-forming galaxies. Most of the galaxies are located in the blue cloud, thoug...
| Autores: | , , , , , , |
|---|---|
| Tipo de recurso: | artículo |
| Fecha de publicación: | 2011 |
| País: | España |
| Institución: | Universidad Complutense de Madrid (UCM) |
| Repositorio: | Docta Complutense |
| Idioma: | inglés |
| OAI Identifier: | oai:docta.ucm.es:20.500.14352/44774 |
| Acceso en línea: | https://hdl.handle.net/20.500.14352/44774 |
| Access Level: | acceso abierto |
| Palabra clave: | 52 Ultraviolet luminosity density Emission-line galaxies Extended groth strip Color-magnitude diagram France redshift survey Aegis field galaxies Lyman-break galaxies Power-law galaxies Hubble-deep-field To-fir analysis Astrofísica Astronomía (Física) |
| Sumario: | In this work we analyze the physical properties of a sample of 153 star-forming galaxies at z ~ 0.84, selected by their Hα flux with a narrowband filter. B-band luminosities of the objects are higher than those of local star-forming galaxies. Most of the galaxies are located in the blue cloud, though some objects are detected in the green valley and in the red sequence. After the extinction correction is applied, virtually all these red galaxies move to the blue sequence, unveiling their dusty nature. A check on the extinction law reveals that the typical extinction law for local starbursts is well suited for our sample but with E(B - V)_stars = 0.55 E(B - V)_gas. We compare star formation rates (SFRs) measured with different tracers (Hα, far-ultraviolet, and infrared), finding that they agree within a factor of three after extinction correction. We find a correlation between the ratios SFR_FUV/SFR_Hα, SFR_IR/SFR_Hα, and the EW(Hα) (i.e., weighted age), which accounts for part of the scatter. We obtain stellar mass estimations by fitting templates to multi-wavelength photometry. The typical stellar mass of a galaxy within our sample is ∼10^10 M_⨀. The SFR is correlated with stellar mass and the specific SFR decreases with it, indicating that massive galaxies are less affected by star formation processes than less massive ones. This result is consistent with the downsizing scenario. To quantify this downsizing we estimated the quenching mass M-Q for our sample at z ~ 0.84, finding that it declines from M_Q ~ 10^12 M_⨀t at z ~ 0.84 to M_Q ~ 8 x 10^10 M_⨀ at the local universe. |
|---|