Detalles de publicación
PP 021017
The OTELO survey: Faint end of the luminosity function of [OII], emitters at
The OTELO survey: Faint end of the luminosity function of [OII], emitters at =1.43
(1) Instituto de Astrofísica de Canarias (IAC), (2) Departamento de Astrofísica, Universidad de La Laguna (ULL), (3) Instituto de Radioastonomía Milimétrica (IRAM), (4) Asociación Astrofísica para la Promoción de la Investigación, Instrumentación y su Desarrollo, ASPID, (5) Centro de Astrobiología (CSIC/INTA), (6) Instituto de Astronomía, Universidad Nacional Autónoma de México, (7) Departamento de Física de la Tierra y Astrofísica, Instituto de Física de Partículas y del Cosmos, IPARCOS. Universidad Complutense de Madrid, (8) DARK, Niels Bohr Institute, University of Copenhagen, (9) Instituto de Física de Cantabria (CSIC-Universidad de Cantabria), (10) Instituto de Astrofísica de Andalucía, (11) ISDEFE for European Space Astronomy Centre (ESAC)/ESA, (12) Instituto de Astronomía, Universidad Nacional Autónoma de México, (13) Fundación Galileo Galilei, Telescopio Nazionale Galileo, (14) Departamento de Física, Escuela Superior de Física y Matemáticas, Instituto Politécnico Nacional
In this paper, we aim to study the main properties and luminosity function (LF) of the [OII], emitters detected in the OTELO survey in order to characterise the star formation processes in low-mass galaxies at $z\sim1.43$ and to constrain the faint-end of the LF.
Here, we describe the selection method and analysis of the emitters obtained from narrow-band scanning techniques. In addition, we present several relevant properties of the emitters and discuss the selection biases and uncertainties in the determination of the LF and the star formation rate density (SFRD).
We confirmed a total of 60 sources from a preliminary list of 332 candidates as [OII], emitters. Approximately 93% of the emitters have masses in the range of $10^{8}<M_{*}/{\rm M_{\odot}}<10^{9}$. All of our emitters are classified as late-type galaxies, with a lower value of $(u-v)$\, when compared with the rest of the emitters of the OTELO survey. We find that the cosmic variance strongly affects the normalisation ($\phi^*$) of the LF and explains the discrepancy of our results when compared with those obtained from surveys of much larger volumes. However, we are able to determine the faint-end slope of the LF, namely, $\alpha=-1.42\pm0.06$, by sampling the LF down to $\sim1$\,dex lower than in previous works. We present our calculation of the SFRD of our sample and compare it to the value obtained in previous studies from the literature.
Here, we describe the selection method and analysis of the emitters obtained from narrow-band scanning techniques. In addition, we present several relevant properties of the emitters and discuss the selection biases and uncertainties in the determination of the LF and the star formation rate density (SFRD).
We confirmed a total of 60 sources from a preliminary list of 332 candidates as [OII], emitters. Approximately 93% of the emitters have masses in the range of $10^{8}<M_{*}/{\rm M_{\odot}}<10^{9}$. All of our emitters are classified as late-type galaxies, with a lower value of $(u-v)$\, when compared with the rest of the emitters of the OTELO survey. We find that the cosmic variance strongly affects the normalisation ($\phi^*$) of the LF and explains the discrepancy of our results when compared with those obtained from surveys of much larger volumes. However, we are able to determine the faint-end slope of the LF, namely, $\alpha=-1.42\pm0.06$, by sampling the LF down to $\sim1$\,dex lower than in previous works. We present our calculation of the SFRD of our sample and compare it to the value obtained in previous studies from the literature.