The OTELO survey Nature and mass-metallicity relation for H alpha emitters at z similar to 0.4
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The OTELO survey Nature and mass-metallicity relation for H alpha emitters at z similar to 0.4. / Nadolny, Jakub; Lara-Lopez, Maritza A.; Cervino, Miguel; Bongiovanni, Angel; Cepa, Jordi; de Diego, Jose A.; Perez Garcia, Ana Maria; Perez Martinez, Ricardo; Sanchez-Portal, Miguel; Alfaro, Emilio; Castaneda, Hector O.; Gallego, Jesus; Jesus Gonzalez, J.; Ignacio Gonzalez-Serrano, J.; Padilla Torres, Carmen P.; Pintos-Castro, Irene; Povic, Mirjana.
In: Astronomy & Astrophysics, Vol. 636, A84, 24.04.2020.Research output: Contribution to journal › Journal article › Research › peer-review
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TY - JOUR
T1 - The OTELO survey Nature and mass-metallicity relation for H alpha emitters at z similar to 0.4
AU - Nadolny, Jakub
AU - Lara-Lopez, Maritza A.
AU - Cervino, Miguel
AU - Bongiovanni, Angel
AU - Cepa, Jordi
AU - de Diego, Jose A.
AU - Perez Garcia, Ana Maria
AU - Perez Martinez, Ricardo
AU - Sanchez-Portal, Miguel
AU - Alfaro, Emilio
AU - Castaneda, Hector O.
AU - Gallego, Jesus
AU - Jesus Gonzalez, J.
AU - Ignacio Gonzalez-Serrano, J.
AU - Padilla Torres, Carmen P.
AU - Pintos-Castro, Irene
AU - Povic, Mirjana
PY - 2020/4/24
Y1 - 2020/4/24
N2 - Context. The OSIRIS Tunable Filter Emission Line Object (OTELO) survey is a very deep, blind exploration of a selected region of the Extended Groth Strip and is designed for finding emission-line sources (ELSs). The survey design, observations, data reduction, astrometry, and photometry, as well as the correlation with ancillary data used to obtain a final catalogue, including photo-z estimates and a preliminary selection of ELS, were described in a previous contribution.Aims. Here, we aim to determine the main properties and luminosity function (LF) of the [O III] ELS sample of OTELO as a scientific demonstration of its capabilities, advantages, and complementarity with respect to other surveys.Methods. The selection and analysis procedures of ELS candidates obtained using tunable filter pseudo-spectra are described. We performed simulations in the parameter space of the survey to obtain emission-line detection probabilities. Relevant characteristics of [O III] emitters and the LF ([O III]), including the main selection biases and uncertainties, are presented.Results. From 541 preliminary emission-line source candidates selected around z & x2004;=& x2004;0.8, a total of 184 sources were confirmed as [O III] emitters. Consistent with simulations, the minimum detectable line flux and equivalent width in this ELS sample are similar to 5 x 10(-19) erg s(-1) cm(2) and similar to 6 angstrom, respectively. We are able to constrain the faint-end slope (alpha & x2004;=& x2004;-1.03 +/- 0.08) of the observed LF ([O III]) at a mean redshift of z & x2004;=& x2004;0.83. This LF reaches values that are approximately ten times lower than those from other surveys. The vast majority (84%) of the morphologically classified [O III] ELSs are disc-like sources, and 87% of this sample is comprised of galaxies with stellar masses of M-& x22c6;& x2004;<& x2004;10(10) M-circle dot.
AB - Context. The OSIRIS Tunable Filter Emission Line Object (OTELO) survey is a very deep, blind exploration of a selected region of the Extended Groth Strip and is designed for finding emission-line sources (ELSs). The survey design, observations, data reduction, astrometry, and photometry, as well as the correlation with ancillary data used to obtain a final catalogue, including photo-z estimates and a preliminary selection of ELS, were described in a previous contribution.Aims. Here, we aim to determine the main properties and luminosity function (LF) of the [O III] ELS sample of OTELO as a scientific demonstration of its capabilities, advantages, and complementarity with respect to other surveys.Methods. The selection and analysis procedures of ELS candidates obtained using tunable filter pseudo-spectra are described. We performed simulations in the parameter space of the survey to obtain emission-line detection probabilities. Relevant characteristics of [O III] emitters and the LF ([O III]), including the main selection biases and uncertainties, are presented.Results. From 541 preliminary emission-line source candidates selected around z & x2004;=& x2004;0.8, a total of 184 sources were confirmed as [O III] emitters. Consistent with simulations, the minimum detectable line flux and equivalent width in this ELS sample are similar to 5 x 10(-19) erg s(-1) cm(2) and similar to 6 angstrom, respectively. We are able to constrain the faint-end slope (alpha & x2004;=& x2004;-1.03 +/- 0.08) of the observed LF ([O III]) at a mean redshift of z & x2004;=& x2004;0.83. This LF reaches values that are approximately ten times lower than those from other surveys. The vast majority (84%) of the morphologically classified [O III] ELSs are disc-like sources, and 87% of this sample is comprised of galaxies with stellar masses of M-& x22c6;& x2004;<& x2004;10(10) M-circle dot.
KW - techniques
KW - imaging spectroscopy
KW - surveys
KW - catalogs
KW - galaxies
KW - starburst
KW - active
KW - luminosity function
KW - mass function
KW - STAR-FORMING GALAXIES
KW - ASSEMBLY GAMA
KW - PHOTOMETRIC REDSHIFTS
KW - LINE GALAXIES
KW - DATA RELEASE
KW - DEEP-FIELD
KW - EVOLUTION
KW - EMISSION
KW - DECOMPOSITION
KW - POPULATION
U2 - 10.1051/0004-6361/201936205
DO - 10.1051/0004-6361/201936205
M3 - Journal article
VL - 636
JO - Astronomy & Astrophysics
JF - Astronomy & Astrophysics
SN - 0004-6361
M1 - A84
ER -
ID: 247160832