Produção Nacional
Revisado por pares
The miniJPAS and J-NEP surveys: Identification and characterization of the Lyα emitter population and the Lyalpha luminosity function at redshift 2.05 < z < 3.75
2023; EDP Sciences; Volume: 680; Linguagem: Inglês
10.1051/0004-6361/202347463
ISSN1432-0746
AutoresAlberto Torralba-Torregrosa, Siddhartha Gurung-López, P. Arnalte-Mur, D. Spinoso, David Izquierdo–Villalba, A. Fernández-Soto, Raúl E. Angulo, Silvia Bonoli, R. M. González Delgado, I. Márquez, Vicent J. Martı́nez, P. T. Rahna, J. M. Vı́lchez, L. Raul Abramo, J. S. Alcaniz, N. Benı́tez, S. Carneiro, J. Cenarro, D. Cristóbal-Hornillos, Renato A. Dupke, A. Ederoclite, A. Hernán-Caballero, C. López-Sanjuán, A. Marín-Franch, C. Mendes de Oliveira, M. Moles, L. Sodré, K. Taylor, J. Varela, H. Vázquez Ramió,
Tópico(s)Galaxies: Formation, Evolution, Phenomena
ResumoWe present the Lyman- α (Ly α ) luminosity function (LF) at 2.05 < z < 3.75, estimated from a sample of 67 Ly α -emitter (LAE) candidates in the Javalambre Physics of the Accelerating Universe Astronomical Survey (J-PAS) pathfinder surveys: miniJPAS and J-NEP. These two surveys cover a total effective area of ∼1.14 deg 2 with 54 narrow band (NB) filters ( FWHM ∼ 145 Å) across the optical range, with typical limiting magnitudes of ∼23. This set of NBs allowed us to probe Ly α emission in a wide and continuous range of redshifts. We developed a method for detecting Ly α emission for the estimation of the Ly α LF using the whole J-PAS filter set. We tested this method by applying it to the miniJPAS and J-NEP data. In order to compute the corrections needed to estimate the Ly α LF and to test the performance of the candidate selection method, we built mock catalogs. These include representative populations of LAEs at 1.9 < z < 4.5 as well as their expected contaminants, namely low- z galaxies and z < 2 quasi-stellar objects (QSOs). We show that our method is able to provide the Ly α LF at the intermediate-bright range of luminosity (43.5 ≲ log 10 ( L Ly α /erg s −1 ) ≲ 44.5) combining both miniJPAS and J-NEP. The photometric information provided by these surveys suggests that our samples are dominated by bright, Ly α -emitting active galactic nuclei (i.e., AGNs). At log 10 ( L Ly α /erg s −1 ) < 44.5, we fit our Ly α LF to a power law with a slope of A = 0.70 ± 0.25. We also fit a Schechter function to our data, obtaining the following: log 10 (Φ ∗ /Mpc −3 ) = −6.30 −0.70 +0.48 , log 10 ( L ∗ /erg s −1 ) = 44.85 −0.32 +0.50 , and α = −1.65 −0.27 +0.29 . Overall, our results confirm the presence of an AGN component at the bright end of the Ly α LF. In particular, we find no significant contribution of star-forming LAEs to the Ly α LF at log 10 ( L Ly α /erg s −1 ) > 43.5. This work serves as a proof of concept for the results that can be obtained with the upcoming data releases of the J-PAS survey.
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