The miniJPAS survey: Photometric redshift catalogue

Hernán-Caballero, A.; Varela, J.; López-Sanjuán, C.; Muniesa, D.; Civera, T.; Chaves-Montero, Jonás; Díaz-García, L. A.; Laur, J.; Hernández-Monteagudo, C.; Abramo, R.; Angulo, Raúl E.; Cristóbal-Hornillos, D.; Delgado, R. M. González; Greisel, N.; Orsi, Álvaro; Queiroz, Carolina; Sobral, David; Tamm, A.; Tempel, Elmo; Vázquez-Ramió, H.; Alcaniz, J. S.; Benı́tez, N.; Bonoli, Silvia; Carneiro, S.; Cenarro, J.; Dupke, Renato A.; Ederoclite, A.; Marín-Franch, A.; Oliveira, C. Mendes de; Moles, M.; Sodré, L.; Taylor, Keith; Cypriano, E. S.; Martínez-Solaeche, Ginés

doi:10.1051/0004-6361/202141236

Cited by 26 publications

(7 citation statements)

References 60 publications

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“…The miniJPAS survey (Bonoli et al 2021) observed four AEGIS (All-wavelength Extended Groth Strip International Survey; Davis et al 2007) fields in 2018-2019 with the pathfinder camera and detected more than 60,000 objects in a total area of 1 deg 2 . The miniJPAS survey demonstrates the capabilities and unique potential of the upcoming J-PAS survey (Hernán-Caballero et al 2021;Martínez-Solaeche et al 2021;Queiroz et al 2022;Martínez-Solaeche et al 2022;Chaves-Montero et al 2022). More detail about the observation and data reduction of mini-JPAS is given in Bonoli et al (2021).…”

Section: J-pas and Mini-jpas Surveysmentioning

confidence: 99%

The miniJPAS Survey: Detection of double-core Lyα morphology of two high-redshift (z>3) QSOs

Rahna¹,

Zheng²,

Chies-Santos³

et al. 2022

Preprint

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The Lyα emission is an important tracer of neutral gas in a circum-galactic medium (CGM) around high redshift QSOs. The origin of Lyα emission around QSOs is still under debate which has significant implications for galaxy formation and evolution. In this paper, we report the detection of double-core morphology in the Lyα images of two high redshift QSOs, SDSS J141935.58+525710.7 at z = 3.128 (hereafter QSO1) and SDSS J141813.40+525240.4 at z = 3.287 (hereafter QSO2), with the contiguous narrow-band (NB) images from the miniJPAS survey in the AEGIS field. The separations of the two Lyα cores are 8.7 kpc (1.15 ) and 9.9 kpc (1.32 ) with Lyα line luminosities of ∼ 3 ×10 44 erg s −1 and ∼ 6 × 10 44 erg s −1 for QSO1 and QSO2, respectively. Both QSOs also show extended morphology in their CIV and HeII (only in QSO1), covering the miniJPAS NB images. The Lyα luminosity-size relation shows that both QSOs are suspected to be Enormous Lyman alpha Nebula (ELAN) due to their high Lyα line luminosity. Current miniJPAS NB emission-line morphology and SDSS spectral line profiles indicate the galactic outflow as the powering mechanism for extended Lyα emission via resonant scattering and/or photoionization and/or shocks. Considering the relative shallow exposures of miniJPAS, the objects found here could be the tip of the iceberg of a promising number of such objects that will be uncovered in the upcoming full J-PAS survey, and deep IFU observations with 8-10m tele-

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Section: J-pas and Mini-jpas Surveysmentioning

confidence: 99%

The miniJPAS Survey: Detection of double-core Lyα morphology of two high-redshift (z>3) QSOs

Rahna¹,

Zheng²,

Chies-Santos³

et al. 2022

Preprint

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“…The photo-z was estimated with the JPHOTOZ package developed by the photo-z team at CEFCA. This package is a customized version of the LePhare code (Arnouts & Ilbert 2011), which has a new set of stellar population synthesis galaxy templates that were optimized for the miniJPAS filter system (Hernán-Caballero et al 2021). At the depth of miniJPAS (5σ limits between ∼ 21.5 and 22.5 mag for the narrowband filters and ∼ 24 mag for the broadband filters in a 3 aperture), there are 17 500 galaxies per deg 2 with valid photo-z estimates (rSDSS < 23), of which ∼ 4 200 have |∆z| < 0.003.…”

Section: Sample and Datamentioning

confidence: 99%

The miniJPAS survey: Identification and characterization of the emission line galaxies down to $z < 0.35$ in the AEGIS field

Martínez-Solaeche,

Delgado,

García-Benito

et al. 2022

Preprint

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The Javalambre-Physics of the Accelerating Universe Astrophysical Survey (J-PAS) is expected to map thousands of square degrees of the northern sky with 56 narrowband filters (spectral resolution of R ∼ 60) in the upcoming years. This resolution allows us to study emission line galaxies (ELGs) with a minimum equivalent width of 10 Å in the Hα emission line for a median signal-to-noise ratio (S/N) of 5. This will make J-PAS a very competitive and unbiased emission line survey compared to spectroscopic or narrowband surveys with fewer filters. The miniJPAS survey covered 1 deg 2 , and it used the same photometric system as J-PAS, but the observations were carried out with the pathfinder J-PAS camera. In this work, we identify and characterize the sample of ELGs from miniJPAS with a redshift lower than 0.35, which is the limit to which the Hα line can be observed with the J-PAS filter system. Using a method based on artificial neural networks, we detect the ELG population and measure the equivalent width and flux of the Hα, Hβ, [O iii], and [N ii] emission lines. We explore the ionization mechanism using the diagrams [OIII]/Hβ versus [NII]/Hα (BPT) and EW(Hα) versus [NII]/Hα (WHAN). We identify 1787 ELGs (83%) from the parent sample (2154 galaxies) in the AEGIS field. For the galaxies with reliable EW values that can be placed in the WHAN diagram (2000 galaxies in total), we obtained that 72.8 ± 0.4 %, 17.7 ± 0.4 % , and 9.4 ± 0.2 % are star-forming (SF), active galactic nucleus (Seyfert), and quiescent galaxies, respectively. The distribution of EW(Hα) is well correlated with the bimodal color distribution of galaxies. Based on the rest-frame (u − r)-stellar mass diagram, 94% of the blue galaxies are SF galaxies, and 97% of the red galaxies are LINERs or passive galaxies. The nebular extinction and star formation rate (SFR) were computed from the Hα and Hβ fluxes. We find that the star formation main sequence is described as log SFR [M yr −1 ] = 0.90 +0.02 −0.02 log M [M ] − 8.85 +0.19 −0.20 and has an intrinsic scatter of 0.20 +0.01 −0.01 . The cosmic evolution of the SFR density (ρ SFR ) is derived at three redshift bins: 0 < z ≤ 0.15, 0.15 < z ≤ 0.25, and 0.25 < z ≤ 0.35, which agrees with previous results that were based on measurements of the Hα emission line. However, we find an offset with respect to other estimates that were based on the star formation history obtained from fitting the spectral energy distribution of the stellar continuum. We discuss the origin of this discrepancy, which is probably a combination of several factors: the escape of ionizing photons, the SFR tracers, and dust attenuation, among others.

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“…We refer to Bonoli et al (2021) for details on the flagging scheme. Removal of flagged sources from the catalogue decreased our sample size, but did not introduce any bias because the fraction of sources that are flagged is independent of their magnitude (Hernán-Caballero et al 2021).…”

Section: Minijpas Survey and Mocksmentioning

confidence: 99%

J-PAS: Measuring emission lines with artificial neural networks

Martínez-Solaeche

Delgado

García-Benito

et al. 2021

A&A

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In the years to come, the Javalambre-Physics of the Accelerated Universe Astrophysical Survey (J-PAS) will observe 8000 deg2 of the northern sky with 56 photometric bands. J-PAS is ideal for the detection of nebular emission objects. This paper presents a new method based on artificial neural networks (ANNs) that is aimed at measuring and detecting emission lines in galaxies up to z = 0.35. These lines are essential diagnostics for understanding the evolution of galaxies through cosmic time. We trained and tested ANNs with synthetic J-PAS photometry from CALIFA, MaNGA, and SDSS spectra. To this aim, we carried out two tasks. First, we clustered galaxies in two groups according to the values of the equivalent width (EW) of Hα, Hβ, [N II], and [O III] lines measured in the spectra. Then we trained an ANN to assign a group to each galaxy. We were able to classify them with the uncertainties typical of the photometric redshift measurable in J-PAS. Second, we utilized another ANN to determine the values of those EWs. Subsequently, we obtained the [N II]/Hα, [O III]/Hβ, and O 3N 2 ratios, recovering the BPT diagram ([O III]/Hβ versus [N II]/Hα). We studied the performance of the ANN in two training samples: one is only composed of synthetic J-PAS photo-spectra (J-spectra) from MaNGA and CALIFA (CALMa set) and the other one is composed of SDSS galaxies. We were able to fully reproduce the main sequence of star-forming galaxies from the determination of the EWs. With the CALMa training set, we reached a precision of 0.092 and 0.078 dex for the [N II]/Hα and [O III]/Hβ ratios in the SDSS testing sample. Nevertheless, we find an underestimation of those ratios at high values in galaxies hosting an active galactic nuclei. We also show the importance of the dataset used for both training and testing the model. Such ANNs are extremely useful for overcoming the limitations previously expected concerning the detection and measurements of the emission lines in such surveys as J-PAS. Furthermore, we show the capability of the method to measure a EW of 10 Å in Hα, Hβ, [N II] and [O III] lines with a signal-to-noise ratio (S/N) of 5, 1.5, 3.5, and 10, respectively, in the photometry. Finally, we compare the properties of emission lines in galaxies observed with miniJPAS and SDSS. Despite the limitation of such a comparison, we find a remarkable correlation in their EWs.

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The miniJPAS survey: Photometric redshift catalogue

Cited by 26 publications

References 60 publications

The miniJPAS Survey: Detection of double-core Lyα morphology of two high-redshift (z>3) QSOs

The miniJPAS Survey: Detection of double-core Lyα morphology of two high-redshift (z>3) QSOs

The miniJPAS survey: Identification and characterization of the emission line galaxies down to $z < 0.35$ in the AEGIS field

J-PAS: Measuring emission lines with artificial neural networks

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