The OTELO survey

Cedrés, B.; Bongiovanni, Á.; Cerviño, M.; Nadolny, Jakub; Cepa, J.; Diego, J. A. de; García, Ana María Pérez; Gallego, J.; Lara-López, M. A.; Sánchez‐Portal, M.; González‐Serrano, J. I.; Alfaro, Emilio J.; Martínez, Rocío Navarro; Martínez, Ricardo Pérez; González, Jesús; Torres, Carmen P. Padilla; Castañeda, H. O.; González, Mauro

doi:10.1051/0004-6361/202039880

Cited by 5 publications

(13 citation statements)

References 72 publications

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“…Indeed, the mean value of the SFR in Hα is 0.125 M e yr −1 , so if we want to observe such SFR in the [O II] line, the value of the luminosity has to be 2.36 × 10 40 erg s −1 . However, the minimum value in luminosity detected for the [O II] galaxy sample is 2.37 × 10 40 erg s −1 (see Cedrés et al 2021). Nevertheless, taking into account the uncertainties, the results for Hα are compatible with the rest of the lines (Hβ and [O II]) in the mass range in which they coincide.…”

Section: Sfr and Ssfrmentioning

confidence: 68%

“…The estimations of E(B − V ) values were sampled by the code in intervals of 0.05 mag. We obtained median extinctions E(B − V ) ; 0.1, E(B − V ) ; 0.1, and E (B − V ) ; 0.15 for Hα, Hβ, and [O II] respectively (see Ramón-Pérez et al 2019;Navarro Martínez et al 2021 andCedrés et al 2021).…”

Section: The Otelo Samplesmentioning

confidence: 84%

“…A direct consequence of the design of the OTELO survey is the favoring of detection of low-mass galaxies (M * < 10 10 M e ), which comprise more than the 87% of the total detected emitters (see, for example, Cedrés et al 2021 andBongiovanni et al 2020).…”

Section: The Otelo Samplesmentioning

confidence: 99%

“…The luminosity functions (LFs) covering the main emission lines for the OTELO emitters has already been calculated in Ramón-Pérez et al (2019), Navarro Martínez et al (2021), and Cedrés et al (2021 for redshifts z ∼ 0.4 (Hα), z ∼ 0.9 (Hβ) and z ∼ 1.43 ([O II]), respectively. An in-depth description of the methods and corrections applied (including the corrections from the presence, completeness, and cosmic variance of active galactic nuclei (AGNs)) can be found in those works.…”

Section: The Otelo Samplesmentioning

confidence: 99%

“…Meanwhile, the SFRD in low-mass galaxies has remained fairly constant with redshift, and it is a clear indication of the downsizing first suggested in Cowie et al (1996) and detected in Weisz et al (2011) or in Rodríguez-Muñoz et al (2015), where it is hinted that at least 90% of the stellar mass for low-mass galaxies is preferably formed at low redshift (z  0.15). (Cedrés et al 2021). Contours correspond to the number of galaxies from the Sloan Digital Sky Survey (SDSS) database obtained by Renzini & Peng (2015) at values of 2.0 × 10 4 (blue), 7.0 × 10 4 (green), and 1.2 × 10 5 (red), the last one being the definition of the local star-forming MS.…”

Section: Sfr Densitymentioning

confidence: 99%

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The OTELO Survey: The Star Formation Rate Evolution of Low-mass Galaxies

Cedrés

Pérez-García

Martínez

et al. 2021

ApJL

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We present the analysis of a sample of Hα, Hβ, and [O II] emission line galaxies from the OTELO survey, with masses typically below * M M log 9.4 ( ) and redshifts between z ∼ 0.4 and 1.43. We study the star formation rate, star formation rate density, and their number density and evolution with redshift. We obtain a robust estimate of the specific star formation rate-stellar mass relation based on the lowest-mass sample published so far. We also determine a flat trend of the star formation rate density (SFRD) and number density with redshift. Our results suggest a scenario of no evolution of the number density of galaxies, regardless of their masses, up to redshift z ∼ 1.4. This implies a gradual change of the relative importance of the star-forming processes, from high-mass galaxies to low-mass galaxies, with decreasing redshift. We also find little or no variation of the SFRD in the redshift range of 0.4 < z < 1.43.

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Section: Sfr and Ssfrmentioning

confidence: 68%

Section: The Otelo Samplesmentioning

confidence: 84%

Section: The Otelo Samplesmentioning

confidence: 99%

Section: The Otelo Samplesmentioning

confidence: 99%

Section: Sfr Densitymentioning

confidence: 99%

See 3 more Smart Citations

The OTELO Survey: The Star Formation Rate Evolution of Low-mass Galaxies

Cedrés

Pérez-García

Martínez

et al. 2021

ApJL

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The miniJPAS survey: A search for extreme emission-line galaxies

Iglésias-Páramo¹,

Arroyo²,

Kehrig³

et al. 2022

A&A

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Context. Galaxies with extreme emission lines (EELGs) may play a key role in the evolution of the Universe, as well as in our understanding of the star formation process itself. For this reason an accurate determination of their spatial density and fundamental properties in different epochs of the Universe will constitute a unique perspective towards a comprehensive picture of the interplay between star formation and mass assembly in galaxies. In addition to this, EELGs are also interesting in order to explain the reionization of the Universe, since their interstellar medium (ISM) could be leaking ionizing photons, and thus they could be low z, analogous of extreme galaxies at high z. Aims. This paper presents a method to obtain a census of EELGs over a large area of the sky by detecting galaxies with rest-frame equivalent widths ≥ 300Å in the emission lines [Oii]λλ3727,3729Å, [Oiii]λ5007Å, and Hα. For this, we aim to use the J-PAS survey, which will image an area of ≈ 8000 deg 2 with 56 narrow band filters in the optical. As a pilot study, we present a methodology designed to select EELGs on the miniJPAS images, which use the same filter dataset as J-PAS, and thus will be exportable to this larger survey. Methods. We make use of the miniJPAS survey data, conceived as a proof of concept of J-PAS, and covering an area of ≈ 1 deg 2 . Objects were detected in the r SDSS images and selected by imposing a condition on the flux in a given narrow-band J-PAS filter with respect to the contiguous ones, which is analogous to requiring an observed equivalent width larger than 300Å in a certain emission line within the filter bandwidth. The selected sources were then classified as galaxies or quasi-stellar objects (QSOs) after a comparison of their miniJPAS fluxes with those of a spectral database of objects known to present strong emission lines. This comparison also provided a redshift for each source, which turned out to be consistent with the spectroscopic redshifts when available (|∆z/(1 + z spec )| ≤ 0.01). Results. The selected candidates were found to show a compact appearance in the optical images, some of them even being classified as point-like sources according to their stellarity index. After discarding sources classified as QSOs, a total of 17 sources turned out to exhibit EW 0 ≥ 300Å in at least one emission line, thus constituting our final list of EELGs. Our counts are fairly consistent with those of other samples of EELGs in the literature, although there are some differences, which were expected due to biases resulting from different selection criteria.

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GLACE survey: OSIRIS/GTC tuneable imaging of the galaxy cluster ZwCl 0024.0+1652

Cedrés,

De Daniloff,

Bongiovanni

et al. 2024

A&A

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In this paper, we revisit the data for the galaxy cluster ZwCl 0024.0+1652 provided by the GLACE survey and study the mass--metallicity function and its relationship with the environment. Here we describe an alternative way to reduce the data from OSIRIS tunable filters. This method gives us better uncertainties in the fluxes of the emission lines and the derived quantities. We present an updated catalogue of cluster galaxies with emission in and We also discuss the biases of these new fluxes and describe the way in which we calculated the mass--metallicity relationship and its uncertainties. We generated a new catalogue of 84 emission-line galaxies with reliable fluxes in and lines from a list of 174 galaxies. We find a relationship between the clustercentric radius and the density of galaxies. We derived the mass--metallicity relationship for ZwCl 0024.0+1652 and compared it with clusters and field galaxies from the literature. We find a difference in the mass--metallicity relationship when compared to more massive clusters, with the latter showing on average higher values of abundance. This could be an effect of the quenching of the star formation, which seems to be more prevalent in low-mass galaxies in more massive clusters. We find little to no difference between ZwCl 0024.0+1652 galaxies and field galaxies located at the same redshift.

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The OTELO survey

Cited by 5 publications

References 72 publications

The OTELO Survey: The Star Formation Rate Evolution of Low-mass Galaxies

The OTELO Survey: The Star Formation Rate Evolution of Low-mass Galaxies

The miniJPAS survey: A search for extreme emission-line galaxies

GLACE survey: OSIRIS/GTC tuneable imaging of the galaxy cluster ZwCl 0024.0+1652

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