J-PLUS: The star formation main sequence and rate density at d  ≲  75 Mpc

Abstract

Aims. Our goal is to estimate the star formation main sequence (SFMS) and the star formation rate density (SFRD) at z ≤ 0.017 (d 75 Mpc) using the Javalambre Photometric Local Universe Survey (J-PLUS) first data release, that probes 897.4 deg 2 with twelve optical bands. Methods. We extract the Hα emission flux of 805 local galaxies from the J-PLUS filter J0660, being the continuum level estimated with the other eleven J-PLUS bands, and the dust attenuation and nitrogen contamination corrected with empirical relations. Stellar masses (M), Hα luminosities (L Hα), and star formation rates (SFRs) were estimated by accounting for parameters covariances. Our sample comprises 689 blue galaxies and 67 red galaxies, classified in the (u − g) vs (g − z) color-color diagram, plus 49 AGN. Results. The SFMS is explored at log M 8 and it is clearly defined by the blue galaxies, with the red galaxies located below them. The SFMS is described as log SFR = 0.83 log M −8.44. We find a good agreement with previous estimations of the SFMS, especially those based on integral field spectroscopy. The Hα luminosity function of the AGN-free sample is well described by a Schechter function with log L * Hα = 41.34, log φ * = −2.43, and α = −1.25. Our measurements provide a lower characteristic luminosity than several previous studies in the literature. Conclusions. The derived star formation rate density at d 75 Mpc is log ρ SFR = −2.10 ± 0.11, with red galaxies accounting for 15% of the SFRD. Our value is lower than previous estimations at similar redshift, and provides a local reference for evolutionary studies regarding the star formation history of the Universe.

J-PLUS: Uncovering a large population of extreme [OIII] emitters in the local Universe

“…This photometric survey has already produced relevant results in the detection and analysis of extragalactic systems presenting emission lines in their spectra. In the local Universe, previous works by Logroño-García et al (2019) and Vilella-Rojo et al (2021) have analyzed Hα emitters and measured accurately the local star formation main sequence. In addition, Spinoso et al (2020) performed a search for highredshift quasars with Lyman α emission in J-PLUS, finding an unprecedented number of very high luminosity sources.…”

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

“…In terms of the SFR density (ρ SFR ), the Universe reached a peak at ∼3 Gyr after the Big Bang, and it has been decreasing ever since (Madau & Dickinson 2014;Driver et al 2018;López Fernández et al 2018;Sánchez et al 2019;Leja et al 2019;Bellstedt et al 2020). Through Hα measurements, astronomers are also able to measure ρ SFR both in the nearby Universe and at intermediate redshift, which has confirmed this trend (Gallego et al 1995;Ly et al 2007;Shioya et al 2008;Dale et al 2010;Westra et al 2010;Drake et al 2013;Sobral et al 2013Sobral et al , 2015Gunawardhana et al 2013;Stroe & Sobral 2015;Van Sistine et al 2016;Khostovan et al 2020;Vilella-Rojo et al 2021).…”

“…While massive galaxies undergo a larger fraction of their star formation at early times, less massive galaxies are still forming stars at a high rate today. The star formation main sequence (SFMS), a tight quasi-linear relation between stellar mass, (M ), and the SFR in log scale (Zahid et al 2012;Renzini & Peng 2015;Cano-Díaz et al 2016Duarte Puertas et al 2017;Belfiore et al 2018;Boogaard et al 2018;Sánchez et al 2019;Shin et al 2021;Vilella-Rojo et al 2021), can reveal indications how this process takes place. Galaxies that are undergoing a starburst, for instance, lie above the SFMS, while galaxies that have already quenched their star formation lie below this relation.…”

“…The definition of the SFMS itself might also lead to significant differences between different works, even though they all trace the SFR through the Hα line. Some authors (e.g., Vilella-Rojo et al 2021, z ≤ 0.017 or Shin et al 2021, z ∼ 0.07−0.5) relied on color-color diagrams. Others selected starforming (SF) galaxies based on the BPT diagrams with a cut in the equivalent width (EW) of Hα or Hβ.…”

J-PLUS: Uncovering a large population of extreme [OIII] emitters in the local Universe

“…Using a set of several narrowband or mediumband filters, sometimes including also broadband ones, these surveys detect easily emission lines by identifying an excess of flux in one of the bands (e.g. Hip-pelein et al 2003;Maier et al 2003;Gronwall et al 2007;Sobral et al 2013Sobral et al , 2015Cava et al 2015;Lumbreras-Calle et al 2019a;Spinoso et al 2020;Vilella-Rojo et al 2021). While usually providing smaller fields of view and less wavelength coverage than broadband or objective prism surveys, they can reach deeper magnitudes than the former and higher spectral resolution than the latter.…”