A large, deep 3 deg2 survey of H α, [O <scp>iii</scp>], and [O <scp>ii</scp>] emitters from LAGER: constraining luminosity functions

Khostovan, Ali Ahmad; Malhotra, Sangeeta; Rhoads, James E.; Jiang, Chunyan; Wang, J.; Wold, Isak; Zheng, Zhen-Ya; Barrientos, L. Felipe; Coughlin, Alicia; Harish, Santosh; Hu, Weida; Infante, L.; Perez, Lucia A.; Pharo, John; Valdés, Francisco; Walker, A. R.; Yang, Huan

doi:10.1093/mnras/staa175

Cited by 28 publications

(35 citation statements)

References 116 publications

(268 reference statements)

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“…Hereafter, when referring to HAEs or O3Es, we also imply that each species lies in these redshift bounds, and that [OIII] refers to [OIII]λ5007 unless otherwise stated. Our 94% overall sample purity is very comparable to the purities seen in narrowband surveys at similar redshifts, e.g., 95% for Hα at z = 0.84 (Sobral et al 2013), 93.7% for Hα at z = 0.47, and 90.4% for [OIII] at z = 0.93 (Khostovan et al 2020). We summarize our spectroscopically confirmed HAEs and O3Es in Table 1.…”

Section: Spectroscopic Redshiftssupporting

confidence: 70%

“…We construct our [OIII] LFs in much the same way as the Hα LFs, except that we do not include an AGN contamination correction. This allows us to make a more direct comparison with other studies that also lack an AGN correction, such as Khostovan et al (2020). In contrast to the Hα LFs, our COSMOS and HEROES ) ∼ 41.75 erg s −1 .…”

Section: Luminosity Functionsmentioning

confidence: 73%

“…While we considered performing a dust attenuation correction of our own data, we found that our spectroscopic datasets were insufficiently calibrated to provide reliable Hα/Hβ line ratios for calibrating dust attenuation with the Balmer decrement. Khostovan et al (2020) noted the same difficulty with the zCOSMOS dataset and instead opted for a dust correction based on g − r colors. We refrained from using such a correction to avoid any potential bias introduced by using g − r color for both dust attenuation and differentiation between HAEs and O3Es.…”

Section: Luminosity Functionsmentioning

confidence: 99%

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Subaru/HSC z-Broadband Excess Selection of Extreme Emission Line Galaxies at z<1

Rosenwasser,

Taylor,

Barger

et al. 2022

Preprint

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We present a search for extreme emission line galaxies (EELGs) at z < 1 in the COSMOS and North Ecliptic Pole (NEP) fields with imaging from Subaru/Hyper Suprime-Cam (HSC) and a combination of new and existing spectroscopy. We select EELGs on the basis of substantial excess flux in the z broadband, which is sensitive to Hα at 0.3 z 0.42 and [OIII]λ5007 at 0.7 z 0.86. We identify 10,470 galaxies with z excesses in the COSMOS dataset and 91,385 in the NEP field. We cross-reference the COSMOS EELG sample with the zCOSMOS and DEIMOS 10k spectral catalogs, finding 1395 spectroscopic matches. We made an additional 71 (46 unique) spectroscopic measurements with Y < 23 using the HYDRA multi-object spectrograph on the WIYN 3.5m telescope, and 204 spectroscopic measurements from the DEIMOS spectrograph on the Keck II telescope, providing a total of 1441/10,470 spectroscopic redshifts for the EELG sample in COSMOS (∼14%). We confirm that 1418 (∼98%) are Hα or [OIII]λ5007 emitters in the above stated redshift ranges. We also identify 240 redshifted Hα and [OIII]λ5007 emitters in the NEP using spectra taken with WIYN/HYDRA and Keck/DEIMOS. Using broadband selection techniques in g − r − i color space, we distinguish between Hα and [OIII]λ5007 emitters with 98.6% accuracy. We test our EELG selection by constructing Hα and [OIII]λ5007 luminosity functions and comparing to recent literature results. We conclude that broadband magnitudes from HSC, the Vera C. Rubin Observatory, and other deep optical multi-band surveys can be used to select EELGs in a straightforward manner.

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Section: Spectroscopic Redshiftssupporting

confidence: 70%

Section: Luminosity Functionsmentioning

confidence: 73%

Section: Luminosity Functionsmentioning

confidence: 99%

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Subaru/HSC z-Broadband Excess Selection of Extreme Emission Line Galaxies at z<1

Rosenwasser,

Taylor,

Barger

et al. 2022

Preprint

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“…On the other hand, our result seems to agreed with the trend observed in other works and cited in Hayashi et al (2013), where the authors found that [O ii]3727 emitters selected by narrow-band (NB) techniques are likely to be dust-poor systems. For example, both Hayashi et al (2013) and Khostovan et al (2020) give A Hα ∼ 0.35 mag for emitters at z ∼ 1.47, Hayashi et al (2015) found A Hα = 0.63 mag for z = 1.5, and Khostovan et al (2015) obtains A Hα = 0.55 ± 0.12 mag for emitters at z = 1.59. Nevertheless, the large dispersion of the mean value derived makes difficult to obtain a clear conclusion about the absorption nature of our emitters.…”

Section: Extinction Correctionmentioning

confidence: 99%

“…Other works have used the combination of Hβ and [O iii], for example De Barros et al (2019) reaching as far as z ∼ 8; Khostovan et al (2015) up to 0.84 < z < 3.24; and Sobral et al (2015) up to z = 1.4. In addition, there are a series of works were the LF is obtained by employing the doublet [O iii] λλ4959,5007 alone, for example, in Ly et al (2007) at 0.41 < z < 0.84; Bongiovanni et al (2020) at z ∼ 0.83; Khostovan et al (2020) at 0.91 < z < 1.10; or Hayashi et al (2020) at 0.05 < z < 0.94.…”

Section: Introductionmentioning

confidence: 99%

The OTELO survey

Cedrés

Bongiovanni

Cerviño

et al. 2021

A&A

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Aims. In this paper, we aim to study the main properties and luminosity function (LF) of the [O II]3727 emitters detected in the OTELO survey in order to characterise the star formation processes in low-mass galaxies at z ∼ 1.43 and to constrain the faint-end of the LF. Methods. Here, we describe the selection method and analysis of the emitters obtained from narrow-band scanning techniques. In addition, we present several relevant properties of the emitters and discuss the selection biases and uncertainties in the determination of the LF and the star formation rate density (SFRD). Results. We confirmed a total of 60 sources from a preliminary list of 332 candidates as [O II]3727 emitters. Approximately 93% of the emitters have masses in the range of 108 < M*/M⊙ < 109. All of our emitters are classified as late-type galaxies, with a lower value of (u − v) when compared with the rest of the emitters of the OTELO survey. We find that the cosmic variance strongly affects the normalisation (ϕ*) of the LF and explains the discrepancy of our results when compared with those obtained from surveys of much larger volumes. However, we are able to determine the faint-end slope of the LF, namely, α = −1.42 ± 0.06, by sampling the LF down to ∼1 dex lower than in previous works. We present our calculation of the SFRD of our sample and compare it to the value obtained in previous studies from the literature.

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

Martínez-Solaeche¹,

Delgado²,

García-Benito³

et al. 2022

A&A

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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 deg2, 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⊙]−8.85−0.20+0.19 and has an intrinsic scatter of 0.20−0.01+0.01. The cosmic evolution of the SFR density (ρSFR) 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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A large, deep 3 deg2 survey of H α, [O iii], and [O ii] emitters from LAGER: constraining luminosity functions

Cited by 28 publications

References 116 publications

Subaru/HSC z-Broadband Excess Selection of Extreme Emission Line Galaxies at z<1

Subaru/HSC z-Broadband Excess Selection of Extreme Emission Line Galaxies at z<1

The OTELO survey

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

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