The nature of [S III]λλ9096, 9532 emitters at z = 1.34 and 1.23

An, FangXia; Zheng, Xianzhong; Meng, Yan-Zhi; Chen, Yang; Wen, ZhangZheng

doi:10.1007/s11433-013-5331-y

Cited by 5 publications

(3 citation statements)

References 54 publications

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“…One disadvantage in the use of sulfur lines is that they shift into the NIR for objects at even moderate redshifts. However, the work of An et al (2013) shows that this is being addressed with new IR instrumentation. The latter work presents a study on the nature of the [SIII]λλ9096, 9532 emitters, showing that these objects are usually star forming systems where a Compton-thick AGN has little or no effect in exciting the sulfur lines.…”

Section: Introductionmentioning

confidence: 99%

Direct determination of oxygen abundances in line-emitting star-forming galaxies at intermediate redshift

Pérez

Hoyos

Díaz

et al. 2015

Mon. Not. R. Astron. Soc.

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We present a sample of 22 blue ((B − V ) AB < 0.45), luminous (M B,AB < −18.9), metal-poor galaxies in the 0.69 < z < 0.88 redshift range, selected from the DEEP2 galaxy redshift survey. Their spectra contain the [OIII] λ4363 auroral line, the [OII]λλ3726, 3729 doublet and the strong nebular [OIII]λλ4959, 5007 emission lines. The ionised gas-phase oxygen abundances of these galaxies lie between 7.62 < 12 + log O/H < 8.19, i.e. between 1/10Z ⊙ and 1/3Z ⊙ . We find that galaxies in our sample have comparable metallicities to other intermediate-redshift samples, but are more metal poor than local systems of similar B-band luminosities and star formation activity. The galaxies here show similar properties to the "green peas" discovered at z ≃ 0.2 − 0.3 though our galaxies tend to be slightly less luminous.

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Section: Introductionmentioning

confidence: 99%

Direct determination of oxygen abundances in line-emitting star-forming galaxies at intermediate redshift

Pérez

Hoyos

Díaz

et al. 2015

Mon. Not. R. Astron. Soc.

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“…Because the narrow-band filter H 2 S(1) has a relatively small band width ∆λ, we attribute the emission line detected in this band to [O III]λ5007 (this will be discussed later in Section 6.1). More details about emission-line sources selection and the EAZY SED fittings refer to An et al (2013) and A14.…”

Section: The Redshift Distribution Of the 34 [O Iii]mentioning

confidence: 99%

The Physical Properties of Star-Forming Galaxies with Strong [O III] Lines at z=3.25

Wen,

An,

Zheng

et al. 2022

Preprint

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We present an analysis of physical properties of 34 [O III] emission-line galaxies (ELGs) at z = 3.254±0.029 in the Extended Chandra Deep Field South (ECDFS). These ELGs are selected from deep narrow H 2 S(1) and broad K s imaging of 383 arcmin 2 obtained with CFHT/WIRCam. We construct spectral energy distributions (SEDs) from U to K s to derive the physical properties of ELGs. These [O III] ELGs are identified as starburst galaxies with strong [O III] lines of L [O III] ∼ 10 42.6−44.2 erg s −1 , and have stellar masses of M * ∼ 10 9.0−10.6 M and star formation rates of ∼ 10-210 M yr −1 . Our results show that 24% of our sample galaxies are dusty with A V > 1 mag and EW([O III]) rest ∼ 70-500 Å, which are often missed in optically-selected [O III] ELG samples. Their rest-frame UV and optical morphologies from HST /ACS and HST /WFC3 deep imaging reveal that these [O III] ELGs are mostly multiple-component systems (likely mergers) or compact. And 20% of them are nearly invisible in the rest-frame UV due to heavy dust attenuation. Interestingly, we find that our samples reside in an overdensity consisting of two components: one South-East (SE) with an overdensity factor of δ gal ∼41 over a volume of 13 3 cMpc 3 and the other North-West (NW) with δ gal ∼38 over a volume of 10 3 cMpc 3 . The two overdense substructures are expected to be virialized at z = 0 with a total mass of ∼ 1.1 × 10 15 M and ∼ 4.8 × 10 14 M , and probably merge into a Coma-like galaxy cluster.

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“…Because the narrowband filter H 2 S(1) has a relatively small bandwidth Δλ, we attribute the emission line detected in this band to [O III] λ5007 (this will be discussed later in Section 6.1). More details about emissionline source selection and the EAZY SED fittings can be found in An et al (2013) and A14.…”

Section: Public Datamentioning

confidence: 99%

The Physical Properties of Star-forming Galaxies with Strong [O iii] Lines at z = 3.25

Wen

Zheng

et al. 2022

ApJ

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We present an analysis of physical properties of 34 [O iii] emission-line galaxies (ELGs) at z = 3.254 ± 0.029 in the Extended Chandra Deep Field South (ECDFS). These ELGs are selected from deep narrow H2S(1) and broad K s imaging of 383 arcmin2 obtained with CFHT/WIRCam. We construct spectral energy distributions (SEDs) from U to K s to derive the physical properties of ELGs. These [O iii] ELGs are identified as starburst galaxies with strong [O iii] lines of L OIII ∼ 1042.6–1044.2 erg s−1 and have stellar masses of M * ∼ 109.0–1010.6 M ⊙ and star formation rates of ∼10–210 M ⊙ yr−1. Our results show that 24% of our sample galaxies are dusty with A V > 1 mag and EW([O iii])rest ∼ 70–500 Å, which are often missed in optically selected [O iii] ELG samples. Their rest-frame UV and optical morphologies from HST/ACS and HST/WFC3 deep imaging reveal that these [O iii] ELGs are mostly multiple-component systems (likely mergers) or compact. And 20% of them are nearly invisible in the rest-frame UV owing to heavy dust attenuation. Interestingly, we find that our sample ELGs reside in an overdensity consisting of two components: one southeast (SE) with an overdensity factor of δ gal ∼ 41 over a volume of 133 cMpc3, and the other northwest (NW) with δ gal ∼ 38 over a volume of 103 cMpc3. The two overdense substructures are expected to be virialized at z = 0 with a total mass of ∼ 1.1 × 1015 M ⊙ and ∼ 4.8 × 1014 M ⊙ and probably merge into a Coma-like galaxy cluster.

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The nature of [S III]λλ9096, 9532 emitters at z = 1.34 and 1.23

Cited by 5 publications

References 54 publications

Direct determination of oxygen abundances in line-emitting star-forming galaxies at intermediate redshift

Direct determination of oxygen abundances in line-emitting star-forming galaxies at intermediate redshift

The Physical Properties of Star-Forming Galaxies with Strong [O III] Lines at z=3.25

The Physical Properties of Star-forming Galaxies with Strong [O iii] Lines at z = 3.25

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