Spectral classification of emission-line galaxies from the Sloan Digital Sky Survey

Marocco, Julien; Hache, Emeric; Lamareille, F.

doi:10.1051/0004-6361/201016143

Cited by 18 publications

(29 citation statements)

References 37 publications

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“…It is key to replace future BAO tracers in the galaxy formation history. With the current sample, we draw simple trends using means and standard deviation of the observed quantities, and we place the ELGs in the galaxy classification made by Lamareille (2010); Marocco et al (2011).…”

Section: Physical Properties Of Elgsmentioning

confidence: 99%

Investigating emission-line galaxy surveys with the Sloan Digital Sky Survey infrastructure

Comparat

Kneib

Escoffier

et al. 2012

Monthly Notices of the Royal Astronomical Society

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The Baryon Acoustic Oscillation (BAO) feature in the power spectrum of galaxies provides a standard ruler to probe the accelerated expansion of the Universe. The current surveys covering a comoving volume sufficient to unveil the BAO scale are limited to redshift z 0.7. In this paper, we study several galaxy selection schemes aiming at building an emission-linegalaxy (ELG) sample in the redshift range 0.6 < z < 1.7, that would be suitable for future BAO studies using the Baryonic Oscillation Spectroscopic Survey (BOSS) spectrograph on the Sloan Digital Sky Survey (SDSS) telescope. We explore two different colour selections using both the SDSS and the Canada France Hawai Telescope Legacy Survey (CFHT-LS) photometry in the u, g, r, and i bands and evaluate their performance selecting luminous ELG. From about 2,000 ELG, we identified a selection scheme that has a 75 percent redshift measurement efficiency. This result confirms the feasibility of massive ELG surveys using the BOSS spectrograph on the SDSS telescope for a BAO detection at redshift z ∼ 1, in particular the proposed eBOSS experiment, which plans to use the SDSS telescope to combine the use of the BAO ruler with redshift space distortions using emission line galaxies and quasars in the redshift 0.6 < z < 2.2.

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Section: Physical Properties Of Elgsmentioning

confidence: 99%

Investigating emission-line galaxy surveys with the Sloan Digital Sky Survey infrastructure

Comparat

Kneib

Escoffier

et al. 2012

Monthly Notices of the Royal Astronomical Society

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“…2.2.1. By considering the separation curve proposed by Marocco et al (2011), plotted in the left hand lower panel of Fig. 1, we classified 262 galaxies (9.9%) as narrow-line AGNs, and thus we rejected them.…”

Section: Selection Of Star-forming Galaxiesmentioning

confidence: 99%

The cosmic evolution of oxygen and nitrogen abundances in star-forming galaxies over the past 10 Gyr

Pérez-Montero

Contini

Lamareille

et al. 2012

A&A

Self Cite

102

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Aims. The chemical evolution of galaxies on a cosmological timescale is still a matter of debate despite the increasing number of available data provided by spectroscopic surveys of star-forming galaxies at different redshifts. The fundamental relations involving metallicity, such as the mass−metallicity relation (MZR) or the fundamental metallicity relation, give controversial results about the reality of evolution of the chemical content of galaxies at a given stellar mass. In this work we shed some light on this issue using the completeness reached by the 20 k bright sample of the zCOSMOS survey and using for the first time the nitrogen-to-oxygen ratio (N/O) as a tracer of the gas phase chemical evolution of galaxies that is independent of the star formation rate. Methods. Emission-line galaxies both in the SDSS and 20 k zCOSMOS bright survey were used to study the evolution from the local Universe of the MZR up to a redshift of ∼1.32, and the relation between stellar mass and N/O (MNOR) up to a redshift of ∼0.42 using the N2S2 parameter. All the physical properties derived from stellar continuum and gas emission-lines, including stellar mass, star formation rates, metallicity and N/O, were calculated in a self-consistent way over the full redshift range. Results. We confirm the trend to find lower metallicities in galaxies of a given stellar mass in a younger Universe. This trend is even observed when taking possible effects into account that are due to the observed larger median star formation rates for galaxies at higher redshifts. We also find a significant evolution of the MNOR up to z ∼ 0.4. Taking the slope of the O/H vs. N/O relation into account for the secondary-nitrogen production regime, the observed evolution of the MNOR is consistent with the trends found for both the MZR and its equivalent relation using new expressions to reduce its dependence on star formation rate.

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“…Tresse et al (1996) and Rola et al (1997) (Lamareille 2010), U -B color (Yan et al 2011), or stellar mass (Juneau et al 2011(Juneau et al , 2013, massexcitation diagnostic, MEx). Marocco et al (2011) also used D n (4000) versus [O III]/Hβ for classification of high-z galaxies. These methods take advantage of the fact that AGNs reside in massive, red galaxies in the local universe, and they are in general efficient in separating pure AGNs and star-forming galaxies.…”

Section: Introductionmentioning

confidence: 99%

A New Diagnostic Diagram of Ionization Sources for High-redshift Emission Line Galaxies

Zhang

Hao

2018

ApJ

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We propose a new diagram, the kinematics-excitation (KEx) diagram, which uses the [O III] λ5007/Hβ line ratio and the [O III] λ5007emission line width (σ [O III] ) to diagnose the ionization source and physical properties of active galactic nuclei (AGNs) and star-forming galaxies (SFGs). The KEx diagram is a suitable tool to classify emission line galaxies at intermediate redshift because it uses only the [O III] λ5007 and Hβ emission lines. We use the main galaxy sample of SDSS DR7 and the Baldwin−Phillips−Terlevich (BPT) diagnostic to calibrate the diagram at low redshift. The diagram can be divided into three regions: the KEx-AGN region, which consists mainly of pure AGNs, the KEx-composite region, which is dominated by composite galaxies, and the KEx-SFG region, which contains mostly SFGs. LINERs strongly overlap with the composite and AGN regions. AGNs are separated from SFGs in this diagram mainly because they preferentially reside in luminous and massive galaxies and have higher [O III]/Hβ than SFGs. The separation between AGNs and SFGs is even cleaner thanks to the additional 0.15/0.12dex offset in σ [O III] at fixed luminosity/stellar mass. We apply the KEx diagram to 7866 galaxies at 0.3<z<1 in the DEEP2 Galaxy Redshift Survey, and compare it to an independent X-ray classification scheme using Chandra observations. X-ray AGNs are mostly located in the KEx-AGN region, while X-ray SFGs are mostly located in the KEx-SFG region. Almost all Type 1 AGNs lie in the KEx-AGN region. These tests support the reliability of this classification diagram for emission line galaxies at intermediate redshift.At z∼2, the demarcation line between SFGs and AGNs is shifted by ∼0.3dex toward higher values of σ [O III] due to evolution effects.

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Spectral classification of emission-line galaxies from the Sloan Digital Sky Survey

Cited by 18 publications

References 37 publications

Investigating emission-line galaxy surveys with the Sloan Digital Sky Survey infrastructure

Investigating emission-line galaxy surveys with the Sloan Digital Sky Survey infrastructure

The cosmic evolution of oxygen and nitrogen abundances in star-forming galaxies over the past 10 Gyr

A New Diagnostic Diagram of Ionization Sources for High-redshift Emission Line Galaxies

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