STRONG NEBULAR LINE RATIOS IN THE SPECTRA of<i>z</i>∼ 2-3 STAR FORMING GALAXIES: FIRST RESULTS FROM KBSS-MOSFIRE

Steidel, Charles C.; Rudie, Gwen C.; Strom, Allison L.; Pettini, Max; Reddy, Naveen A.; Shapley, Alice E.; Trainor, Ryan F.; Erb, Dawn K.; Turner, Monica L.; Konidaris, Nick; Kulas, Kristin R.; Mace, Gregory N.; Matthews, K.; McLean, Ian S.

doi:10.1088/0004-637x/795/2/165

Cited by 657 publications

(1,349 citation statements)

References 135 publications

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“…To verify this conclusion with our sample we show in Fig. 9 star-forming galaxies at z > 2 by Cullen et al (2014) (stars), star-forming galaxies at 2.0 < z < 2.6 by Steidel et al (2014) (filled circles), star-forming galaxies at redshifts z ∼ 3.5 by Maiolino et al (2008) (filled squares), star-forming galaxies with z ∼ 2 by Maier et al (2014) (crosses), and star-forming galaxies with z ∼ 3.4 by Troncoso et al (2014) (asterisks). The relation for galaxies with z ∼ 2.3 by Sanders et al (2015) is shown by thick yellow solid line.…”

Section: Stellar Mass -Metallicity Relationsupporting

confidence: 59%

“…The mass-metallicity relation by Tremonti et al (2004) is often used as a benchmark for comparisons with similar relations obtained for low-z and high-z galaxies (e.g. Lee et al 2006;Maiolino et al 2008;Amorín et al 2010;Manucci et al 2010;Maier et al 2014;Steidel et al 2014;Zahid et al 2011Zahid et al , 2012Zahid et al , 2013Zahid et al , 2014a. However, we note that Tremonti et al (2004) selected all star-forming galaxies, including galaxies with low-excitation H ii regions, while only galaxies with high-excitation H ii regions are present in high-z samples.…”

Section: Introductionmentioning

confidence: 74%

“…Therefore, strong-line methods calibrated with the Te-method can be applied. Steidel et al (2014) compared SFRs obtained for their sample from the UV continuum luminosities and Hα luminosities and found good agreement. They derived oxygen abundances by using strong-line O3N 2 calibration, similar to that applied for our sample.…”

Section: Hβ Luminosity -Metallicity Relationmentioning

confidence: 81%

“…The dashed lines are maximum-likelihood linear fits only for the galaxies with EW(Hβ) 100Å shown by magenta symbols. The location of star-forming galaxies with redshifts 2.0 < z < 2.6 by Steidel et al (2014) and with redshifts z > 2 by Cullen et al (2014) is shown by grey rectangles. Star-forming galaxies with redshifts z ∼ 3.4 by Troncoso et al (2014) are indicated by dark asterisks.…”

Section: Absolute G-band Magnitude -Metallicity Relationmentioning

confidence: 99%

“…(2004) is shown by thin dashed lines and dot-dashed lines are 1σ dispersions. The location of stacked data for star-forming galaxies at z > 2 by Cullen et al (2014) and of data for ninety six star-forming galaxies at 2.0 < z < 2.6 by Steidel et al (2014) are shown by dark-grey filled stars and open circles, respectively. Star-forming galaxies at z ∼ 3.5 by Maiolino et al (2008) and at z ∼ 2 by Maier et al (2014) are shown by dark-grey filled squares and crosses, respectively.…”

Section: Absolute G-band Magnitude -Metallicity Relationmentioning

confidence: 99%

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On the universality of luminosity–metallicity and mass–metallicity relations for compact star-forming galaxies at redshifts 0 < z < 3

Izotov

Гусева

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et al. 2015

Monthly Notices of the Royal Astronomical Society

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We study relations between global characteristics of low-redshift (0 < z < 1) compact star-forming galaxies, including absolute optical magnitudes, Hβ emission-line luminosities (or equivalently star-formation rates), stellar masses, and oxygen abundances. The sample consists of 5182 galaxies with high-excitation H ii regions selected from the SDSS DR7 and SDSS/BOSS DR10 surveys adopting a criterion [O iii]λ4959/Hβ 1. These data were combined with the corresponding data for high-redshift (2 z 3) star-forming galaxies. We find that in all diagrams low-z and high-z star-forming galaxies are closely related indicating a very weak dependence of metallicity on stellar mass, redshift, and star-formation rate. This finding argues in favour of the universal character of the global relations for compact star-forming galaxies with high-excitation H ii regions over redshifts 0 < z < 3.

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Section: Stellar Mass -Metallicity Relationsupporting

confidence: 59%

Section: Introductionmentioning

confidence: 74%

Section: Hβ Luminosity -Metallicity Relationmentioning

confidence: 81%

Section: Absolute G-band Magnitude -Metallicity Relationmentioning

confidence: 99%

Section: Absolute G-band Magnitude -Metallicity Relationmentioning

confidence: 99%

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On the universality of luminosity–metallicity and mass–metallicity relations for compact star-forming galaxies at redshifts 0 < z < 3

Izotov

Гусева

Fricke

et al. 2015

Monthly Notices of the Royal Astronomical Society

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Gas Accretion and Galactic Chemical Evolution: Theory and Observations

Finlator

2017

Gas Accretion Onto Galaxies

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This chapter reviews how galactic inflows influence galaxy metallicity. The goal is to discuss predictions from theoretical models, but particular emphasis is placed on the insights that result from using models to interpret observations. Even as the classical "G-dwarf problem" endures in the latest round of observational confirmation, a rich and tantalizing new phenomenology of relationships between M * , Z, SFR, and gas fraction is emerging both in observations and in theoretical models. A consensus interpretation is emerging in which star-forming galaxies do most of their growing in a quiescent way that balances gas inflows and gas processing, and metal dilution with enrichment. Models that explicitly invoke this idea via equilibrium conditions can be used to infer inflow rates from observations, while models that do not assume equilibrium growth tend to recover it self-consistently. Mergers are an overall subdominant mechanism for delivering fresh gas to galaxies, but they trigger radial flows of previously-accreted gas that flatten radial gas-phase metallicity gradients and temporarily suppress central metallicities. Radial gradients are generically expected to be steep at early times and then flattened by mergers and enriched inflows of recycled gas at late times. However, further theoretical work is required in order to understand how to interpret observations. Likewise, more observational work is needed in order to understand how metallicity gradients evolve to high redshifts.

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Observations of Ly$$\alpha $$ Emitters at High Redshift

Ouchi

2019

Lyman-Alpha as an Astrophysical and Cosmological Tool

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In this series of lectures, I review our observational understanding of highz Lyα emitters (LAEs) and relevant scientific topics. Since the discovery of LAEs in the late 1990s, significant progresses in LAE studies have been made over the past two decades by deep multi-wavelength observations. More than ten (one) thousand(s) of LAEs have been identified photometrically (spectroscopically) in optical and near-infrared data, and the redshifts of these LAEs range from z ∼ 0 to z ∼ 10. These large samples of LAEs are useful to address two major astrophysical issues, galaxy formation and cosmic reionization. Statistical studies have revealed the general picture of LAEs' physical properties: young stellar populations, remarkable luminosity function evolutions, compact morphologies, highly ionized inter-stellar media (ISM) with low metal/dust contents, low masses of dark-matter halos. Typical LAEs represent low-mass high-z galaxies, high-z analogs of dwarf galaxies, some of which are thought to be candidates of population III galaxies. These observational studies have also pinpointed rare bright Lyα sources extended over ∼ 10 − 100 kpc, dubbed Lyα blobs, whose physical origins are under debate. LAEs are used as probes of cosmic reionization history through the Lyα damping wing absorption given by the neutral hydrogen of the inter-galactic medium (IGM), which complement the cosmic microwave background radiation and 21cm observations targeting the epoch of reionization. The low-mass and highly-ionized population of LAEs can be major sources of cosmic reionization, and physical parameters including the ionizing photon escape fraction have been extensively investigated. The budget of ionizing photons for cosmic reionization has been constrained, although there remain large observational uncertainties in the parameters. Beyond these two established topics of LAEs, galaxy formation and cosmic reionization, several new usages of LAEs for science frontiers have been suggested such as the distribution of HI gas in the circum-galactic medium and filaments of large-scale structures. Ongoing 10 mclass optical telescope programs and future telescope projects, such as JWST, ELTs,

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STRONG NEBULAR LINE RATIOS IN THE SPECTRA ofz∼ 2-3 STAR FORMING GALAXIES: FIRST RESULTS FROM KBSS-MOSFIRE

Cited by 657 publications

References 135 publications

On the universality of luminosity–metallicity and mass–metallicity relations for compact star-forming galaxies at redshifts 0 < z < 3

On the universality of luminosity–metallicity and mass–metallicity relations for compact star-forming galaxies at redshifts 0 < z < 3

Gas Accretion and Galactic Chemical Evolution: Theory and Observations

Observations of Ly$$\alpha $$ Emitters at High Redshift

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