LBT/LUCIFER OBSERVATIONS OF THE<i>z</i>∼ 2 LENSED GALAXY J0900+2234

Bian, Fuyan; Fan, Xiaohui; Bechtold, Jill; McGreer, Ian D.; Just, Dennis W.; Sand, David J.; Green, Richard F.; Thompson, D. J.; Peng, Chien Y.; Seifert, W.; Ageorges, N.; Juette, M.; Knierim, Volker; Buschkamp, P.

doi:10.1088/0004-637x/725/2/1877

Cited by 70 publications

(82 citation statements)

References 52 publications

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“…In this paper we use data for 44 lensed galaxies at 1 < z < 5 complied from the literature (Teplitz et al 2000;Siana et al 2008;Swinbank et al 2009;Hainline et al 2009;Bian et al 2010;Pettini et al 2010;Christensen et al 2010;Jones et al 2010;Richard et al 2011;Wuyts et al 2012a;Christensen et al 2012b,a;Wuyts et al 2012b;Yuan et al 2012;Jones et al 2013;Belli et al 2013), again avoiding duplications.…”

Section: Data Setsmentioning

confidence: 99%

A break in the high-redshift stellar mass Tully–Fisher relation

Christensen¹,

Hjorth²

2017

Monthly Notices of the Royal Astronomical Society

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We investigate the stellar-mass Tully-Fisher relation (TFR) between the stellar mass and the integrated gas velocity dispersion, quantified by the kinematic estimator S 0.5 measured from strong emission lines in spectra of galaxies at 0 < z < 5. We combine luminosity-selected galaxies ('high-luminosity sample') with galaxies selected in other ways ('low-luminosity sample') to cover a range in stellar mass that spans almost five orders of magnitude: 7.0 ∼ < log M * /M ⊙ ∼ < 11.5. We find that the logarithmic power-law slope and normalisation of the TFR are independent of redshift out to z ∼ 3. The scatter in the TFR is < 0.5 dex such that the gas velocity dispersion can be used as a proxy for the stellar mass of a galaxy independently of its redshift. At z > 3 the scatter increases and the existence of a correlation is not obvious. The high-luminosity sample exhibits a flatter slope of 1.5±0.2 at z < 3 compared to the lowluminosity sample slope of 2.9±0.3, suggesting a turnover in the TFR. The combined sample is well fit with a break in the TFR at a characteristic stellar mass scale of M * ∼ 10 10 M ⊙ , with no significant evolution out to z ∼ 3. We demonstrate that a break in the TFR with a steeper slope at the low-mass end is a natural consequence of galaxy models with a mass-dependent stellar to halo-mass ratio.

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Section: Data Setsmentioning

confidence: 99%

A break in the high-redshift stellar mass Tully–Fisher relation

Christensen¹,

Hjorth²

2017

Monthly Notices of the Royal Astronomical Society

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“…High redshift field galaxies appear to have larger [N II]/Hα and/or [O III]/Hβ optical line ratios (by ∼0.3 dex) compared with local field galaxies (Erb et al 2006;Hainline et al 2009;Bian et al 2010;Rigby et al 2011;Yabe et al 2012;Zahid et al 2013a;Holden et al 2014;Shapley et al 2015;Steidel et al 2014). These elevated line ratios may indicate a major change in the ionized gas or star formation properties as a function of time.…”

Section: Introductionmentioning

confidence: 97%

Z-FIRE: ISM PROPERTIES OF THEz= 2.095 COSMOS CLUSTER

Kewley

Yuan

Nanayakkara

et al. 2016

ApJ

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We investigate the ISM properties of 13 star-forming galaxies within thez 2 COSMOS cluster. We show that the cluster members have [N II]/Hα and [O III]/Hβ emission-line ratios similar toz 2 field galaxies, yet systematically different emission-line ratios (by ∼0.17 dex) from the majority of local star-forming galaxies. We find no statistically significant difference in the [N II]/Hα and [O III]/Hβ line ratios or ISM pressures among thẽ z 2 cluster galaxies and field galaxies at the same redshift. We show that our cluster galaxies have significantly larger ionization parameters (by up to an order of magnitude) than local star-forming galaxies. We hypothesize that these high ionization parameters may be associated with large specific star formation rates (SFRs; i.e., a large SFR per unit stellar mass). If this hypothesis is correct, then this relationship would have important implications for the geometry and/or the mass of stars contained within individual star clusters as a function of redshift.

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“…PP04 compiled an extensive sample of H II regions in nearby spiral, irregular and blue compact galaxies and fit the relationship between the metallicities mostly from direct temperature (T e ) method 1 and strong emissionline ratios, including the N 2 = log([N II]λ6584/Hα) and O3N 2 = log[([O III]λ5007/Hβ)/([N II]λ6584/Hα)] ratios. These two empirical calibrations based on local H II regions have been widely used to estimate the metallicities of high-redshift galaxies (e.g., Erb et al 2006;Hainline et al 2009;Bian et al 2010;Steidel et al 2014;Sanders et al 2015).…”

Section: Introductionmentioning

confidence: 99%

Mass–metallicity Relation for Local Analogs of High-Redshift Galaxies: Implications for the Evolution of the Mass–metallicity Relations

Bian

Kewley

Dopita

et al. 2016

ApJ

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We revisit the evolution of the mass-metallicity relation of low-and high-redshift galaxies by using a sample of local analogs of high-redshift galaxies. These analogs share the same location of the UV-selected star-forming galaxies at z ∼ 2 on the [O III]λ5007/Hβ versus [N II]λ6584/Hα nebular emission-line diagnostic (or BPT) diagram. Their physical properties closely resemble those in z ∼ 2 UV-selected star-forming galaxies being characterized in particular by high ionization parameters (log q ≈ 7.9) and high electron densities (n e ≈ 100 cm −3 ). With the full set of well-detected rest-frame optical diagnostic lines, we measure the gas-phase oxygen abundance in the SDSS galaxies and these local analogs using the empirical relations and the photoionization models. We find that the metallicity difference between the SDSS galaxies and our local analogs in the 8.5 < log(M * /M ⊙ ) < 9.0 stellar mass bin varies from -0.09 to 0.39 dex, depending on strong-line metallicity measurement methods. Due to this discrepancy the evolution of mass-metallicity should be used to compare with the cosmological simulations with caution. We use the [S II]/Hα and [O I]/Hα BPT diagram to reduce the potential AGN and shock contamination in our local analogs. We find that the AGN/shock influences are negligible on the metallicity estimation.

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LBT/LUCIFER OBSERVATIONS OF THEz∼ 2 LENSED GALAXY J0900+2234

Cited by 70 publications

References 52 publications

A break in the high-redshift stellar mass Tully–Fisher relation

A break in the high-redshift stellar mass Tully–Fisher relation

Z-FIRE: ISM PROPERTIES OF THEz= 2.095 COSMOS CLUSTER

Mass–metallicity Relation for Local Analogs of High-Redshift Galaxies: Implications for the Evolution of the Mass–metallicity Relations

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