Chemical Abundances of DEEP2 Star-forming Galaxies at z~1.0-1.5

By A. Shapley, A. Coil, Chung-Pei Ma, K. Bundy. 2005

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We present the results of near-infrared spectroscopic observations for a sample of 12 star-forming galaxies at 1.0 < z < 1.5, drawn from the DEEP2 Galaxy Redshift Survey. Hβ, [O III], Hα, and [N II] emission line fluxes are measured for these galaxies. Application of the O3N2 and N2 strong-line abundance indicators implies average gas-phase oxygen abundances of 50%-80% solar. We find preliminary evidence of luminosity-metallicity (L-Z) and mass-metallicity (M-Z) relationships within our sample, which spans from MB = -20.3 to -23.1 in rest-frame optical luminosity and from 4 × 109 to 2 × 1011 M☉ in stellar mass. At fixed oxygen abundance, these relationships are displaced from the local ones by several magnitudes toward brighter absolute B-band luminosity and more than an order of magnitude toward larger stellar mass. If individual DEEP2 galaxies in our sample follow the observed global evolution in the B-band luminosity function of blue galaxies between z ~ 1 and z ~ 0 (Willmer et al. 2005), they will fade on average by ~1.3 mag in MB. To fall on local L-Z and M-Z relationships, these galaxies must increase by a factor of 6-7 in M/LB between z ~ 1 and z ~ 0 and by factor of 2 in both stellar mass and metallicity. Such concurrent increases in stellar mass and metallicity are consistent with the expectations of a "closed-box" chemical evolution model, in which the effects of feedback and large-scale outflows are not important. While Ks < 20.0 z ~ 2 star-forming galaxies have similar [N II]/Ha ratios and rest-frame optical luminosities to those of the DEEP2 galaxies presented here, their higher M/LB ratios and clustering strengths indicate that they will experience different evolutionary paths to z ~ 0. Finally, emission-line diagnostic ratios indicate that the z > 1 DEEP2 galaxies in our sample are significantly offset from the excitation sequence observed in nearby H II regions and SDSS emission-line galaxies. This offset implies that physical conditions are different in the H II regions of distant galaxies hosting intense star formation, and may affect the chemical abundances derived from strong-line ratios for such objects.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

• The origin of the galaxy mass-metallicity relation and implications for galactic outflows (2007, background): “…metallicities across five decades in stellar mass. Finally, the MZR is observed to evolve slowly such that galaxies of a given stellar mass are only moderately more enriched today as compared to in the early Universe (Shapley et al. 2005; Savaglio et al. 2005; Erb et al. 2006; Berger et al. 2006).”
• Dissipation and Extra Light in Galactic Nuclei. I. Gas-Rich Merger Remnants (2008, background): “…well with those observed in local disks of the same stellar mass (for stellar masses 0.1–1 M , where most of our sample lies, observations imply typical disk gas fractions 0.2 at z ¼ 0 to 0.3 at z ¼ 1, with a factor 2 intrinsic scatter at both redshifts; Bell & de Jong 2000; Shapley et al. 2005).”
• Emission-line diagnostics of low-metallicity active galactic nuclei (2006, methodology): “If the Shapley et al. (2005) and Erb et al. (2006) galaxies are composite AGN/starforming galaxies, this may imply that low metallicity AGN are more common at high redshifts.”
• THE MOSDEF SURVEY: MASS, METALLICITY, AND STAR-FORMATION RATE AT z ∼ 2.3 (2014, background): “There is mounting evidence in the literature that high-redshift star-forming galaxies have markedly different emission line ratios from those of local starforming galaxies (Shapley et al. 2005; Liu et al. 2008; Hainline et al. 2009; Masters et al. 2014; Steidel et al. 2014).”
• Optical Star Formation Rate Indicators (2005, unknown): “Maier et al. (2005) and Shapley et al. (2005) measure H and H in their respective intermediate-redshift samples, while Savaglio et al. (2005) and Liang et al. (2004a) only measure H and H .”
• PHYSICAL PROPERTIES OF EMISSION-LINE GALAXIES AT z ∼ 2 FROM NEAR-INFRARED SPECTROSCOPY WITH MAGELLAN FIRE (2014, background): “…on average, in galaxies at high redshift, possibly as a result of higher nebular electron densities, harder ionizing radiation fields, different gas volume filling factors, or some combination of these (Shapley et al. 2005; Brinchmann et al. 2008b; Shirazi et al. 2013; Kewley et al. 2013a,b).”
• A fundamental relation between mass, SFR and metallicity in local and high redshift galaxies (2010, background): “…182 objects, having published values of emission line fluxes, M?, and dust extinction: 0.5<z<0.9 (Savaglio et al. 2005, GDDS galaxies), 1.0<z<1.6 (Shapley et al. 2005; Liu et al. 2008; Wright et al. 2009; Epinat et al. 2009), and 2.0<z<2.5 (Law et al. 2009; Lehnert et al. 2009; Förster…”
• The Mass-Metallicity Relation at z≳2 (2006, methodology): “Starforming galaxies at z ∼ 2 have lower average mass-tolight ratios M/L than local galaxies, and the variation in M/L at a given rest-frame optical luminosity can be as much as a factor of ∼ 70 (Shapley et al. 2005b).”
• STRONG NEBULAR LINE RATIOS IN THE SPECTRA of z ∼ 2–3 STAR FORMING GALAXIES: FIRST RESULTS FROM KBSS-MOSFIRE (2014, methodology): “…and 21 are good fits, and there is no obvious sign that 30 The results are insensitive to the exact value adopted; 0.16 dex is the median estimated uncertainty in the stellar mass estimates for similar galaxy samples (Shapley et al. 2005b; Erb et al. 2006c) either of the MZRs flattens at high M∗.”
• THE MASS–METALLICITY AND LUMINOSITY–METALLICITY RELATIONS FROM DEEP2 AT z ∼ 0.8 (2010, methodology): “However, many recent investigations have provided compelling evidence for evolution of the LZ relation over cosmological times (Kobulnicky & Koo 2000; Pettini et al. 2001; Kobulnicky et al. 2003; Kobulnicky & Kewley 2004; Maier et al. 2004; Shapley et al. 2004, 2005).”
• Ionization state of inter-stellar medium in galaxies: evolution, SFR-M * -Z dependence, and ionizing photon escape (2013, background): “In contrast, high-z galaxies depart from the local star-forming sequence towards higher [O III]/Hβ ratio (e.g. Shapley et al. 2005; Erb et al. 2006; Liu et al. 2008; Hainline et al. 2009; Finkelstein et al. 2009; Yabe et al. 2012).”
• On Extending the Mass-Metallicity Relation of Galaxies by 2.5 Decades in Stellar Mass (2006, background): “…(see, e.g., Kobulnicky & Zaritsky 1999; Kobulnicky et al. 2003; Liang et al. 2004; Kobulnicky & Kewley 2004; Shapley et al. 2004; Gallazzi et al. 2005; Hoyos et al. 2005; Maier et al. 2005; Savaglio et al. 2005; Shapley et al. 2005; Erb et al. 2006; Lamareille et al. 2006; Liang et al. 2006).”
• THE COSMIC BPT DIAGRAM: CONFRONTING THEORY WITH OBSERVATIONS (2013, methodology): “We supplement the zCOSMOS data with 6 galaxies at z ∼ 0.8 from the DEEP2 Galaxy Redshift Survey (Davis et al. 2003; Faber et al. 2007) observed by Shapley et al. (2005) and Liu et al. (2008).”
• GRB hosts through cosmic time - VLT/X-Shooter emission-line spectroscopy of 96 γ-ray-burst-selected galaxies at 0.1 (2015, background): “A similar offset is well-observed in many high redshift galaxy samples (e.g., Shapley et al. 2005; Kriek et al. 2007; Steidel et al. 2014) and also for galaxies hosting H-poor superluminous supernovae (Leloudas et al. 2015).”
• REST-FRAME OPTICAL SPECTRA OF THREE STRONGLY LENSED GALAXIES AT z ∼ 2 (2009, methodology): “Shapley et al. (2005) report an aperture-corrected mean SFR for a local sample of SDSS galaxies of 2.0 M⊙ yr −1.”
• THE MOSDEF SURVEY: ELECTRON DENSITY AND IONIZATION PARAMETER AT z ∼ 2.3 (2015, background): “…work has been produced showing that galaxies at z ∼ 1− 2 display certain emission line ratios that are atypical of local star-forming galaxies (e.g., Shapley et al. 2005; Erb et al. 2006; Liu et al. 2008; Hainline et al. 2009; Holden et al. 2014; Nakajima & Ouchi 2014; Steidel et al. 2014;…”
• SDSS-IV MaNGA : the impact of diffuse ionized gas on emission-line ratios, interpretation of diagnostic diagrams and gas metallicity measurements (2016, background): “…redshift star-forming galaxies are systematically offset towards higher [O iii]/Hβ on the BPT diagram relative to the local star-forming galaxy locus (Shapley et al. 2005; Erb at U niversity of Portsm outh L ibrary on January 6, 2017 http://m nras.oxfordjournals.org/ D ow nloaded from Figure 28.”