Metallicity evolution, metallicity gradients, and gas fractions at z ~ 3.4

By P. Troncoso, R. Maiolino, V. Sommariva, G. Cresci, F. Mannucci, A. Marconi, Massimo Meneghetti, A. Grazian, A. Cimatti, A. Fontana and 2 more. 2013

195 citations recorded by the source corpus.

This work was funded by the Marie Curie Initial Training Network ELIXIR 214227 of the European Commission. We also acknowledge partial support by INAF. Alessandro Marconi acknowledges support from grant PRIN-MIUR 2010-2011 “The dark Universe and the cosmic evolution of baryons: from current surveys to Euclid”.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/7e79f53fdfefc7c395e2e3d4132a4be4ff2ec34b

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In Astronomy and Astrophysics

1. P. Hopkins
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In Instrumentation

1. C. Conroy
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6. R. Dav'e
7. Christopher J. Conselice
8. M. Cappellari

Citations in the corpus

• New fully empirical calibrations of strong-line metallicity indicators in star forming galaxies (2016, background): “E-mail:mcurti@arcetri.astro.it found (e.g Erb 2006; Maiolino et al. 2008; Mannucci et al. 2009; Zahid et al. 2012; Cresci et al. 2012; Troncoso et al. 2014).”
• xCOLD GASS: The Complete IRAM 30 m Legacy Survey of Molecular Gas for Galaxy Evolution Studies (2017, background): “It is also an ideal z = 0 reference point for studies of molecular gas at higher redshifts (e.g. Combes et al. 2013; Troncoso et al. 2014; Seko et al. 2016; Genzel et al. 2015; Tacconi et al. 2017), and provides powerful constraints for theoretical models and numerical simulations (e.g. Lagos et…”
• THE MOSDEF SURVEY: MASS, METALLICITY, AND STAR-FORMATION RATE AT z ∼ 2.3 (2014, background): “We find z ∼ 2.3 star-forming galaxies are ∼ 0.1 dex lower in metallicity for a given M∗ and SFR than the local FMR predicts, in agreement with some high redshift studies (Zahid et al. 2013; Cullen et al. 2014; Troncoso et al. 2014; Wuyts et al. 2014).”
• The galaxy stellar mass function at 3.5 ≤z ≤ 7.5 in the CANDELS/UDS, GOODS-South, and HUDF fields (2015, background): “…a constant temperature and electron density, which is probably a somewhat rough approximation, but nonetheless gives realistic results, as shown in Castellano et al. (2014) for a sample of galaxies at z = 3−4 (taken mainly from the AMAZE sample of Maiolino et al. 2008; and Troncoso et al. 2014).”
• OVERVIEW OF THE SDSS-IV MaNGA SURVEY: MAPPING NEARBY GALAXIES AT APACHE POINT OBSERVATORY (2014, background): “These features have been detected in small samples of galaxies at high redshift (Cresci et al. 2010; Troncoso et al. 2014).”
• The KMOS Redshift One Spectroscopic Survey (KROSS):dynamical properties, gas and dark matter fractions of typical z~1 star-forming galaxies (2016, methodology): “…Shapiro et al. 2008; Förster Schreiber et al. 2009 [Spectroscopic Imaging survey in the Near-infrared with SINFONI, (SINS)]; Gnerucci et al. 2011; Troncoso et al. 2014 [Assessing the Mass-Abundances redshift (Z) Evolution (AMAZE) and Lyman-break galaxies Stellar population and Dynamics (LSD)];…”
• GOODS-HERSCHEL: STAR FORMATION, DUST ATTENUATION, AND THE FIR–RADIO CORRELATION ON THE MAIN SEQUENCE OF STAR-FORMING GALAXIES UP TO z ≃ 4 (2014, background): “…to nicely fit andexplain some recent observations of metallicity and gas masses at high redshift (see, e.g., Ouchi et al. 2013; Tan et al. 2013; Troncoso et al. 2014), should be carefully taken into account when dealing with high redshift sources and deriving more general conclusions on the…”
• THE MOSDEF SURVEY: ELECTRON DENSITY AND IONIZATION PARAMETER AT z ∼ 2.3 (2015, background): “It is well-established that galaxies at z > 1 have lower metallicities than local galaxies at fixed stellar mass (Erb et al. 2006; Maiolino et al. 2008; Belli et al. 2013; Henry et al. 2013; Stott et al. 2013; Cullen et al. 2014; Steidel et al. 2014; Troncoso et al. 2014; Sanders et al. 2015).”
• THE GRISM LENS-AMPLIFIED SURVEY FROM SPACE (GLASS). I. SURVEY OVERVIEW AND FIRST DATA RELEASE (2015, background): “Measurements for a large sample of galaxies over a range of redshift thus provide important constraints on galaxy assembly history (e.g., Troncoso et al. 2014).”
• JWST Census for the Mass–Metallicity Star Formation Relations at z = 4–10 with Self-consistent Flux Calibration and Proper Metallicity Calibrators (2023, methodology): “…we remove these The gray open symbols represent the averages of lower-redshift samples of continuum-selected galaxies ( Nakajima & Ouchi 2014; Troncoso et al. 2014; Sanders et al. 2016; Onodera et al. 2016; Strom et al. 2017 ) and Ly α emitting galaxies ( LAEs; Nakajima & Ouchi 2014; Erb et…”
• A Redshift-independent Efficiency Model: Star Formation and Stellar Masses in Dark Matter Halos at z ≳ 4 (2018, background): “Troncoso et al. (2014) and Onodera et al. (2016) measured the oxygen abundance for star-forming galaxies at z = 3 − 4, finding 12 + log(O/H) ≈ 7.5 − 8.5 with a weak trend in mass (higher mass galaxies have a higher metallicity).”
• GRB hosts through cosmic time - VLT/X-Shooter emission-line spectroscopy of 96 γ-ray-burst-selected galaxies at 0.1 (2015, background): “The predicted [O iii]/[O ii] ratio at z = 3.3 is remarkably similar to the ratio of the composite LBG spectrum at z ∼ 3.5 (Maiolino et al. 2008; Troncoso et al. 2014).”
• Evolution of the dust emission of massive galaxies up to z=4 and constraints on their dominant mode of star formation (2014, background): “For instance, Troncoso et al. (2014) measured a ∼0.5 dex lower normalization at z ∼ 3.4 compared to the functional form of the FMR at low redshift.”
• STRONG NEBULAR LINE RATIOS IN THE SPECTRA of z ∼ 2–3 STAR FORMING GALAXIES: FIRST RESULTS FROM KBSS-MOSFIRE (2014, background): “…Center, MS 211-1, Moffett Field, CA 94035 11 Alfred P. Sloan Foundation Research Fellow Mannucci et al. 2010; Henry et al. 2013; Cullen et al. 2014; Troncoso et al. 2014; Wuyts et al. 2014), samples of high redshift galaxies for which a reasonably complete set of strong lines has been measured…”
• Star formation sustained by gas accretion (2014, background): “The parameterization of the FMR by Mannucci et al. (2010), seems to hold until z < 2, and then it changes substantially at higher redshift (e.g., Mannucci et al. 2010; Yabe et al. 2012; Ly et al. 2014; Troncoso et al. 2014; Cullen et al. 2014).”
• The SINS/zC-SINF Survey of z ∼ 2 Galaxy Kinematics: SINFONI Adaptive Optics–assisted Data and Kiloparsec-scale Emission-line Properties (2018, methodology): “…by the SINS/zC-SINF AO galaxies to mitigate evolutionary effects (e.g. Erb et al. 2006a; Jones et al. 2010a, 2013; E. Wuyts et al. 2014a, 2016; Troncoso et al. 2014; Zahid et al. 2014; Sanders et al. 2015; Leethochawalit et al. 2016), and to results obtained from the same N2 indicator as used…”
• THE UNIVERSAL RELATION OF GALACTIC CHEMICAL EVOLUTION: THE ORIGIN OF THE MASS–METALLICITY RELATION (2014, background): “A relation between stellar mass, metallicity and star formation rate (SFR) is observed in local (Mannucci et al. 2010; Lara-López et al. 2010; Yates et al. 2012; Andrews & Martini 2013) and high redshift galaxies (Zahid et al. 2013b; Yabe et al. 2014; Troncoso et al. 2014).”
• CO excitation of normal star forming galaxies out to $z=1.5$ as regulated by the properties of their interstellar medium (2014, background): “Their metal content is decreasing, with metallicity at fixed stellar mass declining by more than a factor of 2 towardsz = 2 (Erb et al 2006; Maier et al 2014; Steidel et al 2014), and with some hints existing of a much more rapid decrease at higher redshifts (Troncoso et al 2014).”