NICMOS measurements of the near-infrared background

By R. Maiolino, Tohru Nagao, A. Grazian, F. Cocchia, A. Marconi, F. Mannucci, A. Cimatti, A. Pipino, S. Ballero, A. Fontana and 7 more. 2007

690 citations recorded by the source corpus.

We present preliminary results of an ESO-VLT large programme (AMAZE) aimed at determining the evolution of the mass-metallicity relation at z~3 by means of deep near-IR spectroscopy. Gas metallicities and stellar masses are measured for an initial sample of nine star forming galaxies at z~3.3. When compared with previous surveys, the mass-metallicity relation inferred at z~3.3 shows an evolution significantly stronger than observed at lower redshifts. There are also some indications that the metallicity evolution of low mass galaxies is stronger relative to high mass systems, an effect which can be considered as the chemical version of the galaxy downsizing. The mass-metallicity relation observed at z~3.3 is difficult to reconcile with the predictions of some hierarchical evolutionary models. We shortly discuss the possible implications of such discrepancies.

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Citations in the corpus

• BARYONS MATTER: WHY LUMINOUS SATELLITE GALAXIES HAVE REDUCED CENTRAL MASSES (2012, methodology): “However, the feedback model employed in this paper has been shown to match the observed mass – metallicity relation for galaxies as a function of redshift (Brooks et al. 2007; Maiolino et al. 2008), the baryonic Tully-Fisher relationship (Christensen et al. in prep.)”
• Faint high-redshift AGN in the Chandra deep field south: the evolution of the AGN luminosity function and black hole demography (2011, methodology): “A16, page 7 of 22 SFR ∼ 440 M /yr, as estimated from UV SED fitting and oxygen lines (Maiolino et al. 2008).”
• Rest-frame ultraviolet-to-optical spectral characteristics of extremely metal-poor and metal-free galaxies (2011, background): “Alvensleben (2003) and Maiolino et al. (2008) (see also Nagao et al. 2006), respectively.”
• The COSMOS2015 galaxy stellar mass function . Thirteen billion years of stellar mass assembly in ten snapshots (2017, background): “These stellar metallicities have been chosen to encompass the range observed up to z ∼ 4−5 (e.g. Maiolino et al. 2008; Sommariva et al. 2012); they are also in agreement with hydrodynamical simulations (Ma et al. 2016).”
• Ionization state of inter-stellar medium in galaxies: evolution, SFR-M * -Z dependence, and ionizing photon escape (2013, methodology): “Mannucci et al. (2010) use metallicities of z 3 galaxies given by Maiolino et al. (2008) and Mannucci et al. (2009) that are estimated with the local empirical relations of Maiolino et al. (2008).”
• ON THE INTERPLAY BETWEEN STAR FORMATION AND FEEDBACK IN GALAXY FORMATION SIMULATIONS (2014, methodology): “We compare the simulations with observational data of galaxies at z ∼ 0.07 (as inferred by Kewley & Ellison 2008), z ∼ 2.2 (Erb et al. 2006) and z ∼ 3.5, where a uniform calibration of metallicity indicators was used across all redshifts (Maiolino et al. 2008).”
• The metallicity of the long GRB hosts and the fundamental metallicity relation of low-mass galaxies (2010, methodology): “We have used these compilations to measure gas-phase metallicities, using the method described in Maiolino et al. (2008) and Cresci et al. (2010), and expressing it in the same scale as in Nagao et al. (2006), Kewley & Ellison (2008), and Mannucci et al. (2010), where solar metallicity is…”
• THE RELATION BETWEEN STAR FORMATION RATE AND STELLAR MASS FOR GALAXIES AT 3.5 ⩽ z ⩽ 6.5 IN CANDELS (2014, background): “Alvensleben 2003; Maiolino et al. 2008).”
• KECK SPECTROSCOPY OF 3 < z < 7 FAINT LYMAN BREAK GALAXIES: THE IMPORTANCE OF NEBULAR EMISSION IN UNDERSTANDING THE SPECIFIC STAR FORMATION RATE AND STELLAR MASS DENSITY (2012, methodology): “We compute the intensities of the lines of common metallic species from the empirical results of Anders et al. (2003), assuming a gas phase metallicity of Z = 0.2 Z⊙, similar to that measured for galaxies at these redshifts (Maiolino et al. 2008, Jones et al. 2012).”
• An ALMA survey of sub-millimetre Galaxies in the Extended Chandra Deep Field South: the far-infrared properties of SMGs (2013, background): “For example, Maiolino et al. (2008) suggest a mass-metallicity-star formation rate plane of Z=8.90+ 0.47×x with x= log(M⋆)− 0.32 log(SFR)− 10.”
• The progenitors of compact-object binaries: impact of metallicity, common envelope and natal kicks (2018, background): “Our knowledge of the stellar metallicity evolution in the Universe is quite more uncertain than our knowledge of the SFR density evolution (see e.g. Maiolino et al. 2008; Mannucci et al. 2009; Madau & Dickinson 2014 and references therein).”
• Forming a large disc galaxy from a z < 1 major merger (2008, methodology): “Without further adjustments, this scheme has been proven to reproduce the relation between metallicity and stellar mass (Brooks et al. 2007; Maiolino et al. 2008) and the abundance of damped Lyman α systems at z = 3 (Pontzen et al. 2008).”
• An Overview of the Dwarf Galaxy Survey (2013, background): “Hierarchical models put dwarf galaxies forward as crucial building blocks of much larger galaxies, yet there is indication that many dwarf galaxies in our local Universe have stellar populations much younger than their larger cousins (e.g., Maiolino et al. 2008).”
• Towards a more realistic population of bright spiral galaxies in cosmological simulations (2013, background): “Our galaxies follow a significantly steeper relation with higher mass galaxies (M⋆ > 2 × 10 10M⊙) agreeing with Maiolino et al. (2008) and Tremonti et al. (2004) and the lower mass galaxies in better agreement with Andrews & Martini (2013), but on average more metal-poor than all three…”
• THE MOSDEF SURVEY: MASS, METALLICITY, AND STAR-FORMATION RATE AT z ∼ 2.3 (2014, methodology): “Analyses were also performed using the N2 calibration of Maiolino et al. (2008), but these results are omitted from this study as they are very similar to those based on the Pettini & Pagel (2004) N2 calibration.”
• The assembly of ‘normal’ galaxies at z ∼ 7 probed by ALMA (2015, background): “However, high redshift galaxies are characterized by lower metallicity than local galaxies (e.g. Maiolino et al. 2008).”
• SDSS IV MaNGA – metallicity and nitrogen abundance gradients in local galaxies (2017, methodology): “Metallicity is calculated making use of the strong line calibration of Maiolino et al. (2008), based on R23, and Pettini & Pagel (2004), based on O3N2.”
• Host Galaxy Properties and Offset Distributions of Fast Radio Bursts: Implications for Their Progenitors (2020, methodology): “For reference, the mass–metallicity relations from Maiolino et al. (2008) are shown for z∼0.07 (solid) and z∼0.7 (dashed).”
• Star formation and mass assembly in high-redshift galaxies (2009, background): “The observed trend can therefore be related to a metallicity trend, which is natural to expect given the observed mass–metallici y relation from low to high redshifts (Maiolino et al. 2008, and references therein).”