Integral field spectroscopy with SINFONI of VVDS galaxies

Queyrel, J.; Contini, T.; Montero, E. Pérez; Garilli, B.; Fèvre, O. Le; Kissler-Patig, M.; Épinat, B.; Vergani, D.; Tresse, L.; Amram, P.; Lemoine-Busserolle, Marie

doi:10.1051/0004-6361/200911994

Cited by 34 publications

(50 citation statements)

References 53 publications

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“…In order to estimate gas phase metallicities of distant galaxies, they must have high surface brightnesses in their emission line gas (see Lehnert et al 2009, and references therein ). It is now reasonably well established that the mass-metallicity relation appears to have evolved over the last 10 Gyr (Savaglio et al 2005;Erb et al 2006;Mannucci et al 2009;Rodrigues et al 2008;Halliday et al 2008;Queyrel et al 2009). However, combining the possible limitations in the observations due to surface brightness dimming and the importance of mergers in initiating intense (high surface brightness) starbursts, it may be the determinations of the evolution in metallicity may be strongly influenced by dilution.…”

Section: Discussionmentioning

confidence: 95%

The dilution peak, metallicity evolution, and dating of galaxy interactions and mergers

Montuori¹,

Matteo

Lehnert

et al. 2010

A&A

116

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Strong inflows of gas from the outer disk to the inner kiloparsecs are induced during the interaction of disk galaxies. This inflow of relatively low-metallicity gas dilutes the metallicity of the circumnuclear gas. This process is critical for the galaxy evolution. We have investigated several aspects of the process as the timing and duration of the dilution and its correlation with the induced star formation. We analysed major (1:1) gas-rich interactions and mergers, spanning a range of initial orbital characteristics. Star formation and metal enrichment from SNe are included in our model. Our results show that the strongest trend is between the star formation rate and the dilution of the metals in the nuclear region; i.e., the more intense the central burst of star formation, the more the gas is diluted. This trend comes from strong inflows of relatively metal-poor gas from the outer regions of both disks, which fuels the intense star formation and lowers the overall metallicity for a time. The strong inflows happen on timescales of about 10 8 years or less (i.e., on an internal dynamical time of the disk in the simulations), and the most intense star formation and lowest gas phase metallicities are seen generally after the first pericentre passage. As the star formation proceeds and the merger advances, the dilution reduces and enrichment becomes dominant -ultimately increasing the metallicity of the circumnuclear gas to a level higher than the initial metallicities of the merging galaxies. The "fly-bys" -pairs that interact but do not merge -also cause some dilution. We even see some dilution early in the merger or in the "fly-bys" and thus do not observe a strong trend between the nuclear metallicities and separation in our simulations until the merger is well advanced. We also analyse the O and Fe enrichment of the ISM, and show that the evolution of the α/Fe ratios, as well as the dilution of the central gas metallicity, can be used as a clock for dating the interaction.

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Section: Discussionmentioning

confidence: 95%

The dilution peak, metallicity evolution, and dating of galaxy interactions and mergers

Montuori¹,

Matteo

Lehnert

et al. 2010

A&A

116

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“…The relation between galaxy mass and metallicity, which was first discovered by Lequeux et al (1979) in irregular galaxies, exists for star-forming galaxies both in the nearby universe (Tremonti et al 2004;Lamareille et al 2004) and at high redshifts z ∼ 0.7−3 (Lamareille et al 2006Queyrel et al 2009;Erb et al 2006;Maiolino et al 2008;Mannucci et al 2009). This trend by more massive galaxies toward higher gas-phase metallicity can be explained by This work is based on observations collected at the European Southern Observatory (ESO) Very Large Telescope, Paranal, Chile, as part of the Programs 179.A-0823, 78.A-0177, and 75.A-0318.…”

Section: Introductionmentioning

confidence: 90%

“…Recent observations have suggested that A&A 539, A93 (2012) galaxies involved in merging events show lower nuclear metallicities that are caused by the infall of pristine gas into the nucleus. Merging events could also account for outliers to the mass-metallicity relation (Kewley et al 2006;Michel-Dansac et al 2008;Peeples et al 2009;Queyrel et al 2009;Alonso et al 2010;Montuori et al 2010;Kewley et al 2010).…”

Section: Introductionmentioning

confidence: 99%

MASSIV: Mass Assembly Survey with SINFONI in VVDS

Contini

Kissler-Patig

Épinat³

et al. 2012

A&A

Self Cite

135

166

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Aims. The estimate of radial abundance gradients in high-redshift galaxies allows to constrain their star formation history and their interplay with the surrounding intergalactic medium. Methods. We present VLT/SINFONI integral-field spectroscopy of a first sample of 50 galaxies at z ∼ 1.2 in the MASSIV survey. Using the N2 ratio between the [N ii]6584 and Hα rest-frame optical emission lines as a proxy for oxygen abundance in the interstellar medium, we measured the metallicity of the sample galaxies. We developed a tool to extract spectra in annular regions, leading to a spatially resolved estimate of the oxygen abundance in each galaxy. We were able to derive a metallicity gradient for 26 galaxies in our sample and discovered a significant fraction of galaxies with a "positive" gradient. Using a simple chemical evolution model, we derived infall rates of pristine gas onto the disks. Results. Seven galaxies display a positive gradient at a high confidence level. Four out of these are interacting, and one is a chain galaxy. We suggest that interactions might be responsible for shallowing and even inverting the abundance gradient. We also identify two interesting correlations in our sample: a) galaxies with higher gas velocity dispersion have shallower/positive gradients; and b) metal-poor galaxies tend to show a positive gradient, whereas metal-rich ones tend to show a negative one. This last observation can be explained by the infall of metal-poor gas into the center of the disks. We address the question of the origin of this infall under the influence of gas flows triggered by interactions and/or cold gas accretion. All the data published in this paper are publicly available at the time of publication following this link: http://cosmosdb.lambrate.inaf.it/VVDS-SINFONI.

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“…For the explanation of the N/O redshift evolution, Queyrel et al (2009), Masters et al (2014), and Yabe et al (2015) have estimated N/O ratios at z ∼ 2, and have claimed the increase of N/O at fixed O/H. The excessive N/O ratios at fixed O/H may be caused by the decrease of O/H due to the pristine gas inflow into galaxies with rich nitrogen gas produced by the secondary nucleosynthesis, while Wolf-Rayet (WR) stars can produce the nitrogen in a time scale shorter than the oxygen production time scale in supernovae (Andrews & Martini 2013).…”

Section: Introductionmentioning

confidence: 99%

Evolution of N/O abundance ratios and ionization parameters from z ∼ 0 to 2 investigated by the direct temperature method

Kojima

Ouchi

Nakajima

et al. 2017

Publications of the Astronomical Society of Japan

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We present N/O abundance ratios, ionization parameters q ion , and oxygen abundance O/H for a total of 41 galaxies (11 individual galaxies and a 30-galaxy stack) including Lyα emitters and Lyman break galaxies at z ∼ 2, and investigate galaxy evolution from z ∼ 0 to 2 in conjunction with 208,529 local SDSS galaxies and 9 green pea galaxies (GPs). In contrast with most of the recent studies, we obtain the N/O ratio, q ion , and O/H measurements by direct T e methods with [O III] λ4363 and O III] λ1665 lines. Based on these reliable measurements, we find that there exist z ∼ 2 galaxies with an excess of N/O falling beyond the local average of N/O-O/H relation, while the majority of the z ∼ 2 galaxies have the N/O ratios nearly comparable with z ∼ 0 galaxies in the N/O-stellar mass relation. Our galaxies place the upper limit of N/O ratio log(N/O) ≤ −1.26 on average, suggesting that the N/O ratio evolves, if at all, by < 0.17 dex. Exploiting our reliable measurements free from the N/O-q ion -O/H degeneracies, we identify, for the first time, that z ∼ 2 galaxies with offsets in the BPT diagram indicate either 1) only an N/O excess, 2) only a q ion excess, or 3) both N/O and q ion excesses. We argue that the BPT offsets at z ∼ 2 are not made by one of 1)-3) galaxy populations alone, but the composite of 1)-3) populations. We confirm that these 1)-3) populations also exist at z ∼ 0, such as GPs and SDSS low-mass and high-SFR galaxies (LMHSs).

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Integral field spectroscopy with SINFONI of VVDS galaxies

Cited by 34 publications

References 53 publications

The dilution peak, metallicity evolution, and dating of galaxy interactions and mergers

The dilution peak, metallicity evolution, and dating of galaxy interactions and mergers

MASSIV: Mass Assembly Survey with SINFONI in VVDS

Evolution of N/O abundance ratios and ionization parameters from z ∼ 0 to 2 investigated by the direct temperature method

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