Chemical gradients in the Milky Way from the RAVE data

Boeche, C.; Siebert, A.; Piffl, Tilmann; Just, A.; Steinmetz, Matthias; Sharma, Sanjib; Kordopatis, G.; Gilmore, G.; Chiappini, Cristina; Williams, M.; Grebel, Eva K.; Bland-Hawthorn, Joss; Gibson, Brad K.; Munari, U.; Siviero, A.; Bienaymé, O.; Navarro, Julio F.; Parker, Quentin A.; Reid, Warren A.; Seabroke, G. M.; Watson, Fred; Wyse, Rosemary F. Ġ.; Zwitter, T.

doi:10.1051/0004-6361/201322085

Cited by 82 publications

(117 citation statements)

References 73 publications

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“…15, we show results for the radial metallicity gradient and the MDF as a function of maximum height above the plane, for both the HQ and the Gold samples (for a complementary work, extending to more inner Galactocentric distances -but without kinematics -see Hayden et al 2013). In the recent paper by Boeche et al (2013b), the authors compare the gradients obtained from a RAVE dwarf sample with those of the Geneva-Copenhagen survey (similar to our approach, the authors provide their results with respect to the orbital parameter space (R g , z max ) 22 , but only for three bins of z max ). For comparison, their results are summarised in Table 3, along with our measured values.…”

Section: Disc Abundance Gradients and Variations Of The Mdf With Heigmentioning

confidence: 98%

Chemodynamics of the Milky Way

Anders

Chiappini

Santiago

et al. 2014

A&A

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Context. The Apache Point Observatory Galactic Evolution Experiment (APOGEE) features the first multi-object high-resolution fiber spectrograph in the near-infrared ever built, thus making the survey unique in its capabilities: APOGEE is able to peer through the dust that obscures stars in the Galactic disc and bulge in the optical wavelength range. Here we explore the APOGEE data included as part of the Sloan Digital Sky Survey's 10th data release (SDSS DR10). Aims. The goal of this paper is to a) investigate the chemo-kinematic properties of the Milky Way disc by exploring the first year of APOGEE data; and b) to compare our results to smaller optical high-resolution samples in the literature, as well as results from lower resolution surveys such as the Geneva-Copenhagen Survey (GCS) and the RAdial Velocity Experiment (RAVE). Methods. We select a high-quality (HQ) sample in terms of chemistry (amounting to around 20 000 stars) and, after computing distances and orbital parameters for this sample, we employ a number of useful subsets to formulate constraints on Galactic chemical and chemodynamical evolution processes in the solar neighbourhood and beyond (e.g., metallicity distributions -MDFs, [α/Fe] vs. [Fe/H] diagrams, and abundance gradients). Results. Our red giant sample spans distances as large as 10 kpc from the Sun. Given our chemical quality requirements, most of the stars are located between 1 and 6 kpc from the Sun, increasing by at least a factor of eight the studied volume with respect to the most recent chemodynamical studies based on the two largest samples obtained from RAVE and the Sloan Extension for Galactic Understanding and Exploration (SEGUE). We find remarkable agreement between the MDF of the recently published local (d < 100 pc) high-resolution high-S/N HARPS sample and our local HQ sample (d < 1 kpc). The local MDF peaks slightly below solar metallicity, and exhibits an extended tail towards [Fe/H] = −1, whereas a sharper cutoff is seen at larger metallicities (the APOGEE sample shows a slight overabundance of stars with metallicities larger than +0.3 with respect to the HARPS sample). Both samples also compare extremely well in an [α/Fe] vs. [Fe/H] diagram. The APOGEE data also confirm the existence of a gap in the abundance diagram. When expanding our sample to cover three different Galactocentric distance bins (inner disc, solar vicinity and outer disc), we find the high-[α/Fe] stars to be rare towards the outer zones (implying a shorter scale-length of the thick disc with respect to the thin disc), as previously suggested in the literature. Finally, we measure the gradients in [Fe/H] and [α/Fe], and their respective MDFs, over a range of 6 < R < 11 kpc in Galactocentric distance, and a 0 < z < 3 kpc range of distance from the Galactic plane. We find a good agreement with the gradients traced by the GCS and RAVE dwarf samples. For stars with 1.5 < z < 3 kpc (not present in the previous samples), we find a positive metallicity gradient and a negative gradient in [α/Fe].

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Section: Disc Abundance Gradients and Variations Of The Mdf With Heigmentioning

confidence: 98%

Chemodynamics of the Milky Way

Anders

Chiappini

Santiago

et al. 2014

A&A

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199

215

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“…Using only stars close to the plane, within |Z| of 300 pc, we derive Δ[Fe/H]/ΔR = −0.068 ± 0.014 dex/kpc or Δ[Fe/H]/ΔR = −0.076 ± 0.010 dex/kpc (stars with ages ≤7 Gyr). Analysing RAVE spectra of disk dwarfs, Boeche et al (2013) found that Δ[Fe/H]/ΔR = −0.065 dex/kpc for Z max < 400 pc. For 300 < Z max < 800 pc, we obtain Δ[Fe/H]/ΔR = −0.114 ± 0.009 dex/kpc.…”

Section: Age-[α/fe] and Age-[fe/h] Relationsmentioning

confidence: 99%

“…Lee et al 2011;Bovy et al 2012b,c;Schlesinger et al 2012;Cheng et al 2012), RAVE (e.g. Boeche et al 2013), and APOGEE (e.g. Anders et al 2014;Hayden et al 2013), as well as smaller samples of stars with high-resolution observations (e.g.…”

Section: Introductionmentioning

confidence: 99%

TheGaia-ESO Survey: radial metallicity gradients and age-metallicity relation of stars in the Milky Way disk

Bergemann

Ruchti

Serenelli

et al. 2014

A&A

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We study the relationship between age, metallicity, and α-enhancement of FGK stars in the Galactic disk. The results are based upon the analysis of high-resolution UVES spectra from the Gaia-ESO large stellar survey. We explore the limitations of the observed dataset, i.e. the accuracy of stellar parameters and the selection effects that are caused by the photometric target preselection. We find that the colour and magnitude cuts in the survey suppress old metal-rich stars and young metal-poor stars. This suppression may be as high as 97% in some regions of the age-metallicity relationship. The dataset consists of 144 stars with a wide range of ages from 0.5 Gyr to 13.5 Gyr, Galactocentric distances from 6 kpc to 9.5 kpc, and vertical distances from the plane 0 < |Z| < 1.5 kpc. On this basis, we find that i) the observed age-metallicity relation is nearly flat in the range of ages between 0 Gyr and 8 Gyr; ii) at ages older than 9 Gyr, we see a decrease in [Fe/H] and a clear absence of metal-rich stars; this cannot be explained by the survey selection functions; iii) there is a significant scatter of [Fe/H] at any age; and iv) [Mg/Fe] increases with age, but the dispersion of [Mg/Fe] at ages >9 Gyr is not as small as advocated by some other studies. In agreement with earlier work, we find that radial abundance gradients change as a function of vertical distance from the plane. The [Mg/Fe] gradient steepens and becomes negative. In addition, we show that the inner disk is not only more α-rich compared to the outer disk, but also older, as traced independently by the ages and Mg abundances of stars.

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“…For example, on global scales they are one of the key parameters in the study of the luminosity-metallicity and massmetallicity relations of galaxies, their evolution with time, and their dependence on environment or star formation rate (e.g., Lequeux et al 1979;Grebel et al 2003;Tremonti et al 2004;Erb et al 2006;Panter et al 2008;Zahid et al 2012;Sánchez et al 2013;Peng & Maiolino 2014;Zahid et al 2014;Izotov et al 2015, to just name a few of the many studies). Local measurements within galaxies reveal the position-dependent metallicity of the chosen tracer population and may show abundance gradients, which in turn hold clues about galaxy evolution (e.g., Searle 1971;Janes 1979;Maciel & Quireza 1999;Harbeck et al 2001;Andrievsky et al 2002;Chen et al 2003;Mehlert et al 2003;Cioni 2009;Haschke et al 2012;Boeche et al 2013Boeche et al , 2014Pilyugin et al 2014Pilyugin et al , 2015.…”

Section: Introductionmentioning

confidence: 99%

New calibrations for abundance determinations in H ii regions

Pilyugin¹,

Grebel²

2016

Mon. Not. R. Astron. Soc.

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Simple relations for deriving the oxygen abundance in H ii regions with intensities of the three strong emission lines R 2 , R 3 , and N 2 (R calibration) or S 2 , R 3 , and N 2 (S calibration) in their spectra are suggested. A sample of 313 reference H ii regions of the counterpart method (C method) is used as calibrating data points. Relations for the determination of nitrogen abundances, the R calibration, are also constructed. We find that the oxygen and nitrogen abundances in high-metallicity H ii regions can be estimated using the intensities of the two strong lines R 2 and N 2 (or S 2 and N 2 for oxygen) only. The corresponding two-dimensional relations are provided. There are considerable advantages of the suggested calibration relations as compared to the existing ones. First, the oxygen and nitrogen abundances estimated through the suggested calibrations agree with the T e -based abundances within ∼ 0.1 dex over the whole metallicity range, i.e., the relative accuracy of the calibration-based abundances is 0.1 dex. Although we constructed distinct relations for high-and low-metallicity objects, the separation between these two can be simply obtained from the intensity of the N 2 line. Moreover, the applicability ranges of the high-and low-metallicity relations overlap for adjacent metallicities, i.e., the transition zone disappears. Second, the oxygen abundances produced by the two suggested calibrations are in remarkable agreement with each other. In fact, the R-based and S -based oxygen abundances agree within ∼0.05 dex in the majority of cases for more than three thousand H ii region spectra.

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Chemical gradients in the Milky Way from the RAVE data

Cited by 82 publications

References 73 publications

Chemodynamics of the Milky Way

Chemodynamics of the Milky Way

TheGaia-ESO Survey: radial metallicity gradients and age-metallicity relation of stars in the Milky Way disk

New calibrations for abundance determinations in H ii regions

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