The Metallicity Distribution of Distant F and G Type Stars in the CFHT Legacy Survey Deep Field

Karataş, Yüksel; Kilic, Mukremin; Güneş, Orhan; Limboz, F.

doi:10.1071/as08014

Cited by 4 publications

(5 citation statements)

References 15 publications

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“…The mean metallicity in interval 5 < r ≤ 8 kpc is about −1.0 and smoothly decreases from −0.6 to −0.8 in interval 2.5 < r ≤ 5 kpc. Our results are consistent with the results of Siegel et al (2009) and Karatas et al (2009). Siegel et al find a monometallic thick disc and halo with abundances of [Fe/H] =−0.8 and −1.4 respectively.…”

Section: Metallicity Distributionsupporting

confidence: 93%

“…The mean metallicity in intervals 5 < r 8 kpc is about −1.0 and the mean metallicity smoothly decreases from −0.6 to −0.8 in intervals 2.5 < r 5 kpc. Our results are consistent with the results of Siegel et al (2009) and Karatas et al (2009) As shown in Fig. 5, at larger distance, r > 10 kpc, compared to the typical error bars, the mean metallicity distributions variation with Galactic longitude is almost flat.…”

Section: Metallicity Variation With Galactic Longitudesupporting

confidence: 92%

“…Accurate determination of the properties of components of the Milky Way requires surveys with sufficient sky coverage to assess the overall geometry (De Jong et al 2010). Most previous investigations of the Galactic metallicity distribution use only one or a few selected line‐of‐sight directions (Du et al 2004; Siegel et al 2009; Karatas et al 2009). In this paper, the BATC photometry survey presented 21 intermediate‐latitude fields in multiple directions.…”

Section: Observations and Datamentioning

confidence: 99%

See 2 more Smart Citations

The stellar metallicity distribution in intermediate-latitude fields with BATC and SDSS data

Peng¹,

Du²,

Wu³

2012

Monthly Notices of the Royal Astronomical Society

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Based on Beijing–Arizona–Taiwan–Connecticut (BATC) and Sloan Digital Sky Survey (SDSS) photometric data, we adopt the spectral energy distribution (SED) fitting method to evaluate the metallicity distribution for ∼40 000 main‐sequence stars in the Galaxy. According to the derived photometric metallicities of these sample stars, we find that the metallicity distribution shifts from metal‐rich to metal‐poor with the increase of distance from the Galactic Centre. The mean metallicity is about −1.5 ± 0.2 dex in the outer halo and −1.3 ± 0.1 dex in the inner halo and smoothly decreases from −0.4 to −0.8 in the interval 0 < r≤ 5 kpc. A fluctuation in mean metallicity with Galactic longitude can be found in the interval 4 < r≤ 8 kpc. There is a vertical abundance gradient d[Fe/H]/dz∼−0.21 ± 0.05 dex kpc−1 for the thin disc (z≤ 2 kpc). At a distance 2 < z≤ 5 kpc, where thick‐disc stars dominate, the gradient is about −0.16 ± 0.06 dex kpc−1; this can be interpreted as a mixture of stellar populations with different mean metallicities at all z levels. The vertical metallicity gradient is −0.05 ± 0.04 dex kpc−1 for the halo (z > 5 kpc), so there is little or no metallicity gradient in the halo.

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Section: Metallicity Distributionsupporting

confidence: 93%

Section: Metallicity Variation With Galactic Longitudesupporting

confidence: 92%

Section: Observations and Datamentioning

confidence: 99%

See 1 more Smart Citation

The stellar metallicity distribution in intermediate-latitude fields with BATC and SDSS data

Peng¹,

Du²,

Wu³

2012

Monthly Notices of the Royal Astronomical Society

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“…Remarkably, their results would be consistent with the complete absence of a thick disc in the Milky Way or its reduction to the metal‐weak thick disc described by Norris (1987). Karataş et al (2009) have also recently analysed ugriz photometry from the Canada‐France‐Hawaii Telescope Legacy Survey Data Release 4 (CFHTLS DR4). In contrast to other studies, they find a vertical abundance gradient in the halo.…”

Section: Introductionsupporting

confidence: 67%

Metallicities and ages of stellar populations at a high Galactic latitude field

Siegel¹,

Karataş²,

Reid³

2009

Monthly Notices of the Royal Astronomical Society

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We present an analysis of UBVRI data from the selected area SA 141. By applying recalibrated methods of measuring ultraviolet excess (UVX), we approximate abundances and absolute magnitudes for 368 stars over 1.3 deg2 out to distances over 10 kpc. With the density distribution constrained from our previous photometric parallax investigations and with sufficient accounting for the metallicity bias in the UVX method, we are able to compare the vertical abundance distribution to those measured in previous studies. We find that the abundance distribution has an underlying uniform component consistent with previous spectroscopic results that posit a monometallic thick disc and halo with abundances of [Fe/H]=−0.8 and −1.4, respectively. However, there are a number of outlying data points that may indicate contamination by more metal‐rich halo streams. The absence of vertical abundance gradients in the Galactic stellar populations and the possible presence of interloping halo streams would be consistent with expectations from merger models of Galaxy formation. We find that our UVX method has limited sensitivity in exploring the metallicity distribution of the distant Galactic halo, owing to the poor constraint on the UBV properties of very metal‐poor stars. The derivation of metallicities from broad‐band UBV photometry remains fundamentally sound for the exploration of the halo but is in need of both improved calibration and superior data.

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“…Accurate determination of the properties of the components of the Galaxy requires surveys with sufficient sky coverage to assess the overall geometry (de Jong et al 2010). Most previous investigations about the Galactic metallicity distribution used only one or a few fields along the lines-of-sight (Du et al 2004;Siegel et al 2009;Karatas et al 2009). The fields used in this paper are toward different directions, the Galactic center, the anticentre at median and high latitudes, 20 • < |b| < 60 • .…”

Section: Batc Survey and Data Reductionmentioning

confidence: 99%

The stellar metallicity distribution of the Galaxy from the BATC survey

Peng

Du²,

et al. 2013

Proc. IAU

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Abstract. Using ∼ 2200 BATC main sequence (MS) stars which include SDSS stellar atmospheric parameters, we develop the polynomial photometric calibration method to evaluate the stellar effective temperature and metallicity for BATC data. This calibration method has been applied to about 160 000 MS stars. The mean stellar metallicity smoothly decreases from −0.65 to −0.78 dex in the interval 0.5 < |Z| 2 kpc. Metallicity distributions in the halo and the thick disk seem invariant with the distance from the Galactic plane.Keywords. Galaxy: disk -Galaxy: halo-Galaxy: metallicity -Galaxy: formation. The metallicity distributionBased on the stellar atmospheric parameters from SDSS spectra for ∼ 2200 MS stars which were also observed in the BATC photometric system, we develop the polynomial photometric calibration method to evaluate the stellar effective temperature and metallicity for BATC photometric data. This calibration method has been applied to about 160 000 MS stars from 67 BATC observed fields. Color index and magnitude are used to choose the MS stars.There is a peak in the stellar metallicity distribution at about −1.5 in the interval 5 < |Z| 14 kpc which corresponds to the halo. The halo metallicity distribution seems invariant with the distance from the plane while the mean thin disk (0.5 < |Z| 2 kpc) metallicity smoothly decreases from −0.65 to −0.78 dex. There is a mean vertical metallicity gradient d[Fe/H]/dz = −0.1 dex kpc −1 for the thin disk stars. The mean vertical gradient about −0.03±0.02 dex kpc −1 for the halo is agreement with the previous work (Du et al. 2006;Peng et al. 2012). In the interval 2 < |Z| 5 kpc, there is a mixture of halo stars and thick disk stars. The peak of the metallicity distribution for the thick disk is about −0.7 dex. Stars with [Fe/H] > −1 and 2 < |Z| 5 kpc are selected to determine the metallicity gradient for the thick disk. A vertical metallicity gradient ∼ −0.03±0.02 dex kpc −1 is found in the thick disk. We believe that the possible cutoff of the thick disk stars is about 5 kpc above and below the Galactic plane which is consistent with the result of the Ivezic et al. (2008). At any distance interval, the variation of the mean metallicity distributions with Galactic longitude is almost flat.

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The Metallicity Distribution of Distant F and G Type Stars in the CFHT Legacy Survey Deep Field

Cited by 4 publications

References 15 publications

The stellar metallicity distribution in intermediate-latitude fields with BATC and SDSS data

The stellar metallicity distribution in intermediate-latitude fields with BATC and SDSS data

Metallicities and ages of stellar populations at a high Galactic latitude field

The stellar metallicity distribution of the Galaxy from the BATC survey

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