• Title/Summary/Keyword: metallicity

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Investigating the relation between AGN gas metallicity and their host galaxy stellar metallicity using a sample of local Seyfert 1 galaxies

  • Shin, Jae-Jin;Woo, Jong-Hak
    • The Bulletin of The Korean Astronomical Society
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    • v.36 no.2
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    • pp.72.1-72.1
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    • 2011
  • We investigate the relation between AGN gas metallicity and their host galaxy stellar metallicity using a sample of local Seyfert 1 galaxies. Stellar metallicity is measured from stellar absorption lines while AGN gas metallicity is derived from the flux ratios of UV emission lines. We use a high quality spectra obtained from the Lick AGN Monitoring Project, to obtain pure host galaxy spectra based on the spectral decomposition analysis, leading to accurate measurements of the Mg2 (5175) and Fe (5270) indices. In the case of AGN gas metallicity, we measure the ratio of NV1240 to CIV1549 lines using UV spectra from the archival IUE and HST STIS data. We will present the results of metallicity measurements and comparison between AGN and stellar metallicity, and discuss the implications of the results.

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Does the linear conversion between calcium infrared triplet and metallicity of simple stellar populations hold in the whole range of metallicity?

  • Chung, Chul;Yoon, Suk-Jin;Lee, Sang-Yoon;Lee, Young-Wook
    • The Bulletin of The Korean Astronomical Society
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    • v.39 no.2
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    • pp.47.1-47.1
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    • 2014
  • The calcium infrared triplet (CaT) is one of the prominent absorption features in the infrared wavelength regime. Recently, this absorption feature has been getting attention in the prediction of metallicity of stellar populations because of its strong sensitivity to the calcium abundance and metallicity of a star. However, we find that measuring metallicity directly from CaT is very dangerous because the formation mechanism of CaT is very inefficient in the cool stars which are abundant in metal-rich populations. This characteristics of CaT make the CaT-metallicity relation to converge around ~ $8{\AA}$ in the metal-rich regime. Our results suggest that, because of the converging CaT-metallicity relation in the metal-rich regime, the metallicity of simple stellar populations greater than [Fe/H]~-0.5 is unreliable when the linear conversion between CaT and metallicity is applied to derive metallicity. Based on these results, we suggest that CaT is not a good metallicity indicator for the metal-rich stellar populations.

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THE NON-LINEARITY EFFECT ON THE COLOR-TO-METALLICITY CONVERSION OF GLOBULAR CLUSTERS IN NGC 5128

  • KIM, HAK-SUB;YOON, SUK-JIN
    • Publications of The Korean Astronomical Society
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    • v.30 no.2
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    • pp.261-263
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    • 2015
  • The metallicity distribution of globular clusters (GCs) provides a crucial clue for the star formation history of their host galaxy. With the assumption that GCs are generally old, GC colors have been used as a proxy for GC metallicities. Bimodal color distributions of GCs observed in most large galaxies have, for decades, been interpreted as bimodal metallicity distributions, indicating the presence of two populations within a galaxy. However, the conventional view has been challenged by a new theory that non-linear GC color-metallicity relations can cause a bimodal color distribution even from a single-peaked metallicity distribution. Using photometric and spectroscopic data of NGC 5128 GCs in combination with stellar population simulation models, we examine the effect of non-linearity in GC color-metallicity relations on transformation of the color distributions into the metallicity distributions. Although in some colors offsets are present between observations and models for the color-metallicity relations, their overall shape agrees well for various colors. After the offsets are corrected, the observed spectroscopic metallicity distribution is well reproduced via modeled color-metallicity relations from various color distributions having different morphologies. We discuss the implications of our results.

Chemically young AGNs at high redshift

  • Shin, Jaejin;Woo, Jong-Hak;Nagao, Tohru
    • The Bulletin of The Korean Astronomical Society
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    • v.42 no.1
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    • pp.49.3-50
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    • 2017
  • Metallicity is one of the most important properties in understanding galaxy evolution. However, measuring metallicity is limited to low redshift (z<3.5) due to the faintness of the metallicity indicators in normal galaxies. For high redshift universe, active galactic nuclei (AGN) can be used to constrain the host galaxy metallicity. Previous studies investigated AGN metallicity using emission line flux ratios (i.e., NV/CIV and FeII/MgII), finding no evolution up to z~6. Those results might be due to selection effect since previous studies are based on very luminous AGNs. The observed luminosity-metallicity relation of AGNs (e.g., Nagao et al. 2006) suggests that luminous AGNs may be already matured at the observed epoch. Considering the luminosity-metallicty relation, we focused on low luminosity AGNs to find young AGNs (i.e., low metallicity). Through the Gemini/GNIRS observation in 2012A and 2015A (K-GMT GN-2015A-Q-203 PI: Shin, J.), we obtained the Gemini/GNIRS data for 7 high redshift AGNs (3.0

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WASHINGTON CCD PHOTOMETRY OF THE OLD OPEN CLUSTER NGC 1245

  • WEE SUN-OK;LEE MYUNG GYOON
    • Journal of The Korean Astronomical Society
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    • v.29 no.2
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    • pp.181-194
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    • 1996
  • We present a study of the metallicity of the old open cluster NGC 1245 , based on the Washington CCD photometry obtained using the 0.6 m telescope at the Sobaeksan Observatory, Korea. NGC 1245 has been known to be a unique cluster among the known open clusters in the sense that the previous metallicity estimates for this cluster are much larger $(by\;\sigma)$ than the value expected from the radial metallicity gradient of the old open clusters in Our galaxy. We have estimated the metallicity of the cluster red giants using the four color-color diagrams, obtaining a value for the mean metallicity of $[Fe/H] = -0.04\pm0.05$ dex. The total error including the error of the metallicity calibration, 0.15 dex, is 0.16 dex. The metallicity estimate of NGC 1245 we have obtained in this study is smaller than previous estimates, and is consistent with the radial metallicity gradient of the old open clusters, showing that the mean metallicity of NGC 1245 is not abnormally high. The reddening, distance, and age of the cluster have also been derived using the isochrones based on the convective overshooting models: the reddening $E(B-V) = 0.28\pm0.03$; the distance $d = 2.5\pm0.2 kpc$ (the corresponding galactocentric distance is RGC = 10.7 kpc, and the distance from the galactic plane is z = -0.4 kpc); and the age $t = 1.1\pm0.1 Gyrs$.

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Investigating the Non-linearity Effect on the Color-to-Metallicity Conversion of Globular Clusters

  • Kim, Hak-Sub;Yoon, Suk-Jin
    • The Bulletin of The Korean Astronomical Society
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    • v.39 no.2
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    • pp.62.1-62.1
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    • 2014
  • Metallicity distribution of globular clusters (GCs) provides an important clue for star formation history of their host galaxy. With an assumption that GCs are generally old, GC colors have been used as a proxy of GC metallicities. Bimodal GC color distributions observed in most large galaxies have, for decades, been interpreted as bimodal metallicity distributions, indicating the presence of two populations within a galaxy. However, the conventional view has been challenged by a new theory that non-linear GC color-metallicity relations (CMRs) can cause a bimodal color distribution even from a single-peaked metallicity distribution. Using the photometric and spectroscopic data of NGC 5128 GCs in combination with stellar population simulation models, we examine the effect of non-linearity in GC CMRs on the transformation of GC color distributions into metallicity distributions. Although, in some colors, offsets are present between observations and models in the CMRs, their overall shape agrees well for various colors. After the offsets are corrected, the observed spectroscopic metallicity distribution is well reproduced via modeled CMRs from various color distributions having different morphologies. On the other hand, the linearly converted metallicity distributions from GC colors show a significant discrepancy with the observed spectroscopic metallicity distribution. We discuss the implications of our results.

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The first of its kind metallicity map of the Large Magellanic Cloud

  • Choudhury, Samyaday;Subramaniam, Annapurni;Cole, Andrew A.
    • The Bulletin of The Korean Astronomical Society
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    • v.41 no.2
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    • pp.30.1-30.1
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    • 2016
  • We have estimated a metallicity map of the Large Magellanic Cloud (LMC) using the Magellanic Cloud Photometric Survey (MCPS) and Optical Gravitational Lensing Experiment (OGLE III) photometric data. This is a first of its kind, high-spatial resolution map of metallicity up to a radius of $4^{\circ}-5^{\circ}$, derived using large area photometric data and calibrated using spectroscopic data of Red Giant Branch (RGB) stars. The RGB is identified in the V, (V - I) colour- magnitude diagrams of small subregions of varying sizes in both data sets. The slope of the RGB is used as an indicator of the mean metallicity of a subregion, and it is calibrated to metallicity using spectroscopic data for field and cluster red giants in selected subregions. The mean metallicity of the LMC is found to be [Fe/H] = -0.37 dex (${\sigma}[Fe/H]=0.12$) from MCPS data, and [Fe/H] = -0.39 dex (${\sigma}[Fe/H]=0.10$) from OGLE III data. The bar is found to have an uniform and higher metallicity compared to the disk, and is indicative of an active bar in the past. Both the data sets suggest a shallow radial metallicity gradient up to a radius of 4 kpc ($-0.049{\pm}0.002$ dex kpc-1 to $-0.066{\pm}0.006$ dex kpc-1). This metallicity gradient of the LMC disk, though shallow, resembles the gradient seen in spiral galaxies, and similar to that found in our Galaxy.

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METALLICITY DETERMINATION FOR A GLOBULAR CLUSTER BY SPECTRAL INDICES

  • LEE SANG-GAK
    • Journal of The Korean Astronomical Society
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    • v.29 no.2
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    • pp.157-170
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    • 1996
  • In order to determine the metallicity of a globuar cluster, M3,by using the spectral indices, a kind of index grid has been establshed by stars in globular clusters, M3, M15, M71 and old open cluster, NGC 188. The indices were measured from the medium resolution spectra of about $2{\AA}$. The summed indices were used to determine metallicity in order to increase signals. It is found that the core depth index is measured more accurately and leads result more accurate than the pseudo-equivalent width index. This method can be further improved by including many more calibration globular clusters of various metallicity to make finer grids. By this method, the metallicity of M3 is determined as $[Fe/H] = -1.46\pm0.15$.

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Measuring gas metallicity of local AGNs using UV spectra

  • Shin, Jae-Jin;Woo, Jong-Hak
    • The Bulletin of The Korean Astronomical Society
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    • v.37 no.1
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    • pp.50.1-50.1
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    • 2012
  • As a tracer of star formation history, metallicity provides crucial information for understanding galaxy evolution. In the case AGN, gas metallicity is often derived from the flux ratio of UV emission lines, i.e., NV1240 and CIV1549. To investigate the dependence of metallicity on AGN luminosity, black hole mass, and accretion rate, we measure NV1240 and CIV1549 line fluxes and derive gas metallicity of a sample of 73 local Seyfert 1 galaxies and QSOs, using archival UV spectra obtained with the HST and IUE. In this work, we will present the metallicity of local AGN and its relation with AGN properties.

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THE CHEMICAL PROPERTIES OF PG QUASARS

  • Shin, Jaejin;Woo, Jong-Hak;Nagao, Tohru
    • The Bulletin of The Korean Astronomical Society
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    • v.37 no.2
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    • pp.74.2-74.2
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    • 2012
  • Metallicity is an important tracer of star formation in galaxy evolution. Based on the flux ratios of broad emission lines, AGN metallicity has shown a correlation with AGN luminosity. However, it is not clear what physical parameter drives the observed correlation. Using a sample 69 Palomar-Green QSOs at low-z (z<0.5), we determine BLR gas metallicity from emission line flux ratios, i.e., N V1240/C IV1549, (Si IV1398+O IV1402)/C IV1549 and N V1240/He II1640 based on the UV spectra from the HST and IUE archives. We compare BLR gas metallicity with various AGN properties, i.e., black hole mass, AGN luminosity and Eddington ratio, in order to investigate physical connection between metal enrichment and AGN activity. In contrast to high-z QSOs, which show the correlation between metallicity and black hole mass, we find that the metallicity of low-z QSOs correlates with Eddington ratio, but not with black hole mass, suggesting that metallicity enrichment mechanism is different between low-z and high-z.

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