Age Determination of Elliptical Galaxies using H γ Profile
| Project/Area Number | 13640230 |
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| Research Category |
Grant-in-Aid for Scientific Research (C)
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| Allocation Type | Single-year Grants |
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| Section | 一般 |
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| Research Field |
Astronomy
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| Research Institution | National Astronomical Observatory |
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Principal Investigator |
ARIMOTO Nobuo National Astronomical Observatory, Optical and Infrared Astronomy Division, Professor, 光赤外研究部, 教授 (60242096)
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| Project Period (FY) |
2001 – 2003
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| Project Status |
Completed(Fiscal Year 2003)
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| Budget Amount *help |
¥4,000,000 (Direct Cost : ¥4,000,000)
Fiscal Year 2003 : ¥900,000 (Direct Cost : ¥900,000)
Fiscal Year 2002 : ¥1,400,000 (Direct Cost : ¥1,400,000)
Fiscal Year 2001 : ¥1,700,000 (Direct Cost : ¥1,700,000)
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| Keywords | Elliptical Galaxies / Galaxy Formation / Galaxy Evolution / Age of Galaxies / Chemical Abundance of Galaxies / 銀河道化 / 星の種族 / 星の生成史 / 銀河の化学進化 / 恒星スペクトル / 星の種族構造 |
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| Research Abstract |
This research aimed to reveal the formation epoch of elliptical galaxies by measuring their spectroscopic ages. We have taken spectra of 27 elliptical galaxies (13 in the field and group of galaxies and 14 in the Virgo cluster of galaxies) of extremely high quality with Subaru (NAOJ), WTT(Spain, UK) and NTT(ESO) telescopes and have measured their ages and chemical abundances by using the Hg profile method, which we have developed by ourselves. The Hg profile method is a quite efficient approach to disentangle age and metallicity effects in galaxy spectra and has been appreciated a lot since it was proposed by Vazdekis & Arimoto (1999). This study is the first one that applies the Hg profile method to a significantly large number of galaxy samples. In this study, we have made it clear how the ages and metallicities of elliptical galaxies depend on galaxy mass, luminosity, and the environment. The spatial distribution of age and metallicity within a galaxy has also been studied. Our resu
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lts show that 1)massive elliptical galaxies in cluster environment are uniformly old (<10 Gyrs), while those in the field show a scatter in ages spanning from 6 Gyrs to 10 Gyrs old. This indicates that some of filed ellipticals had experienced long lasting star formation until rather recently. 2)Dwarf elliptical galaxies show wide scatter in their ages, from 3 Gyrs to 10 Gyrs old, independent of where they locate. This suggests a rather complicated history of star formation in contrast to what has been thought previously. 3)Mg/Fe ratio of elliptical galaxies shows strong correlation with galaxy mass,; ie., moremassive galaxies tend to have smaller Mg/Fe ratio, suggesting shorter star formation period in more massive elliptical galaxies. 4) In a dwarf elliptical M32 (a companion galaxy of M31 spiral galaxy), the stellar age decreases towards galaxy centre and Mg/Fe ratio too. This is a strong evidence for a long lasting star formation at the galaxy center due to perhaps dissipative gas infall.
In summary we could say that although it is true that formation of elliptical galaxies shows wide variety (in particular among dwarf ellipticals) more massive galaxies formed earlier in the dense cluster environment. Less
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Research Products
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