“SAMI”的版本间差异
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无编辑摘要 |
无编辑摘要 |
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| （未显示同一用户的5个中间版本） | |||
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* 13 integral field units (IFUs),each with a field of view of 15arcsec |
* 13 integral field units (IFUs),each with a field of view of 15arcsec |
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:12 galaxies and 1 secondary star |
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* each IFU consists of a bundle of 61 optical fibers a high filling factor ~75%) |
* each IFU consists of a bundle of 61 optical fibers a high filling factor ~75%) |
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* installed on the 3.9-m Anglo-Australian Telescope (AAT) |
* installed on the 3.9-m Anglo-Australian Telescope (AAT),1 deg FOV |
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* 370–570 nm with R=1730 in the blue arm, and 625–735 nm with R = 4500 in the red arm. |
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'''SAMI Galaxy survey''' |
'''SAMI Galaxy survey''' |
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:a field and group sample from [[GAMA]] G09, G12 and G15 fields |
:a field and group sample from [[GAMA]] G09, G12 and G15 fields |
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:a cluster sample from a set of eight galaxy clusters. |
:a cluster sample from a set of eight galaxy clusters. |
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:: 数据预期在2018年释放 |
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:: r<19.5 |
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* EDR, 107 galaxies [http://sami-survey.org/edr] |
* EDR, 107 galaxies [http://sami-survey.org/edr] |
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'''光谱处理''' |
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*SAMI的光谱发射线拟合程序LZIFU,Ho et al. (2014) |
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:which utilizes pPXF for stellar template fitting and the MPFIT library (MILES templates) for estimating emission-line properties. |
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2017年3月6日 (一) 05:29的最新版本
Sydney-AAO Multi-object Integral field spectrograph (SAMI)
- 13 integral field units (IFUs),each with a field of view of 15arcsec
- 12 galaxies and 1 secondary star
- each IFU consists of a bundle of 61 optical fibers a high filling factor ~75%)
- installed on the 3.9-m Anglo-Australian Telescope (AAT),1 deg FOV
- 370–570 nm with R=1730 in the blue arm, and 625–735 nm with R = 4500 in the red arm.
SAMI Galaxy survey
- aim: IFS data for 3400 galaxies
- Sample:
- a field and group sample from GAMA G09, G12 and G15 fields
- a cluster sample from a set of eight galaxy clusters.
- 数据预期在2018年释放
- r<19.5
- EDR, 107 galaxies [1]
光谱处理
- SAMI的光谱发射线拟合程序LZIFU,Ho et al. (2014)
- which utilizes pPXF for stellar template fitting and the MPFIT library (MILES templates) for estimating emission-line properties.