“星系巡天”的版本间差异
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'''这里主要是光学的，其它波段参考[[Multi-wavelength]]''' |
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==综合== |
==综合== |
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[[SDSS |
[[SDSS]] |
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[[SDSS IV]] |
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==测光巡天== |
==测光巡天== |
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[[AEGIS]]:2007 |
[[AEGIS]]:2007 |
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[[ |
[[AGES]] |
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[[ |
[[ALHAMBRA]] |
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[[CANDLES]] |
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[[CLAUDS]] |
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[[CFHTLS]] |
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[[COSMOS]] |
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[[文件:Survey comparison.png|缩略图|Survey_comparison]] |
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[[DES]] |
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[[HSC-SSP]] |
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[[GASS]] |
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[[MGC]] |
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[[VIKING]] |
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[[KIDS]] |
[[KIDS]] |
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[[ |
[[UKIDSS]] |
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[[Pan-STAR]] |
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[[SERVS]] |
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[[SkyMapper]] |
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[[VIDEO]] |
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[[J-PLUS]] |
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[[SCUSS]] |
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[[巡天仿真]] |
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==红移巡天== |
==红移巡天== |
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[[VIPERS]] |
[[VIPERS]] |
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[[SHELS]] |
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[[GAMA]] |
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[[DEEP2]] |
[[DEEP2]] |
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[[VVDS]] |
[[VVDS]] |
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[[VUDS]] |
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[[LEGA-C]] |
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[[VANDELS]] |
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===大望远镜=== |
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*PFS |
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*CFHT MSE |
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:10m |
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==IFS== |
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*[[CALIFA]] |
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*[[ATLAS3D]] |
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*[[MaNGA]]: 同时17个源 |
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*[[SAMI]]: 同时观测12个源 |
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*[[MASSIVE]] galaxy survey [Ma et al. 2014] |
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===VLT上的两个IFS终端=== |
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*MUSE |
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:*a giant IFS on VLT wth 1 arcmin FoV, 0.2" spaxel, wide simultaneous wavelength coverage (4650 − 9300Å), relatively high spectral resolution (R ∼ 3000), and high throughput (35% end-to-end). |
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:*The concept of MUSE foresees the splitting of the adaptive optics corrected field of view in 24 sub-fields. Each of these sub-fields is fed into a spectrograph (called Integral Field Unit, IFU). An image slicer in front of each IFU serves as entrance slit, thus producing a spatially resolved spectrum of the full sub-field. |
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*KMOS |
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:The K-band Multi Object Spectrograph (KMOS). IFS in the near-infrared bands for 24 targets simultaneously. |
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:14x14 spectra with ~1000 Nyquist-sampled spectral resolution elements for each of the 24 independent sub-fields. |
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:Each IFU has a square field of view of 2.8 x 2.8 arcsec;ensures uniform spatial sampling of 0.2 x 0.2 arcsec whilst maintaining Nyquist sampling (~2 pixel) |
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===[[JWST]]上的NIRspec=== |
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*NIRSpec is equipped with an integral field unit optimized for the spectroscopic study of complex extended objects. It will provide 900 spectra per exposure over a field of view of 3 x 3 arcminutes.（0.6-5mu） |
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==Keck上的终端== |
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*MOSFIRE |
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:Multi-Object Spectrometer for Infra-Red Exploration |
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===100%filling IFUs=== |
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:SAURON:33"x4" |
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:WiFeS:38"x25" |
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==星系团== |
==星系团== |
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2024年6月18日 (二) 02:18的最新版本
这里主要是光学的，其它波段参考Multi-wavelength
综合
测光巡天
AEGIS:2007
红移巡天
大望远镜
- PFS
- CFHT MSE
- 10m
IFS
VLT上的两个IFS终端
- MUSE
- a giant IFS on VLT wth 1 arcmin FoV, 0.2" spaxel, wide simultaneous wavelength coverage (4650 − 9300Å), relatively high spectral resolution (R ∼ 3000), and high throughput (35% end-to-end).
- The concept of MUSE foresees the splitting of the adaptive optics corrected field of view in 24 sub-fields. Each of these sub-fields is fed into a spectrograph (called Integral Field Unit, IFU). An image slicer in front of each IFU serves as entrance slit, thus producing a spatially resolved spectrum of the full sub-field.
- KMOS
- The K-band Multi Object Spectrograph (KMOS). IFS in the near-infrared bands for 24 targets simultaneously.
- 14x14 spectra with ~1000 Nyquist-sampled spectral resolution elements for each of the 24 independent sub-fields.
- Each IFU has a square field of view of 2.8 x 2.8 arcsec;ensures uniform spatial sampling of 0.2 x 0.2 arcsec whilst maintaining Nyquist sampling (~2 pixel)
JWST上的NIRspec
- NIRSpec is equipped with an integral field unit optimized for the spectroscopic study of complex extended objects. It will provide 900 spectra per exposure over a field of view of 3 x 3 arcminutes.（0.6-5mu）
Keck上的终端
- MOSFIRE
- Multi-Object Spectrometer for Infra-Red Exploration
100%filling IFUs
- SAURON:33"x4"
- WiFeS:38"x25"