PAUS - 版本历史

2016年1月8日 (五) 03:02 Shen

2016-01-08T03:02:39Z

←上一版本		2016年1月8日 (五) 03:02的版本
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	*a 100 deg2 PAUS with 45 color bands is equivalent to 4500 deg2 single band imaging survey		*a 100 deg2 PAUS with 45 color bands is equivalent to 4500 deg2 single band imaging survey
	* Observe ∼100 deg2 to iAB ≈ 23-24 to reach a volume of 0.3-0.5 (Gpc/h)3 with a few million redshifts split into 3 to 4 wide fields (of several tens of deg2 each)		* Observe ∼100 deg2 to iAB ≈ 23-24 to reach a volume of 0.3-0.5 (Gpc/h)3 with a few million redshifts split into 3 to 4 wide fields (of several tens of deg2 each)
	* where Broad-Band (BB) photometric measurements have already been obtained by CFHTLenS and KiDS, and in which spectroscopic redshifts for calibration are available from the GAMA, VIPERS, DEEP2 and zCOSMOS redshift surveys.		* where Broad-Band (BB) photometric measurements have already been obtained by [[CFHTLenS]] and [[KiDS]], and in which spectroscopic redshifts for calibration are available from the [[GAMA]], [[VIPERS]], [[DEEP2]] and [[zCOSMOS]] redshift surveys.

Shen：/* PAUS */

2016-01-08T03:00:13Z

PAUS

←上一版本		2016年1月8日 (五) 03:00的版本
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	==PAUS==		==PAUS==
		⚫	[[文件:Science data1.png\|缩略图\|surveys]]

	*survey with PAUCam		*survey with PAUCam
	*a 100 deg2 PAUS will provide 3 million redshifts to iAB>22.5 (30 times more than currently available)		*a 100 deg2 PAUS will provide 3 million redshifts to iAB>22.5 (30 times more than currently available)
	*a 100 deg2 PAUS with 45 color bands is equivalent to 4500 deg2 single band imaging survey		*a 100 deg2 PAUS with 45 color bands is equivalent to 4500 deg2 single band imaging survey
	* Observe ∼100 deg2 to iAB ≈ 23-24 to reach a volume of 0.3-0.5 (Gpc/h)3 with a few million redshifts split into 3 to 4 wide fields (of several tens of deg2 each)		* Observe ∼100 deg2 to iAB ≈ 23-24 to reach a volume of 0.3-0.5 (Gpc/h)3 with a few million redshifts split into 3 to 4 wide fields (of several tens of deg2 each)
⚫	[[文件:Science data1.png\|缩略图\|surveys]]
	* where Broad-Band (BB) photometric measurements have already been obtained by CFHTLenS and KiDS, and in which spectroscopic redshifts for calibration are available from the GAMA, VIPERS, DEEP2 and zCOSMOS redshift surveys.		* where Broad-Band (BB) photometric measurements have already been obtained by CFHTLenS and KiDS, and in which spectroscopic redshifts for calibration are available from the GAMA, VIPERS, DEEP2 and zCOSMOS redshift surveys.

Shen：/* PAUS */

2016-01-08T02:59:25Z

PAUS

←上一版本		2016年1月8日 (五) 02:59的版本
第12行：		第12行：
	*a 100 deg2 PAUS with 45 color bands is equivalent to 4500 deg2 single band imaging survey		*a 100 deg2 PAUS with 45 color bands is equivalent to 4500 deg2 single band imaging survey
	* Observe ∼100 deg2 to iAB ≈ 23-24 to reach a volume of 0.3-0.5 (Gpc/h)3 with a few million redshifts split into 3 to 4 wide fields (of several tens of deg2 each)		* Observe ∼100 deg2 to iAB ≈ 23-24 to reach a volume of 0.3-0.5 (Gpc/h)3 with a few million redshifts split into 3 to 4 wide fields (of several tens of deg2 each)
			[[文件:Science data1.png\|缩略图\|surveys]]
	* where Broad-Band (BB) photometric measurements have already been obtained by CFHTLenS and KiDS, and in which spectroscopic redshifts for calibration are available from the GAMA, VIPERS, DEEP2 and zCOSMOS redshift surveys.		* where Broad-Band (BB) photometric measurements have already been obtained by CFHTLenS and KiDS, and in which spectroscopic redshifts for calibration are available from the GAMA, VIPERS, DEEP2 and zCOSMOS redshift surveys.

Shen：/* PAUS */

2016-01-08T02:58:28Z

PAUS

←上一版本		2016年1月8日 (五) 02:58的版本
第11行：		第11行：
	*a 100 deg2 PAUS will provide 3 million redshifts to iAB>22.5 (30 times more than currently available)		*a 100 deg2 PAUS will provide 3 million redshifts to iAB>22.5 (30 times more than currently available)
	*a 100 deg2 PAUS with 45 color bands is equivalent to 4500 deg2 single band imaging survey		*a 100 deg2 PAUS with 45 color bands is equivalent to 4500 deg2 single band imaging survey
	* Observe ∼100 deg2 to iAB ≈ 23-24 to reach a volume of 0.3-0.5 (Gpc/h)3 with a few million redshifts split into 3 to 4 wide fields (of several tens of deg2 each),		* Observe ∼100 deg2 to iAB ≈ 23-24 to reach a volume of 0.3-0.5 (Gpc/h)3 with a few million redshifts split into 3 to 4 wide fields (of several tens of deg2 each)
			* where Broad-Band (BB) photometric measurements have already been obtained by CFHTLenS and KiDS, and in which spectroscopic redshifts for calibration are available from the GAMA, VIPERS, DEEP2 and zCOSMOS redshift surveys.

Shen：/* PAUS */

2016-01-08T02:54:21Z

PAUS

←上一版本		2016年1月8日 (五) 02:54的版本
第11行：		第11行：
	*a 100 deg2 PAUS will provide 3 million redshifts to iAB>22.5 (30 times more than currently available)		*a 100 deg2 PAUS will provide 3 million redshifts to iAB>22.5 (30 times more than currently available)
	*a 100 deg2 PAUS with 45 color bands is equivalent to 4500 deg2 single band imaging survey		*a 100 deg2 PAUS with 45 color bands is equivalent to 4500 deg2 single band imaging survey
			* Observe ∼100 deg2 to iAB ≈ 23-24 to reach a volume of 0.3-0.5 (Gpc/h)3 with a few million redshifts split into 3 to 4 wide fields (of several tens of deg2 each),

2016年1月8日 (五) 02:53 Shen

2016-01-08T02:53:11Z

←上一版本		2016年1月8日 (五) 02:53的版本
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	The camera is installed with 6 large ugrizY filters covering each the total focal plane and 5 trays containing 40 narrow band filters (10 nm) covering the range between 450-850 nm on the 8 central CCDs. Additionally, there is the possibility to install two external custom filters.		The camera is installed with 6 large ugrizY filters covering each the total focal plane and 5 trays containing 40 narrow band filters (10 nm) covering the range between 450-850 nm on the 8 central CCDs. Additionally, there is the possibility to install two external custom filters.

			==PAUS==
			*survey with PAUCam
			*a 100 deg2 PAUS will provide 3 million redshifts to iAB>22.5 (30 times more than currently available)
			*a 100 deg2 PAUS with 45 color bands is equivalent to 4500 deg2 single band imaging survey

Shen：创建页面，内容为“==PAUcam== PAUCam is an optical imaging camera to be used at the prime focus of the William Herschel Telescope (WHT). FOV 1 deg x 1 deg Pixel Scale 0.265″ *...”

2016-01-08T02:51:30Z

创建页面，内容为“==PAUcam== PAUCam is an optical imaging camera to be used at the prime focus of the William Herschel Telescope (WHT). *FOV 1 deg x 1 deg *Pixel Scale 0.265″ *...”

新页面

==PAUcam==
PAUCam is an optical imaging camera to be used at the prime focus of the William Herschel Telescope ([[WHT]]).
*FOV 1 deg x 1 deg
*Pixel Scale 0.265″
*18 Hamamatsu Fully-Depleted 4K x 2K CCD detectors

The camera is installed with 6 large ugrizY filters covering each the total focal plane and 5 trays containing 40 narrow band filters (10 nm) covering the range between 450-850 nm on the 8 central CCDs. Additionally, there is the possibility to install two external custom filters.

PAUS - 版本历史

2016年1月8日 (五) 03:02 Shen

Shen：​/* PAUS */

Shen：​/* PAUS */

Shen：​/* PAUS */

Shen：​/* PAUS */

2016年1月8日 (五) 02:53 Shen

Shen：​创建页面，内容为“==PAUcam== PAUCam is an optical imaging camera to be used at the prime focus of the William Herschel Telescope (WHT). *FOV 1 deg x 1 deg *Pixel Scale 0.265″ *...”

Shen：/* PAUS */

Shen：/* PAUS */

Shen：/* PAUS */

Shen：/* PAUS */

Shen：创建页面，内容为“==PAUcam== PAUCam is an optical imaging camera to be used at the prime focus of the William Herschel Telescope (WHT). FOV 1 deg x 1 deg Pixel Scale 0.265″ *...”