Research highlights - 版本历史

Shen：/* Three dimensional Galactic dust distribution */

2018-10-29T02:27:30Z

Three dimensional Galactic dust distribution

←上一版本		2018年10月29日 (一) 02:27的版本
第11行：		第11行：

	===Three dimensional Galactic dust distribution===		===Three dimensional Galactic dust distribution===
	Using a sample of over six million stars from LAMOST spectral survey, our study shows that the overall distribution of the interstellar dust in the Milky Way can be well described by a disk-like structure with an exponential decrease in both radial and vertical densities, after subtracting two very prominent substructures near the sun. The scale-length of the dust disk is up to 10,000 light-years, while the scale-height is only about 330 light-years. In contrast to the structural parameters of the Milky Way's stellar disks, also based on LAMOST survey data, the Galactic dust disk is also more stretched on the radial scale and thinner in the vertical. That is to say, if we are far enough away, the Milky Way we see will be very similar to Sombrero Galaxy from the edge-on view.		Using a sample of over six million stars from LAMOST spectral survey, our study shows that the overall distribution of the interstellar dust in the Milky Way can be well described by a disk-like structure with an exponential decrease in both radial and vertical densities, after subtracting two very prominent substructures near the sun. The scale-length of the dust disk is up to 10,000 light-years, while the scale-height is only about 330 light-years. In contrast to the structural parameters of the Milky Way's stellar disks, also based on LAMOST survey data, the Galactic dust disk is also more stretched on the radial scale and thinner in the vertical. That is to say, if we are far enough away, the Milky Way we see will be very similar to Sombrero Galaxy from the edge-on view. (Li et al. 2018 [http://adsabs.harvard.edu/abs/2018ApJ...858...75L ADS])

	[[file:Galactic_dust.png\|none\|800px\|Sag]]		[[file:Galactic_dust.png\|none\|800px\|Sag]]

Shen：/* Three dimensional Galactic dust distribution */

2018-10-29T02:26:12Z

Three dimensional Galactic dust distribution

←上一版本		2018年10月29日 (一) 02:26的版本
第11行：		第11行：

	===Three dimensional Galactic dust distribution===		===Three dimensional Galactic dust distribution===
			Using a sample of over six million stars from LAMOST spectral survey, our study shows that the overall distribution of the interstellar dust in the Milky Way can be well described by a disk-like structure with an exponential decrease in both radial and vertical densities, after subtracting two very prominent substructures near the sun. The scale-length of the dust disk is up to 10,000 light-years, while the scale-height is only about 330 light-years. In contrast to the structural parameters of the Milky Way's stellar disks, also based on LAMOST survey data, the Galactic dust disk is also more stretched on the radial scale and thinner in the vertical. That is to say, if we are far enough away, the Milky Way we see will be very similar to Sombrero Galaxy from the edge-on view.

			[[file:Galactic_dust.png\|none\|800px\|Sag]]

	===Hyper-velocity stars ===		===Hyper-velocity stars ===

Shen：/* Discovers and insights from LAMOST */

2018-10-29T02:20:16Z

Discovers and insights from LAMOST

←上一版本		2018年10月29日 (一) 02:20的版本
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	==Discovers and insights from LAMOST==		==Discovers and insights from LAMOST==

			===Three dimensional Galactic dust distribution===


	===Hyper-velocity stars ===		===Hyper-velocity stars ===

Shen：/* 科学报道 Public reports */

2018-10-29T02:19:04Z

科学报道 Public reports

←上一版本		2018年10月29日 (一) 02:19的版本
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	==科学报道 Public reports==		==科学报道 Public reports==
			*精确测量银河系的尘埃分布。[http://www.shao.ac.cn/xwzx/kyjz/201804/t20180424_5001669.html]
			*精确测量银河系的尘埃消光。[http://www.cas.cn/syky/201702/t20170206_4589903.shtml]
			*宇宙是透明的吗？[http://www.shao.ac.cn/xwzx/ttxw/201503/t20150318_4323735.html]
	*郭守敬望远镜发现一批离太阳最近的晚型高速/超高速星。[http://www.shao.ac.cn/xwzx/kydt/201406/t20140627_4144889.html]		*郭守敬望远镜发现一批离太阳最近的晚型高速/超高速星。[http://www.shao.ac.cn/xwzx/kydt/201406/t20140627_4144889.html]
	*最亮的星系有多亮？[http://www.shao.ac.cn/xwzx/kydt/201401/t20140113_4021901.html]		*最亮的星系有多亮？[http://www.shao.ac.cn/xwzx/kydt/201401/t20140113_4021901.html]

Cluster：/* Ages of stars */

2014-09-10T00:51:07Z

Ages of stars

←上一版本		2014年9月10日 (三) 00:51的版本
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	If we want to dissect the formation history of the Galaxy, we ideally need to know the ages of the stars we are studying. Ages are notoriously difficult to determine, but with precise stellar parameters from high-resolution spectroscopic surveys, such as APOGEE, this is becoming possible. SHAO postdoc Emma Small is working on developing tools to estimate ages for red giant and red clump stars (Fig. 3). The resulting catalogues, which combine ages with the detailed kinematics and chemistry, will allow us to probe the formation histories of the disc, bulge and halo.		If we want to dissect the formation history of the Galaxy, we ideally need to know the ages of the stars we are studying. Ages are notoriously difficult to determine, but with precise stellar parameters from high-resolution spectroscopic surveys, such as APOGEE, this is becoming possible. SHAO postdoc Emma Small is working on developing tools to estimate ages for red giant and red clump stars (Fig. 3). The resulting catalogues, which combine ages with the detailed kinematics and chemistry, will allow us to probe the formation histories of the disc, bulge and halo.

	[[file:Age1.jpg\|left\|~~320px~~\|Age1]][[file:Age2.jpg\|center\|~~640px~~\|Age2]]		[[file:Age1.jpg\|left\|300px\|Age1]][[file:Age2.jpg\|center\|600px\|Age2]]
	Figure 3. This figure demonstrates how we are determining star formation histories from spectroscopic surveys such as LAMOST or APOGEE (Small et al., in prep). We have generated a mock population of stars (left) with measured stellar parameters (e.g. gravity, temperature, metallicity), and used these to recover the underlying star formation history (right; red shows the input history, black shows the recovered one).		Figure 3. This figure demonstrates how we are determining star formation histories from spectroscopic surveys such as LAMOST or APOGEE (Small et al., in prep). We have generated a mock population of stars (left) with measured stellar parameters (e.g. gravity, temperature, metallicity), and used these to recover the underlying star formation history (right; red shows the input history, black shows the recovered one).

Cluster：/* Ages of stars */

2014-09-10T00:45:10Z

Ages of stars

←上一版本		2014年9月10日 (三) 00:45的版本
第25行：		第25行：
	If we want to dissect the formation history of the Galaxy, we ideally need to know the ages of the stars we are studying. Ages are notoriously difficult to determine, but with precise stellar parameters from high-resolution spectroscopic surveys, such as APOGEE, this is becoming possible. SHAO postdoc Emma Small is working on developing tools to estimate ages for red giant and red clump stars (Fig. 3). The resulting catalogues, which combine ages with the detailed kinematics and chemistry, will allow us to probe the formation histories of the disc, bulge and halo.		If we want to dissect the formation history of the Galaxy, we ideally need to know the ages of the stars we are studying. Ages are notoriously difficult to determine, but with precise stellar parameters from high-resolution spectroscopic surveys, such as APOGEE, this is becoming possible. SHAO postdoc Emma Small is working on developing tools to estimate ages for red giant and red clump stars (Fig. 3). The resulting catalogues, which combine ages with the detailed kinematics and chemistry, will allow us to probe the formation histories of the disc, bulge and halo.

	[[file:Age1.jpg\|left\|320px\|Age1]][[file:Age2.jpg\|center\|~~680px~~\|Age2]]		[[file:Age1.jpg\|left\|320px\|Age1]][[file:Age2.jpg\|center\|640px\|Age2]]
	Figure 3. This figure demonstrates how we are determining star formation histories from spectroscopic surveys such as LAMOST or APOGEE (Small et al., in prep). We have generated a mock population of stars (left) with measured stellar parameters (e.g. gravity, temperature, metallicity), and used these to recover the underlying star formation history (right; red shows the input history, black shows the recovered one).		Figure 3. This figure demonstrates how we are determining star formation histories from spectroscopic surveys such as LAMOST or APOGEE (Small et al., in prep). We have generated a mock population of stars (left) with measured stellar parameters (e.g. gravity, temperature, metallicity), and used these to recover the underlying star formation history (right; red shows the input history, black shows the recovered one).

Cluster：/* Ages of stars */

2014-09-10T00:44:49Z

Ages of stars

←上一版本		2014年9月10日 (三) 00:44的版本
第25行：		第25行：
	If we want to dissect the formation history of the Galaxy, we ideally need to know the ages of the stars we are studying. Ages are notoriously difficult to determine, but with precise stellar parameters from high-resolution spectroscopic surveys, such as APOGEE, this is becoming possible. SHAO postdoc Emma Small is working on developing tools to estimate ages for red giant and red clump stars (Fig. 3). The resulting catalogues, which combine ages with the detailed kinematics and chemistry, will allow us to probe the formation histories of the disc, bulge and halo.		If we want to dissect the formation history of the Galaxy, we ideally need to know the ages of the stars we are studying. Ages are notoriously difficult to determine, but with precise stellar parameters from high-resolution spectroscopic surveys, such as APOGEE, this is becoming possible. SHAO postdoc Emma Small is working on developing tools to estimate ages for red giant and red clump stars (Fig. 3). The resulting catalogues, which combine ages with the detailed kinematics and chemistry, will allow us to probe the formation histories of the disc, bulge and halo.

	[[file:Age1.jpg\|left\|320px\|Age1]][[file:Age2.jpg\|~~left~~\|680px\|Age2]]		[[file:Age1.jpg\|left\|320px\|Age1]][[file:Age2.jpg\|center\|680px\|Age2]]
	Figure 3. This figure demonstrates how we are determining star formation histories from spectroscopic surveys such as LAMOST or APOGEE (Small et al., in prep). We have generated a mock population of stars (left) with measured stellar parameters (e.g. gravity, temperature, metallicity), and used these to recover the underlying star formation history (right; red shows the input history, black shows the recovered one).		Figure 3. This figure demonstrates how we are determining star formation histories from spectroscopic surveys such as LAMOST or APOGEE (Small et al., in prep). We have generated a mock population of stars (left) with measured stellar parameters (e.g. gravity, temperature, metallicity), and used these to recover the underlying star formation history (right; red shows the input history, black shows the recovered one).

Cluster：/* Ages of stars */

2014-09-10T00:43:50Z

Ages of stars

←上一版本		2014年9月10日 (三) 00:43的版本
第25行：		第25行：
	If we want to dissect the formation history of the Galaxy, we ideally need to know the ages of the stars we are studying. Ages are notoriously difficult to determine, but with precise stellar parameters from high-resolution spectroscopic surveys, such as APOGEE, this is becoming possible. SHAO postdoc Emma Small is working on developing tools to estimate ages for red giant and red clump stars (Fig. 3). The resulting catalogues, which combine ages with the detailed kinematics and chemistry, will allow us to probe the formation histories of the disc, bulge and halo.		If we want to dissect the formation history of the Galaxy, we ideally need to know the ages of the stars we are studying. Ages are notoriously difficult to determine, but with precise stellar parameters from high-resolution spectroscopic surveys, such as APOGEE, this is becoming possible. SHAO postdoc Emma Small is working on developing tools to estimate ages for red giant and red clump stars (Fig. 3). The resulting catalogues, which combine ages with the detailed kinematics and chemistry, will allow us to probe the formation histories of the disc, bulge and halo.

	[[file:Age1.jpg\|left\|320px\|Age1]][[file:Age2.jpg\|~~right~~\|680px\|Age2]]		[[file:Age1.jpg\|left\|320px\|Age1]][[file:Age2.jpg\|left\|680px\|Age2]]
	Figure 3. This figure demonstrates how we are determining star formation histories from spectroscopic surveys such as LAMOST or APOGEE (Small et al., in prep). We have generated a mock population of stars (left) with measured stellar parameters (e.g. gravity, temperature, metallicity), and used these to recover the underlying star formation history (right; red shows the input history, black shows the recovered one).		Figure 3. This figure demonstrates how we are determining star formation histories from spectroscopic surveys such as LAMOST or APOGEE (Small et al., in prep). We have generated a mock population of stars (left) with measured stellar parameters (e.g. gravity, temperature, metallicity), and used these to recover the underlying star formation history (right; red shows the input history, black shows the recovered one).

Cluster：/* Ages of stars */

2014-09-10T00:42:43Z

Ages of stars

←上一版本		2014年9月10日 (三) 00:42的版本
第25行：		第25行：
	If we want to dissect the formation history of the Galaxy, we ideally need to know the ages of the stars we are studying. Ages are notoriously difficult to determine, but with precise stellar parameters from high-resolution spectroscopic surveys, such as APOGEE, this is becoming possible. SHAO postdoc Emma Small is working on developing tools to estimate ages for red giant and red clump stars (Fig. 3). The resulting catalogues, which combine ages with the detailed kinematics and chemistry, will allow us to probe the formation histories of the disc, bulge and halo.		If we want to dissect the formation history of the Galaxy, we ideally need to know the ages of the stars we are studying. Ages are notoriously difficult to determine, but with precise stellar parameters from high-resolution spectroscopic surveys, such as APOGEE, this is becoming possible. SHAO postdoc Emma Small is working on developing tools to estimate ages for red giant and red clump stars (Fig. 3). The resulting catalogues, which combine ages with the detailed kinematics and chemistry, will allow us to probe the formation histories of the disc, bulge and halo.

	[[file:Age1.jpg\|~~none~~\|320px\|Age1]][[file:Age2.jpg\|right\|680px\|Age2]]		[[file:Age1.jpg\|left\|320px\|Age1]][[file:Age2.jpg\|right\|680px\|Age2]]
	Figure 3. This figure demonstrates how we are determining star formation histories from spectroscopic surveys such as LAMOST or APOGEE (Small et al., in prep). We have generated a mock population of stars (left) with measured stellar parameters (e.g. gravity, temperature, metallicity), and used these to recover the underlying star formation history (right; red shows the input history, black shows the recovered one).		Figure 3. This figure demonstrates how we are determining star formation histories from spectroscopic surveys such as LAMOST or APOGEE (Small et al., in prep). We have generated a mock population of stars (left) with measured stellar parameters (e.g. gravity, temperature, metallicity), and used these to recover the underlying star formation history (right; red shows the input history, black shows the recovered one).

Cluster：/* Ages of stars */

2014-09-10T00:39:23Z

Ages of stars

←上一版本		2014年9月10日 (三) 00:39的版本
第25行：		第25行：
	If we want to dissect the formation history of the Galaxy, we ideally need to know the ages of the stars we are studying. Ages are notoriously difficult to determine, but with precise stellar parameters from high-resolution spectroscopic surveys, such as APOGEE, this is becoming possible. SHAO postdoc Emma Small is working on developing tools to estimate ages for red giant and red clump stars (Fig. 3). The resulting catalogues, which combine ages with the detailed kinematics and chemistry, will allow us to probe the formation histories of the disc, bulge and halo.		If we want to dissect the formation history of the Galaxy, we ideally need to know the ages of the stars we are studying. Ages are notoriously difficult to determine, but with precise stellar parameters from high-resolution spectroscopic surveys, such as APOGEE, this is becoming possible. SHAO postdoc Emma Small is working on developing tools to estimate ages for red giant and red clump stars (Fig. 3). The resulting catalogues, which combine ages with the detailed kinematics and chemistry, will allow us to probe the formation histories of the disc, bulge and halo.

	[[file:Age1.jpg\|~~left~~\|320px\|Age1]][[file:Age2.jpg\|right\|680px\|Age2]]		[[file:Age1.jpg\|none\|320px\|Age1]][[file:Age2.jpg\|right\|680px\|Age2]]
	Figure 3. This figure demonstrates how we are determining star formation histories from spectroscopic surveys such as LAMOST or APOGEE (Small et al., in prep). We have generated a mock population of stars (left) with measured stellar parameters (e.g. gravity, temperature, metallicity), and used these to recover the underlying star formation history (right; red shows the input history, black shows the recovered one).		Figure 3. This figure demonstrates how we are determining star formation histories from spectroscopic surveys such as LAMOST or APOGEE (Small et al., in prep). We have generated a mock population of stars (left) with measured stellar parameters (e.g. gravity, temperature, metallicity), and used these to recover the underlying star formation history (right; red shows the input history, black shows the recovered one).

Research highlights - 版本历史

Shen：​/* Three dimensional Galactic dust distribution */

Shen：​/* Three dimensional Galactic dust distribution */

Shen：​/* Discovers and insights from LAMOST */

Shen：​/* 科学报道 Public reports */

Cluster：​/* Ages of stars */

Cluster：​/* Ages of stars */

Cluster：​/* Ages of stars */

Cluster：​/* Ages of stars */

Cluster：​/* Ages of stars */

Cluster：​/* Ages of stars */

Shen：/* Three dimensional Galactic dust distribution */

Shen：/* Three dimensional Galactic dust distribution */

Shen：/* Discovers and insights from LAMOST */

Shen：/* 科学报道 Public reports */

Cluster：/* Ages of stars */

Cluster：/* Ages of stars */

Cluster：/* Ages of stars */

Cluster：/* Ages of stars */

Cluster：/* Ages of stars */

Cluster：/* Ages of stars */