Herschel Space Observatory - Revision history

Powers at 21:16, 2 February 2013

2013-02-02T21:16:44Z

Powers at 19:53, 2 February 2013

2013-02-02T19:53:23Z

Powers at 19:52, 2 February 2013

2013-02-02T19:52:24Z

Powers at 19:51, 2 February 2013

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Powers at 19:14, 2 February 2013

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Powers at 19:01, 2 February 2013

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Powers at 18:59, 2 February 2013

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Powers at 18:58, 2 February 2013

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Powers at 18:48, 2 February 2013

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Powers at 18:46, 2 February 2013

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-   A work in progress:
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-[[File:IR.gif|400px|left]]
+[[File:IR.gif|600px|left]]
 [[File:Poster.pdf]] Click on link to see pictures from ESA and pictures from Herschel on Dust and Star Formation in the Milky Way.

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-[[File:IR.jpg]]
+[[File:IR.gif|400px|left]]
 [[File:Poster.pdf]] Click on link to see pictures from ESA and pictures from Herschel on Dust and Star Formation in the Milky Way.

← Older revision		Revision as of 19:51, 2 February 2013
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		+	[[File:IR.jpg]]
	[[File:Poster.pdf]] Click on link to see pictures from ESA and pictures from Herschel on Dust and Star Formation in the Milky Way.		[[File:Poster.pdf]] Click on link to see pictures from ESA and pictures from Herschel on Dust and Star Formation in the Milky Way.

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 [[file:curves.jpg|400px|thumb|right]]
-In fact all objects glow (emit electromagnetic radiation), and they do this in the part of the electromagnetic spectrum that depends on their temperature. The diagram below shows how bright objects of different temperatures appear at difference wavelengths.
+In fact all objects glow (emit electromagnetic radiation), and they do this in the part of the electromagnetic spectrum that depends on their temperature. The diagram on the right shows how bright objects of different temperatures appear at difference wavelengths.
 The Sun has a surface temperature of nearly 6000 Kelvin (where the Kelvin temperature scale is the same as the familiar Centigrade scale except that the zero degrees C is about 273 degrees Kelvin). Its radiation peaks in the visible part of the spectrum at wavelengths of about half a micron, as shown by the yellow-green line in the graph above.

← Older revision		Revision as of 19:01, 2 February 2013
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−	[[File:Poster.pdf]]	+	[[File:Poster.pdf]] Click on link to see pictures from ESA and pictures from Herschel on Dust and Star Formation in the Milky Way.
−	~~[[File:Poster~~.~~pdf\|600px\|thumb\|left]]~~

← Older revision		Revision as of 18:59, 2 February 2013
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	[[File:Poster.pdf]]		[[File:Poster.pdf]]
		+	[[File:Poster.pdf\|600px\|thumb\|left]]

← Older revision		Revision as of 18:58, 2 February 2013
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	[[File:Sed-line.jpg\|300px\|thumb\|right\|Zoom-in on a typical spectral feature that can be observed by Herschel. The Herschel range contains many hundreds of such features due to many different atoms and molecules.]]		[[File:Sed-line.jpg\|300px\|thumb\|right\|Zoom-in on a typical spectral feature that can be observed by Herschel. The Herschel range contains many hundreds of such features due to many different atoms and molecules.]]

−	But the clouds from which stars form are made of dust and gas – in fact most of the material is in the form of gas. All three Herschel instruments have spectrometers which can zoom in on very narrow wavelength bands to examine the radiation coming from particular atoms and molecules in the gas. These appear as small features on top of the thermal spectrum, such as the one illustrated ~~below~~. The wavelength range that Herschel covers is teeming with such spectral signatures from atoms like carbon, oxygen, and nitrogen, and molecules such as carbon monoxide (CO), and water (H2O). These are the constituents of planets such as the Earth, and indeed of ourselves. With Herschel we will be able to study them in space and how they are involved in the formation of new stars and planetary systems. From Herschel’s observations it is be possible to find out what distant objects are composed of, the temperature, the density, and how the gas is moving - for instance whether a cloud is collapsing.	+	But the clouds from which stars form are made of dust and gas – in fact most of the material is in the form of gas. All three Herschel instruments have spectrometers which can zoom in on very narrow wavelength bands to examine the radiation coming from particular atoms and molecules in the gas. These appear as small features on top of the thermal spectrum, such as the one illustrated on the right. The wavelength range that Herschel covers is teeming with such spectral signatures from atoms like carbon, oxygen, and nitrogen, and molecules such as carbon monoxide (CO), and water (H2O). These are the constituents of planets such as the Earth, and indeed of ourselves. With Herschel we will be able to study them in space and how they are involved in the formation of new stars and planetary systems. From Herschel’s observations it is be possible to find out what distant objects are composed of, the temperature, the density, and how the gas is moving - for instance whether a cloud is collapsing.

← Older revision		Revision as of 18:48, 2 February 2013
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−	[[File:~~Galactic_poster_A4_portrait_UK~~.pdf]]	+	[[File:Poster.pdf]]

← Older revision		Revision as of 18:46, 2 February 2013
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−	[[~~file~~:Galactic_poster_A4_portrait_UK.pdf]]	+	[[File:Galactic_poster_A4_portrait_UK.pdf]]