Astronomical Spectroscopy - Revision history

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← Older revision		Revision as of 17:27, 24 November 2014
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		+	== Astronomical Spectroscopy Project ==
		+
		+	[http://hank.uoregon.edu/experiments/Astronomical-Spectroscopy/astro.html Astronomical Spectroscopy Web Page]
		+
	The overall goal of the Astronomical Spectroscopy Project is to be able to collect and reduce data gathered from astronomical objects. Before spectra can be collected, the system needs to be prepared. This preparation involves aligning the telescope-fiber system and calculating the efficiency of the ratio to determine that the project is feasible with the current setup.		The overall goal of the Astronomical Spectroscopy Project is to be able to collect and reduce data gathered from astronomical objects. Before spectra can be collected, the system needs to be prepared. This preparation involves aligning the telescope-fiber system and calculating the efficiency of the ratio to determine that the project is feasible with the current setup.

← Older revision		Revision as of 23:27, 12 June 2014
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	[https://docs.google.com/presentation/d/1IBA_8ghSto6H9ivADDnq0qd3YHWw_VMEhpLkqUiVbXs/edit#slide=id.p9 Fall2013]		[https://docs.google.com/presentation/d/1IBA_8ghSto6H9ivADDnq0qd3YHWw_VMEhpLkqUiVbXs/edit#slide=id.p9 Fall2013]

−	~~[https//docs.google.com/presentation/d/1N1EG0J1AYbyJMr7mxVVqbPUZWQTekEKcCnZLlGymBAY/edit#slide=id.p9 Winter2014]~~	+

@@ Line 37: / Line 37: @@
 During the winter term of 2014 the Astronomical Spectroscopy group, comprised of Gerald Buxton, William McNichols, and Justin Stockwell, made some good headway in determining how best to rebuild the fiber setup.  To do so we focused on precisely determining the visual spot size of a calibrated beam coming out of the telescope.  This was done through the use of a calibrated light source placed across the room and a beam profiler. Our results form this test are shown below.
-[[File:Beam Profile Winter 2014.jpg]]
+               [[File:Beam Profile Winter 2014.jpg|750px]]
 The key measurement needed to determine the feasibility of our setup is the Effective Beam Diameter.  This measurement measures the number of pixels above a Clip Level of 1%.  This effectively means that 99% of the light is focused into a spot with a precise diameter of 656nm.  Our fiber size is 600nm so we are able to capture almost the entire amount of light from a calibrated light source.

@@ Line 50: / Line 50: @@
 We also wanted to determine the overall efficiency our our spectrometer.  That is, we wanted to determine a photons/count number at a particular wavelength.  To do this we used a laser setup that consisted of a laser, a converging lens, two focusing aluminum plates, three neutral density filters and then our fiber fed spectrometer. This set up looks like this.
-                                           [[File:Laser Setup 2 Fall 2013.jpg|350]]
+                                           [[File:Laser Setup 2 Fall 2013.jpg|350px]]
 Through the use of a power meter we were able to a power meter we were able to accurately determine the laser thruput coming out of our fiber.  Then by converting that power into number of photons/second we were able to compare that with the number of counts recorded by our spectrometer.  The math for this is shown below.
                                            [[File:20140612_161231.jpg|350px]]

@@ Line 33: / Line 33: @@
 [[File:Vega.png]]
 During the winter term of 2014 the Astronomical Spectroscopy group, comprised of Gerald Buxton, William McNichols, and Justin Stockwell, made some good headway in determining how best to rebuild the fiber setup.  To do so we focused on precisely determining the visual spot size of a calibrated beam coming out of the telescope.  This was done through the use of a calibrated light source placed across the room and a beam profiler. Our results form this test are shown below.
@@ Line 42: / Line 44: @@
 Next term we plan on using the information gleaned from the beam profiler to rebuild our fiber adapter setup.  This should allow us to couple at least 80% of the incoming light into our fiber, which is far better than the 1.1% we were coupling during the Fall term.  We need to machine a new adapter that directly attaches the flip mirror to the telescope, as well adapter that couples the fiber with the flip mirror at an approximate distance of 11.88cm from the back of the telescope.  With these adapters built, we should be able to take advantage of the nicer weather and get some better spectra of some astronomical objects.
 '''Presentations:'''

@@ Line 35: / Line 35: @@
 During the winter term of 2014 the Astronomical Spectroscopy group, comprised of Gerald Buxton, William McNichols, and Justin Stockwell, made some good headway in determining how best to rebuild the fiber setup.  To do so we focused on precisely determining the visual spot size of a calibrated beam coming out of the telescope.  This was done through the use of a calibrated light source placed across the room and a beam profiler. Our results form this test are shown below.
-[[File:Https://drive.google.com/|thumbnail|Beam Profiler Results]]
+[[File:file:///T:/documents/Astr/Beam%20Profile%20Winter%202014.jpg]]
 The key measurement needed to determine the feasibility of our setup is the Effective Beam Diameter.  This measurement measures the number of pixels above a Clip Level of 1%.  This effectively means that 99% of the light is focused into a spot with a precise diameter of 656nm.  Our fiber size is 600nm so we are able to capture almost the entire amount of light from a calibrated light source.

@@ Line 42: / Line 42: @@
 Next term we plan on using the information gleaned from the beam profiler to rebuild our fiber adapter setup.  This should allow us to couple at least 80% of the incoming light into our fiber, which is far better than the 1.1% we were coupling during the Fall term.  We need to machine a new adapter that directly attaches the flip mirror to the telescope, as well adapter that couples the fiber with the flip mirror at an approximate distance of 11.88cm from the back of the telescope.  With these adapters built, we should be able to take advantage of the nicer weather and get some better spectra of some astronomical objects.
 '''Presentations:'''
@@ Line 48: / Line 49: @@
 [https://docs.google.com/presentation/d/1IBA_8ghSto6H9ivADDnq0qd3YHWw_VMEhpLkqUiVbXs/edit#slide=id.p9 Fall2013]
-[https//docs.google.com/presentation/d/1N1EG0J1AYbyJMr7mxVVqbPUZWQTekEKcCnZLlGymBAY/edit#slide=id.p Winter 2014]
+[https//docs.google.com/presentation/d/1N1EG0J1AYbyJMr7mxVVqbPUZWQTekEKcCnZLlGymBAY/edit#slide=id.p9 Winter2014]

← Older revision		Revision as of 20:26, 21 March 2014
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	[https://docs.google.com/presentation/d/1IBA_8ghSto6H9ivADDnq0qd3YHWw_VMEhpLkqUiVbXs/edit#slide=id.p9 Fall2013]		[https://docs.google.com/presentation/d/1IBA_8ghSto6H9ivADDnq0qd3YHWw_VMEhpLkqUiVbXs/edit#slide=id.p9 Fall2013]

−	[~~[File:~~//docs.google.com/presentation/d/1N1EG0J1AYbyJMr7mxVVqbPUZWQTekEKcCnZLlGymBAY/edit#slide=id.p Winter 2014]	+	[https//docs.google.com/presentation/d/1N1EG0J1AYbyJMr7mxVVqbPUZWQTekEKcCnZLlGymBAY/edit#slide=id.p Winter 2014]

← Older revision		Revision as of 20:25, 21 March 2014
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	[https://docs.google.com/presentation/d/1IBA_8ghSto6H9ivADDnq0qd3YHWw_VMEhpLkqUiVbXs/edit#slide=id.p9 Fall2013]		[https://docs.google.com/presentation/d/1IBA_8ghSto6H9ivADDnq0qd3YHWw_VMEhpLkqUiVbXs/edit#slide=id.p9 Fall2013]

−	[[File://docs.google.com/presentation/d/1N1EG0J1AYbyJMr7mxVVqbPUZWQTekEKcCnZLlGymBAY/edit~~\|thumbnail]~~Winter 2014]	+	[[File://docs.google.com/presentation/d/1N1EG0J1AYbyJMr7mxVVqbPUZWQTekEKcCnZLlGymBAY/edit#slide=id.p Winter 2014]