relationship to speckle imaging #36

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davidwhogg opened this Issue May 8, 2012 · 3 comments

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davidwhogg commented May 8, 2012

we need to figure out how we are related -- conceptually and in performance -- to speckle imaging. I think it might be pretty similar when you drill down to the actual operations.

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fedhere May 8, 2012

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BJ has speckle code so he can be very helpful in this

On Tue, May 8, 2012 at 9:53 AM, David W. Hogg <
reply@reply.github.com

wrote:

we need to figure out how we are related -- conceptually and in
performance -- to speckle imaging. I think it might be pretty similar when
you drill down to the actual operations.


Reply to this email directly or view it on GitHub:
https://github.com/davidwhogg/LuckyImaging/issues/36


federica bianco
UCSB-Las Cumbres Observatory
Global Telescope Network
6740 Cortona Dr, Suite 102 | /
Goleta, CA |/
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fedhere commented May 8, 2012

BJ has speckle code so he can be very helpful in this

On Tue, May 8, 2012 at 9:53 AM, David W. Hogg <
reply@reply.github.com

wrote:

we need to figure out how we are related -- conceptually and in
performance -- to speckle imaging. I think it might be pretty similar when
you drill down to the actual operations.


Reply to this email directly or view it on GitHub:
https://github.com/davidwhogg/LuckyImaging/issues/36


federica bianco
UCSB-Las Cumbres Observatory
Global Telescope Network
6740 Cortona Dr, Suite 102 | /
Goleta, CA |/
|
*LCOGT.net * o
http://secure.lcogt.net/user/fbianco/dev/


/|/
|* Please consider the environment before printing this e-mail

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bjfultn May 9, 2012

I simply sum the 2-d fourier transforms of all the images (http://adsabs.harvard.edu/abs/1970A%26A.....6...85L). The resulting "fringe pattern" can be used to measure the separation and position angle of a binary source (with a 180 degree degeneracy). I believe this method is called "speckle interferometry" rather than "speckle imaging" since I do not reconstruct an image of the stars. From my experience it seems as though the speckle imaging performance is equivalent to lucky imaging performance, but it allows one to measure the positions of the sources with much greater precision.

bjfultn commented May 9, 2012

I simply sum the 2-d fourier transforms of all the images (http://adsabs.harvard.edu/abs/1970A%26A.....6...85L). The resulting "fringe pattern" can be used to measure the separation and position angle of a binary source (with a 180 degree degeneracy). I believe this method is called "speckle interferometry" rather than "speckle imaging" since I do not reconstruct an image of the stars. From my experience it seems as though the speckle imaging performance is equivalent to lucky imaging performance, but it allows one to measure the positions of the sources with much greater precision.

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fedhere May 10, 2012

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but it should be noticed that it is only applicable for small delta mag
ranges and the stars have to be very close to each other, to prodice the
fringes

On Wed, May 9, 2012 at 4:17 PM, bjfultn <
reply@reply.github.com

wrote:

I simply sum the 2-d fourier transforms of all the images (
http://adsabs.harvard.edu/abs/1970A%26A.....6...85L). The resulting
"fringe pattern" can be used to measure the separation and position angle
of a binary source (with a 180 degree degeneracy). I believe this method is
called "speckle interferometry" rather than "speckle imaging" since I do
not reconstruct an image of the stars. From my experience it seems as
though the speckle imaging performance is equivalent to lucky imaging
performance, but it allows one to measure the positions of the sources with
much greater precision.


Reply to this email directly or view it on GitHub:
https://github.com/davidwhogg/LuckyImaging/issues/36#issuecomment-5614397


federica bianco
UCSB-Las Cumbres Observatory
Global Telescope Network
6740 Cortona Dr, Suite 102 | /
Goleta, CA |/
|
*LCOGT.net * o
http://secure.lcogt.net/user/fbianco/dev/


/|/
|* Please consider the environment before printing this e-mail

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fedhere commented May 10, 2012

but it should be noticed that it is only applicable for small delta mag
ranges and the stars have to be very close to each other, to prodice the
fringes

On Wed, May 9, 2012 at 4:17 PM, bjfultn <
reply@reply.github.com

wrote:

I simply sum the 2-d fourier transforms of all the images (
http://adsabs.harvard.edu/abs/1970A%26A.....6...85L). The resulting
"fringe pattern" can be used to measure the separation and position angle
of a binary source (with a 180 degree degeneracy). I believe this method is
called "speckle interferometry" rather than "speckle imaging" since I do
not reconstruct an image of the stars. From my experience it seems as
though the speckle imaging performance is equivalent to lucky imaging
performance, but it allows one to measure the positions of the sources with
much greater precision.


Reply to this email directly or view it on GitHub:
https://github.com/davidwhogg/LuckyImaging/issues/36#issuecomment-5614397


federica bianco
UCSB-Las Cumbres Observatory
Global Telescope Network
6740 Cortona Dr, Suite 102 | /
Goleta, CA |/
|
*LCOGT.net * o
http://secure.lcogt.net/user/fbianco/dev/


/|/
|* Please consider the environment before printing this e-mail

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