The Formation of Astronomical Images
description
Transcript of The Formation of Astronomical Images
![Page 1: The Formation of Astronomical Images](https://reader036.fdocuments.us/reader036/viewer/2022062323/56815454550346895dc26b48/html5/thumbnails/1.jpg)
Tod R. Lauer (NOAO)July 19, 2010
The Formation of Astronomical Images
Tod R. Lauer
![Page 2: The Formation of Astronomical Images](https://reader036.fdocuments.us/reader036/viewer/2022062323/56815454550346895dc26b48/html5/thumbnails/2.jpg)
Tod R. Lauer (NOAO)July 19, 2010
Astronomical Images
• A set of points at which a quantity is measured within a space. Pictures, spectra, IFU “data cubes” are all examples of images.
• In this talk we will focus on 2-D flux maps with regularly spaced samples, but this is only a subset of possible images.
• To understand imaging, you need to understand how an object is represented by its image.
![Page 3: The Formation of Astronomical Images](https://reader036.fdocuments.us/reader036/viewer/2022062323/56815454550346895dc26b48/html5/thumbnails/3.jpg)
Tod R. Lauer (NOAO)July 19, 2010
Image Formation
I = O ( P ) Ш + N I Image Observed
O Intrinsic Object
P PSF
Pixel Kernel
Ш Sampling Comb
N Noise
Effective or total PSF
![Page 4: The Formation of Astronomical Images](https://reader036.fdocuments.us/reader036/viewer/2022062323/56815454550346895dc26b48/html5/thumbnails/4.jpg)
Tod R. Lauer (NOAO)July 19, 2010
The Image Source
![Page 5: The Formation of Astronomical Images](https://reader036.fdocuments.us/reader036/viewer/2022062323/56815454550346895dc26b48/html5/thumbnails/5.jpg)
Tod R. Lauer (NOAO)July 19, 2010
The Point Spread Function
![Page 6: The Formation of Astronomical Images](https://reader036.fdocuments.us/reader036/viewer/2022062323/56815454550346895dc26b48/html5/thumbnails/6.jpg)
Tod R. Lauer (NOAO)July 19, 2010
The Observed Image
![Page 7: The Formation of Astronomical Images](https://reader036.fdocuments.us/reader036/viewer/2022062323/56815454550346895dc26b48/html5/thumbnails/7.jpg)
Tod R. Lauer (NOAO)July 19, 2010
The Fourier Transform
• The FT decomposes an image into a set of waves, with variable amplitude, phase, and direction.
• This allows information of different spatial scales to be isolated, analyzed, and processed.
• Convolution in Images space is multiplication in Fourier (and vice-versa).
• Complete symmetry and complementarity with Space.• Reciprocal Fourier/Image space scale relationship.• Critical for understanding resolution, filtering, sampling, and on
and on…
![Page 8: The Formation of Astronomical Images](https://reader036.fdocuments.us/reader036/viewer/2022062323/56815454550346895dc26b48/html5/thumbnails/8.jpg)
Tod R. Lauer (NOAO)July 19, 2010
The Fourier Transform
![Page 9: The Formation of Astronomical Images](https://reader036.fdocuments.us/reader036/viewer/2022062323/56815454550346895dc26b48/html5/thumbnails/9.jpg)
Tod R. Lauer (NOAO)July 19, 2010
The Fourier Domain Perspective
![Page 10: The Formation of Astronomical Images](https://reader036.fdocuments.us/reader036/viewer/2022062323/56815454550346895dc26b48/html5/thumbnails/10.jpg)
Tod R. Lauer (NOAO)July 19, 2010
And then add noise…
![Page 11: The Formation of Astronomical Images](https://reader036.fdocuments.us/reader036/viewer/2022062323/56815454550346895dc26b48/html5/thumbnails/11.jpg)
Tod R. Lauer (NOAO)July 19, 2010
Noise in the Fourier Domain
![Page 12: The Formation of Astronomical Images](https://reader036.fdocuments.us/reader036/viewer/2022062323/56815454550346895dc26b48/html5/thumbnails/12.jpg)
Tod R. Lauer (NOAO)July 19, 2010
Understanding Noise
• Noise sets the limit on the photometric and structural information recovered from an image.
• Noise limits the spatial resolution of features. Noise can mimic fine-scale features.
• Separating noise from signal is the major task of image analysis.
![Page 13: The Formation of Astronomical Images](https://reader036.fdocuments.us/reader036/viewer/2022062323/56815454550346895dc26b48/html5/thumbnails/13.jpg)
Tod R. Lauer (NOAO)July 19, 2010
Filtering Noise
![Page 14: The Formation of Astronomical Images](https://reader036.fdocuments.us/reader036/viewer/2022062323/56815454550346895dc26b48/html5/thumbnails/14.jpg)
Tod R. Lauer (NOAO)July 19, 2010
Filtering in the Fourier Domain
![Page 15: The Formation of Astronomical Images](https://reader036.fdocuments.us/reader036/viewer/2022062323/56815454550346895dc26b48/html5/thumbnails/15.jpg)
Tod R. Lauer (NOAO)July 19, 2010
Filters and Measures
• Filters isolate signal from noise, specific signals from other signals, interpolate images, etc.
• All measurements from an image can be regarded as forms of filters.
• Good filtering means understanding exactly how both noise and signal respond to the filter.
![Page 16: The Formation of Astronomical Images](https://reader036.fdocuments.us/reader036/viewer/2022062323/56815454550346895dc26b48/html5/thumbnails/16.jpg)
Tod R. Lauer (NOAO)July 19, 2010
Image Sampling
• Accuracy of photometry, astrometry, etc. depends on good sampling.
• Where possible, strive for “Nyquist-sampling,” which requires sampling at 2 highest spatial frequency present in image.
• Roughly-speaking - two pixels per PSF FWHM.
• No need to oversample! Harry Nyquist
![Page 17: The Formation of Astronomical Images](https://reader036.fdocuments.us/reader036/viewer/2022062323/56815454550346895dc26b48/html5/thumbnails/17.jpg)
Tod R. Lauer (NOAO)July 19, 2010
Sampling
![Page 18: The Formation of Astronomical Images](https://reader036.fdocuments.us/reader036/viewer/2022062323/56815454550346895dc26b48/html5/thumbnails/18.jpg)
Tod R. Lauer (NOAO)July 19, 2010
Sampling
• Sampling draws values at discrete points from a continuous function - this includes the pixel kernel.
• Samples = data pixels are pure delta functions. Distinguish data pixels from detector and display pixels.
• Under-sampling beats sampling frequency against spatial frequencies, aliasing them as bogus lower or higher spatial frequency power.
• Well-sampled data can be measured, interpolated, recast, etc. without resolution or photometric losses.
• Under-sampled data contain intrinsic photometric errors and cannot be resampled or interpolated without incurring additional signal degradation.
![Page 19: The Formation of Astronomical Images](https://reader036.fdocuments.us/reader036/viewer/2022062323/56815454550346895dc26b48/html5/thumbnails/19.jpg)
Tod R. Lauer (NOAO)July 19, 2010
The Sinc, or Interpolating-Function
• The assumption that the image is well-sampled and continuous implies the use of sinc(x). A “cutoff” box in the Fourier domain is sinc(x) in the image space.
• Sinc(x) interpolates with no loss of resolution, smoothing, etc.
• Any other interpolator is ad hoc.
• Sinc is sensitive to artifacts, thus well-reduced images are required.
• Sinc(x,y) is separable - it results from multiplying to 1-D functions.
• Taper as needed.
![Page 20: The Formation of Astronomical Images](https://reader036.fdocuments.us/reader036/viewer/2022062323/56815454550346895dc26b48/html5/thumbnails/20.jpg)
Tod R. Lauer (NOAO)July 19, 2010
Display vs. Data Pixels
![Page 21: The Formation of Astronomical Images](https://reader036.fdocuments.us/reader036/viewer/2022062323/56815454550346895dc26b48/html5/thumbnails/21.jpg)
Tod R. Lauer (NOAO)July 19, 2010
Detector Pixel Shapes
![Page 22: The Formation of Astronomical Images](https://reader036.fdocuments.us/reader036/viewer/2022062323/56815454550346895dc26b48/html5/thumbnails/22.jpg)
Tod R. Lauer (NOAO)July 19, 2010
Aliasing in the Fourier Domain
Well-Sampled
Under-Sampled - Satellites Overlap
![Page 23: The Formation of Astronomical Images](https://reader036.fdocuments.us/reader036/viewer/2022062323/56815454550346895dc26b48/html5/thumbnails/23.jpg)
Tod R. Lauer (NOAO)July 19, 2010
3X3 Sub-Sampled F555W WFC PSF
Single Native PSF
![Page 24: The Formation of Astronomical Images](https://reader036.fdocuments.us/reader036/viewer/2022062323/56815454550346895dc26b48/html5/thumbnails/24.jpg)
Tod R. Lauer (NOAO)July 19, 2010
Fourier-Space 3X3 F555W WFC Image reconstruction
![Page 25: The Formation of Astronomical Images](https://reader036.fdocuments.us/reader036/viewer/2022062323/56815454550346895dc26b48/html5/thumbnails/25.jpg)
Tod R. Lauer (NOAO)July 19, 2010
Photometric Errors Due to Undersampling
NIC3 J-Band
![Page 26: The Formation of Astronomical Images](https://reader036.fdocuments.us/reader036/viewer/2022062323/56815454550346895dc26b48/html5/thumbnails/26.jpg)
Tod R. Lauer (NOAO)July 19, 2010
Dithering to Fix Undersampled Data
• Many cameras with large pixels produce undersampled data.
• The pixel + PSF sets the resolution.• Shifting the camera by sub-pixel amounts recovers
Nyquist-sampling given optical PSF + pixel kernal = total or effective PSF.
• Dithering now standard on HST and other spacecraft - does require PSF stability over dither sequence.
• Distinguish this dithering from large-scale dithering to mitigate detector defects and sensitivity variations.
![Page 27: The Formation of Astronomical Images](https://reader036.fdocuments.us/reader036/viewer/2022062323/56815454550346895dc26b48/html5/thumbnails/27.jpg)
Tod R. Lauer (NOAO)July 19, 2010
Dithering