Documentation/Nightly/Modules/AstroSmoothing - Revision history

Grundlett: Text replacement - "\[http:\/\/www\.slicer\.org\/slicerWiki\/index\.php\/([^ ]+) ([^]]+)]" to "$2"

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Text replacement - "\[http:\/\/www\.slicer\.org\/slicerWiki\/index\.php\/([^ ]+) ([^]]+)]" to "$2"

Davide at 11:00, 11 December 2017

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Davide at 14:09, 10 December 2017

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Davide at 12:01, 28 March 2017

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Davide at 12:00, 14 September 2016

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@@ Line 26: / Line 26: @@
 * Thijs van der Hulst, <email>J.M.van.der.Hulst@astro.rug.nl</email>
 * Jos Roerdink <email>j.b.t.m.roerdink@rug.nl</email>
-[http://www.slicer.org/slicerWiki/index.php/Documentation/Nightly/Extensions/SlicerAstro Back to SlicerAstro home]
+[[Documentation/Nightly/Extensions/SlicerAstro|Back to SlicerAstro home]]
 {{documentation/{{documentation/version}}/module-introduction-end}}

← Older revision		Revision as of 11:00, 11 December 2017
Line 46:		Line 46:

	[[File:AstroSmoothing.png \| 1000px]]		[[File:AstroSmoothing.png \| 1000px]]
		+	<br> <br>
	A comparative layout of the output generated by the AstroSmoothing module is shown. The interface includes a widget for changing the input parameters for the smoothing and a table showing the output segmentations generated after the smoothing process. This includes the widgets for changing the input (such as the filter choice, the computational hardware and the smoothing parameters) and visualizing the output segmentation objects generated by the smoothing process. The comparative layout is composed of two 3D views and three 2D views. In the left 3D view and the 2D views the data are shown. In the right 3D view the filtered version of the data is shown. The data are rendered in different colors that highlight the data at different intensity levels: green, blue and red correspond to 3, 7 and 15 times the rms noise respectively. The colored segmentations represent masks automatically calculated by the filtering algorithm. The light blue and yellow segmentations (visualized as contour plots in the 2D views) are a 3 rms thresholding of the input data and the filtered data, respectively.		A comparative layout of the output generated by the AstroSmoothing module is shown. The interface includes a widget for changing the input parameters for the smoothing and a table showing the output segmentations generated after the smoothing process. This includes the widgets for changing the input (such as the filter choice, the computational hardware and the smoothing parameters) and visualizing the output segmentation objects generated by the smoothing process. The comparative layout is composed of two 3D views and three 2D views. In the left 3D view and the 2D views the data are shown. In the right 3D view the filtered version of the data is shown. The data are rendered in different colors that highlight the data at different intensity levels: green, blue and red correspond to 3, 7 and 15 times the rms noise respectively. The colored segmentations represent masks automatically calculated by the filtering algorithm. The light blue and yellow segmentations (visualized as contour plots in the 2D views) are a 3 rms thresholding of the input data and the filtered data, respectively.

@@ Line 46: / Line 46: @@
 [[File:AstroSmoothing.png | 1000px]]
-A comparative layout of the output generated by the AstroSmoothing module is shown. The interface includes a widget for changing the input parameters for the smoothing and a table showing the output segmentations generated after the smoothing process. This includes the widgets for changing the input (such as the filter choice, the computational hardware and the smoothing parameters) and visualizing the output segmentation objects generated by the smoothing process. The comparative layout is composed of two 3-D views and three 2-D views. In the left 3-D view and the 2-D views the data are shown. In the right 3-D view the filtered version of the data is shown. The data are rendered in different colors that highlight the data at different intensity levels: green, blue and red correspond to 3, 7 and 15 times the rms noise respectively. The colored segmentations represent masks automatically calculated by the filtering algorithm. The light blue and yellow segmentations (visualized as contour plots in the 2-D views) are a 3 rms thresholding of the input data and the filtered data, respectively.
+A comparative layout of the output generated by the AstroSmoothing module is shown. The interface includes a widget for changing the input parameters for the smoothing and a table showing the output segmentations generated after the smoothing process. This includes the widgets for changing the input (such as the filter choice, the computational hardware and the smoothing parameters) and visualizing the output segmentation objects generated by the smoothing process. The comparative layout is composed of two 3D views and three 2D views. In the left 3D view and the 2D views the data are shown. In the right 3D view the filtered version of the data is shown. The data are rendered in different colors that highlight the data at different intensity levels: green, blue and red correspond to 3, 7 and 15 times the rms noise respectively. The colored segmentations represent masks automatically calculated by the filtering algorithm. The light blue and yellow segmentations (visualized as contour plots in the 2D views) are a 3 rms thresholding of the input data and the filtered data, respectively.
 <!-- ---------------------------- -->

@@ Line 40: / Line 40: @@
 <br />
-The intensity-driven gradient filter, due to its adaptive characteristics, is the optimal choice for HI data (see [Punzo2016](https://arxiv.org/pdf/1609.03782.pdf)). Therefore, it is the default method when the automatic mode has been chosen. This algorithm preserves the detailed structure of the signal with high signal-to-noise ratio (> 3) at the highest resolution, while smoothing only the faint part of the signal (signal-to-noise ratio < 3). For more information regarding the filters and their performance, default parameters, advantages and disadvantages, we refer to [Punzo2016](https://arxiv.org/pdf/1609.03782.pdf).
+The intensity-driven gradient filter, due to its adaptive characteristics, is the optimal choice for HI data (see [https://arxiv.org/pdf/1609.03782.pdf]). Therefore, it is the default method when the automatic mode has been chosen. This algorithm preserves the detailed structure of the signal with high signal-to-noise ratio (> 3) at the highest resolution, while smoothing only the faint part of the signal (signal-to-noise ratio < 3). For more information regarding the filters and their performance, default parameters, advantages and disadvantages, we refer to [https://arxiv.org/pdf/1609.03782.pdf].
 <!-- ---------------------------- -->

@@ Line 31: / Line 31: @@
 <!-- ---------------------------- -->
 {{documentation/{{documentation/version}}/module-section|Module Description}}
-The **AstroSmoothing** module contains a set of filters aimed to denoise astronomical (HI) dataset:
+The <b>AstroSmoothing</b> module contains a set of filters aimed to denoise astronomical (HI) dataset:
 * Anisotropic Box;

@@ Line 39: / Line 39: @@
 <!-- ---------------------------- -->
 {{documentation/{{documentation/version}}/module-section|Panels and their use}}
-* [[File:SlicerAstroWiki8.png|1000px]]
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 {{documentation/{{documentation/version}}/module-section|References}}
 <pre>
-@ARTICLE{2016arXiv160903782P,
+@ARTICLE{2016A&C....17..163P,
     author = {{Punzo}, D. and {van der Hulst}, J.~M. and {Roerdink}, J.~B.~T.~M.
 	},
-     title = "{Finding faint HI structure in and around galaxies: scraping the barrel}",
+     title = "{Finding faint H I structure in and around galaxies: Scraping the barrel}",
-   journal = {ArXiv e-prints},
+   journal = {Astronomy and Computing},
 archivePrefix = "arXiv",
     eprint = {1609.03782},
   primaryClass = "astro-ph.IM",
-  keywords = {Astrophysics - Instrumentation and Methods for Astrophysics},
+  keywords = {Radio lines: galaxies, Techniques: image processing, Scientific visualization},
       year = 2016,
-     month = sep,
+     month = oct,
-    adsurl = {http://adsabs.harvard.edu/abs/2016arXiv160903782P},
+    volume = 17,
-  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
+    pages = {163-176},
+}
 </pre>

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 Contributors: <br>
 <b>Steve Pieper</b> (Isomics) <br>
 Acknowledgements: <br>
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 {{documentation/{{documentation/version}}/module-section|Panels and their use}}
 * [[File:SlicerAstroWiki8.png|750px]]