Applies a scaled window to the input sequence x. Wire data to the x input to determine the instance to use.
A real vector.
Default: [0]{}
The window to apply to x.
0 | 0 | Rectangle (default) |
1 | 1 | Hanning |
2 | 2 | Hamming |
3 | 3 | Blackman-Harris |
4 | 4 | Exact Blackman |
5 | 5 | Blackman |
6 | 6 | Flat Top |
7 | 7 | 4 Term B-Harris |
8 | 8 | 7 Term B-Harris |
9 | 9 | Low Sidelobe |
11 | 11 | Blackman Nuttall |
30 | 30 | Triangle |
31 | 31 | Bartlett-Hanning |
32 | 32 | Bohman |
33 | 33 | Parzen |
34 | 34 | Welch |
60 | 60 | Kaiser |
61 | 61 | Dolph-Chebyshev |
62 | 62 | Gaussian |
Default: 0
Beta parameter for a Kaiser window, the standard deviation for a Gaussian window, and the ratio, s, of the main lobe to the side lobe for a Dolph-Chebyshev window. If window is any other window, this VI ignores this input. The default value of window parameter is NaN, which sets beta to 0 for a Kaiser window, the standard deviation to 0.2 for a Gaussian window, and s to 60 for a Dolph-Chebyshev window.
The input signal with the window applied.
Coherent gain and equivalent noise bandwidth of the window.
Equivalent noise bandwidth of the window. You can use eq noise BW to divide a sum of individual power spectra or to compute the power in a given frequency span.
Inverse of the scaling factor this VI applies to the window.
A value that represents any error or warning that occurs when this node executes.
Installed By: LabVIEW Communications System Design Suite (introduced in 1.0)
Where This Node Can Run:
Desktop OS: Windows
FPGA: Not supported
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