Next: Data Selection Up: State Previous: Units, Doppler and Frequency . ASAP reads the line rest frequency from the RPFITS file when reading the data. ... Select for specified source/IF ASAP> scans.set_restfreqs(freqs=1.667359e9, source='NGC253', theif=0) # Select for all sources and IFs ASAP> scans.set_restfreqs(freqs=1.667359e9) . ... Set rest frequency for all IFs ASAP> scans.set_restfreqs(freqs=[1.6654018e9,1.667359e9,]) . ...

Next: A Simple Example With Up: CHIRPLET TRANSFORM SUBSPACES Previous: CHIRPLET TRANSFORM SUBSPACES . We begin by discussing the CF plane, and then present an argument for re-parameterizing this plane in terms of two frequency indices, leading to what we will be calling ``frequency-frequency'' (FF) analysis. ... Computing the CF plane of a signal, s ( t ), is equivalent to correlating the signal with a family of chirps that are parameterized by chirprate, c and center frequency, . ... Figure 7 . ...

spaceweb@oulu.fi - last update: 24 November 1998, 1335 UT . Radiowave Frequency Ranges . ... Extremely Low Frequencies . 30 - 300 Hz . ... 0.3 - 3 kHz . ... Very Low Frequencies . ... Low Frequencies . ... High Frequencies . ... 0.3 - 3 GHz . ... The International Telecommunication Union (ITU) has defined the radiowave frequency ranges as shown in the table. ... Their high frequency limit corresponds to magnetospheric ion gyrofrequencies (which are low because of small B and high m). ...

Next: Structure of the Galaxy Up: Model of the Galaxy Previous: Model of the Galaxy . As discussed above (Section  6 ), galactic binary systems are assumed to be distributed logarithmically along their semi-major axis A (Abt and Levy, 1976[ 2 ]), . ... Figure 40: Number of binary stars per frequency decade. ... As the observed distribution of binary periods is flat (equation ( 15.3.1 )), the normalization constant is the total number of galactic binaries per frequency decade: . ...

. This is the CIMA smart frequency switching menu: . The following is the on-line help page for smart frequency switching: . You can return to the main CIMA page by clicking here .

... HST . ... Home . ... Data . ... HST Peer Review Process . ... WFPC2 Home . ... Instrument Home . ... Calibration . Calibration Home . Calibration Plan . ... LRF Data . ... Data Analysis . Data Analysis Home . Data Analysis Library . ... Instrument Handbook . Data Handbook . ... Dither Handbook . ... Input "Frequency 0 " in relation: Flux = Flux 0 ( Frequency / Frequency 0 ) -(Spectral Index) . ... Values above 10 7 are taken to be frequency in Hz. ...

Site Map . ... Glossary . Timeline . ... Magnetic Field . ... Aurora . ... 3a. Loomis Aurora . 3b. Fritz Aurora . ... Hermann Fritz . Shown here is a map of the frequency with which auroras are seen, produced in 1881 by the German scientist Hermann Fritz (1830-1883). The line of greatest frequency lists 100 auroras per year, while in the center of the pattern auroras are much less frequent. ... Timeline Expanded timeline Glossary . ...

Next: Analysis in the Up: MIDAS utilities for Previous: Fourier analysis . For the detection of smooth signals, e.g. sinusoids, use either SCARGLE/TSA or AOV/TSA with bins. ... SCARGLE/TSA -- . Scargle sine model: This command computes Scargle's (1982) periodogram for unevenly spaced observations x . ... In this way, the command can be used to perform a CLEAN