Static Fourier spectrometers are often used for spectral measurements of the ionosphere emissions. There are two main advantages of Fourier spectrometers (FS) - large geometric factor and high spectral resolution; these parameters are two orders better than for grating spectral instruments. ... In scanning Fourier spectrometer optical and electric modulation of signal is used to avoid this problem, for static Fourier spectrometer there are no such ways. ...

A press release on the Canadian Galactic Plane Survey was associated with this poster. ... Below are maps of HI emission, HISA, and 12 CO emission in the eastern 25% of the survey, given as projections along the velocity ( Figure 1 ) and latitude ( Figure 2 ) axes. ... 2000, A. J. , submitted . ... GIF | ... We are developing automated methods of locating HISA in velocity cubes by removing large-scale emission in space and velocity and flagging small-scale dark residuals. ...

Integration and performance of the flight configuration SIR on TELIS P. Yagoubov1, G. de Lange1, A. de Lange, M. Romanini, R. Hoogeveen1, V. Koshelets2, G. Wagner3, M. Birk 1Nation 3 al Institute for ... Netherlands 2Institute of Radio Engineering and Electronics, IREE, Russia 3Institute for Remote Sensing Technology, DLR, Germany Abstract TELIS (Terahertz and submm Limb Sounder) is a cooperation between European institutes, DLR, RAL and SRON, to build a three- ... LO frequency 624.93 GHz. ...

... Galaxies 99 Cosmic background with model of cloudy interstellar medium Yu. ... Figure 1: Averaged spectrum of the cosmic background I f in frequency range 0.25 200 MHz for the Galactic poles. ... First interpretation of the cosmic noise background spectrum at broad band frequency range 0.25 200 MHz with a model of the cloudy interstellar medium ISM is presented here. ... Synthesized background spectra I f for regions of the Galactic poles at the frequency range 0.25 200 MHz is presented in Fig. ...

... As part of discussions aimed at extending ESA's participation in HST beyond the year 2001, consideration is being given to the possibility of ESA providing an advanced scientific instrument for installation during the 2002 HST servicing mission. ... In order to solicit the advice of the astronomical community and assist in identifying the scientifically most worthwhile instrument concepts, a second more scientifically oriented study group consisting of a number of representative HST users was set up...

Some recent results ( see ) attracted the attentions of astronomers working on field which could benefits from photon counting techniques with high speed and spatial resolutions as adaptive optics. ... Fasti has been designed to be fast and largerly configurable. ... The data rate attined in the best case (30 Mhz), give no impossible load to the digital acquisition in the photon counting mode, since data are 1 bit only, they can be parallelized, giving a maximum speed of about 940.000 32 bit word/sec. ...

... The calibration of astrophysical spectra in wavelength based on calibration lamp data suffers from different kinds of uncertainties. Besides inaccuracies in the observational phase, common data reduction practice adds ``pixelation'' errors, due to the fact that the centering method does not use the correct PSF. These model mismatch errors depend, for a given feature, on the sub-pixel location of the line center (David & Verschueren, private communication). ...

... Science . ... Science Users Information > Science Publications > Science Announcements > New GIRAFFE Spectral Resolutions Characterised For All Settings . ... ESO Data . ... The spectral resolution characterisation has been completed for all grating settings and the new resolving powers are listed under the FLAMES News . ... In some settings the spectral resolution is much higher, and in almost all HR settings there is an increase of 20-30% with respect to the values before the February intervention...

Observing Strategies at cm wavelengths Making good decisions Jessica Chapman Synthesis Workshop May 2003 Radio Continuum Observations · Frequencies · Angular resolution (/B) · Array configurations · Calibration strategies · Integration times · Interference and confusion ATCA - cm continuum observations 3 6 (cm): (GHz): 8.0 4 9.2 4.4 46.7 Prim.beam (arcmin): 5 Synth. ... For complex sources ­ it is often advisable to use 2 or more configurations. ...