... The procedure simply observes ON your source for x minutes and then takes a `blank sky' observation OFF your source for the same amount of time and tracking the same azimuth and zenith angle range. ... If your scans are for 5 minutes or less, your wait time should be set to 1 minute (the default setting). ... 2 (scan duration) + (slew time) + (calibration time) A 5 minute ON/OFF + 10s CAL takes 11.3 minutes. A 7 minute ON/OFF, (which has a 2 minute slew time plus a cal) takes 16.3 minutes. ...

FGS Instrument Handbook for Cycle 24 . ... Fine Guidance Sensor Instrument Handbook for Cycle 24 > Chapter 4: Observing with the FGS > 4.3 Position Mode Observing Strategies . ... 4.3.2 Drift and Exposure Sequencing . 4.3.3 Cross Filter Observations . 4.3.4 Moving Target Observation Strategy . ... In Position mode, the FGS can track a bright target (V ) whose motion is less than ~ 0.1 arcsec per second. ... Transfer mode observations of moving targets are discussed in the next section. ...

These observations are aimed at fully charactering FORS1 photometric system (UBVRI zero-points, color-terms and extinction coefficients) for the Tektronix 2048x2048 pixel CCD (24µm px) . To this aim, the two Landolt/Stetson photometric fields SA95 and SA101 will be observed on a number of epochs and at different airmasses during February and March 2007. ... SA101 . ... OBs for SA101 have to be observed during evenigh twilight (exceptions are expected for the second half of March) . ...

... Load the rpfits file and inspect d = scantable('2003-03-16_082048_t0002.rpf') print d # Make the quotient spectra q = d.auto_quotient(mode='time') print q del d # Plot/select in velocity q.set_freqframe('LSRK') q.set_unit('km/s') # Correct for gain/el effects q.recalc_azel() # Tid does not write the elevation q.gain_el() q.opacity(0.05) # Seperate data from the (1,1)&(2,2) and (4,4) transitions g1 = q.get_scan(range(6)) # scans 0..5 g2 = q.get_scan(range(6,12)) # scans 6.. ...

... The new emission line galaxies are listed in Table 2 containing the following information: . column 1: The object's IAU-type name with the prefix HS. ... This was not corrected in the figure shown in Appendix A. HS1214+3801 : This is seemingly a supergiant H II -region at the very rim of the nearby edge-on disc galaxy (SA(s)cd) NGC 4244 (V hel = 224 kms -1 and B T =10.88). ... To check this option one needs a detailed map of the NGC 4244 velocity field including HS 1214+3801. ...

Follow-up astrometry and recoveries are made with the ANU 40 inch (1.0-m) f/8 reflector at Siding Spring Observatory (IAU code 413). ... A routine follow-up of 2003 WY153 on 2003 Dec 15 became much more than routine when a faint object with unusual motion vector was found close to the target asteroid. ... During routine astrometry with the 1.0-m to improve the orbit of the Apollo asteroid 2004 CB, the asteroid was found on March 30 to have a short tail! ... Siding Spring Survey Main Page . ...

... 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. ...

... The choice of the spectrograph design (Fig.2) is determined by the quantity R, the overall dimensions of the PF cage and the restrictions on the rigidity of the structure of the device. ... As the camera's objective a fast 4-lens aplanat is used having a focal distance F cam =140 mm and a relative aperture of 1:1.8, the resolution at the centre is no less than 80 gr/mm, that over the field at a distance of 3 mm from the edge along the frame ( ) diagonal is 35 gr/mm. ...