... HST . ... Data . ... HST Overview . Overview . ... Instruments . ... Instrument Handbook . COS Data Handbook . ... For more information about the use of this FP-POS option see Section 5.8.2 of the COS Instrument Handbook. ... COS has the advantage of a fairly large aperture so that there are only small aperture losses ( see Section 5.1.9 of the COS IHB). ... The available spectroscopic resolving powers (R) available to observers with COS are listed in Table 5.1 of the COS Instrument Handbook. ...

... We will consider the rms, (K), for observations with a receiver of system temperature, T , frequency resolution, per polarization, and total integration time per observing cycle, . ... For ``in-band'' frequency switching, the line under investigation is always in the observing band. ... Position Switching or ``Out-of-Band'' Frequency Switching: Here the line is only observed for one half of the time, with noise being present all of the time. ...

Next: Pulsar bin-mode observations Up: ATCA Bin Mode Observations Previous: ATCA Correlator Bin Modes . Miriad 's atlod task has an option, options=hires which converts a RPFITS file observed in high time resolution bin-mode into an apparently normal dataset with fine time resolution. ... In high resolution time mode, the time difference between consecutive integrations might be smaller than this tolerance. ... Miriad manager . ...

Next: Gravitational Wave Background from Previous: Galactic Gravitational Wave Background . ... It is intuitively clear that at frequencies above the critical ones for our Galaxy, one will detect rare bright jerks produced by coalescing white dwarfs   (at a rate of 1 per 100 year) and NS (at a rate of 1 per - year) in our Galaxy, against a background of the extragalactic stochastic GW. ... Firstly we consider GWB from close individual galaxies, and then will discuss overall extragalactic GWB. ...

... The J, H and K bands are characterized by a bright background, such a background is mainly due to the emission of atmospheric lines and of thermal radiation. ... If the source cover a large fraction of the slit, spectra off-source must be observed to adequately sample the sky background. ... The on chip integration time (time spent in each position of the slit) must not exceed 40 seconds in J and H bands and 60 seconds in K band. ... We suggest a sequence of 10 for each elementary integration time. ...

... December 21, 1997 . ... Advantages are briefly discussed of gaining in spectral resolution, which is accompanied by losses in signal level, as compared with the attempts to improve the accuracy of measurement of line parameters by means of rising the S/N ratio alone with increasing the exposure time. To partially solve the problem of observations of faint objects at the BTA a new design echelle spectrometer is proposed. high resolution spectroscopy . ...

... Science Publications > Science Announcements > 8th VLTI Summer School: High angular resolution in astrophysics: optical interferometry from theory to observations . ... Observing with ESO Telescopes . ... ESO-MIDAS . ... ESO Data . ... ESO HST Image Galleries . ... ESO Data Access Policy . ... ESO Science Newsletter . ... Optical/infrared long-baseline interferometry has reached a new stage with the advent of multi-telescope arrays accessible to a broad community of astronomers, most notably VLTI . ...

M1 image More About M1 Nice Color Picture . ... M16 image More About M16 HST image . ... M31 image More About M31 Nice Color Picture . ... M42 image ; M43 image More About M42/43 Nice Color CCD Picture . M51 image More About M51 Color Image of M51 M51 Supernova . M57 image More About M57 Nice Color CCD Picture Very Deep M57 Image . ... M81 image More About M81 M81 Supernova Ultraviolet Image of M81 More about Ultraviolet Imaging . M82 image More About M82 M82 False Color M82 True Color . ...

... Data Analysis SAS News What is SAS? ... Back to Calibration Homepage The most recent Canned Response Matrices can be downloaded here (please refer to Update 2014-11-24 ) and can be used to estimate EPIC count rates in AO15. ... PN response files . ... MOS response files . Since SAS 6.5 the full set of ready-made MOS response files is not provided (see "Update 2005-12-15" ). ... Note: MOS response files before SAS 6.5 had a different nomenclature as the one listed above (see "Update 2005-12-15" ). ...

... 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. ...

... A radio galaxy is a galaxy that emits an unusually big amount of energy at radio wavelengths. ... Inside of each galaxy with an active nucleus (radio galaxies are among them) there must be a system of a "central machine" responsible for the colossal amount of the emitted energy from radio to gamma ranges. ... Sometimes a radio source in an active galaxy may flare again if the needed conditions appear (a new portion of matter would fall into the furnace of the "central machine"). ...

... The following charts/text are intended as tools for monitoring the Type Ia supernovae ( SNe ) event visually or photographically (utilizing telescope equipped CCD equipment).The files include: A replication of The Type Ia SNe , V- magnitude (with data point checks from other cited references)and color index (B-V) templete (to indicate a general color-related trend of the type Ia ... I believe this might help alleviate some of the problems involving the making of acceptable amateur light curves...

... Exposure Time Calculator (ETC) . ... ESO - Public Surveys . ... the recommended values to use for DIT, . ... Detector on-chip integration (DIT): seconds. to your chosen value - a separate page gives recommended values to use for DIT - for modes 1 and 2 below you may wish to start with the maximum recommended values as these will minimize the effect of read noise (a total object exposure of Y secs with DIT=X secs will produce Y/X lots of read noise) and give you a lower limit on the time needed. ...

Next: AXAF Recipes Up: ROSAT HRI Recipes Previous: Quantum Efficiency Correction (a.k.a. For some observations, a significant amount of data may have been rejected during SASS processing because the background level was higher than the calculated threshold for rejection. ... REJECTED EVENTS . ... The recipe will allow the user to include rejected events in the generation of a new qpoe file and filter on the background level. ... This creates a qpoe file with standard + rejected events. ...

... We can help students grasp the significance of Hubble's extremely keen eye, and learn a bit about angles and math in the process, with the following in-class activity. ... Looking through binoculars or telescopes allows us to magnify a small section of the sky. To measure sizes or distances in that small section, astronomers divide a degree into 60 smaller pieces called arcminutes, and further subdivide minutes into 60 smaller sections called arcseconds. ... 30 feet = . ... 36 seconds . ...

... Astrophysics Group . ... VSA . ... CAT . ... The Very Small Array is a custom-built radio telescope (operating between 26-36 GHz), designed expressly to make high resolution observations of the cosmic microwave background (CMB) radiation on angular scales around and below one degree. ... The VSA has been operated in ?compact array? and ?extended array? configurations (see the technical description below) and data collected to achieve high sensitivity in both regimes have been analysed. ... 1.75 GHz)...

... The MMT optical spectra of SBS 0335-052W were obtained on 1996 January 19 with the Red Channel of the MMT Spectrograph. ... The linear scale is 1 = 263 pc at the distance to SBS 0335-052W of 54.1 Mpc. ... In Table 1, the observed line intensities and intensities corrected for interstellar extinction for SBS 0335-052W are shown along with extinction coefficient C (H ), observed flux of the H emission line, the equivalent width EW (H ) and equivalent width of absorption Balmer hydrogen lines EW (abs)....

In 2007-2008, the planet Uranus will reach one of its annual equinoxes for the first time since 1966. As a consequence, its five major satellites orbiting in the equatorial plane will undergo a season of mutual eclipses and occultations very similar to the one that Jupiter's Galilean satellites undergo every 6 years. ... Some of these events occur when Uranus is at conjunction, or the satellite is transiting or too close to the limb of the planet. ... Complete table of events . ...

. Statistics of sunspot activity . The sunspot indices . My observations . NGDC's observations . The solar regions . Links . About authors . Russian pages . About authors . Observer: Alexey Ryback . Web-design: Alexander Burkov .

RADIOASTROPHYSICAL DEPARTMENT • INSTITUTE OF SOLAR-TERRESTRIAL PHYSICS RAS SB . General information Main characteristics of the Radio telescope Observing programs General view of the antenna array Main research areas Principle of generation of radio images Radio telescope 's beam Receiving systems Main characteristics of the base receiving-recording complex Calibrations Data archive and databases Publication SSRT - Siberian Solar Radio Telescope . ...