... Dodson, Legge et al, ApJ, 2003 Spectral Line Sources · Requirement of high brightness temperatures means no thermal emission · Masers: Galactic Extragalactic · OH, H2O · OH, H2O, SiO, CH3OH · Galactic extra-galactic HI absorption VLBI arrays · VLBA (Very Long Baseline Array) Dedicated US array of ten 25m telescopes 330 MHz ­ 90 GHz · EVN (European VLBI Network) Formal collaboration of radio telescopes in Europe, Asia and South Africa ~15 telescopes 15m to 100m 330 MHz ­ 22/43 GHz ...

... Дни открытых дверей к юбилею САО РАН (12-14 апреля 2016 г.) . Международная конференция "Dark Ages and White Nights (Spectroscopy of the CMB)" (20-24 июня 2016 г.) . ... Международная конференция MULTI-SPIN GALAXIES - 2016 (26-30 сентября 2016 г.) . Международная астрономическая конференция "Физика звезд: от коллапса до коллапса" (3-7 октября 2016 г.) Архив . ... Подробнее.. ... 10.02.16 . ... БТА в реальном времени . ... Цейсс-1000 в реальном времени . ... Последнее обновление: 22/03/2016 ...

COS Instrument Handbook for Cycle 24 . ... Cosmic Origins SpectrographInstrument Handbook for Cycle 24 > Chapter 2: Special Considerations for Cycle 24 > 2.2 COS Observations Below 1150 е: Resolution and Wavelength Calibration Issues . ... COS Observations Below 1150 е: Resolution and Wavelength Calibration Issues . ... In such cases, for each CENWAVE and FP-POS position, a separate GO-wavecal exposure should be taken with Segment A ?on? immediately adjacent to the Segment B science observations. ...

... Science Users Information > Science Publications > Science Announcements > Improvement to FLAMES Spectral Resolution and Sensitivity . ... The FLAMES GIRAFFE spectrograph is not kept at a controlled temperature, and thus, at the beginning of every observing block, GIRAFFE is re-focussed to take account of collimator temperature. ... The updated values lead to a substantial increase in spectral resolution and sensitivity across all settings, particularly for the high resolution ( HR ) settings. ...

... Full details of the observations, data reduction and calibration of this survey, and the production of the 7C(G) compact source list, are described in Vessey & Green (1998, MNRAS, 294, 607) . ... b |<5њ, with a resolution of about 1.2 ? ... The survey consisted of 24 fields, spaced 3њ.5 in l , and alternating between b = +3њ and -3њ, but with a gap near l = 110њ. ... Please refer to the source list description for details of the entries ; the catalogue itself is available as: . ...

... 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. ...

... Thomson's multiple window method of spectral estimationthomson provides a very good estimate of the power spectrum by measuring the energy contained within a collection of rectangular shaped frequency intervals. ... Often, much of the fine structure of a spectral estimate is due to noise. It should be stressed that while other methods of spectral estimation (such as the Welchoppenheim method) exist, the Thomson method is particularly noteworthy for its precisely defined rectangular frequency bins. ...

... 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 . ...

Spectrophotometric resources (galaxies and stars) . HyperLeda home | ... LL_ELODIE "low-resolution" ELODIE archive . Resolution 0.055 nm (FWHM); W-range: 400 - 680 nm; 1388 stars; 1962 spectra . ... Resolution 0.013 nm (FWHM); W-range: 400 - 680 nm; 1388 stars; 1962 spectra . ... Resolution 0.4 nm; W-range: 580 - 1020 nm; 137 spectra; 126 stars . ... Resolution 1 nm; W-range: 480 to 770 nm; 18 spectra; 18 stars . ... Resolution 0.15 nm (FWHM); W-range: 395 - 475 nm; 78 spectra; 78 stars . ...

... R-band images obtained at 0.8 arcsec seeing conditions have allowed us to separate foreground star from point-like extragalactic source and estimate their brightness separately. ... To study the nature and properties of the source, we observed it under high spatial resolution. ... CONCLUSION RTT150 optical observations with sub-arcsecond seeing and low resolution spectra confirm the hypothesis of superposition of a radio source onto a `normal' F/G galactic star proposed by [1]. ...

HIGH RESOLUTION IONOSPHERIC MASS SPECTROMETER P-11 . ... Onboard mass-spectrometric equipment for study of neutral and ionized components of Earth upper atmosphere. Mass-spectrometer P-11 is one of P-series modifications of the on board radio-frequency monopole spectrometers. ... The instruments of P-series have passed successful approbation in space experiments aboard geophysical rockets MP-12, launched for investigation of Earth upper atmosphere (Ref. ... Measured mass number range, AMU - 1.. ...

... 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). ...

An efficient low-resolution NIR classification scheme for M, L, and T dwarfs and its application to young brown dwarfs L. Testi1, A. Natta1, F. D'Antona2, E. Oliva1,3, A. MagazzЫ3,4, F. Ghinassi3, J. Licandro3, Baffa1, G. Comoretto1, S. Gennari1 ... Telescopio Nazionale Galileo, 4INAF-Osservatorio di Catania) We present the preliminary results of a programme aimed at defining a low-resolution near-infrared spectral ... 2002). ... 2002, A&A, submitted Oliva 2000, Mem. ...

Next: PSF1DRB Up: PIXTOPIXSENS Previous: Generation from Ground Calibration Contents . Ideally the in-orbit PixToPixSens file will be generated from internal calibration measurements using the fullframe high resolution engineering mode. However due to their large data volume the fullframe high resolution data won't be available frequently enough to base the in-flight generation of the PixToPixSens file on the high resolution data. ... i.e. the average counts per pixel per CCD-frame . ...

... Aloisi, A. The Old Stellar Population . Alonso-Herrero, A. HST /NICMOS Observations of the . ... Balcells, M. HST-NICMOS Observations of Galactic . ... Baum, S.A. Investigating the Evolution of . ... Becklin, E.E. A Coronagraphic Search for . ... Clampin, M. The Old Stellar Population . ... Close, L. HST NICMOS Observations of . ... The Stellar Population in . Geballe, T.R. HST NICMOS Observations of . ... Greggio, L. The Old Stellar Population . ... Leitherer, C. The Old Stellar Population . ...

Next: Extragalactic Gravitational Wave Background Previous: Transparency of the Stochastic . Let the sky be observed with a detector having a pencil beam diagram across. The number of stars per frequency decade that is swept by the detector is a function of celestial coordinates (say, galactic coordinates l , b ): . ... It is clear from the figure that for an all-sky detector the Galaxy becomes transparent above the frequency  Hz. ...

Superconducting Integrated Submm Spectrometer for Laboratory Applications Specification: · Input frequency range : 200 ­ 700 GHz (covered by four exchangeable sensor modules each one covering range of about 100-150 GHz ); · Output frequency (IF) range : 1-2 GHz · Receiver noise temperature: below 500 K (direct ... The SIR chip is a superconducting integrated circuit comprising a quantum-noise-limited SIS mixer and a tunable Josephson local oscillator (LO). ...

... Thus all regions of the 0.94-2.50 micron wavelength range accessible from Mauna Kea can be recorded using five fixed angle gratings. ... Grating Angle . ... Efficiencies for the NIFS gratings are shown above. The NIFS spectrograph uses a Bouwers collimator and a refractive camera. ... With these assumptions, the NIFS system efficiency including the Gemini telescope optics but excluding the transmission of the adaptive optics system is about 0.17 e - /photon at J , and 0.22 e - /photon at H and K . ...

... 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. ...

High resolution IR-spectrometer . ... Determination of concentration of atmospheric greenhouse gases (carbon dioxide and methane) from ground-based or spacecraft platforms. ... Compact eschelle spectrometer is built by autocollimation scheme with diffraction grating operating in high orders of diffraction, allowing thereby to reach the resolution up to ?/ 20 000. ... For observations at the ground-based platforms and aboard the ISS the instrument modification RUSALKA will be used. ...