... HST . ... HST Overview . ... Data Analysis . ... Instrument Handbook . ... Important information on sensitivity can be found in Chapter 4: Imaging of the NICMOS Instrument Handbook, as well as in Appendix 1: Imaging Reference Material of the NICMOS Instrument Handbook. ... Important updates, discoveries and developments that could potentially affect NICMOS observations, calibration, or data analysis. ... The HST Data Handbook is the primary guide for calibration, reduction and analysis of NICMOS...

... 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. ...

In calculating the NIFS sensitivity, we adopt a read noise of 5 e - , a dark current of 0.01 e - s -1 pix -1 , and a maximum exposure time of 3600 s. Grating . ... e/pix) . ... OH Cont. (e/pix) . ... NIFS should achieve signal-to-noise ratios of ~ 10 per spectral pixel in a 0.1" 0.1" aperture for single 1800 s exposures on uniform, extended, continuum sources with surface brightnesses of J = 15.4, J = 15.0, H = 14.8, and K = 13.5 mag arcsec -2 using the Z , J , H , and K gratings, respectively. ...

. Next: Finding periodic signals Up: Searches and surveys Previous: Searches and surveys . љ . Individual pulses detected for few pulsars . Detectability peaks new 400MHz for most . Typical sky background Jy . Typical pulsar flux few MJy . љ љ . Figure 9: Sensitivity of the Parkes survey . Jon Bell . Thu Dec 19 15:15:11 GMT 1996

. Next: Spectral-Line Observing Up: Astronomer's Guide to the Previous: Pulsar Observing . The prospective new user may be unfamiliar with computing the sensitivities to be expected from using the Arecibo telescope. Hence, we present here some formulae for calculating the rms noises that can be expected for various forms of observing at Arecibo. Subsections . Spectral-Line Observing . Pulsars . Robert Minchin 2012-02-22

... 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 following table gives the sensitivity of field center, distortion, and image size to various misalignments of the optical elements in the 2.5 m telescope. ... The repointing is done so as to keep the center of the focal plane pointed to the same position on the sky. ... Field shift (this is the mean shift in object positions in the focal plane before repointing the telescope) . ... Image properties are measured for an array of points in the focal plane. ...

In the PROJECT we are using the following peculiar . features of RATAN-600 . ... Brightness temperature sensitivity being equal to the antenna temperature sensitivity .. ... Receiver system .. ... Using aperture averaging effect. dual- beam and dual (multi-) frequency filtration, we demonstrated full filtration of the atmosphere noise down to the receiver noise at all scales of acoustics peaks ( Fig.1 , Fig 2 ). ... We select this frequency as the central one in our project. ... Antenna surface . ...

Next: X--ray Quiet PMS Up: Contents Previous: Fits to Evolutionary . The X--ray selected PMS candidates may not constitute a complete list. The primary factor is the sensitivity limit, complicated by the vignetting in the field of the PSPC which was used to make the source list. ... In order to better understand the completeness of the X--ray data, photometry of every star in both regions was undertaken. ... The X--ray quiet sources are distributed evenly across the field (see Figure 8 ). ...

... Telescope concept . ... The Submillimetron Project is dedicated to astronomical studies at the submillimeter and far infrared wavelengths using a cryogenic telescope located on the Russian segment of the International Space Station (ISS). The Astro Space Center of the Lebedev Institute of the Russian Academy of Sciences is responsible for developing the Submillimetron Project. ... Currently, the Astro Space Center is carrying out a pre-Project study under contract with the Russian Space Agency. ...

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... Extreme sensitivity photon counting systems . ... Resolution to 3080 x 2304 pixels x 16 on photon counting systems . ... These can be coupled to a suitable scintillator to match customers' requirements, and to provide imaging covering the electromagnetic spectrum from UV to high energy gamma rays and particles. ... Photek image intensifiers and photon counting tubes are used in CERN and are chosen for the ACE explorer satellite system for reading out arrays of scintillating plastic fibre. ...

Detector of hydrogen isotopes (ISIV) . ... Measurements of hydrogen isotopes content in surface layer of a solid (provided that the content is more than 0.01 %). ... Content of hydrogen isotopes of a sample is measured by nondestructive technique of direct measurements in the surface layer. ... Measurable hydrogen isotopes content   ~0.01 wt. ... Area surface of sample                                         ~10 cm 2 . ... G. Dolnikov +7(495)333-25-66, ggd@iki.rssi.ru . ...

Sensitivity for indexes 05: S D-0.25'/mm= 1.56nT/mm, S H-0.63nT/mm, S Z-0.27nT/mm Base values for indexes 05: Do=2*35,8', Ho=21300nT, Zo=43765nT Sensitivity for indexes 10: SD-9.3nT/mm, SH-10nT/mm, SZ- 9.3nT/mm

... Over the first 4 years, its X-ray telescopes eROSITA and ART-XC will survey the whole sky with a record sensitivity in the 0.5-10 keV energy band. ... The goal of the second international Spectrum-RG conference is to discuss the different scientific topics addressed by the mission, synergies with surveys at other wavelengths, and requirements to follow-up observations.Contributed talks and poster presentations are invited on the topics related to the SRG science goals. ... Active galactic nuclei . ...

... Status of the ELECTRON experiment . ... The objective of the ELECTRON experiment is to perform 3-D measurements of the plasma electrons in the energy range from 10 eV to 26000 eV, with good angular resolution, sensitivity and large dynamical range. ... Figure 1 presents the ELECTRON sensor. ... Click on the picture to view large one) . ... Figure 3 shows dynamical spectra with counting rate measurements performed by ELECTRON experiment during very multiple magnetopause crossings on February, 4, 1996...

... 2004: . Creation of a unique set of the spectral and polarization complex of high resolution in the range of 6-18 GHz, consisting of 64 channels with a 1% analysis stripe was concluded. Based on the combination of key parameters - the frequency overlap and resolution, sensitivity and accuracy of polarization measurements, such a complex is the first instrument of its kind in the practice of solar astronomy. ... Archive . ...

... Armagh Observatory, College Hill, Armagh BT61 9DG, +44 (0)28 3752 2928 . ... The present-day DD population is examined as a function of Galactic star-formation history alone. It is shown that the frequency distribution, in particular, is a sensitive function of the Galactic star formation history and could be used to measure the time since the last major star-formation epoch. ... Last Revised: 2012 November 22nd . ...

The basic characteristics of the instrument are set by the aperture, focal length and resolution of the image forming lens, the dispersion of the spectrometer, and the sensitivity of the detector. ... The lens is internally focused, and maintains acceptable focus (2 pixels in the detector plane) over a typical spectral coverage of one grating setting. ... along the spatial dimension of a 25mm square detector in the final spectral image plane the 400mm lens is 3.2њ. ... Diffraction grating . ...

The new generation radio interferometer . ... 5000 km on the basis of square kilometer phased arrays. It is shown that this interferometer will have the sensitivity ~ 1 mJy at a frequency 100 MHz. ... VLBI interferometer, Active Galactic Nuclei, cosmology, effective area, sensitivity. ... Для исследований физических условий в активных ядрах галактик и космологических исследований необходимы низкочастотные наблюдения компактных радиоисточников с большой чувствительностью и разрешением. ...