... HST . ... Home . ... Data . ... HST Peer Review Process . ... WFPC2 Home . ... Instrument Home . ... Calibration . Calibration Home . Calibration Plan . ... LRF Data . ... Data Analysis . Data Analysis Home . Data Analysis Library . ... Instrument Handbook . Data Handbook . ... Dither Handbook . ... Input "Frequency 0 " in relation: Flux = Flux 0 ( Frequency / Frequency 0 ) -(Spectral Index) . ... Values above 10 7 are taken to be frequency in Hz. ...

... Energy Levels . ... Examining the Balmer formula and also the Ritz combination principle (further below), Bohr suggested that atoms could exist (even briefly) only in certain energy levels , and light was emitted only when an atom descended from some higher energy level to a lower one. ... When an electron descends from a higher energy (large n) to a lower one (smaller n), by Balmer's formula together with Einstein's, the energy of the photon emitted was exactly the amount of energy given up: . ...

. ASME Paper 95-GT-437. Jacques Lewalle, jlewalle@syr.edu

The CHIANTI database consists of 4 primary ASCII files for each ion in the database. contains the energy levels in cm^(-1) It includes both experimental data and theoretical values of the levels energies. ... 2.0, March 1999, NIST Physical Reference Data %theoretical energy levels: Tayal S.S., 2000, ApJ, 530, 1091 %produced as part of the Arcetri/Cambridge/NRL 'CHIANTI' atomic data base collaboration % % P.R. Young, Feb 2000 . ... Tayal only tabulates transitions from levels 1 to 10 to higher levels. ...

A1629 2002-Feb-01 21:42:46 Technical Page Proposal Type: Regular General Category : Astronomy Sub- Category : Spectroscopy Observation Category : Extragalactic Total Time Requested: 24 Hours Proposal Title: A mini-survey for CO Emission at redshifts greater than 10 ABSTRACT: An exploratory program will place limits on faint spectral signals from the radio sky at 3 cm wavelength, which is a ... X Maybe Part of the observing run. ...

... Science Users Information > Science Activities > Instrument Commissioning > HARPS Laser Frequency Comb . ... HARPS Laser Frequency Comb . ... The first commissioning run of the HARPS Laser Frequency Comb ( LFC ) was held from 8 тАУ 17 April 2015. ... During this commissioning, the emphasis was mainly on calibration but several science spectra were acquired: four asteroids and twenty stars were repeatedly observed to monitor their radial velocity variations and to compare with published data. ...

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The Australia Telescope Compact Array ( ATCA ) is a radio interferometer consisting of six 22-m antennae aligned along a 6-km-long, east-west track. ... The ATCA Upgrade , which is part of the Major National Research Facility ( MNRF ) program, will allow astronomers to observe at even higher frequencies, around 22 GHz (12 mm) and 90 GHz (3.5 mm). ... The ATCA Upgrade will open a number of new opportunities; these are set out below. ... The ATCA Upgrade involves the following projects: . ...

... They are known: active quantum frequency standards on the ammonia molecules beams (molecular generator) on the hydrogen generator (hydrogen generator) passive quantum frequency standards on the Cs atoms’ beam (cerium atomic beam tube); active and passive quantum frequency standards with an optical pumping of Cs or Rb steams. The stability of atomic beam quantum frequency standard achieves 10^ - 14. ...

For calculating model spectra of early-type helium stars in LTE, we maintain a database of atomic data for, mostly, blue-visual absorption lines of light elements. The data is sorted with one file for each ion. ... III = ++ . ... It will work on both complete linelists (including the atomic data at the start and references at the end) or raw ion files (such as Ni2.d). ... A Fortran utility to convert linelists downloaded from the Vienna Atomic Line Database into the new QUB format. synspec_qub . ...

Next: Broadening Function Up: Basic Equations Previous: Basic Equations . After having crossed an absorbing cloud, the intensity of a source, I , is received by the observer as I( ) = I , where is the optical depth of the cloud. ... broadening function . ... l : lower level of the atomic transition . k : upper level of the atomic transition . rest wavelength of the transition . g : statistical weight of the lower level . g : statistical weight of the upper level . ...

Feed cabin Nr. ... Fig. ... This allows to realize the sensitivity at frequency ranges 4.8, 11.2 and 30.0 GHz of 5, 7 and 12 mK by double beam switching mode and by the integration time of the output filter 1s. Input waveguide paths were very long and had big losses. ... The focal line of the feed cabin Nr. ... Data Acquisition and Control System . The Data acquisition system of the feed cabin Nr 2 is based on the new measurement ER-DAS system (Embedded Radiometric Data Acquisition System). ...

... Астронет | ... рда.) область сантиметровых волн (длин волн) . ... рда.) сантиметровый диапазон (длин волн) . ... рда.) область декаметровых волн (длин волн) . ... рда.) декаметровыи диапазон (длин волн) . ... рда.) область дециметровых волн (длин волн) . ... рда.) дециметровый диапазон (длин волн) . ... рда.) область метровых волн (длин волн) . ... рда.) метровый диапазон (длин волн) . ... рда.) область миллиметровых волн (длин волн) . ... рда.) область субмиллиметровых волн (длин волн) . ...

The Laboratory of Electronic Kinetics ( LEK ) has powerful radio-frequency, microwave , cryogenic and high- magnetic - field sets of equipment , allowing to carry out precision phase-sensitive measurements of current and voltage in a frequency range 0-10 MHz and the microwave response of crystalline materials in cm-and mm- wavelength range in the temperature interval (0.1-300) K and in magnetic fields up to 18 T. Methodical principle of ... Magnetic field up to 18 T . ... Equipment . ...

... 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. ...

... We show the analysis of low-hard and intermediate states of sources XTE J1550-564, H 1743-322, GX 339-4, XTE J1859-226, XTE J1650-500 and GRS 1915+105. ... Directly applying the scaling technique we also obtain that a ratio of the BH masses in XTE J1859-226 and in XTE J1550-564 is , and the corresponding ratio for XTE J1650-500 and XTE J1550-564 is . These values of scaling factors r implies that BH masses are ; solar masses in XTE J1859-226 and XTE J1650-500 respectively. ...

spaceweb@oulu.fi - last update: 24 November 1998, 1335 UT . Radiowave Frequency Ranges . ... Extremely Low Frequencies . 30 - 300 Hz . ... 0.3 - 3 kHz . ... Very Low Frequencies . ... Low Frequencies . ... High Frequencies . ... 0.3 - 3 GHz . ... The International Telecommunication Union (ITU) has defined the radiowave frequency ranges as shown in the table. ... Their high frequency limit corresponds to magnetospheric ion gyrofrequencies (which are low because of small B and high m). ...

... The formation of spectral disturbances of Cosmic Background Radiation (CBR) during the period of hydrogen recombination at redshift is considered. Special attention is paid to the decimeter and meter wavelength band. ... In this paper we will return to the question on the spectral lines caused by recombination of hydrogen discussed by Dubrovich (1975) , in the longer wavelength part of spectrum of the CBR. ... A synthesis of recombination radiolines spectra is divided into several stages. ...

... Bad Astronomy . ... Mad Science . ... How fast must an object be travelling so the sound I perceive as it directly passes me will drop in pitch exactly one octave? ... When an object is moving past another object, any sound emitted by the first object is changed in pitch due to the relative motion. ... wl(emitted)" is the wavelength of sound emitted by the object at rest, "wl(heard)" is the wavelength you hear from the object, "v" is the velocity of the object, and "c" is the speed of sound. ...

To a special Solar Physics issue on the Bastille Day Event: . ... Multi-scale temporal features of the 14 July 2000 meter-wavelength dynamic radio spectrum compared with TRACE data . ... Figure 1 (100 KB). SOHO/EIT (a) and LASCO/C2 (b) images show the region of the eruptive flare event of 14 July 2000 and related halo CME. ... Figure 2 (47 KB). ... Figure 3 (115 KB). Medium-scale dynamic spectrum (a), 204 MHz metric (b) and 3000 MHz microwave (c) profiles of the "Bastille Day" event. ...