Next: Radial velocity of the Up: Optical spectrum of IRAS04296 Previous: Observations and spectra reduction . ... However, molecular emission features are only very rarely observed in the optical spectra of PPNe. ... On the other hand, it is well known that cometary nuclei spectra show prominent Swan band emission. In both spectra of IRAS04296 we have discovered strong emission in the (0;0) and (0;1) bands of the Swan system of the molecule. ... Now consider the case of IRAS04296. ...

... 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. ...

... References: %observed energies (n=2,3,4): Del Zanna , Chidichimo, Mason, 2005 , A , 432, 1137 %observed energy levels (n=5): Shirai,T., et al, 2000, J.Phys.Chem.Ref.Data, Monograph 8 %observed energy levels (97,100): Landi Phillips 2005 , ApJ, in press %observed energy levels (above ionization): Palmeri P., Mendoza C., Kallman T.R., Bautista M.A., 2003, A , 403, 1175 %theoretical energies ( ...

The figure below shows what stellar spectra are like in this wavelength range. All stars hotter than about 3000 K effective temperature radiate like a hot blackbody at these long wavelengths, possibly with a very few atomic lines (of Hydrogen, in the A-type stars) or molecular bands (the CO band overtone near 2.25 microns for example, in K-type stars and G-type stars). ... unusual features: mixed chemistry sources, Wolf-Rayet stars, ice bands, featureless carbon-star spectra ...

... 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. ...

Observation and modelling of main sequence star chromospheres. ... We compare our calculations to recent high res­ olution observations for selected stars in a narrow spectral range ((R­I) џ =0.875\Sigma0.05); we show that Hff line profiles behave as expected, with a tight correlation be­ tween the line width and equivalent width. ... We show that the hydrogen series dominate the radiative cooling in the spectral lines (form 40% to 90%) for Hff emission line stars. ...

... In order to compare the number of different evolutionary stages obtained and X-ray luminosity of the chosen X-ray sources with the observed galactic values we use the sum of C/O+O/C , where C and O are the calculated and observed values of a given binary type, respectively. If we make comparison for a number of different binary species (for example, we compare the number of CV, number of X-ray pulsars,   total X-ray luminosity of LMXB, etc.), we write this criterion in the form: . ...

... 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 ...

... Fitting the observed dependence includes calculations of the polarization cross-sections averaged over particles orientation and size distribution, their normalization and the comparison of obtained dependencies with Serkowski's curve representing observational data for a chosen star. ... Variations of the polarization factors with wavelength are shown in Fig. 16 for homogeneous spheroidal particles with PF orientation. ... The distinction between prolate and oblate spheroids is also clearly seen. ...

function flux _to_em, emis , flux = flux , logT = logT , wvl = wvl ,Z=Z,NH=NH,defEM=defEM,$ noph=noph, thresh = thresh , _extra=e ;+ ;function flux _to_em ; return emission measures (-1 where undeterminable) at various ; temperatures consistent with given line fluxes and line emissivities. ; ; for each temperature, assume a delta-function emission measure, ; compute ...

RADIOASTROPHYSICAL DEPARTMENT • INSTITUTE OF SOLAR-TERRESTRIAL PHYSICS RAS SB . Research results on fast active processes 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 ... Distribution of the recorded spikes in duration . ...

... Science Users Information > Science Publications > Science Announcements > Observing Time Calcaulation for APEX Instruments Artemis and Supercam . ... Observing with ESO Telescopes . ... A new observing time calculator is now available for the Artemis 350ТЕm camera offered on APEX in Period 94 . ... However, to estimate the observing time request, the Swedish Heterodyne Facility Instrument ( SHFI ) on-the-fly calculator should be used, and the time request should be divided by a factor of 13 . ...

Appendix C Radiative Transfer for a Two-Level System This appendix details how to derive the total column density of a linear rigid-rotor molecule, such as CO, from the observed brightness of its rotational transition. ... C.2 Radiative Transfer for a Two-Level System I now consider emission in a two-level system from an upper J + 1 (denoted `u') to lower J (denoted `l') state. ... Spontaneous emission is controlled by the A coefficient, with a rate Aul nu . ... Tex exp(-31. ...

We report here on those proposed UIT targets that, in fact, were successfully acquired. ... Note on Filters: . A1 centered at 2500 angstroms with a width of 1200 angstroms . ... NGC 2300 is in a small group of galaxies which has a substantial amount of X-ray emission. ... LUNA again for 777 through lots of filters. ... Supernova 1987A in the Large Magellanic Cloud was observed for 3740 seconds through B5, A1 and B1. ... NGC 5128 or Cen A was observed for 1454 seconds through the B1 filter. ...

PENTICTON SOLAR RADIO FLUX VALUES (from SGD Explanation of Data Reports) Daily Solar Flux Values - Penticton -- Daily measurements of the integrated emission from the solar disc at 2800MHz (10.7cm wavelength) have been made by the National Research Council of Canada since 1947. ... The data are tabulated in two forms: the "observed flux" (S), and the "adjusted flux" (Sa). ... The "observed flux" values are useful in ionospheric physics and other terrestrial consequences of solar activity. ...

Solar Eruptive Event of 4 November 2001 observed with the SPIRIT Telescope on Board the CORONAS-F Satellite . ... Based on the data of the SPIRIT telescope on board the CORONAS-F satellite in three EUV channels 175, 284, 304 , we have analyzed large-scale manifestations of the post-eruptive so-lar activity followed one of the most considerable and geoeffective coronal mass ejection (CME) in the 23rd cycle which occurred on 4 November 2001. ... Posteruptive arcade on the CORONAS-F/SPIRIT movies at . ...

... 8 February , 2014 SAI seminar (Ryde et al 2010) 5 Thermal emission from GRB jet progenitor observer photon jet Photosphere (=1) · · · · Photons are not produced at the photosphere We have to calculate radiative transfer We need to know where the photons are produced We construct the expression for effective optical depth in relativistic flow considering random walk process in relativistic flow SAI seminar 6 8 ... 8 February, 2014 SAI seminar 28 ...

The problem of solar wind data correlation for the observations onboard several spacecraft is very important for three points of view: . ... This problem is studied now in detail by systematic determination of ion flux and ion velocity data correlations by INTERBALL-1 (IKI group), WIND and IMP 8 (both - MIT group). ... Solar wind plasma correlation lengths from IMP 8, WIND and INTERBALL-1. ... Correlation of solar wind observations onboard several spacecraft: INTERBALL-1, IMP 8 and WIND data. ...

... 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...