Next: Emission molecular bands Up: Optical spectrum of IRAS04296 Previous: Optical spectrum of IRAS04296 . We have obtained spectra of IRAS04296 with the CCD (1140 1170 pixels) equipped echelle spectrometer PFES mounted at the prime focus of the 6m telescope of SAO RAS (Panchuk et al. ... Figure: The IRAS04296+3429 spectrum near . Next: Emission molecular bands Up: Optical spectrum of IRAS04296 Previous: Optical spectrum of IRAS04296 Klochkova V.G. 12/20/1999 ...

Next: Accretion Disks with Up: StarsStellar Populations, Previous: Spectroscopic Analysis of . ... We present and discuss spatially resolved spectra of the accretion disk and the gas stream region as a function of distance from disk center, the spectrum of the uneclipsed light, and the radial temperature distribution in the ultraviolet. Keywords: Accretion disks, Cataclysmic variables . ... In this paper we report on the HST spectral mapping of the nova-like UX UMa. ...

... Many extragalactic objects for which radial velocities are desired display strong emission lines. ... EMSAO, a companion to the cross-correlation task XCSAO (Kurtz et al. 1992), was written to find emission lines automatically, compute redshifts for each identified line, and combine them into a single radial velocity. ... Figure: This EMSAO Summary page shows line centers and fit information for a night sky spectrum. ... To test EMSAO adequately, a lot of emission line spectra were needed. ...

... 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. ...

... In Fig. 2 the spectrum of the host galaxy HS1035+4758 is shown, in which typical HII-galaxy narrow emission lines are seen: H 4861, [OIII] 4959,5007, H 6562, [NII] 6548,6584 and [SII] 6716,6731 ?. ... The spectral evolution of SN 1998bv is illustrated in Fig. ... The change of the spectrum between April 6 and 19 with clear reddening shortward of H during these 2 weeks indicates seemingly that the 1st spectrum was observed in the period between the 20th and 30th days after the peak of the light curve...

... Publications with ESO Data . ... The tools have been developed for ESO by a team of astronomers at the Institute for Astro- and Particle Physics at the University of Innsbruck, as part of an in-kind contribution to ESO , which includes as well a model of the sky emission and transmission spectrum at Cerro Paranal. ... Skycorr provides an advanced instrument-independent sky-correction tool that removes sky emission in science spectra by means of sky spectra taken at a different time and sky location....

... The resulting spectra were analyzed with a kinematic Monte Carlo model which allows estimation of the OH production rate, neutral gas outflow velocity, and distribution of the out-gassing from the nucleus. ... The best-fit model spectrum is shown together with the observed line. ... Both models are scaled to match the average off spectrum. When the same scaling is applied to the nucleus-centered model spectra, shown on the right, it is clear that only the quenched model matches the observations. ...

... We have started a programme of observations of nearby starburst and AGN galaxies with MICHELLE, with the aim of investigating the spatial extent of "Unidentified Infrared Bands (UIB)" emission in these galaxies, and in particular relating these to multi-frequency matched resolution radio maps. ... The spatially integrated MICHELLE spectrum of NGC 7469 in the 8 - 11.5µm range shows an equivalent width of 11.3µm UIB feature which is much smaller then measured by ISO. ...

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