No Arabic abstract
From the available STIS data of RR Tel, that have provided a coverage with absolutely calibrated data in a wide wavelength range, we have obtained a new determination of its reddening (E(B-V)=0.00) from the comparison of the observed HeII Paschen lines decrement relative to HeII lambda 4686 (for 24 HeII Paschen lines down to the region of the head of the series near lambda 2060 A) with the theoretical one as given in Storey and Hummer (1995) for case B, T=10,000 K and log Ne=6. This new E(B-V)=0.0 value has been confirmed from a re-analysis of the IUE low resolution data. We recall that the so far generally adopted value in the literature has been E(B-V)=0.10 as obtained by Penston et al. (1983).
The exceptional resolution of UVES has allowed the detection of weak spectral features and the separation of components in blended lines. The intensities of all of the OIII fluorescence lines produced by the O1, O3 and other channels, including the 5592 Angstrom charge-exchange line, have been measured and their ratios compared with models.
A new measure of reddening (E$_{(B-V)}$$sim$0.00) has been obtained from the comparison between the observed and the theoretical intensity decrement for 20 emission lines of the $ion{He}{ii}$ Fowler (n$to$3) series. This value has been confirmed by the STIS and IUE continuum distribution, and by the value of n$_H$ from the damped profile of the IS H Ly-$alpha$ line. We have obtained very accurate measurements for about thirty Bowen lines of $ion{O}{iii}$ and a precise determination of the efficiency in the O1 and O3 excitation channels (18 % and 0.7 %, respectively). The relative $ion{O}{iii}$ intensities are in good agreement with the predictions by Froese Fischer (1994). A detailed study of the decays from all levels involved in the Bowen mechanism has lead to the detection of two new $ion{O}{iii}$ Bowen lines near $lambda$ 2190. High resolution IUE data have shown a nearly linear decline with time, from 1978 to 1995, in the efficiency of the O1 and O3 processes, with a steeper slope for the O3 channel. A detailed study of the $ion{N}{iii}$ $lambda$ 4640 lines and of their excitation mechanism has shown that, recombination and continuum fluorescence being ruled out, line fluorescence remains the only viable mechanism to pump the 3d $^2D_{5/2}$ and 3d $^2D_{3/2}$ levels of $ion{N}{iii}$. We point out the important role of multiple scattering in the resonance lines of $ion{O}{iii}$ and $ion{N}{iii}$ near $lambda$ 374 and show that the observed $ion{N}{iii}$ line ratios and intensities can be explained in terms of line fluorescence by the three resonance lines of $ion{O}{iii}$ at $lambda$$lambda$ 374.432, 374.162 and 374.073 under optically thick conditions.
We present here the first results of UVES observations of RR Tel. The exceptional performances of the instrument have allowed the detection of new spectral features and have led to an improvement in the identifications of several emission lines. A direct comparison with the IUE observations in the range 3045-3300 A has revealed the appearance of many weak and shallow lines, most of them lacking a convincing identification. The Balmer lines are visible up to H38 and are accompanied by the He II lines of the Pickering series. Also, all of the He II emissions of the Pfund series, from 5858 A to 6408 A have been detected. We made definite identifications of additional TiO bands at 4955 A (alpha R_2 1-0), 5167 A (alpha R_2 0-0), 5445 A (alpha R_2 0-1), 5598 A (beta R_1 0-0), 5847 A (gamma R_1 1-0), and 6148 A (gamma {^S} R_21 0-0). The Halpha line has very wide wings, extending to at least 5000 km/s, which are similar to those reported for the planetary nebula IC 4997 and attributed to Raman scattering by Ly beta photons. A selective pumping mechanism via the HeII 237 A emission is proposed to explain the intensity of the high-lying lines of O IV mult. 1 and 2.
We present new high-resolution (R~14,000) spectra of the two brightest HeII-transparent quasars in the far-UV (FUV) at z>3.5, HE2QSJ2311-1417 (z=3.70) and HE2QSJ1630+0435 (z=3.81), obtained with the Cosmic Origins Spectrograph (COS) on the Hubble Space Telescope (HST). In the predominantly saturated HeII absorption spectra, both sightlines show several isolated resolved (full width at half maximum FWHM>50 km/s) transmission spikes in HeII Ly$alpha$ and HeII Ly$beta$. The incidence of such spikes decreases with increasing redshift, but both sightlines show significant spikes at z>3.5, signaling the presence of fully ionized regions in the z>3.5 intergalactic medium (IGM). We employ an automated algorithm to compare the number of detected HeII transmission spikes to predictions from mock spectra created from the outputs of a cubic (100/h cMpc)^3 optically thin Nyx hydrodynamical simulation, assuming a range of UV background photoionization rates $Gamma_mathrm{HeII}$. From the incidence of Ly$alpha$ and Ly$beta$ transmission spikes we infer similar photoionization rates of $Gamma_mathrm{HeII}=2.0^{+0.6}_{-0.5}times 10^{-15}$s$^{-1}$ at 3.51<z<3.66 and $Gamma_mathrm{HeII}=0.9pm0.3 times 10^{-15}$s$^{-1}$ at 3.460<z<3.685, respectively. Because the transmission spikes indicate fully ionized regions at z>3.5 along both lines of sight, our observations provide further evidence that HeII reionization had substantially progressed at these redshifts.
We present far- and near-ultraviolet absorption spectroscopy of the $sim$23 Myr edge-on debris disk surrounding the A0V star $eta$ Telescopii, obtained with the Hubble Space Telescope Space Telescope Imaging Spectrograph. We detect absorption lines from C I, C II, O I, Mg II, Al II, Si II, S II, Mn II, Fe II, and marginally N I. The lines show two clear absorption components at $-22.7pm0.5$ km s$^{-1}$ and $-17.8pm0.7$ km s$^{-1}$, which we attribute to circumstellar (CS) and interstellar (IS) gas, respectively. CO absorption is not detected, and we find no evidence for star-grazing exocomets. The CS absorption components are blueshifted by $-16.9pm2.6$ km s$^{-1}$ in the stars reference frame, indicating that they are outflowing in a radiatively driven disk wind. We find that the C/Fe ratio in the $eta$ Tel CS gas is significantly higher than the solar ratio, as is the case in the $beta$ Pic and 49 Cet debris disks. Unlike those disks, however, the measured C/O ratio in the $eta$ Tel CS gas is consistent with the solar value. Our analysis shows that because $eta$ Tel is an earlier type star than $beta$ Pic and 49 Cet, with more substantial radiation pressure at the dominant C II transitions, this species cannot bind the CS gas disk to the star as it does for $beta$ Pic and 49 Cet, resulting in the disk wind.