Results 1 - 10 of 4160
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[en] Careful reductions of the short wave prime camera (SWP) spectrum was carried out. A line by line inspection of the spectrum was used to eliminate spurious spikes and a median filter applied to eliminate high frequency noise. Upper limits were obtained for far ultraviolet emission from a hot galactic halo
[en] We present absorption line analysis of the outflow in the quasar IRAS F04250-5718. Far-ultraviolet data from the Cosmic Origins Spectrograph on board the Hubble Space Telescope reveal intrinsic narrow absorption lines from high ionization ions (e.g., C IV, N V, and O VI) as well as low ionization ions (e.g., C II and Si III). We identify three kinematic components with central velocities ranging from ∼-50 to ∼-230 km s-1. Velocity-dependent, non-black saturation is evident from the line profiles of the high ionization ions. From the non-detection of absorption from a metastable level of C II, we are able to determine that the electron number density in the main component of the outflow is ∼<30 cm-3. Photoionization analysis yields an ionization parameter log UH ∼ -1.6 ± 0.2, which accounts for changes in the metallicity of the outflow and the shape of the incident spectrum. We also consider solutions with two ionization parameters. If the ionization structure of the outflow is due to photoionization by the active galactic nucleus, we determine that the distance to this component from the central source is ∼>3 kpc. Due to the large distance determined for the main kinematic component, we discuss the possibility that this outflow is part of a galactic wind.
[en] The far-ultraviolet (FUV) number counts of galaxies constrain the evolution of the star formation rate density of the universe. We report the FUV number counts computed from FUV imaging of several fields including the Hubble Ultra Deep Field, the Hubble Deep Field North, and small areas within the GOODS-North and South fields. These data were obtained with the Hubble Space Telescope (HST) Solar Blind Channel of the Advance Camera for Surveys. The number counts sample an FUV AB magnitude range from 21 to 29 and cover a total area of 15.9 arcmin2, ∼4 times larger than the most recent HST FUV study. Our FUV counts intersect bright FUV Galaxy Evolution Explorer counts at 22.5 mag and they show good agreement with recent semi-analytic models based on dark matter 'merger trees' by R. S. Somerville et al. We show that the number counts are ∼35% lower than in previous HST studies that use smaller areas. The differences between these studies are likely the result of cosmic variance; our new data cover more lines of sight and more area than previous HST FUV studies. The integrated light from field galaxies is found to contribute between 65.9+8-8 and 82.6+12-12 photons s-1 cm-2 sr-1 A-1 to the FUV extragalactic background. These measurements set a lower limit for the total FUV background light.
[en] The spectrum of the observed far-ultraviolet background at high galactic latitudes provides superficial evidence of radiation from neutrino decay, but the spectrum is so uncertain that conclusions are not possible. A limit of approximately 300 photons (cm2 sec ster A)-1 is set on any non-stellar ultraviolet flux above latitude 200. The disagreement between the Berkeley and the Johns Hopkins ultraviolet background radiation data is analysed
[en] Two modifications of photomultipliers - with massive and translucent photocathodes are described. Cesium iodide is used as photocathode material. Main specifications are as follows: range of spectral sensitivity, Mm:0.11-0.24 (MgF2); 0.12-0.24(CaF2); spectral anode sensitivity within λ=120 nm wavelength with 2x104A/W, time of anode pulse increase -≤3ns; maximal anode current - 200 mA; amplification ratio -105-106; dark current at the anode - 200 mA; at 20 deg C ambient temperature and at 3 kV supply voltage - maximum 3x10-10A; supply voltage - 2.5-3 kV
[en] A review is presented of the young field of extreme-ultraviolet astronomy at wavelengths from 50 Angstroem to 912 Angstroem. In recent years, it was realized that observations in this wavelength band could be performed due to the lucky circumstance that the sun is located in an extended region of extremely low interstellar gas density. Hence, the horizon for observations at 100 Angstroem due to the photoelectric opacity of the interstellar medium is typically at a distance of about 200 pc. Since 1975 a series of rocket and satellite observations have yielded the first positive results. Sources which radiate primarily in the extreme ultraviolet have been detected and even the small list of currently observed objects has had immediate impact on the studies of both stellar evolution and the interstellar medium. Diffuse emission from the interstellar medium results from a hot 105 to 106 K component of the interstellar gas. Prime stellar candidates for extreme-ultraviolet observations are (1) hot low-luminosity stars at the blue end of the HR diagram as, e.g., white dwarfs at the beginning of the cooling sequence, (2) atmospheric emission from stars surrounded by a hot corona or with flaring activity, (3) mass-exchanging binary systems as, e.g., main-sequence close binaries or catalysmic variables. The article discusses the prospects of extreme-ultraviolet astronomy and reviews the existing observations of extreme-ultraviolet emission from the interstellar medium and from stellar sources of the different categories. (orig.)
[en] A series of plane-parallel photodissociation region (PDR) models are calculated using the spectral synthesis code CLOUDY. These models span a wide range of physical conditions, with gas densities of n = 102 - 106 cm-3 and incident far-ultraviolet (FUV) fields of G0 = 100 - 106 (where G0 is the FUV flux in units of the local interstellar value), which are comparable with various astrophysical environments from interstellar diffuse clouds to the dense neutral gas around galactic compact H II regions. Based on the calculated results, we study the thermal balance of PDR gas and the emissions of [C II], [C I] and [O I] fine-structure lines under different physical conditions. The intensities and strength ratios of the studied lines, which are frequently used as PDR diagnostics, are presented using contour diagrams as functions of n and G0. We compare the calculated PDR surface gas temperatures Ts with those from Kaufman et al. and find that Ts from our models are systematically higher over most of the adopted n-G0 parameter space. The predicated line intensities and ratios from our work and those from Kaufman et al. can be different by a factor greater than 10, and such large differences usually occur near the border of our parameter space. The different methods of treating the dust grain physics, the change of H2 formation and dissociation rates, and the improvement in the radiation transfer of line emissions in our CLOUDY models are likely to be the major reasons for the divergences. Our models represent an up-to-date treatment of PDR diagnostic calculations and can be used to interpret observational data. Meanwhile, the uncertainties in the treatment of microphysics and chemical processes in PDR models have significant effects on PDR diagnostics.