The catalogue is a compilation of the principal observed parameters of pulsars, including positions, timing parameters, pulse widths, flux densities, proper motions, distances, and dispersion, rotation, and scattering measures. It also lists the orbital elements of binary pulsars, and some commonly used parameters derived from the basic measurements. The catalogue includes all published rotation-powered pulsars, including those detected only at high energies. It also includes Anomalous X-ray Pulsars (AXPs) and Soft Gamma-ray Repeaters (SGRs) for which coherent pulsations have been detected. However, it excludes accretion-powered pulsars such as Her X-1 and the recently discovered X-ray millisecond pulsars.
A form to search the VAMDC species list published on the TAP service
at http://dc.g-vo.org/tap. Enter parts of species names or chemical
formulae here and get back matching names, inchis and inchikeys.
We report observations of atomic carbon (C I [^3^P - ^3^P_0_]) for a sample of 49 southern hemisphere H II regions using the Antarctic Submillimeter Telescope and Remote Observatory. The sources are compact and isolated members of the Wilson et al. (1970) H109{alpha} radio recombination line (RRL) catalog. The fourth Galactic quadrant is well covered by the sample. Atomic carbon emission is detected toward all of the regions, with multiple C I emission components found toward most sources. The RRL velocity is used to identify the C I emission associated with the H II region. We measure the mean velocity difference between the C I and RRL emission to be 0.8{+/-}2.8 km s^-1^. Within the measurement errors this is exact agreement in velocity; we conclude that all H II regions have associated C I emission. The mean C I line temperature of these components is 2.4{+/-}1.8 K, compared with 0.7{+/-}0.7 K for the C I emission components not associated with the H II region. This suggests that C I intensity is dominated by local heating. The FWHM line width of C I gas associated with H II regions also is marginally greater than that found for unassociated gas (6.7{+/-}3.0, compared with 4.8{+/-}2.4 km s-1).
We present results from an analysis of FUSE spectroscopy of the z_em_=0.57 quasar PKS 0405-123. We focus on the intervening metal-line systems identified along the sight line and investigate their ionization mechanism, ionization state, and chemical abundances. Including Hubble Space Telescope STIS spectroscopy, we survey the entire sight line and identify six O VI absorbers to a 3{sigma} equivalent width (EW) limit of 60m{AA}.
Radiative and Auger decay data have been calculated for modeling the K lines of the aluminium isonuclear sequence, from Al0 to Al11+. Level energies, transition wavelengths, radiative transition probabilities, and radiative and Auger widths have been determined using Cowan's Hartree-Fock with relativistic corrections (HFR) method. Results are compared with data sets computed with the AUTOSTRUCTURE and GRASP atomic structure codes and with available experimental and theoretical values, mainly in highly ionized ions and in the solid state.
We present the results of a new large-scale intermediate-coupling frame transformation R-matrix scattering calculation for electron collisional excitation of Fe IX. The target includes all the main configurations up to n=5, to improve our earlier R-matrix and distorted-wave (DW) calculations for the n=3,4 levels. Unlike similar calculations which we carried out for the other coronal iron ions, in this case the larger target does not significantly affect the collision strengths of the strongest transitions to the n=3,4 levels. Some differences are however present for a few transitions, in particular for the 3d-4p line at 197.86{AA}. For the weaker transitions, significant enhancements due to extra resonances resulting from this much bigger target are found. Several new line identifications are suggested. We find excellent agreement between predicted and observed line intensities in the EUV (Hinode EIS) showing that Fe IX lines provide a reliable temperature diagnostic. We also show that the visible forbidden lines are a good diagnostic to measure electron densities.
Complete data sets of level energies, transition wavelengths, A-values, radiative and Auger widths and fluorescence yields for K-vacancy levels of the F, Na, P, Cl, K, Sc, Ti, V, Cr, Mn, Co, Cu and Zn isonuclear sequences have been computed by a Hartree-Fock method that includes relativistic corrections as implemented in Cowan's atomic structure computer suite. The atomic parameters for more than 3 million fine- structure K lines have been determined. Ions with electron number N>9 are treated for the first time, and detailed comparisons with available measurements and theoretical data for ions with N=<9 are carried out in order to estimate reliable accuracy ratings.
We present multi-configuration Breit-Pauli distorted-wave photoionization (PI) cross sections and radiative recombination (RR) and dielectronic recombination (DR) rate coefficients for the first six krypton ions. These were calculated with the AUTOSTRUCTURE code, using semi-relativistic radial wavefunctions in intermediate coupling.
The atomic data required to analyse low density coronal plasmas have been calculated and used to interpret X-ray spectra observed by the Flat Crystal Spectrometer of the SMM/NASA satellite in the 14-19 A wavelength range. The emission lines correspond mainly to Fe XVI, Fe XVII, Fe XVIII and some ones to O VII, O VIII.
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