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Browsing by Author "Shull, J. M."

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    HST/COS observations of galactic high-velocity clouds: four active galactic nucleus sight lines through complex C
    Shull, J. M.; Stevans, M.; Danforth, C.; Penton, S. V.; Lockman, F. J.; Arav, Nahum (IOP Publishing Ltd., 2011-10)
    We report ultraviolet spectra of Galactic high-velocity clouds (HVCs) in Complex C, taken by the Cosmic Origins Spectrograph (COS) on the Hubble Space Telescope (HST), together with new 21 cm spectra from the Green Bank Telescope. The wide spectral coverage and higher signal-to-noise ratio, compared to previous HST spectra, provide better velocity definition of the HVC absorption, additional ionization species (including high ions), and improved abundances in this halo gas. Complex C has a metallicity of 10%-30% solar and a wide range of ions, suggesting dynamical and thermal interactions with hot gas in the Galactic halo. Spectra in the COS medium-resolution G130M (1133-1468 angstrom) and G160M (1383-1796 angstrom) gratings detect ultraviolet absorption lines from eight elements in low-ionization states (O I, N I, C II, S II, Si II, Al II, Fe II, P II) and three elements in intermediate-and high-ionization states (Si III, Si IV, C IV, N V). Our four active galactic nucleus sight lines toward Mrk 817, Mrk 290, Mrk 876, and PG 1259+593 have high-velocity Hi and Ovi column densities, log N-H (I) = 19.39-20.05 and logN(OVI) = 13.58-14.10, with substantial amounts of kinematically associated photoionized gas. The high-ion abundance ratios are consistent with cooling interfaces between photoionized and collisionally ionized gas: N(C IV)/N(O vi) approximate to 0.3-0.5, N(Si IV)/N(O VI) approximate to 0.05-0.11, N(N V)/N(O VI) approximate to 0.07-0.13, and N(Si IV)/N(Si III) approximate to 0.2.
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    Ultraviolet and X-ray Variability of the Seyfert 1.5 Galaxy Markarian 817
    Winter, L. M.; Danforth, C.; Vasudevan, R.; Brandt, W. N.; Scott, J.; Froning, C.; Keeney, B.; Shull, J. M.; Penton, S.; Mushotzky, R. F.; Schneider, D. P.; Arav, Nahum (IOP PUBLISHING LTD, 2011-02)
    We present an investigation of the ultraviolet and X-ray spectra of the Seyfert 1.5 galaxy Markarian 817. The ultraviolet analysis includes two recent observations taken with the Cosmic Origins Spectrograph (COS) in 2009 August and December, as well as archival spectra from the International Ultraviolet Explorer and the Hubble Space Telescope. Twelve Ly alpha absorption features are detected in the 1997 Goddard High Resolution Spectrograph (GHRS) and 2009 COS spectra-of these, four are associated with high-velocity clouds in the interstellar medium, four are at low significance, and the remaining four are intrinsic features, which vary between the GHRS and COS observations. The strongest intrinsic absorber in the 1997 spectrum has a systemic velocity of similar to-4250 km s(-1). The corresponding feature in the COS data is five times weaker than the GHRS absorber. The three additional weak (equivalent width from 13 to 54 m angstrom) intrinsic Lya absorbers are at systemic velocities of -4100 km s(-1), -3550 km s(-1), and -2600 km s(-1). However, intrinsic absorption troughs from highly ionized Civ and N v are not detected in the COS observations. No ionized absorption signatures are detected in the similar to 14 ks XMM-Newton EPIC spectra. The factor of five change in the intrinsic Lya absorber is most likely due to bulk motions in the absorber, since there is no drastic change in the UV luminosity of the source from the GHRS to the COS observations. In a study of the variability of Mrk 817, we find that the X-ray luminosity varies by a factor of similar to 40 over 20 years, while the UV continuum/emission lines vary by at most a factor of similar to 2.3 over 30 years. The variability of the X-ray luminosity is strongly correlated with the X-ray power-law index, but no correlation is found with the simultaneous optical/UV photometry.