Virginia Tech
    • Log in
    View Item 
    •   VTechWorks Home
    • College of Science (COS)
    • Department of Physics
    • Scholarly Works, Department of Physics
    • View Item
    •   VTechWorks Home
    • College of Science (COS)
    • Department of Physics
    • Scholarly Works, Department of Physics
    • View Item
    JavaScript is disabled for your browser. Some features of this site may not work without it.

    Mass Outflow in the Seyfert 1 Galaxy NGC 5548

    Thumbnail
    View/Open
    Main article (504.1Kb)
    Downloads: 307
    Date
    2009-06
    Author
    Crenshaw, D. M.
    Kraemer, S. B.
    Schmitt, H. R.
    Kaastra, J. S.
    Arav, Nahum
    Gabel, J. R.
    Korista, K. T.
    Metadata
    Show full item record
    Abstract
    We present a study of the intrinsic UV absorption and emission lines in an historically low-state spectrum of the Seyfert 1 galaxy NGC 5548, which we obtained in 2004 February at high spatial and spectral resolution with the Space Telescope Imaging Spectrograph on the Hubble Space Telescope. We isolate a component of emission with a width of 680 km s(-1) that arises from an "intermediate-line region" (ILR), similar to that we discovered in NGC 4151, at a distance of similar to 1 pc from the central continuum source. From a detailed analysis of the five intrinsic absorption components in NGC 5548 and their behavior over a span of eight years, we present evidence that most of the UV absorbers only partially cover the ILR and do not cover an extended region of UV continuum emission, most likely from hot stars in the circumnuclear region. We also find that four of the UV absorbers are at much greater distances (greater than 70 pc) than the ILR, and none have sufficient N V or C IV column densities to be the ILR in absorption. At least a portion of the UV absorption component 3, at a radial velocity of -530 km s(-1), is likely responsible for most of the X-ray absorption, at a distance less than 7 pc from the central source. The fact that we see the ILR in absorption in NGC 4151 and not in NGC 5548 suggests that the ILR is located at a relatively large polar angle (similar to 45 degrees) with respect to the narrow-line region outflow axis.
    URI
    http://hdl.handle.net/10919/25850
    Collections
    • Scholarly Works, Department of Physics [811]

    If you believe that any material in VTechWorks should be removed, please see our policy and procedure for Requesting that Material be Amended or Removed. All takedown requests will be promptly acknowledged and investigated.

    Virginia Tech | University Libraries | Contact Us
     

     

    VTechWorks

    AboutPoliciesHelp

    Browse

    All of VTechWorksCommunities & CollectionsBy Issue DateAuthorsTitlesSubjectsThis CollectionBy Issue DateAuthorsTitlesSubjects

    My Account

    Log inRegister

    Statistics

    View Usage Statistics

    If you believe that any material in VTechWorks should be removed, please see our policy and procedure for Requesting that Material be Amended or Removed. All takedown requests will be promptly acknowledged and investigated.

    Virginia Tech | University Libraries | Contact Us