Fig. 1 -
    Overall radio structure - the 2012 JVLA C+B-array image
    of radio intensity at 5.5 GHz, constructed with uniform
    weighting and cleaned with MFS-MS algorithm, showing the
    central 15' radio bright zone (RBZ) at the Galactic center.
    The rms noise is 8 μJ/beam with a FWHM beam (1.6" x 0.6", PA=11o)

 
 
Fig. 2 -
    a 5.5 GHz image in Galactic coordinates (increasing
    Galactic longitude is up) showing with dashed rectangles
    the regions containing the SE (lower-left) and NW (upper-right)
    "wings" that extend from the Mini-spiral arms, in the direction
    nearly perpendicular to the Galactic plane.
    the top image.

 
 
Fig. 3 -
    Superposition of the 5.5 GHz JVLA continuum image (blue),
    and the CN molecular line image (red) observed with the SMA
    (Mart ́ et al. 2012). The combination results in a pink colo
    for the CND. Radio continuum emission from the Mini-spiral HII
    g as ın appears in light blue.

 
 
Fig. 4 -
    Radio contours (from JVLA) overlaid on the Chandra X-ray
    image integrated over 1 Msec (Markoff 2010). Thecoordinate
    frames between the X-ray and radio images were aligned using
    a dozen X-ray compact sources with positions given by Muno et al.
    (2009) include Sgr A* and the Cannonball (Park et al. 2005; Zhao,
    Morris & Goss 2013). In this figure, the X-ray and radio lobes are
    oriented almost horizontally, or at a position angle of ~ -75o
    with respect to equatorial north.

 
 
Fig. 5 -
    Radio lobes displayed in the JVLA 5.5 GHz image; the red vector
    line indicates the direction of an X-ray feature (blue segment)
    that has been proposed to be part of a jet from Sgr A* (Li et al. 2013);
    the green vector line points to the tip of the "V"-shaped feature,
    SEblb-5, in the SE Lobe (c.f., section 3.4.2 and Fig. 8.).
    Download postscript - Figure 5

 
 
Fig. 6 -
    The 5.5 GHz radio image showing the emission streamers as labelled
    in the NW radio lobe with the FWHM beam of 1.6" x 0.6" (PA=11o).
    Also the radio counterpart of the compact X-ray source CXOUGCJ174538.0-285911
    is marked with an open arrow. The inset at top left shows the head-tail
    structure of the southern arch of source "M", located in the region
    marked with open rectangle. The contours of this inset are 1 σ x
    (100, 150, 250, 400, 600, 850), σ = 8μ /y beam, and the beam is marked
    on the top-right corner. The bottom-right inset presents the radio image
    as contours (at 10μ Jy / beam) x 2n and n = 2, 7, 9, 10, 11, ..., 16) overlaid
    on the HST/NICMOS Pα image(color) (Wang et al. 2010). Both radio and Pα image
    have been smoothed with a circular Gaussian of FWHM 2". The equatorial
    coordinate frame in this inset has been rotated 15o (clockwise).
    The directions of the major axes of the radio streamers in the NW Lobe as
    well as the predominant axis of the amorphous blobs in the SW Lobe are marked
    by open arrows.

 
 
Fig. 7 -
    Top: VLA image of 5.5 GHz radio emission from the outermost portions
    of the NW Lobe, showing details of the structures that we refer to as
    "Smoke Rings" (SmR 1, SmR 2 and SmR 3, from right to left). Equatorial
    North is up. The FWHM beam is 1.6" x 0.6" (PA=11o ). No correction
    for primary beam attenuation has been applied. Bottom: The HST/NICMOS
    image of Pα emission Wang et al. 2010; Dong et al. 2011) corresponding
    to the same region. Minor differences between the two images can be
    attributed to foreground extinction features that affect the Pα distribution
    . The green circles mark two massive stars in the region, as discussed in the text.

 
 
Fig. 8 -
    Top panel a: a section of the radio image showing the distribution of amorphous
    radio blobs in the SE Lobe. The FWHM beam of 1.6" x 0.6" (PA=11o).
    Top panel b: an HST/NICMOS image showing the Pα counterpart of the same region
    . The individual components are marked with their sequential numbers in both images.
    The inset at top-right shows an image of the SW Shell (marked in Fig. 5) in radio
    (color) and Pα contours) to verify the alignment between the radio and IR coordinate
    frames. The bottom eight panels show the details of individual components of the
    amorphous radio blobs (color) overlaid with contours of Pα emission that has bee
    smoothed with a 2-D Gaussian function identical to the radio clean beam of
    1.6" x 0.6" (PA=11o).
    The central positions (offsets in arcseconds
    from the field center, see footnote of Table 1) of the eight regions are
    (65,-190), (86,-164), (50,-170), (14,-165), (55,-145), (28,-133), (37.5,-101)
    and (14,-115.5).