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Captions for Colour Plates Captions for Colour Plates Plate 1 (Fig. 1, Block et al.) Spiral galaxies in the dust penetrated regime are binned according to three quantitative criteria: firstly, Hm, where m is the dominant Fourier harmonic (illustrated here are the two-armed H2 family). Next, follows the dust penetrated pitch angle families 0:, {3 or 'Y (for class 0:, the pitch angles range from r-v 4-15°; for class (3, the deprojected pitch angles range from r-v 15-30°, while open-armed class 'Y spirals have pitch an­ gles ranging between r-v 35- 75°). Finally, we compute the gravitational torque, which is identical to the bar torque in galaxies presenting a bar. Bar torques are not derived from bar ellipticities but exploit the full gravitational potential of the disk within which it is embedded. Note that early type b spirals (NGC 3992, NGC 2543, NGC 7083, NGC 5371 and NGC 1365) are distributed within all three families (0:, {3 and "(). Hubble type and dust penetrated class are uncorrelated. Plate 2 (Buta) An issue of much debate at the Conference, was observational ev­ idence for bar dissolution and bar reformation. Seen here is an HST image of NGC 3081, which might be considered in the category of the bar dissolution. John Kormendy writes: "To me, a weak bar is suggestive evidence for bar suicide. Do we really believe that global disk instabilities or tickling by encounters can make a bar that is a few percent of the disk mass? This is not what happens in simulations. The bars that get made by these processes contain most of the disk mass that is interior to the end of the bar. Would it not be easier to understand the formation of a bar that is a few percent of the disk mass if it formed as a much stronger perturbation and then decayed?" Plate courtesy Ron Buta. Plate 3 (Fig. 7, Beckman et al.) (a) Surface brightness map in Ho: of NGC 1530, from a TAURUS data cube from the 4.2m WHT La Palma. (b) Radial velocity map of ionized gas from the peaks of the Ho: emission lines across the face of the galaxy, using the same data cube. (c) Contours of Ho: surface brightness superposed on a two-dimensional projection of the rotation curve derived from the velocity field shown in (b). (d) Map of the residual, non-circular velocity field, obtained by subtracting off the 850 Colour Plate Captions projected rotation curve in (c) from the complete velocity field in (b). The strong non-circular velocity field aligned with the bar is clearly seen here, as the galaxy inclination causes the flow along one side to be directed towards us, and away from us along the other side of the bar (see text for more details, also see Zurita et al. 2004). Plate 4 (Fig. 3, Kormendy and Cornell) Nuclear star formation rings in barred and oval galaxies. Sources: NGC 4314 - Benedict et al. (2002); NGC 4736 - NOAa; NGC 1326 - Buta et al. (2000) and Zolt Levay (STScI); NGC 1512 - Maoz et al. (2001); NGC 6782 - Windhorst et al. (2002) and the Hubble Heritage Program. This figure is from Kormendy & Kennicutt (2004). Plate 5 (Fig. 4, Kormendy and Cornell) Nuclear star formation in the unbarred galaxies M51 and NGC 4321 (M100). Dust lanes on the trailing side of the global spiral arms reach in to small radii. As in barred spirals, they are are indicative of gas inflow. Both galaxies have concentrations of star formation near their centers that resemble those in Figure 3. These images are from the Hubble Space Telescope and are reproduced here courtesy of STScl. Plate 6 (Section 5, Fazio et al.) Mosaic of galaxies at infrared wavelengths taken with the IRAC instrument on the Spitzer Space Telescope. Colors are coded as 3.6 (blue), 4.5 (green), and 8.0J,tm (red). The galaxies are arranged ac­ cording to traditional, optical morphological classifications. Starlight appears blue at these mid-infrared wavelengths, while warm dust (emit­ ting in the PAH emission lines) appears red. AGN emission is also red and point-like (e.g., NGC 5548). There is a clear transition from blue, stellar-dominated emission for the early-type galaxies to red, ISM-dominated emission for the late-type galaxies. Plate 7 (Section 5, Fazio et al.) Four galaxies observed with the Spitzer Space Telescope. (Top left): NGC 4203 is a lenticular galaxy, presenting striking rings of dust (coded red) in the central domains. (Top right): Masks of dust are well seen in the edge-on galaxy NGC 5746. (Bottom left): NGC 1961 is a late-type spiral with an unusual morphology. (Bottom right): We finally show the nearby spiral NGC 300. The reader is referred to Fazio et al. for further details. Plate 8 (Fig. 6, Ford et al.) A composite ACS i,z image of the brighter of the two most conspic­ uous sub-clusters in CL0152. The field size is 90" (rv 690 kpc in the Colour Plate Captions 851 rest frame ) Spectroscopically confirmed members are circled (6" diame­ ter; rv 50 kpc in the restframe). There are several thin arcs from lensed background galaxies that are much bluer than the early-type galaxies in the cluster. The lensed galaxy at the center has two components that are mirror images, indicating that the galaxy is very close to a caustic. Plate 9 (Fig. 7, Ford et al.) Star-forming galaxies in CL0152 and morphology of the X-ray emit­ ting gas. Spectroscopically confirmed passive galaxies are circled and galaxies with star formation, as indicated by [OIIj,\3737 emission, are shown with a "star". The latter are typically spirals and late-type galaxies, while the former are mostly E/SOs. The insets show typical morphologies and spectra. The spatial segregation of the star forming later type galaxies is very striking. The Chandra X-ray isophotes (De­ marco et al. 2004; Maughan et al. 2003) are 3, 5, 7, 10,20 and 30 sigma above the background. Plate 10 (Top: Fig. 2, Vlahakis et at.; Bottom: Fig. 1, Zurita et al.) Top: Example from the optically-selected SLUGS: NGC 3987. 850 }.Lm S/N map (10" contours) overlaid onto Digitised Sky Survey optical image. Bottom: (a) Intensity map of the Ha: emission in zone of the bar. (b) V band image. Velocity gradients parallel (c) and perpendicular (d) to the bar. (e) Non-circular residual velocity map. (f) Non-thermal velocity dispersion map. All images (a to f) show the same zone of the galaxy. Plate 11 Top: SOC member Bruce Elmegreen photographed at our Gala Din­ ner, with Mrs M. Keeton. Mrs Keeton is CEO of the Anglo American Chairman's Fund, the principal sponsor of our Conference. Bottom: Venus Transit medallions were handed out at the Gala Dinner by Governor Tito Mboweni and SOC co-chair David Block. Governor Mboweni is the Governor of the Reserve Bank of South Africa. Plate 12 Top: Trevor Gould photographed at our Gala Dinner. Trevor showed delegates the glories of the African winter skies, each evening after dinner. He also served on the LOC and on the Medallion Committee. Bottom: SOC co-chair Ken Freeman, delivering his address at Sun City, South Africa. Ken Freeman warmly paid tribute to the sponsors, without whom this Conference would never have seen the light of day. 852 Colour Plate Captions Plate 13 Top: The 2004 Venus Transit occurred during the week of our con­ ference. This stunning image was secured by Sylvie Beland on June 8, 2004 at 5h 53m (EDT). The site was the Observatory of "Centre de la Nature" in Laval, Quebec, Canada. She used a Nikon Coolpix 4300 IS0400 at f/2.8, exposure time 1/2 second. For this image, Beland employed a 25mm Lanthanum eyepiece, a Baader filter and her 8-inch f/5 Newton Dobsonian Telescope. Bottom: The Transit of Venus as photographed by David Finlay. People are seen viewing the transit from the famous Sydney bridge in Australia. Photograph reproduced by permission of Access All Areas Photography, at email [email protected]. Plate 14 Top: On the Friday before our Conference, Francoise Combes de­ livered a popular lecture on extrasolar planets to school children in Kagiso, South Africa. Seen here with Francoise in the school library is student Aifheli Rabambi. Bottom: A group of students from S G Mafaesa high-school (Kag­ iso) travelled from Kagiso to view the transit of Venus together with conference delegates. Venus could be identified as a minute black dot against the orange disk of the Sun, through these eclipse glasses. Front left: Tsolofelo Suping; Front right: Ntombi Peters. Plate 15 Top: David Block photographed with students from the Nirvana Secondary School in Lenasia, South Africa, during the Venus transit. The students seen here also formed part of a special video conference link-up to Cambridge University (UK). Venus took rv 6 hours to cross the disk of the Sun. At left front is Mrs. Mboweni (snr) , family of Reserve Bank Governor Tito Mboweni. Bottom: Students from S G Mafaesa Secondary school in Kagiso and the Nirvana Secondary School in Lenasia attended a special pre-transit dinner at The Palace, Sun City. Photographed at the Palace are Venus Transit lecturer William Sheehan, and students N tshieni Menaneshe (back) and Mpho Rabambi (front). Plate 16 Top: The obverse shows the symbolic transit of Venus, using a sable antelope (first discovered not far from the Pilanesberg in South Africa) charging across the Sun, which is shown just above the horizon, during the early morning time of the transit.
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