Captions for Colour Plates

Plate 1 (Fig. 1, Block et al.) Spiral 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 , 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 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 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 , 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. The horizon line represents the flat horizon of the Savannah, perhaps the most famous landscape of South Africa and has been positioned to represent the path of Venus Colour Plate CaptIOns 853 across the face of the Sun, relative to the edge of the medallion. A typical African tree emphasizes the horizon line, which depicts (not to scale) a silhouette of Venus on the line of transit. The main text is "Venus Transits the Sun," while in the disc of the Sun is the Latin inscription, "Soli Deo Gloria" which means "To God alone be the Glory." Beneath the horizon is an African proverb, "Walala Wasala." This phrase means "You snooze, you lose!" The date '8 June 2004' and 'South Africa' also appear. Bottom: Mary Cummings and her role in the previous transit of Venus, is the theme of the reverse of the medallion. Her image is displayed against a background of the paths of previous and future transits. Mary was a teacher at the Huguenot Seminary for girls in Wellington South Africa. She was a member of the Class of 1876 at Mt. Holyoke Seminary in Massachusetts (USA) and moved to Wellington to teach at the Huguenot Seminary in 1877. In 1882, just in time for the transit of Venus, the 6" Fitz refractor telescope that Mary had used as a student at Mt. Holyoke was moved to Wellington and set up by the Astronomer Royal at the Cape, Sir David Gill. This Amer• ican connection in South Africa led Prof Simon Newcomb of the US Naval Observatory to set up his own telescope for the Venus transit observations in the Seminary Garden. Mary observed the transit and documented its timing with precise chronometer readings, right along• side her more famous mentor, Newcomb, and is still credited today for her part in this important observation. Mary Cummings symbolizes the essential role played by women in astronomy, and is particularly famous for her observations of the last transit of Venus in South Africa on December 6, 1882. 855

a y

Plate I 856

Plate 2 857

.,v o

40' 309 4h23m20s 10' 40' 30· 4h23m 20· 10' R A (2000) R A (2000)

Plate 3 858

Plate 4 859

Plate 5 860

Plate 6 861

Plate 7 862

Plate 8 863

Plate 9 864

10

I 18 ~ 50" 75°1i40"

40 30' R A (2000) 4~23m20"

Plate 10 865

Plate 11 866

Plate 12 867

Plate 13 868

Plate 14 869

Plate 15 870

Plate 16 871

LIST OF PARTICIPANTS

Ronald J. Allen Space Telescope Science Institute, USA Silvia Baes-Fischlmair Institut fur Astronomie der Universitat Wien, Austria Nicholas M. Ball Astronomy Centre, University of Sussex, UK John E. Beckman Instituto de Astrofisica de Canarias, Spain David L. Block School of Computational and Applied Mathematics, University of Witwatersrand, South Africa HarryBlom Kluwer Publishers, Holland Francois Boulanger Institut d' Astrophysique Spatiale, Universite Paris XI, France Frederic Bournaud LERMA, Observatoire de Paris, France Sarah Bryan University of KwaZulu-Natal, Pietermaritzburg, South Africa Martin Bureau Columbia Astrophysics Laboratory, USA Andreas M. Burkert University Observatory Munich, Germany Ronald J. Buta Department of Physics & Astronomy, University of Alabama, USA Gabriela Canalizo Department of Sciences and IGPP, University of California, USA Roberto Capuzzo-Dolcetta Department of Physics, Univ. of Roma La Sapienza, Italy Claude Carignan LAB, Universite de Montreal, Canada Francoise Combes LERMA, Observatoire de Paris, France Christopher J. Conselice California Institute of Technology, USA Enrico M. Corsini Dipartimento di Astronomia, Universita di Padova, Italy Catherine Cress University of KwaZulu-Natal, Pietermaritzburg, South Africa Barbara Cunow Department of Mathematics, Applied Mathematics and Astronomy, University of South Africa, South Africa Anna Curir INAF - Astronomical Observatory of Torino, Italy Elena D'Onghia Max-Planck-Institut fur extraterrestrische Physik, Germany Bruce G. Elmegreen IBM Research Division, T.J. Watson Research Center, USA Eric Emsellem Centre de Recherche Astronomique de Lyon, France Paul B. Eskridge Department of Physics & Astronomy, Minnesota State University, USA Giovanni G. Fazio Harvard-Smithsonian Center for Astrophysics, USA Holland Ford Johns Hopkins University, USA 872

Didier Fraix-Burnet Laboratoire d' Astrophysique de Grenoble, France Ken C. Freeman Mt Stromlo Observatory, RSAA, Australian National University, Australia Uta Fritze - v. Alvensleben Universitatssternwarte Gottingen, Germany Alister W. Graham Department of Astronomy, University of Florida, USA Robert Groess School of Computational and Applied Mathematics, University of Witwatersrand, South Africa Preben Grosbol European Southern Observatory, Germany Luis C. Ho The Observatories of the Carnegie Institution of Washington, USA Kelly Holley-Bockelmann University of Massachusetts, USA Susanne Huttemeister Astronomisches Institut, Ruhr-Universitat Bochum, Germany Leslie K. Hunt Istituto di RadioastronomialSezione Firenze, Italy Garth Illingworth UC ObservatorieslLick Observatory & Department of Astronomy and Astrophysics, University of California, USA Rolf Jansen Dept. of Physics and Astronomy, Arizona State University, USA Shardha Jogee Space Telescope Science Institute, USA Dong-Woo Kim Smithsonian Astrophysical Observatory, USA Ivan King Astronomy Department, University of Washington, USA Johan H. Knapen Centre for Astrophysics Research, University of Hertfordshire, UK David C. Koo UC ObservatorieslLick Observatory & Department of Astronomy and Astrophysics, University of California, USA John Kormendy Department of Astronomy, University of Texas, USA George Lake Washington State University, USA Eija Laurikainen Division of Astronomy, Dept. of Phys. Sciences, Univ. of Oulu, Finland Alex Lazarian University of Wisconsin-Madison, Dept. of Astronomy, USA Olivier Le Fevre Laboratoire d' Astrophysique de Marseille, France Aigen Li Theoretical Astrophysics Program, University of Arizona, USA Jeremy Lim Inst. of Astronomy & Astrophysics, Academia Sinica, Taiwan Witold Maciejewski Obserwatorium Astronomiczne Uniwersytetu Jagiellonskiego, Poland Paul Martini Harvard-Smithsonian Center for Astrophysics, USA Karin Menendez-Delmestre California Institute of Technology, USA George Miley Sterrewacht Leiden, The Netherlands Julio F. Navarro CIAR and Guggenheim Fellow, Department of Physics and Astronomy, University of Victoria, Canada Masafumi Noguchi Tohoku University, Japan Stephen C. Odewahn HET, University of Texas, USA 873

Jan Palous Astronomical Institute, Academy of Sciences of the Czech Republic, Czech Republic Isabel Perez Kapteyn Institute, University of Groningen, The Netherlands Daniel Pfenniger Geneva Observatory, University of Geneva, Switzerland Michael Pohlen Instituto de Astrofisica de Canarias, Spain Ivanio Puerari INAOE, Mexico Jean-Loup Puget Institut d' Astrophysique Spatiale, Universite Paris Sud, France Michael Regan Space Telescope Science Institute, USA Brigitte Rocca-Volmerange Institut d' Astrophysique de Paris, France Heikki Salo Division of Astronomy, Dept. of Phys. Sciences, Univ. of Oulu, Finland Marc S. Seigar Joint Astronomy Centre, Hilo, USA William Sheehan Willmar, MN, USA Kartik Sheth California Institute of Technology, USA Frank Shu National Tsing Hua University, Taiwan, ROC Philip B. Stark Dept. of Statistics, University of California, USA Thomas Steiman-Cameron Astronomy Dept., Indiana Univ., USA Margarita Valdez-Gutierrez Departamento de Astronomia, Universidad de Guanajuato, Mexico Catherine Vlahakis School of Physics and Astronomy, Cardiff University, UK Rogier Windhorst Department of Physics and Astronomy, Arizona State University, USA Guy Worthey Astronomy Program, Washington State University, USA Chi Yuan Inst. of Astronomy & Astrophysics, Academia Sinica, Taiwan Xiaolei Zhang US Naval Research Laboratory, USA Almudena Zurita Universidad de Granada, Dept. de Fisica Teorica y del Cosmos, Spain

Teachers from the Nirvana Secondary School (Lenasia), Cliffview Primary School (Fairlands) and the S G Mafaesa School (Kagiso) participated in our outreach to schools, during the Venus Transit.

Students Participation

The students below also formed part of the Venus Transit video link-up to Cambridge University (UK): Nehal Badal, Fabian Francis, Deepika Goolab, Pauline Kgongoane, Navitha Latchman, Lester Mancasa, Solomon Matlmong, Ashvira Moodley, Muhanganei Munyai, Lindiwe Mwanda, Nisha Naka, Kash• mira Naran, Ntsieni Nemanashi, Michael Nobu, Meera Ooka, Emelia Pillay, 874

Aifueli Rabambi, Mpho Rabambi, Kashmira Rawjee, Lebogang Seloi, Petunia Shuping, Staff from the Nirvana Secondary School (Lenasia), Cliffview Primary School (Fairlands) and the S G Mafaesa School (Kagiso) who came to the Pilanes• berg with students, included: Sue Ie Sueur, Yvonne Kekana (Wits Marketing), Angsha Nathoo, Pauline Kgongoane, Berendien van Aswegen.

Figure I. Our group photograph at the Pllanesberg National Park. Astrophysics and Space Science Library

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