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Using excerpts from a letter written by famed astronomer Galileo in
1615, two modern-day astronomers explore the relationship between
science and faith, arguing that our notion of ultimate truth must
include both the physical and spiritual domains.
Stars are Small Dark-Coloured Things That Live in Holes in the
Ground.- Shrouds of the Night - Galaxies and Rene Magritte.- Twin
Masks of Spiral Structure? A Local Perspective.- The Mask of
Complexity in Disk Galaxies.- Cosmic Magnetic Fields - An
Overview.- The Gaseous Halo Mask.- Molecular Gas Properties of
Galaxies: The SMA CO(2-1) B0DEGA Legacy Project.- The DiVA's Mask:
Iconifying Galaxies and Revealing HI Anomalies.- Enigmatic Masks of
Cosmic Dust: Lessons from Nearby Galaxies Through the Eyes of the
Spitzer Space Telescope.- The Large Magellanic Cloud: A Power
Spectral Analysis of Spitzer Images.- Light Cores Behind Dark
Masks.- Globalization, Open Access Publishing, and the
Disappearance of Print: Threat or Opportunity?.- Super Star
Clusters and Supernovae in Interacting LIRGs Unmasked by NIR
Adaptive Optics.- Structure, Mass, and Stability of Galactic
Disks.- What Can the Radial Surface Brightness Profiles of Galaxy
Discs Tell Us About Their Evolution?.- The Complex Interplay of
Dust and Star Light in Spiral Galaxy Discs.- Galaxy Morphology
Revealed By SDSS: Blue Elliptical Galaxies.- Rings and Bars:
Unmasking Secular Evolution of Galaxies.- Bars and Bulges Through
Masks of Time.- Tidal Trails and Mass-Segregated Isothermal
Clusters.- Stellar Debris Streams: New Probes of Galactic Structure
and Formation.- Chemical Enrichment in Galaxies: Constraints on
Nucleogenesis and Galaxy Evolution.- Chemodynamical Simulations of
Galaxies.- Elemental Abundance Patterns of Disk Substructure.-
Searching for Structures and Streams in the Extended Solar
Neighbourhood with RAVE.- On the Age-Metallicity-Velocity Relation
in the Nearby Disk Using the RAVE Survey.- The HERMES Project:
Reconstructing Galaxy Formation.- Stellar Halos: Unmasking a
Galaxy's History.- The Outer Halos of Elliptical Galaxies.-
Galaxies: Lighthouses in the Shoals of Dark Halos.- Dark Haloes as
Seen with Gravitational Lensing.- Behind the Mask: Resolving the
Core-Cusp Problem in Spiral Galaxies.- A GALAXY BASELINE:
Multiwavelength Study of a Sample of the Most Isolated Galaxies in
the Local Universe.- Diffuse Light and Galaxy Interactions in the
Core of Nearby Clusters.- Feedback in Star and Galaxy Formation.-
When Bad Masks Turn Good.- Spitzer's View of Galaxies in the
High-Redshift Universe.- Bandshifting and Other Masks of the Clumpy
Populations in High-Redshift Galaxies.- Supernovae, Dust, and
Cosmology.
THE EDITORS: DAVID L. BLOCK AND KENNETH C. FREEMAN (SOC CO-CHAIRS),
IVANIO PUERARI, ROBERT GROESS AND LIZ K. BLOCK 1. Harvard College
Observatory, 1958 The past century has truly brought about an
explosive period of growth and discovery for the physical sciences
as a whole, and for astronomy in particular. Galaxy morphology has
reached a renaissance . . The year: 1958. The date: October 1. The
venue: Harvard College Observatory. The lecturer: Walter Baade.
With amazing foresight, Baade penned these words: "Young stars,
supergiants and so on, make a terrific splash - lots of light. The
total mass of these can be very small compared to the total mass of
the system". Dr Layzer then asked the key question: " . . . the
discussion raises the point of what this classification would look
like if you were to ignore completely all the Population I, and
just focus attention on the Population II . . . " We stand on the
shoulders of giants. The great observer E. E. Barnard, in his
pioneering efforts to photograph the Milky Way, devoted the major
part of his life to identifying and numbering dusty "holes" and
dust lanes in our Milky Way. No one could have dreamt that the
pervasiveness of these cosmic dust masks (not only in our Galaxy
but also in galaxies at high redshift) is so great, that their
"penetration" is truly one of the pioneering challenges from both
space-borne telescopes and from the ground.
What is the nature and composition of the dust grains responsible
for the visual extinction in our Galaxy and in other galaxies
beyond? What are the ranges in temperature of dust grains? Can
these be less than 2.7K? Can the distribution of cold grains be
studied optically at unprecedented arcsecond resolution? How does
the presence of dust affect the morphology of a galaxy? Is this new
dust-penetrated view bringing us to the verge of a breakthrough in
understanding the connection between galaxy morphology and the
underlying physics of galaxies? How large are the amounts of cold
molecular hydrogen gas and cold dust in galactic disks? These are
some of the key issues addressed in this book, which takes the
postgraduate reader and professional researcher to the cutting edge
of this rapidly developing field. Unique features of the book
include fourteen in-depth invited review papers and twenty-six
pages of discussion transcribed from a television tape. The
contributions reflect the entire proceedings of an intensive one
week International Conference on cold dust and galaxy morphology
held in Johannesburg, South Africa, during January 1996.
The year: 1660. The date: November 28. Present: The Lord Brouncker,
Mr Boyle, Mr Bruce, Sir Robert Moray, Sir Paule Neile, Dr Wilkins,
Dr Goddard, Dr Petty, Mr Ball, Mr Hooke, Mr Wren, and Mr Hill.
Occasion: A lecture by Mr Wren at Gresham College, United Kingdom.
AfterChristopherWrenhaddeliveredhislectureatGreshamCollegeonthathistoric
occasion in November 1660, "they did according to the usual manner,
withdraw for mutual converse." It was in 1660 that the Royal
Society was founded, with 12 persons present. This year, 2010, is
thus a special year for scientists worldwide: it celebrates the
350th anniversary of the founding of the Royal Society, whose
current President is Martin Rees. One of the enormous challenges
facing scientists in the 1600s was the great need fortheclassi
cationofobjectstheywerestudying,particularlyinthe eldofbotany. The
seeds for classi cation lie in the works of the British naturalist
John Ray (1628-1705), who commencing in 1660 with
hisCatalogusplantarumcirca Cantabrigiamnascentium (Catalogue of
Cambridge Plants) - published in the year in which the Royal
Society was founded - and ending with the posthumous publi- tion
ofSynopsisMethodicaAviumetPiscium in 1713, pioneered systematic
studies on plants, birds, mammals, sh, and insects.
THE EDITORS: DAVID L. BLOCK AND KENNETH C. FREEMAN (SOC CO-CHAIRS),
IVANIO PUERARI, ROBERT GROESS AND LIZ K. BLOCK 1. Harvard College
Observatory, 1958 The past century has truly brought about an
explosive period of growth and discovery for the physical sciences
as a whole, and for astronomy in particular. Galaxy morphology has
reached a renaissance . . The year: 1958. The date: October 1. The
venue: Harvard College Observatory. The lecturer: Walter Baade.
With amazing foresight, Baade penned these words: "Young stars,
supergiants and so on, make a terrific splash - lots of light. The
total mass of these can be very small compared to the total mass of
the system". Dr Layzer then asked the key question: " . . . the
discussion raises the point of what this classification would look
like if you were to ignore completely all the Population I, and
just focus attention on the Population II . . . " We stand on the
shoulders of giants. The great observer E. E. Barnard, in his
pioneering efforts to photograph the Milky Way, devoted the major
part of his life to identifying and numbering dusty "holes" and
dust lanes in our Milky Way. No one could have dreamt that the
pervasiveness of these cosmic dust masks (not only in our Galaxy
but also in galaxies at high redshift) is so great, that their
"penetration" is truly one of the pioneering challenges from both
space-borne telescopes and from the ground.
What is the nature and composition of the dust grains responsible
for the visual extinction in our Galaxy and in other galaxies
beyond? What are the ranges in temperature of dust grains? Can
these be less than 2.7K? Can the distribution of cold grains be
studied optically at unprecedented arcsecond resolution? How does
the presence of dust affect the morphology of a galaxy? Is this new
dust-penetrated view bringing us to the verge of a breakthrough in
understanding the connection between galaxy morphology and the
underlying physics of galaxies? How large are the amounts of cold
molecular hydrogen gas and cold dust in galactic disks? These are
some of the key issues addressed in this book, which takes the
postgraduate reader and professional researcher to the cutting edge
of this rapidly developing field. Unique features of the book
include fourteen in-depth invited review papers and twenty-six
pages of discussion transcribed from a television tape. The
contributions reflect the entire proceedings of an intensive one
week International Conference on cold dust and galaxy morphology
held in Johannesburg, South Africa, during January 1996.
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