The last major conference on infrared astronomy was the IAU Symposium No. 96 in June 1980. Since then, the discipline has continued to mature and to contribute to all branches of astrophysics. One particular area of growth has been in spectroscopic capabilities at all infrared wavelengths. The purpose of the Symposium in Toledo was to review the scientific questions to be addressed via infrared spectroscopy and to provide, in the proceedings, a useful summary of the field. The sensitivity of infrared spectroscopic observations is still generally limited by detector characteristics or by thermal background radiation. However in recent years improvements in detector technology together with developments in spectroscopic instrumentation have made possible both quite detailed spectroscopy of the brighter members of many classes of galactic sources and also begun to open up some infrared spectroscopy of extragalactic sources. The potential of the field in the next decade or two is clear. The lRAS mission has completed one of the pre-requisites, namely an all-sky photometric survey. Major space missions utilising cryogenic infrared telescopes have been approved in Europe (ISO) and seem likely in the USA (SIRTF); plans for space submillimeter telescopes are firming up. On the ground large telescopes optimized for infrared observations are now in operation at high altitude sites and specialized submillimeter facilities are under construction. The particular advantages of planned, very large telescopes for infrared observations are widely accepted.

This textbook presents the basics of philosophy that are necessary for the student and researcher in science in order to better understand scientific work. The approach is not historical but formative: tools for semantical analysis, ontology of science, epistemology, and scientific ethics are presented in a formal and direct way. The book has two parts: one with the general theory and a second part with application to some problems such as the interpretation of quantum mechanics, the nature of mathematics, and the ontology of spacetime. The book addresses questions such as "What is meaning?", "What is truth?", "What are truth criteria in science?", "What is a theory?", "What is a model?" "What is a datum?", "What is information?", "What does it mean to understand something?", "What is space?", "What is time?", "How are these concepts articulated in science?" "What are values?" "What are the limits of science?", and many more. The philosophical views presented are "scientific" in the sense that they are informed by current science, they are relevant for scientific research, and the method adopted uses the hypothetical-deductive approach that is characteristic of science. The results and conclusions, as any scientific conclusion, are open to revision in the light of future advances. Hence, this philosophical approach opposes to dogmatic philosophy. Supported by end-of-chapter summaries and a list of special symbols used, the material will be of interest for students and researchers in both science and philosophy. The second part will appeal to physicists and mathematicians.

Although recent works on Galileo's trial have reached new heights of erudition, documentation, and sophistication, they often exhibit inflated complexities, neglect 400 years of historiography, or make little effort to learn from Galileo. This book strives to avoid such lacunae by judiciously comparing and contrasting the two Galileo affairs, that is, the original controversy over the earth's motion ending with his condemnation by the Inquisition in 1633, and the subsequent controversy over the rightness of that condemnation continuing to our day. The book argues that the Copernican Revolution required that the hypothesis of the earth's motion be not only constructively supported with new reasons and evidence, but also critically defended from numerous old and new objections. This defense in turn required not only the destructive refutation, but also the appreciative understanding of those objections in all their strength. A major Galilean accomplishment was to elaborate such a reasoned, critical, and fair-minded defense of Copernicanism. Galileo's trial can be interpreted as a series of ecclesiastic attempts to stop him from so defending Copernicus. And an essential thread of the subsequent controversy has been the emergence of many arguments claiming that his condemnation was right, as well as defenses of Galileo from such criticisms. The book's particular yet overarching thesis is that today the proper defense of Galileo can and should have the reasoned, critical, and fair-minded character which his own defense of Copernicus had.

Greenwich has been a centre for scientific computing since the foundation of the Royal Observatory in 1675. Early Astronomers Royal gathered astronomical data with the purpose of enabling navigators to compute their longitude at sea. Nevil Maskelyne in the 18th century organised the work of computing tables for the Nautical Almanac, anticipating later methods used in safety-critical computing systems. The 19th century saw influential critiques of Charles Babbage's mechanical calculating engines, and in the 20th century Leslie Comrie and others pioneered the automation of computation. The arrival of the Royal Naval College in 1873 and the University of Greenwich in 1999 has brought more mathematicians and different kinds of mathematics to Greenwich. In the 21st century computational mathematics has found many new applications. This book presents an account of the mathematicians who worked at Greenwich and their achievements. Features A scholarly but accessible history of mathematics at Greenwich, from the seventeenth century to the present day, with each chapter written by an expert in the field The book will appeal to astronomical and naval historians as well as historians of mathematics and scientific computing.

Beginning with the famous Olber's paradox, paradoxes such as the missing mass, dark energy, baryon to photon ratio and cosmic zero-point energy are examined in detail. The Heisenberg-Lemaitre's units, based on the total enormous but finite mass of the Universe, are introduced and rigorous solutions of Einstein's cosmological equations for an open Universe with cosmological constant are obtained. Energy conservation after the Big Bang is consistently required.This book discusses such paradoxes in depth with physical and logical content and historical perspective, and has not too technical content in order to serve a wide audience. In the second edition, the content is updated and new sections are added.

After three decades of intense research in X-ray and gamma-ray astronomy, the time was ripe to summarize basic knowledge on X-ray and gamma-ray spectroscopy for interested students and researchers ready to become involved in new high-energy missions. This volume exposes both the scientific basics and modern methods of high-energy spectroscopic astrophysics. The emphasis is on physical principles and observing methods rather than a discussion of particular classes of high-energy objects, but many examples and new results are included in the three chapters as well.

Beginning with the famous Olber's paradox, paradoxes such as the missing mass, dark energy, baryon to photon ratio and cosmic zero-point energy are examined in detail. The Heisenberg-Lemaitre's units, based on the total enormous but finite mass of the Universe, are introduced and rigorous solutions of Einstein's cosmological equations for an open Universe with cosmological constant are obtained. Energy conservation after the Big Bang is consistently required.This book discusses such paradoxes in depth with physical and logical content and historical perspective, and has not too technical content in order to serve a wide audience. In the second edition, the content is updated and new sections are added.

'Why'? Why is the world, the Universe the way it is? Is space infinitely large? How small is small? What happens when one continues to divide matter into ever smaller pieces? Indeed, what is matter? Is there anything else besides what can be seen? Pursuing the questions employing the leading notions of physics, one soon finds that the tangible and visible world dissolves - rather unexpectedly - into invisible things and domains that are beyond direct perception. A remarkable feature of our Universe is that most of its constituents turn out to be invisible, and this fact is brought out with great force by this book.Exploring the Invisible Universe covers the gamut of topics in advanced modern physics and provides extensive and well substantiated answers to these questions and many more. Discussed in a non-technical, yet also non-trivial manner, are topics dominated by invisible things - such as Black Holes and Superstrings as well as Fields, Gravitation, the Standard Model, Cosmology, Relativity, the Origin of Elements, Stars and Planetary Evolution, and more. Just giving the answer, as so many books do, is really not telling anything at all. To truly answer the 'why' questions of nature, one needs to follow the chain of reasoning that scientists have used to come to the conclusions they have. This book does not shy away from difficult-to-explain topics by reducing them to one-line answers and power phrases suitable for a popular talk show. The explanations are rigorous and straight to the point. This book is rarely mathematical without being afraid, however, to use elementary mathematics when called for. In order to achieve this, a large number of detailed figures, specially developed for this book and found nowhere else, convey insights that otherwise might either be inaccessible or need lengthy and difficult-to-follow explanations.After Exploring the Invisible Universe, a reader will have a deeper insight into our current understanding of the foundations of Nature and be able to answer all the questions above and then some. To understand Nature and the cutting edge ideas of contemporary physics, this is the book to have.

This is a revealing account of the family life and achievements of the Third Earl of Rosse, a hereditary peer and resident landlord at Birr Castle, County Offaly, in nineteenth-century Ireland, before, during and after the devastating famine of the 1840s. He was a remarkable engineer, who built enormous telescopes in the cloudy middle of Ireland. The book gives details, in an attractive non-technical style which requires no previous scientific knowledge, of his engineering initiatives and the astronomical results, but also reveals much more about the man and his contributions - locally in the town and county around Birr, in political and other functions in an Ireland administered by the Protestant Ascendancy, in the development and activities of the Royal Society, of which he was President from 1848-54, and the British Association for the Advancement of Science. The Countess of Rosse, who receives full acknowledgement in the book, was a woman of many talents, among which was her pioneering work in photography, and the book includes reproductions of her artistic exposures, and many other attractive illustrations. -- .

The studies brought together in this second collection of articles by Paul Kunitzsch continue the lines of research evident in his previous volume (The Arabs and the Stars). The Arabic materials discussed stem mostly from the early period of the development of Arabic-Islamic astronomy up to about 1000AD, while the Latin materials belong to the first stage of Western contact with Arabic science at the end of the 10th century, and to the peak of Arabic-Latin translation activity in 12th century Spain. The first set of articles focuses upon Ptolemy in the Arabic-Latin tradition, followed by further ones on Arabic astronomy and its reception in the West; the final group looks at details of the transmission of Euclid's Elements.

This book is an attempt to demystify the activities of a celestial object such as the Sun appealing to basic physics already available to high school students. Building on simple logic, the contents begin with measurements of the gross properties of the Sun like size (volume) and mass from which the average density of solar material is shown to be almost equal to water's density. Then the temperature is obtained using the colour of sunlight, and the gravitational force is discussed to indicate how the solar material is compressed at the centre of the Sun leading to heating which further causes nuclear reactions. The roles of all the forces of nature, viz. strong, weak, electromagnetic and gravitation are shown in the construction of the Sun. The generation of magnetic fields by solar rotation and the eruptions of solar atmospheric material are also included.To further demystify the methods of obtaining all such facts about the Sun, a chapter is solely devoted to the different kinds of solar telescopes operating at different wavelengths and also at different locations ranging from outer space to deep underground, where solar neutrino flux is measured. The entire discussion is interspersed with historical encounters between giants of science to show the human face of scientific research.

The hydrogen Lyman-alpha line is of utmost importance to many fields of astrophysics. This UV line being conveniently redshifted with distance to the visible and even near infrared wavelength ranges, it is observable from the ground, and provides the main observational window on the formation and evolution of high redshift galaxies. Absorbing systems that would otherwise go unnoticed are revealed through the Lyman-alpha forest, Lyman-limit, and damped Lyman-alpha systems, tracing the distribution of baryonic matter on large scales, and its chemical enrichment. We are living an exciting epoch with the advent of new instruments and facilities, on board of satellites and on the ground. Wide field and very sensitive integral field spectrographs are becoming available on the ground, such as MUSE at the ESO VLT. The giant E-ELT and TMT telescopes will foster a quantum leap in sensitivity and both spatial and spectroscopic resolution, to the point of being able, perhaps, to measure directly the acceleration of the Hubble flow. In space, the JWST will open new possibilities to study the Lyman-alpha emission of primordial galaxies in the near infrared. As long as the Hubble Space Telescope will remain available, the UV-restframe properties of nearby galaxies will be accessible to our knowledge. Therefore, this Saas-Fee course appears very timely and should meet the interest of many young researchers.

Is the Earth the right model and the only universal key to understand habitability, the origin and maintenance of life? Are we able to detect life elsewhere in the universe by the existing techniques and by the upcoming space missions? This book tries to give answers by focusing on environmental properties, which are playing a major role in influencing planetary surfaces or the interior of planets and satellites. The book gives insights into the nature of planets or satellites and their potential to harbor life. Different scientific disciplines are searching for the clues to classify planetary bodies as a habitable object and what kind of instruments and what kind of space exploration missions are necessary to detect life. Results from model calculations, field studies and from laboratory studies in planetary simulation facilities will help to elucidate if some of the planets and satellites in our solar system as well as in extra-solar systems are potentially habitable for life.

Astronomy isthemostancientsciencehumanshavepracticedonEarth. Itisascienceofextremesandoflargenumbers:extremesoftime-fromthe big bang to in?nity -, of distances, of temperatures, of density and masses, ofmagnetic?eld,etc.Itisasciencewhichishighlyvisible,notonlybecause stars and planets are accessible in the sky to the multitude, but also - cause the telescopes themselves are easily distinguishable, usually on top of scenic mountains, and also because their cost usually represent a subst- tialproportionofthenation'sbudgetandofthetaxpayerscontributionsto that budget. As such, astronomy cannot pass unnoticed. It touches on the origins of matter, of the Universe where we live, on life and on our destiny. It touches on philosophy as well as on religion. Astronomy is the direct c- tactofhumankindwithitsoriginsandtheimmensityofuniversalnature.It is indeed a science of observation where experimentation is practically - possible and which is ruled by mathematics, physics, chemistry, statistical analysis and modelling, while o?ering the largest number of veri?cations of the most advanced theories of fundamental physics such as general r- st ativity and gravitation. At the beginning of the 21 century astronomy is clearly a multidisciplinary activity touching on all aspects of science. It is therefore logical that in the past and still now, astronomy has attracted the most famous scientists, be they pure observers, mathematicians, physicists, biologists, experimentalists, and even politicians.

The aim of the VIRGO investigation (Variability of solar IRradiance and Gravity Oscillations) on SOHO (SOlar and Heliospheric Observatory) is to determine the characteristics of pressure and internal gravity oscillations by observing irradiance and radiance variations, to measure the solar total and spectral irradiance and to quantify their variability over periods of days to the duration of the mission. VIRGO contains two different active-cavity radiometers for monitoring the sol- ar 'constant' (DIARAD and PM06-V), two three-channel sunphotometers (SPM) for the measurement of the spectral irradiance at 402, 500, and 862 nm with a bandwidth of 5 nm, and a low-resolution imager (Luminosity Oscillation Imager, LOI) with 12 'scientific' and 4 guiding pixels, for measuring the radiance dis- tribution over the solar disk: at 500 nm. The instrumentation has been described in detail by Frohlich et al. (1995). In addition, the observed in-flight performance and operational aspects of the irradiance observations are described by Frohlich et al. (1997), and those of the LOI by Appourchaux et al. (1997).

Photopolarimetric remote sensing is vital in fields as diverse as medical diagnostics, astrophysics, atmospheric science, environmental monitoring and military intelligence. The areas considered here include: radiative transfer; dynamic systems; backscatter polarization; biological systems; astrophysical phenomena; comets; and instrumentation. Subtopics include observational information including determining morphology and chemistry, light-scattering models, and characterization methodologies. While this introductory text highlights the latest advances in this multi-disciplinary topic, it is also a reference guide for the advanced researcher.

The book consists of four Chapters. Chapter 1 shortly describes main properties of space plasmas and primary CR, different types of CR interactions with space plasmas components (matter, photons, and frozen in magnetic fields). Chapter 2 considers the problem of CR propagation in space plasmas described by the kinetic equation and different types of diffusion approximations (diffusion in momentum space and in pitch-angle space, anisotropic diffusion, anomaly CR diffusion and compound diffusion, the influence of magnetic clouds on CR propagation, non-diffusive CR particle pulse transport). Chapter 3 is devoted to CR non-linear effects in space plasmas caused by CR pressure and CR kinetic stream instabilities with the generation of Alfven turbulence (these effects are important in galaxies, in the Heliosphere, in CR and gamma-ray sources and in the processes of CR acceleration). considered: the development of the Fermi statistical mechanism, acceleration in the turbulent plasma, Alfven mechanism of magnetic pumping, induction mechanisms, acceleration during magnetic collapse and compression, cumulative acceleration mechanism near the zero lines of a magnetic field, acceleration in shear flows, shock-wave diffusion (regular) acceleration. The book ends with a list providing more than 1,300 full references, a discussion on future developments and unsolved problems, as well as Object and Author indexes. This book will be useful for experts and students in CR research, Astrophysics and Geophysics, and in Space Physics.