A Fourteen-Band Photometric Study of A2443

1 INTRODUCTION As the largest gravitational bound systems in the universe, clusters of galaxies are important laboratories for understanding the evolution of galaxies, and for constraining cosmological quantities (Bahcall 1988; Postman et al. 1992; Brunne…     

A Differential Abundance Analysis of HD219175 A and B

The abundances of the wide binary pair HD 219175 A and B are determined and compared using a line-by-line differential analysis. No evidence for difference has been found in the abundances of Fe, O, Na, Mg, Al, Si, K, Ca, Sc, Ti, V, Cr, Mn, Ni, Cu and Ba. Our results support a physical relation between the two components of HD 219175.     

The Precursor of GRB211211A:A Tide-induced Giant Quake?

The equilibrium configuration of a solid strange star in the final inspiral phase with another compact object is generally discussed,and the starquake-related issue is revisited,for a special purpose to understand the precursor emission of binary compact star merger events(e.g.,that of GRB211211A).As the binary system inspirals inward due to gravitational wave radiation,the ellipticity of the solid strangeon star increases due to the growing tidal field of its compact companion.Elastic energy is...     

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FIRI—A far-infrared interferometer

Half of the energy ever emitted by stars and accreting objects comes to us in the far-infrared (FIR) waveband and has yet to be properly explored. We propose a powerful Far-InfraRed Interferometer mission, FIRI, to carry out high-resolution imaging spectroscopy in the FIR. This key observational capability is essential to reveal how gas and dust evolve into stars and planets, how the first luminous objects in the Universe ignited, how galaxies formed, and when super-massive black holes grew. FIRI will disentangle the cosmic histories of star formation and accretion onto black holes and will trace the assembly and evolution of quiescent galaxies like our Milky Way. Perhaps most importantly, FIRI will observe all stages of planetary system formation and recognise the birth of planets via its ability to image the dust structures in planetary systems. FIRI is an observatory-class mission concept: three cold, 3.5-m apertures, orbiting a beam-combining module, with separations of up to 1 km, free-flying or tethered, operating between 25 and 385 μm, using the interferometric direct-detection technique to ensure μJy sensitivity and 0.02” resolution at 100 μm, across an arcmin² instantaneous field of view, with a spectral resolution, R ~ 5,000 and a heterodyne system with R ~ 1 million. Although FIRI is an ambitious mission, we note that FIR interferometry is appreciably less demanding than at shorter wavelengths. On behalf of the following scientists: Javier Alcolea, David Alexander, Philippe Andre, Rafael Bachiller, Mike Barlow, Andrey Baryshev, Alain Baudry, Carlton Baugh, Dominic Benford, Ted Bergin, Frank Bertoldi, Geoffrey Blake, Andrew Blain, Sylvain Bontemps, Franois Bouchet, Francois Boulanger, Jeroen Bouwman, Jonathan Braine, Bernhard Brandl, Valentin Bujarrabal, Sylvie Cabrit, Martin Caldwell, Daniela Calzetti, John Carpenter, Emmanuel Caux, Cecilia Ceccarelli, Jose Cernicharo Quintanilla, Pierre Chanial, Andrea Cimatti, John Conway, Pierre Cox, Dave Clements, Bill Dent, Gianfranco De Zotti, Carsten Dominik, Loretta Dunne, Steve Eales, Nicholas Elias, Duncan Farrah, Mike Fich, Jacqueline Fischer, Alberto Franceschini, David Frayer, Carlos Frenk, Gary Fuller, Maryvonne Gerin, Martin Giard, Thijs de Graauw, Gian Luigi Granato, Jane Greaves, Matt Griffin, Rolf Guesten, Stephane Guilloteau, Martin Harwit, Thomas Henning, Eric Herbst, Michiel Hogerheijde, Kate Isaak, Christine Joblin, Eelco van Kampen, Hubert Klahr, Kirsten Kraiberg Knudsen, Oliver Krause, Cedric Lacey, Robert Laing, Jean-Michel Lamarre, Huib Jan van Langevelde, David Leisawitz, Simon Lilly, Darek Lis, Rene Liseau, Enrico Lorenzini, Dieter Lutz, Michael Macintyre, Suzanne Madden, Roberto Maiolino, Jesus Martin-Pintado, Karine Mercier, Karl Menton, Vincent Minier, Raphael Moreno, Harvey Moseley, Takao Nakagawa, David Neufeld, Michael Olberg, Seb Oliver, Luca Olmi, Goran Olofsson, Hans Olofsson, Mat Page, Pantelis Papadopoulos, Juan Pardo, John Pearson, Ismael Perez-Fournon, Sabine Philipp, Rene Plume, Albrecht Poglitsch, Jean-Loup Puget, John Richer, Dimitra Rigopoulou, Stephen Rinehart, Peter Roelfsema, Paolo Saraceno, Rudolf Schieder, Karl-Friedrich Schuster, Gene Serabyn, Stephen Serjeant, Robert Simon, Ian Smail, Luigi Spinoglio, Jason Stevens, Eckhard Sturm, Juergen Stutzki, Bruce Swinyard, Emma Taylor, Floris van der Tak, Leonardo Testi, Wing-Fai Thi, Mattia Vaccari, Lars Venema, Laurent Vigroux, Serena Viti, Catherine Vlahakis, Christoffel Waelkens, Malcolm Walmsley, Fabian Walter, Rens Waters, Paul van der Werf, Paul Wesselius, Glenn White, Wolfgang Wild, Tom Wilson, Adam Woodcraft, Gillian Wright, FriedrichWyrowski, Harold Yorke, Min Yun, Jonas Zmuidzinas     

Centaurus A – NGC 5128

Summary. At a distance of 3.4 Mpc, NGC 5128 (Centaurus A) is by far the nearest active radio galaxy. It is often considered to be the prototype Fanaroff-Riley Class I ‘low-luminosity’ radio galaxy, and as such it plays an important role in our understanding of a major class of active galaxies. Its proximity has spawned numerous detailed investigations of its properties, yielding unrivalled but still incomplete knowledge of its structure and dynamics. The massive elliptical host galaxy is moderately triaxial and contains a thin, strongly warped disk rich in dust, atomic and molecular gas and luminous young stars. Its globular cluster ensemble has a bimodal distribution of metallicities. Deep optical images reveal faint major axis extensions as well as a system of filaments and shells. These and other characteristics are generally regarded as strong evidence that NGC 5128 has experienced a major merging events at least once in its past. The galaxy has a very compact, subparsec nucleus exhibiting noticeable intensity variations at radio and X-ray wavelengths, probably powered by accretion events. The central object may be a black hole of moderate mass. Towards the nucleus, rich absorption spectra of atomic hydrogen and various molecular species suggest the presence of significant amounts of material falling into the nucleus, presumably ‘feeding the monster’. Emanating from the nucleus are linear radio/X-ray jets, becoming subrelativistic at a few parsec from the nucleus. At about 5 kpc from the nucleus, the jets expand into plumes. Huge radio lobes extend beyond the plumes out to to 250 kpc. A compact circumnuclear disk with a central cavity surrounds the nucleus. Its plane, although at an angle to the minor axis of the galaxy, is perpendicular to the inner jets. The jet-collimating mechanism, probably connected to the circumnuclear disk, appears to precess on timescales of order a few times 10 years. This review summarizes the present state of knowledge of NGC 5128 and its associated radio source Centaurus A. Underlying physical processes are outside its scope: they are briefly referred to, but not discussed. Received 30 December 1997