APEX-SZ a Sunyaev–Zel’dovich galaxy cluster survey     

D. Schwan  F. Bertoldi  S. Cho  M. Dobbs  R. Guesten  N. W. Halverson  W. L. Holzapfel  E. Kreysa  T. M. Lanting  A. T. Lee  M. Lueker  J. Mehl  K. Menten  D. Muders  M. Myers  T. Plagge  A. Raccanelli  P. Schilke  P. L. Richards  H. Spieler  M. White 《New Astronomy Reviews》2003,47(11-12):933

The APEX-SZ experiment is a sky survey designed to discover galaxy clusters via the Sunyaev–Zel’dovich effect at millimeter wavelengths. We describe the components of the instrument, including the 12 m Atacama Pathfinder Experiment telescope, optics, Transition-edge sensor bolometer array and SQUID readout. APEX-SZ will begin observations in 2004.  相似文献   

Coordinated Observations of Comet Hale–Bopp between 32 and 860 GHz     

Wink  J. E.  Altenhoff  W. J.  Bieging  J.  Butler  B.  Butner  H.  Haslam  C.G.T.  Kreysa  E.  Martin  R.  Mauersberger  R.  McMullin  J.  Muders  D.  Peters  W.  Schmidt  J.  Schraml  J. B.  Sievers  A.  Stumpff  P.  Von Kapp-Herr  A.  Thum  C.  Zylka  R. 《Earth, Moon, and Planets》1997,77(3):165-165

Earth, Moon, and Planets - The concept of simultaneous multifrequency continuum observations, successfully tested on Comet Hyakutake, was applied to Comet Hale-Bopp, using the Heinrich Hertz...  相似文献   

APEX-SZ first light and instrument status     

M. Dobbs  N.W. Halverson  P.A.R. Ade  K. Basu  A. Beelen  F. Bertoldi  C. Cohalan  H.M. Cho  R. Güsten  W.L. Holzapfel  Z. Kermish  R. Kneissl  A. Kovcs  E. Kreysa  T.M. Lanting  A.T. Lee  M. Lueker  J. Mehl  K.M. Menten  D. Muders  M. Nord  T. Plagge  P.L. Richards  P. Schilke  D. Schwan  H. Spieler  A. Weiss  M. White 《New Astronomy Reviews》2006,50(11-12):960

The apex-sz instrument is designed for the discovery and study of galaxy clusters at mm-wavelengths using the Sunyaev Zel’dovich effect. The receiver consists of 320 superconducting transition edge sensor (TES) bolometers cooled to 250 mK with the combination of a three stage He sorption fridge and mechanical pulse tube cooler. The detectors are instrumented with a frequency domain multiplexing readout system. The receiver is mounted on the 12 m apex telescope located at 5100 m on the Atacama plateau in Chile. For the first light engineering deployment of December 2005, the receiver was configured with a 55 element wedge of the bolometers and operating in the 150 GHz atmospheric window. During the engineering run we achieved significant milestones in our instrumentation development efforts, including celestial observations with a monolithically fabricated TES bolometer array cooled with a mechanical cooler and successful implementation of a SQUID-based MHz AC-biased readout. These technology demonstrations point the way toward future large TES bolometer array instruments. Here we describe the results of this deployment and future plans for the apex-sz instrument.  相似文献   

    

J. E. Wink  W. J. Altenhoff  J. Bieging  B. Butler  H. Butner  C.G.T. Haslam  E. Kreysa  R. Martin  R. Mauersberger  J. McMullin  D. Muders  W. Peters  J. Schmidt  J. B. Schraml  A. Sievers  P. Stumpff  A. Von Kapp-Herr  C. Thum  R. Zylka 《Earth, Moon, and Planets》1997,77(3):165

The concept of simultaneous multifrequency continuum observations, successfully tested on Comet Hyakutake, was applied to Comet Hale-Bopp, using the Heinrich Hertz Submillimeter Telescope (HHT) with the four color bolometer between 250 and 870 GHz, the IRAM 30m telescope at 240 Ghz, the MPIfR 100-m telescope at 32 GHz, and the IRAM interferometer near 90 and 240 GHz. Near-simultaneous measurements were done between February 15 and April 26, 1997, mainly concentrated in mid March shortly before perigee of the comet. The measurements gave the following preliminary results: Interferometer detection of the nuclear thermal emission. If the signal at the longest interferometer spacing of 170 mis due to thermal emission from the nucleus only, its equivalent diameter is ∼49 km. If, however, this signal contains a contribution from a strongly centrally peaked halo distribution(e.g., r⁻² density variation) the diameter may be as low as 35 km. The emission found interferometrically was always 5″ north and 0.1 sec east from the position predicted by Yeoman's solution 55.The comparison of the interferometric continuum emission with the simultanously obtained molecular line observations (reported on this conference) shows the origin of the strongest line emission concentrated on the nucleus. The 30-m observations show a radio halo with a gaussian FWHP of ∼11, corresponding to a diameter of 11000 km at geocentric distance of 1.2 a.u. A spectral index of ∼3.0 for the total signal, which may indicate a smaller mean particle size than for Hyakutake. Assuming an average cometary density of 0.5 gcm⁻³, the mass contained in the nucleus is ∼1$#x2013;3 10¹⁹ g and 10¹² g in the particle halo. This revised version was published online in July 2006 with corrections to the Cover Date.  相似文献