Griffin, M. J. and Hristov, V. and Lange, A. E. and Latter, W. and Levenson, L. and Lu, N. and Schulz, B. and Schwartz, A. and Shupe, D. L. and Xu, C. K. and Zemcov, M. and Zhang, L. (2010) The Herschel-SPIRE instrument and its in-flight performance. Astronomy and Astrophysics, 518 . L3. ISSN 0004-6361 http://resolver.caltech.edu/CaltechAUTHORS:20101117-104045678
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The Spectral and Photometric Imaging REceiver (SPIRE), is the Herschel Space Observatory`s submillimetre camera and spectrometer. It contains a three-band imaging photometer operating at 250, 350 and 500 μm, and an imaging Fourier-transform spectrometer (FTS) which covers simultaneously its whole operating range of 194–671 μm (447–1550 GHz). The SPIRE detectors are arrays of feedhorn-coupled bolometers cooled to 0.3 K. The photometer has a field of view of 4´× 8´, observed simultaneously in the three spectral bands. Its main operating mode is scan-mapping, whereby the field of view is scanned across the sky to achieve full spatial sampling and to cover large areas if desired. The spectrometer has an approximately circular field of view with a diameter of 2.6´. The spectral resolution can be adjusted between 1.2 and 25 GHz by changing the stroke length of the FTS scan mirror. Its main operating mode involves a fixed telescope pointing with multiple scans of the FTS mirror to acquire spectral data. For extended source measurements, multiple position offsets are implemented by means of an internal beam steering mirror to achieve the desired spatial sampling and by rastering of the telescope pointing to map areas larger than the field of view. The SPIRE instrument consists of a cold focal plane unit located inside the Herschel cryostat and warm electronics units, located on the spacecraft Service Module, for instrument control and data handling. Science data are transmitted to Earth with no on-board data compression, and processed by automatic pipelines to produce calibrated science products. The in-flight performance of the instrument matches or exceeds predictions based on pre-launch testing and modelling: the photometer sensitivity is comparable to or slightly better than estimated pre-launch, and the spectrometer sensitivity is also better by a factor of 1.5–2.
|Additional Information:||© 2010 ESO. Received 26 March 2010; Accepted 21 April 2010; Published online 16 July 2010. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA (USA).|
|Subject Keywords:||instrumentation: photometers; instrumentation: spectrographs; space vehicles: instruments; submillimeter: general|
|Official Citation:||The Herschel-SPIRE instrument and its in-flight performance M. J. Griffin, A. Abergel, A. Abreu, P. A. R. Ade, P. André, J.-L. Augueres, T. Babbedge, Y. Bae, T. Baillie, J.-P. Baluteau, M. J. Barlow, G. Bendo, D. Benielli, J. J. Bock, P. Bonhomme, D. Brisbin, C. Brockley-Blatt, M. Caldwell, C. Cara, N. Castro-Rodriguez, R. Cerulli, P. Chanial, S. Chen, E. Clark, D. L. Clements, L. Clerc, J. Coker, D. Communal, L. Conversi, P. Cox, D. Crumb, C. Cunningham, F. Daly, G. R. Davis, P. De Antoni, J. Delderfield, N. Devin, A. Di Giorgio, I. Didschuns, K. Dohlen, M. Donati, A. Dowell, C. D. Dowell, L. Duband, L. Dumaye, R. J. Emery, M. Ferlet, D. Ferrand, J. Fontignie, M. Fox, A. Franceschini, M. Frerking, T. Fulton, J. Garcia, R. Gastaud, W. K. Gear, J. Glenn, A. Goizel, D. K. Griffin, T. Grundy, S. Guest, L. Guillemet, P. C. Hargrave, M. Harwit, P. Hastings, E. Hatziminaoglou, M. Herman, B. Hinde, V. Hristov, M. Huang, P. Imhof, K. J. Isaak, U. Israelsson, R. J. Ivison, D. Jennings, B. Kiernan, K. J. King, A. E. Lange, W. Latter, G. Laurent, P. Laurent, S. J. Leeks, E. Lellouch, L. Levenson, B. Li, J. Li, J. Lilienthal, T. Lim, S. J. Liu, N. Lu, S. Madden, G. Mainetti, P. Marliani, D. McKay, K. Mercier, S. Molinari, H. Morris, H. Moseley, J. Mulder, M. Mur, D. A. Naylor, H. Nguyen, B. O'Halloran, S. Oliver, G. Olofsson, H.-G. Olofsson, R. Orfei, M. J. Page, I. Pain, P. Panuzzo, A. Papageorgiou, G. Parks, P. Parr-Burman, A. Pearce, C. Pearson, I. Pérez-Fournon, F. Pinsard, G. Pisano, J. Podosek, M. Pohlen, E. T. Polehampton, D. Pouliquen, D. Rigopoulou, D. Rizzo, I. G. Roseboom, H. Roussel, M. Rowan-Robinson, B. Rownd, P. Saraceno, M. Sauvage, R. Savage, G. Savini, E. Sawyer, C. Scharmberg, D. Schmitt, N. Schneider, B. Schulz, A. Schwartz, R. Shafer, D. L. Shupe, B. Sibthorpe, S. Sidher, A. Smith, A. J. Smith, D. Smith, L. Spencer, B. Stobie, R. Sudiwala, K. Sukhatme, C. Surace, J. A. Stevens, B. M. Swinyard, M. Trichas, T. Tourette, H. Triou, S. Tseng, C. Tucker, A. Turner, M. Vaccari, I. Valtchanov, L. Vigroux, E. Virique, G. Voellmer, H. Walker, R. Ward, T. Waskett, M. Weilert, R. Wesson, G. J. White, N. Whitehouse, C. D. Wilson, B. Winter, A. L. Woodcraft, G. S. Wright, C. K. Xu, A. Zavagno, M. Zemcov, L. Zhang and E. Zonca A&A 518 L3 (2010) DOI: 10.1051/0004-6361/201014519|
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|Deposited By:||Jason Perez|
|Deposited On:||17 Nov 2010 23:36|
|Last Modified:||26 Dec 2012 12:39|
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