@Article{Griffin_etal2010,
author="Griffin, M. J.
and Abergel, A.
and Abreu, A.
and Ade, P. A. R.
and Andr{\'e}, P.
and Augueres, J-L
and Babbedge, T.
and Bae, Y.
and Baillie, T.
and Baluteau, J-P
and Barlow, M. J.
and Bendo, G.
and Benielli, D.
and Bock, J. J.
and Bonhomme, P.
and Brisbin, D.
and Brockley-Blatt, C.
and Caldwell, M.
and Cara, C.
and Castro-Rodriguez, N.
and Cerulli, R.
and Chanial, P.
and Chen, S.
and Clark, E.
and Clements, D. L.
and Clerc, L.
and Coker, J.
and Communal, D.
and Conversi, L.
and Cox, P.
and Crumb, D.
and Cunningham, C.
and Daly, F.
and Davis, G. R.
and de Antoni, P.
and Delderfield, J.
and Devin, N.
and di Giorgio, A.
and Didschuns, I.
and Dohlen, K.
and Donati, M.
and Dowell, A.
and Dowell, C. D.
and Duband, L.
and Dumaye, L.
and Emery, R. J.
and Ferlet, M.
and Ferrand, D.
and Fontignie, J.
and Fox, M.
and Franceschini, A.
and Frerking, M.
and Fulton, T.
and Garcia, J.
and Gastaud, R.
and Gear, W. K.
and Glenn, J.
and Goizel, A.
and Griffin, D. K.
and Grundy, T.
and Guest, S.
and Guillemet, L.
and Hargrave, P. C.
and Harwit, M.
and Hastings, P.
and Hatziminaoglou, E.
and Herman, M.
and Hinde, B.
and Hristov, V.
and Huang, M.
and Imhof, P.
and Isaak, K. J.
and Israelsson, U.
and Ivison, R. J.
and Jennings, D.
and Kiernan, B.
and King, K. J.
and Lange, A. E.
and Latter, W.
and Laurent, G.
and Laurent, P.
and Leeks, S. J.
and Lellouch, E.
and Levenson, L.
and Li, B.
and Li, J.
and Lilienthal, J.
and Lim, T.
and Liu, S. J.
and Lu, N.
and Madden, S.
and Mainetti, G.
and Marliani, P.
and McKay, D.
and Mercier, K.
and Molinari, S.
and Morris, H.
and Moseley, H.
and Mulder, J.
and Mur, M.
and Naylor, D. A.
and Nguyen, H.
and O{\textquoteright}Halloran, B.
and Oliver, S.
and Olofsson, G.
and Olofsson, H-G
and Orfei, R.
and Page, M. J.
and Pain, I.
and Panuzzo, P.
and Papageorgiou, A.
and Parks, G.
and Parr-Burman, P.
and Pearce, A.
and Pearson, C.
and P{\'e}rez-Fournon, I.
and Pinsard, F.
and Pisano, G.
and Podosek, J.
and Pohlen, M.
and Polehampton, E. T.
and Pouliquen, D.
and Rigopoulou, D.
and Rizzo, D.
and Roseboom, I. G.
and Roussel, H.
and Rowan-Robinson, M.
and Rownd, B.
and Saraceno, P.
and Sauvage, M.
and Savage, R.
and Savini, G.
and Sawyer, E.
and Scharmberg, C.
and Schmitt, D.
and Schneider, N.
and Schulz, B.
and Schwartz, A.
and Shafer, R.
and Shupe, D. L.
and Sibthorpe, B.
and Sidher, S.
and Smith, A.
and Smith, A. J.
and Smith, D.
and Spencer, L.
and Stobie, B.
and Sudiwala, R.
and Sukhatme, K.
and Surace, C.
and Stevens, J. A.
and Swinyard, B. M.
and Trichas, M.
and Tourette, T.
and Triou, H.
and Tseng, S.
and Tucker, C.
and Turner, A.
and Vaccari, M.
and Valtchanov, I.
and Vigroux, L.
and Virique, E.
and Voellmer, G.
and Walker, H.
and Ward, R.
and Waskett, T.
and Weilert, M.
and Wesson, R.
and White, G. J.
and Whitehouse, N.
and Wilson, C. D.
and Winter, B.
and Woodcraft, A. L.
and Wright, G. S.
and Xu, C. K.
and Zavagno, A.
and Zemcov, M.
and Zhang, L.
and Zonca, E.",
title="The Herschel-SPIRE instrument and its in-flight performance",
journal="Astron. Astrophys.",
year="2010",
volume="518",
pages="7",
optkeywords="SPIRE",
abstract="The Spectral and Photometric Imaging REceiver (SPIRE), is the Herschel Space Observatory{\textquoteleft}s submillimetre camera and spectrometer. It contains a three-band imaging photometer operating at 250, 350 and 500 $\mu$m, and an imaging Fourier-transform spectrometer (FTS) which covers simultaneously its whole operating range of 194-671 $\mu$m (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{\^A}{\textasciiacute}{\texttimes} 8{\^A}{\textasciiacute}, 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{\^A}{\textasciiacute}. 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.",
optnote="exported from refbase (https://db.rplab.ru/refbase/show.php?record=695), last updated on Sat, 04 Jun 2016 09:40:13 -0500"
}