Herschel-SPIRE: design, ground test results, and predicted performance

Griffin, Matthew Joseph; Swinyard, Bruce; Vigroux, L.; Abergel, A.; Ade, Peter A. R.; André, P.; Baluteau, Jean-Paul; Bock, J. J.; Franceschini, A.; Gear, Walter Kieran; Glenn, J.; Huang, M.; Griffin, Douglas; King, K. J.; Lellouch, E.; Naylor, David; Oliver, Seb; Olofsson, G.; Pérez-Fournón, I.; Page, M. J.; Rowan-Robinson, M.; Saraceno, P.; Sawyer, Eric; Wright, Gillian; Zavagno, A.; Abreu, A.; Bendo, G. J.; Dowell, A. A. Mac; Dowell, Darren; Ferlet, Marc; Fulton, T.; Hargrave, Peter Charles; Laurent, G. T.; Leeks, S. J.; Lim, T.; Lu, N.; Nguyen, Hien; Pearce, Alan; Polehampton, E. T.; Rizzo, D.; Schulz, B.; Sidher, S.; Smith, David L.; Spencer, L. D.; Valtchanov, I.; Woodcraft, A.; Xu, Kevin; Zhang, Lijun

doi:10.1117/12.788312

Cited by 36 publications

(17 citation statements)

References 27 publications

(32 reference statements)

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“…We use telluric transmission models with 0.5 mm and 0.72 mm PWV for APEX and CSO (at band center) respectivelyappropriate for good submillimeter nights at their sites (APEX windows < 300 μm use 0.2 mm). Also plotted is the sensitivity of ZEUS, the published preflight sensitivities of the 3 spectrometers on the Herschel telescope 33,34,35 with HIFI and PACS scaled to the resolving power of ZEUS-2: R = 1000, or Δυ = 300 km s -1 , appropriate for typical extragalactic line widths. ZEUS-2 is ~10 times more sensitive in the primary bands.…”

Section: Discussionmentioning

confidence: 99%

ZEUS-2: a second generation submillimeter grating spectrometer for exploring distant galaxies

et al. 2010

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ZEUS-2, the second generation (z)Redshift and Early Universe Spectrometer, like its predecessor is a moderate resolution (R~1000) long-slit, echelle grating spectrometer optimized for the detection of faint, broad lines from distant galaxies. It is designed for studying star-formation across cosmic time. ZEUS-2 employs three TES bolometer arrays (555 pixels total) to deliver simultaneous, multi-beam spectra in up to 4 submillimeter windows. The NIST Boulder-built arrays operate at ~100mK and are readout via SQUID multiplexers and the Multi-Channel Electronics from the University of British Columbia. The instrument is cooled via a pulse-tube cooler and two-stage ADR. Various filter configurations give ZEUS-2 access to 7 different telluric windows from 200 to 850 micron enabling the simultaneous mapping of lines from extended sources or the simultaneous detection of the 158 micron [CII] line and the [NII] 122 or 205 micron lines from z = 1-2 galaxies. ZEUS-2 is designed for use on the CSO, APEX and possibly JCMT.

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Section: Discussionmentioning

confidence: 99%

ZEUS-2: a second generation submillimeter grating spectrometer for exploring distant galaxies

et al. 2010

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“…E.g. the HERSCHEL/SPIRE instrument design 6 , which was used as the starting point for SPICA/SAFARI, had two roof-tops. The original SAFARI design 5 had two cat's-eyes, see Figure 1.…”

Section: Original 2009 Designmentioning

confidence: 99%

Spectroscopic closed loop control of penetration depth in laser beam welding process

Sibillano¹,

Ancona²,

Rizzi

et al. 2012

High Power Laser Materials Processing: Lasers, Beam Delivery, Diagnostics, and Applications

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TNO, together with its partners, have designed a cryogenic scanning mechanism for use in the SAFARI 1 Fourier Transform Spectrometer (FTS) on board of the SPICA mission. SPICA is one of the M-class missions competing to be launched in ESA's Cosmic Vision Programme 2 in 2022. JAXA 3 leads the development of the SPICA satellite and SRON is the prime investigator of the Safari instrument.The FTS scanning mechanism (FTSM) has to meet a 35 mm stroke requirement with an Optical Path Difference resolution of less then 15 nm and must fit in a small volume. It consists of two back-to-back roof-top mirrors mounted on a small carriage, which is moved using a magnetic bearing linear guiding system in combination with a magnetic linear motor serving as the OPD actuator. The FTSM will be used at cryogenic temperatures of 4 Kelvin inducing challenging requirements on the thermal power dissipation and heat leak.The magnetic bearing enables movements over a scanning stroke of 35.5 mm in a small volume. It supports the optics in a free-floating way with no friction, or other non-linearities, with sub-nanometer accuracy. This solution is based on the design of the breadboard ODL (Optical Delay Line) developed for the ESA Darwin mission 4 and the MABE mechanism developed by Micromega Dynamics.During the last couple of years the initial design of the SAFARI instrument, as described in an earlier SPIE 2010 paper 5 , was adapted by the SAFARI team in an evolutionary way to meet the changing requirements of the SPICA payload module. This presentation will focus on the evolution of the FTSM to meet these changing requirements. This work is supported by the Netherlands Space Office (NSO).

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“…The tests performed at instrument level are described in references [8][9][10]. The tests performed at this level were both environmental tests (Mechanical, Thermal, EMC) for both qualification and acceptance) and performance / calibration tests.…”

Section: Instrument Level Testmentioning

confidence: 99%

Herschel: Testing of Cryogenics Instruments at Spacecraft Level and Early Flight Results

Collaudin¹,

Montet²,

Roche³

et al. 2010

AIP Conference Proceedings

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Herschel cryogenics instrument (HIFI, PACS, SPIRE) flight models have been delivered to ESA & Prime contractor Thales Alenia Space mid 2007, to be integrated and tested on the Herschel spacecraft, for a launch mid May 2009.The instrument integration and test campaign at spacecraft level was performed between mid 2007 and end 2008 in Astrium GmbH, Immenstadt (Gernany) and later in ESA's test facilities at Estec, Noordwijk (Nederland). The objective of these tests was to demonstrate full operability and performances of the instruments in spacecraft configuration, and their compatibility with the launch and space environment, while maintaining full compliance with the underlying requirements. A set of short functional tests were developed and used repeatedly to quickly check the health of each instrument at key points in the test campaign. Typically, this was after integration of a major component, prior to a major environmental test or before/after movement of the spacecraft. A set of full 1510 CREDIT LINE (BELOW) TO BE INSERTED ON THE FIRST PAGE OF EACHPAPER EXCEPT FOR ARTICLES ON pp. 18-25, 26-33, 68-75, 121-127, 136-142, 207-214, 246-253, 355-362, 388-395, 499-506, 507-514, 609-614, 780-787, 796-803, 804-811, 905-912, 1291-1300, 1301-1308, 1369-1376, 1581-1592, 1593-1600, and 1647-1651 functional tests were also performed after launch vibration tests, and during Thermal vacuum test in order to provide a more complete picture of the instruments functional health. Finally a set of instrument specific tests were performed to verify the performance of the instrument under the most representative operational conditions possible on ground (i.e. the environmental test campaign). The paper will describe instruments and the instruments related tests performed at spacecraft level, focusing on cryogenics aspects.

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Herschel-SPIRE: design, ground test results, and predicted performance

Cited by 36 publications

References 27 publications

ZEUS-2: a second generation submillimeter grating spectrometer for exploring distant galaxies

ZEUS-2: a second generation submillimeter grating spectrometer for exploring distant galaxies

Spectroscopic closed loop control of penetration depth in laser beam welding process

Herschel: Testing of Cryogenics Instruments at Spacecraft Level and Early Flight Results

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