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1. Thermal conductance at millikelvin temperatures of woven ribbon cable with phosphor-bronze clad superconducting wires

Author: Adam Woodcraft, Wayne S. Holland, V. Martelli, and G. Ventura
Subjects: Materials science, Phosphor bronze, Niobium, General Physics and Astronomy, chemistry.chemical_element, Cryogenics, Conductivity, Cladding (fiber optics), law.invention, Thermal conductivity, Ribbon cable, chemistry, law, Ribbon, General Materials Science, Composite material
Abstract: Woven Nomex® ribbon cables made up with superconducting niobium–titanium wire are used at millikelvin temperatures in many large cryogenic instruments. It is important to know how much heat in transmitted down such cables. However, the conductivity of the materials used is not well known. Another problem is that the wires are normally clad with alloys which exhibit some magnetism. This is a potential problem for instruments employing superconducting detectors. A safe non-magnetic alternative to the usual materials is phosphor-bronze clad niobium–titanium wiring. However, there is little experience with such wires. We have therefore measured the conductance of a ribbon cable made up with these wires. The measured values are in good agreement with our predictions, suggesting that the values we have used to model the cable are sufficiently accurate, and could therefore be used to predict the performance of ribbon cables using other cladding materials, so long as the conductivity of the cladding is reasonably well known. As part of our analysis, we consider the likely variation in thermal conductivity values for C51000 phosphor bronze caused by legitimate variations in composition.
Published: 2010
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2. Thermal conductivity of Tecamax® SRP from millikelvin temperatures to room temperature

Author: G. Ventura, V. Martelli, and Adam Woodcraft
Subjects: chemistry.chemical_classification, Materials science, General Physics and Astronomy, Thermodynamics, Cryogenics, Polymer, Conductivity, Amorphous solid, Thermal conductivity, chemistry, Ultimate tensile strength, Molecule, General Materials Science, Cryogenic temperature
Abstract: Tecamax® SRP (self-reinforced polyphenylene) is a new commercially available amorphous polymer which is suitable for use at cryogenic temperatures. It has a high tensile strength (210 MPa at room temperature), resulting from the molecular structure of the polymer rather than by the addition of reinforcing materials. We have measured the thermal conductivity between 60 mK and 280 K. We find that the conductivity below 10 K is similar to, but lower than, most amorphous materials, and the material offers a good combination of low conductivity at low temperatures and high tensile strength. Our results suggest that the material may in fact have a small crystalline component, which may be a partial explanation for the low conductivity. Above 10 K, the temperature dependence of the conductivity is different from most amorphous materials. We are unaware of previous measurements of the thermal conductivity of this material, even at room temperature.
Published: 2010
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3. Thermal design and performance of the SCUBA-2 instrument 1-K and mK systems

Author: Matthew I. Hollister, Wayne S. Holland, David C. Gostick, Fred Gannaway, Dan Bintley, and Adam Woodcraft
Subjects: Cryostat, Materials science, Thermal conductivity, business.industry, Thermal, Detector, Refrigerator car, General Physics and Astronomy, General Materials Science, Dilution refrigerator, Cryogenics, Aerospace engineering, business
Abstract: Various research fields require large and complex instrumen ts containing detectors operating at millikelvin temperatures. The materials and techniques traditionally used in cryogenics are often unsuitable for the demanding requirements of such instruments. We describe the thermal design and performance of the 1-K and millikelvin systems of the SCUBA-2 instrument. This is an astronomical “camera” operating at wavelengths of 450 and 850 µm. It is the largest and most complex instrument ever built for sub-mm astronomy, and the first to use a cryogen-free dilution refrigerator. The design con sists of a mix of traditional techniques (but used in demanding situations) as well as novel elements. The thermal performance has been stable and very successful, and we hope that the details described here will be useful to the designers of future large instruments.
Published: 2009
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4. Proposed designs for a 'dry' dilution refrigerator with a 1K condenser

Author: Adam Woodcraft and Matthew I. Hollister
Subjects: Cryostat, Materials science, Nuclear engineering, Joule–Thomson effect, Refrigerator car, General Physics and Astronomy, Thermodynamics, Cryogenics, Heat sink, Cryocooler, symbols.namesake, symbols, General Materials Science, Dilution refrigerator, Condenser (heat transfer)
Abstract: Recent development of “dry” dilution refrigerators has used mechanical cryocoolers and Joule–Thomson expansion stages to cool and liquefy the circulating ^3He. While this approach has been highly successful, we propose three alternative designs that use independently-cooled condensers. In the first, the circulating helium is precooled by a mechanical cooler, and liquified by self-contained ^4He sorption coolers. In the second, the helium is liquefied by a closed-cycle, continuous flow ^4He refrigerator operating from a room temperature pump. Finally, the third scheme uses a separate ^4He Joule–Thomson stage to cool the ^3He condenser. The condensers in all these schemes are analogous to the “1-K pot” in a conventional dilution refrigerator. Such an approach would be advantageous in certain applications, such as instrumentation for astronomy and particle physics experiment, where a thermal stage at approximately 1 K would allow an alternative heat sink to the still for electronics and radiation shielding, or quantum computer research where a large number of coaxial cables must be heat sunk in the cryostat. Furthermore, the behaviour of such a refrigerator is simplified due to the separation of the condenser stage from the dilution circuit, removing the complex interaction between the 4-K, Joule–Thomson, still and mixing chamber stages found in current dry DR designs.
Published: 2009
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5. Detectors for sub-millimetre continuum astronomy

Author: Adam Woodcraft
Subjects: Physics, Nuclear and High Energy Physics, Explosive material, Pixel, Continuum (topology), Instrumentation, Bolometer, Detector, Astronomy, law.invention, Single pixel, law, Millimeter
Abstract: Sub-mm astronomy has seen an explosive growth in recent years. This has been driven by improvements in detector technology, and in particular the move from single pixel photometric instruments to ones containing arrays of hundreds and even thousands of pixels. Sub-mm detectors are different from those used in astronomy at most other wavelengths in that they are not produced commercially. Instead, research, development and construction is carried out in universities and government laboratories. We are also at an interesting point in that several competing detector technologies are under development and it is not yet clear which will be used in future instruments. I review current instruments as well as the issues facing us in developing the next generation of instruments, operating both on the ground and from space.
Published: 2009
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6. Thermal conductivity measurements of pitch-bonded graphites at millikelvin temperatures: Finding a replacement for AGOT graphite

Author: Adam Woodcraft, Lara Risegari, G. Ventura, L. Lolli, V. Martelli, Peter Hastings, and Marco Barucci
Subjects: Materials science, business.industry, Orders of magnitude (temperature), General Physics and Astronomy, Insulator (electricity), Conductivity, Thermal conductivity, Operating temperature, Thermal insulation, General Materials Science, Graphite, Composite material, business, Electrical conductor
Abstract: Pitch-bonded graphites are among the best known thermal insulators at sub-kelvin temperatures, but are very good conductors at higher temperatures. This makes them ideal for mechanical supports which must provide good thermal isolation at an operating temperature below 1 K, but must have good conductance at higher temperatures to aid in initially cooling down an instrument (a “passive heat switch”). One type of graphite, AGOT, has been known as having the lowest thermal conductivity below 1 K not only among graphites, but also compared with any other material. It is, however, no longer available. We have carried out thermal conductivity measurements at temperatures between 60 mK and 4 K on a proposed replacement, POCO AXM-5Q graphite, as well as a sample of AGOT graphite. Our measurements show that both graphites have a difference of about six orders of magnitude in conductivity between room temperature and 100 mK, but that AGOT graphite is not as good an insulator as previously believed. We conclude that AXM-5Q graphite is not only a suitable replacement for AGOT, but in fact is somewhat superior.
Published: 2009
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7. Millikelvin thermal conductance measurements of compact rigid thermal isolation joints using sapphire–sapphire contacts, and of copper and beryllium–copper demountable thermal contacts

Author: Fred Gannaway, Dan Bintley, and Adam Woodcraft
Subjects: Thermal contact conductance, Materials science, General Physics and Astronomy, chemistry.chemical_element, Beryllium copper, engineering.material, Thermal conduction, Copper, Thermal conductivity, chemistry, Bolted joint, Sapphire, engineering, General Materials Science, Composite material, Joint (geology)
Abstract: We present thermal conductance measurements of different types of bolted joint at sub-Kelvin temperatures. Joints containing sapphire surfaces provided good thermal isolation; the mechanism appears to be the existence of a very small area over which the surfaces are actually in contact. Various configurations were measured at temperatures between 100 mK and 4 K. The best joint contained sapphire discs separated by diamond powder and had a conductance of 0.26 μW K−1 (T/1 K)2.9, where T is temperature. A mechanical support structure constructed from similar joints, but using alumina powder, had a measured heat leak of 2.57 μW between 80 mK and 1.1 K and was capable of supporting a mass of over 10 kg. Joints between metal surfaces provided good thermal conduction; a bolted joint between copper and a beryllium–copper alloy (C17510 TF00) had a measured conductance of 46 mW K−1 at 100 mK, increasing linearly with temperature. Measurements were also made on a copper–copper compression joint using differential thermal contraction to provide the clamping force. The performance was approximately an order of magnitude worse than for the bolted joint. These measurements were all made as part of the development programme for the SCUBA-2 astronomical instrument; the design requirements were achieved for both insulating and conducting joints.
Published: 2007
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8. The design, construction and measurement of a quasi-optical multiplexer and antenna for space-borne atmospheric measurements from 56 to 425 GHz

Author: Xu Hongxin, Stuart Froud, Peter A. R. Ade, Carole Tucker, Xie Zhenchao, A. Hornsby, Jiang Lifei, Adam Woodcraft, Stephen M. Hanham, William J. Otter, Richard Wylde, and Kevin J. Pike
Subjects: Physics, Optics, business.industry, Terahertz radiation, Horn (acoustic), Detector, Radiometry, Antenna (radio), Wideband, business, Dichroic glass, Multiplexer
Abstract: We have developed a low-loss quasi-optical multiplexer (QOM) for future space-based meteorological radiometry covering nearly a decade of frequencies — from 54 GHz to 425 GHz. We have shown that very low loss can be combined with high channel co-alignment in a compact package, suitable for surviving the launch environment. The QOM uses shallow angle low-loss dichroic plates (DCP's) allowing polarization diversity and ultra-Gaussian horn feeds to minimize both component size and standing waves. The losses in the multiplexer were measured using a novel double path S 11 VNA technique, and beam co-alignment was verified by scanning with a wideband detector.
Published: 2015
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9. Recommended values for the thermal conductivity of aluminium of different purities in the cryogenic to room temperature range, and a comparison with copper

Author: Adam Woodcraft
Subjects: Materials science, General Physics and Astronomy, chemistry.chemical_element, Thermodynamics, Cryogenics, Atmospheric temperature range, Conductivity, Temperature measurement, Copper, Thermal conductivity, chemistry, Aluminium, Electrical resistivity and conductivity, General Materials Science
Abstract: The thermal conductivity of pure aluminium at cryogenic temperatures varies by many orders of magnitude depending on purity and treatment, and there is little information in the literature on the likely values to be obtained for samples of a given purity. A compilation of measurements from the literature has been assembled and used to provide recommended ranges of values for aluminium of different purities (4N, 5N and 6N) in the normal (non superconducting) state. The number of direct thermal conductivity measurements is too limited to be used alone. Electrical resistivity measurements have thus also been used by converting to thermal conductivity using the Wiedemann–Franz law, which is shown to be valid. Since low temperature measurements can easily be extrapolated to higher temperatures, the results cover the range from 1.2 K (the superconducting transition temperature) to room temperature. Values for 5N purity copper have also been examined in a similar manner, to allow a comparison between the two materials. The main application of these results is in the design of cryogenic thermal links; a discussion of the advantages and disadvantages of both materials for this use is given. The use of silver is also investigated briefly. Trends in the behaviour of the conductivity of aluminium in the superconducting state (to temperatures as low as 50 mK) are also discussed.
Published: 2005
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10. Predicting the thermal conductivity of aluminium alloys in the cryogenic to room temperature range

Author: Adam Woodcraft
Subjects: Materials science, General Physics and Astronomy, chemistry.chemical_element, Thermodynamics, Cryogenics, Atmospheric temperature range, Temperature measurement, Thermal conductivity measurement, Thermal conductivity, chemistry, Aluminium, Electrical resistivity and conductivity, visual_art, Aluminium alloy, visual_art.visual_art_medium, General Materials Science, Composite material
Abstract: Aluminium alloys are being used increasingly in cryogenic systems. However, cryogenic thermal conductivity measurements have been made on only a few of the many types in general use. This paper describes a method of predicting the thermal conductivity of any aluminium alloy between the superconducting transition temperature (approximately 1 K) and room temperature, based on a measurement of the thermal conductivity or electrical resistivity at a single temperature. Where predictions are based on low temperature measurements (approximately 4 K and below), the accuracy is generally better than 10%. Useful predictions can also be made from room temperature measurements for most alloys, but with reduced accuracy. This method permits aluminium alloys to be used in situations where the thermal conductivity is important without having to make (or find) direct measurements over the entire temperature range of interest. There is therefore greater scope to choose alloys based on mechanical properties and availability, rather than on whether cryogenic thermal conductivity measurements have been made. Recommended thermal conductivity values are presented for aluminium 6082 (based on a new measurement), and for 1000 series, and types 2014, 2024, 2219, 3003, 5052, 5083, 5086, 5154, 6061, 6063, 6082, 7039 and 7075 (based on low temperature measurements in the literature).
Published: 2005
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11. Prototype detector technology for the SCUBA-2 submillimetre bolometer array

Author: Camelia Dunare, Kent D. Irwin, Wayne S. Holland, Andrew Bunting, Adam Woodcraft, H. McGregor, Stewart Smith, Anthony J. Walton, P. A. R. Ade, R. V. Sudiwala, Eric F Schulte, William Parkes, Joel N. Ullom, J.T.M. Stevenson, William Duncan, Alan M. Gundlach, Michael D. Audley, Gene C. Hilton, and Jonathan G. Terry
Subjects: Microelectromechanical systems, Materials science, business.industry, Bolometer, Detector, Condensed Matter Physics, law.invention, Surface micromachining, law, Microsystem, Optoelectronics, General Materials Science, Electronics, Electrical and Electronic Engineering, Transition edge sensor, business, James Clerk Maxwell Telescope
Abstract: This paper reports the latest design and the associated fabrication technology of the Mk II prototype infrared (IR) detector for the two 5120 pixel SCUBA-2 (submillimetre common user bolometer arry) instruments, which are to be mounted on the James Clerk Maxwell telescope (JCMT) in Hawaii. Progress is described on the design and the technology modules being developed for the new detector, which is based upon silicon micromachining. The two arrays of transition edge sensors (TES) are used to detect incoming radiation with wavelengths of 450 and 850 μ respectively and as the SCUBA-2 detector operates at about 100 mK, it consequently involves integration with low-temperature electronics and careful design of the associated interconnect. A key aspect of the connection between the TES detector and readout electronics is the use of indium flip-chip bumps, which become superconducting at cryogenic temperatures. The integration of nanoscale membranes and transition edge sensors together with microsystem technology enables SCUBA-2 to have of the order of 10 -17W (1 Hz bandwidth) sensitivity to incoming radiation.
Published: 2005
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12. Thermal conductance measurements of bolted copper to copper joints at sub-Kelvin temperatures

Author: Dan Bintley, Peter Charles Hargrave, Iris Didschuns, and Adam Woodcraft
Subjects: Thermal contact conductance, Materials science, General Physics and Astronomy, Thermal contact, Conductance, chemistry.chemical_element, Cryogenics, Copper, Thermal conductivity, chemistry, Electrical resistance and conductance, Narrow range, General Materials Science, Composite material
Abstract: We have measured the thermal contact conductance of several demountable copper joints below 1 K. Joints were made by bolting together either two flat surfaces or a clamp around a rod. Surfaces were gold plated, and no intermediate materials were used. A linear dependence on temperature was seen. Most of the measured conductance values fell into a narrow range: 0.1–0.2 W K−1 at 1 K. Results in the literature for similar joints consist of predictions based on electrical resistance measurements using the Wiedemann–Franz law. There is little evidence of the validity of this law in the case of joints. Nevertheless, our results are in good agreement with the literature predictions, suggesting that such predictions are a reasonable approximation.
Published: 2004
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13. SCUBA-2 arrays to system interfaces

Author: William Parkes, T. Baillie, M. Cliffe, Maureen A. Ellis, J. Molnar, Kent D. Irwin, L. Ferreira, Wayne S. Holland, Dan Bintley, A. D. Ruthven, Gene C. Hilton, M. Fich, C. D. Reintsema, Jan Kycia, T. Hodson, H. McGregor, M. J. MacIntosh, Fred Gannaway, Xiaofeng Gao, Camelia Dunare, Adam Woodcraft, J. N. Ullom, Jonathan G. Terry, William B. Doriese, D. Audley, M. Halpern, T. Peacocke, Ian Robson, Anthony Walton, G. Mitchell, Carole Tucker, David Atkinson, Matthew Joseph Griffin, Peter A. R. Ade, L. R. Vale, David C. Gostick, B. Burger, Ian Walker, D. Kelly, Eric F Schulte, Tom Stevenson, D. Naylor, W. D. Duncan, Stewart Smith, Rashmikant V. Sudiwala, Alan M. Gundlach, P. Bastien, and I. Smith
Subjects: Physics, business.industry, Stray light, Bolometer, Electrical engineering, General Medicine, Multiplexer, law.invention, Interferometry, Optics, Pathfinder, law, Electromagnetic shielding, Measuring instrument, Astronomical interferometer, business
Abstract: Submillimeter common user bolometer array (SCUBA)-2 is a wide field sub-mm bolometer camera designed to replace the existing SCUBA instrument on the JCMT in Hawaii. It will be many hundreds of times faster in large area mapping than SCUBA and will also go deeper in a single frame. It will enable the many discoveries of SCUBA to be followed up with deep systematic surveys and help act as a pathfinder for the ALMA interferometer. The key technologies for making the arrays have been demonstrated and will be put together to fabricate the first prototype later this year (2003). The wide field nature of the SCUBA-2 bolometer camera, combined with the diffraction limit at sub-mm wavelengths, leads to physically large focal planes where the issues of stray light control, magnetic shielding, and electrical, thermal and mechanical connection must be carefully addressed in order to realise a successful instrument. We describe the solutions we have adopted for these problem areas.
Published: 2004
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14. Hopping Conduction in NTD Germanium: Comparison Between Measurement and Theory

Author: Adam Woodcraft, R. V. Sudiwala, E. Wakui, and C. Paine
Subjects: Physics, Work (thermodynamics), Condensed matter physics, business.industry, Thermistor, chemistry.chemical_element, Germanium, Condensed Matter Physics, Thermal conduction, Variable-range hopping, Atomic and Molecular Physics, and Optics, Optics, chemistry, Electrical resistivity and conductivity, Calibration, General Materials Science, Neutron, business
Abstract: We present precise measurements of the resistance-temperature variation of several samples of neutron transmutation doped (NTD) germanium, at temperatures from 70 mK to 1 K. This material is widely used for sensitive thermometry, often as the thermistor element in bolometers and microcalorimeters. It is also used in investigations of the low temperature conductivity of highly doped semiconductors. The resistance, R, is expected to follow the variable range hopping equation R(T)=R 0 exp(T 0/T) p , where T is temperature and R 0 and T 0 are material parameters. A value of p=0.5 is predicted theoretically, and generally seems to be in good agreement with experimental measurements. However, some theories and numerical calculations predict different values of p. Knowledge of the correct resistance-temperature relationship is important for the accurate calibration of thermometers, and also delivers insight into the basic physics involved. Most experimental measurements on germanium have not had sufficient precision to distinguish between the different predicted values of p. We show that such measurements are nevertheless possible. Our results are all in excellent agreement with the expected variable range hopping behaviour. However, the values of p appear to vary with doping density, in disagreement with most theories. We have considered and rejected both random and systematic errors as an explanation for the observed behaviour, and have confirmed the results by making measurements in two different systems with independent readout systems and temperature calibrations. The situation is complicated by the possibility of temperature dependence of R 0. The expected form is R 0(T)∝T q; however, there is considerable disagreement over the predicted value of q. We show that in general it is not possible to determine both p and q from resistance measurements. However, our results can only be explained if either or both of q and p vary from sample to sample. Such behaviour is not generally expected. We show that neglecting the q term can lead to serious errors when calibrating thermometers. However, the degeneracy between p and q means that for a calibration the q term can be neglected, and good fits obtained if p is allowed to vary. Our results suggest that further theoretical work is required in this area, backed up by more comprehensive measurements.
Published: 2004
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15. [Untitled]

Author: A. D. Turner, Adam Woodcraft, Fred Gannaway, P. A. R. Ade, E. Wakui, J. J. Bock, Matthew Joseph Griffin, Carole Tucker, S. Sethuraman, R. V. Sudiwala, Jeffrey W. Beeman, Bruno Maffei, and C. V. Haynes
Subjects: Physics, Radiation, business.industry, Thermistor, Cosmic microwave background, Detector, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Biasing, Astrophysics::Cosmology and Extragalactic Astrophysics, Condensed Matter Physics, law.invention, Optics, Semiconductor, law, Electrical and Electronic Engineering, Adiabatic process, business, Instrumentation
Abstract: We describe techniques for testing and characterising semiconductor bolometers, using the bolometer model presented in Sudiwala et. al. [1]. The procedures are illustrated with results from a prototype bolometer for the high frequency instrument (HFI) in the Planck Surveyor cosmic microwave background mission. This is a bolometer using spider-web geometry and a neutron transmutation doped (NTD) germanium thermistor, designed for operation at 100 mK. Details are given of the laboratory facility used to take data at temperatures from 70 mK to 350 mK. This employs an adiabatic demagnetisation refrigerator to cool the detector and optics. The spatial and spectral properties of the optical system are controlled using feedhorns and edge filters. To characterise the bolometer, blanked and optically loaded load curves were measured over a range of temperatures, and the response to modulated radiation was measured as a function of modulation frequency, temperature and bias current. Results for the prototype bolometer show that its behaviour is well represented by an ideal thermal detector down to a temperature of approximately 100 mK. Below this, non-thermal effects such as electron-phonon decoupling or electric field dependent resistance appear to lead to departure from ideal behaviour. The performance was in good agreement with the design goals for the bolometer.
Published: 2002
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16. [Untitled]

Author: Adam Woodcraft, Matthew Joseph Griffin, and Rashmikant V. Sudiwala
Subjects: Physics, Radiation, Observational error, business.industry, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Radiant energy, Astrophysics::Cosmology and Extragalactic Astrophysics, Condensed Matter Physics, law.invention, Optics, Semiconductor, law, Thermal, Range (statistics), Classical electromagnetism, Electrical and Electronic Engineering, business, Degeneracy (mathematics), Instrumentation
Abstract: A revised version of the Griffin & Holland ideal semiconductor bolometer model is presented and its use in determining bolometer properties and parameters from experimental load curve measurements is discussed. We show that degeneracy between some bolometer parameters can only be broken by model fitting a family of load curves over a range of bath temperatures, and that measurements with the bolometer blanked (zero absorbed radiant power) are essential for unambiguous determination of the main parameters. The influence of measurement errors on parameter recovery is analysed using synthetic noisy data sets.
Published: 2002
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17. Evanescent holes for power monitoring of a Pulsed Cloud Radar

Author: Alexander Geise, Adam Woodcraft, John Howes, Nobuhiro Takahashi, Richard Wylde, Richard Thompson Hans-Joachim Schoedel, Hiroaki Horie, Kevin J. Pike, and Hirotaka Nakatsuka
Subjects: Physics, Electromagnetics, business.industry, Pulse-Doppler radar, Curved mirror, law.invention, Continuous-wave radar, Optics, Radar engineering details, law, Radar imaging, Radar, business, Beam (structure)
Abstract: Evanescent holes in a curved mirror will be used to provide an ultra-stable high-loss path to monitor the power in a 94 GHz transmitted beam for the Pulsed Cloud Radar on the EarthCARE satellite. Here we present details of the calculations to determine the hole size necessary and preliminary measurements on a functional model.
Published: 2014
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18. The thermal conductivity of C17510 beryllium–copper alloy below 1 K

Author: Adam Woodcraft, R. V. Sudiwala, and R. S. Bhatia
Subjects: Materials science, Alloy, General Physics and Astronomy, chemistry.chemical_element, Beryllium copper, Conductivity, engineering.material, Thermal conduction, Thermal conductivity, chemistry, Electrical resistivity and conductivity, Beryllium-Copper Alloy, engineering, General Materials Science, Beryllium, Composite material
Abstract: We have measured the low temperature thermal conductivity of the beryllium–copper alloy C17510 TF00. This is a high conductivity (low beryllium content) alloy. Measurements were made at temperatures between 100 mK and 1 K. A conductivity of 2.39 (T/1 K ) 0.99 W m −1 K −1 was found. The linear variation with temperature and good agreement with the prediction from the electrical resistivity at 4.2 K suggest that thermal conduction is predominately electronic. The conductivity is considerably higher than for high strength (2% beryllium) beryllium–copper alloys. This is therefore a useful material when high strength and thermal conductivity are both required. The accuracy of the measurements was checked by measuring the thermal conductivity of aluminium 6061-T6 above the superconducting transition temperature; good agreement was seen with data in the literature.
Published: 2001
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19. Thermal conductivity of ME771 glass–epoxy laminate from millikelvin temperatures to 4K

Author: Adam Woodcraft, V. Martelli, and G. Ventura
Subjects: Materials science, Thermal conductivity, Ultimate tensile strength, Glass epoxy, medicine, General Physics and Astronomy, General Materials Science, Cryogenics, Composite material, medicine.symptom, Cryogenic temperature, Confusion
Abstract: Permaglas ME771 is a glass–epoxy laminate which is suitable for use at cryogenic temperatures. We have measured the thermal conductivity of a sample of this material between 64 mK and 4.2 K in the direction parallel to the reinforcing fibres, enabling us to make a comparison with the better known material G-10CR. The thermal conductivity follows the form that would be expected for such a material, and is similar to that of G-10CR, which has a similar (room temperature) tensile strength. We comment on some confusion that has arisen over the difference between G-10CR, a material specifically produced for cryogenic use, and G-10, the more common equivalent.
Published: 2010
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20. Modeling of Planck-high frequency instrument bolometers using non-linear effects in the thermometers

Author: Adam Woodcraft, J. P. Torre, E. Bréelle, M. Piat, Alain Coulais, Warren Holmes, R. V. Sudiwala, APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Service d'aéronomie (SA), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), PLANCK, PLANCK-HFI, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS-PSL), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), and Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES)
Subjects: Nuclear and High Energy Physics, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Electrical field effect, Cosmic microwave background, Spider web bolometer, Field effect, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, law.invention, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 010309 optics, symbols.namesake, Optics, law, Planck HFI, 0103 physical sciences, Electron-phonon decoupling effect, Planck, 010306 general physics, Instrumentation, [PHYS.PHYS.PHYS-AO-PH]Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph], Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], business.industry, Bolometer, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Decoupling (cosmology), Non-linear effects, 95.55.Jz, Thermometer, symbols, Electron–phonon decoupling effect, business
Abstract: Proceedings of the 11th International Workshop on Low Temperature Detectors - LTD-11; International audience; The Planck satellite, which is planned to be launched in 2007, is dedicated to surveying the Cosmic Microwave Background (CMB) to a high precision. Aboard this mission, the High-Frequency Instrument (HFI) will use 52 NTD Ge spiderweb bolometers made by Caltech-JPL and cooled to 100 mK by a dilution cooler. In this paper, we present a model of these detectors that includes non-linear effects seen in NTD Ge thermometers: electron-phonon decoupling and electrical field effect. We show that this model leads to consider only electrical field effect. Furthermore, the optical characterization of the HFI bolometers clearly shows a non-ideal behavior that is explained by non-linear effects in the thermometer. We finally show that these effects have to be taken into account for optimized CMB observations and to fully understand the physics of semi-conducting bolometers.
Published: 2006
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21. Fabrication of prototype imaging arrays for SCUBA-2

Author: Anthony J. Walton, Barry L. Zink, J.T.M. Stevenson, Adam Woodcraft, J.P. Sienicki, William B. Doriese, William Parkes, J. A. Beall, Kent D. Irwin, Wayne S. Holland, Y. Xu, M. J. MacIntosh, Eric F Schulte, Joel N. Ullom, L. Ferreira, E. Corrales, Gene C. Hilton, William Duncan, Carl D. Reintsema, Michael D. Audley, Alan M. Gundlach, Andrew Bunting, Leila R. Vale, Dan Bintley, Mark Halpern, Camelia Dunare, R. V. Sudiwala, and Peter A. R. Ade
Subjects: Physics, Nuclear and High Energy Physics, Fabrication, Physics::Instrumentation and Detectors, Terahertz radiation, business.industry, Detector, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Multiplexer, Computer Science::Other, law.invention, SQUID, Optics, law, Wafer, Transition edge sensor, business, Instrumentation
Abstract: Prototype imaging subarrays for SCUBA-2 (the Submillimeter Common-User Bolometer Array) have been fabricated and tested. The pixel count (1280) of these wafer-scale imagers is significantly larger than any other low-temperature detectors produced to date, and represents a major step forward for the low-temperature detector community. These transition-edge-sensor (TES) based imagers utilize several innovations including in-focal-plane superconducting quantum intereference device (SQUID) multiplexers, micromachined Si block absorbers, and superconducting wafer hybridization. In this paper, we review the fabrication processes developed for these imagers and present recent optical data from a prototype imaging subarray.
Published: 2006
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22. Scuba-2: The 10 000 pixel bolometer camera on the james clerk maxwell telescope

Author: David Atkinson, Ian Smail, Douglas Scott, David Lunney, Jessica Dempsey, Gene C. Hilton, R. V. Sudiwala, Tim Jenness, Michel Fich, Mandana Amiri, Simon C. Craig, Andy Gibb, B. Sibthorpe, Mark Halpern, E. I. Robson, E. L. Chapin, Gary R. Davis, Anthony J. Walton, Peter A. R. Ade, H. McGregor, Jan Kycia, David Montgomery, M. J. MacIntosh, Carl D. Reintsema, Harriet Parsons, Antonio Chrysostomou, Frossie Economou, Adam Woodcraft, David S. Berry, Per Friberg, William Parkes, Matthew I. Hollister, Remo P. J. Tilanus, Eli Atad-Ettedgui, Craig Walther, Xiaofeng Gao, H. Thomas, Joel N. Ullom, I. M. Coulson, William B. Doriese, B. Burger, Kent D. Irwin, Wayne S. Holland, William Duncan, Timothy C. Chuter, Michael D. Niemack, D. Bintley, Camelia Dunare, and B. D. Kelly
Subjects: Physics - Instrumentation and Detectors, media_common.quotation_subject, Astronomy, FOS: Physical sciences, Spica, law.invention, Telescope, Data acquisition, submillimetre, law, Planet, Submillimetre, Instrumentation and Methods for Astrophysics (astro-ph.IM), James Clerk Maxwell Telescope, media_common, Physics, instrumentation, detectors [instrumentation], Pixel, general [submillimetre], Bolometer, Detectors, Astronomy and Astrophysics, Instrumentation and Detectors (physics.ins-det), Sky, Space and Planetary Science, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: SCUBA-2 is an innovative 10000 pixel bolometer camera operating at submillimetre wavelengths on the James Clerk Maxwell Telescope (JCMT). The camera has the capability to carry out wide-field surveys to unprecedented depths, addressing key questions relating to the origins of galaxies, stars and planets. With two imaging arrays working simultaneously in the atmospheric windows at 450 and 850 microns, the vast increase in pixel count means that SCUBA-2 maps the sky 100-150 times faster than the previous SCUBA instrument. In this paper we present an overview of the instrument, discuss the physical characteristics of the superconducting detector arrays, outline the observing modes and data acquisition, and present the early performance figures on the telescope. We also showcase the capabilities of the instrument via some early examples of the science SCUBA-2 has already undertaken. In February 2012, SCUBA-2 began a series of unique legacy surveys for the JCMT community. These surveys will take 2.5 years and the results are already providing complementary data to the shorter wavelength, shallower, larger-area surveys from Herschel. The SCUBA-2 surveys will also provide a wealth of information for further study with new facilities such as ALMA, and future telescopes such as CCAT and SPICA., 23 pages, 20 figures, 3 tables. Accepted by MNRAS
Published: 2013
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23. Scaling the summit of the submillimetre: instrument performance of SCUBA-2

Author: Adam Woodcraft, William Parkes, Gene C. Hilton, Michael D. Niemack, Michael J. MacIntosh, Matthew Hasselfield, Dan Bintley, John Kuroda, Xiaofeng Gao, Camelia Dunare, Mandana Amiri, Kent D. Irwin, Wayne S. Holland, Mark Halpern, Craig Walther, B. Burger, H. Thomas, Peter A. R. Ade, R. V. Sudiwala, V. Asboth, Edward L. Chapin, Jessica Dempsey, Anthony J. Walton, Erik G. Starman, and Per Friberg
Subjects: Physics, Pixel, business.industry, media_common.quotation_subject, Bolometer, Cryogenics, Submillimetre astronomy, law.invention, Cardinal point, Optics, Sky, law, Transition edge sensor, business, James Clerk Maxwell Telescope, Remote sensing, media_common
Abstract: SCUBA-2 is a revolutionary 10,000 pixel wide-field submillimetre camera, recently commissioned and now operational at the James Clerk Maxwell Telescope (JCMT). Twin focal planes each consist of four 32 by 40 sub-arrays of superconducting Transition Edge Sensor (TES) bolometers, the largest combined low temperature bolometer arrays in operation, to provide simultaneous imaging at wavelengths of 450 and 850 microns. SCUBA-2 was designed to map large areas of sky more than 100 times faster than the original ground breaking SCUBA instrument and has achieved this goal. In this paper we describe the performance of the instrument and present results of characterising the eight science grade TES bolometer arrays. We discuss the steps taken to optimise the setup of the TES arrays to maximise mapping speed and show how critical changes to the sub-array module thermal design, the introduction of independent focal plane and 1K temperature control and enhancements to the cryogenics have combined to significantly improve the overall performance of the instrument.
Published: 2012
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24. Scientific objectives of Einstein Telescope

Author: V. Fafone, C. Kant Mishra, M. Doets, A. Cumming, M. Lorenzini, Tjonnie G. F. Li, B. Lagrange, M. R. Abernathy, J. H. Hough, Roman Schnabel, Michael Britzger, F. Brueckner, J. F. J. van den Brand, Martin Hendry, Adam Woodcraft, K. V. Tokmakov, Valeria Ferrari, J. Franc, Graham Woan, F. Richard, N. Beveridge, Bernard F. Schutz, A. Morgia, M. van Veggel, G. D. Hammond, C. Graef, Sascha Husa, Alberto Vecchio, S. Chelkowski, Ian Hawke, E. Chassande-Mottin, Kostas Glampedakis, Frédérique Marion, Rosa Poggiani, N. Lastzka, Sheila Rowan, Lucía Santamaría, R. O'. Shaughnessy, Paul Fulda, P. Weßels, B. Mours, Moritz Mehmet, D. J. A. McKechan, A. Colla, Henning Vahlbruch, Alicia M. Sintes, Benno Willke, Badri Krishnan, Hartmut Grote, Ronny Nawrodt, F. Y. Khalili, G. Losurdo, Mauro Tonelli, Loriano Storchi, C. Palomba, E. Genin, S. Van Der Putten, Fumiko Kawazoe, Christian D. Ott, K. Haughian, Tania Regimbau, H. Rehbein, S. P. Vyatchanin, S. L. Danilishin, Ilya Mandel, Ettore Majorana, Ik Siong Heng, Stefanie Kroker, C. Robinson, Paolo Falferi, M. Galimberti, D. Passuello, Y. Minenkov, M. Barsuglia, Benjamin William Allen, Karsten Danzmann, John Nelson, Riccardo Bassiri, S. Braccini, S. Reid, Bangalore Suryanarayana Sathyaprakash, G. M. Guidi, R. Vaccarone, Giancarlo Cella, Carlos F. Sopuerta, L. Moscatelli, C. Van Den Broeck, Mark Beker, V. Re, H. J. Bulten, P. G. Murray, A. Gennai, A. Pasqualetti, L. Naticchioni, G. Parguez, Kostas D. Kokkotas, Jonathan R. Gair, Jan Harms, Leor Barack, Pau Amaro-Seoane, C. N. Colacino, E. Chalkley, Kazuaki Kuroda, J. Dueck, L. Di Fiore, E. J. Daw, M. Punturo, E. Hennes, Daniel Friedrich, P. J. Sutton, R. Passaquieti, E. Coccia, M. A. Bizouard, Federico Ferrini, A. Viceré, A. Giazotto, Aiko Samblowski, B. Kley, Christine Michel, P. Ajith, Benjamin Taylor, G. A. Prodi, R. Flaminio, A. Rocchi, P. Astone, F. Vetrano, M. Di Paolo Emilio, F. Piergiovanni, Angela Delli Paoli, Rajesh Kumar, Massimo Bassan, P. Puppo, Craig A. Bond, L. Cunningham, J. M. Hallam, S. Márka, Kenneth A. Strain, C. Schwarz, F. Fidecaro, Nils Andersson, K. G. Arun, H. Lück, A. Thürin, B. Sorazu, Paul Campsie, Wolfango Plastino, Andrea Chincarini, John K. Scott, I. W. Martin, D. Heinert, F. Ricci, W. Del Pozzo, E. Cuoco, Vuk Mandic, M. V. Plissi, L. Bosi, S. E. Strigin, H. Tournefier, A. Corsi, Patricia Schmidt, Fiona C. Speirits, Benoit Sassolas, R. De Salvo, S. Mosca, John Veitch, Francesco Marin, S. H. Huttner, P. Popolizio, Laurent Pinard, Helge Müller-Ebhardt, Stefan Hild, Suvadeep Bose, R. Gouaty, Sofiane Aoudia, Enrico Calloni, G. T. Jones, P. Rapagnani, Andreas Freise, Kazuhiro Yamamoto, James S. Clark, Mirko Prato, J. Colas, M. Edwards, Matthew Pitkin, W. Graham, F. Frasconi, D. Mc. Leod, M. Granata, D. S. Rabeling, I. Kamaretsos, István Rácz, Jocelyn Read, R. Schilling, Rocco Romano, M. Perciballi, A. Di. Cintio, Marc Favata, J. Marque, L. Carbone, Tomasz Bulik, W. Winkler, V. Malvezzi, N. Morgado, Fabrizio Barone, T. Dent, R. De Rosa, Fausto Acernese, Kentaro Somiya, C. Bradaschia, D. I. Jones, Stephen Fairhurst, Edward K. Porter, B. Barr, Bala R. Iyer, A. Rüdiger, Oliver Burmeister, Gianluca Gemme, S. P. Tarabrin, Paul Seidel, Keiko Kokeyama, D. Huet, A. Dietz, Mark Hannam, S. Gossan, A. Di Virgilio, Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), (Astro)-Particles Physics, Mathematical Analysis, Sathyaprakash, B, Abernathy, M, Acernese, F, Ajith, P, Allen, B, Amaro Seoane, P, Andersson, N, Aoudia, S, Arun, K, Astone, P, Krishnan, B, Barack, L, Barone, F, Barr, B, Barsuglia, M, Bassan, M, Bassiri, R, Beker, M, Beveridge, N, Bizouard, M, Bond, C, Bose, S, Bosi, L, Braccini, S, Bradaschia, C, Britzger, M, Brueckner, F, Bulik, T, Bulten, Hj, Burmeister, O, Calloni, E, Campsie, P, Carbone, L, Cella, G, Chalkley, E, Chassande Mottin, E, Chelkowski, S, Chincarini, A, Cintio, Ad, Clark, J, Coccia, E, Colacino, Cn, Colas, J, Colla, A, Corsi, A, Cumming, A, Cunningham, L, Cuoco, E, Danilishin, S, Danzmann, K, Daw, E, De Salvo, R, Pozzo, Wd, Dent, T, De Rosa, R, Fiore, Ld, Emilio, Mdp, Virgilio, Ad, Dietz, A, Doets, M, Dueck, J, Edwards, M, Fafone, V, Fairhurst, S, Falferi, P, Favata, M, Ferrari, V, Ferrini, F, Fidecaro, F, Flaminio, R, Franc, J, Frasconi, F, Freise, A, Friedrich, D, Fulda, P, Gair, J, Galimberti, M, Gemme, G, Genin, E, Gennai, A, Giazotto, A, Glampedakis, K, Gossan, S, Gouaty, R, Graef, C, Graham, W, Granata, M, Grote, H, Guidi, G, Hallam, J, Hammond, G, Hannam, M, Harms, J, Haughian, K, Hawke, I, Heinert, D, Hendry, M, Heng, I, Hennes, E, Hild, S, Hough, J, Huet, D, Husa, S, Huttner, S, Iyer, B, Jones, Di, Jones, G, Kamaretsos, I, Mishra, Ck, Kawazoe, F, Khalili, F, Kley, B, Kokeyama, K, Kokkotas, K, Kroker, S, Kumar, R, Kuroda, K, Lagrange, B, Lastzka, N, Li, Tgf, Lorenzini, M, Losurdo, G, Lück, H, Majorana, E, Malvezzi, V, Mandel, I, Mandic, V, Marka, S, Marin, F, Marion, F, Marque, J, Martin, I, Leod, Dm, Mckechan, D, Mehmet, M, Michel, C, Minenkov, Y, Morgado, N, Morgia, A, Mosca, S, Moscatelli, L, Mours, B, Müller Ebhardt, H, Murray, P, Naticchioni, L, Nawrodt, R, Nelson, J, Shaughnessy, Ro, Ott, Cd, Palomba, C, Paoli, A, Parguez, G, Pasqualetti, A, Passaquieti, R, Passuello, D, Perciballi, M, Piergiovanni, F, Pinard, L, Pitkin, M, Plastino, Wolfango, Plissi, M, Poggiani, R, Popolizio, P, Porter, E, Prato, M, Prodi, G, Punturo, M, Puppo, P, Rabeling, D, Racz, I, Rapagnani, P, Re, V, Read, J, Regimbau, T, Rehbein, H, Reid, S, Ricci, F, Richard, F, Robinson, C, Rocchi, A, Romano, R, Rowan, S, Rüdiger, A, Samblowski, A, Santamaría, L, Sassolas, B, Schilling, R, Schmidt, P, Schnabel, R, Schutz, B, Schwarz, C, Scott, J, Seidel, P, Sintes, Am, Somiya, K, Sopuerta, Cf, Sorazu, B, Speirits, F, Storchi, L, Strain, K, Strigin, S, Sutton, P, Tarabrin, S, Taylor, B, Thürin, A, Tokmakov, K, Tonelli, M, Tournefier, H, Vaccarone, R, Vahlbruch, H, Van Den Brand, Jfj, Van Den Broeck, C, Van Der Putten, S, Van Veggel, M, Vecchio, A, Veitch, J, Vetrano, F, Vicere, A, Vyatchanin, S, Weels, P, Willke, B, Winkler, W, Woan, G, Woodcraft, A, Yamamoto, K., B., Sathyaprakash, M., Abernathy, F., Acernese, P., Ajith, B., Allen, P., Amaro Seoane, N., Andersson, S., Aoudia, K., Arun, P., Astone, B., Krishnan, L., Barack, F., Barone, B., Barr, M., Barsuglia, M., Bassan, R., Bassiri, M., Beker, N., Beveridge, M., Bizouard, C., Bond, S., Bose, L., Bosi, S., Braccini, C., Bradaschia, M., Britzger, F., Brueckner, T., Bulik, H. J., Bulten, O., Burmeister, Calloni, Enrico, P., Campsie, L., Carbone, G., Cella, E., Chalkley, E., Chassande Mottin, S., Chelkowski, A., Chincarini, A., Di Cintio, J., Clark, E., Coccia, C. N., Colacino, J., Cola, A., Colla, A., Corsi, A., Cumming, L., Cunningham, E., Cuoco, S., Danilishin, K., Danzmann, E., Daw, R., De Salvo, W., Del Pozzo, T., Dent, DE ROSA, Rosario, L., Di Fiore, M., Di Paolo Emilio, A., Di Virgilio, A., Dietz, M., Doet, J., Dueck, M., Edward, V., Fafone, S., Fairhurst, P., Falferi, M., Favata, V., Ferrari, F., Ferrini, F., Fidecaro, R., Flaminio, J., Franc, F., Frasconi, A., Freise, D., Friedrich, P., Fulda, J., Gair, M., Galimberti, G., Gemme, E., Genin, A., Gennai, A., Giazotto, K., Glampedaki, S., Gossan, R., Gouaty, C., Graef, W., Graham, M., Granata, H., Grote, G., Guidi, J., Hallam, G., Hammond, M., Hannam, J., Harm, K., Haughian, I., Hawke, D., Heinert, M., Hendry, I., Heng, E., Henne, S., Hild, J., Hough, D., Huet, S., Husa, S., Huttner, B., Iyer, D. I., Jone, G., Jone, I., Kamaretso, C., Kant Mishra, F., Kawazoe, F., Khalili, B., Kley, K., Kokeyama, K., Kokkota, S., Kroker, R., Kumar, K., Kuroda, B., Lagrange, N., Lastzka, T. G. F., Li, M., Lorenzini, G., Losurdo, H., Lück, E., Majorana, V., Malvezzi, I., Mandel, V., Mandic, S., Marka, F., Marin, F., Marion, J., Marque, I., Martin, D., Mc Leod, D., Mckechan, M., Mehmet, C., Michel, Y., Minenkov, N., Morgado, A., Morgia, S., Mosca, L., Moscatelli, B., Mour, H., Müller Ebhardt, P., Murray, L., Naticchioni, R., Nawrodt, J., Nelson, R., O’ Shaughnessy, C. D., Ott, C., Palomba, A., Paoli, G., Parguez, A., Pasqualetti, R., Passaquieti, D., Passuello, M., Perciballi, F., Piergiovanni, L., Pinard, M., Pitkin, W., Plastino, M., Plissi, R., Poggiani, P., Popolizio, E., Porter, M., Prato, G., Prodi, M., Punturo, P., Puppo, D., Rabeling, I., Racz, P., Rapagnani, V., Re, J., Read, T., Regimbau, H., Rehbein, S., Reid, F., Ricci, F., Richard, C., Robinson, A., Rocchi, R., Romano, S., Rowan, A., Rüdiger, A., Samblowski, L., Santamaría, B., Sassola, R., Schilling, P., Schmidt, R., Schnabel, B., Schutz, C., Schwarz, J., Scott, P., Seidel, A. M., Sinte, K., Somiya, C. F., Sopuerta, B., Sorazu, F., Speirit, L., Storchi, K., Strain, S., Strigin, P., Sutton, S., Tarabrin, B., Taylor, A., Thürin, K., Tokmakov, M., Tonelli, H., Tournefier, R., Vaccarone, H., Vahlbruch, J. F. J., van den Brand, C., Van Den Broeck, S., van der Putten, M., van Veggel, A., Vecchio, J., Veitch, F., Vetrano, A., Vicere, S., Vyatchanin, P., Weßel, B., Willke, W., Winkler, G., Woan, A., Woodcraft, K., Yamamoto, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire des matériaux avancés (LMA), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), APC - Cosmologie, Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), APC - Gravitation (APC-Gravitation), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), and Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Physics and Astronomy (miscellaneous), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Physics::Instrumentation and Detectors, Interferometers, Gravitational waves detectors and experiments, Observatories and site testing, GRAVITATIONAL-WAVE OBSERVATIONS, FOS: Physical sciences, GAMMA-RAY BURSTS, BLACK-HOLE, PHYSICS, INTERMEDIATE, BINARIES, TAILS, General Relativity and Quantum Cosmology (gr-qc), onde gravitazionali, Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, Cosmology, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Observational astronomy, Settore FIS/05 - Astronomia e Astrofisica, antenne gravitazionali iterferometriche, gravitazione, 0103 physical sciences, 010306 general physics, ComputingMilieux_MISCELLANEOUS, [PHYS]Physics [physics], Physics, Detection of gravitational waves, Einstein Telescope, 010308 nuclear & particles physics, Detector, Settore FIS/01 - Fisica Sperimentale, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Cosmology and Extragalactic Astrophysics, BINARY, Interferometry, Fundamental physics, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The advanced interferometer network will herald a new era in observational astronomy. There is a very strong science case to go beyond the advanced detector network and build detectors that operate in a frequency range from 1 Hz-10 kHz, with sensitivity a factor ten better in amplitude. Such detectors will be able to probe a range of topics in nuclear physics, astronomy, cosmology and fundamental physics, providing insights into many unsolved problems in these areas., 18 pages, 4 figures, Plenary talk given at Amaldi Meeting, July 2011
Published: 2012
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25. Effect of heat treatment on mechanical dissipation in Ta2O5 coatings

Author: S. Penn, Roger K. Route, C. Schwarz, Stuart Reid, A. M. Gretarsson, Sheila Rowan, Ian MacLaren, Adam Woodcraft, Paul Seidel, J. H. Hough, Ronny Nawrodt, Gregory M. Harry, I. W. Martin, Riccardo Bassiri, Martin M. Fejer, E. K. Gustafson, John D. Scott, SUPA School of Physics and Astronomy [Glasgow], University of Glasgow, Institute of Solid State Physics, Friedrich-Schiller-Universität = Friedrich Schiller University Jena [Jena, Germany], Ginzton Laboratory [Stanford], Stanford University, Embry-Riddle Aeronautical University, LIGO Laboratory, California Institute of Technology (CALTECH), Massachusetts Institute of Technology (MIT), Department of Physics, Hobart and William Smith Colleges [Geneva, NY], Institute for Astronomy [Edinburgh] (IfA), University of Edinburgh, UK Astronomy Technology Centre (UK ATC), and Science and Technology Facilities Council (STFC)
Subjects: Physics - Instrumentation and Detectors, Physics and Astronomy (miscellaneous), 61.43.Er, FOS: Physical sciences, Dielectric, General Relativity and Quantum Cosmology (gr-qc), engineering.material, 01 natural sciences, Sensitivity (explosives), General Relativity and Quantum Cosmology, chemistry.chemical_compound, Coating, 0103 physical sciences, Tantalum pentoxide, 68.60.Bs, Composite material, 010306 general physics, Spectroscopy, Physics, 010308 nuclear & particles physics, System of measurement, Instrumentation and Detectors (physics.ins-det), Dissipation, 05.40.Jc, 04.80.Nn, 42.60.Da Scottish Universities Physics Alliance, Interferometry, chemistry, engineering, 95.55.Ym
Abstract: Thermal noise arising from mechanical dissipation in dielectric reflective coatings is expected to critically limit the sensitivity of precision measurement systems such as high-resolution optical spectroscopy, optical frequency standards and future generations of interferometric gravitational wave detectors. We present measurements of the effect of post-deposition heat treatment on the temperature dependence of the mechanical dissipation in ion-beam sputtered tantalum pentoxide between 11\,K and 300\,K. We find the temperature dependence of the dissipation is strongly dependent on the temperature at which the heat treatment was carried out, and we have identified three dissipation peaks occurring at different heat treatment temperatures. At temperatures below 200\,K, the magnitude of the loss was found to increase with higher heat treatment temperatures, indicating that heat treatment is a significant factor in determining the level of coating thermal noise., Comment: accepted Classical and Quantum Gravity 2010
Published: 2010
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26. Planck pre-launch status: The HFI instrument, from specification to actual performance

Author: Peter A. R. Ade, V. Yurchenko, F. Piacentini, R. Pons, M. Nexon, G. Recouvreur, Christopher G. Paine, C. Dumesnil, Philippe Camus, J. Pahn, O. Perdereau, M. Tristram, Sarah E. Church, M.-A. Miville-Deschênes, A. Coulais, J. J. Bock, F.-X. Désert, J. Lande, G. Serra, J. F. Macías-Pérez, F. Pajot, J.-L. Beney, F. Bouchet, Simon Prunet, J.-P. Torre, C. Leroy, N. Ponthieu, Bruno Maffei, E. Bréelle, M. Giard, B. P. Crill, J.-L. Puget, L. Vibert, W. A. Holmes, T. C. Koch, E. Hivon, J. Haissinski, R. V. Sudiwala, B. Mansoux, L. Montier, K. Dassas, C. Renault, C. Evesque, R. S. Bhatia, Alain Benoit, J. Charra, Sophie Henrot-Versille, W. C. Jones, Y. Blanc, P. de Bernardis, A. Arondel, F. Couchot, C. Rosset, Martin Crook, C. Marty, Stéphane Plaszczynski, B. Leriche, Etienne Pointecouteau, D. Rambaud, D. Santos, J.-F. Sygnet, M. Charra, Tom Bradshaw, J.-M. Delouis, I. Ristorcelli, P. Eng, Jan Tauber, Thierry Maciaszek, Karim Benabed, H. Lagardère, D. Yvon, A. Moneti, J. Narbonne, Giorgio Savini, Andrew E. Lange, X. Dupac, Y. Longval, A. Catalano, R. Gispert, P. de Marcillac, P. Lami, George Efstathiou, C. Mercier, Silvia Masi, Jacques Delabrouille, J. A. Murphy, Ken Ganga, J.-Ph. Bernard, M. Piat, Adam Woodcraft, J.-M. Lamarre, G. Guyot, L. Guglielmi, P. Stassi, J.-J. Fourmond, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Hélium : du fondamental aux applications (NEEL - HELFA), Institut Néel (NEEL), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Cryogénie (NEEL - Cryo), APC - Gravitation (APC-Gravitation), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), APC - Cosmologie, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES), Département de Physique des Particules (ex SPP) (DPhP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, PLANCK, École normale supérieure - Paris (ENS Paris), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Hélium : du fondamental aux applications (HELFA), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Cryogénie (Cryo), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPP), École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), HELFA - Hélium : du fondamental aux applications, Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Cryo - Cryogénie, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)
Subjects: cosmic microwave background, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Point source, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Cosmic microwave background, Cosmic background radiation, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Radio spectrum, law.invention, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, techniques: photometric, Optics, law, space vehicles: instruments, submillimeter: general, techniques: polarimetric, 0103 physical sciences, Calibration, Planck, 010303 astronomy & astrophysics, QB, Physics, 010308 nuclear & particles physics, business.industry, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Space and Planetary Science, symbols, business
Abstract: Context. The High Frequency Instrument (HFI) is one of the two focal instruments of the Planck mission. It will observe the whole sky in six bands in the 100 GHz–1 THz range.\ud \ud Aims. The HFI instrument is designed to measure the cosmic microwave background (CMB) with a sensitivity limited only by fundamental sources: the photon noise of the CMB itself and the residuals left after the removal of foregrounds. The two high frequency bands will provide full maps of the submillimetre sky, featuring mainly extended and point source foregrounds. Systematic effects must be kept at negligible levels or accurately monitored so that the signal can be corrected. This paper describes the HFI design and its characteristics deduced from ground tests and calibration.\ud \ud Methods. The HFI instrumental concept and architecture are feasible only by pushing new techniques to their extreme capabilities, mainly: (i) bolometers working at 100 mK and absorbing the radiation in grids; (ii) a dilution cooler providing 100 mK in microgravity conditions; (iii) a new type of AC biased readout electronics and (iv) optical channels using devices inspired from radio and infrared techniques.\ud \ud Results. The Planck-HFI instrument performance exceeds requirements for sensitivity and control of systematic effects. During ground-based calibration and tests, it was measured at instrument and system levels to be close to or better than the goal specification.
Published: 2010
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27. Characterising and calibrating the SCUBA-2 superconducting bolometer arrays for science observing

Author: Xiaofeng Gao, Dennis Kelly, Mandana Amiri, Andy Gibb, Adam Woodcraft, Douglas Scott, Matthew I. Hollister, Tim Jenness, Carl D. Reintsema, E. L. Chapin, H. Thomas, Kent D. Irwin, Wayne S. Holland, Dan Bintley, Gene C. Hilton, Michael J. MacIntosh, David S. Berry, B. Burger, William F. Grainger, Matthew Hasselfield, Mark Halpern, Michael D. Niemack, Peter A. R. Ade, Lorenzo Moncelsi, Jessica T. Dempsey, and Per Friberg
Subjects: Physics, Optics, Pixel, law, business.industry, Terahertz radiation, Bolometer, Calibration, business, Wide field, James Clerk Maxwell Telescope, law.invention, Remote sensing
Abstract: SCUBA-2 is a 10,000 pixel wide field sub-millimeter camera which started science observing on James Clerk Maxwell Telescope (JCMT) in the spring of 2010. We present the results of characterising individual 1280 bolometer science grade sub-arrays, as well as experience from operating the instrument.
Published: 2010
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28. Planck pre-launch status: The optical architecture of the HFI

Author: Rashmikant V. Sudiwala, Adam Woodcraft, I. Ristorcelli, J.-L. Puget, Bruno Maffei, F. Noviello, J.-M. Lamarre, Giorgio Savini, Carole Tucker, Y. Longval, A. Catalano, Emily Gleeson, Sarah E. Church, Peter A. R. Ade, V. Yurchenko, Andrew E. Lange, F.-X. Désert, F. Pajot, W. C. Jones, R. Colgan, J. A. Murphy, APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), École normale supérieure - Paris (ENS Paris), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), and Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)
Subjects: cosmic microwave background, Experimental Physics, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Cosmic microwave background, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, law.invention, 010309 optics, Telescope, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, techniques: photometric, Optics, law, 0103 physical sciences, Planck, space vehicles: instruments, 010303 astronomy & astrophysics, Image resolution, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, QB, Physics, Gregorian telescope, business.industry, instrumentation: detectors, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, instrumentation: polarimeters, Astronomy and Astrophysics, submillimeter: general, Spectral bands, Cardinal point, Space and Planetary Science, symbols, business
Abstract: The Planck High Frequency Instrument, HFI, has been designed to allow a clear unobscured view of the CMB sky through an offaxis Gregorian telescope. The prime science target is to measure the polarized anisotropy of the CMB with a sensitivity of 1 part in 10^6 with a maximum spatial resolution of 5 arcmin (C_l ~ 3000) in four spectral bands with two further high-frequency channels measuring total power for foreground removal. These requirements place critical constraints on both the telescope configuration and the receiver coupling and require precise determination of the spectral and spatial characteristics at the pixel level, whilst maintaining control of the polarisation. To meet with the sensitivity requirements, the focal plane needs to be cooled with the optics at a few Kelvin and detectors at 100 mK. To limit inherent instrumental thermal emission and diffraction effects, there is no vacuum window, so the detector feedhorns view the telescope secondary directly. This requires that the instrument is launched warm with the cooler chain only being activated during its cruise to L2. Here we present the novel optical configuration designed to meet with all the above criteria.
Published: 2010
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29. Characterising the SCUBA-2 superconducting bolometer arrays

Author: Matthew I. Hollister, Dennis Kelly, Kent D. Irwin, Wayne S. Holland, Matthew Hasselfield, Per Friberg, Adam Woodcraft, C. G. A. Mugford, Anthony J. Walton, Carl D. Reintsema, Mandana Amiri, Xiaofeng Gao, Julian Steven House, Jan Kycia, B. Burger, Craig Walther, Lauren Persaud, Mark Halpern, William F. Grainger, Jeff T. Hill, Peter A. R. Ade, Lorenzo Moncelsi, William Parkes, Michael D. Niemack, Gene C. Hilton, Michael J. MacIntosh, Dan Bintley, Camelia Dunare, David Atkinson, Holland, Wayne S., and Zmuidzinas, Jonas
Subjects: Physics, business.industry, Amplifier, Bolometer, Submillimetre astronomy, law.invention, Telescope, SQUID, Optics, law, Dilution refrigerator, Transition edge sensor, business, James Clerk Maxwell Telescope
Abstract: SCUBA-2 is a state of the art 10,000 pixel submillimeter camera installed and being commissioned at the James Clerk Maxwell Telescope (JCMT) providing wide-field simultaneous imaging at wavelengths of 450 and 850 microns. At each wavelength there are four 32 by 40 sub-arrays of superconducting Transition Edge Sensor (TES) bolometers, each packaged with inline SQUID multiplexed readout and amplifier. In this paper we present the results of characterising individual 1280 bolometer science grade sub-arrays, both in a dedicated 50mk dilution refrigerator test facility and in the instrument installed at the JCMT.
Published: 2010

30. Initial highlights of the HOBYS key program, the Herschel imaging survey of OB young stellar objects

Author: Annie Zavagno, Nicola Schneider, Sergio Molinari, Jason M. Kirk, Pierre Didelon, Timea Csengeri, Zoltan Balog, L. D. Anderson, Matthew Joseph Griffin, D. Russeil, Peter Charles Hargrave, S. J. Leeks, Adam Woodcraft, Marc Sauvage, Christine D. Wilson, Alain Abergel, M. Hennemann, Q. Nguyen-Luong, Vincent Minier, Maohai Huang, J.-P. Baluteau, D. Teyssier, Pierrick Martin, Lise Deharveng, Alexander Men'shchikov, P. Persi, Derek Ward-Thompson, H. Roussel, Glenn J. White, Ph. André, Sylvain Bontemps, Leonardo Testi, S. Sadavoy, Pierre Cox, A. M. di Giorgio, Tracey Hill, R. Vavrek, Stefano Pezzuto, Luigi Spinoglio, Frédérique Motte, P. Saraceno, G. Olofsson, A. Marston, H. Aussel, Jin-Zeng Li, B. Sibthorpe, J. Di Francesco, J.-Ph. Bernard, Nicolas Peretto, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Observatoire Astronomique de Marseille Provence (OAMP), Université de Provence - Aix-Marseille 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Herzberg Institute of Astrophysics, National Research Council of Canada (NRC), Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), School of Physics and Astronomy [Cardiff], Cardiff University, STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), AUTRES, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, National Astronomical Observatories [Beijing] (NAOC), Chinese Academy of Sciences [Beijing] (CAS), CITA, University of Toronto, Stockholm University, Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Royal Observatory Edinburgh (ROE), University of Edinburgh, Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), European Southern Observatory (ESO), Herschel Science Center [Madrid], European Space Astronomy Centre (ESAC), European Space Agency (ESA)-European Space Agency (ESA), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), and School of Physics and Astronomy
Subjects: Physics, H II region, stars: formation, stars: protostars, 010308 nuclear & particles physics, Star formation, extinction, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Young stellar object, Astronomy, Astronomy and Astrophysics, telescopes, Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 01 natural sciences, stars: massive, H ii regions, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Protostar, dust, 010303 astronomy & astrophysics, QB
Abstract: International audience; We present the initial highlights of the HOBYS key program, which are based on Herschel images of the Rosette molecular complex and maps of the RCW120 H ii region. Using both SPIRE at 250/350/500 μm and PACS at 70/160 μm or 100/160 μm, the HOBYS survey provides an unbiased and complete census of intermediate- to high-mass young stellar objects, some of which are not detected by Spitzer. Key core properties, such as bolometric luminosity and mass (as derived from spectral energy distributions), are used to constrain their evolutionary stages. We identify a handful of high-mass prestellar cores and show that their lifetimes could be shorter in the Rosette molecular complex than in nearby low-mass star-forming regions. We also quantify the impact of expanding H ii regions on the star formation process acting in both Rosette and RCW 120. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.Figures 4 and 5 are only available in electronic form at http://www.aanda.org
Published: 2010
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31. Small-scale structure in the Rosette molecular cloud revealed by Herschel

Author: Alexander Men'shchikov, Jean-Paul Baluteau, B. Sibthorpe, Peter Charles Hargrave, J. Di Francesco, Nicola Schneider, Matthew Joseph Griffin, Jason M. Kirk, Pierre Didelon, R. Vavrek, Sarah Sadavoy, A. M. di Giorgio, Annie Zavagno, D. Teyssier, Sylvain Bontemps, Peter Timothy Cox, Luigi Spinoglio, Stefano Pezzuto, Jin-Zeng Li, Timea Csengeri, M. Hennemann, Zoltan Balog, Lise Deharveng, Pierrick Martin, P. Persi, P. Saraceno, Glenn J. White, Leonardo Testi, Ph. André, Sarah Leeks, Adam Woodcraft, Marc Sauvage, Sergio Molinari, Christine D. Wilson, Vincent Minier, Maohai Huang, D. Russeil, Frédérique Motte, Derek Ward-Thompson, J.-Ph. Bernard, G. Olofsson, A. Marston, Alain Abergel, Herzberg Institute of Astrophysics, National Research Council of Canada (NRC), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Observatoire Astronomique de Marseille Provence (OAMP), Université de Provence - Aix-Marseille 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), School of Physics and Astronomy [Cardiff], Cardiff University, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, National Astronomical Observatories [Beijing] (NAOC), Chinese Academy of Sciences [Beijing] (CAS), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), CITA, University of Toronto, Stockholm University, Royal Observatory Edinburgh (ROE), University of Edinburgh, Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), European Southern Observatory (ESO), Herschel Science Center [Madrid], European Space Astronomy Centre (ESAC), European Space Agency (ESA)-European Space Agency (ESA), University of Exeter, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), and School of Physics and Astronomy
Subjects: Physics, 010308 nuclear & particles physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Molecular cloud, Young stellar object, Continuum (design consultancy), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Space observatory, Rosette (botany), Spire, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Scale structure, Mass spectrum, 010303 astronomy & astrophysics, QB
Abstract: We present a preliminary analysis of the small-scale structure found in new 70-520 micron continuum maps of the Rosette molecular cloud (RMC), obtained with the SPIRE and PACS instruments of the Herschel Space Observatory. We find 473 clumps within the RMC using a new structure identification algorithm, with sizes up to ~1.0 pc in diameter. A comparison with recent Spitzer maps reveals that 371 clumps are "starless" (without an associated young stellar object), while 102 are "protostellar." Using the respective values of dust temperature, we determine the clumps have masses (M_C) over the range -0.75, 6 pages, to be published in Astronomy & Astrophysics
Published: 2010
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32. In-flight calibration of the Herschel-SPIRE instrument

Author: L. Zhang, Hien Nguyen, A. Rykala, Helene Roussel, Douglas Griffin, S. Ronayette, James J. Bock, A. Conley, Edward Polehampton, Dominique Benielli, Bruce Sibthorpe, George J. Bendo, Dimitra Rigopoulou, H. Triou, Markos Trichas, L. R. Levenson, Arnold A. Schwartz, Bernhard Schulz, Darren Dowell, T. Fulton, Andreas Papageorgiou, B. M. Swinyard, K. J. King, Jean-Paul Baluteau, S. C. Jones, Ivan Valtchanov, P. Imhof, S. Guest, L. Conversi, David L. Shupe, Drew Brisbin, Matthew Joseph Griffin, Peter A. R. Ade, Gibion Makiwa, M. J. Barlow, Michael Pohlen, C. P. Pearson, D. Pouliquen, Locke D. Spencer, C. K. Xu, A. Dowell, Anthony J. Smith, Kate Gudrun Isaak, Roger Wesson, S. D. Sidher, Adrian M. Glauser, Adam Woodcraft, Jason Glenn, Seb Oliver, David A. Naylor, Pasquale Panuzzo, Giorgio Savini, Marc Ferlet, Herve Aussel, Michael Zemcov, Nanyao Y. Lu, T. L. Lim, S. J. Leeks, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Solar System, Fourier transform spectrometers, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Spectral line, law.invention, 010309 optics, Telescope, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, [INFO]Computer Science [cs], space vehicles: instruments, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, instrumentation: spectrographs, Remote sensing, Physics, Data processing, Spectrometer, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Photometer, instrumentation: photometers, Wavelength, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: SPIRE, the Spectral and Photometric Imaging Receiver, is the Herschel Space Observatory'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) covering 194-671 {\mu}m (447-1550 GHz). In this paper we describe the initial approach taken to the absolute calibration of the SPIRE instrument using a combination of the emission from the Herschel telescope itself and the modelled continuum emission from solar system objects and other astronomical targets. We present the photometric, spectroscopic and spatial accuracy that is obtainable in data processed through the "standard" pipelines. The overall photometric accuracy at this stage of the mission is estimated as 15% for the photometer and between 15 and 50% for the spectrometer. However, there remain issues with the photometric accuracy of the spectra of low flux sources in the longest wavelength part of the SPIRE spectrometer band. The spectrometer wavelength accuracy is determined to be better than 1/10th of the line FWHM. The astrometric accuracy in SPIRE maps is found to be 2 arcsec when the latest calibration data are used. The photometric calibration of the SPIRE instrument is currently determined by a combination of uncertainties in the model spectra of the astronomical standards and the data processing methods employed for map and spectrum calibration. Improvements in processing techniques and a better understanding of the instrument performance will lead to the final calibration accuracy of SPIRE being determined only by uncertainties in the models of astronomical standards., Comment: Accepted for publication in Astronomy&Astrophysics, Herschel First Results special issue
Published: 2010
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33. Status of the SPIRE photometer data processing pipelines during the early phases of the Herschel Mission

Author: B. O'Halloran, Marc Ferlet, Louis Levenson, James J. Bock, Adam Woodcraft, Tanya Lim, Seb Oliver, George J. Bendo, Bruce Swinyard, Pierre Chanial, Bruce Sibthorpe, C. Kevin Xu, David L. Shupe, Hien Nguyen, Helene Roussel, David L. Clements, Huw R. Morris, Ken J. King, Michael Pohlen, Lijun Zhang, C. Darren Dowell, Edward Polehampton, Dominique Benielli, Matthew Joseph Griffin, R. Gastaud, Sarah Leeks, S. Guest, Bernhard Schulz, Jason Glenn, Nanyao Lu, Luca Conversi, Sunil Sidher, Ivan Valtchanov, Markos Trichas, Anthony J. Smith, Arnold A. Schwartz, Trevor Fulton, Nicola Schneider, Pasquale Panuzzo, Tim Grundy, Andreas Papageorgiou, Chris Pearson, Dimitra Rigopoulou, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Oschmann, Jacobus M., Clampin, Mark C., and MacEwen, Howard A.
Subjects: Physics, Data processing, business.industry, Point source, Detector, Photometer, 01 natural sciences, law.invention, 010309 optics, Photometry (optics), Telescope, Optics, Cardinal point, law, 0103 physical sciences, [INFO]Computer Science [cs], Ground segment, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Remote sensing
Abstract: We describe the current state of the ground segment of Herschel-SPIRE photometer data processing, approximately one year into the mission. The SPIRE photometer operates in two modes: scan mapping and chopped point source photometry. For each mode, the basic analysis pipeline - which follows in reverse the effects from the incidence of light on the telescope to the storage of samples from the detector electronics - is essentially the same as described pre-launch. However, the calibration parameters and detailed numerical algorithms have advanced due to the availability of commissioning and early science observations, resulting in reliable pipelines which produce accurate and sensitive photometry and maps at 250, 350, and 500 μm with minimal residual artifacts. We discuss some detailed aspects of the pipelines on the topics of: detection of cosmic ray glitches, linearization of detector response, correction for focal plane temperature drift, subtraction of detector baselines (offsets), absolute calibration, and basic map making. Several of these topics are still under study with the promise of future enhancements to the pipelines.
Published: 2010
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34. The Herschel first look at protostars in the Aquila Rift

Author: Matthew Joseph Griffin, Adam Woodcraft, Marc Sauvage, Stefano Pezzuto, Vera Könyves, Bruce Sibthorpe, Frédérique Motte, Vincent Minier, Doris Arzoumanian, Pierre Cox, Peter Charles Hargrave, P. Didelon, Nicolas Peretto, Annie Zavagno, Alexander Men'shchikov, J.-Ph. Bernard, Glenn J. White, Ph. André, Leonardo Testi, Bruno Merín, J. Di Francesco, Göran Olofsson, C. D. Wilson, R. Vavrek, M. Attard, Alain Abergel, Sylvain Bontemps, Maohai Huang, A. M. Di Giorgo, J.-P. Baluteau, Timo Prusti, P. Saraceno, Nicola Schneider, Jason M. Kirk, Anaëlle Maury, Derek Ward-Thompson, Peter Martin, Jin-Zeng Li, Sergio Molinari, Helene Roussel, D. Russeil, L. Spinoglio, L. Cambrésy, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), European Southern Observatory (ESO), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Herzberg Institute of Astrophysics, National Research Council of Canada (NRC), School of Physics and Astronomy [Cardiff], Cardiff University, National Astronomical Observatories [Beijing] (NAOC), Chinese Academy of Sciences [Beijing] (CAS), School of Physics and Astronomy, Photochimie moléculaire et macromoléculaire (PMM), Université Blaise Pascal - Clermont-Ferrand 2 (UBP)-Centre National de la Recherche Scientifique (CNRS), CITA, University of Toronto, Stockholm University, Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Royal Observatory Edinburgh (ROE), University of Edinburgh, Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), University of Exeter, Observatoire Astronomique de Marseille Provence (OAMP), Université de Provence - Aix-Marseille 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Centre National de la Recherche Scientifique (CNRS)-Université Blaise Pascal - Clermont-Ferrand 2 (UBP)-Institut de Chimie du CNRS (INC), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), and Université Blaise Pascal - Clermont-Ferrand 2 (UBP)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, Rift, Serpens, 010308 nuclear & particles physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Global statistics, Spire, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Protostar, 010303 astronomy & astrophysics, Dust emission
Abstract: As part of the science demonstration phase of the Herschel mission of the Gould Belt Key Program, the Aquila Rift molecular complex has been observed. The complete ~ 3.3deg x 3.3deg imaging with SPIRE 250/350/500 micron and PACS 70/160 micron allows a deep investigation of embedded protostellar phases, probing of the dust emission from warm inner regions at 70 and 160 micron to the bulk of the cold envelopes between 250 and 500 micron. We used a systematic detection technique operating simultaneously on all Herschel bands to build a sample of protostars. Spectral energy distributions are derived to measure luminosities and envelope masses, and to place the protostars in an M_env - L_bol evolutionary diagram. The spatial distribution of protostars indicates three star-forming sites in Aquila, with W40/Sh2-64 HII region by far the richest. Most of the detected protostars are newly discovered. For a reduced area around the Serpens South cluster, we could compare the Herschel census of protostars with Spitzer results. The Herschel protostars are younger than in Spitzer with 7 Class 0 YSOs newly revealed by Herschel. For the entire Aquila field, we find a total of ~ 45-60 Class 0 YSOs discovered by Herschel. This confirms the global statistics of several hundred Class~0 YSOs that should be found in the whole Gould Belt survey., Comment: 6 pages, 6 figures, publication in A&A
Published: 2010
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35. Herschel observations of embedded protostellar clusters in the Rosette Molecular Cloud

Author: Peter G. Martin, Alain Abergel, Sylvain Bontemps, J.-Ph. Bernard, S. J. Leeks, Annie Zavagno, Peter Charles Hargrave, Pierre Cox, P. Didelon, J.-P. Baluteau, Martin Hennemann, Glenn J. White, P. Saraceno, Adam Woodcraft, Bruce Sibthorpe, Frédérique Motte, Marc Sauvage, Babar Ali, Ph. André, Alexander Men'shchikov, Derek Ward-Thompson, Q. Nguyen Luong, Leonardo Testi, A. Di Giorgio, Stefano Pezzuto, A. Marston, T. Csengeri, Matthew Joseph Griffin, C. D. Wilson, J. Di Francesco, Zoltan Balog, Sergio Molinari, T. Hill, B. Horeau, Jin-Zeng Li, Maohai Huang, D. Russeil, L. Spinoglio, Nicola Schneider, Jason M. Kirk, Paolo Persi, Göran Olofsson, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Herzberg Institute of Astrophysics, National Research Council of Canada (NRC), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Observatoire Astronomique de Marseille Provence (OAMP), Université de Provence - Aix-Marseille 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, School of Physics and Astronomy [Cardiff], Cardiff University, Département d'Astrophysique (ex SAP) (DAP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, National Astronomical Observatories [Beijing] (NAOC), Chinese Academy of Sciences [Beijing] (CAS), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), CITA, University of Toronto, Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), Stockholm University, Royal Observatory Edinburgh (ROE), University of Edinburgh, Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), European Southern Observatory (ESO), University of Exeter, Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), School of Physics and Astronomy, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), and National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR)
Subjects: Physics, education.field_of_study, 010308 nuclear & particles physics, Infrared, Star formation, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Molecular cloud, Young stellar object, Population, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Luminosity, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Cluster (physics), Protostar, education, 010303 astronomy & astrophysics, QB
Abstract: The Herschel OB young stellar objects survey (HOBYS) has observed the Rosette molecular cloud, providing an unprecedented view of its star formation activity. These new far-infrared data reveal a population of compact young stellar objects whose physical properties we aim to characterise. We compiled a sample of protostars and their spectral energy distributions that covers the near-infrared to submillimetre wavelength range. These were used to constrain key properties in the protostellar evolution, bolometric luminosity, and envelope mass and to build an evolutionary diagram. Several clusters are distinguished including the cloud centre, the embedded clusters in the vicinity of luminous infrared sources, and the interaction region. The analysed protostellar population in Rosette ranges from 0.1 to about 15 Msun with luminosities between 1 and 150 Lsun, which extends the evolutionary diagram from low-mass protostars into the high-mass regime. Some sources lack counterparts at near- to mid-infrared wavelengths, indicating extreme youth. The central cluster and the Phelps & Lada 7 cluster appear less evolved than the remainder of the analysed protostellar population. For the central cluster, we find indications that about 25% of the protostars classified as Class I from near- to mid-infrared data are actually candidate Class 0 objects. As a showcase for protostellar evolution, we analysed four protostars of low- to intermediate-mass in a single dense core, and they represent different evolutionary stages from Class 0 to Class I. Their mid- to far-infrared spectral slopes flatten towards the Class I stage, and the 160 to 70um flux ratio is greatest for the presumed Class 0 source. This shows that the Herschel observations characterise the earliest stages of protostellar evolution in detail., Astronomy & Astrophysics letter, 6 pages, 4 figures, accepted for publication in the Special Issue for Herschel first results
Published: 2010
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36. From filamentary clouds to prestellar cores to the stellar IMF: Initial highlights from the Herschel Gould Belt survey

Author: Alexander Men'shchikov, Pierre Cox, L. Cambrésy, Jin-Zeng Li, Aurora Sicilia-Aguilar, Adam Woodcraft, Marc Sauvage, A. Di Giorgio, Nicola Schneider, Stefano Pezzuto, J. Di Francesco, Jason M. Kirk, Timo Prusti, Alain Abergel, D. Russeil, Helene Roussel, Milena Benedettini, Pierre Royer, Bruce Sibthorpe, C. Waelkens, Th. Henning, J.-P. Baluteau, L. Spinoglio, Vincent Minier, Frédérique Motte, Doris Arzoumanian, Glenn J. White, R. Vavrek, Annie Zavagno, Vera Könyves, Ph. André, Peter Charles Hargrave, Sergio Molinari, M. Attard, Nicolas Peretto, P. Didelon, Sylvain Bontemps, Martin Hennemann, Ralf Launhardt, Oliver Krause, Leonardo Testi, Peter G. Martin, Bruno Merín, J. Le Pennec, J.-Ph. Bernard, Maohai Huang, Herve Aussel, Anaëlle Maury, C. D. Wilson, S. J. Leeks, Matthew Joseph Griffin, Peter A. R. Ade, Derek Ward-Thompson, Paolo Saraceno, Alain Omont, Joris Blommaert, Göran Olofsson, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), School of Physics and Astronomy [Cardiff], Cardiff University, Herzberg Institute of Astrophysics, National Research Council of Canada (NRC), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), European Southern Observatory (ESO), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Laboratoire des Sciences du Climat et de l'Environnement [Gif-sur-Yvette] (LSCE), Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS), LEOSPHERE France, LEOSPHERE, AUTRES, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), National Astronomical Observatories [Beijing] (NAOC), Chinese Academy of Sciences [Beijing] (CAS), School of Physics and Astronomy, CITA, University of Toronto, Stockholm University, Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Royal Observatory Edinburgh (ROE), University of Edinburgh, Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Observatoire Astronomique de Marseille Provence (OAMP), Université de Provence - Aix-Marseille 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), ITA, GBR, FRA, DEU, and BEL
Subjects: Physics, Gravitational instability, Initial mass function, 010308 nuclear & particles physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Molecular cloud, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics - Astrophysics of Galaxies, 01 natural sciences, law.invention, Spire, Polaris, Space and Planetary Science, law, Astrophysics of Galaxies (astro-ph.GA), Core formation, 0103 physical sciences, Protostar, 010303 astronomy & astrophysics, Flare, QB
Abstract: We summarize the first results from the Gould Belt survey, obtained toward the Aquila Rift and Polaris Flare regions during the 'science demonstration phase' of Herschel. Our 70-500 micron images taken in parallel mode with the SPIRE and PACS cameras reveal a wealth of filamentary structure, as well as numerous dense cores embedded in the filaments. Between ~ 350 and 500 prestellar cores and ~ 45-60 Class 0 protostars can be identified in the Aquila field, while ~ unbound starless cores and no protostars are observed in the Polaris field. The prestellar core mass function (CMF) derived for the Aquila region bears a strong resemblance to the stellar initial mass function (IMF), already confirming the close connection between the CMF and the IMF with much better statistics than earlier studies. Comparing and contrasting our Herschel results in Aquila and Polaris, we propose an observationally-driven scenario for core formation according to which complex networks of long, thin filaments form first within molecular clouds, and then the densest filaments fragment into a number of prestellar cores via gravitational instability., 7 pages, 4 figures. Accepted for publication in Astronomy and Astrophysics, Herschel Special Issue
Published: 2010
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37. SPIRE — The state-of-the-art in semiconductor bolometers for astronomy

Author: Bruce Swinyard, Bruce Sibthorpe, Adam Woodcraft, Bernhard Schulz, Matthew Joseph Griffin, James J. Bock, and Hien Nguyen
Subjects: Physics, Terahertz radiation, business.industry, Bolometer, Astronomy, Astrophysics, Submillimetre astronomy, law.invention, Spire, Semiconductor, law, Calibration, State (computer science), Adaptive optics, business
Abstract: SPIRE is one of three instruments on the Herschel Space Observatory. The bolometer arrays it contains are among the best understood and well characterized of any sub-mm astronomy instrument to date, and represent the state-of-the-art for this technology. The results from years of testing on the ground have shown them to be extremely stable and to possess simple behaviour. We describe the results from these tests and show that under the stable conditions expected in flight, this should enable physical models to be used in their calibration, in constrast to previous instruments.
Published: 2009
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38. Cryogenic magnetic shielding for SCUBA-2

Author: Michael J. MacIntosh, Dan Bintley, Wayne S. Holland, Matthew I. Hollister, Adam Woodcraft, and Helen McGregor
Subjects: Physics, Physics::Instrumentation and Detectors, business.industry, Magnetism, Detector, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Magnetic field, law.invention, SQUID, Optics, law, Electromagnetic shielding, Transition edge sensor, business, Astrophysics::Galaxy Astrophysics, James Clerk Maxwell Telescope
Abstract: SCUBA-2 is a new wide-field submillimeter continuum instrument being commissioned on the James Clerk Maxwell Telescope on Mauna Kea in Hawaii. SCUBA-2 uses large-scale arrays of superconducting bolometers with SQUID- (superconducting quantum interference device) based multiplexing and amplification. The sensitivity of the devices that compose the detector arrays to magnetic fields is such that magnetic shielding, consisting of superconducting and high-permeability materials, was fitted to the detector enclosure at 1 K to reduce the magnetic field strength at the focal plane. This paper describes the design and construction of the cryogenic shielding, and presents verification measurements. The shielding performance was found to meet the instrument requirements, and compared well to the modelled results.
Published: 2008
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39. Understanding the Herschel-SPIRE bolometers

Author: Adam Woodcraft, Hien Nguyen, James J. Bock, Bernhard Schulz, Bruce Sibthorpe, Bruce Swinyard, Matthew Joseph Griffin, Duncan, William D., Holland, Wayne S., Withington, Stafford, and Zmuidzinas, Jonas
Subjects: Physics, Pixel, business.industry, Bolometer, Detector, Particle detector, law.invention, Spire, Optics, law, Observatory, Calibration, Satellite, business
Abstract: Bolometers are very simple devices. In principle, the behaviour of a bolometer can be described by a simple model along with a small number of parameters. The SPIRE instrument for the Herschel Space Observatory contains five arrays of NTD germanium spiderweb bolometers containing up to 139 pixels. We show from characterisation measurements on the ground using the flight read-out system that the bolometers follow the ideal model extremely well, are very stable, and that the read-out system is sufficiently well behaved to take advantage of this. Calibration should be greatly simplified by being able to take advantage of this behaviour.
Published: 2008
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40. Performance of the SCUBA-2 dilution refrigerator

Author: Adam Woodcraft, Matthew I. Hollister, Wayne S. Holland, and Dan Bintley
Subjects: Physics, Liquid helium, business.industry, Bolometer, chemistry.chemical_element, Cryogenics, Particle detector, law.invention, Telescope, Optics, chemistry, law, Dilution refrigerator, business, James Clerk Maxwell Telescope, Helium
Abstract: SCUBA-2 is a new wide-field submillimeter continuum instrument being commissioned on the James Clerk Maxwell Telescope on Mauna Kea in Hawaii. SCUBA-2 images simultaneously at 450 and 850 μm using large-scale arrays of superconducting bolometers, with over five thousand pixels at each wavelength. The arrays are cooled to less than 100 mK by the mixing chamber of a dilution refrigerator (DR), with a radiation shield at a nominal temperature of 1 K cooled by the DR still. The DR is a "dry" system, using a pulse tube cooler for precooling of the circulating helium in place of a liquid helium bath. This paper presents key performance data for the DR.
Published: 2008
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41. Herschel-SPIRE: design, ground test results, and predicted performance

Author: Jean-Paul Baluteau, Edward Polehampton, Sunil Sidher, Walter Kieran Gear, Paolo Saraceno, Hien Nguyen, K. J. King, Marc Ferlet, Philippe André, L. Vigroux, Alberto Franceschini, G. J. Bendo, David J. Smith, Peter Charles Hargrave, Glenn Laurent, A. Abreu, Tanya Lim, Adam Woodcraft, Alain Abergel, Jason Glenn, Trevor Fulton, Gillian S. Wright, M. Rowan-Robinson, Locke D. Spencer, Alan Pearce, D. Rizzo, Seb Oliver, Bernhard Schulz, David A. Naylor, Kevin Xu, Nanyao Lu, Darren Dowell, Ivan Valtchanov, Maohai Huang, Bruce Swinyard, Emmanuel Lellouch, Lijun Zhang, Matthew Joseph Griffin, Peter A. R. Ade, Eric Sawyer, Göran Olofsson, Alan Dowell, Douglas Griffin, James J. Bock, Ismael Perez-Fournon, Mat Page, Annie Zavagno, Sarah Leeks, Service d'Astrophysique, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Recherche en épidémiologie et biostatistique, Université Paris-Sud - Paris 11 (UP11)-Institut National de la Santé et de la Recherche Médicale (INSERM), Observatoire Astronomique de Marseille Provence (OAMP), Université de Provence - Aix-Marseille 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Astronomy Centre, University of Sussex, Imperial College London, CEA Cadarache, Ton Duc Thang University [Hô-Chi-Minh-City], University of Pisa - Università di Pisa, NASA Herschel Science Center, Infrared Processing and Analysis Center (IPAC), California Institute of Technology (CALTECH)-California Institute of Technology (CALTECH), Herschel Science Centre, Agence Spatiale Européenne = European Space Agency (ESA), Department of Informatics and Mathematical Modelling [Lyngby] (IMM), Danmarks Tekniske Universitet = Technical University of Denmark (DTU), Oschmann, Jacobus M., Jr. and de Graauw, Mattheus W.~M. and MacEwen, Howard A., Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Mathematics and Statistics, La Trobe University, Agro-Systèmes Territoires Ressources Mirecourt (ASTER Mirecourt), Institut National de la Recherche Agronomique (INRA), NASA-California Institute of Technology (CALTECH), European Space Agency (ESA), and Technical University of Denmark [Lyngby] (DTU)
Subjects: Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Spectrometer, Spacecraft, business.industry, Instrumentation, Field of view, Photometer, 01 natural sciences, law.invention, 010309 optics, Telescope, Spire, Optics, [SDU]Sciences of the Universe [physics], law, 0103 physical sciences, Spectral resolution, business, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Remote sensing
Abstract: International audience; SPIRE, the Spectral and Photometric Imaging Receiver, is a submillimetre camera and spectrometer for Herschel. It comprises a three-band camera operating at 250, 350 and 500 Â\textmum, and an imaging Fourier Transform Spectrometer covering 194-672 \ensuremathμm. The photometer field of view is 4x8 arcmin., viewed simultaneously in the three bands. The FTS has an approximately circular field of view of 2.6 arcmin. diameter and spectral resolution adjustable between 0.04 and 2 cm^-1 ( \ensuremathλ/▵\ensuremathλ=20-1000 at 250 \ensuremathμm). Following successful testing in a dedicated facility designed to simulate the in-flight operational conditions, SPIRE has been integrated in the Herschel spacecraft and is now undergoing system-level testing prior to launch. The main design features of SPIRE are reviewed, the key results of instrument testing are outlined, and a summary of the predicted in-flight performance is given.
Published: 2008
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42. SCUBA-2: A 10000-pixel submillimetre camera for astronomy

Author: Adam Woodcraft
Subjects: Physics, Set (abstract data type), Optics, Pixel, Terahertz radiation, business.industry, Astronomy, business, Multiplexer, Submillimetre astronomy
Abstract: We describe the current status of the SCUBA-2 sub-mm camera for astronomy. We describe the first measurements made while operating an entire sub-array, rather than small subsections as has previously been the case. These results demonstrate that the procedure required to set up the multiplexer for full sub-array operation can be carried out entirely automatically, and that the pixels are sufficiently uniform for the whole sub- array to be usefully operated simultaneously.
Published: 2007
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43. Electrical and optical measurements on the first SCUBA-2 prototype 1280 pixel submillimeter superconducting bolometer array

Author: Cynthia L. Hunt, Peter A. R. Ade, Dan Bintley, M. J. MacIntosh, William Parkes, Camelia Dunare, William Duncan, Carl D. Reintsema, Kent D. Irwin, Eric F Schulte, Wayne S. Holland, Anthony J. Walton, Michael D. Audley, Julian Steven House, Jan Kycia, Mark Halpern, William B. Doriese, Gene C. Hilton, Joel N. Ullom, Rashmikant V. Sudiwala, Maureen A. Ellis, and Adam Woodcraft
Subjects: Physics, Pixel, business.industry, Detector, Bolometer, Multiplexer, Noise (electronics), law.invention, Optics, law, Transition edge sensor, business, Instrumentation, Noise-equivalent power, James Clerk Maxwell Telescope
Abstract: SCUBA-2 is a submillimeter camera being built for the James Clerk Maxwell Telescope in Hawaii. Bringing CCD style imaging to the submillimeter for the first time, with over 10 000 pixels, it will provide a revolutionary improvement in sensitivity and mapping speed. We present results of the first tests on a prototype 1280 pixel SCUBA-2 subarray; the full instrument will be made up of eight such subarrays. The array is made up of transition edge sensor TES detectors, with Mo/Cu bilayers as the sensing element. To keep the number of wires reasonable, a multiplexed readout is used. Unlike previous TES arrays, an in-focal plane multiplexer configuration is used, in which the multiplexing elements are located beneath each pixel. To achieve the required performance, the detectors are operated at a temperature of approximately 120 mK. We describe the results of a basic electrical and optical characterization of the array, demonstrating that it is fully operational. Noise measurements were made on several pixels and gave a noise equivalent power below 2.5 10 17 WH Z 0.5 , within the requirements for SCUBA-2. The construction of the testbed used to carry out these measurements is also described. © 2007 American Institute of Physics. DOI: 10.1063/1.2436839
Published: 2007

44. SCUBA-2: A large-format CCD-style imager for submillimeter astronomy

Author: Cynthia L. Hunt, Dan Bintley, Xiaofeng Gao, Adam Woodcraft, Kent D. Irwin, William Parkes, Wayne S. Holland, Maureen A. Ellis, Peter A. R. Ade, Joel N. Ullom, Ian Walker, Anthony J. Walton, Gene C. Hilton, Carl D. Reintsema, Rashmikant V. Sudiwala, I. Smith, David Atkinson, David A. Naylor, Camelia Dunare, H. McGregor, Gayle F Mitchell, T. Hodson, Fred Gannaway, Ian Robson, Jan Kycia, David Montgomery, Leila R. Vale, Mark Halpern, Pierre Bastien, M. Fich, M. J. MacIntosh, Giampaolo Pisano, Randy Doriese, M. Cliffe, David C. Gostick, Michael D. Audley, William Duncan, and D. Kelly
Subjects: Physics, instrumentation, detector arrays, media_common.quotation_subject, Bolometer, Astronomy, Large format, Astrophysics, Galaxy, Submillimetre astronomy, law.invention, Sky, law, Astronomical interferometer, Galaxy formation and evolution, Transition edge sensor, TES detectors, Millimetre wave astronomy, instrumentation, TES detectors, detector arrays, Millimetre wave astronomy, media_common
Abstract: We describe the capabilities of SCUBA-2, the first CCD-like imager for submillimeter astronomy, and the technologies that make it possible. Unlike previous detectors using discrete bolometers, SCUBA-2 has two dc-coupled, monolithic arrays with a total of ~10,000 bolometers. SCUBA-2’s absorber-coupled pixels use superconducting transition edge sensors operating at ~ 120mK for photon-noise limited performance and a SQUID time-domain multiplexer for readout. It will offer simultaneous imaging of an 8 × 8 arcmin field of view at wavelengths of 850 μm and 450 μm. SCUBA-2 is expected to have a huge impact on the study of galaxy formation and evolution in the early Universe as well as star and planet formation in our own Galaxy. Mapping the sky to the same S/N up to 1000 times faster than SCUBA, SCUBA-2 will also act as a pathfinder for submillimeter interferometers such as ALMA. SCUBA-2 will begin operation on the JCMT in 2006.
Published: 2007

45. Preliminary results from Herschel-SPIRE flight instrument testing

Author: Adam Woodcraft, Sunil Sidher, Bruce Swinyard, Asier A. Aramburu, Jean-Paul Baluteau, Bernhard Schulz, David A. Naylor, Matthew Joseph Griffin, K. J. King, Edward Polehampton, David J. Smith, Marc Ferlet, Trevor Fulton, Douglas Griffin, Tanya Lim, Tim Waskett, Eric Sawyer, Peter Charles Hargrave, I. Valtchanov, Steven Guest, Sarah Leeks, Hien Nguyen, D. Rizzo, Locke D. Spencer, and James J. Bock
Subjects: Scientific instrument, Physics, Spire, Spectrometer, law, Instrumentation, Bolometer, Photometer, Space observatory, Flight instruments, law.invention, Remote sensing
Abstract: The Spectral and Photometric Imaging REceiver (SPIRE) is one of the three scientific instruments to fly on the European Space Agency's Herschel Space Observatory, and contains a three-band imaging submillimetre photometer and an imaging Fourier transform spectrometer. The flight model of the SPIRE cold focal plane unit has been built up in stages with a cold test campaign associated with each stage. The first campaign focusing on the spectrometer took place in early 2005 and the second campaign focusing on the photometer was in Autumn 2005. SPIRE is currently undergoing its third cold test campaign following cryogenic vibration testing. Test results to date show that the instrument is performing very well and in general meets not only its requirements but also most of its performance goals. We present an overview of the instrument tests performed to date, and the preliminary results.
Published: 2006
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46. SCUBA-2: a 10,000 pixel submillimeter camera for the James Clerk Maxwell Telescope

Author: Gene C. Hilton, Camelia Dunare, Dan Bintley, Tim Jenness, Michel Fich, Peter A. R. Ade, Kent D. Irwin, Wayne S. Holland, Carl D. Reintsema, William Duncan, Jan Kycia, Michael J. MacIntosh, Ian Robson, David C. Gostick, David James Montgomery, Andy Gibb, Adam Woodcraft, Eli Atad-Ettedgui, Mark Halpern, Janos Molnar, Ian Walker, Anthony J. Walton, Frossie Economou, Maureen A. Ellis, Dennis Kelly, Tomas Chylek, Simon C. Craig, Douglas Scott, E. L. Chapin, Gary R. Davis, William Parkes, Matthew I. Hollister, and Alasdair Fairley
Subjects: Physics, Pixel, business.industry, Amplifier, Bolometer, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics, Submillimetre astronomy, law.invention, Optics, law, Planet, Dilution refrigerator, business, James Clerk Maxwell Telescope, Data reduction
Abstract: SCUBA-2 is an innovative 10,000 pixel submillimeter camera due to be delivered to the James Clerk Maxwell Telescope in late 2006. The camera is expected to revolutionize submillimeter astronomy in terms of the ability to carry out wide-field surveys to unprecedented depths addressing key questions relating to the origins of galaxies, stars and planets. This paper presents an update on the project with particular emphasis on the laboratory commissioning of the instrument. The assembly and integration will be described as well as the measured thermal performance of the instrument. A summary of the performance results will be presented from the TES bolometer arrays, which come complete with in-focal plane SQUID amplifiers and multiplexed readouts, and are cooled to 100mK by a liquid cryogen-free dilution refrigerator. Considerable emphasis has also been placed on the operating modes of the instrument and the common-user aspect of the user interface and data reduction pipeline. These areas will also be described in the paper., 15 pages; in Proceedings of Millimeter and Submillimeter Detectors and Instrumentation, SPIE, in press
Published: 2006

47. Characterization of a prototype SCUBA-2 1280-pixel submillimetre superconducting bolometer array

Author: Julian Steven House, Jan Kycia, Adam Woodcraft, Gene C. Hilton, Michael J. MacIntosh, Maureen A. Ellis, Mandana Amiri, Cynthia L. Hunt, Dan Bintley, William Parkes, William Duncan, Matthew I. Hollister, Carl D. Reintsema, Mark Halpern, Anthony J. Walton, Kent D. Irwin, Wayne S. Holland, R. V. Sudiwala, B. Burger, Xiaofeng Gao, Camelia Dunare, and Peter A. R. Ade
Subjects: Physics, Pixel, business.industry, Bolometer, Large format, Submillimetre astronomy, law.invention, Optics, Cardinal point, law, Transition edge sensor, business, Noise-equivalent power, James Clerk Maxwell Telescope
Abstract: We present the results of characterization measurements on a 1280 pixel superconducting bolometer array designed for operation at wavelengths around 450 μm. The array is a prototype for the sub-arrays which will form the focal plane for the SCUBA-2 sub-mm camera, being built for the James Clerk Maxwell Telescope (JCMT) in Hawaii. With over 10 000 pixels in total, it will provide a huge improvement in both sensitivity and mapping speed over existing instruments. The array consists of molybdenum-copper bi-layer TES (transition edge sensor) pixels, bonded to a multiplexer. The detectors operate at a temperature of approximately 175 mK, and require a heat sink at a temperature of approximately 60 mK. In contrast to previous TES arrays, the multiplexing elements are located beneath each pixel (an "in-focal plane" configuration). We present the results of electrical and optical measurements, and show that the optical NEP (noise equivalent power) is less than 1.4 × 10-16 W Hz-0.5 and thus within the goal of 1.5 × 10-16 W Hz-0.5.
Published: 2006
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48. First Tests of Prototype SCUBA-2 Superconducting Bolometer Array

Author: Michael D. Audley, Peter A. R. Ade, Rashmikant V. Sudiwala, Carl D. Reintsema, Cynthia L. Hunt, Kent D. Irwin, Wayne S. Holland, Dan Bintley, Adam Woodcraft, M. J. MacIntosh, and Gene C. Hilton
Subjects: Physics, Pixel, business.industry, Bolometer, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Electrical engineering, Cryogenics, Multiplexing, law.invention, Optics, law, Proximity effect (audio), Transition edge sensor, business, James Clerk Maxwell Telescope
Abstract: We present results of the first tests on a 1280 pixel superconducting bolometer array, a prototype for SCUBA‐2, a sub‐mm camera being built for the James Clerk Maxwell Telescope in Hawaii. The bolometers are TES (transition edge sensor) detectors; these take advantage of the large variation of resistance with temperature through the superconducting transition. To keep the number of wires reasonable, a multiplexed read‐out is used. Each pixel is read out through an individual DC SQUID; room temperature electronics switch between rows in the array by biasing the appropriate SQUIDs in turn. Arrays of 100 SQUIDs in series for each column then amplify the output. Unlike previous TES arrays, the multiplexing elements are located beneath each pixel, making large arrays possible, but construction more challenging. The detectors are constructed from Mo/Cu bi‐layers; this technique enables the transition temperature to be tuned using the proximity effect by choosing the thickness of the normal and superconducting materials. To achieve the required performance, the detectors are operated at a temperature of approximately 120 mK. We describe the results of a basic characterisation of the array, demonstrating that it is fully operational, and give the results of signal to noise measurements.
Published: 2006
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49. A software simulator for the Herschel-SPIRE imaging photometer

Author: B. Sibthorpe, Matthew Joseph Griffin, Steven Lloyd Watkin, and Adam Woodcraft
Subjects: Physics, Spectrometer, business.industry, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Photometer, Orbital mechanics, law.invention, Telescope, Spire, Software, law, business, Astrophysics::Galaxy Astrophysics, Data reduction, Remote sensing
Abstract: SPIRE, the Spectral and Photometric Imaging Receiver, is one of three instruments to be flown on ESA's Herschel Space Observatory. It contains a three-band submillimetre camera and an imaging Fourier transform spectrometer, and uses arrays of feedhorn-coupled bolometric detectors operating at a temperature of 300 mK. Detailed software simulators are being developed for the SPIRE photometer and spectrometer. The photometer simulator is based on an adaptable modular representation of the relevant instrument and telescope subsystems, and is designed to produce highly realistic science and housekeeping data timelines. It will be used for a variety of purposes, including instrument characterisation during ground testing and in orbit, testing and optimisation of operating modes and strategies, evaluation of data reduction software using simulated data streams (derived by "observing" a simulated sky intensity distribution with the simulator), observing time estimation, and diagnostics of instrument systematics. In this paper we present the current status of the photometer simulator and the future development and implementation strategy.
Published: 2004
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50. First results from Herschel-SPIRE performance tests

Author: Douglas Griffin, Locke D. Spencer, Sunil Sidher, Adam Woodcraft, David A. Naylor, David J. Smith, James J. Bock, Bruce Swinyard, K. J. King, Bernhard Schulz, Tanya L. Lim, Eric Sawyer, Samuel Ronayette, Asier A. Aramburu, Peter Charles Hargrave, Matthew Joseph Griffin, Marc Ferlet, Sarah Leeks, and Mather, John C.
Subjects: Photometry (optics), Scientific instrument, Spire, Noise, Far infrared, Computer science, Stray light, Instrumentation, Detector, Electromagnetic interference, Simulation
Abstract: The Spectral and Photometric Imaging REceiver (SPIRE) is one of the three scientific instruments on the European Space Agency's Herschel mission. At the start of 2004 the Cryogenic Qualification Model (CQM) of SPIRE was tested with the aim of verifying the instrument system design and evaluating key performance parameters. We present a description of the test facility, an overview of the instrument tests carried out on the CQM, and the first results from the analysis of the test data. Instrument optical efficiency and detector noise levels are close to the values expected from unit-level tests, and the SPIRE instrument system works well, with no degradation in performance from stray light, electromagnetic interference or microphonically induced noise. Some anomalies and imperfections in the instrument performance, test set-up, and test procedures have been identified and will be addressed in the next test campaign.
Published: 2004
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