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51. Optical design and verification of the 4mm receiver for the 20m telescope at Onsala Space Observatory

Author

Walker, George William, Kalinauskaite, Eimante, McCarthy, D., Trappe, Neil, Murphy, J.Anthony, Helldner, Leif, Pantaleev, Miroslav, Flygare, Jonas, Walker, George William, Kalinauskaite, Eimante, McCarthy, D., Trappe, Neil, Murphy, J.Anthony, Helldner, Leif, Pantaleev, Miroslav, and Flygare, Jonas

Abstract

The work of this research is the design, analysis and verification of the optical performance of a 4 mm receiver channel for the 20 m telescope at Onsala Space Observatory, Onsala, Sweden. The 4 mm (75 GHz) receiver is a newly proposed channel designed to be installed parallel to the existing 3 mm (100 GHz) channel targeting new science at that longer wavelength. Gaussian beam mode analysis is used to produce the fundamental optical design of the system. The design is then analysed more accurately with the physical optics approximation. We report on the comparison of simulation and measurement and verification of the system design.

Published
2016

52. Determination of the Phase Centers of Millimeter-Wave Horn Antennas Using a Holographic Interference Technique

Author

McAuley, I., Murphy, J.Anthony, McCarthy, Darragh, Gradziel, Marcin, Mahon, R., O'Sullivan, Créidhe, Trappe, Neil, McAuley, I., Murphy, J.Anthony, McCarthy, Darragh, Gradziel, Marcin, Mahon, R., O'Sullivan, Créidhe, and Trappe, Neil

Abstract

In this paper, we discuss how a holographic interference technique can be applied in the experimental determination of the phase centers of non-standard horn antennas in the millimeter-waveband. The phase center is the point inside the horn from which the radiation appears to emanate when viewed from the far-field, and knowing its location is necessary for optimizing coupling efficiencies to quasi-optical systems. For non-standard horn designs, and other feed structures, the phase center may be difficult to reliably predict by simulation, in which case, before committing to antenna manufacture, there is a requirement for it to be determined experimentally. Although the phase center can be recovered by direct phase measurement of the far-field beam pattern, this usually involves expensive instrumentation such as a vector network analyzer for millimeter wave horn antennas. In this paper, we describe one inexpensive alternative, which is based on measuring the interference pattern in intensity between the radiation from the horn of interest and a reference beam derived from the same coherent source in an off-axis holography setup. The accuracy of the approach is improved by comparison with the interference pattern of a well-understood standard horn (such as a corrugated conical horn) in the same experimental setup. We present an example of the technique applied to a profiled smooth-walled horn antenna, which has been especially designed for cosmic microwave background (CMB) polarization experiments.

Published
2016

53. Modeling multimode feed-horn coupled bolometers for millimeter-wave and terahertz astronomical instrumentation

Author

Kalinauskaite, Eimante, additional, Murphy, Anthony, additional, McAuley, Ian, additional, Trappe, Neil A., additional, Bracken, Colm P., additional, McCarthy, Darragh N., additional, Doherty, Stephen, additional, Gradziel, Marcin L., additional, O'Sullivan, Creidhe, additional, Maffei, Bruno, additional, Lamarre, Jean-Michel A., additional, Ade, Peter A. R., additional, and Savini, Giorgio, additional

Published
2016
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58. The Polarized Radiation Imaging and Spectroscopy Mission

Author

André, Philippe, Baccigalupi, Carlo, Banday, Anthony, Barbosa, Domingos, Barreiro, Belen, Bartlett, James, Bartolo, Nicola, Battistelli, Elia, Battye, Richard, Bendo, George, Benoȋt, Alain, Bernard, Jean-Philippe, Bersanelli, Marco, Béthermin, Matthieu, Bielewicz, Pawel, Bonaldi, Anna, Bouchet, François, Boulanger, François, Brand, Jan, Bucher, Martin, Burigana, Carlo, Cai, Zhen-Yi, Camus, Philippe, Casas, Francisco, Casasola, Viviana, Castex, Guillaume, Challinor, Anthony, Chluba, Jens, Chon, Gayoung, Colafrancesco, Sergio, Comis, Barbara, Cuttaia, Francesco, D'Alessandro, Giuseppe, Da Silva, Antonio, Davis, Richard, de Avillez, Miguel, de Bernardis, Paolo, de Petris, Marco, de Rosa, Adriano, de Zotti, Gianfranco, Delabrouille, Jacques, Désert, François-Xavier, Dickinson, Clive, Diego, Jose Maria, Dunkley, Joanna, Enßlin, Torsten, Errard, Josquin, Falgarone, Edith, Ferreira, Pedro, Ferrière, Katia, Finelli, Fabio, Fletcher, Andrew, Fosalba, Pablo, Fuller, Gary, Galli, Silvia, Ganga, Ken, García-Bellido, Juan, Ghribi, Adnan, Giard, Martin, Giraud-Héraud, Yannick, Gonzalez-Nuevo, Joaquin, Grainge, Keith, Gruppuso, Alessandro, Hall, Alex, Hamilton, Jean-Christophe, Haverkorn, Marijke, Hernandez-Monteagudo, Carlos, Herranz, Diego, Jackson, Mark, Jaffe, Andrew, Khatri, Rishi, Kunz, Martin, Lamagna, Luca, Lattanzi, Massimiliano, Leahy, Paddy, Lesgourgues, Julien, Liguori, Michele, Liuzzo, Elisabetta, Lopez-Caniego, Marcos, Macias-Perez, Juan, Maffei, Bruno, Maino, Davide, Mangilli, Anna, Martinez-Gonzalez, Enrique, Martins, Carlos J.A.P., Masi, Silvia, Massardi, Marcella, Matarrese, Sabino, Melchiorri, Alessandro, Melin, Jean-Baptiste, Mennella, Aniello, Mignano, Arturo, Miville-Deschênes, Marc-Antoine, Monfardini, Alessandro, Murphy, Anthony, Naselsky, Pavel, Nati, Federico, Natoli, Paolo, Negrello, Mattia, Noviello, Fabio, O'Sullivan, Créidhe, Paci, Francesco, Pagano, Luca, Paladino, Rosita, Palanque-Delabrouille, Nathalie, Paoletti, Daniela, Peiris, Hiranya, Perrotta, Francesca, Piacentini, Francesco, Piat, Michel, Piccirillo, Lucio, Pisano, Giampaolo, Polenta, Gianluca, Pollo, Agnieszka, Ponthieu, Nicolas, Remazeilles, Mathieu, Ricciardi, Sara, Roman, Matthieu, Rosset, Cyrille, Rubino-Martin, Jose-Alberto, Salatino, Maria, Schillaci, Alessandro, Shellard, Paul, Silk, Joseph, Starobinsky, Alexei, Stompor, Radek, Sunyaev, Rashid, Tartari, Andrea, Terenzi, Luca, Toffolatti, Luigi, Tomasi, Maurizio, Trappe, Neil, Tristram, Matthieu, Trombetti, Tiziana, Tucci, Marco, Van de Weijgaert, Rien, Van Tent, Bartjan, Verde, Licia, Vielva, Patricio, Wandelt, Ben, Watson, Robert, Withington, Stafford, and Cabrera, Nicolas

Subjects
Astrophysics and Astronomy, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

PRISM (Polarized Radiation Imaging and Spectroscopy Mission) was proposed to ESA in May 2013 as a large-class mission for investigating within the framework of the ESA Cosmic Vision program a set of important scientific questions that require high resolution, high sensitivity, full-sky observations of the sky emission at wavelengths ranging from millimeter-wave to the far-infrared. PRISM's main objective is to explore the distant universe, probing cosmic history from very early times until now as well as the structures, distribution of matter, and velocity flows throughout our Hubble volume. PRISM will survey the full sky in a large number of frequency bands in both intensity and polarization and will measure the absolute spectrum of sky emission more than three orders of magnitude better than COBE FIRAS. The aim of this Extended White Paper is to provide a more detailed overview of the highlights of the new science that will be made possible by PRISM PRISM (Polarized Radiation Imaging and Spectroscopy Mission) was proposed to ESA in May 2013as a large-class mission for investigating within the framework of the ESA Cosmic Visionprogram a set of important scientific questions that require high resolution, high sensitivity, full-skyobservations of the sky emissionat wavelengths ranging from millimeter-wave to the far-infrared.PRISM's main objective is to explore the distant universe, probing cosmichistory from very early times until now as well as the structures, distribution ofmatter, and velocity flows throughout our Hubble volume. PRISM willsurvey the full sky in a large number of frequency bands in bothintensity and polarization and will measure the absolute spectrum of sky emission more thanthree orders of magnitude better than COBE FIRAS. The data obtained will allow usto precisely measure the absolute sky brightness and polarization of all the components of thesky emission in the observed frequency range,separating the primordial and extragalactic components cleanly from the galactic and zodiacal light emissions.The aim of this Extended White Paper is to provide a more detailed overview of the highlightsof the new science that will be made possible by PRISM, which include: (1) the ultimategalaxy cluster survey using the Sunyaev-Zeldovich (SZ) effect, detecting approximately 106clusters extending to large redshift, including a characterization of the gas temperature ofthe brightest ones (through the relativistic corrections to the classic SZ template) as wellas a peculiar velocity survey using the kinetic SZ effect that comprises our entire Hubblevolume; (2) a detailed characterization of the properties and evolution of dusty galaxies, wherethe most of the star formation in the universe took place, the faintest population of whichconstitute the diffuse CIB (Cosmic Infrared Background); (3) a characterization of the B modes fromprimordial gravity waves generated during inflation and from gravitational lensing, as wellas the ultimate search for primordial non-Gaussianity using CMB polarization, which is lesscontaminated by foregrounds on small scales than the temperature anisotropies; (4) a searchfor distortions from a perfect blackbody spectrum, which include some nearly certain signalsand others that are more speculative but more informative; and (5) a study of the role of themagnetic field in star formation and its interaction with other components of theinterstellar medium of our Galaxy. These are but a few of the highlights presented herealong with a description of the proposed instrument. PRISM (Polarized Radiation Imaging and Spectroscopy Mission) was proposed to ESA in May 2013 as a large-class mission for investigating within the framework of the ESA Cosmic Vision program a set of important scientific questions that require high resolution, high sensitivity, full-sky observations of the sky emission at wavelengths ranging from millimeter-wave to the far-infrared. PRISM's main objective is to explore the distant universe, probing cosmic history from very early times until now as well as the structures, distribution of matter, and velocity flows throughout our Hubble volume. PRISM will survey the full sky in a large number of frequency bands in both intensity and polarization and will measure the absolute spectrum of sky emission more than three orders of magnitude better than COBE FIRAS. The aim of this Extended White Paper is to provide a more detailed overview of the highlights of the new science that will be made possible by PRISM

Published
2013

59. Measurements of the optical performance of bolometers for SPICA/SAFARI

Author

Audley, Michael D., de Lange, Gert, Gao, Jian-Rong, Khosropanah, Pourya, Ridder, Marcel, Ferrari, Lorenza, Laauwen, Wouter M., Ranjan, Manisha, Mauskopf, Philip D., Morozov, Dmitry, Trappe, Neil A., and Holland, Wayne S.

Subjects
Physics, Spectrometer, business.industry, Stray light, Detector, Bolometer, Imaging spectrometer, Spica, law.invention, Optics, law, Dilution refrigerator, Transition edge sensor, business
Abstract

We have measured the optical response of detectors designed for SAFARI, the far-infrared imaging spectrometer for the SPICA satellite. To take advantage of SPICA's cooled optics, SAFARI’s three bolometer arrays are populated with extremely sensitive (NEP~2×10-19 W/√Hz) transition edge sensors with a transition temperature close to 100 mK. The extreme sensitivity and low saturation power (~4 fW) of SAFARI’s detectors present challenges to characterizing them. We have therefore built up an ultra-low background test facility with a cryogen-free high-capacity dilution refrigerator, paying careful attention to stray-light exclusion. Our use of a pulse-tube cooler to pre-cool the dilution refrigerator required that the SAFARI Detector System Test Facility provide a high degree electrical, magnetic, and mechanical isolation for the detectors. We have carefully characterized the performance of the test facility in terms of background power loading. The test facility has been designed to be flexible and easily reconfigurable with internal illuminators that allow us to characterize the optical response of the detectors. We describe the test facility and some of the steps we took to create an ultra-low background test environment. We have measured the optical response of two detectors designed for SAFARI’s short-wave wavelength band in combination with a spherical backshort and conical feedhorn. We find an overall optical efficiency of 40% for both, compared with an ideal-case predicted optical efficiency of 66%.

Published
2012

61. Analysis and Optical Characterisation of Bolometric Integrating Cavities Including a Free Space Gap in the Waveguide Structure

Author

McCarthy, Darragh, Trappe, Neil, Doherty, Stephen, Murphy, J.Anthony, Bracken, Colm, Gradziel, Marcin, O'Sullivan, Créidhe, van der Vorst, M., Audley, Michael D., de Lange, G., McCarthy, Darragh, Trappe, Neil, Doherty, Stephen, Murphy, J.Anthony, Bracken, Colm, Gradziel, Marcin, O'Sullivan, Créidhe, van der Vorst, M., Audley, Michael D., and de Lange, G.

Abstract

Bolometric integrating cavities have been used with great success in previous far-infrared space missions, and are planned for extensive use in future missions where ever increasing sensitivity is required. It is critical for the purposes of design and the interpretation of results that these systems are thoroughly understood and optically characterised fully. Such systems, for manufacturing and mechanical reasons, may contain free space gaps between the feed horn antenna and the integrating cavity, and so it is necessary to include the effect of these waveguide openings in simulations. Since these pixels are electrically large, it is more feasible to model them by using the computationally efficient mode-matching approach. In this paper we discuss the elements required to model such pixels within the mode-matching approach and apply it to a typical pixel containing a free space gap, based on an experimental Transition Edge Sensor (TES) cavity waveguide pixel at SRON Groningen.

Published
2015

62. Quasi-optical phase retrieval of radiation patterns of non-standard horn antennas at millimetre and submillimetre wavelengths

Author

Murphy, J.Anthony, McAuley, Ian, McCarthy, Darragh, Trappe, Neil, Gradziel, Marcin, O'Sullivan, Créidhe, Mahon, R., Murphy, J.Anthony, McAuley, Ian, McCarthy, Darragh, Trappe, Neil, Gradziel, Marcin, O'Sullivan, Créidhe, and Mahon, R.

Abstract

The location of the phase centres of antenna feeds is critical for optimised sensitivity and resolution on reflector antennas and telescopes. While the measurement of the far-field intensity patterns of such feeds is relatively straightforward, the direct recovery of their phase patterns requires access to expensive phase sensitive instrumentation such as a vector network analyzer. We present an inexpensive alternative quasi-optical technique, analogous to off-axis holography at visible wavelengths, that allows for the phase curvature of the feed pattern, and thus the phase centre, to be recovered with sufficient accuracy for optimizing aperture efficiency and resolution on a reflector antenna. We discuss the accuracy of the technique and compare results for the case of a specialized horn antenna for CMB polarization operating at 100GHz, using both the quasi-optical method and a vector network analyzer as a bench mark measurement tool for verification of the approach. We also include some measurements made of a lens antenna fed by a bare waveguide radiator.

Published
2015

63. Cross-polarization characterization of GORE—TEX© at ALMA band 9 frequencies

Author

Candotti, Massimo, Baryshev, A., Trappe, Neil, Hesper, R., Murphy, J.Anthony, and Barkhol, J.

Abstract

GORE-TEX material, commonly used in radomes, is known to be transparent at microwave bands. In ALMA a thin GORE-TEX membrane will cover the aperture through which the RF beam enters the cabin at the primary vertex hole. Slabs of GORE-TEX are also generally employed in windows for intermediate temperature shields inside the cryostat. The purpose of these windows ideally is to allow the beam to pass through them without introducing any alteration to the beam properties. The main concern is RF loss, but also cross-polarization efficiency degradation. This paper will concentrate on the results we have obtained for ALMA band 9 (602-720 GHz), in relation of loss of cross-polarization efficiency of a linearly polarized beam passing through a GORE-TEX slab, depending on its orientation relative to the direction of polarization of the beam. In order to spot anisotropic behavior of the material under test, an ad hoc measurements set-up has been used. Systematic measurements of cross-polarization properties for different thicknesses of GORE-TEX slabs were undertaken. Cross-polarization information is given in relation of the relative angle between the incident beam polarization and the material under test.

Published
2006

65. Modal Analysis and Experimental Study of High-Order Mode Contribution to Standing Waves in Quasi-Optical Systems

Author

Jellema, Willem, Withington, S., Trappe, Neil, Murphy, J. A., Wild, Wolfgang, and Astronomy

Abstract

In many submillimeter-wave optical systems performance is in some way affected by the presence of standing waves. Usually these effects are studied empirically or only modeled to first-order by assuming a quasi-sinusoidal variation with distance and wavelength. In this paper we present an analytical technique to calculate the coupling between two corrugated horns including the total transmission and reflection properties. In our model we have combined the waveguide mode matching technique with a Gaussian beam mode description of the free space propagation. We illustrate the approach for the case of two coupled corrugated horns as the distance between them is varied. We furthermore present experimental test results confirming that multiple reflections do not always result in a classical periodic standing wave pattern. In particular when the horns are close together and the fields are not well matched, high Q cavity effects are observed resulting in irregular standing wave patterns. These cavity effects can be attributed to high-order modes which get trapped between transmitting and receiving horn. We finally discuss the consequences of our observations for a few examples of typical quasi-optical arrangements illustrating that the presented effects can have important consequences for submillimeter-wave optical systems.

Published
2004

66. Measurements of the Optical Performance of Prototype TES Bolometers for SAFARI

Author

Audley, Michael D., de Lange, G., Ranjan, M., Gao, J.R., Khosropanah, P., Ridder, Marcel, Mauskopf, P.D., Morozov, Dmitry, Doherty, Stephen, Trappe, Neil, Withington, S., Audley, Michael D., de Lange, G., Ranjan, M., Gao, J.R., Khosropanah, P., Ridder, Marcel, Mauskopf, P.D., Morozov, Dmitry, Doherty, Stephen, Trappe, Neil, and Withington, S.

Published
2014

67. Multimode horn antennas for far-infrared astronomy

Author

Murphy, J.Anthony, Bracken, Carl, Doherty, Stephen, McAuley, Ian, Wilson, D., O'Sullivan, Créidhe, Trappe, Neil, Gradziel, Marcin, Ade, P.A.R., Gleeson, E., Maffei, B., Lamarre, J.-M., Noviello, F., Peacocke, T., Pisano, G., Puget, J.-L., Savini, G., Sudiwala, R., Withington, S., Wylde, R.J., Yurchenko, V., Murphy, J.Anthony, Bracken, Carl, Doherty, Stephen, McAuley, Ian, Wilson, D., O'Sullivan, Créidhe, Trappe, Neil, Gradziel, Marcin, Ade, P.A.R., Gleeson, E., Maffei, B., Lamarre, J.-M., Noviello, F., Peacocke, T., Pisano, G., Puget, J.-L., Savini, G., Sudiwala, R., Withington, S., Wylde, R.J., and Yurchenko, V.

Abstract

Multi-mode horns combined with bolometric or incoherent detectors are finding application in astronomical receivers for which partially coherent operation can provide increased throughput and thus sensitivity. This is advantageous when observing faint sources, especially if diffraction limited resolution is not required, or if the horn beam is truncated by a cold stop in the optical train. We discuss how such horns can be simulated and present examples from receiver instrumentation on the Planck and SPICA space telescopes.

Published
2014

68. PRISM (Polarized Radiation Imaging and Spectroscopy Mission): an extended white paper

Author

Philippe, A, Baccigalupi, C, Anthony, B, Domingos, B, Barreiro, B, James, B, Bartolo, N, Stefano Battistelli, E, Battye, R, Bendo, G, Benoit, A, Bernard, J, Bersanelli, M, Bethermin, M, Pawel, B, Bonaldi, A, Francois, B, Jan, B, Martin, B, Burigana, C, Cai, Z, Philippe, C, Casas, F, Casasola, V, Guillaume, C, Anthony, C, Jens, C, Chon, G, Colafrancesco, S, Comis, B, Cuttaia, F, D'Alessandro, G, Da Silva, A, Davis, R, Avillez Miguel, D, Bernardis, P, De Bernardis, P, De Petris, M, De Rosa, A, De Zotti, G, Jacques, D, Desert, F, Dickinson, C, Maria Diego, J, Dunkley, J, Ensslin, T, Errard, J, Falgarone, E, Ferreira, P, Ferriere, K, Finelli, F, Andrew, F, Fosalba, P, Gary, F, Galli, S, Ken, G, Juan, G, Ghribi, A, Martin, G, Giraud-Heraud, Y, Gonzalez-Nuevo, J, Keith, G, Gruppuso, A, Alex, H, Hamilton, J, Haverkorn, M, Hernandez-Monteagudo, C, Herranz, D, Mark, J, Andrew, J, Khatri, R, Martin, K, Lamagna, L, Lattanzi, M, Leahy, P, Julien, L, Liguori, M, Liuzzo, E, Marcos, L, Juan, M, Maffei, B, Maino, D, Mangilli, A, Martinez-Gonzalez, E, Martins, C, Masi, S, Massardi, M, Matarrese, S, Melchiorri, A, Melin, J, Mennella, A, Mignano, A, Miville-Deschenes, M, Monfardini, A, Anthony, M, Pavel, N, Nati, F, Natoli, P, Negrello, M, Noviello, F, O'Sullivan, C, Paci, F, Pagano, L, Paladino, R, Nathalie, P, Paoletti, D, Peiris, H, Perrotta, F, Piacentini, F, Piat, M, Piccirillo, L, Pisano, G, Polenta, G, Pollo, A, Nicolas, P, Mathieu, R, Ricciardi, S, Roman, M, Rosset, C, Rubino-Martin, J, Salatino, M, Schillaci, A, Paul, S, Silk, J, Starobinsky, A, Stompor, R, Rashid, S, Tartari, A, Terenzi, L, Toffolatti, L, Tomasi, M, Neil, T, Tristram, M, Trombetti, T, Tucci, M, Van De Weijgaert, R, Van Tent, B, Verde, L, Vielva, P, Ben, W, Watson, R, Stafford, W, André Philippe, Carlo Baccigalupi, Banday Anthony, Barbosa Domingos, Belen Barreiro, Bartlett James, Nicola Bartolo, Elia Stefano Battistelli, Richard Battye, George Bendo, Alain Benoit, Jean-Philippe Bernard, Marco Bersanelli, Matthieu Bethermin, Bielewicz Pawel, Anna Bonaldi, Bouchet Francois, Boulanger Francois, Brand Jan, Bucher Martin, Carlo Burigana, Zhen-Yi Cai, Camus Philippe, Francisco Casas, Viviana Casasola, Castex Guillaume, Challinor Anthony, Chluba Jens, Gayoung Chon, Sergio Colafrancesco, Barbara Comis, Francesco Cuttaia, Giuseppe D'Alessandro, Antonio Da Silva, Richard Davis, D.E. Avillez Miguel, Paolo D.E. Bernardis, Paolo De Bernardis, Marco De Petris, Adriano De Rosa, Gianfranco De Zotti, Delabrouille Jacques, Francois-Xavier Desert, Clive Dickinson, Jose Maria Diego, Joanna Dunkley, Torsten Ensslin, Josquin Errard, Edith Falgarone, Pedro Ferreira, Katia Ferriere, Fabio Finelli, Fletcher Andrew, Pablo Fosalba, Fuller Gary, Silvia Galli, Ganga Ken, García-Bellido Juan, Adnan Ghribi, Giard Martin, Yannick Giraud-Heraud, Joaquin Gonzalez-Nuevo, Grainge Keith, Alessandro Gruppuso, Hall Alex, Jean-Christophe Hamilton, Marijke Haverkorn, Carlos Hernandez-Monteagudo, Diego Herranz, Jackson Mark, Jaffe Andrew, Rishi Khatri, Kunz Martin, Luca Lamagna, Massimiliano Lattanzi, Paddy Leahy, Lesgourgues Julien, Michele Liguori, Elisabetta Liuzzo, Lopez-Caniego Marcos, Macias-Perez Juan, Bruno Maffei, Davide Maino, Anna Mangilli, Enrique Martinez-Gonzalez, Carlos J.A.P. Martins, Silvia Masi, Marcella Massardi, Sabino Matarrese, Alessandro Melchiorri, Jean-Baptiste Melin, Aniello Mennella, Arturo Mignano, Marc-Antoine Miville-Deschenes, Alessandro Monfardini, Murphy Anthony, Naselsky Pavel, Federico Nati, Paolo Natoli, Mattia Negrello, Fabio Noviello, Créidhe O'Sullivan, Francesco Paci, Luca Pagano, Rosita Paladino, Palanque-Delabrouille Nathalie, Daniela Paoletti, Hiranya Peiris, Francesca Perrotta, Francesco Piacentini, Michel Piat, Lucio Piccirillo, Giampaolo Pisano, Gianluca Polenta, Agnieszka Pollo, Ponthieu Nicolas, Remazeilles Mathieu, Sara Ricciardi, Matthieu Roman, Cyrille Rosset, Jose-Alberto Rubino-Martin, Maria Salatino, Alessandro Schillaci, Shellard Paul, Joseph Silk, Alexei Starobinsky, Radek Stompor, Sunyaev Rashid, Andrea Tartari, Luca Terenzi, Luigi Toffolatti, Maurizio Tomasi, Trappe Neil, Matthieu Tristram, Tiziana Trombetti, Marco Tucci, Rien Van De Weijgaert, Bartjan Van Tent, Licia Verde, Patricio Vielva, Wandelt Ben, Robert Watson, Withington Stafford, Philippe, A, Baccigalupi, C, Anthony, B, Domingos, B, Barreiro, B, James, B, Bartolo, N, Stefano Battistelli, E, Battye, R, Bendo, G, Benoit, A, Bernard, J, Bersanelli, M, Bethermin, M, Pawel, B, Bonaldi, A, Francois, B, Jan, B, Martin, B, Burigana, C, Cai, Z, Philippe, C, Casas, F, Casasola, V, Guillaume, C, Anthony, C, Jens, C, Chon, G, Colafrancesco, S, Comis, B, Cuttaia, F, D'Alessandro, G, Da Silva, A, Davis, R, Avillez Miguel, D, Bernardis, P, De Bernardis, P, De Petris, M, De Rosa, A, De Zotti, G, Jacques, D, Desert, F, Dickinson, C, Maria Diego, J, Dunkley, J, Ensslin, T, Errard, J, Falgarone, E, Ferreira, P, Ferriere, K, Finelli, F, Andrew, F, Fosalba, P, Gary, F, Galli, S, Ken, G, Juan, G, Ghribi, A, Martin, G, Giraud-Heraud, Y, Gonzalez-Nuevo, J, Keith, G, Gruppuso, A, Alex, H, Hamilton, J, Haverkorn, M, Hernandez-Monteagudo, C, Herranz, D, Mark, J, Andrew, J, Khatri, R, Martin, K, Lamagna, L, Lattanzi, M, Leahy, P, Julien, L, Liguori, M, Liuzzo, E, Marcos, L, Juan, M, Maffei, B, Maino, D, Mangilli, A, Martinez-Gonzalez, E, Martins, C, Masi, S, Massardi, M, Matarrese, S, Melchiorri, A, Melin, J, Mennella, A, Mignano, A, Miville-Deschenes, M, Monfardini, A, Anthony, M, Pavel, N, Nati, F, Natoli, P, Negrello, M, Noviello, F, O'Sullivan, C, Paci, F, Pagano, L, Paladino, R, Nathalie, P, Paoletti, D, Peiris, H, Perrotta, F, Piacentini, F, Piat, M, Piccirillo, L, Pisano, G, Polenta, G, Pollo, A, Nicolas, P, Mathieu, R, Ricciardi, S, Roman, M, Rosset, C, Rubino-Martin, J, Salatino, M, Schillaci, A, Paul, S, Silk, J, Starobinsky, A, Stompor, R, Rashid, S, Tartari, A, Terenzi, L, Toffolatti, L, Tomasi, M, Neil, T, Tristram, M, Trombetti, T, Tucci, M, Van De Weijgaert, R, Van Tent, B, Verde, L, Vielva, P, Ben, W, Watson, R, Stafford, W, André Philippe, Carlo Baccigalupi, Banday Anthony, Barbosa Domingos, Belen Barreiro, Bartlett James, Nicola Bartolo, Elia Stefano Battistelli, Richard Battye, George Bendo, Alain Benoit, Jean-Philippe Bernard, Marco Bersanelli, Matthieu Bethermin, Bielewicz Pawel, Anna Bonaldi, Bouchet Francois, Boulanger Francois, Brand Jan, Bucher Martin, Carlo Burigana, Zhen-Yi Cai, Camus Philippe, Francisco Casas, Viviana Casasola, Castex Guillaume, Challinor Anthony, Chluba Jens, Gayoung Chon, Sergio Colafrancesco, Barbara Comis, Francesco Cuttaia, Giuseppe D'Alessandro, Antonio Da Silva, Richard Davis, D.E. Avillez Miguel, Paolo D.E. Bernardis, Paolo De Bernardis, Marco De Petris, Adriano De Rosa, Gianfranco De Zotti, Delabrouille Jacques, Francois-Xavier Desert, Clive Dickinson, Jose Maria Diego, Joanna Dunkley, Torsten Ensslin, Josquin Errard, Edith Falgarone, Pedro Ferreira, Katia Ferriere, Fabio Finelli, Fletcher Andrew, Pablo Fosalba, Fuller Gary, Silvia Galli, Ganga Ken, García-Bellido Juan, Adnan Ghribi, Giard Martin, Yannick Giraud-Heraud, Joaquin Gonzalez-Nuevo, Grainge Keith, Alessandro Gruppuso, Hall Alex, Jean-Christophe Hamilton, Marijke Haverkorn, Carlos Hernandez-Monteagudo, Diego Herranz, Jackson Mark, Jaffe Andrew, Rishi Khatri, Kunz Martin, Luca Lamagna, Massimiliano Lattanzi, Paddy Leahy, Lesgourgues Julien, Michele Liguori, Elisabetta Liuzzo, Lopez-Caniego Marcos, Macias-Perez Juan, Bruno Maffei, Davide Maino, Anna Mangilli, Enrique Martinez-Gonzalez, Carlos J.A.P. Martins, Silvia Masi, Marcella Massardi, Sabino Matarrese, Alessandro Melchiorri, Jean-Baptiste Melin, Aniello Mennella, Arturo Mignano, Marc-Antoine Miville-Deschenes, Alessandro Monfardini, Murphy Anthony, Naselsky Pavel, Federico Nati, Paolo Natoli, Mattia Negrello, Fabio Noviello, Créidhe O'Sullivan, Francesco Paci, Luca Pagano, Rosita Paladino, Palanque-Delabrouille Nathalie, Daniela Paoletti, Hiranya Peiris, Francesca Perrotta, Francesco Piacentini, Michel Piat, Lucio Piccirillo, Giampaolo Pisano, Gianluca Polenta, Agnieszka Pollo, Ponthieu Nicolas, Remazeilles Mathieu, Sara Ricciardi, Matthieu Roman, Cyrille Rosset, Jose-Alberto Rubino-Martin, Maria Salatino, Alessandro Schillaci, Shellard Paul, Joseph Silk, Alexei Starobinsky, Radek Stompor, Sunyaev Rashid, Andrea Tartari, Luca Terenzi, Luigi Toffolatti, Maurizio Tomasi, Trappe Neil, Matthieu Tristram, Tiziana Trombetti, Marco Tucci, Rien Van De Weijgaert, Bartjan Van Tent, Licia Verde, Patricio Vielva, Wandelt Ben, Robert Watson, and Withington Stafford

Abstract

PRISM (Polarized Radiation Imaging and Spectroscopy Mission) was proposed to ESA in May 2013 as a large-class mission for investigating within the framework of the ESA Cosmic Vision program a set of important scientific questions that require high resolution, high sensitivity, full-sky observations of the sky emission at wavelengths ranging from millimeter-wave to the far-infrared. PRISM's main objective is to explore the distant universe, probing cosmic history from very early times until now as well as the structures, distribution of matter, and velocity flows throughout our Hubble volume. PRISM will survey the full sky in a large number of frequency bands in both intensity and polarization and will measure the absolute spectrum of sky emission more than three orders of magnitude better than COBE FIRAS. The data obtained will allow us to precisely measure the absolute sky brightness and polarization of all the components of the sky emission in the observed frequency range, separating the primordial and extragalactic components cleanly from the galactic and zodiacal light emissions. The aim of this Extended White Paper is to provide a more detailed overview of the highlights of the new science that will be made possible by PRISM, which include: (1) the ultimate galaxy cluster survey using the Sunyaev-Zeldovich (SZ) effect, detecting approximately 10 6 clusters extending to large redshift, including a characterization of the gas temperature of the brightest ones (through the relativistic corrections to the classic SZ template) as well as a peculiar velocity survey using the kinetic SZ effect that comprises our entire Hubble volume; (2) a detailed characterization of the properties and evolution of dusty galaxies, where the most of the star formation in the universe took place, the faintest population of which constitute the diffuse CIB (Cosmic Infrared Background); (3) a characterization of the B modes from primordial gravity waves generated during inflation and fro

Published
2014

69. PRISM (Polarized Radiation Imaging and Spectroscopy Mission): an extended white paper

Author

André, P., Baccigalupi, C., Banday, A.J., Barbosa, D., Barreiro, B., Bartlett, J., Bartolo, N., Battistelli, E., Battye, R., Bendo, G., Benoit, A., Bernard, J.-P., Bersanelli, M., Béthermin, M., Bielewicz, P., Bonaldi, A., Bouchet, F.R., Brand, J., Bucher, M., Burigana, C., Cai, Z.Y., Camus, P., Casas, F.J., Casasola, V., Castex, G., Challinor, A., Chluba, J., Chon, G., Colafrancesco, S., Comis, B., Cuttaia, F., D'Alessandro, Giuseppe, Da Silva, A., Davis, R.J., de Avillez, M., De Bernardis, P., De Petris, M., de Rosa, A., de Zotti, G., Delabrouille, J., Desert, F.-X., Dickinson, C., Diego, J.M., Dunkley, J., Enßlin, T.A., Errard, J., Falgarone, E., Ferreira, P., Ferrière, K., Finelli, F., Fletcher, A., Fosalba, P., Fuller, G., Galli, S., Ganga, K., García-Bellido, J., Ghribi, A., Giard, M., Giraud-Héraud, Y., Gonzalez-Nuevo, J., Grainge, K.J.B., Gruppuso, A., Hall, Alex, Hamilton, J.-Ch., Haverkorn, M., Hernandez-Monteagudo, C., Herranz, D., Jackson, M., Jaffe, A.H., Khatri, R., Kunz, M., Lamagna, L., Lattanzi, M., Leahy, P., Lesgourgues, J., Liguori, M., Liuzzo, E., Lopez-Caniego, M., Macias-Perez, J.F., Maffei, B., Maino, D., Mangilli, A., Martinez-Gonzalez, E., Martins, C.J.A.P., Masi, S., Massardi, M., Matarrese, S., Melchiorri, A., Melin, J.-B., Mennella, A., Mignano, A., Miville-Deschenes, M.-A., Monfardini, A., Murphy, J.Anthony, Naselsky, P., Nati, F., Natoli, P., Negrello, M., Noviello, F., O'Sullivan, Créidhe, Paci, F., Pagano, L., Paladino, R., Palanque-Delabrouille, N., Paoletti, D., Peiris, H., Perrotta, F., Piacentini, F., Piat, M., Piccirillo, L., Pisano, G., Polenta, G., Pollo, A., Ponthieu, N., Remazeilles, M., Ricciardi, S., Roman, M., Rosset, C., Rubino-Martin, J.A., Salatino, M., Schillaci, A., Shellard, P., Silk, J., Starobinsky, Alexei A., Stompor, R., Sunyaev, R., Tartari, A., Terenzi, L., Toffolatti, L., Tomasi, M., Trappe, Neil, Tristram, M., Trombetti, T., Tucci, M., van de Weijgaert, R., Van Tent, B., Verde, L., Vielva, P., Wandelt, B.D., Watson, Robert, Withington, Stafford, André, P., Baccigalupi, C., Banday, A.J., Barbosa, D., Barreiro, B., Bartlett, J., Bartolo, N., Battistelli, E., Battye, R., Bendo, G., Benoit, A., Bernard, J.-P., Bersanelli, M., Béthermin, M., Bielewicz, P., Bonaldi, A., Bouchet, F.R., Brand, J., Bucher, M., Burigana, C., Cai, Z.Y., Camus, P., Casas, F.J., Casasola, V., Castex, G., Challinor, A., Chluba, J., Chon, G., Colafrancesco, S., Comis, B., Cuttaia, F., D'Alessandro, Giuseppe, Da Silva, A., Davis, R.J., de Avillez, M., De Bernardis, P., De Petris, M., de Rosa, A., de Zotti, G., Delabrouille, J., Desert, F.-X., Dickinson, C., Diego, J.M., Dunkley, J., Enßlin, T.A., Errard, J., Falgarone, E., Ferreira, P., Ferrière, K., Finelli, F., Fletcher, A., Fosalba, P., Fuller, G., Galli, S., Ganga, K., García-Bellido, J., Ghribi, A., Giard, M., Giraud-Héraud, Y., Gonzalez-Nuevo, J., Grainge, K.J.B., Gruppuso, A., Hall, Alex, Hamilton, J.-Ch., Haverkorn, M., Hernandez-Monteagudo, C., Herranz, D., Jackson, M., Jaffe, A.H., Khatri, R., Kunz, M., Lamagna, L., Lattanzi, M., Leahy, P., Lesgourgues, J., Liguori, M., Liuzzo, E., Lopez-Caniego, M., Macias-Perez, J.F., Maffei, B., Maino, D., Mangilli, A., Martinez-Gonzalez, E., Martins, C.J.A.P., Masi, S., Massardi, M., Matarrese, S., Melchiorri, A., Melin, J.-B., Mennella, A., Mignano, A., Miville-Deschenes, M.-A., Monfardini, A., Murphy, J.Anthony, Naselsky, P., Nati, F., Natoli, P., Negrello, M., Noviello, F., O'Sullivan, Créidhe, Paci, F., Pagano, L., Paladino, R., Palanque-Delabrouille, N., Paoletti, D., Peiris, H., Perrotta, F., Piacentini, F., Piat, M., Piccirillo, L., Pisano, G., Polenta, G., Pollo, A., Ponthieu, N., Remazeilles, M., Ricciardi, S., Roman, M., Rosset, C., Rubino-Martin, J.A., Salatino, M., Schillaci, A., Shellard, P., Silk, J., Starobinsky, Alexei A., Stompor, R., Sunyaev, R., Tartari, A., Terenzi, L., Toffolatti, L., Tomasi, M., Trappe, Neil, Tristram, M., Trombetti, T., Tucci, M., van de Weijgaert, R., Van Tent, B., Verde, L., Vielva, P., Wandelt, B.D., Watson, Robert, and Withington, Stafford

Abstract

PRISM (Polarized Radiation Imaging and Spectroscopy Mission) was proposed to ESA in May 2013 as a large-class mission for investigating within the framework of the ESA Cosmic Vision program a set of important scientific questions that require high resolution, high sensitivity, full-sky observations of the sky emission at wavelengths ranging from millimeter-wave to the far-infrared. PRISM 's main objective is to explore the distant universe, probing cosmic history from very early times until now as well as the structures, distribution of matter, and velocity ows throughout our Hubble volume. PRISM will survey the full sky in a large number of frequency bands in both intensity and polarization and will measure the absolute spectrum of sky emission more than three orders of magnitude better than COBE FIRAS. The data obtained will allow us to precisely measure the absolute sky brightness and polarization of all the components of the sky emission in the observed frequency range, separating the primordial and extragalactic components cleanly from the galactic and zodiacal light emissions. The aim of this Extended White Paper is to provide a more detailed overview of the highlights of the new science that will be made possible by PRISM, which include: (1) the ultimate galaxy cluster survey using the Sunyaev-Zeldovich (SZ) effect, detecting approximately 106 clusters extending to large redshift, including a characterization of the gas temperature of the brightest ones (through the relativistic corrections to the classic SZ template) as well as a peculiar velocity survey using the kinetic SZ effect that comprises our entire Hubble volume; (2) a detailed characterization of the properties and evolution of dusty galaxies, where the most of the star formation in the universe took place, the faintest population of which constitute the diffuse CIB (Cosmic Infrared Background); (3) a characterization of the B modes from primordial gravity waves generated during in ation and from g

Published
2014

70. Refractive telescope systems for future cosmic microwave background polarimetry experiments

Author

Hargrave, P.C., Savini, G., Gradziel, Marcin, Trappe, Neil, Tynan, Niall, Candotti, Massimo, Challinor, A., Sørenson, Stig, Ade, P.A.R., Sudiwala, R., van der Vorst, M., Hargrave, P.C., Savini, G., Gradziel, Marcin, Trappe, Neil, Tynan, Niall, Candotti, Massimo, Challinor, A., Sørenson, Stig, Ade, P.A.R., Sudiwala, R., and van der Vorst, M.

Abstract

This paper presents the key findings of an ESA-funded programme of work to investigate refractive systems and their application to precision polarimetry experiments. We briefly summarize the derivation of requirements on the optical system for CMB polarimetry, and the design of a refractive telescope system which meets these stringent requirements. An extensive programme of experimental work was undertaken in order to better understand the optical, thermal and mechanical characteristics of the lens material, and of lenses made from this material. A repeatable and controllable antireflection coating procedure was developed and validated, and used to coat lenses used in this study. Optical measurements before and after coating have been used to validate a new module for an industry-standard antenna modelling software package.

Published
2014

75. Experimental Verification of Electromagnetic Simulations of a HIFI Mixer Sub-Assembly

Author

Jellema, Willem, Wesselius, P., Withington, Stafford, Yassin, Ghassan, Murphy, J. Anthony, O'Sullivan, Créidhe, Trappe, Neil, Peacocke, T., and Leone, B.

Abstract

Phase II of the study "Far-Infrared Optics Design & Verification", commissioned by the European Space Agency (ESA), we investigate the ability of several commercial software packages (GRASP, CODEV, GLAD and ASAP) to predict the performance of a representative example of a submillimeter-wave optical system. In this paper, we use the software packages to predict the behaviour of a Mixer Sub-Assembly (MSA) of HIFI, and we compare the simulations with near-field measurements at 480 GHz. In order to be able to distinguish between the predictions of the packages, we move the corrugated horn of the MSA through its nominal focus position. A unique feature of the experimental arrangement is that the measured position of every field point is known absolutely to within fractions of a wavelength. In this paper we present the results of this through-focus experiment, which give a good first-order indication of the agreement between measured and simulated behaviour of a typical submillimeter-wave optical system.

Published
2003

76. Coated dielectric lens design, modelling and measurements for future CMB polarimetry missions

Author

Hargrave, P.C., Savini, G., Trappe, Neil, Challinor, A., Sørensen, S.B., Ade, P.A.R., Sudiwala, R., Walker, I.K., Gradziel, Marcin, Tynan, Niall, van der Vorst, M., Hargrave, P.C., Savini, G., Trappe, Neil, Challinor, A., Sørensen, S.B., Ade, P.A.R., Sudiwala, R., Walker, I.K., Gradziel, Marcin, Tynan, Niall, and van der Vorst, M.

Abstract

We present an ongoing programme of work to investigate the use of large dielectric lenses with coating layers for future satellite-based cosmic microwave background (CMB) polarimetry missions. The primary purpose of this study is to validate modelling and manufacturing techniques. We present details of the study, and preliminary results of material and lens testing.

Published
2013

77. Coated dielectric lenses for applications in high purity THz electromagnetic wave polarization detection

Author

Hargrave, P.C., Savini, G., Gradziel, Marcin, Tynan, Niall, Trappe, Neil, Sørensen, S.B., Ade, P.A.R., Sudiwala, R., Walker, I.K., van der Vorst, M., Hargrave, P.C., Savini, G., Gradziel, Marcin, Tynan, Niall, Trappe, Neil, Sørensen, S.B., Ade, P.A.R., Sudiwala, R., Walker, I.K., and van der Vorst, M.

Abstract

A comprehensive test programme has been implemented to enable the consideration of large refractive components with coating layers in the design of future satellite-based cosmic microwave background polarimetry missions. This requires understanding of systematic effects to an unprecedented level of precision, and validation of modelling tools and manufacturing techniques. We present the details of this study, and key results of the material and lens testing programme.

Published
2013

79. The SPICA-SAFARI Detector System: TES Detector Arrays with Frequency Division Multiplexed SQUID Readout

Author

Jackson, B.D., de Korte, P.A.J., van der Kuur, J., Mauskopf, P.D., Beyer, J., Bruijn, M.P., Cros, A., Gao, J.R., Griffin, D., den Hartog, R., Kiviranta, M., de Lange, G., van Leeuwen, B.-J., Macculi, C., Ravera, L., Trappe, Neil, van Weers, H., Withington, S., Jackson, B.D., de Korte, P.A.J., van der Kuur, J., Mauskopf, P.D., Beyer, J., Bruijn, M.P., Cros, A., Gao, J.R., Griffin, D., den Hartog, R., Kiviranta, M., de Lange, G., van Leeuwen, B.-J., Macculi, C., Ravera, L., Trappe, Neil, van Weers, H., and Withington, S.

Published
2012

80. Quasi-optical multiplexing using reflection phase gratings

Author

Lanigan, W., Trappe, Neil, Murphy, J. Anthony, Colgan, R., O'Sullivan, Créidhe, and Withington, Stafford

Subjects
Physics::Optics
Abstract

Heterodyne array receiver systems for both ground based and satellite telescope facilities are now becoming feasible for imaging in the submillimetre/terahertz regions of the EM spectrum. Phase gratings can be usefully employed as high efficiency passive multiplexing devices in the local oscillator (LO) injection chain of such receivers, ensuring that each element of the array is adequately biased and that the reflected LO power level at the array is minimised. For the wavelengths of interest both transmission and reflection gratings can be manufactured by milling an appropriate pattern of slots into the surface(s) of a suitable material. Thus, the required phase modulation is produced by the resulting pattern of varying optical path lengths suffered by the incident wave-front. We report on work we are undertaking to develop all reflection quasi-optical multiplexing systems so as to reduce reflection losses at the grating and minimise the number of surfaces that can contribute to standing wave effects in the optical system. As part of this endeavour we have also developed a quasi-optical technique for analysing the inevitable degradation due to multiple reflections on transmission grating design. This analysis is based on the Gaussian beam mode technique, and a further application of this technique allows one to assess tolerance limitations on the grating.

Published
2000

81. Herschel observations of EXtra-Ordinary Sources (HEXOS): Methanol as a probe of physical conditions in Orion KL

Author

Wang, S., Bergin, E.A., Crockett, N.R., Goldsmith, P.F., Lis, D.C., Pearson, J.C., Schilke, P., Bell, T.A., Comito, C., Blake, G.A., Caux, E., Ceccarelli, C., Cernicharo, J., Daniel, F., Dubernet, M.-L., Emprechtinger, M., Encrenaz, P., Gerin, M., Giesen, T.F., Goicoechea, J.R., Gupta, H., Herbst, E., Joblin, C., Johnstone, D., Langer, W.D., Latter, W.B., Lord, S.D., Maret, S., Martin, P.G., Melnick, G.J., Menten, K.M., Morris, P., Muller, H.S.P., Murphy, J.Anthony, Neufeld, D.A., Ossenkopf, V., Perault, M., Phillips , T.G., Plume, R., Qin, S.-L., Schlemmer, S., Stutzki, J., Trappe, Neil, van der Tak, F.F.S., Vastel, C., Yorke, H.W., Yu, S., Zmuidzinas, J., Wang, S., Bergin, E.A., Crockett, N.R., Goldsmith, P.F., Lis, D.C., Pearson, J.C., Schilke, P., Bell, T.A., Comito, C., Blake, G.A., Caux, E., Ceccarelli, C., Cernicharo, J., Daniel, F., Dubernet, M.-L., Emprechtinger, M., Encrenaz, P., Gerin, M., Giesen, T.F., Goicoechea, J.R., Gupta, H., Herbst, E., Joblin, C., Johnstone, D., Langer, W.D., Latter, W.B., Lord, S.D., Maret, S., Martin, P.G., Melnick, G.J., Menten, K.M., Morris, P., Muller, H.S.P., Murphy, J.Anthony, Neufeld, D.A., Ossenkopf, V., Perault, M., Phillips , T.G., Plume, R., Qin, S.-L., Schlemmer, S., Stutzki, J., Trappe, Neil, van der Tak, F.F.S., Vastel, C., Yorke, H.W., Yu, S., and Zmuidzinas, J.

Published
2011

82. Efficient design of THz security systems

Author

Tinkiel, Demien, White, David R., Trappe, Neil, Tinkiel, Demien, White, David R., and Trappe, Neil

Abstract

The Terahertz (THz) frequency band has traditionally been of interest for the past 30 years in astronomy. However, recent advancements in technology in this band have sparked interest in other applications such as security. The THz frequency band is specially suited to this task, given that it has the penetration aspects of higher frequencies without the harmful ionizing effects. Although the area of airport security systems has seen new developments in hardware and commercial products, it is still largely underdeveloped in terms of efficient software. There are two potential considerations for efficiency in this area: personal privacy and detection speed. Both are addressed in our research.

Published
2011

83. Optical requirements and modelling of coupling devices for the SAFARI instrument on SPICA

Author

Trappe, Neil, Gao, J.R., Glowacka, D.M., Goldie, D.J., Griffin, D., Khosropanah, P., Mauskopf, P.D., Morozov, Dmitry, Murphy, J.Anthony, O'Sullivan, Créidhe, Ridder, Marcel, Withington, Stafford, Trappe, Neil, Gao, J.R., Glowacka, D.M., Goldie, D.J., Griffin, D., Khosropanah, P., Mauskopf, P.D., Morozov, Dmitry, Murphy, J.Anthony, O'Sullivan, Créidhe, Ridder, Marcel, and Withington, Stafford

Abstract

The next generation of space missions targeting far-infrared bands will require large-format arrays of extremely low-noise detectors. The development of Transition Edge Sensors (TES) array technology seems to be a viable solution for future mm-wave to Far-Infrared (FIR) space applications where low noise and high sensitivity is required. In this paper we concentrate on a key element for a high sensitivity TES detector array, that of the optical coupling between the incoming electromagnetic field and the phonon system of the suspended membrane. An intermediate solution between free space coupling and a single moded horn is where over-moded light pipes are used to concentrate energy onto multi-moded absorbers. We present a comparison of modelling techniques to analyse the optical efficiency of such light pipes and their interaction with the front end optics and detector cavity.

Published
2011

84. Modal analysis of the quasi-optical performance of phase gratings

Author

Murphy, Anthony J., O'Sullivan, Créidhe, Trappe, Neil, Lanigan, William, Colgan, R., and Withington, Stafford

Subjects
Experimental Physics, Physics::Optics
Abstract

This paper is concerned with the analysis of phase gratings as passive quasi-optical multiplexing devices. One important application of such components is in the local oscillator injection chain of heterodyne array receivers. Gaussian beam mode analysis can be applied as a powerful tool when modelling the optical performance of phase gratings in a real submillimeter system of finite throughput and bandwidth. In our experimental investigations we have concentrated on the Dammann Grating (DG) which is a binary optical component and thus straightforward to manufacture. A number of quartz gratings were fabricated and carefully tested to evaluate the practical limitations of such quasi-optical components. Because of its convenient refractive index quartz can be used to produce gratings with very low reflection losses. The results presented confirm DGs to be particularly suitable multiplexers for sparse arrays of finite bandwidth.

Published
1999

85. Detection of interstellar oxidaniumyl: Abundant H2O+ towards the star-forming regions DR21, Sgr B2, and NGC6334

Author

Ossenkopf, V., Muller, H.S.P., Lis, D.C., Schilke, P., Bell, T.A., Bruderer, S., Bergin, E.A., Ceccarelli, C., Comito, C., Stutzki, J., Bacman, A., Baudry, A., Benz, A.O., Benedettini, M., Berne, O., Blake, G.A., Boogert, A., Bottinelli, S., Boulanger, F., Cabrit, S., Caselli, P., Caux, E., Cernicharo, J., Codella, C., Coutens, A., Crimier, N., Crockett, N.R., Daniel, F., Demyk, K., Dieleman, P., Dominik, C., Dubernet, M.-L., Emprechtinger, M., Encrenaz, P., Falgarone, E., France, K., Fuente, A., Gerin, M., Giesen, T.F., Di Giorgio, A.M., Goicoechea, J.R., Goldsmith, P.F., Gusten, R., Harris, A., Helmich, F., Herbst, E., Hily-Blant, P., Jacobs, K., Jacq, T., Joblin, Ch., Johnstone, D., Kahane, C., Kama, M., Klein, T., Klotz, A., Kramer, C., Langer, W., Lefloch, B., Leinz, C., Lorenzani, A., Lord, S.D., Maret, S., Martin, P.G., Martin-Pintado, J., McCoey, C., Melchior, M., Melnick, G.J., Menten, K.M., Mookerjea, B., Morris, P., Murphy, J.Anthony, Neufeld, D.A., Nisini, B., Pacheco, S., Pagini, L., Parise, B., Pearson, J.C., Perault, M., Phillips, T.G., Plume, R., Quin, S.-L., Rizzo, R., Rollig, M., Salez, M., Saraceno, P., Schlemmer, S., Simon, R., Schuster, K., van der Tak, F.F.S., Tielens, A.G.G.M., Teyssier, D., Trappe, Neil, Vastel, C., Viti, S., Wakelam, V., Walters, A., Wang, S., Whyborn, N., van der Wiel, M., Yorke, H.W., Yu, S., Zmuidzinas, J., Ossenkopf, V., Muller, H.S.P., Lis, D.C., Schilke, P., Bell, T.A., Bruderer, S., Bergin, E.A., Ceccarelli, C., Comito, C., Stutzki, J., Bacman, A., Baudry, A., Benz, A.O., Benedettini, M., Berne, O., Blake, G.A., Boogert, A., Bottinelli, S., Boulanger, F., Cabrit, S., Caselli, P., Caux, E., Cernicharo, J., Codella, C., Coutens, A., Crimier, N., Crockett, N.R., Daniel, F., Demyk, K., Dieleman, P., Dominik, C., Dubernet, M.-L., Emprechtinger, M., Encrenaz, P., Falgarone, E., France, K., Fuente, A., Gerin, M., Giesen, T.F., Di Giorgio, A.M., Goicoechea, J.R., Goldsmith, P.F., Gusten, R., Harris, A., Helmich, F., Herbst, E., Hily-Blant, P., Jacobs, K., Jacq, T., Joblin, Ch., Johnstone, D., Kahane, C., Kama, M., Klein, T., Klotz, A., Kramer, C., Langer, W., Lefloch, B., Leinz, C., Lorenzani, A., Lord, S.D., Maret, S., Martin, P.G., Martin-Pintado, J., McCoey, C., Melchior, M., Melnick, G.J., Menten, K.M., Mookerjea, B., Morris, P., Murphy, J.Anthony, Neufeld, D.A., Nisini, B., Pacheco, S., Pagini, L., Parise, B., Pearson, J.C., Perault, M., Phillips, T.G., Plume, R., Quin, S.-L., Rizzo, R., Rollig, M., Salez, M., Saraceno, P., Schlemmer, S., Simon, R., Schuster, K., van der Tak, F.F.S., Tielens, A.G.G.M., Teyssier, D., Trappe, Neil, Vastel, C., Viti, S., Wakelam, V., Walters, A., Wang, S., Whyborn, N., van der Wiel, M., Yorke, H.W., Yu, S., and Zmuidzinas, J.

Published
2010

86. Origin of the hot gas in low-mass protostars, Herschel-PACS spectroscopy of HH 46

Author

van Kempen, T.A., Kristensen, L.E., Herczeg, G.J., Visser, R., van Dishoeck, E.F., Wampfler, S.F., Bruderer, S., Benz, A.O., Doty, S.D., Brinch, C., Hogerheijde, M.R., Jorgensen, J.K., Tafalla, M., Neufeld, D., Bachiller, R., Baudry, A., Benedettini, M., Bergin, E.A., Bjerkeli, P., Blake, G.A., Bontemps, S., Braine, J., Caselli, P., Cernicharo, J., Codella, C., Daniel, F., Di Giorgio, A.M., Dominik, C., Encrenaz, P., Fich, M., Fuente, A., Giannini, T., Goicoechea, J.R., de Graauw, Th., Helmich, F., Herpin, F., Jacq, T., Johnstone, D., Kaufman, M.J., Larsson, B., Lis, D.C., Liseau, R., Marseille, M., McCoey, C., Melnick, G., Nisini, B., Olberg, M., Parise, B., Pearson, J.C., Plume, R., Risacher, C., Santiago-Garcia, J., Saraceno, P., Shipman, R., van der Tak, F.F.S., Wyrowski, F., Yildiz, U.A., Ciechanowicz, M., Dubbeldam, L., Glenz, S., Huisman, R., Lin, R.H., Morris, P., Murphy, J.Anthony, Trappe, Neil, van Kempen, T.A., Kristensen, L.E., Herczeg, G.J., Visser, R., van Dishoeck, E.F., Wampfler, S.F., Bruderer, S., Benz, A.O., Doty, S.D., Brinch, C., Hogerheijde, M.R., Jorgensen, J.K., Tafalla, M., Neufeld, D., Bachiller, R., Baudry, A., Benedettini, M., Bergin, E.A., Bjerkeli, P., Blake, G.A., Bontemps, S., Braine, J., Caselli, P., Cernicharo, J., Codella, C., Daniel, F., Di Giorgio, A.M., Dominik, C., Encrenaz, P., Fich, M., Fuente, A., Giannini, T., Goicoechea, J.R., de Graauw, Th., Helmich, F., Herpin, F., Jacq, T., Johnstone, D., Kaufman, M.J., Larsson, B., Lis, D.C., Liseau, R., Marseille, M., McCoey, C., Melnick, G., Nisini, B., Olberg, M., Parise, B., Pearson, J.C., Plume, R., Risacher, C., Santiago-Garcia, J., Saraceno, P., Shipman, R., van der Tak, F.F.S., Wyrowski, F., Yildiz, U.A., Ciechanowicz, M., Dubbeldam, L., Glenz, S., Huisman, R., Lin, R.H., Morris, P., Murphy, J.Anthony, and Trappe, Neil

Published
2010

87. A TES focal plane for SPICA-SAFARI

Author

Mauskopf, P.D., Ade, P.A.R., Beyer, J., Bruijn, M.P., Gao, J.R., Glowacka, D.M., Goldie, D.J., Griffin, D., Griffin, M., Hoevers, H.F.C., Khosropanah, P., Kooijma, P., de Korte, P.A.J., Morozov, Dmitry, Murphy, J.Anthony, O'Sullivan, Créidhe, Ridder, Marcel, Trappe, Neil, van Weers, H., van der Kuur, J., Withington, Stafford, Mauskopf, P.D., Ade, P.A.R., Beyer, J., Bruijn, M.P., Gao, J.R., Glowacka, D.M., Goldie, D.J., Griffin, D., Griffin, M., Hoevers, H.F.C., Khosropanah, P., Kooijma, P., de Korte, P.A.J., Morozov, Dmitry, Murphy, J.Anthony, O'Sullivan, Créidhe, Ridder, Marcel, Trappe, Neil, van Weers, H., van der Kuur, J., and Withington, Stafford

Published
2010

88. Calibration of the Herschel HIFI Instrument using Gas Cell Measurements

Author

Higgins, Daniel Ronan, Teyssier, D., Pearson, J.C., Risacher, C., Trappe, Neil, Higgins, Daniel Ronan, Teyssier, D., Pearson, J.C., Risacher, C., and Trappe, Neil

Abstract

The Heterodyne Instrument for the Far- Infrared (HIFI) was launched aboard the Herschel space telescope on the 14th of May 2009. HIFI’s frequency range is spread over 7 mixer bands. Bands 1-5 (480-1270 GHz) use Superconducting-Insulator- Superconducting (SIS) mixer technology while bands 6 & 7 (1410-1910 GHz) use Hot Electron Bolometer (HEB) mixer technology. HIFI is a double sideband instrument and hence contains both the upper and lower sideband of the down converted sky signal. The gain in the upper and lower sideband is not always equal. This effect introduces a calibration uncertainty that must be understood in order to achieve the HIFI calibration goal of 3%. To determine the frequency dependent sideband ratio for each mixer band, a gas cell test set up was developed [1]. During the instrument level testing a number of simple (12CO, 13CO and OCS) and complex (CH3CN and CH3OH) molecules were observed using the HIFI instrument. Using a radiative transfer model with the measured pressure and optical path length of the gas cell and molecular line parameters taken from the JPL and HITRAN catalogs, model spectra can be generated. By comparing the generated spectra with the observed spectra the sideband gain can be determined. In this paper we present the analysis of 12CO gas cell data in bands 1 & 2 and the application of the determined side gain ratios to flight data.

Published
2010

89. A modal approach to the modeling of rectangular detector horns and cavities at THz frequencies

Author

Doherty, Stephen, Trappe, Neil, O'Sullivan, Créidhe, Murphy, J.Anthony, Doherty, Stephen, Trappe, Neil, O'Sullivan, Créidhe, and Murphy, J.Anthony

Abstract

Far-IR space telescopes use horn antenna coupled bolometers for achieving high levels of sensitivity. Unfortunately at THz frequencies large cavity coupled horns prove significantly challenging to simulate accurately. This paper will outline alternative simulation concepts for such problems.

Published
2010

90. Herschel observations of EXtra-Ordinary Sources (HEXOS): detecting spiral arm clouds by CH absorption lines

Author

Qin, S.-L., Schilke, P., Comito, C., Moller, T., Rolff, R., Muller, H.S.P., Belloche, A., Menten, K.M., Lis, D.C., Phillips , T.G., Bergin, E.A., Bell, T.A., Crockett, N.R., Blake, G.A., Cabrit, S., Caux, E., Ceccarelli, C., Cernicharo, J., Daniel, F., Dubernet, M.-L., Emprechtinger, M., Encrenaz, P., Falgarone, E., Gerin, M., Giesen, T.F., Goicoechea, J.R., Goldsmith, P.F., Gupta, H., Herbst, E., Joblin, C., Johnstone, D., Langer, W.D., Lord, S.D., Maret, S., Martin, P.G., Melnick, G.J., Morris, P., Murphy, J.Anthony, Neufeld, D.A., Ossenkopf, V., Pagani, L., Pearson, J.C., Perault, M., Plume, R., Salez, M., Schlemmer, S., Stutzki, J., Trappe, Neil, van der Tak, F.F.S., Vastel, C., Wang, S., Yorke, H.W., Yu, S., Zmuidzinas, J., Boogert, A., Gusten, R., Hartogh, P., Honingh, E., Karpov, A., Kooi, J., Krieg, J.-M., Schieder, R., Diez-Gonzalez, M.C., Bachiller, R., Martin-Pintado, J., Baechtold, W., Olberg, M., Nordh, L.H., Gill, J.L., Chattopadhyay, G., Qin, S.-L., Schilke, P., Comito, C., Moller, T., Rolff, R., Muller, H.S.P., Belloche, A., Menten, K.M., Lis, D.C., Phillips , T.G., Bergin, E.A., Bell, T.A., Crockett, N.R., Blake, G.A., Cabrit, S., Caux, E., Ceccarelli, C., Cernicharo, J., Daniel, F., Dubernet, M.-L., Emprechtinger, M., Encrenaz, P., Falgarone, E., Gerin, M., Giesen, T.F., Goicoechea, J.R., Goldsmith, P.F., Gupta, H., Herbst, E., Joblin, C., Johnstone, D., Langer, W.D., Lord, S.D., Maret, S., Martin, P.G., Melnick, G.J., Morris, P., Murphy, J.Anthony, Neufeld, D.A., Ossenkopf, V., Pagani, L., Pearson, J.C., Perault, M., Plume, R., Salez, M., Schlemmer, S., Stutzki, J., Trappe, Neil, van der Tak, F.F.S., Vastel, C., Wang, S., Yorke, H.W., Yu, S., Zmuidzinas, J., Boogert, A., Gusten, R., Hartogh, P., Honingh, E., Karpov, A., Kooi, J., Krieg, J.-M., Schieder, R., Diez-Gonzalez, M.C., Bachiller, R., Martin-Pintado, J., Baechtold, W., Olberg, M., Nordh, L.H., Gill, J.L., and Chattopadhyay, G.

Abstract

We have observed CH absorption lines (J = 3/2, N = 1 ← J = 1/2, N = 1) against the continuum source Sgr B2(M) using the Herschel/HIFI instrument. With the high spectral resolution and wide velocity coverage provided by HIFI, 31 CH absorption features with different radial velocities and line widths are detected and identified. The narrower line width and lower column density clouds show “spiral arm” cloud characteristics, while the absorption component with the broadest line width and highest column density corresponds to the gas from the Sgr B2 envelope. The observations show that each “spiral arm” harbors multiple velocity components, indicating that the clouds are not uniform and that they have internal structure. This line-of-sight through almost the entire Galaxy offers unique possibilities to study the basic chemistry of simple molecules in diffuse clouds, as a variety of different cloud classes are sampled simultaneously. We find that the linear relationship between CH and H2 column densities found at lower AV by UV observations does not continue into the range of higher visual extinction. There, the curve flattens, which probably means that CH is depleted in the denser cores of these clouds.

Published
2010

91. Reversal of infall in SgrB2(M) revealed by Herschel/HIFI observations of HCN lines at THz frequencies

Author

Rolffs, R., Schilke, P., Comito, C., Bergin, E.A., van der Tak, F.F.S., Lis, D.C., Qin, S.-L., Menten, K.M., Gusten, R., Bell, T.A., Blake, G.A., Caux, E., Ceccarelli, C., Cernicharo, J., Crockett, N.R., Daniel, F., Dubernet, M.-L., Emprechtinger, M., Encrenaz, P., Gerin, M., Giesen, T.F., Goicoechea, J.R., Goldsmith, P.F., Gupta, H., Herbst, E., Joblin, C., Johnstone, D., Langer, W.D., Latter, W.D., Lord, S.D., Maret, S., Martin, P.G., Melnick, G.J., Morris, P., Muller, H.S.P., Murphy, J.Anthony, Ossenkopf, V., Pearson, J.C., Perault, M., Phillips , T.G., Plume, R., Schlemmer, S., Stutzki, J., Trappe, Neil, Vastel, C., Wang, S., Yorke, H.W., Yu, S., Zmuidzinas, J., Diez-Gonzalez, C., Bachiller, R., Martin-Pintado, J., Baechtold, W., Olberg, M., Nordh, L.H., Gill, J.J., Chattopadhyay, G., Rolffs, R., Schilke, P., Comito, C., Bergin, E.A., van der Tak, F.F.S., Lis, D.C., Qin, S.-L., Menten, K.M., Gusten, R., Bell, T.A., Blake, G.A., Caux, E., Ceccarelli, C., Cernicharo, J., Crockett, N.R., Daniel, F., Dubernet, M.-L., Emprechtinger, M., Encrenaz, P., Gerin, M., Giesen, T.F., Goicoechea, J.R., Goldsmith, P.F., Gupta, H., Herbst, E., Joblin, C., Johnstone, D., Langer, W.D., Latter, W.D., Lord, S.D., Maret, S., Martin, P.G., Melnick, G.J., Morris, P., Muller, H.S.P., Murphy, J.Anthony, Ossenkopf, V., Pearson, J.C., Perault, M., Phillips , T.G., Plume, R., Schlemmer, S., Stutzki, J., Trappe, Neil, Vastel, C., Wang, S., Yorke, H.W., Yu, S., Zmuidzinas, J., Diez-Gonzalez, C., Bachiller, R., Martin-Pintado, J., Baechtold, W., Olberg, M., Nordh, L.H., Gill, J.J., and Chattopadhyay, G.

Abstract

Aims. To investigate the accretion and feedback processes in massive star formation, we analyze the shapes of emission lines from hot molecular cores, whose asymmetries trace infall and expansion motions. Methods. The high-mass star forming region SgrB2(M) was observed with Herschel/HIFI (HEXOS key project) in various lines of HCN and its isotopologues, complemented by APEX data. The observations are compared to spherically symmetric, centrally heated models with density power-law gradient and different velocity fields (infall or infall+expansion), using the radiative transfer code RATRAN. Results. The HCN line profiles are asymmetric, with the emission peak shifting from blue to red with increasing J and decreasing line opacity (HCN to H13CN). This is most evident in the HCN 12–11 line at 1062 GHz. These line shapes are reproduced by a model whose velocity field changes from infall in the outer part to expansion in the inner part. Conclusions. The qualitative reproduction of the HCN lines suggests that infall dominates in the colder, outer regions, but expansion dominates in the warmer, inner regions. We are thus witnessing the onset of feedback in massive star formation, starting to reverse the infall and finally disrupting the whole molecular cloud. To obtain our result, the THz lines uniquely covered by HIFI were critically important.

Published
2010

92. Herschel observations of deuterated water towards Sgr B2(M)

Author

Comito, C., Schilke, P., Rolffs, R., Lis, D.C., Belloche, A., Bergin, E.A., Phillips , T.G., Bell, T.A., Crockett, N.R., Wang, S., Blake, G.A., Caux, E., Ceccarelli, C., Cernicharo, J., Daniel, F., Dubernet, M.-L., Emprechtinger, M., Encrenaz, P., Gerin, M., Giesen, T.F., Goicoechea, J.R., Goldsmith, P.F., Gupta, H., Herbst, E., Joblin, C., Johnstone, D., Langer, W.D., Latter, W.D., Lord, S.D., Maret, S., Martin, P.G., Melnick, G.J., Menten, K.M., Morris, P., Muller, H.S.P., Murphy, J.Anthony, Neufeld, D.A., Ossenkopf, V., Pearson, J.C., Perault, M., Plume, R., Qin, S.-L., Schlemmer, S., Stutzki, J., Trappe, Neil, van der Tak, F.F.S., Vastel, C., Yorke, H.W., Yu, S., Olberg, M., Szczerba, R., Larsson, B., Liseau, R., Lin, R.H., Samoska, L.A., Schlecht, E., Comito, C., Schilke, P., Rolffs, R., Lis, D.C., Belloche, A., Bergin, E.A., Phillips , T.G., Bell, T.A., Crockett, N.R., Wang, S., Blake, G.A., Caux, E., Ceccarelli, C., Cernicharo, J., Daniel, F., Dubernet, M.-L., Emprechtinger, M., Encrenaz, P., Gerin, M., Giesen, T.F., Goicoechea, J.R., Goldsmith, P.F., Gupta, H., Herbst, E., Joblin, C., Johnstone, D., Langer, W.D., Latter, W.D., Lord, S.D., Maret, S., Martin, P.G., Melnick, G.J., Menten, K.M., Morris, P., Muller, H.S.P., Murphy, J.Anthony, Neufeld, D.A., Ossenkopf, V., Pearson, J.C., Perault, M., Plume, R., Qin, S.-L., Schlemmer, S., Stutzki, J., Trappe, Neil, van der Tak, F.F.S., Vastel, C., Yorke, H.W., Yu, S., Olberg, M., Szczerba, R., Larsson, B., Liseau, R., Lin, R.H., Samoska, L.A., and Schlecht, E.

Abstract

Observations of HDO are an important complement for studies of water, because they give strong constraints on the formation processes – grain surfaces versus energetic process in the gas phase, e.g. in shocks. The HIFI observations of multiple transitions of HDO in Sgr B2(M) presented here allow the determination of the HDO abundance throughout the envelope, which has not been possible before with ground-based observations only. The abundance structure has been modeled with the spherical Monte Carlo radiative transfer code RATRAN, which also takes radiative pumping by continuum emission from dust into account. The modeling reveals that the abundance of HDO rises steeply with temperature from a low abundance (2.5 × 10−11) in the outer envelope at temperatures below 100 K through a medium abundance (1.5 × 10−9) in the inner envelope/outer core at temperatures between 100 and 200 K, and finally a high abundance ( 3.5 × 10−9) at temperatures above 200 K in the hot core.

Published
2010

93. Herschel/HIFI measurements of the ortho/para ratio in water towards Sagittarius B2(M) and W31C

Author

Lis, D.C., Phillips, T.G., Goldsmith, P.F., Neufeld, D.A., Herbst, E., Comito, C., Schilke, P., Muller, H.S.P., Bergin, E.A., Gerin, M., Bell, T.A., Emprechtinger, M., Black, J., Blake, G.A., Boulanger, F., Caux, E., Ceccarelli, C., Cernicharo, J., Coutens, A., Crockett, N.R., Daniel, F., Dartois, E., De Luca, M., Dubernet, M.-L., Encrenaz, P., Falgarone, E., Geballe, T.R., Godard, B., Giesen, T.F., Goicoechea, J.R., Gry, C., Gupta, H., Hennebelle, P., Hily-Blant, P., Kolos, R., Krelowski, J., Joblin, C., Johnstone, D., Kazmierczak, M., Lord, S.D., Maret, S., Martin, P.G., Martin-Pintado, J., Melnick, G.J., Menten, K.M., Monjel, R., Mookerjea, B., Morris, P., Murphy, J.Anthony, Ossenkopf, V., Pearson, J.C., Perault, M., Persson, C., Plume, R., Qin, S.-L., Salez, M., Schlemmer, S., Schmidt, M., Sonnentrucker, P., Stutzki, J., Teyssier, D., Trappe, Neil, van der Tak, F.F.S., Vastel, C., Wang, S., Yorke, H.W., Yu, S., Zmuidzinas, J., Boogert, A., Erickson, N., Karpov, A., Kooi, J., Maiwald, F.W., Schieder, R., Zaal, P., Lis, D.C., Phillips, T.G., Goldsmith, P.F., Neufeld, D.A., Herbst, E., Comito, C., Schilke, P., Muller, H.S.P., Bergin, E.A., Gerin, M., Bell, T.A., Emprechtinger, M., Black, J., Blake, G.A., Boulanger, F., Caux, E., Ceccarelli, C., Cernicharo, J., Coutens, A., Crockett, N.R., Daniel, F., Dartois, E., De Luca, M., Dubernet, M.-L., Encrenaz, P., Falgarone, E., Geballe, T.R., Godard, B., Giesen, T.F., Goicoechea, J.R., Gry, C., Gupta, H., Hennebelle, P., Hily-Blant, P., Kolos, R., Krelowski, J., Joblin, C., Johnstone, D., Kazmierczak, M., Lord, S.D., Maret, S., Martin, P.G., Martin-Pintado, J., Melnick, G.J., Menten, K.M., Monjel, R., Mookerjea, B., Morris, P., Murphy, J.Anthony, Ossenkopf, V., Pearson, J.C., Perault, M., Persson, C., Plume, R., Qin, S.-L., Salez, M., Schlemmer, S., Schmidt, M., Sonnentrucker, P., Stutzki, J., Teyssier, D., Trappe, Neil, van der Tak, F.F.S., Vastel, C., Wang, S., Yorke, H.W., Yu, S., Zmuidzinas, J., Boogert, A., Erickson, N., Karpov, A., Kooi, J., Maiwald, F.W., Schieder, R., and Zaal, P.

Abstract

We present Herschel/HIFI observations of the fundamental rotational transitions of ortho- and para-H16 2 O and H18 2 O in absorption towards Sagittarius B2(M) and W31C. The ortho/para ratio in water in the foreground clouds on the line of sight towards these bright continuum sources is generally consistent with the statistical high-temperature ratio of 3, within the observational uncertainties. However, somewhat unexpectedly, we derive a low ortho/para ratio of 2.35±0.35, corresponding to a spin temperature of ∼27 K, towards Sagittarius B2(M) at velocities of the expanding molecular ring. Water molecules in this region appear to have formed with, or relaxed to, an ortho/para ratio close to the value corresponding to the local temperature of the gas and dust.

Published
2010

94. Detection of OH+ and H2O+ towards Orion KL

Author

Gupta, H., Rimmer, P., Pearson, J.C., Yu, S., Herbst, E., Harada, N., Bergin, E.A., Neufeld, D.A., Melnick, G.J., Bachiller, R., Bell, T.A., Blake, G.A., Caux, E., Ceccarelli, C., Cernicharo, J., Chattopadhyay, G., Comito, C., Cabrit, S., Crockett, N.R., Daniel, F., Falgarone, E., Diez-Gonzalez, M.C., Dubernet, M.-L., Erickson, N., Emprechtinger, M., Encrenaz, P., Gerin, M., Gill, J.J., Giesen, T.F., Goicoechea, J.R., Goldsmith, P.F., Joblin, C., Johnstone, D., Langer, W.D., Larsson, B., Latter, W.B., Lin, R.J., Lis, D.C., Liseau, R., Lord, S.D., Maiwald, F.W., Maret, S., Martin, P.G., Martin-Pintado, J., Menten, K.M., Morris, P., Muller, H.S.P., Murphy, J.Anthony, Nordh, L.H., Olberg, M., Ossenkopf, V., Pagani, L., Perault, M., Phillips , T.G., Plume, R., Qin, S.-L., Salez, M., Samoska, L.A., Schilke, P., Schlecht, E., Schlemmer, S., Szczerba, R., Stutzki, J., Trappe, Neil, van der Tak, F.F.S., Vastel, C., Wang, S., Yorke, H.W., Zmuidzinas, J., Boogert, A., Gusten, R., Hartogh, P., Honigh, N., Karpov, A., Kooi, J., Krieg, J.-M., Schieder, R., Zaal, P., Gupta, H., Rimmer, P., Pearson, J.C., Yu, S., Herbst, E., Harada, N., Bergin, E.A., Neufeld, D.A., Melnick, G.J., Bachiller, R., Bell, T.A., Blake, G.A., Caux, E., Ceccarelli, C., Cernicharo, J., Chattopadhyay, G., Comito, C., Cabrit, S., Crockett, N.R., Daniel, F., Falgarone, E., Diez-Gonzalez, M.C., Dubernet, M.-L., Erickson, N., Emprechtinger, M., Encrenaz, P., Gerin, M., Gill, J.J., Giesen, T.F., Goicoechea, J.R., Goldsmith, P.F., Joblin, C., Johnstone, D., Langer, W.D., Larsson, B., Latter, W.B., Lin, R.J., Lis, D.C., Liseau, R., Lord, S.D., Maiwald, F.W., Maret, S., Martin, P.G., Martin-Pintado, J., Menten, K.M., Morris, P., Muller, H.S.P., Murphy, J.Anthony, Nordh, L.H., Olberg, M., Ossenkopf, V., Pagani, L., Perault, M., Phillips , T.G., Plume, R., Qin, S.-L., Salez, M., Samoska, L.A., Schilke, P., Schlecht, E., Schlemmer, S., Szczerba, R., Stutzki, J., Trappe, Neil, van der Tak, F.F.S., Vastel, C., Wang, S., Yorke, H.W., Zmuidzinas, J., Boogert, A., Gusten, R., Hartogh, P., Honigh, N., Karpov, A., Kooi, J., Krieg, J.-M., Schieder, R., and Zaal, P.

Abstract

We report observations of the reactive molecular ions OH+, H2O+, and H3O+ towards Orion KL with Herschel/HIFI. All three N = 1−0 finestructure transitions of OH+ at 909, 971, and 1033 GHz and both fine-structure components of the doublet ortho-H2O+ 111−000 transition at 1115 and 1139 GHz were detected; an upper limit was obtained for H3O+. OH+ and H2O+ are observed purely in absorption, showing a narrow component at the source velocity of 9 km s−1, and a broad blueshifted absorption similar to that reported recently for HF and para-H18 2 O, and attributed to the low velocity outflow of Orion KL.We estimate column densities of OH+ and H2O+ for the 9 kms−1 component of 9±3×1012 cm−2 and 7±2×1012 cm−2, and those in the outflow of 1.9±0.7×1013 cm−2 and 1.0±0.3×1013 cm−2. Upper limits of 2.4×1012 cm−2 and 8.7×1012 cm−2 were derived for the column densities of ortho and para-H3O+ from transitions near 985 and 1657 GHz. The column densities of the three ions are up to an order of magnitude lower than those obtained from recent observations ofW31C and W49N. The comparatively low column densities may be explained by a higher gas density despite the assumption of a very high ionization rate.

Published
2010

95. Herschel observations of EXtra-Ordinary Sources (HEXOS): The present and future of spectral surveys with Herschel/HIFI

Author

Bergin, E.A., Phillips , T.G., Comito, C., Crockett, N.R., Lis, D.C., Schilke, P., Wang, S., Bell, T.A., Blake, G.A., Bumble, B., Caux, E., Cabrit, S., Ceccarelli, C., Cernicharo, J., Daniel, F., de Graauw, Th., Dubernet, M.-L., Emprechtinger, M., Encrenaz, P., Falgarone, E., Gerin, M., Giesen, T.F., Goicoechea, J.R., Goldsmith, P.F., Gupta, H., Hartogh, P., Helmich, F.P., Herbst, E., Joblin, C., Johnstone, D., Kawamura, J.H., Langer, W.D., Latter, W.B., Lord, S.D., Maret, S., Martin, P.G., Melnick, G.J., Menten, K.M., Morris, P., Muller, H.S.P., Murphy, J.Anthony, Neufeld, D.A., Ossenkopf, V., Pagani, L., Pearson, J.C., Perault, M., Plume, R., Qin, S.-L., Roelfsema, P., Salez, M., Schlemmer, S., Stutzki, J., Tielens, A.G.G.M., Trappe, Neil, van der Tak, F.F.S., Vastel, C., Yorke, H.W., Yu, S., Zmuidzinas, J., Bergin, E.A., Phillips , T.G., Comito, C., Crockett, N.R., Lis, D.C., Schilke, P., Wang, S., Bell, T.A., Blake, G.A., Bumble, B., Caux, E., Cabrit, S., Ceccarelli, C., Cernicharo, J., Daniel, F., de Graauw, Th., Dubernet, M.-L., Emprechtinger, M., Encrenaz, P., Falgarone, E., Gerin, M., Giesen, T.F., Goicoechea, J.R., Goldsmith, P.F., Gupta, H., Hartogh, P., Helmich, F.P., Herbst, E., Joblin, C., Johnstone, D., Kawamura, J.H., Langer, W.D., Latter, W.B., Lord, S.D., Maret, S., Martin, P.G., Melnick, G.J., Menten, K.M., Morris, P., Muller, H.S.P., Murphy, J.Anthony, Neufeld, D.A., Ossenkopf, V., Pagani, L., Pearson, J.C., Perault, M., Plume, R., Qin, S.-L., Roelfsema, P., Salez, M., Schlemmer, S., Stutzki, J., Tielens, A.G.G.M., Trappe, Neil, van der Tak, F.F.S., Vastel, C., Yorke, H.W., Yu, S., and Zmuidzinas, J.

Abstract

We present initial results from the Herschel GT key program: Herschel observations of EXtra-Ordinary Sources (HEXOS) and outline the promise and potential of spectral surveys with Herschel/HIFI. The HIFI instrument offers unprecedented sensitivity, as well as continuous spectral coverage across the gaps imposed by the atmosphere, opening up a largely unexplored wavelength regime to high-resolution spectroscopy. We show the spectrum of Orion KL between 480 and 560 GHz and from 1.06 to 1.115 THz. From these data, we confirm that HIFI separately measures the dust continuum and spectrally resolves emission lines in Orion KL. Based on this capability we demonstrate that the line contribution to the broad-band continuum in this molecule-rich source is ∼20−40% below 1 THz and declines to a few percent at higher frequencies. We also tentatively identify multiple transitions of HD18O in the spectra. The first detection of this rare isotopologue in the interstellar medium suggests that HDO emission is optically thick in the Orion hot core with HDO/H2O ∼ 0.02. We discuss the implications of this detection for the water D/H ratio in hot cores.

Published
2010

96. Herschel/HIFI discovery of interstellar chloronium (H2Cl+)

Author

Lis, D.C., Pearson, J.C., Neufeld, D.A., Schilke, P., Muller, H.S.P., Gupta, H., Bell, T.A., Comito, C., Phillips , T.G., Bergin, E.A., Ceccarelli, C., Goldsmith, P.F., Blake, G.A., Bacmann, A., Baudry, A., Benedettini, M., Benz, A.O., Black, J., Boogert, A., Bottinelli, S., Cabrit, S., Caselli, P., Castets, A., Caux, E., Cernicharo, J., Codella, C., Coutens, A., Crimier, N., Crockett, N.R., Daniel, F., Demyk, K., Dominic, C., Dubernet, M.-L., Emprechtinger, M., Encrenaz, P., Falgarone, E., Fuente, A., Gerin, M., Giesen, T.F., Goicoechea, J.R., Helmich, F., Hennebelle, P., Henning, Th., Herbst, E., Hily-Blant, P., Hjalmarson, A., Hollenbach, D., Jack, T., Joblin, C., Johnstone, D., Kahane, C., Kama, M., Kaufman, M., Klotz, A., Langer, W.D., Larsson, B., Le Bourlot, J., Lefloch, B., Le Petit, F., Li, D., Liseau, R., Lord, S.D., Lorenzani, A., Maret, S., Martin, P.G., Melnick, G.J., Menten, K.M., Morris, P., Murphy, J.Anthony, Nagy, Z., Nisini, B., Ossenkopf, V., Pacheco, S., Pagani, L., Parise, B., Perault, M., Plume, R., Qin, S.-L., Roueff, E., Salez, M., Sandqvist, A., Saraceno, P., Schlemmer, S., Schuster, K., Snell, R., Stutzki, J., Tielens, A., Trappe, Neil, van der Tak, F.F.S., van der Wiel, M., van Dishoeck, E.F., Vastel, C., Viti, S., Wakelam, V., Walters, A., Wang, S., Wyrowski, F., Yorke, H.W., Yu, S., Zmuidzinas, J., Delorme, Y., Desbat, J.-P., Gustens, R., Krieg, J.-M., Delforge, B., Lis, D.C., Pearson, J.C., Neufeld, D.A., Schilke, P., Muller, H.S.P., Gupta, H., Bell, T.A., Comito, C., Phillips , T.G., Bergin, E.A., Ceccarelli, C., Goldsmith, P.F., Blake, G.A., Bacmann, A., Baudry, A., Benedettini, M., Benz, A.O., Black, J., Boogert, A., Bottinelli, S., Cabrit, S., Caselli, P., Castets, A., Caux, E., Cernicharo, J., Codella, C., Coutens, A., Crimier, N., Crockett, N.R., Daniel, F., Demyk, K., Dominic, C., Dubernet, M.-L., Emprechtinger, M., Encrenaz, P., Falgarone, E., Fuente, A., Gerin, M., Giesen, T.F., Goicoechea, J.R., Helmich, F., Hennebelle, P., Henning, Th., Herbst, E., Hily-Blant, P., Hjalmarson, A., Hollenbach, D., Jack, T., Joblin, C., Johnstone, D., Kahane, C., Kama, M., Kaufman, M., Klotz, A., Langer, W.D., Larsson, B., Le Bourlot, J., Lefloch, B., Le Petit, F., Li, D., Liseau, R., Lord, S.D., Lorenzani, A., Maret, S., Martin, P.G., Melnick, G.J., Menten, K.M., Morris, P., Murphy, J.Anthony, Nagy, Z., Nisini, B., Ossenkopf, V., Pacheco, S., Pagani, L., Parise, B., Perault, M., Plume, R., Qin, S.-L., Roueff, E., Salez, M., Sandqvist, A., Saraceno, P., Schlemmer, S., Schuster, K., Snell, R., Stutzki, J., Tielens, A., Trappe, Neil, van der Tak, F.F.S., van der Wiel, M., van Dishoeck, E.F., Vastel, C., Viti, S., Wakelam, V., Walters, A., Wang, S., Wyrowski, F., Yorke, H.W., Yu, S., Zmuidzinas, J., Delorme, Y., Desbat, J.-P., Gustens, R., Krieg, J.-M., and Delforge, B.

Abstract

We report the first detection of chloronium, H2Cl+, in the interstellar medium, using the HIFI instrument aboard the Herschel Space Observatory. The 212−101 lines of ortho-H35 2 Cl+ and ortho-H37 2 Cl+ are detected in absorption towards NGC 6334I, and the 111−000 transition of para-H35 2 Cl+ is detected in absorption towards NGC 6334I and Sgr B2(S). The H2Cl+ column densities are compared to those of the chemically-related species HCl. The derived HCl/H2Cl+ column density ratios, ∼1–10, are within the range predicted by models of diffuse and dense photon dominated regions (PDRs). However, the observed H2Cl+ column densities, in excess of 1013 cm−2, are significantly higher than the model predictions. Our observations demonstrate the outstanding spectroscopic capabilities of HIFI for detecting new interstellar molecules and providing key constraints for astrochemical models.

Published
2010

97. Herschel observations of ortho- and para-oxidaniumyl (H2O+) in spiral arm clouds toward Sagittarius B2(M)

Author

Schilke, P., Comito, C., Muller, H.S.P., Bergin, E.A., Herbst, E., Lis, D.C., Neufeld, D.A., Phillips , T.G., Bell, T.A., Blake, G.A., Cabrit, S., Caux, E., Ceccarelli, C., Cernicharo, J., Crockett, N.R., Daniel, F., Dubernet, M.-L., Emprechtinger, M., Encrenaz, P., Falgarone, E., Gerin, M., Giesen, T.F., Goicoechea, J.R., Goldsmith, P.F., Gupta, H., Joblin, C., Johnstone, D., Langer, W.D., Latter, W.B., Lord, S.D., Maret, S., Martin, P.G., Melnick, G.J., Menten, K.M., Morris, P., Murphy, J.Anthony, Ossenkopf, V., Pagini, L., Pearson, J.C., Perault, M., Plume, R., Qin, S.-L., Salez, M., Schlemmer, S., Stutzki, J., Trappe, Neil, van der Tak, F.F.S., Vastel, C., Wang, S., Yorke, H.W., Yu, S., Erickson, N., Maiwald, F.W., Kooi, J., Karpov, A., Zmuidzinas, J., Boogert, A., Schieder, R., Zaal, P., Schilke, P., Comito, C., Muller, H.S.P., Bergin, E.A., Herbst, E., Lis, D.C., Neufeld, D.A., Phillips , T.G., Bell, T.A., Blake, G.A., Cabrit, S., Caux, E., Ceccarelli, C., Cernicharo, J., Crockett, N.R., Daniel, F., Dubernet, M.-L., Emprechtinger, M., Encrenaz, P., Falgarone, E., Gerin, M., Giesen, T.F., Goicoechea, J.R., Goldsmith, P.F., Gupta, H., Joblin, C., Johnstone, D., Langer, W.D., Latter, W.B., Lord, S.D., Maret, S., Martin, P.G., Melnick, G.J., Menten, K.M., Morris, P., Murphy, J.Anthony, Ossenkopf, V., Pagini, L., Pearson, J.C., Perault, M., Plume, R., Qin, S.-L., Salez, M., Schlemmer, S., Stutzki, J., Trappe, Neil, van der Tak, F.F.S., Vastel, C., Wang, S., Yorke, H.W., Yu, S., Erickson, N., Maiwald, F.W., Kooi, J., Karpov, A., Zmuidzinas, J., Boogert, A., Schieder, R., and Zaal, P.

Abstract

H2O+ has been observed in its ortho- and para- states toward the massive star forming core Sgr B2(M), located close to the Galactic center. The observations show absorption in all spiral arm clouds between the Sun and Sgr B2. The average o/p ratio of H2O+ in most velocity intervals is 4.8, which corresponds to a nuclear spin temperature of 21 K. The relationship of this spin temperature to the formation temperature and current physical temperature of the gas hosting H2O+ is discussed, but no firm conclusion is reached. In the velocity interval 0–60 km s−1, an ortho/para ratio of below unity is found, but if this is due to an artifact of contamination by other species or real is not clear.

Published
2010

98. Herschel observations of EXtra-Ordinary Sources (HEXOS): Observations of H2O and its isotopologues towards Orion KL

Author

Melnick, G.J., Tolls, V., Neufeld, D.A., Bergin, E.A., Phillips , T.G., Wang, S., Crockett, N.R., Bell, T.A., Blake, G.A., Cabrit, S., Caux, E., Ceccarelli, C., Cernicharo, J., Comito, C., Daniel, F., Dubernet, M.-L., Emprechtinger, M., Encrenaz, P., Falgarone, E., Gerin, M., Giesen, T.F., Goicoechea, J.R., Goldsmith, P.F., Herbst, E., Joblin, C., Johnstone, D., Langer, W.D., Latter, W.D., Lis, D.C., Lord, S.D., Maret, S., Martin, P.G., Menten, K.M., Morris, P., Muller, H.S.P., Murphy, J.Anthony, Ossenkopf, V., Pagani, L., Pearson, J.C., Perault, M., Plume, R., Qin, S.-L., Salez, M., Schilke, P., Schlemmer, S., Stutzki, J., Trappe, Neil, van der Tak, F.F.S., Vastel, C., Yorke, H.W., Yu, S., Zmuidzinas, J., Melnick, G.J., Tolls, V., Neufeld, D.A., Bergin, E.A., Phillips , T.G., Wang, S., Crockett, N.R., Bell, T.A., Blake, G.A., Cabrit, S., Caux, E., Ceccarelli, C., Cernicharo, J., Comito, C., Daniel, F., Dubernet, M.-L., Emprechtinger, M., Encrenaz, P., Falgarone, E., Gerin, M., Giesen, T.F., Goicoechea, J.R., Goldsmith, P.F., Herbst, E., Joblin, C., Johnstone, D., Langer, W.D., Latter, W.D., Lis, D.C., Lord, S.D., Maret, S., Martin, P.G., Menten, K.M., Morris, P., Muller, H.S.P., Murphy, J.Anthony, Ossenkopf, V., Pagani, L., Pearson, J.C., Perault, M., Plume, R., Qin, S.-L., Salez, M., Schilke, P., Schlemmer, S., Stutzki, J., Trappe, Neil, van der Tak, F.F.S., Vastel, C., Yorke, H.W., Yu, S., and Zmuidzinas, J.

Abstract

We report the detection of more than 48 velocity-resolved ground rotational state transitions of H 16 2 O, H 18 2 O, and H 17 2 O – most for the first time – in both emission and absorption toward Orion KL using Herschel/HIFI. We show that a simple fit, constrained to match the known emission and absorption components along the line of sight, is in excellent agreement with the spectral profiles of all the water lines. Using the measured H 18 2 O line fluxes, which are less affected by line opacity than their H 16 2 O counterparts, and an escape probability method, the column densities of H 18 2 O associated with each emission component are derived. We infer total water abundances of 7.4 × 10−5, 1.0× 10−5, and 1.6 × 10−5 for the plateau, hot core, and extended warm gas, respectively. In the case of the plateau, this value is consistent with previous measures of the Orion-KL water abundance as well as those of other molecular outflows. In the case of the hot core and extended warm gas, these values are somewhat higher than water abundances derived for other quiescent clouds, suggesting that these regions are likely experiencing enhanced water-ice sublimation from (and reduced freeze-out onto) grain surfaces due to the warmer dust in these sources.

Published
2010

99. Herschel observations of EXtra-Ordinary Sources (HEXOS): The Terahertz spectrum of Orion KL seen at high spectral resolution

Author

Crockett, N.R., Bergin, E.A., Wang, S., Lis, D.C., Bell, T.A., Blake, G.A., Boogert, A., Bumble, B., Cabrit, S., Caux, E., Ceccarelli, C., Cernicharo, J., Comito, C., Daniel, F., Dubernet, M.-L., Emprechtinger, M., Encrenaz, P., Falgarone, E., Gerin, M., Giesen, T.F., Goicoechea, J.R., Goldsmith, P.F., Gupta, H., Gusten, R., Hartogh, P., Helmich, F., Herbst, E., Honingh, E., Joblin, C., Johnstone, D., Karpov, A., Kawamura, J., Kooi, J., Krieg, J.-M., Langer, W., Latter, W.B., Lord, S.D., Maret, S., Martin, P.G., Melnick, G.J., Menten, K.M., Morris, P., Muller, H.S.P., Murphy, J.Anthony, Neufeld, D.A., Ossenkopf, V., Pearson, J.C., Perault, M., Phillips , T.G., Plume, R., Qin, S.-L., Roelfsema, P.R., Schieder, R., Schilke, P., Schlemmer, S., Stutzki, J., van der Tak, F.F.S., Tielens, A., Trappe, Neil, Vastel, C., Yorke, H.W., Yu, S., Zmuidzinas, J., Crockett, N.R., Bergin, E.A., Wang, S., Lis, D.C., Bell, T.A., Blake, G.A., Boogert, A., Bumble, B., Cabrit, S., Caux, E., Ceccarelli, C., Cernicharo, J., Comito, C., Daniel, F., Dubernet, M.-L., Emprechtinger, M., Encrenaz, P., Falgarone, E., Gerin, M., Giesen, T.F., Goicoechea, J.R., Goldsmith, P.F., Gupta, H., Gusten, R., Hartogh, P., Helmich, F., Herbst, E., Honingh, E., Joblin, C., Johnstone, D., Karpov, A., Kawamura, J., Kooi, J., Krieg, J.-M., Langer, W., Latter, W.B., Lord, S.D., Maret, S., Martin, P.G., Melnick, G.J., Menten, K.M., Morris, P., Muller, H.S.P., Murphy, J.Anthony, Neufeld, D.A., Ossenkopf, V., Pearson, J.C., Perault, M., Phillips , T.G., Plume, R., Qin, S.-L., Roelfsema, P.R., Schieder, R., Schilke, P., Schlemmer, S., Stutzki, J., van der Tak, F.F.S., Tielens, A., Trappe, Neil, Vastel, C., Yorke, H.W., Yu, S., and Zmuidzinas, J.

Abstract

We present the first high spectral resolution observations of Orion KL in the frequency ranges 1573.4–1702.8 GHz (band 6b) and 1788.4–1906.8 GHz (band 7b) obtained using the HIFI instrument on board the Herschel Space Observatory. We characterize the main emission lines found in the spectrum, which primarily arise from a range of components associated with Orion KL including the hot core, but also see widespread emission from components associated with molecular outflows traced by H2O, SO2, and OH. We find that the density of observed emission lines is significantly diminished in these bands compared to lower frequency Herschel/HIFI bands.

Published
2010

100. The Herschel-Heterodyne Instrument for the Far-Infrared (HIFI)

Author

de Graauw, Th., Helmich, F.P., Phillips , T.G., Stutzki, J., Caux, E., Whyborn, N.D., Dieleman, P., Roelfsema, P.R., Aarts, H., Assendorp, R., Bachiller, R., Baechtold, W., Barcia, A., Beintema, D.A., Belitsky, V., Benz, A.O., Bieber, R., Boogert, A., Borys, C., Bumble, B., Cais, P., Caris, M., Cerulli-Irelli, P., Chattopadhyay, G., Cherednichenko, S., Ciechanowicz, M., Coeur-Joly, O., Comito, C., Cros, A., de Jonge, A., de Lange, G., Delforges, B., Delorme, Y., den Boggende, T., Desbat, J.-M., Diez-Gonzalez, C., Di Giorgio, A.M., Dubbeldam, L., Edwards, K., Eggens, M., Erickson, N., Evers, J., Fich, M., Finn, T., Franke, B., Gaier, T., Gal, C., Gao, J.R., Gallego, J.-D., Gauffre, S., Gill, J.J., Glenz, S., Golstein, H., Goulooze, H., Gunsing, T., Gusten, R., Hartogh, P., Hatch, W.A., Higgins, R., Honingh, E.C., Huisman, R., Jackson, B.D., Jacobs, H., Jacobs, K., Jarchow, C., Javadi, H., Jellema, W., Justen, M., Karpov, A., Kasemann, C., Kawamura, J., Keizer, G., Kester, D., Klapwijk, T.M., Klein, Th., Kollberg, E., Kooi, J., Kooiman, P.-P., Kopf, B., Krause, M., Krieg, J.-M., Kramer, C., Kruizenga, B., Kuhn, T., Laauwen, W., Lai, R., Larsson, B., Leduc, H.G., Leinz, C., Lin, R.H., Liseau, R., Liu, G.S., Loose, A., Lopez-Fernandez, I., Lord, S., Luinge, W., Marston, A., Martin-Pintado, J., Maestrini, A., Maiwald, F.W., McCoey, C., Mehdi, I., Megej, A., Melchior, M., Meinsma, L., Merkel, H., Michalska, M., Monstein, C., Moratschke, D., Morris, P., Muller, H., Murphy, J.Anthony, Naber, A., Natale, E., Nowosielski, W., Nuzzolo, F., Olberg, M., Olbrich, M., Orfei, R., Orleanski, P., Ossenkopf, V., Peacock, T., Pearson, J.C., Peron, I., Phillip-May, S., Piazzo, L., Planesas, P., Rataj, M., Ravera, L., Risacher, C., Salez, M., Samoska, L.A., Saraceno, P., Schieder, R., Schlecht, E., Schloder, F., Schmulling, F., Schultz, M., Schuster, K., Siebertz, O., Smit, H., Szczerba, R., Shipman, R., Steinmetz, E., Stern, J.A., Stokroos, M., Teipen, R., Teyssier, D., Tils, T., Trappe, Neil, van Baaren, C., van Leeuwen, B.-J., van de Stadt, H., Visser, H., Wildeman, K.J., Wafelbakker, C.K., Ward, J.S., Wesselius, P., Wild, W., Wulff, S., Wunsch, H.-J., Tielens, X., Zaal, P., Zirath, H., Zmuidzinas, J., Zwart, F., de Graauw, Th., Helmich, F.P., Phillips , T.G., Stutzki, J., Caux, E., Whyborn, N.D., Dieleman, P., Roelfsema, P.R., Aarts, H., Assendorp, R., Bachiller, R., Baechtold, W., Barcia, A., Beintema, D.A., Belitsky, V., Benz, A.O., Bieber, R., Boogert, A., Borys, C., Bumble, B., Cais, P., Caris, M., Cerulli-Irelli, P., Chattopadhyay, G., Cherednichenko, S., Ciechanowicz, M., Coeur-Joly, O., Comito, C., Cros, A., de Jonge, A., de Lange, G., Delforges, B., Delorme, Y., den Boggende, T., Desbat, J.-M., Diez-Gonzalez, C., Di Giorgio, A.M., Dubbeldam, L., Edwards, K., Eggens, M., Erickson, N., Evers, J., Fich, M., Finn, T., Franke, B., Gaier, T., Gal, C., Gao, J.R., Gallego, J.-D., Gauffre, S., Gill, J.J., Glenz, S., Golstein, H., Goulooze, H., Gunsing, T., Gusten, R., Hartogh, P., Hatch, W.A., Higgins, R., Honingh, E.C., Huisman, R., Jackson, B.D., Jacobs, H., Jacobs, K., Jarchow, C., Javadi, H., Jellema, W., Justen, M., Karpov, A., Kasemann, C., Kawamura, J., Keizer, G., Kester, D., Klapwijk, T.M., Klein, Th., Kollberg, E., Kooi, J., Kooiman, P.-P., Kopf, B., Krause, M., Krieg, J.-M., Kramer, C., Kruizenga, B., Kuhn, T., Laauwen, W., Lai, R., Larsson, B., Leduc, H.G., Leinz, C., Lin, R.H., Liseau, R., Liu, G.S., Loose, A., Lopez-Fernandez, I., Lord, S., Luinge, W., Marston, A., Martin-Pintado, J., Maestrini, A., Maiwald, F.W., McCoey, C., Mehdi, I., Megej, A., Melchior, M., Meinsma, L., Merkel, H., Michalska, M., Monstein, C., Moratschke, D., Morris, P., Muller, H., Murphy, J.Anthony, Naber, A., Natale, E., Nowosielski, W., Nuzzolo, F., Olberg, M., Olbrich, M., Orfei, R., Orleanski, P., Ossenkopf, V., Peacock, T., Pearson, J.C., Peron, I., Phillip-May, S., Piazzo, L., Planesas, P., Rataj, M., Ravera, L., Risacher, C., Salez, M., Samoska, L.A., Saraceno, P., Schieder, R., Schlecht, E., Schloder, F., Schmulling, F., Schultz, M., Schuster, K., Siebertz, O., Smit, H., Szczerba, R., Shipman, R., Steinmetz, E., Stern, J.A., Stokroos, M., Teipen, R., Teyssier, D., Tils, T., Trappe, Neil, van Baaren, C., van Leeuwen, B.-J., van de Stadt, H., Visser, H., Wildeman, K.J., Wafelbakker, C.K., Ward, J.S., Wesselius, P., Wild, W., Wulff, S., Wunsch, H.-J., Tielens, X., Zaal, P., Zirath, H., Zmuidzinas, J., and Zwart, F.

Abstract

Aims. This paper describes the Heterodyne Instrument for the Far-Infrared (HIFI) that was launched onboard ESA’s Herschel Space Observatory in May 2009. Methods. The instrument is a set of 7 heterodyne receivers that are electronically tuneable, covering 480−1250 GHz with SIS mixers and the 1410−1910 GHz range with hot electron bolometer (HEB) mixers. The local oscillator (LO) subsystem comprises a Ka-band synthesizer followed by 14 chains of frequency multipliers and 2 chains for each frequency band. A pair of auto-correlators and a pair of acousto-optical spectrometers process the two IF signals from the dual-polarization, single-pixel front-ends to provide instantaneous frequency coverage of 2 × 4 GHz, with a set of resolutions (125 kHz to 1 MHz) that are better than 0.1 kms−1. Results. After a successful qualification and a pre-launch TB/TV test program, the flight instrument is now in-orbit and completed successfully the commissioning and performance verification phase. The in-orbit performance of the receivers matches the pre-launch sensitivities. We also report on the in-orbit performance of the receivers and some first results of HIFI’s operations.

Published
2010

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