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1. SPIRE Point Source Catalog Explanatory Supplement

Author: Schulz, Bernhard, Marton, Gábor, Valtchanov, Ivan, García, Ana María Pérez, Pintér, Sándor, Appleton, Phil, Kiss, Csaba, Lim, Tanya, Lu, Nanyao, Papageorgiou, Andreas, Pearson, Chris, Rector, John, Portal, Miguel Sánchez, Shupe, David, Tóth, Viktor L., Van Dyk, Schuyler, Varga-Verebélyi, Erika, and Xu, Kevin
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The Spectral and Photometric Imaging Receiver (SPIRE) was launched as one of the scientific instruments on board of the space observatory Herschel. The SPIRE photometer opened up an entirely new window in the Submillimeter domain for large scale mapping, that up to then was very difficult to observe. There are already several catalogs that were produced by individual Herschel science projects. Yet, we estimate that the objects of only a fraction of these maps will ever be systematically extracted and published by the science teams that originally proposed the observations. The SPIRE instrument performed its standard photometric observations in an optically very stable configuration, only moving the telescope across the sky, with variations in its configuration parameters limited to scan speed and sampling rate. This and the scarcity of features in the data that require special processing steps made this dataset very attractive for producing an expert reduced catalog of point sources that is being described in this document. The Catalog was extracted from a total of 6878 unmodified SPIRE scan map observations. The photometry was obtained by a systematic and homogeneous source extraction procedure, followed by a rigorous quality check that emphasized reliability over completeness. Having to exclude regions affected by strong Galactic emission, that pushed the limits of the four source extraction methods that were used, this catalog is aimed primarily at the extragalactic community. The result can serve as a pathfinder for ALMA and other Submillimeter and Far-Infrared facilities. 1,693,718 sources are included in the final catalog, splitting into 950688, 524734, 218296 objects for the 250\mu m, 350\mu m, and 500\mu m bands, respectively. The catalog comes with well characterized environments, reliability, completeness, and accuracies, that single programs typically cannot provide.
Published: 2017

2. The Herschel Point Source Catalogue

Author: Marton, Gábor, Schulz, Bernhard, Altieri, Bruno, Calzoletti, Luca, Kiss, Csaba, Lim, Tanya, Lu, Nanyao, Paladini, Roberta, Papageorgiou, Andreas, Pearson, Chris, Rector, John, Shupe, David, Valtchanov, Ivan, Varga-Verebélyi, Erika, and Xu, Kevin
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The Herschel Space Observatory was the fourth cornerstone mission in the European Space Agency (ESA) science programme with excellent broad band imaging capabilities in the sub-mm and far-infrared part of the spectrum. Although the spacecraft finished its observations in 2013, it left a large legacy dataset that is far from having been fully scrutinised and still has a large potential for new scientific discoveries. This is specifically true for the photometric observations of the PACS and SPIRE instruments. Some source catalogues have already been produced by individual observing programs, but there are many observations that risk to remain unexplored. To maximise the science return of the SPIRE and PACS data sets, we are in the process of building the Herschel Point Source Catalogue (HPSC) from all primary and parallel mode observations. Our homogeneous source extraction enables a systematic and unbiased comparison of sensitivity across the different Herschel fields that single programs will generally not be able to provide. The catalogue will be made available online through archives like the Herschel Science Archive (HSA), the Infrared Science Archive (IRSA), and the Strasbourg Astronomical Data Center (CDS)., Comment: 2 pages, 1 figure
Published: 2015
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3. The Mid-Infrared Instrument for JWST, II: Design and Build

Author: Wright, G. S., Wright, David, Goodson, G. B., Rieke, G. H., Aitink-Kroes, Gabby, Amiaux, J., Aricha-Yanguas, Ana, Azzolini, Ruyman, Banks, Kimberly, Barrado-Navascues, D., Belenguer-Davila, T., Bloemmart, J. A. D. L., Bouchet, Patrice, Brandl, B. R., Colina, L., Detre, Ors, Diaz-Catala, Eva, Eccleston, Paul, Friedman, Scott D., Garcia-Marin, Macarena, Guedel, Manuel, Glasse, Alistair, Glauser, Adrian M., Greene, T. P., Groezinger, Uli, Grundy, Tim, Hastings, Peter, Henning, Th., Hofferbert, Ralph, Hunter, Faye, Jessen, N. C., Justtanont, K., Karnik, Avinash R., Khorrami, Mori A., Krause, Oliver, Labiano, Alvaro, Lagage, P. -O., Langer, Ulrich, Lemke, Dietrich, Lim, Tanya, Lorenzo-Alvarez, Jose, Mazy, Emmanuel, McGowan, Norman, Meixner, M. E., Morris, Nigel, Morrison, Jane E., Mueller, Friedrich, Norgaard-Nielson, H. -U., Olofsson, Goeran, O'Sullivan, Brian, Pel, J. -W., Penanen, Konstantin, Petach, M. B., Pye, J. P., Ray, T. P., Renotte, Etienne, Renouf, Ian, Ressler, M. E., Samara-Ratna, Piyal, Scheithauer, Silvia, Schneider, Analyn, Shaughnessy, Bryan, Stevenson, Tim, Sukhatme, Kalyani, Swinyard, Bruce, Sykes, Jon, Thatcher, John, Tikkanen, Tuomo, van Dishoeck, E. F., Waelkens, C., Walker, Helen, Wells, Martyn, and Zhender, Alex
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The Mid-InfraRed Instrument (MIRI) on the James Webb Space Telescope (JWST) provides measurements over the wavelength range 5 to 28.5 microns. MIRI has, within a single 'package', four key scientific functions: photometric imaging, coronagraphy, single-source low-spectral resolving power (R ~ 100) spectroscopy, and medium-resolving power (R ~ 1500 to 3500) integral field spectroscopy. An associated cooler system maintains MIRI at its operating temperature of < 6.7 K. This paper describes the driving principles behind the design of MIRI, the primary design parameters, and their realization in terms of the 'as-built' instrument. It also describes the test program that led to delivery of the tested and calibrated Flight Model to NASA in 2012, and the confirmation after delivery of the key interface requirements.
Published: 2015
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4. The EChO science case

Author: Tinetti, Giovanna, Drossart, Pierre, Eccleston, Paul, Hartogh, Paul, Isaak, Kate, Linder, Martin, Lovis, Christophe, Micela, Giusi, Ollivier, Marc, Puig, Ludovic, Ribas, Ignasi, Snellen, Ignas, Allard, Bruce Swinyard. France, Barstow, Joanna, Cho, James, Coustenis, Athena, Cockell, Charles, Correia, Alexandre, Decin, Leen, de Kok, Remco, Deroo, Pieter, Encrenaz, Therese, Forget, Francois, Glasse, Alistair, Griffith, Caitlin, Guillot, Tristan, Koskinen, Tommi, Lammer, Helmut, Leconte, Jeremy, Maxted, Pierre, Mueller-Wodarg, Ingo, Nelson, Richard, North, Chris, Pallé, Enric, Pagano, Isabella, Piccioni, Guseppe, Pinfield, David, Selsis, Franck, Sozzetti, Alessandro, Stixrude, Lars, Tennyson, Jonathan, Turrini, Diego, Beaulieu, Mariarosa Zapatero-Osorio. Jean-Philippe, Grodent, Denis, Guedel, Manuel, Luz, David, Nørgaard-Nielsen, Hans Ulrik, Ray, Tom, Rickman, Hans, Selig, Avri, Banaszkiewicz, Mark Swain. Marek, Barlow, Mike, Bowles, Neil, Branduardi-Raymont, Graziella, Foresto, Vincent Coudé du, Gerard, Jean-Claude, Gizon, Laurent, Hornstrup, Allan, Jarchow, Christopher, Kerschbaum, Franz, Kovacs, Géza, Lagage, Pierre-Olivier, Lim, Tanya, Lopez-Morales, Mercedes, Malaguti, Giuseppe, Pace, Emanuele, Pascale, Enzo, Vandenbussche, Bart, Wright, Gillian, Adriani, Gonzalo Ramos Zapata. Alberto, Azzollini, Ruymán, Balado, Ana, Bryson, Ian, Burston, Raymond, Colomé, Josep, Crook, Martin, Di Giorgio, Anna, Griffin, Matt, Hoogeveen, Ruud, Ottensamer, Roland, Irshad, Ranah, Middleton, Kevin, Morgante, Gianluca, Pinsard, Frederic, Rataj, Mirek, Reess, Jean-Michel, Savini, Giorgio, Schrader, Jan-Rutger, Stamper, Richard, Abe, Berend Winter. L., Abreu, M., Achilleos, N., Ade, P., Adybekian, V., Affer, L., Agnor, C., Agundez, M., Alard, C., Alcala, J., Prieto, C. Allende, Floriano, F. J. Alonso, Altieri, F., Iglesias, C. A. Alvarez, Amado, P., Andersen, A., Aylward, A., Baffa, C., Bakos, G., Ballerini, P., Banaszkiewicz, M., Barber, R. J., Barrado, D., Barton, E. J., Batista, V., Bellucci, G., Avilés, J. A. Belmonte, Berry, D., Bézard, B., Biondi, D., Błęcka, M., Boisse, I., Bonfond, B., Bordé, P., Börner, P., Bouy, H., Brown, L., Buchhave, L., Budaj, J., Bulgarelli, A., Burleigh, M., Cabral, A., Capria, M. T., Cassan, A., Cavarroc, C., Cecchi-Pestellini, C., Cerulli, R., Chadney, J., Chamberlain, S., Charnoz, S., Jessen, N. Christian, Ciaravella, A., Claret, A., Claudi, R., Coates, A., Cole, R., Collura, A., Cordier, D., Covino, E., Danielski, C., Damasso, M., Deeg, H. J., Delgado-Mena, E., Del Vecchio, C., Demangeon, O., De Sio, A., De Wit, J., Dobrijévic, M., Doel, P., Dominic, C., Dorfi, E., Eales, S., Eiroa, C., Contreras, M. Espinoza, Esposito, M., Eymet, V., Fabrizio, N., Fernández, M., Castella, B. Femenía, Figueira, P., Filacchione, G., Fletcher, L., Focardi, M., Fossey, S., Fouqué, P., Frith, J., Galand, M., Gambicorti, L., Gaulme, P., López, R. J. García, Garcia-Piquer, A., Gear, W., Gerard, J. -C., Gesa, L., Giani, E., Gianotti, F., Gillon, M., Giro, E., Giuranna, M., Gomez, H., Gomez-Leal, I., Hernandez, J. Gonzalez, Merino, B. González, Graczyk, R., Grassi, D., Guardia, J., Guio, P., Gustin, J., Hargrave, P., Haigh, J., Hébrard, E., Heiter, U., Heredero, R. L., Herrero, E., Hersant, F., Heyrovsky, D., Hollis, M., Hubert, B., Hueso, R., Israelian, G., Iro, N., Irwin, P., Jacquemoud, S., Jones, G., Jones, H., Justtanont, K., Kehoe, T., Kerschbaum, F., Kerins, E., Kervella, P., Kipping, D., Koskinen, T., Krupp, N., Lahav, O., Laken, B., Lanza, N., Lellouch, E., Leto, G., Goldaracena, J. Licandro, Lithgow-Bertelloni, C., Liu, S. J., Cicero, U. Lo, Lodieu, N., Lognonné, P., Lopez-Puertas, M., Lopez-Valverde, M. A., Rasmussen, I. Lundgaard, Luntzer, A., Machado, P., MacTavish, C., Maggio, A., Maillard, J. -P., Magnes, W., Maldonado, J., Mall, U., Marquette, J. -B., Mauskopf, P., Massi, F., Maurin, A. -S., Medvedev, A., Michaut, C., Miles-Paez, P., Montalto, M., Rodríguez, P. Montañés, Monteiro, M., Montes, D., Morais, H., Morales, J. C., Morales-Calderón, M., Morello, G., Martín, A. Moro, Moses, J., Bedon, A. Moya, Alcaino, F. Murgas, Oliva, E., Orton, G., Palla, F., Pancrazzi, M., Pantin, E., Parmentier, V., Parviainen, H., Ramírez, K. Y. Peña, Peralta, J., Perez-Hoyos, S., Petrov, R., Pezzuto, S., Pietrzak, R., Pilat-Lohinger, E., Piskunov, N., Prinja, R., Prisinzano, L., Polichtchouk, I., Poretti, E., Radioti, A., Ramos, A. A., Rank-Lüftinger, T., Read, P., Readorn, K., López, R. Rebolo, Rebordão, J., Rengel, M., Rezac, L., Rocchetto, M., Rodler, F., Béjar, V. J. Sánchez, Lavega, A. Sanchez, Sanromá, E., Santos, N., Forcada, J. Sanz, Scandariato, G., Schmider, F. -X., Scholz, A., Scuderi, S., Sethenadh, J., Shore, S., Showman, A., Sicardy, B., Sitek, P., Smith, A., Soret, L., Sousa, S., Stiepen, A., Stolarski, M., Strazzulla, G., Tabernero, H. M, Tanga, P., Tecsa, M., Temple, J., Terenzi, L., Tessenyi, M., Testi, L., Thompson, S., Thrastarson, H., Tingley, B. W., Trifoglio, M., Torres, J. Martín, Tozzi, A., Turrini, D., Varley, R., Vakili, F., de Val-Borro, M., Valdivieso, M. L., Venot, O., Villaver, E., Vinatier, S., Viti, S., Waldmann, I., Waltham, D., Ward-Thompson, D., Waters, R., Watkins, C., Watson, D., Wawer, P., Wawrzaszk, A., White, G., Widemann, T., Winek, W., Wiśniowski, T., Yelle, R., Yung, Y., and Yurchenko, S. N.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: The discovery of almost 2000 exoplanets has revealed an unexpectedly diverse planet population. Observations to date have shown that our Solar System is certainly not representative of the general population of planets in our Milky Way. The key science questions that urgently need addressing are therefore: What are exoplanets made of? Why are planets as they are? What causes the exceptional diversity observed as compared to the Solar System? EChO (Exoplanet Characterisation Observatory) has been designed as a dedicated survey mission for transit and eclipse spectroscopy capable of observing a large and diverse planet sample within its four-year mission lifetime. EChO can target the atmospheres of super-Earths, Neptune-like, and Jupiter-like planets, in the very hot to temperate zones (planet temperatures of 300K-3000K) of F to M-type host stars. Over the next ten years, several new ground- and space-based transit surveys will come on-line (e.g. NGTS, CHEOPS, TESS, PLATO), which will specifically focus on finding bright, nearby systems. The current rapid rate of discovery would allow the target list to be further optimised in the years prior to EChO's launch and enable the atmospheric characterisation of hundreds of planets. Placing the satellite at L2 provides a cold and stable thermal environment, as well as a large field of regard to allow efficient time-critical observation of targets randomly distributed over the sky. A 1m class telescope is sufficiently large to achieve the necessary spectro-photometric precision. The spectral coverage (0.5-11 micron, goal 16 micron) and SNR to be achieved by EChO, thanks to its high stability and dedicated design, would enable a very accurate measurement of the atmospheric composition and structure of hundreds of exoplanets., Comment: 50 pages, 30 figures. Experimental Astronomy
Published: 2015
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5. The high-resolution map of Oxia Planum, Mars; the landing site of the ExoMars Rosalind Franklin rover mission

Author: European Space Agency, Centre National D'Etudes Spatiales (France), U.S. Geological Survey, Centre National de la Recherche Scientifique (France), University of Bern, European Commission, UK Space Agency, Istituto Nazionale di Astrofisica, Ministerio de Economía y Competitividad (España), University of Arizona, National Aeronautics and Space Administration (US), Ministry of Education and Science of the Russian Federation, Agencia Estatal de Investigación (España), Science and Technology Facilities Council (UK), Agenzia Spaziale Italiana, Martin-Torres, Javier [0000-0001-6479-2236], Zorzano, Maria-Paz [0000-0002-4492-9650], Fawdon, Peter, Orgel, Csilla, Adeli, Solmaz, Balme, Matt, Calef, Fred J., Davis, Joel M., Frigeri, Alessandro, Grindrod, Peter, Hauber, Ernst, Deit, Laetitia Le, Loizeau, Damien, Nass, Andrea, Quantin-Nataf, Cathy, Sefton-Nash, Elliot, Thomas, Nick, Torres, Ines, Vago, Jorge L., Volat, Matthieu, De Witte, Sander, Altieri, Francesca, Apuzzo, Andrea, Aramendia, Julene, Arana, Gorka, Singh Bahia, Rickbir, Banham, Steven G., Barnes, Robert, Barrett, Alexander M., Benedix, Wolf-Stefan, Bhardwaj, Anshuman, Boazman, Sarah Jane, Bontognali, Tomaso R. R., Bridges, John, Bultel, Benjamin, Ciarletti, Valérie, De Sanctis, Maria Cristina, Dickeson, Zach, Favaro, Elena A., Ferrari, Marco, Foucher, Frédéric, Goetz, Walter, Haldemann, Albert F. C., Harrington, Elise, Kapatza, Angeliki, Koschny, Detlef, Krzesinska, Agata M., Le Gall, Alice, Lewis, Stephen R., Lim, Tanya, Madariaga, Juan Manuel, Man, Benjamin James, Mandon, Lucia, Mangold, Nicolas, Martin-Torres, Javier, McNeil, Joseph D., Molina-Jurado, Antonio, Moral, Andoni G., Motaghian, Sara, Nikiforov, Sergei, Oudart, Nicolas, Pacifici, Andrea, Parkes Bowen, Adam, Plettemeier, Dirk, Poulakis, Pantelis, Putri, Alfiah Rizky Diana, Ruesch, Ottaviano, Sam, Lydia, Schröder, Christian, Statz, Christoph, Thomas, Rebecca, Tirsch, Daniela, Toth, Zsuzsanna, Turner, Stuart, Voelker, Martin, Werner, Stephanie C., Westall, Frances, Whiteside, Barry J., Williams, Adam, Williams, Rebecca M. E., Wright, Jack, Zorzano, Maria-Paz, European Space Agency, Centre National D'Etudes Spatiales (France), U.S. Geological Survey, Centre National de la Recherche Scientifique (France), University of Bern, European Commission, UK Space Agency, Istituto Nazionale di Astrofisica, Ministerio de Economía y Competitividad (España), University of Arizona, National Aeronautics and Space Administration (US), Ministry of Education and Science of the Russian Federation, Agencia Estatal de Investigación (España), Science and Technology Facilities Council (UK), Agenzia Spaziale Italiana, Martin-Torres, Javier [0000-0001-6479-2236], Zorzano, Maria-Paz [0000-0002-4492-9650], Fawdon, Peter, Orgel, Csilla, Adeli, Solmaz, Balme, Matt, Calef, Fred J., Davis, Joel M., Frigeri, Alessandro, Grindrod, Peter, Hauber, Ernst, Deit, Laetitia Le, Loizeau, Damien, Nass, Andrea, Quantin-Nataf, Cathy, Sefton-Nash, Elliot, Thomas, Nick, Torres, Ines, Vago, Jorge L., Volat, Matthieu, De Witte, Sander, Altieri, Francesca, Apuzzo, Andrea, Aramendia, Julene, Arana, Gorka, Singh Bahia, Rickbir, Banham, Steven G., Barnes, Robert, Barrett, Alexander M., Benedix, Wolf-Stefan, Bhardwaj, Anshuman, Boazman, Sarah Jane, Bontognali, Tomaso R. R., Bridges, John, Bultel, Benjamin, Ciarletti, Valérie, De Sanctis, Maria Cristina, Dickeson, Zach, Favaro, Elena A., Ferrari, Marco, Foucher, Frédéric, Goetz, Walter, Haldemann, Albert F. C., Harrington, Elise, Kapatza, Angeliki, Koschny, Detlef, Krzesinska, Agata M., Le Gall, Alice, Lewis, Stephen R., Lim, Tanya, Madariaga, Juan Manuel, Man, Benjamin James, Mandon, Lucia, Mangold, Nicolas, Martin-Torres, Javier, McNeil, Joseph D., Molina-Jurado, Antonio, Moral, Andoni G., Motaghian, Sara, Nikiforov, Sergei, Oudart, Nicolas, Pacifici, Andrea, Parkes Bowen, Adam, Plettemeier, Dirk, Poulakis, Pantelis, Putri, Alfiah Rizky Diana, Ruesch, Ottaviano, Sam, Lydia, Schröder, Christian, Statz, Christoph, Thomas, Rebecca, Tirsch, Daniela, Toth, Zsuzsanna, Turner, Stuart, Voelker, Martin, Werner, Stephanie C., Westall, Frances, Whiteside, Barry J., Williams, Adam, Williams, Rebecca M. E., Wright, Jack, and Zorzano, Maria-Paz
Abstract: This 1:30,000 scale geological map describes Oxia Planum, Mars, the landing site for the ExoMars Rosalind Franklin rover mission. The map represents our current understanding of bedrock units and their relationships prior to Rosalind Franklin’s exploration of this location. The map details 15 bedrock units organised into 6 groups and 7 textural and surficial units. The bedrock units were identified using visible and near-infrared remote sensing datasets. The objectives of this map are (i) to identify where the most astrobiologically relevant rocks are likely to be found, (ii) to show where hypotheses about their geological context (within Oxia Planum and in the wider geological history of Mars) can be tested, (iii) to inform both the long-term (hundreds of metres to ∼1 km) and the short-term (tens of metres) activity planning for rover exploration, and (iv) to allow the samples analysed by the rover to be interpreted within their regional geological context.
Published: 2024

6. Relative pointing offset analysis of calibration targets with repeated observations with Herschel-SPIRE Fourier-Transform Spectrometer

Author: Valtchanov, Ivan, Hopwood, Rosalind, Polehampton, Edward, Benielli, Dominique, Fulton, Trevor, Imhof, Peter, Konopczynski, Tomasz, Lim, Tanya, Lu, Nanyao, Marchili, Nicola, Naylor, David, and Swinyard, Bruce
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: We present a method to derive the relative pointing offsets for SPIRE Fourier-Transform Spectrometer (FTS) solar system object (SSO) calibration targets, which were observed regularly throughout the Herschel mission. We construct ratios of the spectra for all observations of a given source with respect to a reference. The reference observation is selected iteratively to be the one with the highest observed continuum. Assuming that any pointing offset leads to an overall shift of the continuum level, then these ratios represent the relative flux loss due to mispointing. The mispointing effects are more pronounced for a smaller beam, so we consider only the FTS short wavelength array (SSW, 958-1546 GHz) to derive a pointing correction. We obtain the relative pointing offset by comparing the ratio to a grid of expected losses for a model source at different distances from the centre of the beam, under the assumption that the SSW FTS beam can be well approximated by a Gaussian. In order to avoid dependency on the point source flux conversion, which uses a particular observation of Uranus, we use extended source flux calibrated spectra to construct the ratios for the SSOs. In order to account for continuum variability, due to the changing distance from the Herschel telescope, the SSO ratios are normalised by the expected model ratios for the corresponding observing epoch. We confirm the accuracy of the derived pointing offset by comparing the results with a number of control observations, where the actual pointing of Herschel is known with good precision. Using the method we derived pointing offsets for repeated observations of Uranus (including observations centred on off-axis detectors), Neptune, Ceres and NGC7027. The results are used to validate and improve the point-source flux calibration of the FTS., Comment: 17 pages, 19 figures, accepted for publication in Experimental Astronomy
Published: 2014
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7. Herschel SPIRE FTS Relative Spectral Response Calibration

Author: Fulton, Trevor, Hopwood, Rosalind, Baluteau, Jean-Paul, Benielli, Dominique, Imhof, Peter, Lim, Tanya, Lu, Nanyao, Marchili, Nicola, Naylor, David, Polehampton, Edward, Swinyard, Bruce, and Valtchanov, Ivan
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Herschel/SPIRE Fourier transform spectrometer (FTS) observations contain emission from both the Herschel Telescope and the SPIRE Instrument itself, both of which are typically orders of magnitude greater than the emission from the astronomical source, and must be removed in order to recover the source spectrum. The effects of the Herschel Telescope and the SPIRE Instrument are removed during data reduction using relative spectral response calibration curves and emission models. We present the evolution of the methods used to derive the relative spectral response calibration curves for the SPIRE FTS. The relationship between the calibration curves and the ultimate sensitivity of calibrated SPIRE FTS data is discussed and the results from the derivation methods are compared. These comparisons show that the latest derivation methods result in calibration curves that impart a factor of between 2 and 100 less noise to the overall error budget, which results in calibrated spectra for individual observations whose noise is reduced by a factor of 2-3, with a gain in the overall spectral sensitivity of 23% and 21% for the two detector bands, respectively., Comment: 15 pages, 13 figures, accepted for publication in Experimental Astronomy
Published: 2014
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8. Herschel SPIRE FTS telescope model correction

Author: Hopwood, Rosalind, Fulton, Trevor, Polehampton, Edward T., Valtchanov, Ivan, Benielli, Dominique, Imhof, Peter, Lim, Tanya, Lu, Nanyao, Marchili, Nicola, Pearson, Chris P., and Swinyard, Bruce M.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Emission from the Herschel telescope is the dominant source of radiation for the majority of SPIRE Fourier transform spectrometer (FTS) observations, despite the exceptionally low emissivity of the primary and secondary mirrors. Accurate modelling and removal of the telescope contribution is, therefore, an important and challenging aspect of FTS calibration and data reduction pipeline. A dust-contaminated telescope model with time invariant mirror emissivity was adopted before the Herschel launch. However, measured FTS spectra show a clear evolution of the telescope contribution over the mission and strong need for a correction to the standard telescope model in order to reduce residual background (of up to 7 Jy) in the final data products. Systematic changes in observations of dark sky, taken over the course of the mission, provide a measure of the evolution between observed telescope emission and the telescope model. These dark sky observations have been used to derive a time dependent correction to the telescope emissivity that reduces the systematic error in the continuum of the final FTS spectra to ~0.35 Jy., Comment: 12 pages, 14 figures, accepted for publication in Experimental Astronomy
Published: 2014
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9. Herschel SPIRE Fourier Transform Spectrometer: Calibration of its Bright-source Mode

Author: Lu, Nanyao, Polehampton, Edward T., Swinyard, Bruce M., Benielli, Dominique, Fulton, Trevor, Hopwood, Rosalind, Imhof, Peter, Lim, Tanya, Marchili, Nicola, Naylor, David A., Schulz, Bernhard, Sidher, Sunil, and Valtchanov, Ivan
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The Fourier Transform Spectrometer (FTS) of the Spectral and Photometric Imaging REceiver (SPIRE) on board the ESA Herschel Space Observatory has two detector setting modes: (a) a nominal mode, which is optimized for observing moderately bright to faint astronomical targets, and (b) a bright-source mode recommended for sources significantly brighter than 500 Jy, within the SPIRE FTS bandwidth of 446.7-1544 GHz (or 194-671 microns in wavelength), which employs a reduced detector responsivity and out-of-phase analog signal amplifier/demodulator. We address in detail the calibration issues unique to the bright-source mode, describe the integration of the bright-mode data processing into the existing pipeline for the nominal mode, and show that the flux calibration accuracy of the bright-source mode is generally within 2% of that of the nominal mode, and that the bright-source mode is 3 to 4 times less sensitive than the nominal mode., Comment: 15 pages, 16 figures, accepted for publication in Experimental Astronomy
Published: 2014
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10. Herschel SPIRE FTS Spectral Mapping Calibration

Author: Benielli, Dominique, Polehampton, Edward, Hopwood, Rosalind, Marín, Ana Belén Griñón, Fulton, Trevor, Imhof, Peter, Lim, Tanya, Lu, Nanyao, Makiwa, Gibion, Marchili, Nicola, Naylor, David, Spencer, Locke, Swinyard, Bruce, Valtchanov, Ivan, and van der Wiel, Matthijs
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: The Herschel SPIRE Fourier transform spectrometer (FTS) performs spectral imaging in the 447-1546 GHz band. It can observe in three spatial sampling modes: sparse mode, with a single pointing on sky, or intermediate or full modes with 1 and 1/2 beam spacing, respectively. In this paper, we investigate the uncertainty and repeatability for fully sampled FTS mapping observations. The repeatability is characterised using nine observations of the Orion Bar. Metrics are derived based on the ratio of the measured intensity in each observation compared to that in the combined spectral cube from all observations. The mean relative deviation is determined to be within 2%, and the pixel-by-pixel scatter is ~7%. The scatter increases towards the edges of the maps. The uncertainty in the frequency scale is also studied, and the spread in the line centre velocity across the maps is found to be ~15 km/s. Other causes of uncertainty are also discussed including the effect of pointing and the additive uncertainty in the continuum., Comment: 12 pages, 9 figures, accepted for publication in Experimental Astronomy
Published: 2014
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11. SPIRE Point Source Photometry

Author: Pearson, Chris, Lim, Tanya, North, Chris, Bendo, George, Conversi, Luca, Dowell, Darren, Griffin, Matt, Jin, Terry, Laporte, Nicolas, Papageorgiou, Andreas, Schulz, Bernhard, Shupe, Dave, Smith, Anthony J., and Xu, Kevin
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The different algorithms appropriate for point source photometry on data from the SPIRE instrument on-board the Herschel Space Observatory, within the Herschel Interactive Processing Environment (HIPE) are compared. Point source photometry of a large ensemble of standard calibration stars and dark sky observations is carried out using the 4 major methods within HIPE: SUSSEXtractor, DAOphot, the SPIRE Timeline Fitter and simple Aperture Photometry. Colour corrections and effective beam areas as a function of the assumed source spectral index are also included to produce a large number of photometric measurements per individual target, in each of the 3 SPIRE bands (250, 350, 500um), to examine both the accuracy and repeatability of each of the 4 algorithms. It is concluded that for flux densities down to the level of 30mJy that the SPIRE Timeline Fitter is the method of choice. However, at least in the 250 and 350um bands, all 4 methods provide photometric repeatability better than a few percent down to at approximately 100mJy. The DAOphot method appears in many cases to have a systematic offset of ~8% in all SPIRE bands which may be indicative of a sub-optimal aperture correction. In general, aperture photometry is the least reliable method, i.e. largest scatter between observations, especially in the longest wavelength band. At the faintest fluxes, <30mJy, SUSSEXtractor or DAOphot provide a better alternative to the Timeline Fitter., Comment: 19 pages, 11 figures, accepted for publication in Experimental Astronomy
Published: 2014
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12. Observing Extended Sources with the \Herschel SPIRE Fourier Transform Spectrometer

Author: Wu, Ronin, Polehampton, Edward T., Etxaluze, Mireya, Makiwa, Gibion, Naylor, David A., Salji, Carl, Swinyard, Bruce M., Ferlet, Marc, van der Wiel, Matthijs H. D., Smith, Anthony J., Fulton, Trevor, Griffin, Matt J., Baluteau, Jean-Paul, Benielli, Dominique, Glenn, Jason, Hopwood, Rosalind, Imhof, Peter, Lim, Tanya, Lu, Nanyao, Panuzzo, Pasquale, Pearson, Chris, Sidher, Sunil, and Valtchanov, Ivan
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The Spectral and Photometric Imaging Receiver (SPIRE) on the European Space Agency's Herschel Space Observatory utilizes a pioneering design for its imaging spectrometer in the form of a Fourier Transform Spectrometer (FTS). The standard FTS data reduction and calibration schemes are aimed at objects with either a spatial extent much larger than the beam size or a source that can be approximated as a point source within the beam. However, when sources are of intermediate spatial extent, neither of these calibrations schemes is appropriate and both the spatial response of the instrument and the source's light profile must be taken into account and the coupling between them explicitly derived. To that end, we derive the necessary corrections using an observed spectrum of a fully extended source with the beam profile and the source's light profile taken into account. We apply the derived correction to several observations of planets and compare the corrected spectra with their spectral models to study the beam coupling efficiency of the instrument in the case of partially extended sources. We find that we can apply these correction factors for sources with angular sizes up to \theta_{D} ~ 17". We demonstrate how the angular size of an extended source can be estimated using the difference between the sub-spectra observed at the overlap bandwidth of the two frequency channels in the spectrometer, at 959<\nu<989 GHz. Using this technique on an observation of Saturn, we estimate a size of 17.2", which is 3% larger than its true size on the day of observation. Finally, we show the results of the correction applied on observations of a nearby galaxy, M82, and the compact core of a Galactic molecular cloud, Sgr B2., Comment: Accepted for publication by A&A
Published: 2013
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13. Centimeter-wave continuum radiation from the rho Ophiuchi molecular cloud

Author: Casassus, Simon, Dickinson, Clive, Cleary, Kieran, Paladini, Roberta, Etxaluze, Mireya, Lim, Tanya, White, Glenn J., Burton, Michael, Indermuehle, Balt, Stahl, Otmar, and Roche, Patrick
Subjects: Astrophysics
Abstract: The rho Oph molecular cloud is undergoing intermediate-mass star formation. UV radiation from its hottest young stars heats and dissociates exposed layers, but does not ionize hydrogen. Only faint radiation from the Rayleigh-Jeans tail of ~10-100K dust is expected at wavelengths longwards of 3mm. Yet Cosmic Background Imager (CBI) observations reveal that the rho Oph W photo-dissociation region (PDR) is surprisingly bright at centimetre wavelengths. We searched for interpretations consistent with the WMAP radio spectrum, new ISO-LWS parallel mode images and archival Spitzer data. Dust-related emission mechanisms at 1 cm, as proposed by Draine & Lazarian, are a possibility. But a magnetic enhancement of the grain opacity at 1cm is inconsistent with the morphology of the dust column maps Nd and the lack of detected polarization. Spinning dust, or electric-dipole radiation from spinning very small grains (VSGs), comfortably explains the radio spectrum, although not the conspicuous absence from the CBI data of the infrared circumstellar nebulae around the B-type stars S1 and SR~3. Allowing for VSG depletion can marginally reconcile spinning dust with the data. As an alternative interpretation we consider the continuum from residual charges in rho Oph W, where most of carbon should be photoionised by the close binary HD147889 (B2IV, B3IV). Electron densities of ~100 cm^{-3}, or H-nucleus densities n_H > 1E6 cm^{-3}, are required to interpret rho Oph W as the CII Stromgren sphere of HD147889. However the observed steep and positive low-frequency spectral index would then require optically thick emission from an hitherto unobserved ensemble of dense clumps or sheets with a filling factor ~1E-4 and n_H ~ 1E7 cm^{-3}., Comment: accepted for publication in MNRAS
Published: 2008
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14. Far-IR Excited OH Lines from Orion KL Outflows

Author: Goicoechea, Javier R., Cernicharo, Jose, Lerate, Mercedes R., Daniel, Fabien, Barlow, Michael J., Swinyard, Bruce M., Lim, Tanya L., Viti, Serena, and Yates, Jeremy
Subjects: Astrophysics
Abstract: As part of the first far-IR line survey towards Orion KL, we present the detection of seven new rotationally excited OH Lambda-doublets (at 48, 65, 71, 79, 98 and 115 um). Observations were performed with the Long Wavelength Spectrometer (LWS) Fabry-Perots on board the Infrared Space Observatory (ISO). In total, more than 20 resolved OH rotational lines, with upper energy levels up to 620 K, have been detected at an angular and velocity resolutions of 80$'' and 33 km s^-1 respectively. OH line profiles show a complex behavior evolving from pure absorption, P-Cygni type to pure emission. We also present a large scale 6' declination raster in the OH ^2\Pi_3/2 J=5/2^+-3/2^- and ^2\Pi_3/2 J=7/2^-5/2^+ lines (at 119.441 and 84.597 um) revealing the decrease of excitation outside the core of the cloud. From the observed profiles, mean intrinsic line widths and velocity offsets between emission and absorption line peaks we conclude that most of the excited OH arises from Orion outflow(s), i.e. the ``plateau'' component. We determine an averaged OH abundance relative to H_2 of X(OH)=(0.5-1.0)x10^-6, a kinetic temperature of 100 K and a density of n(H_2)=5x10^5 cm^-3. Even with these conditions, the OH excitation is heavily coupled with the strong dust continuum emission from the inner hot core regions and from the expanding flow itself., Comment: Pre-print version(5 pages, 3 figures). Accepted in ApJ letters, 2006 March 2
Published: 2006
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15. Far-Infrared and Millimeter Continuum Studies of K Giants: Alpha Boo and Alpha Tau

Author: Cohen, Martin, Carbon, Duane F., Welch, William J., Lim, Tanya, Schulz, Bernhard, McMurry, A. D., Forster, James R., and Goorvitch, David
Subjects: Astrophysics
Abstract: We have imaged two normal, non-coronal, infrared-bright K giants, Alpha Tau and Alpha Boo, in the 1.4-mm and 2.8-mm continuum using the Berkeley Illinois Maryland Association millimeter array. These stars have been used as important absolute calibrators for several infrared infrared satellites. Our goals are: (1) to establish whether these stars radiate as simple photospheres or possess long-wavelength chromospheres; and (2) to make a connection between millimeter wave and far-infrared absolute flux calibrations. To accomplish these goals we also present Infrared Space Observatory Long Wavelength Spectrometer measurements of both these K giants. The far-infrared and millimeter continuum radiation is produced in the vicinity of the temperature minimum in Alpha Tau and Alpha Boo. We find that current photospheric models predict fluxes in reasonable agreement with those observed for wavelengths which sample the upper photosphere, namely <=125 microns in Alpha Tau and Alpha Boo. We clearly detect chromospheric radiation from both stars by 2.8mm (by 1.4mm in the case of Alpha Boo). Only additional observations can determine precisely where beyond 125 microns the purely radiative models fail. Until then, purely radiative models for these stars can only be used with confidence for calibration purposes below 125 microns., Comment: 36 pages with 12 Postscript figures; AASTEX5. To be published in The Astronomical Journal
Published: 2005
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16. Observations of Water Vapor Outflow from NML Cygnus

Author: Zubko, Viktor, Li, Di, Lim, Tanya, Feuchtgruber, Helmut, and Harwit, Martin
Subjects: Astrophysics
Abstract: We report new observations of the far infrared and submillimeter water vapor emission of NML Cygnus based on data gathered with the Infrared Space Observatory and the Submillimeter Wave Astronomy Satellite. We compare the emission from NML Cyg to that previously published for VY CMa and W Hya in an attempt to establish the validity of recently proposed models for the outflow from evolved stars. The data obtained support the contention by Ivezi\'{c} & Elitzur (1995, 1997) that the atmospheres of evolved stars obey a set of scaling laws in which the optical depth of the outflow is the single most significant scaling parameter, affecting both the radiative transfer and the dynamics of the outflow. Specifically, we provide observations comparing the water vapor emission from NML Cyg, VY CMa and W Hya, and find, to the extent permitted by the quality of our data, that the results are in reasonable agreement with a model developed by Zubko & Elitzur (2000). Using this model we derive a mass loss based on the dust opacities, spectral line fluxes, and outflow velocities of water vapor observed in the atmospheres of these oxygen-rich giants. For VY CMa and NML Cyg we also obtain an estimate of the stellar mass., Comment: 6 figures, accepted by ApJ
Published: 2004
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17. ISO-LWS Serendipity Survey and Source Catalogue

Author: Vivarès, Florence, Lim, Tanya, Day, Tom, Caux, Emmanuel, Beig, R., editor, Ehlers, J., editor, Frisch, U., editor, Hepp, K., editor, Hillebrandt, W., editor, Imboden, D., editor, Jaffe, R. L., editor, Kippenhahn, R., editor, Lipowsky, R., editor, v. Löhneysen, H., editor, Ojima, I., editor, Weidenmüller, H. A., editor, Wess, J., editor, Zittartz, J., editor, Lemke, D., editor, Stickel, M., editor, and Wilke, K., editor
Published: 2000
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18. The ISO LWS Parallel Mode

Author: Lim, Tanya, Vivares, Florence, Caux, Emmanuel, Beig, R., editor, Ehlers, J., editor, Frisch, U., editor, Hepp, K., editor, Hillebrandt, W., editor, Imboden, D., editor, Jaffe, R. L., editor, Kippenhahn, R., editor, Lipowsky, R., editor, v. Löhneysen, H., editor, Ojima, I., editor, Weidenmüller, H. A., editor, Wess, J., editor, Zittartz, J., editor, Lemke, D., editor, Stickel, M., editor, and Wilke, K., editor
Published: 2000
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19. The EChO payload instrument – an overview

Author: Eccleston, Paul, Swinyard, Bruce, Tessenyi, Marcel, Tinetti, Giovanna, Waldmann, Ingo, Ferlet, Marc, Irshad, Ranah, Lim, Tanya, Middleton, Kevin, Bradshaw, Tom, Crook, Martin, Hunt, Tom, Winter, Berend, Bryson, Ian, Bezawada, Naidu, Taylor, William, Bowles, Neil, Pascale, Enzo, Morgante, Gianluca, Pace, Emanuele, Adriani, Alberto, Reess, Jean-Michel, Ollivier, Marc, Ottensamer, Roland, Rataj, Mirek, Zapata, Gonzalo Ramos, Schrader, Jan-Rutger, Selig, Avri, Isaak, Kate, Linder, Martin, and Puig, Ludovic
Published: 2015
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20. The ExoMars Rosalind Franklin Rover: Continuing Mission Preparations

Author: Sefton-Nash, Elliot, primary, Vago, Jorge L., additional, Torres, Ines, additional, Fonteyne, Romain, additional, Orgel, Csilla, additional, Bahia, Rickbir, additional, Joudrier, Luc, additional, Haessig, Frederic, additional, Williams, Adam, additional, Guerbuez, Caglayan, additional, Lim, Tanya, additional, Ball, Andrew J., additional, and Mitschdoerfer, Pia, additional
Published: 2022
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21. ESA’s Planetary Science Archive: present and future

Author: Docasal, Ruben, primary, Felix-Redondo, Fernando, additional, Oliveira, Joaquim, additional, Osinde, Jose, additional, Raga, Francisco, additional, Saiz, Jaime, additional, Valles, Ricardo, additional, Merin, Bruno, additional, Bentley, Mark, additional, Coia, Daniela, additional, Grotheer, Emmanuel, additional, Heather, David, additional, and Lim, Tanya, additional
Published: 2022
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22. ESA’s Planetary Science Archive: current status and future plans

Author: Bentley, Mark, primary, Breitfellner, Michael, additional, Coia, Daniela, additional, Docasal, Ruben, additional, Heather, David, additional, Grotheer, Emmanuel, additional, Lim, Tanya, additional, Merín, Bruno, additional, Oliveira, Joaquim, additional, Osinde, Jose, additional, Raga, Fran, additional, Saiz, Jaime, additional, and Valles, Ricardo, additional
Published: 2022
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23. Herschel celestial calibration sources: Four large main-belt asteroids as prime flux calibrators for the far-IR/sub-mm range

Author: Müller, Thomas, Balog, Zoltán, Nielbock, Markus, Lim, Tanya, Teyssier, David, Olberg, Michael, Klaas, Ulrich, Linz, Hendrik, Altieri, Bruno, Pearson, Chris, Bendo, George, and Vilenius, Esa
Published: 2014
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24. The EChO science case

Author: Tinetti, Giovanna, primary, Drossart, Pierre, additional, Eccleston, Paul, additional, Hartogh, Paul, additional, Isaak, Kate, additional, Linder, Martin, additional, Lovis, Christophe, additional, Micela, Giusi, additional, Ollivier, Marc, additional, Puig, Ludovic, additional, Ribas, Ignasi, additional, Snellen, Ignas, additional, Swinyard, Bruce, additional, Allard, France, additional, Barstow, Joanna, additional, Cho, James, additional, Coustenis, Athena, additional, Cockell, Charles, additional, Correia, Alexandre, additional, Decin, Leen, additional, de Kok, Remco, additional, Deroo, Pieter, additional, Encrenaz, Therese, additional, Forget, Francois, additional, Glasse, Alistair, additional, Griffith, Caitlin, additional, Guillot, Tristan, additional, Koskinen, Tommi, additional, Lammer, Helmut, additional, Leconte, Jeremy, additional, Maxted, Pierre, additional, Mueller-Wodarg, Ingo, additional, Nelson, Richard, additional, North, Chris, additional, Pallé, Enric, additional, Pagano, Isabella, additional, Piccioni, Guseppe, additional, Pinfield, David, additional, Selsis, Franck, additional, Sozzetti, Alessandro, additional, Stixrude, Lars, additional, Tennyson, Jonathan, additional, Turrini, Diego, additional, Zapatero-Osorio, Mariarosa, additional, Beaulieu, Jean-Philippe, additional, Grodent, Denis, additional, Guedel, Manuel, additional, Luz, David, additional, Nørgaard-Nielsen, Hans Ulrik, additional, Ray, Tom, additional, Rickman, Hans, additional, Selig, Avri, additional, Swain, Mark, additional, Banaszkiewicz, Marek, additional, Barlow, Mike, additional, Bowles, Neil, additional, Branduardi-Raymont, Graziella, additional, du Foresto, Vincent Coudé, additional, Gerard, Jean-Claude, additional, Gizon, Laurent, additional, Hornstrup, Allan, additional, Jarchow, Christopher, additional, Kerschbaum, Franz, additional, Kovacs, Géza, additional, Lagage, Pierre-Olivier, additional, Lim, Tanya, additional, Lopez-Morales, Mercedes, additional, Malaguti, Giuseppe, additional, Pace, Emanuele, additional, Pascale, Enzo, additional, Vandenbussche, Bart, additional, Wright, Gillian, additional, Ramos Zapata, Gonzalo, additional, Adriani, Alberto, additional, Azzollini, Ruymán, additional, Balado, Ana, additional, Bryson, Ian, additional, Burston, Raymond, additional, Colomé, Josep, additional, Crook, Martin, additional, Di Giorgio, Anna, additional, Griffin, Matt, additional, Hoogeveen, Ruud, additional, Ottensamer, Roland, additional, Irshad, Ranah, additional, Middleton, Kevin, additional, Morgante, Gianluca, additional, Pinsard, Frederic, additional, Rataj, Mirek, additional, Reess, Jean-Michel, additional, Savini, Giorgio, additional, Schrader, Jan-Rutger, additional, Stamper, Richard, additional, Winter, Berend, additional, Abe, L., additional, Abreu, M., additional, Achilleos, N., additional, Ade, P., additional, Adybekian, V., additional, Affer, L., additional, Agnor, C., additional, Agundez, M., additional, Alard, C., additional, Alcala, J., additional, Prieto, C. Allende, additional, Alonso Floriano, F. J., additional, Altieri, F., additional, Alvarez Iglesias, C. A., additional, Amado, P., additional, Andersen, A., additional, Aylward, A., additional, Baffa, C., additional, Bakos, G., additional, Ballerini, P., additional, Banaszkiewicz, M., additional, Barber, R. J., additional, Barrado, D., additional, Barton, E. J., additional, Batista, V., additional, Bellucci, G., additional, Belmonte Avilés, J. A., additional, Berry, D., additional, Bézard, B., additional, Biondi, D., additional, Błęcka, M., additional, Boisse, I., additional, Bonfond, B., additional, Bordé, P., additional, Börner, P., additional, Bouy, H., additional, Brown, L., additional, Buchhave, L., additional, Budaj, J., additional, Bulgarelli, A., additional, Burleigh, M., additional, Cabral, A., additional, Capria, M. T., additional, Cassan, A., additional, Cavarroc, C., additional, Cecchi-Pestellini, C., additional, Cerulli, R., additional, Chadney, J., additional, Chamberlain, S., additional, Christian Jessen, N., additional, Ciaravella, A., additional, Claret, A., additional, Claudi, R., additional, Coates, A., additional, Cole, R., additional, Collur, A., additional, Cordier, D., additional, Covino, E., additional, Danielski, C., additional, Damasso, M., additional, Deeg, H. J., additional, Delgado-Mena, E., additional, Del Vecchio, C., additional, Demangeon, O., additional, De Sio, A., additional, De Wit, J., additional, Dobrijévi, M., additional, Doel, P., additional, Dominic, C., additional, Dorfi, E., additional, Eales, S., additional, Eiroa, C., additional, Espinoza Contreras, M., additional, Esposito, M., additional, Eymet, V., additional, Fabrizio, N., additional, Fernández, M., additional, Femenía Castella, B., additional, Figueira, P., additional, Filacchione, G., additional, Fletcher, L., additional, Focardi, M., additional, Fossey, S., additional, Fouqué, P., additional, Frith, J., additional, Galand, M., additional, Gambicorti, L., additional, Gaulme, P., additional, García López, R. J., additional, Garcia-Piquer, A., additional, Gear, W., additional, Gerard, J. -C., additional, Gesa, L., additional, Giani, E., additional, Gianotti, F., additional, Gillon, M., additional, Giro, E., additional, Giuranna, M., additional, Gomez, H., additional, Gomez-Leal, I., additional, Gonzalez Hernandez, J., additional, GonzÁlez Merino, B., additional, Graczyk, R., additional, Grassi, D., additional, Guardia, J., additional, Guio, P., additional, Gustin, J., additional, Hargrave, P., additional, Haigh, J., additional, Hébrard, E., additional, Heiter, U., additional, Heredero, R. L., additional, Herrero, E., additional, Hersant, F., additional, Heyrovsky, D., additional, Hollis, M., additional, Hubert, B., additional, Hueso, R., additional, Israelian, G., additional, Iro, N., additional, Irwin, P., additional, Jacquemoud, S., additional, Jones, G., additional, Jones, H., additional, Justtanont, K., additional, Kehoe, T., additional, Kerschbaum, F., additional, Kerins, E., additional, Kervell, P., additional, Kipping, D., additional, Koskinen, T., additional, Krupp, N., additional, Lahav, O., additional, Laken, B., additional, Lanza, N., additional, Lellouch, E., additional, Leto, G., additional, Goldaracena, J. Licandro, additional, Bertelloni, C. Lithgow, additional, Liu, S. J., additional, Cicero, U. Lo, additional, Lodieu, N., additional, Lognonné, P., additional, Puertas, M. Lopez, additional, Valverde, M. A. Lopez, additional, Rasmussen, I. Lundgaard, additional, Luntzer, A., additional, Machado, P., additional, Tavish, C. Mac, additional, Maggio, A., additional, Maillard, J. P., additional, Magnes, W., additional, Maldonado, J., additional, Mall, U., additional, Marquette, J. B., additional, Mauskopf, P., additional, Massi, F., additional, Maurin, A. S., additional, Medvedev, A., additional, Michaut, C., additional, Paez, P. Miles, additional, Montalto, M., additional, Rodríguez, P. Montañés, additional, Monteiro, M., additional, Montes, D., additional, Morais, H., additional, Morale, J. C., additional, Morales-Calderón, M., additional, Morello, G., additional, Martín, A. Moro, additional, Moses, J., additional, Bedon, A. Moya, additional, Alcaino, F. Murgas, additional, Oliva, E., additional, Orton, G., additional, Palla, F., additional, Pancrazzi, M., additional, Pantin, E., additional, Parmentier, V., additional, Parviainen, H., additional, Ramirez, Y. Pena, additional, Peralta, J., additional, Perez-Hoyos, S., additional, Petrov, R., additional, Pezzuto, S., additional, Pietrzak, R., additional, Pilat-Lohinger, E., additional, Piskunov, N., additional, Prinja, R., additional, Prisinzano, L., additional, Polichtchouk, I., additional, Poretti, E., additional, Radioti, A., additional, Ramos, A., additional, Rank-Luftinger, T., additional, Read, P., additional, Readorn, K., additional, Lopez, R. Rebolo, additional, Rebordao, J., additional, Rengel, M., additional, Rezac, L., additional, Rocchetto, M., additional, Rodler, F., additional, Bejar, J. Sanchez, additional, Sanchez Lavega, A., additional, Sanroma, E., additional, Santos, N., additional, Forcada, J. Sanz, additional, Scandariato, G., additional, Schmider, F.- X., additional, Scholz, A., additional, Scuderi, S., additional, Sethenadh, J., additional, Shore, S., additional, Showman, A., additional, Sicardy, B., additional, Sitek, P., additional, Smith, A., additional, Soret, L., additional, Sousa, S., additional, Stiepen, A., additional, Stolarski, M., additional, Strazzulla, G., additional, Tabernero, H. M., additional, Tanga, P., additional, Tecsa, M., additional, Temple, J., additional, Terenzi, L., additional, Tessenyi, M., additional, Testi, L., additional, Thompson, S., additional, Thrastarson, H., additional, Tingley, B. W., additional, Trifoglio, M., additional, Torres, J. Martin, additional, Tozzi, A., additional, Turrini, D., additional, Varley, R., additional, Vakili, F., additional, de Val-Borro, M., additional, Valdivieso, M. L., additional, Venot, O., additional, Villaver, E., additional, Vinatier, S., additional, Viti, S., additional, Waldmann, I., additional, Waltham, D., additional, Ward-Thompson, D., additional, Waters, R., additional, Watkins, C., additional, Watson, D., additional, Wawer, P., additional, Wawrzaszk, A., additional, White, G., additional, Widemann, T., additional, Winek, W., additional, Wi.niowski, T., additional, Yelle, R., additional, Yung, Y., additional, and Yurchenko, S. N., additional
Published: 2015
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25. The EChO payload instrument ‑ an overview

Author: Eccleston, Paul, primary, Swinyard, Bruce, additional, Tessenyi, Marcel, additional, Tinetti, Giovanna, additional, Waldmann, Ingo, additional, Ferlet, Marc, additional, Irshad, Ranah, additional, Lim, Tanya, additional, Middleton, Kevin, additional, Bradshaw, Tom, additional, Crook, Martin, additional, Hunt, Tom, additional, Winter, Berend, additional, Bryson, Ian, additional, Bezawada, Naidu, additional, Taylor, William, additional, Bowles, Neil, additional, Pascale, Enzo, additional, Morgante, Gianluca, additional, Pace, Emanuele, additional, Adriani, Alberto, additional, Reess, Jean-Michel, additional, Ollivier, Marc, additional, Ottensamer, Roland, additional, Rataj, Mirek, additional, Zapata, Gonzalo Ramos, additional, Schrader, Jan-Rutger, additional, Selig, Avri, additional, Isaak, Kate, additional, Linder, Martin, additional, and Puig, Ludovic, additional
Published: 2014
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26. TNOs are Cool: A Survey of the Transneptunian Region: A Herschel Open Time Key Programme

Author: Müller, Thomas G., Lellouch, Emmanuel, Böhnhardt, Hermann, Stansberry, John, Barucci, Antonella, Crovisier, Jacques, Delsanti, Audrey, Doressoundiram, Alain, Dotto, Elisabetta, Duffard, René, Fornasier, Sonia, Groussin, Olivier, Gutiérrez, Pedro J., Hainaut, Olivier, Harris, Alan W., Hartogh, Paul, Hestroffer, Daniel, Horner, Jonathan, Jewitt, Dave, Kidger, Mark, Kiss, Csaba, Lacerda, Pedro, Lara, Luisa, Lim, Tanya, Mueller, Michael, Moreno, Raphael, Ortiz, Jose-Luis, Rengel, Miriam, Santos-Sanz, Pablo, Swinyard, Bruce, Thomas, Nicolas, Thirouin, Audrey, and Trilling, David
Published: 2009
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27. The 3.1 μm absorption feature on asteroids (24) Themis and (65) Cybele is not due to surface water ice

Author: O'Rourke, Laurence, primary, Müller, Thomas G., additional, Biver, Nicolas, additional, Bockelée-Morvan, Dominique, additional, Hasegawa, Sunao, additional, Valtchanov, Ivan, additional, Küppers, Michael, additional, Fornasier, Sonia, additional, Campins, Humberto, additional, Fujiwara, Hideaki, additional, Teyessier, David, additional, and Lim, Tanya, additional
Published: 2021
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28. ExoMars 2022 Rover Science Operations Preparations

Author: Sefton-Nash, Elliot, primary, Vago, Jorge L., additional, Joudrier, Luc, additional, Haessig, Frederic, additional, Williams, Adam, additional, Mitschdoerfer, Pia, additional, Koschny, Detlef, additional, Lim, Tanya, additional, Toni, Andrea, additional, Fonteyne, Romain, additional, Orgel, Csilla, additional, and Bahia, Rickbir, additional
Published: 2021
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29. ESA’s Planetary Science Archive efforts to support the scientific community

Author: Besse, Sébastien, primary, Barbarisi, Isa, additional, de Marchi, Guido, additional, Merin, Bruno, additional, Arenas, Javier, additional, Bentley, Mark, additional, Docasal, Ruben, additional, Coia, Daniela, additional, Grotheer, Emmanuel, additional, Heather, David, additional, Lim, Tanya, additional, Martinez, Santa, additional, Montero, Angel, additional, Osinde, Jose, additional, Raga, Fran, additional, Ruano, Jorge, additional, and Saiz, Jaime, additional
Published: 2021
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30. Space Operation and Performance of Doped Germanium Photo-Conducting Detectors in the Far Infrared: Experience from the ISO LWS

Author: Swinyard, Bruce, Clegg, Peter, Leeks, Sarah, Griffin, Matt, Lim, Tanya, and Burgdorf, Martin
Published: 2000
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31. Low Water outgassing from (24) Themis and (65) Cybele – Implications on 3.1 µm water absorption spectra understanding

Author: O'Rourke, Laurence, primary, Müller, Thomas, additional, Biver, Nicolas, additional, Bockelée-Morvan, Dominique, additional, Hasegawa, Sunao, additional, Valtchanov, Ivan, additional, Küppers, Michael, additional, Fornasier, Sonia, additional, Campins, Humberto, additional, Fujiwara, Hideaki, additional, Teyssier, David, additional, and Lim, Tanya, additional
Published: 2020
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32. GIS Architecture and its Applicability for the Planetary Science Archive

Author: Docasal, Ruben, primary, Barbarisi, Isa, additional, Arenas, Javier, additional, De Castro, Silvia, additional, Montero, Angel, additional, Osinde, Jose, additional, Raga, Francisco, additional, Ruano, Jorge, additional, Saiz, Jaime, additional, Merin, Bruno, additional, Besse, Sebastien, additional, Bentley, Mark, additional, Coia, Daniela, additional, Fraga, Diego, additional, Grotheer, Emmanuele, additional, Heather, David, additional, Lim, Tanya, additional, and Martinez, Santa, additional
Published: 2020
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33. ESA’s Planetary Science Archive, updates since last year!

Author: Besse, Sébastien, primary, Barbarisi, Isa, additional, de Marchi, Guido, additional, Merin, Bruno, additional, Arenas, Javier, additional, Bentley, Mark, additional, de Castro, Silvia, additional, Docasal, Ruben, additional, Coia, Daniela, additional, Fraga, Diego, additional, Grotheer, Emmanuel, additional, Heather, David, additional, Lim, Tanya, additional, Martinez, Santa, additional, Montero, Angel, additional, Osinde, Jose, additional, Raga, Francisco, additional, Ruano, Jorge, additional, and Saiz, Jaime, additional
Published: 2020
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34. The ISO LWS Parallel Mode

Author: Lim, Tanya, primary, Vivares, Florence, additional, and Caux, Emmanuel, additional
Published: 2000
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35. ISO-LWS Serendipity Survey and Source Catalogue

Author: Vivarès, Florence, primary, Lim, Tanya, additional, Day, Tom, additional, and Caux, Emmanuel, additional
Published: 2000
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36. Far-Infrared and Millimeter Continuum Studies of K-Giants: Alpha Boo and Alpha Tau

Author: Cohen, Martin, Carbon, Duane F, Welch, William J, Lim, Tanya, Forster, James R, Goorvitch, David, and Thigpen, William
Subjects: Optics
Abstract: We have imaged two normal, non-coronal, infrared-bright K-giants, alpha Boo and alpha Tau, in the 1.4-millimeter and 2.8-millimeter continuum using BIMA. These stars have been used as important absolute calibrators for several infrared satellites. Our goals are: (1) to probe the structure of their upper photospheres; (2) to establish whether these stars radiate as simple photospheres or possess long-wavelength chromospheres; and (3) to make a connection between millimeter-wave and far-infrared absolute flux calibrations. To accomplish these goals we also present ISO Long Wavelength Spectrometer (LWS) measurements of both these K-giants. The far-infrared and millimeter continuum radiation is produced in the vicinity of the temperature minimum in a Boo and a Tau, offering a direct test of the model photospheres and chromospheres for these two cool giants. We find that current photospheric models predict fluxes in reasonable agreement with those observed for those wavelengths which sample the upper photosphere, namely less than or equal to 170 micrometers in alpha Tau and less than or equal to 125 micrometers in alpha Boo. It is possible that alpha Tau is still radiative as far as 0.9 - 1.4 millimeters. We detect chromospheric radiation from both stars by 2.8 millimeters (by 1.4 millimeters in alpha Boo), and are able to establish useful bounds on the location of the temperature minimum. An attempt to interpret the chromospheric fluxes using the two-component "bifurcation model" proposed by Wiedemann et al. (1994) appears to lead to a significant contradiction.
Published: 2002

37. The ExoMars 2016 mission in the new ESA Planetary Science Archive

Author: Lim, Tanya
Subjects: Science data management
Abstract: ExoMars 2016 will be the first operational ESA mission to use PDS4 the new version of the NASAâs Planetary Data System (PDS) standards. The data produced will be housed in the new Planetary Science Archive (PSA) which is currently under development at ESAC. This talk will introduce the ExoMars 2016 mission and its payload. The adaptation of the PDS4 standard for ExoMars 2016 and other future missions in the PSA will be discussed along with a progress report on the new PSA development.
Published: 2015
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38. 'TNOs are Cool: A survey of the trans-Neptunian region'. Results from the PACS and SPIRE observations with the Herschel Space Observatory

Author: Fornasier, Sonia, Lellouch, Emmanuel, Mueller, Thomas G., Panuzzo, Pasquale, Santos-Sanz, Pablo, Lim, Tanya L., Kiss, Csaba, Vilenius, Esa, Stansberry, John A., Delsanti, Audrey, Henry, Florence, Boehnhardt, Hermann, Pál, A., Duffard, René, Barucci, Maria Antonella, Giesen, N., Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)
Subjects: [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience
Published: 2012

39. TNOs are Cool: A Survey of the Trans-Neptunian Region

Author: Mommert, Michael, Müller, Thomas, Böhnhardt, Hermann, Lellouch, Emmanuel, Stansberry, John, Barucci, Antonella, Crovisier, Jacques, Delsanti, Audrey, Doressoundiram, Alain, Dotto, Elisabetta, Duffard, René D., Fornasier, Sonia, Groussin, Olivier, Guilbert, Aurelie, Gutiérrez Buenestado, Pedro J., Hainaut, Olivier, Harris, Alan W., Hartogh, Paul, Henry, Florence, Hestroffer, Daniel, Horner, Jonathan, Jewitt, Dave, Kidger, Mark, Kiss, Csaba, Lacerda, Pedro, Lara López, Luisa M., Lim, Tanya, Mueller, Michael, Moreno, Raphael, Ortiz Moreno, Jose Luis, Pal, Andras, Protopapa, Silvia, Rengel, Miriam, Santos Sanz, Pablo, Swinyard, Bruce, Thomas, Nicolas, Thirouin, Audrey, Trilling, David, Vilenius, Esa, and Szalai, Nikolett
Subjects: thermal modeling, Herschel, TNO, thermophysical modeling
Published: 2011

40. The Mid-Infrared Instrument for the James Webb Space Telescope, II: Design and Build

Author: Wright, G. S., Wright, David, Goodson, G. B., Rieke, G. H., Aitink-Kroes, Gabby, Amiaux, J., Aricha-Yanguas, Ana, Azzollini, Ruyman, Banks, Kimberly, Barrado-Navascues, D., Belenguer-Davila, T., Bloemmart, J. A. D. L., Bouchet, Patrice, Brandl, B. R., Colina, L., Detre, Oers, Diaz-Catala, Eva, Eccleston, Paul, Friedman, Scott D., Garcia-Marin, Macarena, Guedel, Manuel, Glasse, Alistair, Glauser, Adrian M., Greene, T. P., Groezinger, Uli, Grundy, Tim, Hastings, Peter, Henning, Th, Hofferbert, Ralph, Hunter, Faye, Jessen, N. C., Justtanont, K., Karnik, Avinash R., Khorrami, Mori A., Krause, Oliver, Labiano, Alvaro, Lagage, P. -O., Langer, Ulrich, Lemke, Dietrich, Lim, Tanya, Lorenzo-Alvarez, Jose, Mazy, Emmanuel, McGowan, Norman, Meixner, M. E., Morris, Nigel, Morrison, Jane E., Mueller, Friedrich, Rgaard-Nielson, H. -U. No, Olofsson, Goran, O'Sullivan, Brian, Pel, J. -W., Penanen, Konstantin, Petach, M. B., Pye, J. P., Ray, T. P., Renotte, Etienne, Renouf, Ian, Ressler, M. E., Samara-Ratna, Piyal, Scheithauer, Silvia, Schneider, Analyn, Shaughnessy, Bryan, Stevenson, Tim, Sukhatme, Kalyani, Swinyard, Bruce, Sykes, Jon, Thatcher, John, Tikkanen, Tuomo, van Dishoeck, E. F., Waelkens, C., Walker, Helen, Wells, Martyn, Zhender, Alex, Wright, G. S., Wright, David, Goodson, G. B., Rieke, G. H., Aitink-Kroes, Gabby, Amiaux, J., Aricha-Yanguas, Ana, Azzollini, Ruyman, Banks, Kimberly, Barrado-Navascues, D., Belenguer-Davila, T., Bloemmart, J. A. D. L., Bouchet, Patrice, Brandl, B. R., Colina, L., Detre, Oers, Diaz-Catala, Eva, Eccleston, Paul, Friedman, Scott D., Garcia-Marin, Macarena, Guedel, Manuel, Glasse, Alistair, Glauser, Adrian M., Greene, T. P., Groezinger, Uli, Grundy, Tim, Hastings, Peter, Henning, Th, Hofferbert, Ralph, Hunter, Faye, Jessen, N. C., Justtanont, K., Karnik, Avinash R., Khorrami, Mori A., Krause, Oliver, Labiano, Alvaro, Lagage, P. -O., Langer, Ulrich, Lemke, Dietrich, Lim, Tanya, Lorenzo-Alvarez, Jose, Mazy, Emmanuel, McGowan, Norman, Meixner, M. E., Morris, Nigel, Morrison, Jane E., Mueller, Friedrich, Rgaard-Nielson, H. -U. No, Olofsson, Goran, O'Sullivan, Brian, Pel, J. -W., Penanen, Konstantin, Petach, M. B., Pye, J. P., Ray, T. P., Renotte, Etienne, Renouf, Ian, Ressler, M. E., Samara-Ratna, Piyal, Scheithauer, Silvia, Schneider, Analyn, Shaughnessy, Bryan, Stevenson, Tim, Sukhatme, Kalyani, Swinyard, Bruce, Sykes, Jon, Thatcher, John, Tikkanen, Tuomo, van Dishoeck, E. F., Waelkens, C., Walker, Helen, Wells, Martyn, and Zhender, Alex
Abstract: The Mid-InfraRed Instrument (MIRI) on the James Webb Space Telescope (JWST) provides measurements over the wavelength range 5 to 28: 5 mu m. MIRI has, within a single package, four key scientific functions: photometric imaging, coronagraphy, single-source low-spectral resolving power (R similar to 100) spectroscopy, and medium-resolving power (R similar to 1500 to 3500) integral field spectroscopy. An associated cooler system maintains MIRI at its operating temperature of <6.7 K. This paper describes the driving principles behind the design of MIRI, the primary design parameters, and their realization in terms of the as-built instrument. It also describes the test program that led to delivery of the tested and calibrated Flight Model to NASA in 2012, and the confirmation after delivery of the key interface requirements.
Published: 2015

41. TNOs are Cool: A Survey of the Trans-Neptunian Region: Radiometric properties of Trans-Neptunian Objects

Author: Mommert, Michael, Müller, Thomas, Böhnhardt, Hermann, Lellouch, Emmanuel, Stansberry, John, Barucci, Antonella, Crovisier, Jacques, Delsanti, Audrey, Doressoundiram, Alain, Dotto, Elisabetta, Duffard, René D., Fornasier, Sonia, Groussin, Olivier, Guilbert, Aurelie, Gutiérrez Buenestado, Pedro J., Hainaut, Olivier, Harris, Alan W., Hartogh, Paul, Henry, Florence, Hestroffer, Daniel, Horner, Jonathan, Jewitt, Dave, Kidger, Mark, Kiss, Csaba, Lacerda, Pedro, Lara López, Luisa M., Lim, Tanya, Mueller, Michael, Moreno, Raphael, Ortiz Moreno, Jose Luis, Pal, Andras, Protopapa, Silvia, Rengel, Miriam, Santos Sanz, Pablo, Swinyard, Bruce, Thomas, Nicolas, Thirouin, Audrey, Trilling, David, and Vilenius, Esa
Subjects: Asteroiden und Kometen, thermal modeling, Herschel, TNO, thermophysical modeling
Abstract: The "TNOs are Cool: A Survey of the Trans-Neptunian Region" project is a Herschel Open Time Key Program awarded some 370 h of Herschel observing time. The observations include PACS and SPIRE point-source photometry on about 140 trans-Neptunian objects with known orbits. The goal is to characterize the individual objects and the full sample using radiometric techniques, in order to probe formation and evolution processes in the Solar System and to establish a benchmark for understanding the Solar System debris disk as well as extra-solar ones. We present results on a set of TNOs which were selected for the Science Demonstration and early mission phases and report on progress in deriving effective sizes, geometric albedos, and thermal characteristics. Our early sample also includes binary objects for which density estimates can be made on the basis of the derived diameters. TNO densities can provide insight into Solar-System formation scenarios.
Published: 2010

42. The Mid-Infrared Instrument for theJames Webb Space Telescope, II: Design and Build

Author: Wright, G. S., primary, Wright, David, additional, Goodson, G. B., additional, Rieke, G. H., additional, Aitink-Kroes, Gabby, additional, Amiaux, J., additional, Aricha-Yanguas, Ana, additional, Azzollini, Ruymán, additional, Banks, Kimberly, additional, Barrado-Navascues, D., additional, Belenguer-Davila, T., additional, Bloemmart, J. A. D. L., additional, Bouchet, Patrice, additional, Brandl, B. R., additional, Colina, L., additional, Detre, Örs, additional, Diaz-Catala, Eva, additional, Eccleston, Paul, additional, Friedman, Scott D., additional, García-Marín, Macarena, additional, Güdel, Manuel, additional, Glasse, Alistair, additional, Glauser, Adrian M., additional, Greene, T. P., additional, Groezinger, Uli, additional, Grundy, Tim, additional, Hastings, Peter, additional, Henning, Th., additional, Hofferbert, Ralph, additional, Hunter, Faye, additional, Jessen, N. C., additional, Justtanont, K., additional, Karnik, Avinash R., additional, Khorrami, Mori A., additional, Krause, Oliver, additional, Labiano, Alvaro, additional, Lagage, P.-O., additional, Langer, Ulrich, additional, Lemke, Dietrich, additional, Lim, Tanya, additional, Lorenzo-Alvarez, Jose, additional, Mazy, Emmanuel, additional, McGowan, Norman, additional, Meixner, M. E., additional, Morris, Nigel, additional, Morrison, Jane E., additional, Müller, Friedrich, additional, Nø rgaard-Nielson, H.-U., additional, Olofsson, Göran, additional, O’Sullivan, Brian, additional, Pel, J.-W., additional, Penanen, Konstantin, additional, Petach, M. B., additional, Pye, J. P., additional, Ray, T. P., additional, Renotte, Etienne, additional, Renouf, Ian, additional, Ressler, M. E., additional, Samara-Ratna, Piyal, additional, Scheithauer, Silvia, additional, Schneider, Analyn, additional, Shaughnessy, Bryan, additional, Stevenson, Tim, additional, Sukhatme, Kalyani, additional, Swinyard, Bruce, additional, Sykes, Jon, additional, Thatcher, John, additional, Tikkanen, Tuomo, additional, van Dishoeck, E. F., additional, Waelkens, C., additional, Walker, Helen, additional, Wells, Martyn, additional, and Zhender, Alex, additional
Published: 2015
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43. TNO Modelling Aspects and First Radiometric Results from the ’TNOs are Cool’ Project

Author: Mommert, Michael, Müller, Thomas, Böhnhardt, Hermann, Lellouch, Emmanuel, Stansberry, John, Barucci, Antonella, Crovisier, Jacques, Delsanti, Audrey, Doressoundiram, Alain, Dotto, Elisabetta, Duffard, René D., Fornasier, Sonia, Groussin, Olivier, Guilbert, Aurelie, Gutiérrez Buenestado, Pedro J., Hainaut, Olivier, Harris, Alan W., Hartogh, Paul, Henry, Florence, Hestroffer, Daniel, Horner, Jonathan, Jewitt, Dave, Kidger, Mark, Kiss, Csaba, Lacerda, Pedro, Lara López, Luisa M., Lim, Tanya, Mueller, Michael, Moreno, Raphael, Ortiz Moreno, Jose Luis, Pal, Andras, Protopapa, Silvia, Rengel, Miriam, Santos Sanz, Pablo, Swinyard, Bruce, Thomas, Nicolas, Thirouin, Audrey, Trilling, David, and Vilenius, Esa
Subjects: Asteroiden und Kometen, thermal modeling, Herschel, TNO, thermophysical modeling
Abstract: The "TNOs are Cool: A Survey of the Trans-Neptunian Region" project is a Herschel Open Time Key Program awarded some 370 h of Herschel observing time. The observations include PACS and SPIRE point-source photometry on about 140 trans-Neptunian objects with known orbits. The goal is to characterize the individual objects and the full sample using radiometric techniques, in order to probe formation and evolution processes in the Solar System and to establish a benchmark for understanding the Solar System debris disk as well as extra-solar ones. We present results on a set of TNOs which were selected for the Science Demonstration and early mission phases and report on progress in deriving effective sizes, geometric albedos, thermal characteristics, and our different approaches using thermal and thermophysical models.
Published: 2010

44. From Clouds to Young Stellar Objects and back again: the all-in-one view from the Herschel infrared Galactic Plane Survey

Author: Molinari, Sergio, Abergel, Alain, Rivera-Ingraham, Alana, Noriega-Crespo, Alberto, Traficante, Alessio, Di Giorgio, Anna, Zavagno, Annie, Chrysostomou, Antonio, Roy, Arabino, Babar, Ali, Maiolo, Berlinda, Schulz, Bernhard, Jiang, Biwei, Sibthorpe, Bruce, Swinyard, Bruce, Battersby, Cara, Burigana, Carlo, Brunt, Chris, Davis, Chris, Joblin, Christine, Waelkens, Christoffel, Meny, Claude, Codella, Claudio, Popescu, Cristina, Polychroni, Danae, Eden, David, Ikhenaode, David, Elia, Davide, Paradis, Deborah, Shepherd, Debra, Russeil, Delphine, Ward-Thompson, D., Stamatellos, Dimitris, Marshall, Douglas, Sturm, Eckhard, Rosolowsky, Erik, Schisano, Eugenio, Faustini, Fabiana, Agostini, Fabio, Massi, Fabrizio, La Morgia, Federico, Piacentini, Francesco, Strafella, Francesco, Boulanger, Francois, Schuller, Frederic, Motte, Frederique, Wyrowski, Friedrich, Fuller, Gary, de Gasperis, Giancarlo, Joncas, Gilles, Giardino, Giovanna, White, Glenn, Umana, Grazia, Lagache, Guilaine, Rivest, Guillaume, Stringfellow, Guy, Yorke, Harold, Ristorcelli, Isabelle, Difrancesco, James, Brand, Jan, Glenn, Jason, Kirk, Jason, Rodon, Javier, Baluteau, Jean-Paul, Bernard, Jean-Philippe, Li, Jinzeng, Neves, Joao, Mottram, Joe, Fischera, Joerg, Bally, John, Richer, John, Blommaert, Joris, Cernicharo, Jose, Ganga, K., Morgan, Larry, Testi, Leonardo, Anderson, Loren, Piazzo, Lorenzo, Campeggio, Loretta, Conversi, Luca, Olmi, Luca, Valenziano, Luca, Montier, Ludovic, Spinoglio, Luigi, Beltran, Maite, Huang, Maohai, Miville-Deschenes, Marc-Antoine, Sauvage, Marc, Veneziani, Marcella, Thompson, Mark, Cohen, Martin, Giard, Martin, Marengo, Massimo, Compiegne, Mathieu, Griffin, Matt, Pomares, Melanie, Hoare, Melvin, Barlow, Michael, Burton, Michael, Reid, Michael, Smith, Michael, Pestalozzi, Michele, Juvela, Mika, Matsuura, Mikako, Benedettini, Milena, Schneider, N., Billot, Nicolas, Peretto, Nicolas, Berne, Olivier, Caselli, Paola, Debernardis, Paolo, Natoli, Paolo, Saraceno, Paolo, Goldsmith, Paul, Garcia Lario, Pedro, Martin, Peter, Schilke, Peter, Lucas, Phil, Andre, Philippe, Royer, Pierre, Zhang, Qizhou, Plume, Rene, Cesaroni, Riccardo, Tuffs, Richard, Paladini, Roberta, Vavrek, Roland, Taylor, Russ, Carey, Sean, Viti, Serena, Masi, Silvia, Pezzuto, Stefano, Lord, Steve, Chakrabarti, Sukanya, Bontemps, Sylvain, Lim, Tanya, Mueller, Thomas, Robitaille, Thomas, Troost, Tobias, Moore, Toby, Minier, Vincent, Reach, William, Fukui, Yasuo, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire Astronomique de Marseille Provence (OAMP), Université de Provence - Aix-Marseille 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Météo-France -Institut de Recherche pour le Développement (IRD)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Service de Neurologie [CHU Pitié-Salpêtrière], IFR70-CHU Pitié-Salpêtrière [AP-HP], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), Neurologie et thérapeutique expérimentale, Université Pierre et Marie Curie - Paris 6 (UPMC)-IFR70-Institut National de la Santé et de la Recherche Médicale (INSERM), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Laboratoire de Physique des Lasers (LPL), Université Paris 13 (UP13)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Radioastronomie (MPIFR), SLAC National Accelerator Laboratory (SLAC), Stanford University, Istituto di Radioastronomia [Bologna] (IRA), Center for Astrophysics and Space Astronomy [Boulder] (CASA), University of Colorado [Boulder], Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Centro de Investigaciones Biológicas (CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Department of Mechanical and Aerospace Engineering [Victoria]], Monash University [Clayton], Istituto Nazionale di Geofisica e Vulcanologia – Sezione di Pisa (INGV), Istituto Nazionale di Geofisica e Vulcanologia, Department of Physics and Astronomy, University of Canterbury [Christchurch], University of Manchester [Manchester], Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), I. Physikalisches Institut [Köln], Universität zu Köln, Recherche en épidémiologie et biostatistique, Université Paris-Sud - Paris 11 (UP11)-Institut National de la Santé et de la Recherche Médicale (INSERM), Laboratoire de Nanotechnologie et d'Instrumentation Optique (LNIO), Institut Charles Delaunay (ICD), Université de Technologie de Troyes (UTT)-Centre National de la Recherche Scientifique (CNRS)-Université de Technologie de Troyes (UTT)-Centre National de la Recherche Scientifique (CNRS), Institute of Atomic Physics, Université de Roumanie, Department of Physics and Astronomy [Calgary], University of Calgary, FORMATION STELLAIRE 2010, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Max-Planck-Institut für Extraterrestrische Physik (MPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Service de neurologie 1 [CHU Pitié-Salpétrière], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-CHU Pitié-Salpêtrière [AP-HP], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU)-Sorbonne Université (SU), Institut National de la Santé et de la Recherche Médicale (INSERM)-IFR70-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), California Institute of Technology (CALTECH)-NASA, Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Assistance publique - Hôpitaux de Paris (AP-HP) (APHP)-CHU Pitié-Salpêtrière [APHP], Université Sorbonne Paris Cité (USPC)-Institut Galilée-Université Paris 13 (UP13)-Centre National de la Recherche Scientifique (CNRS), Stanford Linear Accelerator Center (SLAC), Stanford University [Stanford], Istituto di Radioastronomia (IRA), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut National de la Santé et de la Recherche Médicale (INSERM), Centre National de la Recherche Scientifique (CNRS)-Université de Technologie de Troyes (UTT)-Centre National de la Recherche Scientifique (CNRS)-Université de Technologie de Troyes (UTT), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), CHU Pitié-Salpêtrière [AP-HP], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Universität zu Köln = University of Cologne, Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), and Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB)
Subjects: [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics::Galaxy Astrophysics
Abstract: Symposium E, session 14, paper number E14-0026-10 (Oral); From diffuse interstellar cirrus to dense atomic and molecular clouds, from protostellar to post-AGB envelopes, from super-shells to supernovae remnants, the Herschel Hi-GAL survey offer an unprecedented snapshot of all the different phases of the Galactic ISM, its evolution and interactions. I will present early results on a variety of topics including the lifetime of massive pre-stellar phases, the fragmentation and collapse of extended structures, the timeline for massive star formation, dust properties in cirrus and molecular clouds.
Published: 2010

45. Herschel Open Time Key Programme---TNOs are Cool: A Survey of the Transneptunian Region

Author: Müller, Thomas G., Lellouch, Emmanuel, Böhnhardt, Hermann, Stansberry, John A., Barucci, Maria Antonella, Crovisier, Jacques, Delsanti, Audrey, Doressoundiram, Alain, Dotto, Elisabetta, Duffard, René, Fornasier, Sonia, Groussin, Olivier, Gutierrez, Pedro J., Hainaut, Olivier, Harris, Alan W., Hartogh, Paul, Hestroffer, Daniel, Horner, Jonathan, Jewitt, Dave, Kidger, Mark R., Kiss, Csaba, Lacerda, Pedro, Lara, Luisa M., Lim, Tanya L., Mueller, Michael, Moreno, Raphaël, Ortiz, José Luiz, Rengel, Miriam, Santos-Sanz, Pablo, Swinyard, Bruce, Thomas, Nicholas, Trilling, David E., Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Astronomie du LESIA, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)
Subjects: [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience
Published: 2008

46. In-orbit performance of the Herschel/SPIRE imaging Fourier transform spectrometer: lessons learned

Author: Oschmann, Jacobus M., Jr., Clampin, Mark, Fazio, Giovanni G., MacEwen, Howard A., Naylor, David A., Baluteau, Jean-Paul, Bendo, George J., Benielli, Dominique, Fulton, Trevor, Gom, Brad G., Griffin, Matthew J., Hopwood, Rosalind, Imhof, Peter, Lim, Tanya L., Lu, Nanyao, Makiwa, Gibion, Marchili, Nicola, Orton, Glen S., Papgeorgiou, Andreas, Pearson, Chris, Polehampton, Edward T., Schulz, Bernhard, Spencer, Locke D., Swinyard, Bruce M., Valtchanov, Ivan, van der Wiel, Matthijs, Veenendaal, Ian T., Wu, Ronin, Oschmann, Jacobus M., Jr., Clampin, Mark, Fazio, Giovanni G., MacEwen, Howard A., Naylor, David A., Baluteau, Jean-Paul, Bendo, George J., Benielli, Dominique, Fulton, Trevor, Gom, Brad G., Griffin, Matthew J., Hopwood, Rosalind, Imhof, Peter, Lim, Tanya L., Lu, Nanyao, Makiwa, Gibion, Marchili, Nicola, Orton, Glen S., Papgeorgiou, Andreas, Pearson, Chris, Polehampton, Edward T., Schulz, Bernhard, Spencer, Locke D., Swinyard, Bruce M., Valtchanov, Ivan, van der Wiel, Matthijs, Veenendaal, Ian T., and Wu, Ronin
Abstract: The Spectral and Photometric Imaging Receiver (SPIRE) is one of three scientific instruments on board the European Space Agency's Herschel Space Observatory which ended its operational phase on 29 April 2013. The low to medium resolution spectroscopic capability of SPIRE is provided by an imaging Fourier transform spectrometer (iFTS) of the Mach-Zehnder configuration. With their high throughput, broad spectral coverage, and variable resolution, coupled with their well-defined instrumental line shape and intrinsic wavelength and intensity calibration, iFTS are becoming increasingly common in far-infrared space astronomy missions. The performance of the SPIRE imaging spectrometer will be reviewed and example results presented. The lessons learned from the measured performance of the spectrometer as they apply to future missions will be discussed.
Published: 2014

47. Design and performance of the Exo-planet Characterisation Observatory (EChO) integrated payload

Author: Swinyard, Bruce, additional, Tessenyi, Marcel, additional, Tinetti, Giovanna, additional, Waldmann, Ingo, additional, Eccleston, Paul, additional, Ferlet, Marc, additional, Irshad, Ranah, additional, Lim, Tanya, additional, Middleton, Kevin, additional, Bradshaw, Tom, additional, Crook, Martin, additional, Hunt, Tom, additional, Winter, Berend, additional, Bryson, Ian, additional, Bezawada, Naidu, additional, Taylor, William, additional, Bowles, Neil, additional, Pascale, Enzo, additional, Morgante, Gianluca, additional, Pace, Emanuele, additional, Adriani, Alberto, additional, Reess, Jean-Michel, additional, Drossart, Pierre, additional, Coudé du Foresto, Vincent, additional, Ollivier, Marc, additional, Ottensamer, Roland, additional, Rataj, Mirek, additional, Ramos Zapata, Gonzalo, additional, Schrader, Jan-Rutger, additional, Selig, Avri, additional, Isaak, Kate, additional, Linder, Martin, additional, Puig, Ludovic, additional, Hartogh, Paul, additional, Lovis, Christophe, additional, Micela, Giusi, additional, Ribas, Ignasi, additional, Snellen, Ignas, additional, and Beaulieu, Jean-Phillippe, additional
Published: 2014
Full Text: View/download PDF

48. In-orbit performance of the Herschel/SPIRE imaging Fourier transform spectrometer: lessons learned

Author: Naylor, David A., additional, Baluteau, Jean-Paul, additional, Bendo, George J., additional, Benielli, Dominique, additional, Fulton, Trevor R., additional, Gom, Brad G., additional, Griffin, Matthew J., additional, Hopwood, Rosalind, additional, Imhof, Peter, additional, Lim, Tanya L., additional, Lu, Nanyao, additional, Makiwa, Gibion, additional, Marchili, Nicola, additional, Orton, Glenn S., additional, Papageorgiou, Andreas, additional, Pearson, Chris, additional, Polehampton, Edward T., additional, Schulz, Bernhard, additional, Spencer, Locke D., additional, Swinyard, Bruce M., additional, Valtchanov, Ivan, additional, van der Wiel, Matthijs H. D., additional, Veenendaal, Ian T., additional, and Wu, Ronin, additional
Published: 2014
Full Text: View/download PDF

49. Graduate recitals

Author: Lim, Tanya Jessica Wan
Abstract: The thesis for the Master of Music degree in Piano Performance consists of one solo recital and one full-length ensemble recital. I performed the recitals on October 14, 2000 and March 24, 2001.
Published: 2003
Full Text: View/download PDF

50. The data processing pipelines for the Herschel/SPIRE imaging Fourier transform spectrometer

Author: Oschmann, Jacobus M., Jr., Clampin, Mark C., MacEwen, Howard A., Fulton, Trevor R., Baluteau, Jean-Paul, Bendo, George, Benielli, Dominique, Gastaud, Rene, Griffin, Matt, Guest, Steve, Imhof, Peter, Lim, Tanya L., Lu, Nanyao, Naylor, David A., Panuzzo, Pasquale, Polehampton, Edward, Schwartz, Arnold, Surace, Christian, Swinyard, Bruce M., Xu, Kevin, Oschmann, Jacobus M., Jr., Clampin, Mark C., MacEwen, Howard A., Fulton, Trevor R., Baluteau, Jean-Paul, Bendo, George, Benielli, Dominique, Gastaud, Rene, Griffin, Matt, Guest, Steve, Imhof, Peter, Lim, Tanya L., Lu, Nanyao, Naylor, David A., Panuzzo, Pasquale, Polehampton, Edward, Schwartz, Arnold, Surace, Christian, Swinyard, Bruce M., and Xu, Kevin
Abstract: We present an update to the data processing pipelines that generate calibrated spectral data products from the Spectral and Photometric Imaging Receiver (SPIRE), one of three scientific instruments onboard the European Space Agency's Herschel Space Observatory launched on 14 May 2009. The pipelines process telemetry from SPIRE's imaging Fourier Transform Spectrometer (FTS) taken in point source, jiggle- and raster-map observing modes, producing calibrated spectra in low-, medium-, high-, and mixed low- and high-spectral resolution. While the order and algorithms of the data processing modules in the spectrometer pipelines remain for the most part unchanged compared to their pre-launch status, some improvements and optimizations have been realized through the analysis of data from the performance verification and science demonstration phases of the mission. The data processing pipelines for the SPIRE FTS as of the beginning of the routine phase of the Herschel mission are presented in their entirety, with more detailed descriptions reserved for those elements that have changed since launch, in particular the first- and second-level correction steps for glitches, the step that corrects for clipped samples, and the process by which Level-1 spectral data are converted to Level-2 products. In addition, we discuss some of the challenging aspects still faced by the automated processing pipelines, such as the removal of the contributions from the Herschel telescope and SPIRE instrument, and the relative spectral response correction and flux conversion steps.
Published: 2010

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