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1. Hi-GAL, the Herschel infrared Galactic Plane Survey: Photometric maps and compact source catalogues: First data release for the inner Milky Way: +68° ≥ l ≥ -70°

Author

Stefano Pezzuto, Annie Zavagno, M. J. Barlow, Nicolas Peretto, S. D. Lord, Yasuo Fukui, Davide Elia, G. Polenta, D. Russeil, Sergio Molinari, Thomas P. Robitaille, R. Del Grande, G. Umana, Riccardo Cesaroni, M. Benedettini, Pascal André, Benjamin L. Schulz, Babar Ali, Pierrick Martin, David Eden, P. Natoli, Göran Pilbratt, Manuel Merello, R. Paladini, Francesco Strafella, Alessio Traficante, Luca Calzoletti, Mathieu Compiegne, Derek Ward-Thompson, Peter Schilke, Gilles Joncas, Rene Plume, Nicola Schneider, Pedro García-Lario, J.-P. Bernard, Kazi L.J. Rygl, Leonardo Testi, M. T. Beltrán, M. R. Pestalozzi, F. Piacentini, A. M. di Giorgio, Eugenio Schisano, Christopher M. Brunt, John Bally, N. Billot, Maggie A. Thompson, Sean K. Carey, Joseph C. Mottram, B. M. Swinyard, Melvin Hoare, F. Faustini, S. J. Liu, S. Martinavarro-Armengol, D. Paradis, Toby J. T. Moore, D. Polychroni, Antonella Palmese, Friedrich Wyrowski, Alberto Noriega-Crespo, Lorenzo Piazzo, Tanya Lim, M. Veneziani, Meng-Lin Huang, Bruce Sibthorpe, and Frédérique Motte

Subjects
Physics, Line-of-sight, 010308 nuclear & particles physics, Infrared, Milky Way, Bolometer, Astronomy and Astrophysics, Astrophysics, Galactic plane, dust, extinction, Galaxy: disk, infrared: ISM, methods: data analysis, stars: formation, techniques: photometric, astronomy and astrophysics, space and planetary science, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, law.invention, symbols.namesake, Wavelength, 13. Climate action, Space and Planetary Science, law, 0103 physical sciences, symbols, Spectral energy distribution, Planck, 010303 astronomy & astrophysics, QC, QB
Abstract

(Abridged) We present the first public release of high-quality data products (DR1) from Hi-GAL, the {\em Herschel} infrared Galactic Plane Survey. Hi-GAL is the keystone of a suite of continuum Galactic Plane surveys from the near-IR to the radio, and covers five wavebands at 70, 160, 250, 350 and 500 micron, encompassing the peak of the spectral energy distribution of cold dust for 8 < T < 50K. This first Hi-GAL data release covers the inner Milky Way in the longitude range 68{\deg} > l > -70{\deg} in a |b, Comment: Astronomy & Astrophysics, accepted

Published
2016

2. The Herschel mission and observing opportunities

Author

Göran Pilbratt

Subjects
Physics, Spectrometer, Payload, General Engineering, Astronomy, Cassegrain reflector, Astronomy and Astrophysics, Astrophysics, Photometry (astronomy), symbols.namesake, Spire, Space and Planetary Science, Observatory, symbols, Ground segment, Planck
Abstract

Herschel is the fourth cornerstone mission in the European Space Agency (ESA) science programme. It will perform imaging photometry and spectroscopy in the far infrared and submillimetre part of the spectrum, covering approximately the 55–672 µmm range and thus bridging the traditional space infrared range with the groundbased capabilities. The key science objectives emphasize fundamental issues connected to the formation and evolution of galaxies and stars and stellar systems. However, Herschel will be an observatory facility and its unique capabilities will be available to the entire astronomical community for a wide range of observations. Herschel is equipped with a passively cooled 3.5 m diameter classical Cassegrain telescope. The science payload complement – two cameras/medium resolution spectrometers (PACS and SPIRE) and a very high resolution heterodyne spectrometer (HIFI) – is housed in a superfluid helium cryostat. The ground segment is jointly developed by the ESA, the three instrument consortia, and NASA/IPAC. Herschel is scheduled to be launched into a transfer trajectory towards its operational orbit around the Earth-Sun L2 point by an Ariane 5 ECA (shared with the ESA cosmic background mapping mission Planck) in 2009. Once operational about half a year after launch, Herschel will offer 3 years of routine science operations. Almost 20 000 hours of observing time will nominally be made available for astronomy, 32% is guaranteed time, the remainder is open time which is offered to the worldwide general astronomical community through a standard competitive proposal procedure.

Published
2009
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3. q$^{\mathsf{1}}$ Eridani: a solar-type star with a planet and a dust belt

Author

Philippe Thebault, M. Fridlund, Christophe Risacher, Carlos Eiroa, G. Olofsson, Alexis Brandeker, Göran Pilbratt, René Liseau, and Ricky Nilsson

Subjects
Physics, Infrared excess, Flux, Minimum mass, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Stars, Wavelength, Space and Planetary Science, Planet, Astrophysics::Solar and Stellar Astrophysics, Millimeter, Black-body radiation, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Only very few solar-type stars exhibiting an infrared excess and harbouring planets are known to date. Indeed, merely a single case of a star-planet-disk system has previously been detected at submillimeter (submm) wavelengths. Consequently, one of our aims is to understand the reasons for these poor statistics, i.e., whether these results reflected the composition and/or the physics of the planetary disks or were simply due to observational bias and selection effects. Finding more examples would be very significant. The selected target, q1 Eri, is a solar-type star, which was known to possess a planet, q1 Eri b, and to exhibit excess emission at IRAS wavelengths, but had remained undetected in the millimeter regime. Therefore, submm flux densities would be needed to better constrain the physical characteristics of the planetary disk. Consequently, we performed submm imaging observations of q1 Eri. The detected dust toward q1 Eri at 870 micron exhibits the remarkable fact that the entire SED, from the IR to mm-wavelengths, is fit by a single temperature blackbody function (60 K). This would imply that the emitting regions are confined to a narrow region (ring) at radial distances much larger than the orbital distance of q1 Eri b, and that the emitting particles are considerably larger than some hundred micron. However, the 870 micron source is extended, with a full-width-half-maximum of roughly 600 AU. Therefore, a physically more compelling model also invokes a belt of cold dust (17 K), located at 300 AU from the star and about 60 AU wide. The minimum mass of 0.04 Mearth (3 Mmoon) of 1 mm-size icy ring-particles is considerable, given the stellar age of about 1 Gyr. These big grains form an inner edge at about 25 AU, which may suggest the presence of an unseen outer planet (q1 Eri c).

Published
2008
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4. Herschel and Beyond: FIR and Submillimetre Space Missions and Possible Synergies with Antarctic Astronomy

Author

Göran Pilbratt, Albrecht Poglitsch, Matthew Joseph Griffin, and T. de Graauw

Subjects
Physics, Photometry (astronomy), Far infrared, Space and Planetary Science, Payload, General Engineering, Astronomy, Astronomy and Astrophysics, Space astronomy, Space exploration, Space observatory
Abstract

The Herschel Space Observatory is the fourth cornerstone mission in the European Space Agency (ESA) science programme, and is scheduled for launch in late 2008. It will perform imaging photometry and spectroscopy at far infrared and submillimetre wavelengths, covering approximately the 60–670 m range. The three payload instruments are briefly described, and examples of their scientific capabilities are given from the Guaranteed Time Key Projects which have already been approved. Prospects for future far infrared/submillimetre space astronomy are briefly reviewed, and the implications for possible Antarctic facilities operating in this spectral region are discussed.

Published
2008
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5. Hi-GAL, the Herschel infrared Galactic Plane Survey: photometric maps and compact source catalogues First data release for the inner Milky Way:+68 degrees >= l >=-70 degrees

Author

Molinari, S., Schisano, E., Elia, D., Pestalozzi, M., Traficante, A., Pezzuto, S., Swinyard, B. M., Noriega Crespo, A., Bally, J., Moore, T. J. T., Plume, R., Zavagno, A., di Giorgio, A. M., Liu, S. J., Pilbratt, G. L., Mottram, J. C., Russeil, D., Piazzo, L., Veneziani, M., Benedettini, M., Calzoletti, L., Faustini, F., Natoli, Paolo, Piacentini, F., Merello, M., Palmese, A., Del Grande, R., Polychroni, D., Ryg, K. L. J., Polenta, G., Barlow, M. J., Bernard, J. P., Martin, P. G., Testi, L., Ali, B., Andre, P., Beltran, M. T., Billot, N., Carey, S., Cesaroni, R., Compiegne, M., Eden, D., Fukui, Y., Garcia Lario, P., Hoare, M. G., Huang, M., Joncas, G., Lim, T. L., Lord, . D., Martinavarro Armengol, S., Motte, F., Paladini, R., Paradis, D., Peretto, N., Robitaille, T., Schilke, P., Schneider, N., Schulz, B., Sibthorpe, B., Strafella, F., Thompson, M. A., Umana, G., Ward Thompson, D., and Wyrowski, F.

Subjects
infrared: ISM, techniques: photometric, stars: formation, extinction, dust, extinction, infrared: ISM, stars: formation, Galaxy: disk, methods: data analysis , techniques: photometric, dust, methods: data analysis, NO, Galaxy: disk, QB
Abstract

Aims. We present the first public release of high-quality data products (DR1) from Hi-GAL, the Herschel infrared Galactic Plane Survey. Hi-GAL is the keystone of a suite of continuum Galactic plane surveys from the near-IR to the radio and covers five wavebands at 70, 160, 250, 350 and 500 μm, encompassing the peak of the spectral energy distribution of cold dust for 8 ≲ T ≲ 50 K. This first Hi-GAL data release covers the inner Milky Way in the longitude range 68° ≳ ℓ ≳ −70° in a | b | ≤ 1° latitude strip.\ud Methods. Photometric maps have been produced with the ROMAGAL pipeline, which optimally capitalizes on the excellent sensitivity and stability of the bolometer arrays of the Herschel PACS and SPIRE photometric cameras. It delivers images of exquisite quality and dynamical range, absolutely calibrated with Planck and IRAS, and recovers extended emission at all wavelengths and all spatial scales, from the point-spread function to the size of an entire 2°× 2° “tile” that is the unit observing block of the survey. The compact source catalogues were generated with the CuTEx algorithm, which was specifically developed to optimise source detection and extraction in the extreme conditions of intense and spatially varying background that are found in the Galactic plane in the thermal infrared.\ud Results. Hi-GAL DR1 images are cirrus noise limited and reach the 1σ-rms predicted by the Herschel Time Estimators for parallel-mode observations at 60′′ s-1 scanning speed in relatively low cirrus emission regions. Hi-GAL DR1 images will be accessible through a dedicated web-based image cutout service. The DR1 Compact Source Catalogues are delivered as single-band photometric lists containing, in addition to source position, peak, and integrated flux and source sizes, a variety of parameters useful to assess the quality and reliability of the extracted sources. Caveats and hints to help in this assessment are provided. Flux completeness limits in all bands are determined from extensive synthetic source experiments and greatly depend on the specific line of sight along the Galactic plane because the background strongly varies as a function of Galactic longitude. Hi-GAL DR1 catalogues contain 123210, 308509, 280685, 160972, and 85460 compact sources in the five bands.

Published
2016

6. The molecular disk surrounding the protostellar binary L1551 IRS5

Author

J. A. Tauber, Göran Pilbratt, C. V. M. Fridlund, Per Bergman, and Glenn J. White

Subjects
Physics, Astronomy, Astronomy and Astrophysics, Astrophysics, Radius, Isotopomers, Core (optical fiber), Space and Planetary Science, TheoryofComputation_ANALYSISOFALGORITHMSANDPROBLEMCOMPLEXITY, Perpendicular, Protostar, Outflow, Line (formation), Envelope (waves)
Abstract

The inner three arcminutes surrounding the Class 0/1 binary protostar L1551 IRS5 have been observed using the J=1→0 transitions of the HCO+, H13CO+, 12CO and 13CO molecular species. Since the line core of HCO+ is self reversed over a substantial part of our map, observations of isotopomers such as H13CO+ are required in order to estimate the mass of the molecular gas in the immediate vicinity of IRS5. Our observations demonstrate the presence of a large ( ~ 7000 AU radius) dense, possibly rotating, molecular disk with a mass of a few M⊙ oriented perpendicular to the major axis of an extended molecular outflow. The disk is surrounded by an envelope with a radius of ~ 10 000 AU that contains two massive (each ~ 1 M⊙) clumps. One of these features appears to be kinematically disconnected from both the disk and the molecular outflow.

Published
2002
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7. The ESA Herschel Space Observatory: first year in-flight and early highlights

Author

Göran Pilbratt

Subjects
Physics, Space and Planetary Science, Launched, General Engineering, Astronomy, Astronomy and Astrophysics, Point (geometry), Astrophysics, Space observatory
Abstract

The ESA Herschel Space Observatory was successfully launched on 14 May 2009, and is currently operating in its routine science phase. Due to the rapidly evolving nature of the mission at this point a short summary with pointers to more up-to-date additional information is provided here.

Published
2011
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8. Hi-GAL, theHerschelinfrared Galactic Plane Survey: photometric maps and compact source catalogues

Author

Molinari, S., Schisano, E., Elia, D., Pestalozzi, M., Traficante, A., Pezzuto, S., Swinyard, B. M., Noriega-Crespo, A., Bally, J., Moore, T. J. T., Plume, R., Zavagno, A., di Giorgio, A. M., Liu, S. J., Pilbratt, G. L., Mottram, J. C., Russeil, D., Piazzo, L., Veneziani, M., Benedettini, M., Calzoletti, L., Faustini, F., Natoli, P., Piacentini, F., Merello, M., Palmese, A., Del Grande, R., Polychroni, D., Rygl, K. L. J., Polenta, G., Barlow, M. J., Bernard, J.-P., Martin, P. G., Testi, L., Ali, B., André, P., Beltrán, M. T., Billot, N., Carey, S., Cesaroni, R., Compiègne, M., Eden, D., Fukui, Y., Garcia-Lario, P., Hoare, M. G., Huang, M., Joncas, G., Lim, T. L., Lord, S. D., Martinavarro-Armengol, S., Motte, F., Paladini, R., Paradis, D., Peretto, N., Robitaille, T., Schilke, P., Schneider, N., Schulz, B., Sibthorpe, B., Strafella, F., Thompson, M. A., Umana, G., Ward-Thompson, Derek, Wyrowski, F., Molinari, S., Schisano, E., Elia, D., Pestalozzi, M., Traficante, A., Pezzuto, S., Swinyard, B. M., Noriega-Crespo, A., Bally, J., Moore, T. J. T., Plume, R., Zavagno, A., di Giorgio, A. M., Liu, S. J., Pilbratt, G. L., Mottram, J. C., Russeil, D., Piazzo, L., Veneziani, M., Benedettini, M., Calzoletti, L., Faustini, F., Natoli, P., Piacentini, F., Merello, M., Palmese, A., Del Grande, R., Polychroni, D., Rygl, K. L. J., Polenta, G., Barlow, M. J., Bernard, J.-P., Martin, P. G., Testi, L., Ali, B., André, P., Beltrán, M. T., Billot, N., Carey, S., Cesaroni, R., Compiègne, M., Eden, D., Fukui, Y., Garcia-Lario, P., Hoare, M. G., Huang, M., Joncas, G., Lim, T. L., Lord, S. D., Martinavarro-Armengol, S., Motte, F., Paladini, R., Paradis, D., Peretto, N., Robitaille, T., Schilke, P., Schneider, N., Schulz, B., Sibthorpe, B., Strafella, F., Thompson, M. A., Umana, G., Ward-Thompson, Derek, and Wyrowski, F.

Abstract

Aims. We present the first public release of high-quality data products (DR1) from Hi-GAL, the Herschel infrared Galactic Plane Survey. Hi-GAL is the keystone of a suite of continuum Galactic plane surveys from the near-IR to the radio and covers five wavebands at 70, 160, 250, 350 and 500 µm, encompassing the peak of the spectral energy distribution of cold dust for 8 < T < 50 K. This first Hi-GAL data release covers the inner Milky Way in the longitude range 68◦ > t > −70◦ in a |b| ≤ 1◦ latitude strip. ∼ ∼ ∼ ∼ Methods. Photometric maps have been produced with the ROMAGAL pipeline, which optimally capitalizes on the excellent sensitivity and stability of the bolometer arrays of the Herschel PACS and SPIRE photometric cameras. It delivers images of exquisite quality and dynamical range, absolutely calibrated with Planck and IRAS, and recovers extended emission at all wavelengths and all spatial scales, from the point-spread function to the size of an entire 2◦ × 2◦ “tile” that is the unit observing block of the survey. The compact source catalogues were generated with the CuTEx algorithm, which was specifically developed to optimise source detection and extraction in the extreme conditions of intense and spatially varying background that are found in the Galactic plane in the thermal infrared. Results. Hi-GAL DR1 images are cirrus noise limited and reach the 1σ-rms predicted by the Herschel Time Estimators for parallel-mode obser- vations at 6011 s−1 scanning speed in relatively low cirrus emission regions. Hi-GAL DR1 images will be accessible through a dedicated web-based image cutout service. The DR1 Compact Source Catalogues are delivered as single-band photometric lists containing, in addition to source posi- tion, peak, and integrated flux and source sizes, a variety of parameters useful to assess the quality and reliability of the extracted sources. Caveats and hints to help in this assessment are provided. Flux completeness limits in all bands are determined

Published
2016

9. Incidence of debris discs around FGK stars in the solar neighbourhood

Author

Montesinos, B., primary, Eiroa, C., additional, Krivov, A. V., additional, Marshall, J. P., additional, Pilbratt, G. L., additional, Liseau, R., additional, Mora, A., additional, Maldonado, J., additional, Wolf, S., additional, Ertel, S., additional, Bayo, A., additional, Augereau, J.-C., additional, Heras, A. M., additional, Fridlund, M., additional, Danchi, W. C., additional, Solano, E., additional, Kirchschlager, F., additional, del Burgo, C., additional, and Montes, D., additional

Published
2016
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10. Hi-GAL, theHerschelinfrared Galactic Plane Survey: photometric maps and compact source catalogues

Author

Molinari, S., primary, Schisano, E., additional, Elia, D., additional, Pestalozzi, M., additional, Traficante, A., additional, Pezzuto, S., additional, Swinyard, B. M., additional, Noriega-Crespo, A., additional, Bally, J., additional, Moore, T. J. T., additional, Plume, R., additional, Zavagno, A., additional, di Giorgio, A. M., additional, Liu, S. J., additional, Pilbratt, G. L., additional, Mottram, J. C., additional, Russeil, D., additional, Piazzo, L., additional, Veneziani, M., additional, Benedettini, M., additional, Calzoletti, L., additional, Faustini, F., additional, Natoli, P., additional, Piacentini, F., additional, Merello, M., additional, Palmese, A., additional, Del Grande, R., additional, Polychroni, D., additional, Rygl, K. L. J., additional, Polenta, G., additional, Barlow, M. J., additional, Bernard, J.-P., additional, Martin, P. G., additional, Testi, L., additional, Ali, B., additional, André, P., additional, Beltrán, M. T., additional, Billot, N., additional, Carey, S., additional, Cesaroni, R., additional, Compiègne, M., additional, Eden, D., additional, Fukui, Y., additional, Garcia-Lario, P., additional, Hoare, M. G., additional, Huang, M., additional, Joncas, G., additional, Lim, T. L., additional, Lord, S. D., additional, Martinavarro-Armengol, S., additional, Motte, F., additional, Paladini, R., additional, Paradis, D., additional, Peretto, N., additional, Robitaille, T., additional, Schilke, P., additional, Schneider, N., additional, Schulz, B., additional, Sibthorpe, B., additional, Strafella, F., additional, Thompson, M. A., additional, Umana, G., additional, Ward-Thompson, D., additional, and Wyrowski, F., additional

Published
2016
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11. Herscheldetects oxygen in theβPictoris debris disk

Author

Brandeker, A., primary, Cataldi, G., additional, Olofsson, G., additional, Vandenbussche, B., additional, Acke, B., additional, Barlow, M. J., additional, Blommaert, J. A. D. L., additional, Cohen, M., additional, Dent, W. R. F., additional, Dominik, C., additional, Di Francesco, J., additional, Fridlund, M., additional, Gear, W. K., additional, Glauser, A. M., additional, Greaves, J. S., additional, Harvey, P. M., additional, Heras, A. M., additional, Hogerheijde, M. R., additional, Holland, W. S., additional, Huygen, R., additional, Ivison, R. J., additional, Leeks, S. J., additional, Lim, T. L., additional, Liseau, R., additional, Matthews, B. C., additional, Pantin, E., additional, Pilbratt, G. L., additional, Royer, P., additional, Sibthorpe, B., additional, Waelkens, C., additional, and Walker, H. J., additional

Published
2016
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12. Filamentary structure and magnetic field orientation in Musca

Author

Cox, N. L. J., primary, Arzoumanian, D., additional, André, Ph., additional, Rygl, K. L. J., additional, Prusti, T., additional, Men’shchikov, A., additional, Royer, P., additional, Kóspál, Á., additional, Palmeirim, P., additional, Ribas, A., additional, Könyves, V., additional, Bernard, J.-Ph., additional, Schneider, N., additional, Bontemps, S., additional, Merin, B., additional, Vavrek, R., additional, Alves de Oliveira, C., additional, Didelon, P., additional, Pilbratt, G. L., additional, and Waelkens, C., additional

Published
2016
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14. Infrared study of transitional disks in Ophiuchus withHerschel

Author

Rebollido, Isabel, primary, Merín, Bruno, additional, Ribas, Álvaro, additional, Bustamante, Ignacio, additional, Bouy, Hervé, additional, Riviere-Marichalar, Pablo, additional, Prusti, Timo, additional, Pilbratt, Göran L., additional, André, Philippe, additional, and Ábrahám, Péter, additional

Published
2015
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16. The β Pictoris disk imaged by Herschel PACS and SPIRE [Letter]

Author

Vandenbussche, B., Sibthorpe, B., Acke, B., Pantin, E., Olofsson, G., Waelkens, C., Dominik, C., Barlow, M. J., Blommaert, J. A. D. L., Bouwman, J., Brandeker, A., Cohen, M., De Meester, W., Dent, W. R. F., Exter, K., Di Francesco, J., Fridlund, M., Gear, Walter Kieran, Glauser, A. M., Gomez, Haley Louise, Greaves, J. S., Hargrave, Peter Charles, Harvey, P. M., Henning, Th., Heras, A. M., Hogerheijde, M. R., Holland, W. S., Huygen, R., Ivison, R. J., Jean, C., Leeks, S. J., Lim, T. L., Liseau, R., Matthews, B. C., Naylor, D. A., Pilbratt, G. L., Polehampton, E. T., Regibo, S., Royer, P., Sicilia-Aguilar, A., Swinyard, B. M., Walker, H. J., and Wesson, R.

Subjects
QB
Abstract

We obtained Herschel PACS and SPIRE images of the thermal emission of the debris disk around the A5V star β Pic. The disk is well resolved in the PACS filters at 70, 100, and 160 μm. The surface brightness profiles between 70 and 160 μm show no significant asymmetries along the disk, and are compatible with 90% of the emission between 70 and 160 μm originating in a region closer than 200 AU to the star. Although only marginally resolving the debris disk, the maps obtained in the SPIRE 250–500 μm filters provide full-disk photometry, completing the SED over a few octaves in wavelength that had been previously inaccessible. The small far-infrared spectral index (β = 0.34) indicates that the grain size distribution in the inner disk (

Published
2010

17. Identification of new transitional disk candidates in Lupus withHerschel

Author

Timo Prusti, Álvaro Ribas, Göran Pilbratt, Hervé Bouy, Ignacio Bustamante, Bruno Merín, Ph. André, European Space Astronomy Centre (ESAC), European Space Agency (ESA), European Space Research and Technology Centre (ESTEC), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Agence Spatiale Européenne = European Space Agency (ESA), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), and 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)

Subjects
Physics, Molecular cloud, protoplanetary disks, Initial sample, Lupus (constellation), FOS: Physical sciences, Astronomy and Astrophysics, stars: pre-main sequence, Astrophysics, Planetary system, Space observatory, Photometry (optics), T Tauri star, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Chamaeleon, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], planetary systems, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

New data from the Herschel Space Observatory are broadening our understanding of the physics and evolution of the outer regions of protoplanetary disks in star forming regions. In particular they prove to be useful to identify transitional disk candidates. The goals of this work are to complement the detections of disks and the identification of transitional disk candidates in the Lupus clouds with data from the Herschel Gould Belt Survey. We extracted photometry at 70, 100, 160, 250, 350 and 500 $\mu$m of all spectroscopically confirmed Class II members previously identified in the Lupus regions and analyzed their updated spectral energy distributions. We have detected 34 young disks in Lupus in at least one Herschel band, from an initial sample of 123 known members in the observed fields. Using the criteria defined in Ribas et al. (2013) we have identified five transitional disk candidates in the region. Three of them are new to the literature. Their PACS-70 $\mu$m fluxes are systematically higher than those of normal T Tauri stars in the same associations, as already found in T Cha and in the transitional disks in the Chamaeleon molecular cloud. Herschel efficiently complements mid-infrared surveys for identifying transitional disk candidates and confirms that these objects seem to have substantially different outer disks than the T Tauri stars in the same molecular clouds., Comment: Accepted for publication in A&A. 16 pages, 9 figures, 7 tables

Published
2015
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18. Herschelview of the large-scale structure in the Chamaeleon dark clouds

Author

Alves de Oliveira, C., primary, Schneider, N., additional, Merín, B., additional, Prusti, T., additional, Ribas, Á., additional, Cox, N. L. J., additional, Vavrek, R., additional, Könyves, V., additional, Arzoumanian, D., additional, Puga, E., additional, Pilbratt, G. L., additional, Kóspál, Á., additional, André, Ph., additional, Didelon, P., additional, Men’shchikov, A., additional, Royer, P., additional, Waelkens, C., additional, Bontemps, S., additional, Winston, E., additional, and Spezzi, L., additional

Published
2014
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19. Correlations between the stellar, planetary, and debris components of exoplanet systems observed byHerschel

Author

Marshall, J. P., primary, Moro-Martín, A., additional, Eiroa, C., additional, Kennedy, G., additional, Mora, A., additional, Sibthorpe, B., additional, Lestrade, J.-F., additional, Maldonado, J., additional, Sanz-Forcada, J., additional, Wyatt, M. C., additional, Matthews, B., additional, Horner, J., additional, Montesinos, B., additional, Bryden, G., additional, del Burgo, C., additional, Greaves, J. S., additional, Ivison, R. J., additional, Meeus, G., additional, Olofsson, G., additional, Pilbratt, G. L., additional, and White, G. J., additional

Published
2014
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20. How dusty isα Centauri?

Author

Wiegert, J., primary, Liseau, R., additional, Thébault, P., additional, Olofsson, G., additional, Mora, A., additional, Bryden, G., additional, Marshall, J. P., additional, Eiroa, C., additional, Montesinos, B., additional, Ardila, D., additional, Augereau, J. C., additional, Bayo Aran, A., additional, Danchi, W. C., additional, del Burgo, C., additional, Ertel, S., additional, Fridlund, M. C. W., additional, Hajigholi, M., additional, Krivov, A. V., additional, Pilbratt, G. L., additional, Roberge, A., additional, White, G. J., additional, and Wolf, S., additional

Published
2014
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21. Correlations between the stellar, planetary, and debris components of exoplanet systems observed byHerschel

Author

G. Olofsson, A. Mora, Brenda C. Matthews, B. Sibthorpe, Jonathan P. Marshall, Grant M. Kennedy, Jesús E. Maldonado, G. Bryden, Jonathan Horner, Jorge Sanz-Forcada, Gwendolyn Meeus, Jane Greaves, Rob Ivison, J.-F. Lestrade, C. del Burgo, Carlos Eiroa, Göran Pilbratt, Amaya Moro-Martin, Mark C. Wyatt, Benjamin Montesinos, G. J. White, Science & Technology Facilities Council, and University of St Andrews. School of Physics and Astronomy

Subjects
Solar System, 010504 meteorology & atmospheric sciences, Metallicity, FOS: Physical sciences, planetary systems [Infrared], Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Luminosity, Effective temperature, Infrared: planetary systems, Planet, 0103 physical sciences, Hot Jupiter, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QB, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Infrared: star, Planet formation, Physics, Second generation, Dust, Astronomy and Astrophysics, Circumstellar matter, Stars, Exoplanet, Extrasolar planets, Circumstellar matters, Dust temperatures, Luminance, 13. Climate action, Space and Planetary Science, stars [Infrared], Debris, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics, Solar system, Planet-disk interactions
Abstract

The $\textit{Herschel}$ DEBRIS, DUNES and GT programmes observed 37 exoplanet host stars within 25 pc at 70, 100 and 160 $\mu$m with the sensitivity to detect far-infrared excess emission at flux density levels only an order of magnitude greater than that of the Solar system's Edgeworth-Kuiper belt. Here we present an analysis of that sample, using it to more accurately determine the (possible) level of dust emission from these exoplanet host stars and thereafter determine the links between the various components of these exoplanetary systems through statistical analysis. We have fitted the flux densities measured from recent \textit{Herschel} observations with a simple two parameter ($T_{d}$, $L_{\rm IR}/L_{\star}$) black body model (or to the 3-$\sigma$ upper limits at 100 $\mu$m). From this uniform approach we calculate the fractional luminosity, radial extent, dust temperature and disc mass. We then plotted the calculated dust luminosity or upper limits against the stellar properties, e.g. effective temperature, metallicity, age, and identified correlations between these parameters. A total of eleven debris discs are identified around the 37 stars in the sample. An incidence of ten cool debris discs around the Sun-like exoplanet host stars (29 $\pm$ 9 %) is consistent with the detection rate found by DUNES (20.2 $\pm$ 2.0 %). For the debris disc systems, the dust temperatures range from 20 to 80 K, and fractional luminosities ($L_{\rm IR}/L_{\star}$) between 2.4 $\times$10$^{-6}$ and 4.1 $\times$10$^{-4}$. In the case of non-detections, we calculated typical 3-$\sigma$ upper limits to the dust fractional luminosities of a few $\times10^{-6}$. We recover the previously identified correlation between stellar metallicity and hot Jupiter planets in our data set. We find a correlation between the increased presence of dust, lower planet masses and lower stellar metallicities. (abridged), Comment: 14 pages, 2 figures, 4 tables, A&A accepted

Published
2014
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22. Potential multi-component structure of the debris disk around HIP 17439 revealed byHerschel/DUNES

Author

Ertel, S., primary, Marshall, J. P., additional, Augereau, J.-C., additional, Krivov, A. V., additional, Löhne, T., additional, Eiroa, C., additional, Mora, A., additional, del Burgo, C., additional, Montesinos, B., additional, Bryden, G., additional, Danchi, W., additional, Kirchschlager, F., additional, Liseau, R., additional, Maldonado, J., additional, Pilbratt, G. L., additional, Schüppler, Ch., additional, Thébault, Ph., additional, White, G. J., additional, and Wolf, S., additional

Published
2014
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23. Herschelobservations of the debris disc around HIP 92043

Author

Marshall, J. P., primary, Krivov, A. V., additional, del Burgo, C., additional, Eiroa, C., additional, Mora, A., additional, Montesinos, B., additional, Ertel, S., additional, Bryden, G., additional, Liseau, R., additional, Augereau, J.-C., additional, Bayo, A., additional, Danchi, W., additional, Löhne, T., additional, Maldonado, J., additional, Pilbratt, G. L., additional, Stapelfeldt, K., additional, Thebault, P., additional, White, G. J., additional, and Wolf, S., additional

Published
2013
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24. TheHerschelGould Belt Survey in Chamaeleon II

Author

Spezzi, L., primary, Cox, N. L. J., additional, Prusti, T., additional, Merín, B., additional, Ribas, Á., additional, Alves de Oliveira, C., additional, Winston, E., additional, Kóspál, Á., additional, Royer, P., additional, Vavrek, R., additional, André, Ph., additional, Pilbratt, G. L., additional, Testi, L., additional, Bressert, E., additional, Ricci, L., additional, Men’shchikov, A., additional, and Könyves, V., additional

Published
2013
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25. DUst around NEarby Stars. The survey observational results

Author

Eiroa, C., primary, Marshall, J. P., additional, Mora, A., additional, Montesinos, B., additional, Absil, O., additional, Augereau, J. Ch., additional, Bayo, A., additional, Bryden, G., additional, Danchi, W., additional, del Burgo, C., additional, Ertel, S., additional, Fridlund, M., additional, Heras, A. M., additional, Krivov, A. V., additional, Launhardt, R., additional, Liseau, R., additional, Löhne, T., additional, Maldonado, J., additional, Pilbratt, G. L., additional, Roberge, A., additional, Rodmann, J., additional, Sanz-Forcada, J., additional, Solano, E., additional, Stapelfeldt, K., additional, Thébault, P., additional, Wolf, S., additional, Ardila, D., additional, Arévalo, M., additional, Beichmann, C., additional, Faramaz, V., additional, González-García, B. M., additional, Gutiérrez, R., additional, Lebreton, J., additional, Martínez-Arnáiz, R., additional, Meeus, G., additional, Montes, D., additional, Olofsson, G., additional, Su, K. Y. L., additional, White, G. J., additional, Barrado, D., additional, Fukagawa, M., additional, Grün, E., additional, Kamp, I., additional, Lorente, R., additional, Morbidelli, A., additional, Müller, S., additional, Mutschke, H., additional, Nakagawa, T., additional, Ribas, I., additional, and Walker, H., additional

Published
2013
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26. Identification of transitional disks in Chamaeleon withHerschel

Author

Ribas, Á., primary, Merín, B., additional, Bouy, H., additional, Alves de Oliveira, C., additional, Ardila, D. R., additional, Puga, E., additional, Kóspál, Á., additional, Spezzi, L., additional, Cox, N. L. J., additional, Prusti, T., additional, Pilbratt, G. L., additional, André, Ph., additional, Matrà, L., additional, and Vavrek, R., additional

Published
2013
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27. Hi-GAL, the Herschel infrared Galactic Plane Survey: photometric maps and compact source catalogues: First data release for the inner Milky Way: +68◦ ≥ l ≥ −70◦.

Author

Molinari, S., Schisano, E., Elia, D., Pestalozzi, M., Traficante, A., Pezzuto, S., Swinyard, B. M., Noriega-Crespo, A., Bally, J., Moore, T. J. T., Plume, R., Zavagno, A., di Giorgio, A. M., Liu, S. J., Pilbratt, G. L., Mottram, J. C., Russeil, D., Piazzo, L., Veneziani, M., and Benedettini, M.

Abstract

Aims. We present the first public release of high-quality data products (DR1) from Hi-GAL, the Herschel infrared Galactic Plane Survey. Hi-GAL is the keystone of a suite of continuum Galactic plane surveys from the near-IR to the radio and covers five wavebands at 70, 160, 250, 350 and 500 μm, encompassing the peak of the spectral energy distribution of cold dust for 8 ≲ T ≲ 50 K. This first Hi-GAL data release covers the inner Milky Way in the longitude range 68° ≳ ℓ ≳ −70° in a | b | ≤ 1° latitude strip. Methods. Photometric maps have been produced with the ROMAGAL pipeline, which optimally capitalizes on the excellent sensitivity and stability of the bolometer arrays of the Herschel PACS and SPIRE photometric cameras. It delivers images of exquisite quality and dynamical range, absolutely calibrated with Planck and IRAS, and recovers extended emission at all wavelengths and all spatial scales, from the point-spread function to the size of an entire 2°× 2° “tile” that is the unit observing block of the survey. The compact source catalogues were generated with the CuTEx algorithm, which was specifically developed to optimise source detection and extraction in the extreme conditions of intense and spatially varying background that are found in the Galactic plane in the thermal infrared. Results. Hi-GAL DR1 images are cirrus noise limited and reach the 1σ-rms predicted by the Herschel Time Estimators for parallel-mode observations at 60′′ s-1 scanning speed in relatively low cirrus emission regions. Hi-GAL DR1 images will be accessible through a dedicated web-based image cutout service. The DR1 Compact Source Catalogues are delivered as single-band photometric lists containing, in addition to source position, peak, and integrated flux and source sizes, a variety of parameters useful to assess the quality and reliability of the extracted sources. Caveats and hints to help in this assessment are provided. Flux completeness limits in all bands are determined from extensive synthetic source experiments and greatly depend on the specific line of sight along the Galactic plane because the background strongly varies as a function of Galactic longitude. Hi-GAL DR1 catalogues contain 123210, 308509, 280685, 160972, and 85460 compact sources in the five bands. [ABSTRACT FROM AUTHOR]

Published
2016
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28. α Centauri A in the far infrared

Author

Liseau, R., primary, Montesinos, B., additional, Olofsson, G., additional, Bryden, G., additional, Marshall, J. P., additional, Ardila, D., additional, Bayo Aran, A., additional, Danchi, W. C., additional, del Burgo, C., additional, Eiroa, C., additional, Ertel, S., additional, Fridlund, M. C. W., additional, Krivov, A. V., additional, Pilbratt, G. L., additional, Roberge, A., additional, Thébault, P., additional, Wiegert, J., additional, and White, G. J., additional

Published
2013
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29. A newHerschelview of the young star T54: not a transitional disk?

Author

Matrà, L., primary, Merín, B., additional, Alves de Oliveira, C., additional, Huélamo, N., additional, Kóspál, A., additional, Cox, N. L. J., additional, Ribas, Á., additional, Puga, E., additional, Vavrek, R., additional, Royer, P., additional, Prusti, T., additional, Pilbratt, G. L., additional, and André, P., additional

Published
2012
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30. Herschelfar-IR observations of the Chamaeleon molecular cloud complex

Author

Winston, E., primary, Cox, N. L. J., additional, Prusti, T., additional, Merín, B., additional, Ribas, A., additional, Royer, P., additional, Vavrek, R., additional, Puga, E., additional, André, Ph., additional, Men’shchikov, A., additional, Könyves, V., additional, Kóspál, Á., additional, Alves de Oliveira, C., additional, Pilbratt, G. L., additional, and Waelkens, C., additional

Published
2012
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31. The dusty environment of HD 97300 as seen byHerschelandSpitzer

Author

Kóspál, Á., primary, Prusti, T., additional, Cox, N. L. J., additional, Pilbratt, G. L., additional, André, Ph., additional, Alves de Oliveira, C., additional, Winston, E., additional, Merín, B., additional, Ribas, A., additional, Royer, P., additional, Vavrek, R., additional, and Waelkens, C., additional

Published
2012
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32. A peculiar class of debris disks fromHerschel/DUNES

Author

Ertel, S., primary, Wolf, S., additional, Marshall, J. P., additional, Eiroa, C., additional, Augereau, J.-C., additional, Krivov, A. V., additional, Löhne, T., additional, Absil, O., additional, Ardila, D., additional, Arévalo, M., additional, Bayo, A., additional, Bryden, G., additional, del Burgo, C., additional, Greaves, J., additional, Kennedy, G., additional, Lebreton, J., additional, Liseau, R., additional, Maldonado, J., additional, Montesinos, B., additional, Mora, A., additional, Pilbratt, G. L., additional, Sanz-Forcada, J., additional, Stapelfeldt, K., additional, and White, G. J., additional

Published
2012
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33. Herschelimages of Fomalhaut

Author

Acke, B., primary, Min, M., additional, Dominik, C., additional, Vandenbussche, B., additional, Sibthorpe, B., additional, Waelkens, C., additional, Olofsson, G., additional, Degroote, P., additional, Smolders, K., additional, Pantin, E., additional, Barlow, M. J., additional, Blommaert, J. A. D. L., additional, Brandeker, A., additional, De Meester, W., additional, Dent, W. R. F., additional, Exter, K., additional, Di Francesco, J., additional, Fridlund, M., additional, Gear, W. K., additional, Glauser, A. M., additional, Greaves, J. S., additional, Harvey, P. M., additional, Henning, Th., additional, Hogerheijde, M. R., additional, Holland, W. S., additional, Huygen, R., additional, Ivison, R. J., additional, Jean, C., additional, Liseau, R., additional, Naylor, D. A., additional, Pilbratt, G. L., additional, Polehampton, E. T., additional, Regibo, S., additional, Royer, P., additional, Sicilia-Aguilar, A., additional, and Swinyard, B. M., additional

Published
2012
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34. Modelling the huge,Herschel-resolved debris ring around HD 207129

Author

Löhne, T., primary, Augereau, J.-C., additional, Ertel, S., additional, Marshall, J. P., additional, Eiroa, C., additional, Mora, A., additional, Absil, O., additional, Stapelfeldt, K., additional, Thébault, P., additional, Bayo, A., additional, del Burgo, C., additional, Danchi, W., additional, Krivov, A. V., additional, Lebreton, J., additional, Letawe, G., additional, Magain, P., additional, Maldonado, J., additional, Montesinos, B., additional, Pilbratt, G. L., additional, White, G. J., additional, and Wolf, S., additional

Published
2012
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35. Herscheldiscovery of a new class of cold, faint debris discs

Author

Eiroa, C., primary, Marshall, J. P., additional, Mora, A., additional, Krivov, A. V., additional, Montesinos, B., additional, Absil, O., additional, Ardila, D., additional, Arévalo, M., additional, Augereau, J.-Ch., additional, Bayo, A., additional, Danchi, W., additional, del Burgo, C., additional, Ertel, S., additional, Fridlund, M., additional, González-García, B. M., additional, Heras, A. M., additional, Lebreton, J., additional, Liseau, R., additional, Maldonado, J., additional, Meeus, G., additional, Montes, D., additional, Pilbratt, G. L., additional, Roberge, A., additional, Sanz-Forcada, J., additional, Stapelfeldt, K., additional, Thébault, P., additional, White, G. J., additional, and Wolf, S., additional

Published
2011
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36. AHerschelresolved far-infrared dust ring around HD 207129

Author

Marshall, J. P., primary, Löhne, T., additional, Montesinos, B., additional, Krivov, A. V., additional, Eiroa, C., additional, Absil, O., additional, Bryden, G., additional, Maldonado, J., additional, Mora, A., additional, Sanz-Forcada, J., additional, Ardila, D., additional, Augereau, J.-Ch., additional, Bayo, A., additional, del Burgo, C., additional, Danchi, W., additional, Ertel, S., additional, Fedele, D., additional, Fridlund, M., additional, Lebreton, J., additional, González-García, B. M., additional, Liseau, R., additional, Meeus, G., additional, Müller, S., additional, Pilbratt, G. L., additional, Roberge, A., additional, Stapelfeldt, K., additional, Thébault, P., additional, White, G. J., additional, and Wolf, S., additional

Published
2011
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38. Herschelfar-IR observations of the Chamaeleon molecular cloud complex

Author

Timo Prusti, Pierre Royer, Ágnes Kóspál, E. Winston, Göran Pilbratt, Álvaro Ribas, Vera Könyves, Ph. André, Alexander Men'shchikov, Elena Puga, C. Waelkens, Nick L. J. Cox, C. Alves de Oliveira, Bruno Merín, and R. Vavrek

Subjects
Physics, Stars, Space and Planetary Science, Star formation, Molecular cloud, Young stellar object, Chamaeleon, Protostar, Astronomy, Astronomy and Astrophysics, Astrophysics, Stellar evolution, Galaxy
Abstract

Context. The Herschel Gould Belt survey of nearby star forming regions is providing great insights into the early stages of the formation and the evolution of stars and their circumstellar disks. The Chamaeleon I dark cloud is an elongated region of dense dust and gas where star formation is ongoing in two centres, a northern region centred on Ced 112 and a southern cluster subdivided into the two regions Ced 110 and 111. Aims. In this initial study we present Herschel data of previously identified young stellar objects (YSOs) in the cluster, focusing on the spatial distribution of the YSOs and the determination of the relative colours of the protostars and the disk-bearing stars in Chamaeleon I. Methods. Chamaeleon I has been observed as part of the Herschel Gould Belt Survey, using the PACS and SPIRE parallel mode imaging at 70, 160, 250, 350, and 500 μm. Source extraction was performed using the getsources software. Results. We have detected 397 sources over the five available PACS and SPIRE bands, and through comparison with previously identified objects in the cluster we have identified 49 YSOs, 4 bright nebular emission features, five CO clumps, and twenty-eight candidate prestellar or starless cores in the Herschel sample. The remaining sample consists of candidate prestellar cores, condensations within the cloud, or background galaxies. The Herschel detected YSOs are highly clustered and mainly associated with the three known Cederblad groups. The observations clearly show that the young stars are forming coincident with the denser regions of cold dust and gas, visible at longer Herschel wavelengths. Those YSOs detected with Herschel were found to have an IRAC m3.6 μm < 10. No difference was found in the Herschel colours between the class I and class II young stars, however the class I sources were brighter than the class II at most Herschel wavelengths. One class III star and three transition disks are detected.

Published
2012
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39. Modelling the huge,Herschel-resolved debris ring around HD 207129

Author

Jesus Maldonado, K. R. Stapelfeldt, Jean-Pierre Lebreton, A. Mora, Pierre Magain, Göran Pilbratt, Torsten Löhne, Sebastian Wolf, P. Thébault, Carlos Eiroa, Glenn J. White, Benjamin Montesinos, Amelia Bayo, C. del Burgo, Jonathan P. Marshall, Géraldine Letawe, Olivier Absil, William C. Danchi, Steve Ertel, Alexander V. Krivov, Jean-Charles Augereau, Universitätsklinikum Friedrich-Schiller-University (FSU), Friedrich-Schiller-Universität = Friedrich Schiller University Jena [Jena, Germany], Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Steward Observatory, University of Arizona, Universidad Autónoma de Madrid (UAM), Departamento de Microbiología y Parasitología [Lugo, Spain], Laboratorio de Referencia de E. coli [Lugo, Spain] (LREC), Universidade de Santiago de Compostela [Spain] (USC )-Universidade de Santiago de Compostela [Spain] (USC ), Université de Liège, NASA Goddard Space Flight Center (GSFC), Polymères Biopolymères Surfaces (PBS), Université de Rouen Normandie (UNIROUEN), Normandie Université (NU)-Normandie Université (NU)-Institut national des sciences appliquées Rouen Normandie (INSA Rouen Normandie), Institut National des Sciences Appliquées (INSA)-Normandie Université (NU)-Institut National des Sciences Appliquées (INSA)-Institut Normand de Chimie Moléculaire Médicinale et Macromoléculaire (INC3M), Université de Caen Normandie (UNICAEN), Normandie Université (NU)-Normandie Université (NU)-École Nationale Supérieure d'Ingénieurs de Caen (ENSICAEN), Normandie Université (NU)-Université Le Havre Normandie (ULH), Normandie Université (NU)-Université de Rouen Normandie (UNIROUEN), Normandie Université (NU)-Institut national des sciences appliquées Rouen Normandie (INSA Rouen Normandie), Institut National des Sciences Appliquées (INSA)-Normandie Université (NU)-Institut National des Sciences Appliquées (INSA)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Université de Caen Normandie (UNICAEN), Normandie Université (NU)-École Nationale Supérieure d'Ingénieurs de Caen (ENSICAEN), Normandie Université (NU)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Instituto Nacional de Astrofísica, Óptica y Electrónica (INAOE), Instituto de Astrofisica de Canarias (IAC), University of Granada/Dept of Paediatrics, Universidad de Granada = University of Granada (UGR), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), UAM. Departamento de Física Teórica, Universidad Autonoma de Madrid (UAM), Institut national des sciences appliquées Rouen Normandie (INSA Rouen Normandie), Institut National des Sciences Appliquées (INSA)-Normandie Université (NU)-Institut National des Sciences Appliquées (INSA)-Normandie Université (NU)-Institut de Chimie du CNRS (INC)-Institut Normand de Chimie Moléculaire Médicinale et Macromoléculaire (INC3M), Institut de Chimie du CNRS (INC)-École Nationale Supérieure d'Ingénieurs de Caen (ENSICAEN), Institut National des Sciences Appliquées (INSA)-Normandie Université (NU)-Institut National des Sciences Appliquées (INSA)-Université Le Havre Normandie (ULH), Normandie Université (NU)-Centre National de la Recherche Scientifique (CNRS)-Université de Caen Normandie (UNICAEN), Normandie Université (NU)-Centre National de la Recherche Scientifique (CNRS), University of Granada [Granada], Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), and European Space Agency (ESA)

Subjects
Planetesimal, 010504 meteorology & atmospheric sciences, Interplanetary medium, Astrophysics, 01 natural sciences, 0103 physical sciences, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Cosmic dust, [PHYS]Physics [physics], Physics, Debris disk, Infrared excess, Física, Astronomy, Astronomy and Astrophysics, Stars: individual: HD 207129, Debris, Fomalhaut, 13. Climate action, Space and Planetary Science, Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, individual: HD 207129 [Stars], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Astronomy and Astrophysics 537 (2013): A110 Reproduced with permission from Astronomy & Astrophysics, Debris disks, which are inferred from the observed infrared excess to be ensembles of dust, rocks, and probably planetesimals, are common features of stellar systems. As the mechanisms of their formation and evolution are linked to those of planetary bodies, they provide valuable information. The few well-resolved debris disks are even more valuable because they can serve as modeling benchmarks and help resolve degeneracies in modelling aspects such as typical grain sizes and distances. Here, we present an analysis of the HD 207129 debris disk, based on its well-covered spectral energy distribution and Herschel/PACS images obtained in the framework of the DUNES (DUst around NEarby Stars) programme. We use an empirical power-law approach to the distribution of dust and we then model the production and removal of dust by means of collisions, direct radiation pressure, and drag forces. The resulting best-fit model contains a total of nearly 10−2 Earth masses in dust, with typical grain sizes in the planetesimal belt ranging from 4 to 7 μm.We constrain the dynamical excitation to be low, which results in very long collisional lifetimes and a drag that notably fills the inner gap, especially at 70 μm. The radial distribution stretches from well within 100 AU in an unusual, outward-rising slope towards a rather sharp outer edge at about 170–190 AU. The inner edge is therefore smoother than that reported for Fomalhaut, but the contribution from the extended halo of barely bound grains is similarly small. Both slowly self-stirring and planetary perturbations could potentially have formed and shaped this disk, Parts of our work were funded by the Deutsche Forschungsgemeinschaft (grants Lo 1715/1-1, Kr 2164/9-1, and Wo 857/7-1). C. Eiroa, J. Maldonado, J. P. Marshall, and B. Montesinos are partly supported by Spanish grant AYA 2008-01727. A. Mora acknowledges support from the Portuguese Fundação para a Ciência e a Tecnologia (grant PEst- E/EEI/UI0066/2011)

Published
2012
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41. HerschelSpace Observatory

Author

Pilbratt, G. L., primary, Riedinger, J. R., additional, Passvogel, T., additional, Crone, G., additional, Doyle, D., additional, Gageur, U., additional, Heras, A. M., additional, Jewell, C., additional, Metcalfe, L., additional, Ott, S., additional, and Schmidt, M., additional

Published
2010
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42. Theβ Pictoris disk imaged byHerschelPACS and SPIRE

Author

Vandenbussche, B., primary, Sibthorpe, B., additional, Acke, B., additional, Pantin, E., additional, Olofsson, G., additional, Waelkens, C., additional, Dominik, C., additional, Barlow, M. J., additional, Blommaert, J. A. D. L., additional, Bouwman, J., additional, Brandeker, A., additional, Cohen, M., additional, De Meester, W., additional, Dent, W. R. F., additional, Exter, K., additional, Di Francesco, J., additional, Fridlund, M., additional, Gear, W. K., additional, Glauser, A. M., additional, Gomez, H. L., additional, Greaves, J. S., additional, Hargrave, P. C., additional, Harvey, P. M., additional, Henning, Th., additional, Heras, A. M., additional, Hogerheijde, M. R., additional, Holland, W. S., additional, Huygen, R., additional, Ivison, R. J., additional, Jean, C., additional, Leeks, S. J., additional, Lim, T. L., additional, Liseau, R., additional, Matthews, B. C., additional, Naylor, D. A., additional, Pilbratt, G. L., additional, Polehampton, E. T., additional, Regibo, S., additional, Royer, P., additional, Sicilia-Aguilar, A., additional, Swinyard, B. M., additional, Walker, H. J., additional, and Wesson, R., additional

Published
2010
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43. Kuiper belts around nearby stars

Author

Nilsson, R., primary, Liseau, R., additional, Brandeker, A., additional, Olofsson, G., additional, Pilbratt, G. L., additional, Risacher, C., additional, Rodmann, J., additional, Augereau, J.-C., additional, Bergman, P., additional, Eiroa, C., additional, Fridlund, M., additional, Thébault, P., additional, and White, G. J., additional

Published
2010
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44. The Vega debris disc: A view fromHerschel

Author

Sibthorpe, B., primary, Vandenbussche, B., additional, Greaves, J. S., additional, Pantin, E., additional, Olofsson, G., additional, Acke, B., additional, Barlow, M. J., additional, Blommaert, J. A. D. L., additional, Bouwman, J., additional, Brandeker, A., additional, Cohen, M., additional, De Meester, W., additional, Dent, W. R. F., additional, Di Francesco, J., additional, Dominik, C., additional, Fridlund, M., additional, Gear, W. K., additional, Glauser, A. M., additional, Gomez, H. L., additional, Hargrave, P. C., additional, Harvey, P. M., additional, Henning, Th., additional, Heras, A. M., additional, Hogerheijde, M. R., additional, Holland, W. S., additional, Ivison, R. J., additional, Leeks, S. J., additional, Lim, T. L., additional, Liseau, R., additional, Matthews, B. C., additional, Naylor, D. A., additional, Pilbratt, G. L., additional, Polehampton, E. T., additional, Regibo, S., additional, Royer, P., additional, Sicilia-Aguilar, A., additional, Swinyard, B. M., additional, Waelkens, C., additional, Walker, H. J., additional, and Wesson, R., additional

Published
2010
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45. Resolving the cold debris disc around a planet-hosting star

Author

Liseau, R., primary, Eiroa, C., additional, Fedele, D., additional, Augereau, J.-C., additional, Olofsson, G., additional, González, B., additional, Maldonado, J., additional, Montesinos, B., additional, Mora, A., additional, Absil, O., additional, Ardila, D., additional, Barrado, D., additional, Bayo, A., additional, Beichman, C. A., additional, Bryden, G., additional, Danchi, W. C., additional, del Burgo, C., additional, Ertel, S., additional, Fridlund, C. W. M., additional, Heras, A. M., additional, Krivov, A. V., additional, Launhardt, R., additional, Lebreton, J., additional, Löhne, T., additional, Marshall, J. P., additional, Meeus, G., additional, Müller, S., additional, Pilbratt, G. L., additional, Roberge, A., additional, Rodmann, J., additional, Solano, E., additional, Stapelfeldt, K. R., additional, Thébault, Ph., additional, White, G. J., additional, and Wolf, S., additional

Published
2010
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46. Cold DUst around NEarby Stars (DUNES). First results

Author

Eiroa, C., primary, Fedele, D., additional, Maldonado, J., additional, González-García, B. M., additional, Rodmann, J., additional, Heras, A. M., additional, Pilbratt, G. L., additional, Augereau, J.-Ch., additional, Mora, A., additional, Montesinos, B., additional, Ardila, D., additional, Bryden, G., additional, Liseau, R., additional, Stapelfeldt, K., additional, Launhardt, R., additional, Solano, E., additional, Bayo, A., additional, Absil, O., additional, Arévalo, M., additional, Barrado, D., additional, Beichmann, C., additional, Danchi, W., additional, del Burgo, C., additional, Ertel, S., additional, Fridlund, M., additional, Fukagawa, M., additional, Gutiérrez, R., additional, Grün, E., additional, Kamp, I., additional, Krivov, A., additional, Lebreton, J., additional, Löhne, T., additional, Lorente, R., additional, Marshall, J., additional, Martínez-Arnáiz, R., additional, Meeus, G., additional, Montes, D., additional, Morbidelli, A., additional, Müller, S., additional, Mutschke, H., additional, Nakagawa, T., additional, Olofsson, G., additional, Ribas, I., additional, Roberge, A., additional, Sanz-Forcada, J., additional, Thébault, P., additional, Walker, H., additional, White, G. J., additional, and Wolf, S., additional

Published
2010
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49. The β Pictoris disk imaged by Herschel PACS and SPIRE

Author

B. Vandenbussche, B. Sibthorpe, B. Acke, E. Pantin, G. Olofsson, C. Waelkens, C. Dominik, M. J. Barlow, J. A. D. L. Blommaert, J. Bouwman, A. Brandeker, M. Cohen, W. De Meester, W. R. F. Dent, K. Exter, J. Di Francesco, M. Fridlund, W. K. Gear, A. M. Glauser, H. L. Gomez, J. S. Greaves, P. C. Hargrave, P. M. Harvey, Th. Henning, A. M. Heras, M. R. Hogerheijde, W. S. Holland, R. Huygen, R. J. Ivison, C. Jean, S. J. Leeks, T. L. Lim, R. Liseau, B. C. Matthews, D. A. Naylor, G. L. Pilbratt, E. T. Polehampton, S. Regibo, P. Royer, A. Sicilia-Aguilar, B. M. Swinyard, H. J. Walker, R. Wesson, and Low Energy Astrophysics (API, FNWI)

Subjects
Photometry (optics), Physics, Debris disk, Spectral index, Wavelength, Radiation pressure, Space and Planetary Science, Particle-size distribution, Beta Pictoris, Astronomy and Astrophysics, Surface brightness, Astrophysics
Abstract

We obtained Herschel PACS and SPIRE images of the thermal emission of the debris disk around the A5V star {\beta} Pic. The disk is well resolved in the PACS filters at 70, 100, and 160 {\mu}m. The surface brightness profiles between 70 and 160 {\mu}m show no significant asymmetries along the disk, and are compatible with 90% of the emission between 70 and 160 {\mu}m originating in a region closer than 200 AU to the star. Although only marginally resolving the debris disk, the maps obtained in the SPIRE 250 - 500 {\mu}m filters provide full-disk photometry, completing the SED over a few octaves in wavelength that had been previously inaccessible. The small far-infrared spectral index ({\beta} = 0.34) indicates that the grain size distribution in the inner disk (

Published
2010

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