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106 results on '"Sibthorpe, Bruce"'

1. Debris disks around M dwarfs: The Herschel DEBRIS survey

Author

Lestrade, Jean-Francois, Matthews, Brenda C., Kennedy, Grant M., Sibthorpe, Bruce, Wyatt, Mark C., Booth, Mark, Greaves, Jean S., Duchene, Gaspard, Moro-Martin, Amaya, and Jobic, Cassien

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The Herschel open-time key program Disc Emission via a Bias-free Reconnaissance in the Infrared and Sub-millimeter (DEBRIS) is an unbiased survey of the nearest ~100 stars for each stellar type A-M observed with a uniform photometric sensitivity to search for cold debris disks around them. The analysis of the Photoconductor Array Camera and Spectrometer (PACS) photometric observations of the 94 DEBRIS M dwarfs of this program is presented in this paper, following upon two companion papers on the DEBRIS A-star and FGK-star subsamples. In the M-dwarf subsample, two debris disks have been detected, around the M3V dwarf GJ581 and the M4V dwarf FomalhautC (LP876-10). This result gives a disk detection rate of 2.1^{+2.7}_{-0.7}% at the 68% confidence level, significantly less than measured for earlier stellar types in the DEBRIS program. However, we show that the survey of the DEBRIS M-dwarf subsample is about ten times shallower than the surveys of the DEBRIS FGK subsamples when studied in the physical parameter space of the disk's fractional dust luminosity versus blackbody radius. Furthermore, had the DEBRIS K-star subsample been observed at the same shallower depth in this parameter space, its measured disk detection rate would have been statistically consistent with the one found for the M-dwarf subsample. Hence, the incidence of debris disks does not appear to drop from the K subsample to the M subsample of the DEBRIS program, when considering disks in the same region of physical parameter space. An alternative explanation is that the only two bright disks discovered in the M-dwarf subsample would not, in fact, be statistically representative of the whole population., Comment: 12 pages, long Table 3 included, accepted for publication in Astronomy & Astrophysics

Published
2025

2. SONS: The JCMT legacy survey of debris discs in the submillimetre

Author

Holland, Wayne S., Matthews, Brenda C., Kennedy, Grant M., Greaves, Jane S., Wyatt, Mark C., Booth, Mark, Bastien, Pierre, Bryden, Geoff, Butner, Harold, Chen, Christine H., Chrysostomou, Antonio, Davies, Claire L., Dent, William R. F., Di Francesco, James, Duchene, Gaspard, Gibb, Andy G., Friberg, Per, Ivison, Rob J., Jenness, Tim, Kavelaars, JJ, Lawler, Samantha, Lestrade, Jean-Francois, Marshall, Jonathan P., Moro-Martin, Amaya, Panic, Olja, Phillips, Neil, Serjeant, Stephen, Schieven, Gerald H., Sibthorpe, Bruce, Vican, Laura, Ward-Thompson, Derek, van der Werf, Paul, White, Glenn J., Wilner, David, and Zuckerman, Ben

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

Debris discs are evidence of the ongoing destructive collisions between planetesimals, and their presence around stars also suggests that planets exist in these systems. In this paper, we present submillimetre images of the thermal emission from debris discs that formed the SCUBA-2 Observations of Nearby Stars (SONS) survey, one of seven legacy surveys undertaken on the James Clerk Maxwell telescope between 2012 and 2015. The overall results of the survey are presented in the form of 850 microns (and 450 microns, where possible) images and fluxes for the observed fields. Excess thermal emission, over that expected from the stellar photosphere, is detected around 49 stars out of the 100 observed fields. The discs are characterised in terms of their flux density, size (radial distribution of the dust) and derived dust properties from their spectral energy distributions. The results show discs over a range of sizes, typically 1-10 times the diameter of the Edgeworth-Kuiper Belt in our Solar System. The mass of a disc, for particles up to a few millimetres in size, is uniquely obtainable with submillimetre observations and this quantity is presented as a function of the host stars' age, showing a tentative decline in mass with age. Having doubled the number of imaged discs at submillimetre wavelengths from ground-based, single dish telescope observations, one of the key legacy products from the SONS survey is to provide a comprehensive target list to observe at high angular resolution using submillimetre/millimetre interferometers (e.g., ALMA, SMA)., Comment: 61 pages, 51 figures

Published
2017
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3. IR-excesses around nearby Lambda Boo stars are caused by debris disks rather than ISM bow waves

Author

Draper, Zachary H, Matthews, Brenda C, Kennedy, Grant M, Wyatt, Mark C, Venn, Kim A, and Sibthorpe, Bruce

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

Lambda Boo stars are predominately A-type stars with solar abundant C, N, O, and S, but up to 2 dex underabundances of refractory elements. The stars' unusual surface abundances could be due to a selective accretion of volatile gas over dust. It has been proposed that there is a correlation between the Lambda Boo phenomenon and IR-excesses which are the result of a debris disk or interstellar medium (ISM) interaction providing the accreting material. We observe 70 or 100 and 160 $\mu$m excess emission around 9 confirmed Lambda Boo stars with the Herschel Space Observatory, to differentiate whether the dust emission is from a debris disk or an ISM bow wave. We find that 3/9 stars observed host well resolved debris disks. While the remaining 6/9 are not resolved, they are inconsistent with an ISM bow wave based on the dust emission being more compact for its temperature and predicted bow wave models produce hotter emission than what is observed. We find the incidence of bright IR-excesses around Lambda Boo stars is higher than normal A-stars. To explain this given our observations, we explore Poynting-Robertson (PR) drag as a mechanism of accretion from a debris disk but find it insufficient. As an alternative, we propose the correlation is due to higher dynamical activity in the disks currently underway. Large impacts of planetesimals or a higher influx of comets could provide enough volatile gas for accretion. Further study on the transport of circumstellar material in relation to the abundance anomalies are required to explain the phenomenon through external accretion., Comment: 19 pages, 8 figures, 8 tables, Accepted to MNRAS

Published
2015
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4. The AU Mic Debris Disk: far-infrared and submillimeter resolved imaging

Author

Matthews, Brenda C., Kennedy, Grant, Sibthorpe, Bruce, Holland, Wayne, Booth, Mark, Kalas, Paul, MacGregor, Meredith, Wilner, David, Vandenbussche, Bart, Olofsson, Göran, Blommaert, Joris, Brandeker, Alexis, Dent, W. R. F., de Vries, Bernard L., Di Francesco, James, Fridlund, Malcolm, Graham, James R., Greaves, Jane, Heras, Ana M., Hogerheijde, Michiel, Ivison, R. J., Pantin, Eric, and Pilbratt, Göran L.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

We present far-infrared and submillimeter maps from the Herschel Space Observatory and the James Clerk Maxwell Telescope of the debris disk host star AU Microscopii. Disk emission is detected at 70, 160, 250, 350, 450, 500 and 850 micron. The disk is resolved at 70, 160 and 450 micron. In addition to the planetesimal belt, we detect thermal emission from AU Mic's halo for the first time. In contrast to the scattered light images, no asymmetries are evident in the disk. The fractional luminosity of the disk is $3.9 \times 10^{-4}$ and its mm-grain dust mass is 0.01 MEarth (+/- 20%). We create a simple spatial model that reconciles the disk SED as a blackbody of 53 +/- 2 K (a composite of 39 and 50 K components) and the presence of small (non-blackbody) grains which populate the extended halo. The best fit model is consistent with the "birth ring" model explored in earlier works, i.e., an edge-on dust belt extending from 8.8-40 AU, but with an additional halo component with an $r^{-1.5}$ surface density profile extending to the limits of sensitivity (140 AU). We confirm that AU Mic does not exert enough radiation force to blow out grains. For stellar mass loss rates of 10-100x solar, compact (zero porosity) grains can only be removed if they are very small, consistently with previous work, if the porosity is 0.9, then grains approaching 0.1 micron can be removed via corpuscular forces (i.e., the stellar wind)., Comment: accepted to the Astrophysical Journal

Published
2015
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5. Kuiper belt structure around nearby super-Earth host stars

Author

Kennedy, Grant M., Matrà, Luca, Marmier, Maxime, Greaves, Jane S., Wyatt, Mark C., Bryden, Geoffrey, Holland, Wayne, Lovis, Christophe, Matthews, Brenda C., Pepe, Francesco, Sibthorpe, Bruce, and Udry, Stéphane

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We present new observations of the Kuiper belt analogues around HD 38858 and HD 20794, hosts of super-Earth mass planets within 1 au. As two of the four nearby G-type stars (with HD 69830 and 61 Vir) that form the basis of a possible correlation between low-mass planets and debris disc brightness, these systems are of particular interest. The disc around HD 38858 is well resolved with Herschel and we constrain the disc geometry and radial structure. We also present a probable JCMT sub-mm continuum detection of the disc and a CO J=2-1 upper limit. The disc around HD 20794 is much fainter and appears marginally resolved with Herschel, and is constrained to be less extended than the discs around 61 Vir and HD 38858. We also set limits on the radial location of hot dust recently detected around HD 20794 with near-IR interferometry. We present HARPS upper limits on unseen planets in these four systems, ruling out additional super-Earths within a few au, and Saturn-mass planets within 10 au. We consider the disc structure in the three systems with Kuiper belt analogues (HD 69830 has only a warm dust detection), concluding that 61 Vir and HD 38858 have greater radial disc extent than HD 20794. We speculate that the greater width is related to the greater minimum planet masses (10-20 $M_\oplus$ vs. 3-5 $M_\oplus$), arising from an eccentric planetesimal population analogous to the Solar System's scattered disc. We discuss alternative scenarios and possible means to distinguish among them., Comment: accepted to MNRAS

Published
2015
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6. Resolved Imaging of the HR 8799 Debris Disk with Herschel

Author

Matthews, Brenda C., Kennedy, Grant, Sibthorpe, Bruce, Booth, Mark, Wyatt, Mark, Broekhoven-Fiene, Hannah, Macintosh, Bruce, and Marois, Christian

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

We present Herschel far-infrared and submillimeter maps of the debris disk associated with the HR 8799 planetary system. We resolve the outer disk emission at 70, 100, 160 and 250 um and detect the disk at 350 and 500 um. A smooth model explains the observed disk emission well. We observe no obvious clumps or asymmetries associated with the trapping of planetesimals that is a potential consequence of planetary migration in the system. We estimate that the disk eccentricity must be <0.1. As in previous work by Su et al. (2009), we find a disk with three components: a warm inner component and two outer components, a planetesimal belt extending from 100 - 310 AU, with some flexibility (+/- 10 AU) on the inner edge, and the external halo which extends to ~2000 AU. We measure the disk inclination to be 26 +/- 3 deg from face-on at a position angle of 64 deg E of N, establishing that the disk is coplanar with the star and planets. The SED of the disk is well fit by blackbody grains whose semi-major axes lie within the planetesimal belt, suggesting an absence of small grains. The wavelength at which the spectrum steepens from blackbody, 47 +/- 30 um, however, is short compared to other A star debris disks, suggesting that there are atypically small grains likely populating the halo. The PACS longer wavelength data yield a lower disk color temperature than do MIPS data (24 and 70 um), implying two distinct halo dust grain populations., Comment: 13 pages, 8 figures (6 color), accepted for publication in the Astrophysical Journal

Published
2013
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7. Herschel Observations of Debris Discs Orbiting Planet-hosting Subgiants

Author

Bonsor, Amy, Kennedy, Grant M., Wyatt, Mark C., Johnson, John A., and Sibthorpe, Bruce

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Debris discs are commonly detected orbiting main-sequence stars, yet little is known regarding their fate as the star evolves to become a giant. Recent observations of radial velocity detected planets orbiting giant stars highlight this population and its importance for probing, for example, the population of planetary systems orbiting intermediate mass stars. Our Herschel survey observed a subset of the Johnson et al program subgiants, finding that 4/36 exhibit excess emission thought to indicate debris, of which 3/19 are planet-hosting stars and 1/17 are stars with no current planet detections. Given the small numbers involved, there is no evidence that the disc detection rate around stars with planets is different to that around stars without planets. Our detections provide a clear indication that large quantities of dusty material can survive the stars' main-sequence lifetime and be detected on the subgiant branch, with important implications for the evolution of planetary systems and observations of polluted or dusty white dwarfs. Our detection rates also provide an important constraint that can be included in models of debris disc evolution., Comment: 12 pages, MNRAS, accepted

Published
2013
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8. Spatially Resolved Images of Dust Belt(s) Around the Planet-hosting Subgiant Kappa CrB

Author

Bonsor, Amy, Kennedy, Grant M., Crepp, Justin R., Johnson, John A., Wyatt, Mark C., Sibthorpe, Bruce, and Su, Kate Y. L.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We present Herschel spatially resolved images of the debris disc orbiting the subgiant Kappa CrB. Not only are these the first resolved images of a debris disc orbiting a subgiant, but Kappa CrB is a rare example of an intermediate mass star where a detailed study of the structure of the planetary system can be made, including both planets and planetesimal belt(s). The only way to discover planets around such stars using the radial velocity technique is to observe 'retired' A stars, which are cooler and slower rotators compared to their main-sequence counterparts. A planetary companion has already been detected orbiting the subgiant Kappa CrB, with revised parameters of m sin i = 2.1MJ and apl = 2.8AU (Johnson et al. 2008a). We present additional Keck I HIRES radial velocity measurements that provide evidence for a second planetary companion, alongside Keck II AO imaging that places an upper limit on the mass of this companion. Modelling of our Herschel images shows that the dust is broadly distributed, but cannot distinguish between a single wide belt (from 20 to 220AU) or two narrow dust belts (at around 40 and 165AU). Given the existence of a second planetary companion beyond approximately 3AU it is possible that the absence of dust within approximately 20AU is caused by dynamical depletion, although the observations are not inconsistent with depletion of these regions by collisional erosion, which occurs at higher rates closer to the star., Comment: Updated abstract

Published
2013
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9. The debris disk around gamma Doradus resolved with Herschel

Author

Broekhoven-Fiene, Hannah, Matthews, Brenda C., Kennedy, Grant M., Booth, Mark, Sibthorpe, Bruce, Lawler, Samantha M., Kavelaars, J. J., Wyatt, Mark C., Qi, Chenruo, Koning, Alice, Su, Kate Y. L., Rieke, George H., Wilner, David J., and Greaves, Jane S.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

We present observations of the debris disk around gamma Doradus, an F1V star, from the Herschel Key Programme DEBRIS (Disc Emission via Bias-free Reconnaissance in the Infrared/Submillimetre). The disk is well-resolved at 70, 100 and 160 micron, resolved along its major axis at 250 micron, detected but not resolved at 350 micron, and confused with a background source at 500 micron. It is one of our best resolved targets and we find it to have a radially broad dust distribution. The modelling of the resolved images cannot distinguish between two configurations: an arrangement of a warm inner ring at several AU (best-fit 4 AU) and a cool outer belt extending from ~55 to 400 AU or an arrangement of two cool, narrow rings at ~70 AU and ~190 AU. This suggests that any configuration between these two is also possible. Both models have a total fractional luminosity of ~10^{-5} and are consistent with the disk being aligned with the stellar equator. The inner edge of either possible configuration suggests that the most likely region to find planets in this system would be within ~55 AU of the star. A transient event is not needed to explain the warm dust's fractional luminosity., Comment: 12 pages, 6 figures, accepted for publication in ApJ

Published
2012
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10. Millimeter Emission Structure in the first ALMA Image of the AU Mic Debris Disk

Author

MacGregor, Meredith A., Wilner, David J., Rosenfeld, Katherine A., Andrews, Sean M., Matthews, Brenda, Hughes, A. Meredith, Booth, Mark, Chiang, Eugene, Graham, James R., Kalas, Paul, Kennedy, Grant, and Sibthorpe, Bruce

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

We present 1.3 millimeter ALMA Cycle 0 observations of the edge-on debris disk around the nearby, ~10 Myr-old, M-type star AU Mic. These observations obtain 0.6 arcsec (6 AU) resolution and reveal two distinct emission components: (1) the previously known dust belt that extends to a radius of 40 AU, and (2) a newly recognized central peak that remains unresolved. The cold dust belt of mass about 1 lunar mass is resolved in the radial direction with a rising emission profile that peaks sharply at the location of the outer edge of the "birth ring" of planetesimals hypothesized to explain the midplane scattered light gradients. No significant asymmetries are discerned in the structure or position of this dust belt. The central peak identified in the ALMA image is ~6 times brighter than the stellar photosphere, which indicates an additional emission process in the inner regions of the system. Emission from a stellar corona or activity may contribute, but the observations show no signs of temporal variations characteristic of radio-wave flares. We suggest that this central component may be dominated by dust emission from an inner planetesimal belt of mass about 0.01 lunar mass, consistent with a lack of emission shortward of 25 microns and a location <3 AU from the star. Future millimeter observations can test this assertion, as an inner dust belt should be readily separated from the central star at higher angular resolution., Comment: 13 pages, 2 figures, 2 tables, accepted by ApJ Letters

Published
2012
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11. Resolved Debris Discs Around A Stars in the Herschel DEBRIS Survey

Author

Booth, Mark, Kennedy, Grant, Sibthorpe, Bruce, Matthews, Brenda C., Wyatt, Mark C., Duchêne, Gaspard, Kavelaars, J. J., Rodriguez, David, Greaves, Jane S., Koning, Alice, Vican, Laura, Rieke, George H., Su, Kate Y. L., Moro-Martín, Amaya, and Kalas, Paul

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

The majority of debris discs discovered so far have only been detected through infrared excess emission above stellar photospheres. While disc properties can be inferred from unresolved photometry alone under various assumptions for the physical properties of dust grains, there is a degeneracy between disc radius and dust temperature that depends on the grain size distribution and optical properties. By resolving the disc we can measure the actual location of the dust. The launch of Herschel, with an angular resolution superior to previous far-infrared telescopes, allows us to spatially resolve more discs and locate the dust directly. Here we present the nine resolved discs around A stars between 20 and 40 pc observed by the DEBRIS survey. We use these data to investigate the disc radii by fitting narrow ring models to images at 70, 100 and 160 {\mu}m and by fitting blackbodies to full spectral energy distributions. We do this with the aim of finding an improved way of estimating disc radii for unresolved systems. The ratio between the resolved and blackbody radii varies between 1 and 2.5. This ratio is inversely correlated with luminosity and any remaining discrepancies are most likely explained by differences to the minimum size of grain in the size distribution or differences in composition. We find that three of the systems are well fit by a narrow ring, two systems are borderline cases and the other four likely require wider or multiple rings to fully explain the observations, reflecting the diversity of planetary systems., Comment: 19 pages, 13 figures, 6 tables. Accepted for publication in MNRAS

Published
2012
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12. Resolving debris discs in the far-infrared: early highlights from the DEBRIS survey

Author

DEBRIS Collaboration, Matthews, Brenda, Sibthorpe, Bruce, Kennedy, Grant, Phillips, Neil, Churcher, Laura, Duchêne, Gaspard, Greaves, Jane, Lestrade, Jean-Francois, Moro-Martin, Amaya, Wyatt, Mark, Bastien, Pierre, Biggs, Andy, Bouvier, Jerome, Butner, Harold, Dent, Bill, Di Francesco, James, Eislöffel, Jochen, Graham, James, Harvey, Paul, Hauschildt, Peter, Holland, Wayne, Horner, Jonti, Ibar, Eduardo, Ivison, Rob, Johnstone, Doug, Kalas, Paul, Kavelaars, JJ, Rodriguez, David, Udry, Stephane, van der Werf, Paul, Wilner, David, and Zuckerman, Ben

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

We present results from the earliest observations of DEBRIS, a Herschel Key Programme to conduct a volume- and flux-limited survey for debris discs in A-type through M-type stars. PACS images (from chop/nod or scan-mode observations) at 100 and 160 micron are presented toward two A-type stars and one F-type star: beta Leo, beta UMa and eta Corvi. All three stars are known disc hosts. Herschel spatially resolves the dust emission around all three stars (marginally, in the case of beta UMa), providing new information about discs as close as 11 pc with sizes comparable to that of the Solar System. We have combined these data with existing flux density measurements of the discs to refine the SEDs and derive estimates of the fractional luminosities, temperatures and radii of the discs., Comment: to be published in A&A, 5 pages, 2 color figures

Published
2010
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13. Gas Evolution in Protoplanetary Disks

Author

Woitke, Peter, Dent, Bill, Thi, Wing-Fai, Sibthorpe, Bruce, Rice, Ken, Williams, Jonathan, Sicilia-Aguilar, Aurora, Brown, Joanna, Kamp, Inga, Pascucci, Ilaria, Alexander, Richard, and Roberge, Aki

Subjects
Astrophysics
Abstract

This article summarizes a Splinter Session at the Cool Stars XV conference in St. Andrews with 3 review and 4 contributed talks. The speakers have discussed various approaches to understand the structure and evolution of the gas component in protoplanetary disks. These ranged from observational spectroscopy in the UV, infrared and millimeter, through to chemical and hydrodynamical models. The focus was on disks around low-mass stars, ranging from classical T Tauri stars to transitional disks and debris disks. Emphasis was put on water and organic molecules, the relation to planet formation, and the formation of holes and gaps in the inner regions., Comment: 9 pages, 6 figures

Published
2008
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14. Characterisation and optimisation of the Herschel-SPIRE imaging through simulations

Author

Sibthorpe, Bruce

Subjects
523.01
Abstract

The Spectral and Photometric Imaging Receiver (SPIRE) is one of the three instruments on-board the European Space Agency's Herschel Space Observatory, due for launch in 2008. SPIRE is a dual instrument comprising a photometer, and imaging Fourier transform spectrometer. This thesis deals with the design and operation of a software simulator for the SPIRE photometer. The simulator architecture and modelling methods are described, and the fidelity of its output verified. This simulation software is then used to optimise and characterise data from the SPIRE photometer. The optimum observing parameters are derived, in order to maximise observing efficiency, and data quality. The impact of uncorrelated 1/f noise on the extraction of sources of arbitrary scale is assessed, and quantified. This work is also extended to include the impact of uncorrected 1/f noise on observations of sources in a confused environment. These results provide important information regarding the quality of SPIRE photometer data for the planning of large survey observations. The simulator is also an active tool within the SPIRE Instrument Control Centre team, and its use in the selection of the SPIRE map making algorithm is described. This thesis also contains an analysis of observations of the Cassiopeia A supernova remnant made with the Balloon-borne Large Aperture submillimetre Telescope (BLAST), an instrument based on the SPIRE photometer design. This analysis assesses the hypothesis that supernovae might be a significant dust formation mechanism in the universe, as proposed in recent literature. Results from this study suggest that this hypothesis may be correct, but that evidence from previous observations might in fact be upper limits to the total mass of dust, rather than an absolute measurement.

Published
2007

15. Debris Discs: From Herschel to SPICA/SAFARI

Author

Sibthorpe, Bruce and DeVries, Bernard L.

Abstract

SPICA Science Conference from Exoplanets to Distant Galaxies: SPICA's New Window on the Cool Universe (June 18-21, 2013. Ito Hall, the University of Tokyo), Bunkyou-ku, Tokyo, Japan, The Herschel Space Observatory has been used to further our understanding of debris discs around nearby stars. Three 'key programmes' were performed, whose primary aim was the characterisation of the population as a whole and, in doing so, to better understand our Solar-System in the wider context. In this article the parameter space probed by these surveys is assessed with respect to previous work performed, at similar wavelengths, with Spitzer and IRAS. This is then further developed, quantifying the potential improvement that could be achieved, for similar surveys, using the SAFARI instrument on-board the forthcoming SPICA space observatory., 形態: カラー図版あり, Physical characteristics: Original contains color illustrations, 資料番号: AA1730027071, レポート番号: JAXA-SP-17-010E

Published
2018

16. SONS: The JCMT legacy survey of debris discs in the submillimetre

Author

Holland, Wayne S., primary, Matthews, Brenda C., additional, Kennedy, Grant M., additional, Greaves, Jane S., additional, Wyatt, Mark C., additional, Booth, Mark, additional, Bastien, Pierre, additional, Bryden, Geoff, additional, Butner, Harold, additional, Chen, Christine H., additional, Chrysostomou, Antonio, additional, Davies, Claire L., additional, Dent, William R. F., additional, Di Francesco, James, additional, Duchêne, Gaspard, additional, Gibb, Andy G., additional, Friberg, Per, additional, Ivison, Rob J., additional, Jenness, Tim, additional, Kavelaars, JJ, additional, Lawler, Samantha, additional, Lestrade, Jean-François, additional, Marshall, Jonathan P., additional, Moro-Martin, Amaya, additional, Panić, Olja, additional, Phillips, Neil, additional, Serjeant, Stephen, additional, Schieven, Gerald H., additional, Sibthorpe, Bruce, additional, Vican, Laura, additional, Ward-Thompson, Derek, additional, van der Werf, Paul, additional, White, Glenn J., additional, Wilner, David, additional, and Zuckerman, Ben, additional

Published
2017
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17. The Debris Disk around \u03b3 Doradus Resolved with Herschel

Author

Broekhoven-Fiene, Hannah, Matthews, Brenda C., Kennedy, Grant M., Booth, Mark, Sibthorpe, Bruce, Lawler, Samantha M., Kavelaars, J. J., Wyatt, Mark C., Qi, Chenruo, Koning, Alice, Su, Kate Y. L., Rieke, George H., Wilner, David J., Greaves, Jane S., Broekhoven-Fiene, Hannah, Matthews, Brenda C., Kennedy, Grant M., Booth, Mark, Sibthorpe, Bruce, Lawler, Samantha M., Kavelaars, J. J., Wyatt, Mark C., Chenruo, Koning, Alice, Kate Y. L., Rieke, George H., Wilner, David J., Greaves, and Jane S.

Published
2013

18. THE AU MIC DEBRIS DISK: FAR-INFRARED AND SUBMILLIMETER RESOLVED IMAGING

Author

Matthews, Brenda C., primary, Kennedy, Grant, additional, Sibthorpe, Bruce, additional, Holland, Wayne, additional, Booth, Mark, additional, Kalas, Paul, additional, MacGregor, Meredith, additional, Wilner, David, additional, Vandenbussche, Bart, additional, Olofsson, Göran, additional, Blommaert, Joris, additional, Brandeker, Alexis, additional, Dent, W. R. F., additional, Vries, Bernard L. de, additional, Francesco, James Di, additional, Fridlund, Malcolm, additional, Graham, James R., additional, Greaves, Jane, additional, Heras, Ana M., additional, Hogerheijde, Michiel, additional, Ivison, R. J., additional, Pantin, Eric, additional, and Pilbratt, Göran L., additional

Published
2015
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19. Resolving debris discs in the far-infrared: early highlights from the DEBRIS survey

Author

Debris, Collaboration, Matthews, Brenda, Sibthorpe, Bruce, Kennedy, Grant, Phillips, Neil, Churcher, Laura, Duchêne, Gaspard, Greaves, Jane, Lestrade, Jean-Francois, Moro-Martin, Amaya, Wyatt, Mark, Bastien, Pierre, Biggs, Andy, Bouvier, Jerome, Butner, Harold, Dent, Bill, Di Francesco, James, Eislöffel, Jochen, Graham, James, Harvey, Paul, Hauschildt, Peter, Holland, Wayne, Horner, Jonti, Ibar, Eduardo, Rob Ivison, Johnstone, Doug, Kalas, Paul, Kavelaars, Jj, Rodriguez, David, Udry, Stephane, Werf, Paul, Wilner, David, Zuckerman, Ben, Laboratoire d'Astrophysique de Grenoble (LAOG), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, Solar System, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Debris, Stars, Far infrared, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Dust emission
Abstract

We present results from the earliest observations of DEBRIS, a Herschel Key Programme to conduct a volume- and flux-limited survey for debris discs in A-type through M-type stars. PACS images (from chop/nod or scan-mode observations) at 100 and 160 micron are presented toward two A-type stars and one F-type star: beta Leo, beta UMa and eta Corvi. All three stars are known disc hosts. Herschel spatially resolves the dust emission around all three stars (marginally, in the case of beta UMa), providing new information about discs as close as 11 pc with sizes comparable to that of the Solar System. We have combined these data with existing flux density measurements of the discs to refine the SEDs and derive estimates of the fractional luminosities, temperatures and radii of the discs., to be published in A&A, 5 pages, 2 color figures

Published
2010

20. Kuiper belt structure around nearby super-Earth host stars

Author

Kennedy, Grant M., primary, Matrà, Luca, additional, Marmier, Maxime, additional, Greaves, Jane S., additional, Wyatt, Mark C., additional, Bryden, Geoffrey, additional, Holland, Wayne, additional, Lovis, Christophe, additional, Matthews, Brenda C., additional, Pepe, Francesco, additional, Sibthorpe, Bruce, additional, and Udry, Stéphane, additional

Published
2015
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21. The Herschel first look at protostars in the Aquila rift [Letter]

Author

Bontemps, S., André, Ph., Könyves, V., Men'shchikov, A., Schneider, N., Maury, A., Peretto, Nicolas, Arzoumanian, D., Attard, M., Motte, F., Minier, V., Didelon, P., Saraceno, P., Abergel, A., Baluteau, J.-P., Bernard, J.-Ph., Cambrésy, L., Cox, P., Di Francesco, J., Di Giorgo, A. M., Griffin, Matthew Joseph, Hargrave, Peter Charles, Huang, M., Kirk, Jason M., Li, J., Martin, P., Merín, B., Molinari, S., Olofsson, G., Pezzuto, S., Prusti, T., Roussel, H., Russeil, D., Sauvage, M., Sibthorpe, Bruce, Spinoglio, L., Testi, L., Vavrek, R., Ward-Thompson, Derek, White, G., Wilson, C., Woodcraft, Adam, and Zavagno, A.

Subjects
QB
Abstract

As part of the science demonstration phase of the Herschel mission of the Gould Belt key program, the Aquila rift molecular complex has been observed. The complete ~ 3.3° × 3.3° imaging with SPIRE 250/350/500 μm and PACS 70/160 μm allows a deep investigation of embedded protostellar phases, probing of the dust emission from warm inner regions at 70 and 160 μm to the bulk of the cold envelopes between 250 and 500 μm. We used a systematic detection technique operating simultaneously on all Herschel bands to build a sample of protostars. Spectral energy distributions are derived to measure luminosities and envelope masses, and to place the protostars in an Menv – Lbol evolutionary diagram. The spatial distribution of protostars indicates three star-forming sites in Aquila, with W40/Sh2-64 HII region by far the richest. Most of the detected protostars are newly discovered. For a reduced area around the Serpens South cluster, we could compare the Herschel census of protostars with Spitzer results. The Herschel protostars are younger than in Spitzer with 7 Class 0 YSOs newly revealed by Herschel. For the entire Aquila field, we find a total of ~45–60 Class 0 YSOs discovered by Herschel. This confirms the global statistics of several hundred Class 0 YSOs that should be found in the whole Gould Belt Survey.

Published
2010

22. Clouds, filaments, and protostars: the Herschel/Hi-GAL Milky Way [Letter]

Author

Molinari, S., Swinyard, B., Bally, J., Barlow, M., Bernard, J.-P., Martin, P., Moore, T., Noriega-Crespo, A., Plume, R., Testi, L., Zavagno, A., Abergel, A., Ali, B., Anderson, L., André, P., Baluteau, J.-P., Battersby, C., Beltrán, M. T., Benedettini, M., Billot, N., Blommaert, J., Bontemps, S., Boulanger, F., Brand, J., Brunt, C., Burton, M., Calzoletti, L., Carey, S., Caselli, P., Cesaroni, R., Cernicharo, J., Chakrabarti, S., Chrysostomou, A., Cohen, M., Compiegne, M., de Bernardis, P., de Gasperis, G., di Giorgio, A. M., Elia, D., Faustini, F., Flagey, N., Fukui, Y., Fuller, G. A., Ganga, K., Garcia-Lario, P., Glenn, J., Goldsmith, P. F., Griffin, Matthew Joseph, Hoare, M., Huang, M., Ikhenaode, D., Joblin, C., Joncas, G., Juvela, M., Kirk, Jason M., Lagache, G., Li, J. Z., Lim, T. L., Lord, S. D., Marengo, M., Marshall, D. J., Masi, S., Massi, F., Matsuura, Mikako, Minier, V., Miville-Deschênes, M.-A., Montier, L. A., Morgan, L., Motte, F., Mottram, J. C., Müller, T. G., Natoli, P., Neves, J., Olmi, L., Paladini, R., Paradis, D., Parsons, H., Peretto, Nicolas, Pestalozzi, M., Pezzuto, S., Piacentini, F., Piazzo, L., Polychroni, D., Pomarès, M., Popescu, C. C., Reach, W. T., Ristorcelli, I., Robitaille, J.-F., Robitaille, T., Rodón, J. A., Roy, A., Royer, P., Russeil, D., Saraceno, P., Sauvage, M., Schilke, P., Schisano, E., Schneider, N., Schuller, F., Schulz, B., Sibthorpe, Bruce, Smith, H. A., Smith, M. D., Spinoglio, L., Stamatelos, Dimitrios, Strafella, F., Stringfellow, G. S., Sturm, E., Taylor, R., Thompson, M. A., Traficante, A., Tuffs, R. J., Umana, G., Valenziano, L., Vavrek, R., Veneziani, M., Viti, S., Waelkens, C., Ward-Thompson, Derek, White, G., Wilcock, Lucy Ann, Wyrowski, F., Yorke, H. W., and Zhang, Q.

Abstract

We present the first results from the science demonstration phase for the Hi-GAL survey, the Herschel key program that will map the inner Galactic plane of the Milky Way in 5 bands. We outline our data reduction strategy and present some science highlights on the two observed 2° × 2° tiles approximately centered at l = 30° and l = 59°. The two regions are extremely rich in intense and highly structured extended emission which shows a widespread organization in filaments. Source SEDs can be built for hundreds of objects in the two fields, and physical parameters can be extracted, for a good fraction of them where the distance could be estimated. The compact sources (which we will call cores' in the following) are found for the most part to be associated with the filaments, and the relationship to the local beam-averaged column density of the filament itself shows that a core seems to appear when a threshold around AV ~ 1 is exceeded for the regions in the l = 59° field; a AV value between 5 and 10 is found for the l = 30° field, likely due to the relatively higher distances of the sources. This outlines an exciting scenario where diffuse clouds first collapse into filaments, which later fragment to cores where the column density has reached a critical level. In spite of core L/M ratios being well in excess of a few for many sources, we find core surface densities between 0.03 and 0.5 g cm-2. Our results are in good agreement with recent MHD numerical simulations of filaments forming from large-scale converging flows.

Published
2010

23. 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

26. SAFARI new and improved: extending the capabilities of SPICA's imaging spectrometer

Author

Roelfsema, Peter, additional, Giard, Martin, additional, Najarro, Francisco, additional, Wafelbakker, Kees, additional, Jellema, Willem, additional, Jackson, Brian, additional, Sibthorpe, Bruce, additional, Audard, Marc, additional, Doi, Yasuo, additional, di Giorgio, Anna, additional, Griffin, Matthew, additional, Helmich, Frank, additional, Kamp, Inga, additional, Kerschbaum, Franz, additional, Meyer, Michael, additional, Naylor, David, additional, Onaka, Takashi, additional, Poglitch, Albrecht, additional, Spinoglio, Luigi, additional, van der Tak, Floris, additional, and Vandenbussche, Bart, additional

Published
2014
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27. Clouds, filaments, and protostars: The Herschel Hi-GAL Milky Way

Author

Molinari, Sergio, Swinyard, Bruce M., Bally, John, Barlow, Michael J., Bernard, Jean P., Martin, Peter G., Moore, Toby J.T., Noriega-Crespo, Alberto, Plume, René, Testi, Leonardo, Zavagno, Annie, Abergel, Alain, Ali, Babar, Anderson, Lynn D., Ándré, P., Baluteau, Jean P., Battersby, Cara, Beltrán, Maria T., Benedettini, Milena, Billot, Nicolas, Blommaert, Joris A.D.L., Bontemps, Sylvain, Boulanger, François, van den Brand, Jan F.J., Brunt, Christopher M., Burton, Michael G., Calzoletti, Luca, Carey, Sean J., Caselli, Paola E.S., Cesaroni, Riccardo, Cernicharo, José R., Chakrabarti, Sukanya, Chrysostomou, Antonio C., Cohen, Martin G., Compiegne, Mathieu, De Bernardis, Paolo, De Gasperis, Giancarlo, Di Giorgio, Anna Maria, Elia, D., Faustini, Fabiana, Flagey, N., Fukui, Yasuo, Fuller, Gary A., Ganga, Ken M., Garcia-Lario, Pedro, Glenn, Jason, Goldsmith, Paul F., Griffin, Matthew J., Hoare, Matthew J., Huang, Maohai, Ikhenaode, David, Joblin, Christine, Joncas, Gilles, Juvela, Mika, Kirk, Jason M., Lagache, Guilaine, Li, Jin Zeng, Lim, Tanya L., Lord, Steven D., Marengo, Massimo, Marshall, Douglas J., Masi, Silvia, Massi, Fabrizio, Matsuura, Makiko, Minier, Vincent, Miville-Deschênes, Marc Antoine, Montier, Ludovic A., Morgan, L.K., Motte, Frédérique, Mottram, Joseph C., Müller, Thomas G., Natoli, Paolo, Neves, J., Olmi, Luca, Paladini, Roberta, Paradis, Delphine, Parsons, Harriet A.L., Peretto, Nicolas, Pestalozzi, Michele R., Pezzuto, Stefano, Piacentini, Francesco, Piazzo, Lorenzo, Polychroni, Danae, Pomarès, M., Popescu, Cristina C., Reach, William T., Ristorcelli, Isabelle, Robitaille, J.F., Robitaille, Thomas P., Rodón, Javier A., Roy, Arabindo, Royer, Pierre, Russeil, Delphine, Saraceno, Paolo, Sauvage, Marc André, Schilke, Peter, Schisano, Eugenio, Schneider, Nicola, Schuller, Frédéric, Schulz, Bernhard, Sibthorpe, Bruce, Smith, Howard A., Smith, Michael D., Spinoglio, Luigi, Stamatellos, Dimitris, Strafella, Francesco, Stringfellow, Guy S., Sturm, Eckhard, Taylor, Russ S., Thompson, M.A., Traficante, Alessio, Tuffs, Richard J., Umana, Grazia M., Valenziano, Luca, Vavrek, Roland, Veneziani, Milena, Viti, Serena, Waelkens, C., Ward-Thompson, Derek, White, Glenn J., Wilcock, Lawrence A., Wyrowski, Friedrich, Yorke, Harold W., Zhang, Qizhou, Molinari, Sergio, Swinyard, Bruce M., Bally, John, Barlow, Michael J., Bernard, Jean P., Martin, Peter G., Moore, Toby J.T., Noriega-Crespo, Alberto, Plume, René, Testi, Leonardo, Zavagno, Annie, Abergel, Alain, Ali, Babar, Anderson, Lynn D., Ándré, P., Baluteau, Jean P., Battersby, Cara, Beltrán, Maria T., Benedettini, Milena, Billot, Nicolas, Blommaert, Joris A.D.L., Bontemps, Sylvain, Boulanger, François, van den Brand, Jan F.J., Brunt, Christopher M., Burton, Michael G., Calzoletti, Luca, Carey, Sean J., Caselli, Paola E.S., Cesaroni, Riccardo, Cernicharo, José R., Chakrabarti, Sukanya, Chrysostomou, Antonio C., Cohen, Martin G., Compiegne, Mathieu, De Bernardis, Paolo, De Gasperis, Giancarlo, Di Giorgio, Anna Maria, Elia, D., Faustini, Fabiana, Flagey, N., Fukui, Yasuo, Fuller, Gary A., Ganga, Ken M., Garcia-Lario, Pedro, Glenn, Jason, Goldsmith, Paul F., Griffin, Matthew J., Hoare, Matthew J., Huang, Maohai, Ikhenaode, David, Joblin, Christine, Joncas, Gilles, Juvela, Mika, Kirk, Jason M., Lagache, Guilaine, Li, Jin Zeng, Lim, Tanya L., Lord, Steven D., Marengo, Massimo, Marshall, Douglas J., Masi, Silvia, Massi, Fabrizio, Matsuura, Makiko, Minier, Vincent, Miville-Deschênes, Marc Antoine, Montier, Ludovic A., Morgan, L.K., Motte, Frédérique, Mottram, Joseph C., Müller, Thomas G., Natoli, Paolo, Neves, J., Olmi, Luca, Paladini, Roberta, Paradis, Delphine, Parsons, Harriet A.L., Peretto, Nicolas, Pestalozzi, Michele R., Pezzuto, Stefano, Piacentini, Francesco, Piazzo, Lorenzo, Polychroni, Danae, Pomarès, M., Popescu, Cristina C., Reach, William T., Ristorcelli, Isabelle, Robitaille, J.F., Robitaille, Thomas P., Rodón, Javier A., Roy, Arabindo, Royer, Pierre, Russeil, Delphine, Saraceno, Paolo, Sauvage, Marc André, Schilke, Peter, Schisano, Eugenio, Schneider, Nicola, Schuller, Frédéric, Schulz, Bernhard, Sibthorpe, Bruce, Smith, Howard A., Smith, Michael D., Spinoglio, Luigi, Stamatellos, Dimitris, Strafella, Francesco, Stringfellow, Guy S., Sturm, Eckhard, Taylor, Russ S., Thompson, M.A., Traficante, Alessio, Tuffs, Richard J., Umana, Grazia M., Valenziano, Luca, Vavrek, Roland, Veneziani, Milena, Viti, Serena, Waelkens, C., Ward-Thompson, Derek, White, Glenn J., Wilcock, Lawrence A., Wyrowski, Friedrich, Yorke, Harold W., and Zhang, Qizhou

Abstract

We present the first results from the science demonstration phase for the Hi-GAL survey, the Herschel key program that will map the inner Galactic plane of the Milky Way in 5 bands. We outline our data reduction strategy and present some science highlights on the two observed 2° × 2° tiles approximately centered at l = 30° and l = 59°. The two regions are extremely rich in intense and highly structured extended emission which shows a widespread organization in filaments. Source SEDs can be built for hundreds of objects in the two fields, and physical parameters can be extracted, for a good fraction of them where the distance could be estimated. The compact sources (which we will call cores' in the following) are found for the most part to be associated with the filaments, and the relationship to the local beam-averaged column density of the filament itself shows that a core seems to appear when a threshold around AV ? 1 is exceeded for the regions in the l = 59° field; a AV value between 5 and 10 is found for the l = 30° field, likely due to the relatively higher distances of the sources. This outlines an exciting scenario where diffuse clouds first collapse into filaments, which later fragment to cores where the column density has reached a critical level. In spite of core L/M ratios being well in excess of a few for many sources, we find core surface densities between 0.03 and 0.5 g cm -2. Our results are in good agreement with recent MHD numerical simulations of filaments forming from large-scale converging flows.

Published
2010

28. Physics based calibration of the Herschel/SPIRE bolometers

Author

Cabrera, B., Miller, A., Young, B., Woodcraft, Adam L., Nguyen, Hien, Bock, James, Griffin, Matthew, Schulz, Bernhard, Sibthorpe, Bruce, Swinyard, Bruce, Cabrera, B., Miller, A., Young, B., Woodcraft, Adam L., Nguyen, Hien, Bock, James, Griffin, Matthew, Schulz, Bernhard, Sibthorpe, Bruce, and Swinyard, Bruce

Abstract

The bolometers (and readout circuitry) in the SPIRE instrument on the Herschel Space Observatory are among the best understood and well characterised of any sub‐mm astronomy instrument to date. SPIRE contains five arrays of NTD germanium spiderweb bolometers with up to 139 pixels per array. Their behaviour has been shown to be extremely stable as seen by repeated measurements in the years between initial array level and final instrument level tests, and can be described extremely well by a simple physical model (the ideal bolometer model). Calibration of the bolometers must take into account the non‐linear response when viewing bright sources, and the effect of fluctuations in the heat sink temperature. The simple and well‐understood behaviour of the detectors, coupled with the stable conditions expected in flight, mean that in contrast to previous sub‐mm instruments, physical models can be used to improve or possibly replace empirical calibration methods. We describe how this can be done, and use the large amount of data from ground measurements to show that we can use models to accurately calculate the absolute power detected by the bolometers.

Published
2009

29. Understanding the Herschel-SPIRE bolometers

Author

Duncan, William D., Holland, Wayne S., Withington, Stafford, Zmuidzinas, Jonas, Woodcraft, Adam L., Nguyen, Hien, Bock, James, Griffin, Matthew, Schulz, Bernhard, Sibthorpe, Bruce, Swinyard, Bruce, Duncan, William D., Holland, Wayne S., Withington, Stafford, Zmuidzinas, Jonas, Woodcraft, Adam L., Nguyen, Hien, Bock, James, Griffin, Matthew, Schulz, Bernhard, Sibthorpe, Bruce, and Swinyard, Bruce

Abstract

Bolometers are very simple devices. In principle, the behaviour of a bolometer can be described by a simple model along with a small number of parameters. The SPIRE instrument for the Herschel Space Observatory contains five arrays of NTD germanium spiderweb bolometers containing up to 139 pixels. We show from characterisation measurements on the ground using the flight read-out system that the bolometers follow the ideal model extremely well, are very stable, and that the read-out system is sufficiently well behaved to take advantage of this. Calibration should be greatly simplified by being able to take advantage of this behaviour.

Published
2008

32. Locating the Dust in A Star Debris Discs

Author

Booth, Mark, primary, Kennedy, Grant, additional, Sibthorpe, Bruce, additional, Matthews, Brenda C., additional, Wyatt, Mark C., additional, Duchêne, Gaspard, additional, Kavelaars, J. J., additional, Rodriguez, David, additional, Greaves, Jane S., additional, Koning, Alice, additional, Vican, Laura, additional, Rieke, George H., additional, Su, Kate Y. L., additional, Moro-Martín, Amaya, additional, and Kalas, Paul, additional

Published
2013
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34. Herschel Observations of the HR 8799 Disk

Author

Matthews, Brenda C., primary, Kennedy, Grant, additional, Sibthorpe, Bruce, additional, Booth, Mark, additional, Broekhoven-Fiene, Hannah, additional, Wyatt, Mark, additional, Macintosh, Bruce, additional, and Marois, Christian, additional

Published
2013
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35. MILLIMETER EMISSION STRUCTURE IN THE FIRST ALMA IMAGE OF THE AU Mic DEBRIS DISK

Author

MacGregor, Meredith A., primary, Wilner, David J., additional, Rosenfeld, Katherine A., additional, Andrews, Sean M., additional, Matthews, Brenda, additional, Hughes, A. Meredith, additional, Booth, Mark, additional, Chiang, Eugene, additional, Graham, James R., additional, Kalas, Paul, additional, Kennedy, Grant, additional, and Sibthorpe, Bruce, additional

Published
2012
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36. THE DEBRIS DISK AROUND γ DORADUS RESOLVED WITHHERSCHEL

Author

Broekhoven-Fiene, Hannah, primary, Matthews, Brenda C., additional, Kennedy, Grant M., additional, Booth, Mark, additional, Sibthorpe, Bruce, additional, Lawler, Samantha M., additional, Kavelaars, J. J., additional, Wyatt, Mark C., additional, Qi, Chenruo, additional, Koning, Alice, additional, Su, Kate Y. L., additional, Rieke, George H., additional, Wilner, David J., additional, and Greaves, Jane S., additional

Published
2012
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37. Status of the SPIRE photometer data processing pipelines during the early phases of the Herschel Mission

Author

Dowell, C. Darren, primary, Pohlen, Michael, additional, Pearson, Chris, additional, Griffin, Matt, additional, Lim, Tanya, additional, Bendo, George J., additional, Benielli, Dominique, additional, Bock, James J., additional, Chanial, Pierre, additional, Clements, Dave L., additional, Conversi, Luca, additional, Ferlet, Marc, additional, Fulton, Trevor, additional, Gastaud, Rene, additional, Glenn, Jason, additional, Grundy, Tim, additional, Guest, Steve, additional, King, Ken J., additional, Leeks, Sarah J., additional, Levenson, Louis, additional, Lu, Nanyao, additional, Morris, Huw, additional, Nguyen, Hien, additional, O'Halloran, Brian, additional, Oliver, Seb, additional, Panuzzo, Pasquale, additional, Papageorgiou, Andreas, additional, Polehampton, Edward, additional, Rigopoulou, Dimitra, additional, Roussel, Helene, additional, Schneider, Nicola, additional, Schulz, Bernhard, additional, Schwartz, Arnold, additional, Shupe, David L., additional, Sibthorpe, Bruce, additional, Sidher, Sunil, additional, Smith, Anthony J., additional, Swinyard, Bruce M., additional, Trichas, Markos, additional, Valtchanov, Ivan, additional, Woodcraft, Adam L., additional, Xu, C. Kevin, additional, and Zhang, Lijun, additional

Published
2010
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39. Gas Evolution in Protoplanetary Disks

Author

Woitke, Peter, primary, Dent, Bill, additional, Thi, Wing-Fai, additional, Sibthorpe, Bruce, additional, Rice, Ken, additional, Williams, Jonathan, additional, Sicilia-Aguilar, Aurora, additional, Brown, Joanna, additional, Kamp, Inga, additional, Pascucci, Ilaria, additional, Alexander, Richard, additional, Roberge, Aki, additional, and Stempels, Eric, additional

Published
2009
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40. Physics based calibration of the Herschel∕SPIRE bolometers

Author

Woodcraft, Adam L., primary, Nguyen, Hien, additional, Bock, James, additional, Griffin, Matthew, additional, Schulz, Bernhard, additional, Sibthorpe, Bruce, additional, Swinyard, Bruce, additional, Young, Betty, additional, Cabrera, Blas, additional, and Miller, Aaron, additional

Published
2009
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41. Understanding the Herschel-SPIRE bolometers

Author

Woodcraft, Adam L., primary, Nguyen, Hien, additional, Bock, James, additional, Griffin, Matthew, additional, Schulz, Bernhard, additional, Sibthorpe, Bruce, additional, and Swinyard, Bruce, additional

Published
2008
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42. The Herschel-SPIRE photometer data processing pipeline

Author

Griffin, Matt, primary, Dowell, C. Darren, additional, Lim, Tanya, additional, Bendo, George, additional, Bock, Jamie, additional, Cara, Christophe, additional, Castro-Rodriguez, Nieves, additional, Chanial, Pierre, additional, Clements, Dave, additional, Gastaud, Rene, additional, Guest, Steve, additional, Glenn, Jason, additional, Hristov, Victor, additional, King, Ken, additional, Laurent, Glenn, additional, Lu, Nanyao, additional, Mainetti, Gabrielle, additional, Morris, Huw, additional, Nguyen, Hien, additional, Panuzzo, Pasquale, additional, Pearson, Chris, additional, Pinsard, Frederic, additional, Pohlen, Michael, additional, Polehampton, Edward, additional, Rizzo, Davide, additional, Schulz, Bernhard, additional, Schwartz, Arnold, additional, Sibthorpe, Bruce, additional, Swinyard, Bruce, additional, Xu, Kevin, additional, and Zhang, Lijun, additional

Published
2008
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43. Physics based calibration of the Herschel/SPIRE bolometers.

Author

Woodcraft, Adam L., Nguyen, Hien, Bock, James, Griffin, Matthew, Schulz, Bernhard, Sibthorpe, Bruce, and Swinyard, Bruce

Subjects
CALIBRATION, PHYSICAL measurements, HEAT sinks (Electronics), DETECTORS, FLUCTUATIONS (Physics)
Abstract

The bolometers (and readout circuitry) in the SPIRE instrument on the Herschel Space Observatory are among the best understood and well characterised of any sub-mm astronomy instrument to date. SPIRE contains five arrays of NTD germanium spiderweb bolometers with up to 139 pixels per array. Their behaviour has been shown to be extremely stable as seen by repeated measurements in the years between initial array level and final instrument level tests, and can be described extremely well by a simple physical model (the ideal bolometer model). Calibration of the bolometers must take into account the non-linear response when viewing bright sources, and the effect of fluctuations in the heat sink temperature. The simple and well-understood behaviour of the detectors, coupled with the stable conditions expected in flight, mean that in contrast to previous sub-mm instruments, physical models can be used to improve or possibly replace empirical calibration methods. We describe how this can be done, and use the large amount of data from ground measurements to show that we can use models to accurately calculate the absolute power detected by the bolometers. [ABSTRACT FROM AUTHOR]

Published
2009
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47. RESOLVED IMAGING OF THE HR 8799 DEBRIS DISK WITH HERSCHEL.

Author

Matthews, Brenda, Kennedy, Grant, Sibthorpe, Bruce, Booth, Mark, Wyatt, Mark, Broekhoven-Fiene, Hannah, Macintosh, Bruce, and Marois, Christian

Subjects
CONSORTIA, CIRCUMSTELLAR matter, INTERSTELLAR medium
Abstract

We present Herschel far-infrared and submillimeter maps of the debris disk associated with the HR 8799 planetary system. We resolve the outer disk emission at 70, 100, 160, and 250 μm and detect the disk at 350 and 500 μm. A smooth model explains the observed disk emission well. We observe no obvious clumps or asymmetries associated with the trapping of planetesimals that is a potential consequence of planetary migration in the system. We estimate that the disk eccentricity must be <0.1. As in previous work by Su et al., we find a disk with three components: a warm inner component and two outer components, a planetesimal belt extending from 100 to 310 AU, with some flexibility (±10 AU) on the inner edge, and the external halo that extends to ∼2000 AU. We measure the disk inclination to be 26° ± 3° from face-on at a position angle of 64° E of N, establishing that the disk is coplanar with the star and planets. The spectral energy distribution of the disk is well fit by blackbody grains whose semi-major axes lie within the planetesimal belt, suggesting an absence of small grains. The wavelength at which the spectrum steepens from blackbody, 47 ± 30 μm, however, is short compared with other A star debris disks, suggesting that there are atypically small grains likely populating the halo. The PACS longer wavelength data yield a lower disk color temperature than do MIPS data (24 and 70 μm), implying two distinct halo dust-grain populations. [ABSTRACT FROM AUTHOR]

Published
2014
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48. Spatially resolved images of dust belt(s) around the planet-hosting subgiant κ CrB.

Author

Bonsor, Amy, Kennedy, Grant M., Crepp, Justin R., Johnson, John A., Wyatt, Mark C., Sibthorpe, Bruce, and Su, Kate Y. L.

Subjects
PLANETARY orbits, IMAGE analysis, DUST, DISKS (Astrophysics), SUBGIANT stars, CHROMIUM compounds
Abstract

We present Herschel spatially resolved images of the debris disc orbiting the subgiant κ Coronae Borealis (κ CrB). Not only are these the first resolved images of a debris disc orbiting a subgiant, but κ CrB is a rare example of an intermediate mass star where a detailed study of the structure of the planetary system can be made, including both planets and planetesimal belt(s). The only way to discover planets using the radial velocity technique around such stars is to observe ‘retired’ A stars, which are cooler and slower rotators compared to their main-sequence counterparts. A planetary companion has already been detected orbiting the subgiant κ CrB, with revised parameters of msin i = 2.1 MJ and apl = 2.8 au (Johnson et al. 2008). We present additional Keck I HIRES (High Resolution Echelle Spectrometer) radial velocity measurements that provide evidence for a second planetary companion, alongside Keck II adaptive optics imaging that places an upper limit on the mass of this companion. Modelling of our Herschel images shows that the dust is broadly distributed, but cannot distinguish between a single wide belt (from 20 to 220 au) or two narrow dust belts (at around 40 and 165 au). Given the existence of a second planetary companion beyond ∼3 au it is possible that the absence of dust within ∼20 au is caused by dynamical depletion, although the observations are not inconsistent with depletion of these regions by collisional erosion, which occurs at higher rates closer to the star. [ABSTRACT FROM AUTHOR]

Published
2013
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49. Resolved debris discs around A stars in the Herschel DEBRIS survey★.

Author

Booth, Mark, Kennedy, Grant, Sibthorpe, Bruce, Matthews, Brenda C., Wyatt, Mark C., Duchêne, Gaspard, Kavelaars, J. J., Rodriguez, David, Greaves, Jane S., Koning, Alice, Vican, Laura, Rieke, George H., Su, Kate Y. L., Moro-Martín, Amaya, and Kalas, Paul

Subjects
SPACE debris, STELLAR photospheres, ASTRONOMICAL photometry, TEMPERATURE effect, PARTICLE size distribution, SPECTRAL energy distribution, CIRCUMSTELLAR matter, SURVEYS
Abstract

The majority of debris discs discovered so far have only been detected through infrared excess emission above stellar photospheres. While disc properties can be inferred from unresolved photometry alone under various assumptions for the physical properties of dust grains, there is a degeneracy between disc radius and dust temperature that depends on the grain size distribution and optical properties. By resolving the disc we can measure the actual location of the dust. The launch of Herschel, with an angular resolution superior to previous far-infrared telescopes, allows us to spatially resolve more discs and locate the dust directly. Here we present the nine resolved discs around A stars between 20 and 40 pc observed by the Disc Emission via a Bias-free Reconnaissance in the Infrared/Submillimetre (DEBRIS) survey. We use these data to investigate the disc radii by fitting narrow ring models to images at 70, 100 and 160 μm and by fitting blackbodies to full spectral energy distributions. We do this with the aim of finding an improved way of estimating disc radii for unresolved systems. The ratio between the resolved and blackbody radii varies between 1 and 2.5. This ratio is inversely correlated with luminosity and any remaining discrepancies are most likely explained by differences to the minimum size of grain in the size distribution or differences in composition. We find that three of the systems are well fit by a narrow ring, two systems are borderline cases and the other four likely require wider or multiple rings to fully explain the observations, reflecting the diversity of planetary systems. [ABSTRACT FROM PUBLISHER]

Published
2013
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