Browsing by Author "Booth, M."
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- ItemDOES THE PRESENCE OF PLANETS AFFECT THE FREQUENCY AND PROPERTIES OF EXTRASOLAR KUIPER BELTS? RESULTS FROM THE HERSCHEL DEBRIS AND DUNES SURVEYS(2015) Moro-Martin, A.; Marshall, J. P.; Kennedy, G.; Sibthorpe, B.; Matthews, B. C.; Eiroa, C.; Wyatt, M. C.; Lestrade, J. -F.; Maldonado, J.; Rodriguez, D.; Greaves, J. S.; Montesinos, B.; Mora, A.; Booth, M.; Duchene, G.; Wilner, D.; Horner, J.The study of the planet-debris disk connection can shed light on the formation and evolution of planetary systems. and may help "predict" the presence of planets around stars with certain disk characteristics. In preliminary analyses of subsamples of the Herschel DEBRIS and DUNES surveys, Wyatt et al. and Marshall et al. identified a tentative correlation between debris and the presence of low-mass planets. Here we use the cleanest possible sample out of these Herschel surveys to assess the presence of such a correlation, discarding stars without known ages, with ages <1 Gyr, and with binary companions <100 AU. to rule out possible correlations due to effects other than planet presence. In our resulting subsample of 204 FGK stars, we do not find evidence that debris disks are more common or more dusty around stars harboring high-mass or low-mass planets compared to a control sample without identified planets. There is no evidence either that the characteristic dust temperature of the debris disks around planet-bearing stars is any different from that in debris disks without identified planets, nor that debris disks are more or less common (or more or less dusty) around stars harboring multiple planets compared to single-planet systems. Diverse dynamical histories may account for the lack of correlations. The data show a correlation between the presence of high-mass planets and stellar metallicity, but no correlation between the presence of low-mass planets or debris and stellar metallicity. Comparing the observed cumulative distribution of fractional luminosity to those expected from a Gaussian distribution in logarithmic scale, we find that a distribution centered on the solar system's value fits the data well, while one centered at 10 times this value can be rejected. This is of interest in the context of future terrestrial planet detection and characterization because it indicates that there are good prospects for finding a large number of debris disk systems (i.e., with evidence of harboring planetesimals, the building blocks of planets) with exozodiacal emission low enough to be appropriate targets for an ATLAST-type mission to search for biosignatures.
- ItemElectrical stimulation therapy of the lower oesophageal sphincter for refractory gastro-oesophageal reflux disease - interim results of an international multicentre trial(2015) Kappelle, W.; Bredenoord, A.; Conchillo, J.; Ruurda, J.; Bouvy, N.; Henegouwen, M.; Chiu, P.; Booth, M.; Hani, A.; Escalona, Alex; Reddy, D.; Bogte, A.; Smout, A.; Wu, J.; Valdovinos, M.; Torres, G.; Siersema, P.
- ItemFrom Scattered-light to Millimeter Emission : A Comprehensive View of the Gigayear-old System of HD 202628 and its Eccentric Debris Ring(2019) Faramaz, V.; Krist, J.; Stapelfeldt, K.R.; Bryden, G.; Mamajek, E.E.; Matra, L.; Booth, M.; Flaherty, K.; Hales, A.S.; Cuadra, Jorge
- ItemIs there really a debris disc around ζ2 reticuli?(2018) Faramaz, V.; Bryden, G.; Stapelfeldt, K.R.; Booth, M.; Bayo, A.; Beust, H.; Casassus, S.; Cuadra Stipetich, Jorge Rodrigo; Hales, A.; Hughes, A.M.; Olofsson, J.; Su, K.Y. L.; Wilner, D.J.
- ItemSub-millimeter non-contaminated detection of the disk around TWA\\,7 by ALMA(2019) Bayo, A.; Olofsson, Johan; Matra, L.; Beamin Muhlenbrock, Juan Carlos; Gallardo, J.; de Gregorio-Monsalvo, I.; Booth, M.; Zamora, C.; Iglesias, D.; Henning, Th.; R. Schreiber, M.; Cáceres Acevedo, Claudio CesarDebris disks can be seen as the left-overs of giant planet formation and the possible nurseries of rocky planets. While M-type stars out-number more massive stars we know very little about the time evolution of their circumstellar disks at ages older than $\sim 10$\,Myr. Sub-millimeter observations are best to provide first order estimates of the available mass reservoir and thus better constrain the evolution of such disks. Here, we present ALMA Cycle\,3 Band\,7 observations of the debris disk around the M2 star TWA\,7, which had been postulated to harbor two spatially separated dust belts, based on unresolved far-infrared and sub-millimeter data. We show that most of the emission at wavelengths longer than $\sim 300$\,$\mu$m is in fact arising from a contaminant source, most likely a sub-mm galaxy, located at about 6.6" East of TWA\,7 (in 2016). Fortunately, the high resolution of our ALMA data allows us to disentangle the contaminant emission from that of the disc and report a significant detection of the disk in the sub-millimeter for the first time with a flux density of 2.1$\pm$0.4 mJy at 870 $\mu$m. With this detection, we show that the SED can be reproduced with a single dust belt.
- ItemSub-millimetre non-contaminated detection of the disc around TWA 7 by ALMA(2019) Beamin Muhlenbrock, Juan Carlos; Bayo, A.; Olofsson, J.; Matrà, L.; Gallardo, J.; de Gregorio-Monsalvo, I.; Booth, M.; Zamora, C.; Iglesias, D.; Henning. Th; Schreiber, M.R.; Cáceres, C.Debris discs can be seen as the leftovers of giant planet formation and the possible nurseries of rocky planets. While M-type stars outnumber more massive stars we know very little about the time evolution of their circumstellar discs at ages older than ∼10 Myr. Sub-millimetre observations are best to provide first order estimates of the available mass reservoir and thus better constrain the evolution of such discs. Here, we present ALMA Cycle 3 Band 7 observations of the debris disc around the M2 star TWA 7, which had been postulated to harbour two spatially separated dust belts, based on unresolved far-infrared and sub-millimetre data. We show that most of the emission at wavelengths longer than ∼300 μm is in fact arising from a contaminant source, most likely a sub-mm galaxy, located at about 6.6 arcsec east of TWA 7 (in 2016). Fortunately, the high resolution of our ALMA data allows us to disentangle the contaminant emission from that of the disc and report a significant detection of the disc in the sub-millimetre for the first time with a flux density of 2.1 ± 0.4 mJy at 870 um. With this detection, we show that the spectral energy distribution can be reproduced with a single dust belt.