<i>Hubble Space Telescope</i>ACS Coronagraphic Imaging of the Circumstellar Disk around HD 141569A

Clampin, Mark; Krist, John; Ardila, D. R.; Golimowski, D. A.; Hartig, G.; Ford, H. C.; Illingworth, G. D.; Bartko, F.; Benı́tez, N.; Blakeslee, John P.; Broadhurst, Tom; Brown, Robert A.; Burrows, Christopher J.; Cheng, E. S.; Cross, N. J. G.; Feldman, P. D.; Franx, Marijn; Grönwall, C.; Infante, L.; Kimble, Randy A.; Lesser, Michael P.; Martel, A. R.; Menanteau, F.; Meurer, G. R.; Miley, G. K.; Postman, Marc; Rosati, P.; Sirianni, M.; Sparks, W. B.; Tran, H. D.; Tsvetanov, Z.; White, R. L.; Zheng, Wei

doi:10.1086/375460

Cited by 157 publications

(191 citation statements)

References 23 publications

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“…Takeuchi & Artymowicz (2001) predict a single ring, while two distinct rings are observed (Weinberger et al 1999;Clampin et al 2003;Biller et al 2015). A Saturn-mass planet embedded in the outer disk could carve out a gap and stir up the grains enough to create two rings (Wyatt 2005), and Biller et al (2015) find tentative evidence of a stellocentric offset that is consistent with perturbations from a planet.…”

Section: Discussionmentioning

confidence: 93%

“…A close passage between one of the companions and the disk would truncate the disk, and excite dust grains just inside this truncation radius leading to the creation of small dust grains (Ardila et al 2005;Reche et al 2009). Such a passage has been invoked to explain the large, low-surface brightness spiral features in the outer reaches of the disk (Clampin et al 2003).…”

Section: Discussionmentioning

confidence: 99%

“…While still fairly young, this system does not exhibit a strong infrared excess; instead its dust emission is more characteristic of an optically thin debris disk with L IR /L * ∼8×10 −3 (Sylvester et al 1996). Scattered light images find small dust grains confined to two narrow rings at 240 and 400 au (Biller et al 2015), with a gap between them (Augereau et al 1999;Weinberger et al 1999) and evidence for spiral arms in the outermost ring (Clampin et al 2003). Interior to these rings there is very little scattered light emission from small dust grains, although mid-infrared thermal dust emission has been detected down to tens of au (Fisher et al 2000;Marsh et al 2002;Moerchen et al 2010).…”

Section: Introductionmentioning

confidence: 88%

“…These scattered light rings are at a radius of roughly 245 and 400 au (Augereau et al 1999;Weinberger et al 1999Weinberger et al , 2000Clampin et al 2003;Biller et al 2015), while the 3σ upper limit on the CO gas outer radius is 245 au. Forcing the models to include gas coincident with the scattered light rings, by extending R out to 405 au, and re-running the MCMC modeling routine, produces a significantly worse fit because the gas is forced to extend further out .…”

Section: Surface Densitymentioning

confidence: 99%

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Resolved Co Gas Interior to the Dust Rings of the Hd 141569 Disk

Flaherty

Hughes

Andrews

et al. 2016

ApJ

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The disk around HD 141569 is one of a handful of systems whose weak infrared emission is consistent with a debris disk, but still has a significant reservoir of gas. Here we report spatially resolved millimeter observations of the CO(3-2) and CO(1-0) emission as seen with the Submillimeter Array and CARMA. We find that the excitation temperature for CO is lower than expected from cospatial blackbody grains, similar to previous observations of analogous systems, and derive a gas mass that lies between that of gas-rich primordial disks and gas-poor debris disks. The data also indicate a large inner hole in the CO gas distribution and an outer radius that lies interior to the outer scattered light rings. This spatial distribution, with the dust rings just outside the gaseous disk, is consistent with the expected interactions between gas and dust in an optically thin disk. This indicates that gas can have a significant effect on the location of the dust within debris disks.

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Section: Discussionmentioning

confidence: 93%

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 88%

Section: Surface Densitymentioning

confidence: 99%

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Resolved Co Gas Interior to the Dust Rings of the Hd 141569 Disk

Flaherty

Hughes

Andrews

et al. 2016

ApJ

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“…Radio and IR observations are well suited to map the extended disk structure. Optical and IR coronographic observations with the HST have provided high-quality images of the disk structure at large (e.g., Clampin et al, 2003). However, UV spectroscopy is the most sensitive tool for determining the column density of hydrogen and the fraction of hydrogen atoms in molecular form (see, for instance, Bouret et al, 2003;Grady et al, 2005).…”

Section: Herbig Ae/be Starsmentioning

confidence: 99%

UV Capabilities to Probe the Formation of Planetary Systems: From the ISM to Planets

Castro

Lecavelier

D’Avillez

et al.

Fundamental Questions in Astrophysics: Guidelines for Future UV Observatories

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Planetary systems are angular momentum reservoirs generated during star formation. Solutions to three of the most important problems in contemporary astrophysics are needed to understand the entire process of planetary system formation:The physics of the ISM. Stars form from dense molecular clouds that contain ∼30% of the total interstellar medium (ISM) mass. The structure, properties and lifetimes of molecular clouds are determined by the overall dynamics and evolution of a very complex system -the ISM. Understanding the physics of the ISM is of prime importance not only for Galactic but also for extragalactic and cosmological studies. Most of the ISM volume (∼65%) is filled with diffuse gas at temperatures between 3000 and 300 000 K, representing about 50% of the ISM mass. ing star formation, the so-called accretion-outflow engine. Elementary physical considerations show that, to be efficient, the acceleration region for the outflows must be located close to the star (within 1 AU) where the gravitational field is strong. According to recent numerical simulations, this is also the region where terrestrial planets could form after 1 Myr. One should keep in mind that today the only evidence for life in the Universe comes from a planet located in this inner disk region (at 1 AU) from its parent star. The temperature of the accretion-outflow engine is between 3000 and 10 7 K. After 1 Myr, during the classical T Tauri stage, extinction is small and the engine becomes naked and can be observed at ultraviolet wavelengths. The physics of planet formation. Observations of volatiles released by dust, planetesimals and comets provide an extremely powerful tool for determining the relative abundances of the vaporizing species and for studying the photochemical and physical processes acting in the inner parts of young planetary systems. This region is illuminated by the strong UV radiation field produced by the star and the accretion-outflow engine. Absorption spectroscopy provides the most sensitive tool for determining the properties of the circumstellar gas as well as the characteristics of the atmospheres of the inner planets transiting the stellar disk. UV radiation also pumps the electronic transitions of the most abundant molecules (H 2 , CO, etc.) that are observed in the UV.Here we argue that access to the UV spectral range is essential for making progress in this field, since the resonance lines of the most abundant atoms and ions at temperatures between 3000 and 300 000 K, together with the electronic transitions of the most abundant molecules (H 2 , CO, OH, CS, Springer 34 Astrophys Space Sci (2006) 303:33-52 S 2 , CO + 2 , C 2 , O 2 , O 3 , etc.) are at UV wavelengths. A powerful UV-optical instrument would provide an efficient mean for measuring the abundance of ozone in the atmosphere of the thousands of transiting planets expected to be detected by the next space missions (GAIA, Corot, Kepler, etc.). Thus, a follow-up UV mission would be optimal for identifying Earth-like candidates.

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Pinpointing Planets in Circumstellar Disks

Quillen

2010

Formation and Evolution of Exoplanets

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A crowning achievement in mathematical science was the prediction by Urbain Le Verrier and John Couch Adams in 1845 of a previously unknown planet that was then subsequently discovered. Irregularities in Uranus's orbit were elegantly explained as being due to a single massive object exerting perturbations on Uranus and the position of the object in the sky was predicted. The planet Neptune was subsequently detected by Johann Gottfried Galle at the Berlin Observatory (cf.[1]). Planets can not only perturb each other, as outlined in the original perturbative theory by Laplace, but also perturb the orbits of smaller particles such as dust that can be much more numerous and so can reemit a detectable fraction of the host star luminosity. Disk morphology can provide dynamical evidence for massive bodies that can be subsequently discovered from direct observations. We can refer to historical examples in our solar system. For example, the prediction of a satellite in the Encke gap in Saturn's rings based on wavy edges seen in the gap [2], was followed by the discovery of the satellite, Pan [3].In this chapter, a broad base of dynamical work relating circumstellar disk morphology to underlying planetary architecture is reviewed. The existence of a planet was predicted on the basis of its interactions with the circumstellar disk in the Fomalhaut system [4] at a semimajor axis of 119 AU. Subsequently, a planet was discovered with an estimated semimajor axis of 115 AU [5], only 4 AU lower than predicted. This is the first planet whose existence was successfully predicted from its interactions with the surrounding circumstellar disk (see Figure 2.1). discovery illustrates that we can, in some cases, predict the presence of planetary bodies from their interactions with disk material. The discrepancies between the predicted planetary orbit and mass from those inferred from observations are and will continue to be interesting. In probing them, we will improve our theoretical understanding and extend our capabilities so that we can accurately infer planetary system architecture at levels below the concurrent detection limits. In this chapter, we discuss some of the broad foundation of work that this prediction and others are built Formation and Evolution of Exoplanets. Edited by Rory Barnes

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Hubble Space TelescopeACS Coronagraphic Imaging of the Circumstellar Disk around HD 141569A

Cited by 157 publications

References 23 publications

Resolved Co Gas Interior to the Dust Rings of the Hd 141569 Disk

Resolved Co Gas Interior to the Dust Rings of the Hd 141569 Disk

UV Capabilities to Probe the Formation of Planetary Systems: From the ISM to Planets

Pinpointing Planets in Circumstellar Disks

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