A Deep Polarimetric Study of the Asymmetrical Debris Disk HD 106906

Crotts, Katie A.; Matthews, Brenda C.; Espósito, Thomas M.; Duchêne, Gaspard; Kalas, Paul; Chen, Christine; Arriaga, Pauline; Millar‐Blanchaer, Maxwell A.; Debes, John H.; Draper, Zachary H.; Fitzgerald, Michael P.; Hom, Justin; MacGregor, Meredith A.; Mazoyer, Johan; Patience, Jennifer; Rice, Malena; Weinberger, Alycia J.; Wilner, David J.; Wolff, Schuyler

doi:10.3847/1538-4357/abff5c

Cited by 17 publications

(49 citation statements)

References 56 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Doing so, we obtain an intrinsic FWHM of 0.12 ± 0 1 for the J and H bands, and 0.14 ± 0 1 for the K1 band (13-15 au), which leads to a aspect ratio of ∼0.28 at 50 au. This aspect ratio is intermediate between similar measurements at 50 au for other near edge-on debris disks such as HD 32297 (0.17; Duchêne et al 2020) and HD 106906 (0.31;Crotts et al 2021), although these comparisons are purely from empirical estimates and not from a proper disk model. A positive trend can be seen in the NW extension in all three bands, showing that the vertical width increases with radial distance on this side, while the SE extension is flat past 0 6.…”

Section: Vertical Structurecontrasting

confidence: 60%

“…In some cases disk structure can be directly traced to a known planet sculpting the disk such as in the case of β Pic (Mouillet et al 1997;Dawson et al 2011;Apai et al 2015). Another example of this is the asymmetrical debris disk HD 106906, which exhibits both a brightness asymmetry and eccentricity (Kalas et al 2015;Lagrange et al 2016;Crotts et al 2021). Through empirical analysis, these asymmetries are shown to be likely due to the 11 M Jup planet in the system that orbits outside of the disk, and unlikely to be due to an ISM interaction (Crotts et al 2021).…”

Section: Introductionmentioning

confidence: 99%

“…Another example of this is the asymmetrical debris disk HD 106906, which exhibits both a brightness asymmetry and eccentricity (Kalas et al 2015;Lagrange et al 2016;Crotts et al 2021). Through empirical analysis, these asymmetries are shown to be likely due to the 11 M Jup planet in the system that orbits outside of the disk, and unlikely to be due to an ISM interaction (Crotts et al 2021). While both β Pic and HD 106906 have known planetary companions, there are other highly asymmetrical debris disks in which no known planets exist.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

A Multiwavelength Study of the Highly Asymmetrical Debris Disk around HD 111520

Crotts

Draper

Matthews

et al. 2022

ApJ

Self Cite

View full text Add to dashboard Cite

We observed the nearly edge-on debris disk system HD 111520 at the HJ and K1 near-infrared (NIR) bands using both the spectral and polarization modes of the Gemini Planet Imager. With these new observations, we have performed an empirical analysis in order to better understand the disk morphology and its highly asymmetrical nature. We find that the disk features a large brightness and radial asymmetry, most prominent at shorter wavelengths. We also find that the radial location of the peak polarized intensity differs on either side of the star by 11 au, suggesting that the disk may be eccentric, although, such an eccentricity does not fully explain the large brightness and radial asymmetry observed. Observations of the disk halo with the Hubble Space Telescope also show the disk to be warped at larger separations, with a bifurcation feature in the northwest, further suggesting that there may be a planet in this system creating an asymmetrical disk structure. Measuring the disk color shows that the brighter extension is bluer compared to the dimmer extension, suggesting that the two sides have different dust grain properties. This finding, along with the large brightness asymmetry, are consistent with the hypothesis that a giant impact occurred between two large bodies in the northern extension of the disk, although confirming this based on NIR observations alone is not feasible. Follow-up imaging with the Atacama Large Millimeter/submillimeter Array to resolve the asymmetry in the dust mass distribution is essential in order to confirm this scenario.

show abstract

Section: Vertical Structurecontrasting

confidence: 60%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

A Multiwavelength Study of the Highly Asymmetrical Debris Disk around HD 111520

Crotts

Draper

Matthews

et al. 2022

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

A Multi-Wavelength Study of the Highly Asymmetrical Debris Disk Around HD 111520

Crotts,

Draper,

Matthews

et al. 2022

Preprint

Self Cite

View full text Add to dashboard Cite

We observed the nearly edge-on debris disk system HD 111520 at J, H, & K1 near infrared (NIR) bands using both the spectral and polarization modes of the Gemini Planet Imager (GPI). With these new observations, we have performed an empirical analysis in order to better understand the disk morphology and its highly asymmetrical nature. We find that the disk features a large brightness and radial asymmetry, most prominent at shorter wavelengths. We also find that the radial location of the peak polarized intensity differs on either side of the star by 11 AU, suggesting that the disk may be eccentric, although, such an eccentricity does not fully explain the large brightness and radial asymmetry observed. Observations of the disk halo with HST also show the disk to be warped at larger separations, with a bifurcation feature in the northwest, further suggesting that there may be a planet in this system creating an asymmetrical disk structure. Measuring the disk color shows that the brighter extension is bluer compared to the dimmer extension, suggesting that the two sides have different dust grain properties. This finding, along with the large brightness asymmetry, are consistent with the hypothesis that a giant impact occurred between two large bodies in the northern extension of the disk, although confirming this based on NIR observations alone is not feasible. Follow-up imaging with ALMA to resolve the asymmetry in the dust mass distribution is essential in order to confirm this scenario.

show abstract

Morphology of the gas-rich debris disk around HD 121617 with SPHERE observations in polarized light

Perrot¹,

Olofsson²,

Kral³

et al. 2023

A&A

View full text Add to dashboard Cite

Context. Debris disks are the signposts of collisionally eroding planetesimal circumstellar belts, whose study can put important constraints on the structure of extrasolar planetary systems. The best constraints on the morphology of such disks are often obtained from spatially resolved observations in scattered light. In this paper, we investigate the young (~16 Myr) bright gas-rich debris disk around HD 121617. Aims. We use new scattered light observations from VLT/SPHERE to characterize the morphology and the dust properties of the debris disk. From these properties, we can then derive constraints on the physical and dynamical environment of this system, for which significant amounts of gas have been detected. Methods. The disk morphology is constrained by linear polarimetric observations in the J band. Based on our modeling results and archival photometry, we also model the spectral energy distribution (SED) to put constraints on the total dust mass and dust size distribution. Finally, we explore different scenarios that could explain these new constraints. Results. We present the first resolved image in scattered light of the debris disk around HD 121617. We fit the morphology of the disk, finding a semi-major axis of 78.3 ± 0.2 au, an inclination of 43.1 ± 0.2°, and a position angle of the major axis with respect to north of 239.8 ± 0.3°, which is compatible with the previous continuum and CO detection with ALMA. Our analysis shows that the disk has a very sharp inner edge, possibly sculpted by a yet-undetected planet or gas drag. While less sharp, its outer edge is steeper than expected for an unperturbed disk, which could also be due to a planet or gas drag, but future observations probing the system farther from the main belt would help explore this possibility further. The SED analysis leads to a dust mass of 0.21 ± 0.02 M⊕ and a minimum grain size of 0.87 ± 0.12 μm, smaller than the blowout size by radiation pressure, which is not unexpected for very bright collisionally active disks.

show abstract

A Deep Polarimetric Study of the Asymmetrical Debris Disk HD 106906

Cited by 17 publications

References 56 publications

A Multiwavelength Study of the Highly Asymmetrical Debris Disk around HD 111520

A Multiwavelength Study of the Highly Asymmetrical Debris Disk around HD 111520

A Multi-Wavelength Study of the Highly Asymmetrical Debris Disk Around HD 111520

Morphology of the gas-rich debris disk around HD 121617 with SPHERE observations in polarized light

Contact Info

Product

Resources

About