The Big Sibling of AU Mic: A Cold Dust-rich Debris Disk around CP−72 2713 in the β Pic Moving Group

Moór, A.; Pawellek, N.; Ábrahám, P.; Kóspál, Á.; Vida, K.; Pál, András; Dutrey, Anne; Folco, E. Di; Hughes, A. Meredith; Kral, Quentin; Pascucci, Ilaria

doi:10.3847/1538-3881/ab8f98

Cited by 18 publications

(20 citation statements)

References 131 publications

(170 reference statements)

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“…More recently, this standard model has been improved upon to include grain-size dependant tensile strengths (Pan & Sari 2005) and velocity distributions (Gáspár et al 2012a;Pan & Schlichting 2012) which result in a range of the grain size distribution exponent between 3 and 4. This theoretically estimated range of is supported by a number of millimetre wavelength observations (Ricci et al 2012(Ricci et al , 2015bMacGregor et al 2016;Marshall et al 2017;Wilner et al 2018;Moór et al 2020). To date, numerical modelling of observations has constrained the parameter to 3.2 < < 3.8 for various grain materials (Hughes et al 2018;Löhne 2020).…”

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confidence: 61%

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Four new planetesimals around typical and pre-main-sequence stars (PLATYPUS) debris discs at 8.8 mm

Norfolk

Maddison

Marshall

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Millimetre continuum observations of debris discs can provide insights into the physical and dynamical properties of the unseen planetesimals that these discs host. The material properties and collisional models of planetesimals leave their signature on the grain size distribution, which can be traced through the millimetre spectral index. We present 8.8 mm observations of the debris discs HD 48370, CPD-72 2713, HD 131488, and HD 32297 using the Australian Telescope Compact Array (ATCA) as part of the PLanetesimals Around TYpical Pre-main seqUence Stars (PLATYPUS) survey. We detect all four targets with a characteristic beam size of 5″ and derive a grain size distribution parameter that is consistent with collisional cascade models and theoretical predictions for parent planetesimal bodies where binding is dominated by self-gravity. We combine our sample with 19 other millimetre-wavelength detected debris discs from the literature and calculate a weighted mean grain size power law index which is close to analytical predictions for a classical steady state collisional cascade model. We suggest the possibility of two distributions of q in our debris disc sample; a broad distribution (where q ∼ 3.2 − 3.7) for ”typical” debris discs (gas-poor/non-detection), and a narrow distribution (where q < 3.2) for bright gas-rich discs. Or alternatively, we suggest that there exists an observational bias between the grain size distribution parameter and absolute flux which may be attributed to the detection rates of faint debris discs at $\rm \sim$cm wavelengths.

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confidence: 61%

“…It resides at a distance of 36.66 ± 0.03 pc (Gaia Collaboration et al 2018) and is a member of the ≈ 24 Myr old Pic moving group (Torres et al 2006;Bell et al 2015;. With new 1.33 mm ALMA observations, Moór et al (2020) estimates the outer radius of the cold debris disc surrounding the host star to be 140±14 au.…”

Section: Cpd-72 2713mentioning

confidence: 99%

Four new planetesimals around typical and pre-main-sequence stars (PLATYPUS) debris discs at 8.8 mm

Norfolk

Maddison

Marshall

et al. 2021

Monthly Notices of the Royal Astronomical Society

Self Cite

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“…Our best-fitting model to the disk scattered light images is one with a peak disk radius at ∼70 au, and a fractional luminosity  L L 6 IR tot 1 2-+ 10 −4 . Recently Moór et al (2020) and Tanner et al (2020) presented the discovery of CP-72 2713, another BPMG member with a cold debris disk, and a relatively high fractional luminosity of 1.1 × 10 −3 , suggesting it is a more massive, dust-rich "sibling" to the debris disk system associated with AU Mic (L IR /L tot ; 3.5 × 10 −4 ; Matthews et al 2015). With a fractional luminosity of  L L 6 IR tot 1 2-+ 10 −4 , our study suggests BD+45°598 could also be considered another dust-rich counterpart to AU Mic.…”

Section: Discussionmentioning

confidence: 99%

Discovery of an Edge-on Circumstellar Debris Disk around BD+45° 598: A Newly Identified Member of the β Pictoris Moving Group

Hinkley

Matthews

Lefèvre

et al. 2021

ApJ

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We report the discovery of a circumstellar debris disk viewed nearly edge-on and associated with the young, K1 star BD+45°598 using high-contrast imaging at 2.2 μm obtained at the W.M. Keck Observatory. We detect the disk in scattered light with a peak significance of ∼5σ over three epochs, and our best-fit model of the disk is an almost edge-on ∼70 au ring, with inclination angle ∼87°. Using the NOEMA interferometer at the Plateau de Bure Observatory operating at 1.3 mm, we find resolved continuum emission aligned with the ring structure seen in the 2.2 μm images. We estimate a fractional infrared luminosity of L IR /L tot  6 1 2 -+ × 10 −4 , higher than that of the debris disk around AU Mic. Several characteristics of BD+45°598, such as its galactic space motion, placement in a color-magnitude diagram, and strong presence of lithium, are all consistent with its membership in the β Pictoris Moving Group with an age of 23 ± 3 Myr. However, the galactic position for BD+45°598 is slightly discrepant from previously known members of the β Pictoris Moving Group, possibly indicating an extension of members of this moving group to distances of at least 70 pc. BD+45°598 appears to be an example from a population of young circumstellar debris systems associated with newly identified members of young moving groups that can be imaged in scattered light, key objects for mapping out the early evolution of planetary systems from ∼10-100 Myr. This target will also be ideal for northern-hemisphere, high-contrast imaging platforms to search for self-luminous, planetary mass companions residing in this system.

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“…Our best fitting model to the disk scattered light images is one with a peak disk radius at ∼70 AU, and a fractional luminosity L IR /L tot 6 +2 −1 ×10 −4 . Recently Moór et al (2020) and Tanner et al (2020) presented the discovery of CP-72 2713, another BPMG member with a cold debris disk, and a relatively high fractional luminosity of 1.1×10 −3 , suggesting it is a more massive, dust-rich "sibling" to the debris disk system associated with AU Mic (L IR /L tot 3.5×10 −4 ; Matthews et al 2015). With a fractional luminosity of L IR /L tot 6 +2 −1 ×10 −4 , our study suggests BD+45 • 598 could also be considered another dust-rich counterpart to AU Mic.…”

Section: Discussionmentioning

confidence: 99%

Discovery of an Edge-on Circumstellar Debris Disk Around BD+45$^{\circ}$598: a Newly Identifed Member of the $β$ Pictoris Moving Group

Hinkley,

Matthews,

Lefevre

et al. 2021

Preprint

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We report the discovery of a circumstellar debris disk viewed nearly edge-on and associated with the young, K1 star BD+45 • 598 using high-contrast imaging at 2.2 µm obtained at the W.M. Keck Observatory. We detect the disk in scattered light with a peak significance of ∼5σ over three epochs, and our best-fit model of the disk is an almost edge-on ∼70 AU ring, with inclination angle ∼87 • . Using the NOEMA interferometer at the Plateau de Bure Observatory operating at 1.3 mm, we find resolved continuum emission aligned with the ring structure seen in the 2.2 µm images. We estimate a fractional infrared luminosity of L IR /L tot 6 +2 −1 × 10 −4 , higher than that of the debris disk around AU Mic. Several characteristics of BD+45 • 598, such as its galactic space motion, placement in a colormagnitude diagram, and strong presence of Lithium, are all consistent with its membership in the β Pictoris Moving Group with an age of 23 ± 3 Myr. However, the galactic position for BD+45 • 598 is slightly discrepant from previously-known members of the β Pictoris Moving Group, possibly indicating an extension of members of this moving group to distances of at least 70 pc. BD+45 • 598 appears to be an example from a population of young circumstellar debris systems associated with newly identified members of young moving groups that can be imaged in scattered light, key objects for mapping out the early evolution of planetary systems from ∼10-100 Myr. This target will also be ideal for northern-hemisphere, high-contrast imaging platforms to search for self-luminous, planetary mass companions residing in this system.

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The Big Sibling of AU Mic: A Cold Dust-rich Debris Disk around CP−72 2713 in the β Pic Moving Group

Cited by 18 publications

References 131 publications

Four new planetesimals around typical and pre-main-sequence stars (PLATYPUS) debris discs at 8.8 mm

Four new planetesimals around typical and pre-main-sequence stars (PLATYPUS) debris discs at 8.8 mm

Discovery of an Edge-on Circumstellar Debris Disk around BD+45° 598: A Newly Identified Member of the β Pictoris Moving Group

Discovery of an Edge-on Circumstellar Debris Disk Around BD+45$^{\circ}$598: a Newly Identifed Member of the $β$ Pictoris Moving Group

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