Deep ALMA search for CO gas in the HD 95086 debris disc

Booth, Mark; Matrà, Luca; Su, Kate; Kral, Quentin; Hales, Antonio; Dent, W. R. F.; Hughes, A. Meredith; MacGregor, Meredith A.; Löhne, T.; Wilner, David J.

doi:10.1093/mnras/sty2993

Cited by 15 publications

(13 citation statements)

References 41 publications

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“…In subsection 2.1, we demonstrated that even if it is a member of LCC, the latest data predict that the RV should then be closer to 16±4 km s −1 and in the more likely case that it is a member of Carina, the RV should be close to 17.1±0.6 km s −1 , in perfect agreement with the spectroscopic measurement of 17±2 km s −1 (Moór et al 2013b). From this we can conclude that the tentative detection of gas from Booth et al (2019) must, in fact, just be a spurious noise signal and no gas has yet been detected in the HD 95086 debris disc.…”

Section: Gas In the Hd 95086 Debris Discsupporting

confidence: 82%

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The age of the carina young association and potential membership of HD 95086

Booth

Burgo

Hambaryan

2020

Monthly Notices of the Royal Astronomical Society

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Carina is a nearby young stellar association. So far, only a small number of stars have been clearly identified as members of this association. In this paper we reanalyse the membership of the association in light of Gaia DR2 data, in particular finding that HD 95086 is a potential member (probability of 71%). This star is noteworthy as one of the few stars that hosts both a detected debris disc and a directly imaged planet. It has previously only been considered as a potential member of the Lower Centaurus Crux (LCC) – part of the Scorpius-Centaurus association. We also reanalyse the age of the Carina association. Using a Bayesian inference code applied to infer a solution from stellar evolution models for the most probable (>99%) members of Carina, we infer an age for the association of 13.3$^{+1.1}_{-0.6}$ Myr, much younger than previous studies. Whilst we have revised HD 95086’s association membership from LCC to Carina, the fact that we also find Carina to have a younger age, similar to that of LCC, means that the estimates of HD 95086b’s mass remain unchanged. However, the younger age of Carina does mean that the companion to another Carina member, HD 44627 (AB Pic), has a mass that is more clearly in the planet rather than brown dwarf range.

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Section: Gas In the Hd 95086 Debris Discsupporting

confidence: 82%

“…So far, however, no publication has considered the possibility that it is a member of a different association. Due to questions about its RV, particularly in relation to the possible presence of CO gas in its debris disc (Booth et al 2019), we have reason to question its association membership.…”

Section: Hd 95086mentioning

confidence: 99%

The age of the carina young association and potential membership of HD 95086

Booth

Burgo

Hambaryan

2020

Monthly Notices of the Royal Astronomical Society

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“…Alternatively, observations at a different wavelength could be used to measure the disc and clump spectral index and see if they differ, which could suggest that the observed residual is background emission. The difference in spectral index was used as an evidence for the extra-galactic origin of a clump in HD 95086 ALMA observations (Su et al 2017;Booth et al 2019).…”

Section: Resultsmentioning

confidence: 99%

A gap in HD 92945’s broad planetesimal disc revealed by ALMA

Marino

Yelverton

Booth

et al. 2019

Monthly Notices of the Royal Astronomical Society

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In the last few years multiwavelength observations have revealed the ubiquity of gaps/rings in circumstellar discs. Here we report the first ALMA observations of HD 92945 at 0.86 mm, that reveal a gap at about 73 ± 3 au within a broad disc of planetesimals that extends from 50 to 140 au. We find that the gap is 20 +10 −8 au wide. If cleared by a planet in situ, this planet must be less massive than 0.6 M Jup , or even lower if the gap was cleared by a planet that formed early in the protoplanetary disc and prevented planetesimal formation at that radius. By comparing opposite sides of the disc we also find that the disc could be asymmetric. Motivated by the asymmetry and the fact that planets might be more frequent closer to the star in exoplanetary systems, we show that the gap and asymmetry could be produced by two planets interior to the disc through secular resonances. These planets excite the eccentricity of bodies at specific disc locations, opening radial gaps in the planetesimal distribution. New observations are necessary to confirm if the disc is truly asymmetric, thus favouring the secular resonance model, or if the apparent asymmetry is due to a background galaxy, favouring the in-situ planet scenario. Finally, we also report the non-detection of CO and HCN gas confirming that no primordial gas is present. The CO and HCN non-detections are consistent with the destruction of volatile-rich Solar System-like comets.

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“…The spectral index has also been used to discriminate between possible origins of sub-mm emission (Su et al 2017;Booth et al 2019), since this differs between optically thin dust from planetesimal collisions, mm ≈2−2.5, and extra-galactic emission, mm ≈3−4. In §3.1.2 we derived the spectral index for the full disc of mm =2.34±0.29, which is consistent with measurements of other debris discs Ricci et al (2015a).…”

Section: Clumpiness From Extra-galactic Emission?mentioning

confidence: 99%

High-resolution ALMA and HST images of q1 Eri: an asymmetric debris disc with an eccentric Jupiter

Lovell

Marino

Wyatt

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present ALMA 1.3 mm and 0.86 mm observations of the nearby (17.34 pc) F9V star q1 Eri (HD 10647, HR 506). This system, with age ∼1.4 Gyr, hosts a ∼2 au radial velocity planet and a debris disc with the highest fractional luminosity of the closest 300 FGK type stars. The ALMA images, with resolution ∼0${^{\prime\prime}_{.}}$5, reveal a broad (34-134 au) belt of millimeter emission inclined by 76.7 ± 1.0 degrees with maximum brightness at 81.6 ± 0.5 au. The images reveal an asymmetry, with higher flux near the southwest ansa, which is also closer to the star. Scattered light observed with the Hubble Space Telescope is also asymmetric, being more radially extended to the northeast. We fit the millimeter emission with parametric models and place constraints on the disc morphology, radius, width, dust mass, and scale height. We find the southwest ansa asymmetry is best fitted by an extended clump on the inner edge of the disc, consistent with perturbations from a planet with mass 8 M⊕ − 11 MJup at ∼60 au that may have migrated outwards, similar to Neptune in our Solar System. If the measured vertical aspect ratio of h = 0.04 ± 0.01 is due to dynamical interactions in the disc, then this requires perturbers with sizes >1200 km. We find tentative evidence for an 0.86 mm excess within 10 au, 70 ± 22 μJy, that may be due to an inner planetesimal belt. We find no evidence for CO gas, but set an upper bound on the CO gas mass of 4 × 10−6 M⊕ (3 σ), consistent with cometary abundances in the Solar System.

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Deep ALMA search for CO gas in the HD 95086 debris disc

Cited by 15 publications

References 41 publications

The age of the carina young association and potential membership of HD 95086

The age of the carina young association and potential membership of HD 95086

A gap in HD 92945’s broad planetesimal disc revealed by ALMA

High-resolution ALMA and HST images of q1 Eri: an asymmetric debris disc with an eccentric Jupiter

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