THE GRAY NEEDLE: LARGE GRAINS IN THE HD 15115 DEBRIS DISK FROM LBT/PISCES/<i>Ks</i>AND LBTI /LMIRcam/<i>L</i>′ ADAPTIVE OPTICS IMAGING

Rodigas, Timothy J.; Hinz, Philip M.; Leisenring, Jarron; Vaitheeswaran, Vidhya; Skemer, Andrew J.; Skrutskie, Michael F.; Su, K. Y. L.; Bailey, Vanessa P.; Schneider, Glenn; Close, Laird M.; Mannucci, F.; Esposito, Simone; Arcidiacono, Carmelo; Pinna, Enrico; Argomedo, Javier; Agapito, Guido; Apai, Dániel; Bono, G.; Boutsia, Kostantina; Briguglio, Runa; Brusa, Guido; Busoni, Lorenzo; Cresci, G.; Currie, Thayne; Desidera, S.; Eisner, J. A.; Falomo, R.; Fini, Luca; Follette, Katherine B.; Fontana, A.; Garnavich, P.; Gratton, R.; Green, Richard; Guerra, Juan Carlos; Hill, John M.; Hoffmann, W. F.; Jones, T. J.; Krejny, M.; Kulesa, Craig; Males, Jared R.; Masciadri, E.; Mesa, D.; McCarthy, D. W.; Meyer, Michael; Miller, Doris I.; Nelson, Matthew J.; Puglisi, Alfio; Quirós-Pacheco, Fernando; Riccardi, Armando; Sani, E.; Stefanini, P.; Testa, V.; Wilson, John C.; Woodward, C. E.; Xompero, Marco

doi:10.1088/0004-637x/752/1/57

Cited by 47 publications

(70 citation statements)

References 35 publications

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“…If this anisotropy is because of the enhanced forward-scattering efficiency of the dust, as is often claimed (Golimowski et al 2006), then the NW side is the closest to the Earth. These g values are compatible with those derived in the near-infrared for other debris discs, for instance |g| = 0.3 ± 0.03 for HD 181327 (Schneider et al 2006), and Rodigas et al (2012) could also explain the bow of HD 15115 detected at L with an anisotropic scattering parametrized by |g| = 0.5.…”

Section: Resultssupporting

confidence: 89%

Very deep images of the innermost regions of theβPictoris debris disc atL′

Milli

Lagrange

Mawet

et al. 2014

A&A

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Context. Very few debris discs have been imaged in scattered light at wavelengths beyond 3 μm because the thermal emission from both the sky and the telescope is generally too strong with respect to the faint emission of a debris disc. We present here the first analysis of a high angular resolution image of the disc of β Pictoris at 3.8 μm. Aims. Our primary objective is to probe the innermost parts of the β Pictoris debris disc and describe its morphology. We performed extensive forward modelling to correct for the biases induced by angular differential imaging on extended objects and derive the physical parameters of the disc. Methods. This work relies on a new analysis of seven archival data sets of β Pictoris observed with the NaCo instrument at the Very Large Telescope in the L band, including observations made with the Annular Groove Phase Mask vortex coronagraph in 2013. The data analysis consists of angular differential imaging associated with disc forward modelling to correct for the biases induced by that technique. The disc model is subtracted from the data and the reduction performed again in order to minimize the residuals in the final image.Results. The disc is detected above a 5σ level between 0.4 and 3.8 . The two extensions have a similar brightness within error bars. We confirm an asymmetry previously observed at larger distances from the star and at shorter wavelengths: the isophotes are more widely spaced on the north-west side (above the disc apparent midplane) than on the south-east side. This is interpreted as a small inclination of the disc combined with anisotropic scattering. Our best-fit model has an inclination of 86 • with an anisotropic HenyeyGreenstein coefficient of 0.36. This interpretation is supported by a new asymmetry detected in the disc: the disc is significantly bowed towards the north-west within 3 (above the apparent midplane). We also detect a possible new asymmetry within 1 , but at this stage we cannot discern between a real feature and an underlying speckle.

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Section: Resultssupporting

confidence: 89%

Very deep images of the innermost regions of theβPictoris debris disc atL′

Milli

Lagrange

Mawet

et al. 2014

A&A

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“…The final image results from the mean of the individual exposures weighted by their exposure times. The signal-to-noise ratio per resolution element (SNRE) is computed as described in Rodigas et al (2012).…”

Section: Data Reductionmentioning

confidence: 99%

“…The final image results from the mean-combination of all derotated reduced images. The SNRE map was also computed as in Rodigas et al (2012). The noise estimations in both NICMOS and SPHERE data sets are thus directly comparable.…”

Section: Data Reductionmentioning

confidence: 99%

First Scattered-light Images of the Gas-rich Debris Disk around 49 Ceti

Choquet

Milli

Wahhaj

et al. 2017

ApJL

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We present the first scattered-light images of the debris disk around 49 Ceti, a ∼40 Myr A1 main-sequence star at 59 pc, famous for hosting two massive dust belts as well as large quantities of atomic and molecular gas. The outer disk is revealed in reprocessed archival Hubble Space Telescope NICMOS-F110W images, as well as new coronagraphic H-band images from the Very Large Telescope SPHERE instrument. The disk extends from 1 1 (65 au) to 4 6 (250 au) and is seen at an inclination of 73°, which refines previous measurements at lower angular resolution. We also report no companion detection larger than 3M Jup at projected separations beyond 20 au from the star (0 34). Comparison between the F110W and H-band images is consistent with a gray color of 49 Ceti's dust, indicating grains larger than 2 μm. Our photometric measurements indicate a scattering efficiency/infrared excess ratio of 0.2-0.4, relatively low compared to other characterized debris disks. We find that 49 Ceti presents morphological and scattering properties very similar to the gas-rich HD 131835 system. From our constraint on the disk inclination we find that the atomic gas previously detected in absorption must extend to the inner disk, and that the latter must be depleted of CO gas. Building on previous studies, we propose a schematic view of the system describing the dust and gas structure around 49 Ceti and hypothetical scenarios for the gas nature and origin.

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“…HIP 11360 hosts a debris disk that is unique for its large asymmetry, being detected out to 315 AU on the east side and more than 550 AU on the west side (Kalas et al 2007). Rodigas et al (2012) showed that the geometry is wavelength dependent and found indications of a gap in the disk at about 1 arcsec. TYC 8484-1507-1 = HD 16699B This star is a new close visual binary from the NaCo-LP observations (sep. 0.06 arcsec = 3.6 AU, ΔH = 0.23 mag).…”

Section: Appendix B: Notes On Individual Objectsmentioning

confidence: 99%

The VLT/NaCo large program to probe the occurrence of exoplanets and brown dwarfs in wide orbits

Desidera

Covino

Messina

et al. 2015

A&A

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Context. Young, close stars are ideal targets for searching planets using the direct imaging technique. The determination of stellar parameters is crucial for the interpretation of imaging survey results, particularly since the luminosity of substellar objects has a strong dependence on system age. Aims. We have conducted a large program with NaCo at the VLT to search for planets and brown dwarfs in wide orbits around 86 stars. A large fraction of the targets observed with NaCo were poorly investigated in the literature. We performed a study to characterize the fundamental properties (age, distance, and mass) of the stars in our sample. To improve target age determinations, we compiled and analyzed a complete set of age diagnostics. Methods. We measured spectroscopic parameters and age diagnostics using dedicated observations acquired with FEROS and CORALIE spectrographs at La Silla Observatory. We also made extensive use of archival spectroscopic data and the results that are available in the literature. Additionally, we exploited photometric time-series, which are available in ASAS and Super-WASP archives, to derive a rotational period for a large fraction of our program stars. Results. We provided updated characterization of all the targets observed in the VLT NaCo Large program, a survey designed to probe the occurrence of exoplanets and brown dwarfs in wide orbits. The median distance and age of our program stars are 64 pc and 100 Myr, respectively. Nearly all the stars have masses between 0.70 and 1.50 M , with a median value of 1.01 M . The typical metallicity is close to solar with a dispersion that is smaller than that of samples usually observed in radial velocity surveys. Several stars are confirmed or proposed here to be members of close young moving groups. Eight spectroscopic binaries are identified.

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THE GRAY NEEDLE: LARGE GRAINS IN THE HD 15115 DEBRIS DISK FROM LBT/PISCES/KsAND LBTI /LMIRcam/L′ ADAPTIVE OPTICS IMAGING

Cited by 47 publications

References 35 publications

Very deep images of the innermost regions of theβPictoris debris disc atL′

Very deep images of the innermost regions of theβPictoris debris disc atL′

First Scattered-light Images of the Gas-rich Debris Disk around 49 Ceti

The VLT/NaCo large program to probe the occurrence of exoplanets and brown dwarfs in wide orbits

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