CaltechAUTHORS
Published December 1, 2021 | Version Accepted Version + Published
Journal Article Open

Multiband Imaging of the HD 36546 Debris Disk: A Refined View from SCExAO/CHARIS

Creators

  • 1. ROR icon University of Oklahoma
  • 2. ROR icon University of Hawaii at Hilo
  • 3. ROR icon Ames Research Center
  • 4. ROR icon Eureka Scientific
  • 5. ROR icon Astrobiology Center
  • 6. ROR icon University of Tokyo
  • 7. ROR icon National Astronomical Observatory of Japan
  • 8. ROR icon Institut de Planétologie et d'Astrophysique de Grenoble
  • 9. ROR icon University of California, Santa Barbara
  • 10. ROR icon University of Arizona
  • 11. ROR icon University of San Francisco
  • 12. ROR icon Princeton University
  • 13. ROR icon Goddard Space Flight Center
  • 14. ROR icon University of Notre Dame
  • 15. ROR icon California Institute of Technology
  • 16. ROR icon Observatoire de la Côte d'Azur
  • 17. ROR icon Lagrange Laboratory
  • 18. ROR icon University College London
  • 19. ROR icon Max Planck Institute for Astronomy
  • 20. ROR icon Space Science Institute
  • 21. ROR icon Infrared Processing and Analysis Center
  • 22. ROR icon NASA Exoplanet Science Institute

Abstract

We present the first multiwavelength (near-infrared; 1.1–2.4 μm) imaging of HD 36546's debris disk, using the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) system coupled with the Coronagraphic High Angular Resolution Imaging Spectrograph (CHARIS). As a 3–10 Myr old star, HD 36546 presents a rare opportunity to study a debris disk at very early stages. SCExAO/CHARIS imagery resolves the disk over angular separations of ρ ∼ 0.″25–1.″0 (projected separations of r_(proj) ∼ 25–101 au) and enables the first spectrophotometric analysis of the disk. The disk's brightness appears symmetric between its eastern and western extents, and it exhibits slightly blue near-infrared colors on average (e.g., J−K = −0.4 ± 0.1)—suggesting copious submicron-sized or highly porous grains. Through detailed modeling adopting a Hong scattering phase function (SPF), instead of the more common Henyey–Greenstein function, and using the differential evolution optimization algorithm, we provide an updated schematic of HD 36546's disk. The disk has a shallow radial dust density profile (α_(in) ≈ 1.0 and α_(out) ≈ −1.5), a fiducial radius of r₀ ≈ 82.7 au, an inclination of i ≈ 79.°1, and a position angle of PA ≈ 80.°1. Through spine tracing, we find a spine that is consistent with our modeling, but also with a "swept-back wing" geometry. Finally, we provide constraints on companions, including limiting a companion responsible for a marginal Hipparcos–Gaia acceleration to a projected separation of ≲0.″2 and to a minimum mass of ≲11 M_(Jup).

Additional Information

© 2021. The American Astronomical Society. Received 2021 May 25; revised 2021 September 2; accepted 2021 September 17; published 2021 December 7. We thank our referee, whose comments helped us to improve both the content and clarity of this manuscript. This research is based on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. We are honored and grateful for the opportunity of observing the Universe from Maunakea, which has cultural, historical, and natural significance in Hawaii. We wish to acknowledge the critical importance of the current and recent Subaru telescope operators, daycrew, computer support, and office staff employees. Their expertize, ingenuity, and dedication is indispensable to the continued successful operation of Subaru. The development of SCExAO was supported by the Japan Society for the Promotion of Science (Grant-in-Aid for Research #23340051, #26220704, #23103002, #19H00703 & #19H00695), the Astrobiology Center of the National Institutes of Natural Sciences, Japan, the Mt Cuba Foundation and the director's contingency fund at Subaru Telescope. We acknowledge funding support from the NASA XRP program via grants 80NSSC20K0252 and NNX17AF88G. T.C. was supported by a NASA Senior Postdoctoral Fellowship. M.T. is supported by JSPS KAKENHI grant Nos.18H05442, 15H02063, and 22000005. K.W. acknowledges support from NASA through the NASA Hubble Fellowship grant HST-HF2-51472.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555.

Attached Files

Published - Lawson_2021_AJ_162_293.pdf

Accepted Version - 2109.08984.pdf

Files

2109.08984.pdf

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Additional details

Identifiers

Eprint ID
112452
Resolver ID
CaltechAUTHORS:20211214-16592000

Related works

Describes
https://arxiv.org/abs/2109.08984 (URL)

Funding

Japan Society for the Promotion of Science (JSPS)
23340051
Japan Society for the Promotion of Science (JSPS)
26220704
Japan Society for the Promotion of Science (JSPS)
23103002
Japan Society for the Promotion of Science (JSPS)
19H00703
Japan Society for the Promotion of Science (JSPS)
19H00695
National Institutes of Natural Sciences of Japan
Mt. Cuba Astronomical Foundation
Subaru Telescope
NASA
80NSSC20K0252
NASA
NNX17AF88G
NASA Postdoctoral Program
Japan Society for the Promotion of Science (JSPS)
18H05442
Japan Society for the Promotion of Science (JSPS)
15H02063
Japan Society for the Promotion of Science (JSPS)
22000005
NASA Hubble Fellowship
HST-HF2-51472.001-A
NASA
NAS5-26555

Dates

Created
2021-12-15
Created from EPrint's datestamp field
Updated
2021-12-15
Created from EPrint's last_modified field

Caltech Custom Metadata

Caltech groups
Infrared Processing and Analysis Center (IPAC)