Abstract
We present new, near-infrared (1.1-2.4 μm) high-contrast imaging of the bright debris disk surrounding HIP 79977 with the Subaru Coronagraphic Extreme Adaptive Optics system (SCExAO) coupled with the CHARIS integral field spectrograph. SCExAO/CHARIS resolves the disk down to smaller angular separations of (0 11; r∼14 au) and at a higher significance than previously achieved at the same wavelengths. The disk exhibits a marginally significant east-west brightness asymmetry in H band that requires confirmation. Geometrical modeling suggests a nearly edge-on disk viewed at a position angle of ∼114°6 east of north. The disk is best-fit by scattered-light models assuming strongly forward-scattering grains (g∼0.5-0.65) confined to a torus with a peak density at r0∼53-75 au. We find that a shallow outer density power law of αout=-1 to -3 and flare index of β=1 are preferred. Other disk parameters (e.g., inner density power law and vertical scale height) are more poorly constrained. The disk has a slightly blue intrinsic color and its profile is broadly consistent with predictions from birth ring models applied to other debris disks. While HIP 79977's disk appears to be more strongly forwardscattering than most resolved disks surrounding 5-30 Myr old stars, this difference may be due to observational biases favoring forward-scattering models for inclined disks versus lower inclination, ostensibly neutral-scattering disks like HR 4796A's. Deeper, higher signal-to-noise SCExAO/CHARIS data can better constrain the disk's dust composition.
| Original language | English (US) |
|---|---|
| Article number | aaeb24 |
| Journal | Astronomical Journal |
| Volume | 156 |
| Issue number | 6 |
| DOIs | |
| State | Published - 2018 |
All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science
Keywords
- Circumstellar matter
- Planetary systems
- Stars: Individual (HIP 79977)
- Techniques: High angular resolution
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SCExAO/CHARIS near-IR high-contrast imaging and integral field spectroscopy of the HIP 79977 debris disk. / Goebel, Sean; Currie, Thayne; Guyon, Olivier et al.
In: Astronomical Journal, Vol. 156, No. 6, aaeb24, 2018.Research output: Contribution to journal › Article › peer-review
TY - JOUR
T1 - SCExAO/CHARIS near-IR high-contrast imaging and integral field spectroscopy of the HIP 79977 debris disk
AU - Goebel, Sean
AU - Currie, Thayne
AU - Guyon, Olivier
AU - Brandt, Timothy D.
AU - Groff, Tyler D.
AU - Jovanovic, Nemanja
AU - Kasdin, N. Jeremy
AU - Lozi, Julien
AU - Hodapp, Klaus
AU - Martinache, Frantz
AU - Grady, Carol
AU - Hayashi, Masa
AU - Kwon, Jungmi
AU - McElwain, Michael W.
AU - Yang, Yi
AU - Tamura, Motohide
N1 - Funding Information: Sean Goebel Thayne Currie Olivier Guyon Timothy D. Brandt Tyler D. Groff Nemanja Jovanovic N. Jeremy Kasdin Julien Lozi Klaus Hodapp Frantz Martinache Carol Grady Masa Hayashi Jungmi Kwon Michael W. McElwain Yi Yang Motohide Tamura Sean Goebel Thayne Currie Olivier Guyon Timothy D. Brandt Tyler D. Groff Nemanja Jovanovic N. Jeremy Kasdin Julien Lozi Klaus Hodapp Frantz Martinache Carol Grady Masa Hayashi Jungmi Kwon Michael W. McElwain Yi Yang Motohide Tamura Institute for Astronomy, University of Hawaii, 640 North A‘ohōkū Place, Hilo, HI 96720, USA Subaru Telescope, National Astronomical Observatory of Japan, 650 North A‘ohōkū Place, Hilo, HI 96720, USA NASA-Ames Research Center, Moffett Field, CA, USA Eureka Scientific, 2452 Delmer Street Suite 100, Oakland, CA, USA Steward Observatory, University of Arizona, Tucson, AZ 85721, USA College of Optical Sciences, University of Arizona, Tucson, AZ 85721, USA Astrobiology Center of NINS, 2-21-1, Osawa, Mitaka, Tokyo, 181-8588, Japan Department of Physics, University of California, Santa Barbara, Santa Barbara, California, USA NASA-Goddard Space Flight Center, Greenbelt, MD, USA Caltech Optical Observatory, Department of Astronomy, California Institute of Technology, 1200 E. California Blvd., Pasadena, CA 91125, USA Department of Mechanical Engineering, Princeton University, Princeton, NJ, USA Universit� C�te d’Azur, Observatoire de la C�te d’Azur, CNRS, Laboratoire Lagrange, France National Astronomical Observatory of Japan, Osawa 2-21-1, Mitaka, Tokyo 181-8588, Japan Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa 252-5210, Japan Department of Astronomy, The Graduate University for Advanced Studies (SOKENDAI), National Astronomical Observatory of Japan, Japan Sean Goebel, Thayne Currie, Olivier Guyon, Timothy D. Brandt, Tyler D. Groff, Nemanja Jovanovic, N. Jeremy Kasdin, Julien Lozi, Klaus Hodapp, Frantz Martinache, Carol Grady, Masa Hayashi, Jungmi Kwon, Michael W. McElwain, Yi Yang and Motohide Tamura 2018-12-01 2018-11-28 17:49:52 cgi/release: Article released bin/incoming: New from .zip yes We present new, near-infrared (1.1–2.4 μ m) high-contrast imaging of the bright debris disk surrounding HIP 79977 with the Subaru Coronagraphic Extreme Adaptive Optics system (SCExAO) coupled with the CHARIS integral field spectrograph. SCExAO/CHARIS resolves the disk down to smaller angular separations of (0.″11; r �∼�14 au) and at a higher significance than previously achieved at the same wavelengths. The disk exhibits a marginally significant east–west brightness asymmetry in H band that requires confirmation. Geometrical modeling suggests a nearly edge-on disk viewed at a position angle of ∼114.�6 east of north. The disk is best-fit by scattered-light models assuming strongly forward-scattering grains ( g �∼�0.5–0.65) confined to a torus with a peak density at r 0 �∼�53–75 au. We find that a shallow outer density power law of α out �=�−1 to −3 and flare index of β �=�1 are preferred. Other disk parameters (e.g., inner density power law and vertical scale height) are more poorly constrained. The disk has a slightly blue intrinsic color and its profile is broadly consistent with predictions from birth ring models applied to other debris disks. While HIP 79977's disk appears to be more strongly forward-scattering than most resolved disks surrounding 5–30 Myr old stars, this difference may be due to observational biases favoring forward-scattering models for inclined disks versus lower inclination, ostensibly neutral-scattering disks like HR 4796A’s. Deeper, higher signal-to-noise SCExAO/CHARIS data can better constrain the disk’s dust composition. � 2018. The American Astronomical Society. All rights reserved. Augereau J. C., Lagrange A. M., Mouillet D., Papaloizou J. C. B. and Grorod P. A. 1999 A&A 348 557 Augereau J. C., Lagrange A. 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PY - 2018
Y1 - 2018
N2 - We present new, near-infrared (1.1-2.4 μm) high-contrast imaging of the bright debris disk surrounding HIP 79977 with the Subaru Coronagraphic Extreme Adaptive Optics system (SCExAO) coupled with the CHARIS integral field spectrograph. SCExAO/CHARIS resolves the disk down to smaller angular separations of (0 11; r∼14 au) and at a higher significance than previously achieved at the same wavelengths. The disk exhibits a marginally significant east-west brightness asymmetry in H band that requires confirmation. Geometrical modeling suggests a nearly edge-on disk viewed at a position angle of ∼114°6 east of north. The disk is best-fit by scattered-light models assuming strongly forward-scattering grains (g∼0.5-0.65) confined to a torus with a peak density at r0∼53-75 au. We find that a shallow outer density power law of αout=-1 to -3 and flare index of β=1 are preferred. Other disk parameters (e.g., inner density power law and vertical scale height) are more poorly constrained. The disk has a slightly blue intrinsic color and its profile is broadly consistent with predictions from birth ring models applied to other debris disks. While HIP 79977's disk appears to be more strongly forwardscattering than most resolved disks surrounding 5-30 Myr old stars, this difference may be due to observational biases favoring forward-scattering models for inclined disks versus lower inclination, ostensibly neutral-scattering disks like HR 4796A's. Deeper, higher signal-to-noise SCExAO/CHARIS data can better constrain the disk's dust composition.
AB - We present new, near-infrared (1.1-2.4 μm) high-contrast imaging of the bright debris disk surrounding HIP 79977 with the Subaru Coronagraphic Extreme Adaptive Optics system (SCExAO) coupled with the CHARIS integral field spectrograph. SCExAO/CHARIS resolves the disk down to smaller angular separations of (0 11; r∼14 au) and at a higher significance than previously achieved at the same wavelengths. The disk exhibits a marginally significant east-west brightness asymmetry in H band that requires confirmation. Geometrical modeling suggests a nearly edge-on disk viewed at a position angle of ∼114°6 east of north. The disk is best-fit by scattered-light models assuming strongly forward-scattering grains (g∼0.5-0.65) confined to a torus with a peak density at r0∼53-75 au. We find that a shallow outer density power law of αout=-1 to -3 and flare index of β=1 are preferred. Other disk parameters (e.g., inner density power law and vertical scale height) are more poorly constrained. The disk has a slightly blue intrinsic color and its profile is broadly consistent with predictions from birth ring models applied to other debris disks. While HIP 79977's disk appears to be more strongly forwardscattering than most resolved disks surrounding 5-30 Myr old stars, this difference may be due to observational biases favoring forward-scattering models for inclined disks versus lower inclination, ostensibly neutral-scattering disks like HR 4796A's. Deeper, higher signal-to-noise SCExAO/CHARIS data can better constrain the disk's dust composition.
KW - Circumstellar matter
KW - Planetary systems
KW - Stars: Individual (HIP 79977)
KW - Techniques: High angular resolution
UR - http://www.scopus.com/inward/record.url?scp=85075081144&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85075081144&partnerID=8YFLogxK
U2 - 10.3847/1538-3881/aaeb24
DO - 10.3847/1538-3881/aaeb24
M3 - Article
AN - SCOPUS:85075081144
SN - 0004-6256
VL - 156
JO - Astronomical Journal
JF - Astronomical Journal
IS - 6
M1 - aaeb24
ER -