Comprehensive Analysis of HD 105, A Young Solar System Analog

Creators: Marshall, J. P.; Milli, J.; Choquet, É.; del Burgo, C.; Kennedy, G. M.; Matrà, L.; Ertel, S.; Boccaletti, A.

Abstract

HD 105 is a nearby, pre-main-sequence G0 star hosting a moderately bright debris disk (L_(dust)/L ~ 2.6 × 10^(−4)). The star and its surroundings might therefore be considered an analog of the young solar system. We refine the stellar parameters based on an improved Gaia parallax distance and identify it as a pre-main-sequence star with an age of 50 ± 16 Myr. The circumstellar disk was marginally resolved by Herschel/PACS imaging at far-infrared wavelengths. Here, we present an archival ALMA observation at 1.3 mm, revealing the extent and orientation of the disk. We also present Hubble Space Telescope (HST)/NICMOS and VLT/SPHERE near-infrared images, where we recover the disk in scattered light at the ≥5σ level. This was achieved by employing a novel annular averaging technique and is the first time this has been achieved for a disk in scattered light. Simultaneous modeling of the available photometry, disk architecture, and detection in scattered light allow better determination of the disk's architecture, and dust grain minimum size, composition, and albedo. We measure the dust albedo to lie between 0.19 and 0.06, the lower value being consistent with Edgeworth–Kuiper Belt objects.

Additional Information

© 2018 The American Astronomical Society. Received 2018 August 22; revised 2018 October 12; accepted 2018 October 25; published 2018 December 6. We thank the anonymous referee for their constructive criticism that improved the manuscript. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2012.1.00437.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan) and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. This research has made use of NASA's Astrophysics Data System. This paper has made use of the Python packages astropy (Astropy Collaboration et al. 2013, 2018), SciPy (Jones et al. 2001), matplotlib (Hunter 2007), and Hyperion (Robitaille 2011). J.P.M. acknowledges this research has been supported by the Ministry of Science and Technology of Taiwan under grants MOST107-2119-M-001-031-MY3 and MOST107-2119-M-001-031-MY3. E.C. acknowledges support from NASA through Hubble Fellowship grant HF2-51355 awarded by STScI, which is operated by AURA, Inc., for NASA under contract NAS5-26555, for research carried out at the Jet Propulsion Laboratory, California Institute of Technology. This work is based on data reprocessed as part of the ALICE program, which was supported by NASA through grants HST-AR-12652 (PI: R. Soummer), HST-GO-11136 (PI: D. Golimowski), HST-GO-13855 (PI: E. Choquet), and HST-GO-13331 (PI: L. Pueyo), and STScI Director's Discretionary Research funds. C.d.B. acknowledges that this work has been supported by Mexican CONACyT research grant CB-2012-183007. G.M.K. is supported by the Royal Society as a Royal Society University Research Fellow. L.M. acknowledges support from the Smithsonian Institution as a Submillimeter Array (SMA) Fellow.

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