Meredith A. MacGregor

Detection of Exocometary CO within the 440 Myr Old Fomalhaut Belt: A Similar CO+CO2 Ice Abundance in Exocomets and Solar System Comets

Author(s): Matra, L; MacGregor, MA; Kalas, P; Wyatt, MC; Kennedy, GM; Wilner, DJ; Duchene, G; Hughes, AM; Pan, M; Shannon, A; Clampin, M; Fitzgerald, MP; Graham, JR; Holland, WS; Panic, O; Su, KYL | Abstract:

A Complete ALMA Map of the Fomalhaut Debris Disk

National Science Foundation Graduate Research Fellowship [DGE1144152]; NRAO Student Observing Support; STFC; European Union through ERC [279973]; NASA [NNX15AC89G, NNX15AD95G/NEXSS, NNX15AK23G, NNX15AM35G]; NSF [AST-1518332, HST-GO-13726, AST-1412647]; NASAs Science Mission Directorate; Royal Society as a Royal Society University Research Fellow; Royal Society Dorothy Hodgkin Fellowship; Center for Exoplanets and Habitable Worlds; Pennsylvania State University; Eberly College of Science; Pennsylvania Space Grant Consortium

An ATCA survey of debris disks at 7 millimeters

We present ATCA continuum observations at a wavelength of 6.8 mm of five debris disks:

ALMA Observations of the Debris Disk of Solar Analogue τ Ceti

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ALMA 1.3 mm Map of the HD 95086 System

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Resolved Millimeter Observations of the HR 8799 Debris Disk

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ALMA and VLA observations of the HD 141569 system

Eridani, HD 107146, HD 181327, and HD 95086. These observations provide the detection at the longest wavelengths obtained to date for all these debris disks. By combining our 6.8 mm data with previous detections at shorter sub-millimeter/millimeter wavelengths we measure the long wavelength spectral index of these sources. We then use previous estimates for the temperature of the emitting dust to derive the spectral index of the dust emissivity. Under the assumption that all the detected flux comes from dust only, we constrain the slope of the solid size distribution, assumed to be a power-law. The values that we infer for the slope of the size distribution range between about 3.36 and 3.50. We compare our findings with the case of the Fomalhaut debris disk and use these results to test the predictions of collisional cascades of planetesimal belts.

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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. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. M.A.M. acknowledges support from a National Science Foundation Graduate Research Fellowship (DGE1144152). S.M.L. gratefully acknowledges support from the NRC Canada Plaskett Fellowship. B.C.M. acknowledges support from a Natural Science and Engineering Research Council (NSERC) Discovery Accelerator Supplement grant. G.M.K. is supported by the Royal Society as a Royal Society University Research Fellow. M.B. acknowledges support from a FONDECYT Postdoctral Fellowship, project no. 3140479 and the Millennium Science Initiative (Chilean Ministry of Economy), through grant RC130007.

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Planets and minor bodies such as asteroids, Kuiper-belt objects and comets are integral components of a planetary system. Interactions among them leave clues about the formation process of a planetary system. The signature of such interactions is most prominent through observations of its debris disk at millimeter wavelengths where emission is dominated by the population of large grains that stay close to their parent bodies. Here we present ALMA 1.3 mm observations of HD 95086, a young early-type star that hosts a directly imaged giant planet b and a massive debris disk with both asteroid- and Kuiper-belt analogs. The location of the Kuiper-belt analog is resolved for the first time. The system can be depicted as a broad (

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