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Far-infrared to millimeter data of protoplanetary disks: dust growth in the Taurus, Ophiuchus, and Chamaeleon I star-forming regions

hal.structure.identifierEuropean Space Astronomy Centre [ESAC]
dc.contributor.authorRIBAS, Álvaro
dc.contributor.authorESPAILLAT, Catherine C.
dc.contributor.authorMACÍAS, Enrique
hal.structure.identifierM2A 2017
dc.contributor.authorBOUY, H.
dc.contributor.authorANDREWS, Sean
dc.contributor.authorCALVET, Nuria
dc.contributor.authorNAYLOR, David A.
hal.structure.identifierEuropean Space Astronomy Centre [ESAC]
dc.contributor.authorRIVIERE-MARICHALAR, Pablo
dc.contributor.authorVAN DER WIEL, Matthijs H. D.
dc.contributor.authorWILNER, David
dc.date.issued2017
dc.identifier.issn0004-637X
dc.description.abstractEnFar-infrared and (sub)millimeter fluxes can be used to study dust in protoplanetary disks, the building blocks of planets. Here, we combine observations from the Herschel Space Observatory with ancillary data of 284 protoplanetary disks in the Taurus, Chamaeleon I, and Ophiuchus star-forming regions, covering from the optical to mm/cm wavelengths. We analyze their spectral indices as a function of wavelength and determine their (sub)millimeter slopes when possible. Most disks display observational evidence of grain growth, in agreement with previous studies. No correlation is found between other tracers of disk evolution and the millimeter spectral indices. A simple disk model is used to fit these sources, and we derive posterior distributions for the optical depth at 1.3 mm and 10 au, the disk temperature at this same radius, and the dust opacity spectral index. We find the fluxes at 70 microns to correlate strongly with disk temperatures at 10 au, as derived from these simple models. We find tentative evidence for spectral indices in Chamaeleon I being steeper than those of disks in Taurus/Ophiuchus, although more millimeter observations are needed to confirm this trend and identify its possible origin. Additionally, we determine the median spectral energy distribution of each region and find them to be similar across the entire wavelength range studied, possibly due to the large scatter in disk properties and morphologies.
dc.language.isoen
dc.publisherAmerican Astronomical Society
dc.subject.enAstrophysics - Solar and Stellar Astrophysics
dc.subject.enAstrophysics - Earth and Planetary Astrophysics
dc.subject.enAstrophysics - Astrophysics of Galaxies
dc.title.enFar-infrared to millimeter data of protoplanetary disks: dust growth in the Taurus, Ophiuchus, and Chamaeleon I star-forming regions
dc.typeArticle de revue
dc.identifier.doi10.3847/1538-4357/aa8e99
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Instrumentation et méthodes pour l'astrophysique [astro-ph.IM]
dc.identifier.arxiv1710.08426
bordeaux.journalThe Astrophysical Journal
bordeaux.volume849
bordeaux.issue1
bordeaux.peerReviewedoui
hal.identifierhal-01623481
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01623481v1
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