Mid-infrared interferometry of the massive young stellar object NGC3603 - IRS 9A

TL;DR

This study uses infrared interferometry to analyze the structure of the massive young stellar object NGC3603 IRS 9A on scales down to 200AU, revealing a complex dust distribution likely involving a flattened structure rather than a spherical envelope.

Contribution

First interferometric analysis of NGC3603 IRS 9A revealing detailed dust structure and constraints on models, favoring disk-like over spherical geometries.

Findings

Resolved the object with T-ReCS, finding an elliptical Gaussian size of 2300 AU by 2000 AU.

Detected a warm unresolved component possibly from the inner dust regions.

Data favor a model with a warm ring and a large envelope over spherical models.

Abstract

We present observations and models for one of these MYSO candidates, NGC3603 IRS 9A. Our goal is to investigate with infrared interferometry the structure of IRS 9A on scales as small as 200AU, exploiting the fact that a cluster of O and B stars has blown away much of the obscuring foreground dust and gas. Observations in the N-band were carried out with the MIDI beam combiner attached to the VLTI. Additional interferometric observations which probe the structure of IRS 9A on larger scales were performed with an aperture mask installed in the T-ReCS instrument of Gemini South. The spectral energy distribution (SED) is constrained by the MIDI N-band spectrum and by data from the Spitzer Space Telescope. Our efforts to model the structure and SED of IRS 9A range from simple geometrical models of the brightness distribution to one- and two-dimensional radiative transfer computations. The target is resolved by T-ReCS, with an equivalent (elliptical) Gaussian width of 330mas by 280mas (2300 AU by 2000 AU). Despite this fact, a warm compact unresolved component was detected by MIDI which is possibly associated with the inner regions of a flattened dust distribution. Based on our interferometric data, no sign of multiplicity was found on scales between about 200AU and 700AU projected separation. A geometric model consisting of a warm (1000 K) ring (400 AU diameter) and a cool (140 K) large envelope provides a good fit to the data. No single model fitting all visibility and photometric data could be found, with disk models performing better than spherical models. While the data are clearly inconsistent with a spherical dust distribution they are insufficient to prove the existence of a disk but rather hint at a more complex dust distribution.