Research

The outer disk chemistry of asymmetric disks as seen with ALMA

Using ALMA observations, the chemical composition of the gas in the outer regions of planet-forming disks can be inferred. My work focuses on the role of dust substructures in setting the observable chemistry. Asymmetric dust traps are of particular interest, as we can directly relate the observed gas emission with the asymmetries seen in the dust.

Related works:

  • The temperature structure of the IRS 48 disk
    IRS 48 is the most asymmetric disk known to date, with the dust emission originating primarily from the southern side of the disk. Previous studies have shown that the emission of most of the observed molecular species is coincidental with the dust thermal emission. A combination of turbulent vertical mixing and sublimation of the icy mantles coating the dust grains is currently the most plausible explanation for the coincidental emission morphologies.

    Using the plethora of lines presented in Booth et al. (2024), I study the temperature structure of the IRS 48 disk as probed by SO₂ and CH₃OH. The temperature structure is investigate through a pixel-by-pixel rotational diagram analysis.

    More information to follow soon!

  • Investigating the asymmetric molecular emission of the disk around HD 142527
    Following my previous work on the asymmetric chemistry in the asymmetric disk HD 142527 (Temmink et al. 2023), where the found gas asymmetries can be explained by continuum oversubtraction effects and potentially by the misalignment of the inner disk.

    Using new ALMA Cycle 10 observations (2023.1.00628.S, PI: M. Temmink) covering molecular transitions in Band 3 and 4, where we expect the dust emission to be less optically thick, I aim to take a deeper look into the main cause of the previously observed gas asymmetries.

    More information to follow soon!

The chemistry of terrestrial planet-forming zones with JWST-MIRI/MRS

As part of the MIRI mid-INfrared Disk Survey (MINDS) JWST Cycle 1 GTO program, I study the chemical composition of the inner regions (<10 au) of planet-forming disks. One of the most interesting molecular reservoir we can probe with JWST-MIRI is that of H₂O, a key ingredient for life as we know it. A question of interest, one that my focus, is the role of radial drift of icy pebbles and the subsequent sublimation of H2O-ice in enhancing the observable abundance.

Related works:

  • The JWST-MIRI/MRS spectrum of the compact disk DR Tau
    My first project as part of MINDS focuses on the compact disk DR Tau, a disk with a maximum dust radius of <60 au. As compact disks are thought to have very efficient drift, we may expect their H₂O abundances to be enhanced (Banzatti et al. 2020). Previous observations with the Spitzer Space Telescope have shown that DR Tau is an incredibly line-rich disk. This project aims to fully characterise the molecular emission seen in the JWST-MIRI/MRS spectrum of DR Tau.

    This project has resulted in two separate papers: the first one focuses mainly on the CO emission and how complementary, high-resolution observations can aid in the understanding of the CO emission as seen with JWST-MIRI/MRS (Temmink et al. 2024a). A second paper (Temmink et al. 2024b) contains a thorough analysis of the tremendous amount of H₂O transitions visible throughout the entire spectrum. In particular, we use a multi-component analysis to describe the full rotational H₂O spectrum (>10 μm). We found that at least 3 temperature (T₁~800 K, T₂~470 K and T₃~180 K) components are needed to fit the rotational lines.

    More information to follow soon!

Outer disk substructures as seen with ALMA

The high sensitivity and angular resolution achievable with ALMA allows for the characterisation of dust substructures in the thermal continuum emission. Analysis of the visibilities can lead to the characterisation of substructures at smaller scales than achievable with the resolving ALMA beam.

Related works:

  • Hunting for substructures in 10 structured disks observed with JWST-MIRI/MRS
    In an upcoming paper, I analysed the ALMA continuum images and visibilities of 10 structured disks, with the aim to homogeneously characterise the substructures in an homogeneous sample. The characterised substructures have been used to investigate potential relations between the observed molecular emission in the inner disk (investigated with JWST-MIRI/MRS spectra) and the substructures observed in the outer disk.

    More information to follow soon!

  • High-resolution observations of 3 compact disks observed with JWST-MIRI/MRS
    With upcoming Cycle 11 ALMA high-resolution observations (2024.1.00448.S), I will characterise the substructures in three disks that are compact in their dust continuum emission (<60 au). The JWST-MIRI/MRS spectra of these three disks show varying strengths of the H2O emission features. Using these high-resolution observations, I aim to investigate the impact of potential substructures on the observable molecular emission in the inner disk.

    More information to follow!