Speaker
Description
It remains an unanswered question what dictates the amount of dust in the interstellar medium. Asymptotic giant branch stars and supernovae produce dust in their cold atmospheres, but dust gets destroyed during star-formation and supernova shockwaves. The timescales for these effects combined with the observed dust masses in galaxies implies that dust also grows in the interstellar medium.
This implies that amount of dust in a galaxy is directly linked to the star formation history and how efficient dust can accrete metals in the ISM.
We can potentially disentangle the evolution effects by adding information on the chemical abundances of several elements in the gas-phase and locked up in dust grains. Oxygen primarily forms in high-mass stars, whereas nitrogen can form in low and intermediate-mass stars. Oxygen is also commonly suggested to accrete more efficiently onto dust grains, whereas nitrogen remains in the gas-phase.
The talk will showcase spatially resolved radial gradients of the stellar mass, gas mass, and dust mass surface density, and O/H and N/O elemental abundance ratios for local spiral galaxies NGC628 (M74), NGC5457 (M101), NGC598 (M33), and NGC300. I will present the results of chemical and dust evolution models capable of disentangling the different evolution mechanisms within these galaxies consistent with previous claims such as inside-out growth.
| Talk category | NOVA Network 1 |
|---|---|
| Preference for a talk or poster | Talk |
| Talk preference for PhD students | 4th year PhD student (I have already given a talk at the NAC last year) |
