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Identification of Young Stellar Objects in IC1348 and IC 1805 (400-2500 parsec)
Identification of Young Stellar Objects in IC1348 and IC 1805 (400-2500 parsec)
The young population in IC 1348
The young population in IC 1348
Class I: protostars embedded in the parental molecular cloud
Class I: protostars embedded in the parental molecular cloud
Class II: Classical T Tauri stars with optically thick discs
Class II: Classical T Tauri stars with optically thick discs
Class III: mostly T Tauri stars with dispersed discs
Class III: mostly T Tauri stars with dispersed discs
Transition discs: Objects with gaps in the discs as observed in the spectral energy distribution (SED)
Transition discs: Objects with gaps in the discs as observed in the spectral energy distribution (SED)
In this work, I identified the young population in IC1348 by first removing some contaminants that mimic the behaviour of YSOs, such as SFGs, PAH emission, etc. (on the left side).
On the right side, we see the different YSO classes labelled in different colours using WISE bands.
The spatial distribution of YSOs in IC1348
Variability of T Tauri stars in IC1805
One of the distinctive properties of T Tauri stars is photometric variability. It occurs due to different mechanisms such as changes in accretion rate, rotational modulation, and obscuration by the circumstellar environment.
We can use surveys like the Zwicky Transient Facility (ZTF) to study YSOs' light curves.
These are some of the ZTF lightcurves belonging to T Tauri stars in IC1805
Both red and green show different ZTF filters. In both cases, we observe an aperiodic change in the brightness of the star.
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