A HST Study of the Substellar Population of NGC 2024

TL;DR

This study uses HST/WFC3-IR imaging to analyze the low-mass and sub-stellar objects in NGC 2024, deriving a luminosity function consistent with a young cluster and exploring extinction effects.

Contribution

First HST/WFC3-IR survey of NGC 2024's substellar population using water absorption features for classification.

Findings

Detected 812 point sources, 550 with high S/N in all filters.

Derived extinction values up to A_V≈40, noting increased A_V with reddening.

Luminosity function aligns with a Salpeter-like IMF for a 1 Myr age.

Abstract

We performed a HST/WFC3-IR imaging survey of the young stellar cluster NGC 2024 in three filters probing the 1.4~$\mu$m H$_2$O absorption feature, characteristic of the population of low mass and sub-stellar mass objects down to a few Jupyter masses. We detect 812 point sources, 550 of them in all 3 filters with signal to noise greater than 5. Using a distance-independent two-color diagram we determine extinction values as high as $A_V\simeq 40$. We also find that the change of effective wavelengths in our filters results in higher $A_V$ values as the reddening increases. Reconstructing a dereddened color-magnitude diagram we derive a luminosity histogram for both the full sample of candidate cluster members and for an extinction-limited sub-sample containing the 50% of sources with $A_V\lesssim 15$. Assuming a standard extinction law like Cardelli et al. (1989) with a nominal $R_V$=3.1 we produce a luminosity function in good agreement with the one resulting from a Salpeter-like Initial Mass Function for a 1~Myr isochrone. There is some evidence of an excess of luminous stars in the most embedded region. We posit that the correlation may be due to those sources being younger, and therefore overluminous than the more evolved and less extinct cluster's stars. We compare our classification scheme based on the depth of the 1.4$\mu$m photometric feature with the results from the spectroscopic survey of Levine et al. (2006), and we report a few peculiar sources and morphological features typical of the rich phenomenology commonly encountered in young star-forming regions.