A bimodal dust grain distribution in the IC 434 H ii region

Abstract

Recent studies of dust in the interstellar medium have challenged the capabilities and validity of current dust models, indicating that the properties of dust evolve as it transits between different phases of the interstellar medium. We conduct a multi-wavelength study of the dust emission from the ionized gas of the IC 434 emission nebula, and combine this with modeling, from large scales that provide insight into the history of the IC 434/L1630 region, to small scales that allow us to infer quantitative properties of the dust content inside the H II region. The dust enters the H II region through momentum transfer with a champagne flow of ionized gas, set up by a chance encounter between the L1630 molecular cloud and the star cluster of $\sigma$ Ori. We observe two clearly separated dust populations inside the ionized gas, that show different observational properties, as well as contrasting optical properties. Population A is colder ($\sim$ 25 K) than predicted by widely-used dust models, its temperature is insensitive to an increase of the impinging radiation field, is momentum-coupled to the gas, and efficiently absorbs radiation pressure to form a dust wave at 1.0 pc ahead of $\sigma$ Ori AB. Population B is characterized by a constant [20/30] flux ratio throughout the HII region, heats up to $\sim$ 75 K close to the star, and is less efficient in absorbing radiation pressure, forming a dust wave at 0.1 pc from the star. We conclude that the dust inside IC 434 is bimodal. The characteristics of population A are remarkable and can not be explained by current dust models. Population B are grains that match the classical description of spherical, compact dust. Our results confirm recent work that stress the importance of variations in the dust properties between different regions of the interstellar medium.