SOFIA/upGREAT far-infrared spectroscopy of bright rimmed pillars in IC 1848

TL;DR

This study uses SOFIA/upGREAT far-infrared spectroscopy to analyze the physical conditions and morphology of bright-rimmed pillars in IC 1848, revealing velocity shifts and discrepancies with PDR models.

Contribution

First detailed spectroscopic mapping of IC 1848's pillars with [C II] and [O I] lines, highlighting limitations of existing PDR models and proposing [O I] line ratios as diagnostic tools.

Findings

Velocity shift at G1 filament head suggests radiation pressure effects.

[C II] traces about 17% of total H2 column density.

Observed [O I] 145 μm line is stronger than model predictions.

Abstract

Using the upGREAT instrument on SOFIA, we have imaged the [C II] 158 {\mu}m fine structure line emission in bright-rimmed pillars located at the southern edge of the IC1848 H II region, and carried out pointed observations of the [O I] 63 and 145 {\mu}m fine structure lines toward selected positions. The observations are used to characterize the morphology, velocity field, and the physical conditions in the G1 - G3 filaments. The velocity-resolved [C II] spectra show evidence of a velocity shift at the head of the brightest G1 filament, possibly caused by radiation pressure from the impinging UV photons or the rocket effect of the evaporating gas. Archival Herschel PACS and SPIRE data imply H2 column densities in the range 10^{21} - 10^{22} cm^{-2}, corresponding to maximum visual extinction AV = 10 mag, and average H2 volume density of about 4500 cm^{-3} in the filaments. The [C II] emission traces ~ 17% of the total H2 column density, as derived from dust SED fits. PDR models are unable to explain the observed line intensities of the two [O I] fine structure lines in IC1848, with the observed [O I] 145 {\mu}m line being too strong compared to the model predictions. The [O I] lines in IC1848 are overall weak and the signal-to-noise ratio is limited. However, our observations suggest that the [O I] 63/145 {\mu}m intensity ratio is a sensitive probe of the physical conditions in photon dominated regions such as IC1848. These lines are thus excellent targets for future high-altitude balloon instruments, less affected by telluric absorption.