Photoionized Herbig-Haro objects in the Orion Nebula through deep high-spectral resolution spectroscopy I: HH529II and III

TL;DR

This study analyzes the physical, chemical, and kinematic properties of bow shocks HH529 II and III in the Orion Nebula using high-resolution spectroscopy and imaging, revealing dust destruction and chemical enrichment in these Herbig-Haro objects.

Contribution

It provides detailed spectroscopic analysis of HH529 II and III, including diagnostics of physical conditions, chemical abundances, and kinematics, with insights into dust destruction and material enrichment.

Findings

Higher gas-phase Fe in HH 529 II and III suggests dust grain destruction.

Chemical overabundances of several elements indicate H-deficient material inclusion.

Proper motions and flow angle of HH 529 are precisely measured.

Abstract

We present the analysis of physical conditions, chemical composition and kinematic properties of two bow shocks -HH529 II and HH529 III- of the fully photoionized Herbig-Haro object HH 529 in the Orion Nebula. The data were obtained with the Ultraviolet and Visual Echelle Spectrograph at the 8.2m Very Large Telescope and 20 years of Hubble Space Telescope imaging. We separate the emission of the high-velocity components of HH529 II and III from the nebular one, determining $n_{\rm e}$ and $T_{\rm e}$ in all components through multiple diagnostics, including some based on recombination lines (RLs). We derive ionic abundances of several ions, based on collisionally excited lines (CELs) and RLs. We find a good agreement between the predictions of the temperature fluctuation paradigm ($t^2$) and the abundance discrepancy factor (ADF) in the main emission of the Orion Nebula. However, $t^2$ can not account for the higher ADF found in HH 529 II and III. We estimate a 6% of Fe in the gas-phase of the Orion Nebula, while this value increases to 14% in HH 529 II and between 10% and 25% in HH 529 III. We find that such increase is probably due to the destruction of dust grains in the bow shocks. We find an overabundance of C, O, Ne, S, Cl and Ar of about 0.1 dex in HH 529 II-III that might be related to the inclusion of H-deficient material from the source of the HH 529 flow. We determine the proper motions of HH 529 finding multiple discrete features. We estimate a flow angle with respect to the sky plane of $58\pm 4^{\circ}$ for HH 529.