A spectacular jet from the bright 244–440 Orion proplyd: The MUSE NFM view^★

¹ Maynooth University Department of Experimental Physics, National University of Ireland Maynooth, Maynooth Co. Kildare, Ireland
e-mail: andrew.miller@mu.ie
² European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748, Garching bei München, Germany
³ Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218, USA
⁴ Space Telescope Science Institute, 3700 San Martin Dr, Baltimore, MD 21218, USA
⁵ Centre for Extragalactic Astronomy, Department of Physics, Durham University, South Road, Durham DH1 3LE, UK
⁶ Institute for Computational Cosmology, Department of Physics, University of Durham, South Road, Durham DH1 3LE, UK
⁷ Dipartimento di Fisica, Universitá degli Studi di Milano, via Celoria 16, 20133 Milano, Italy
⁸ Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany
⁹ Instituto de Astrofísica e Ciências do Espaco, Universidade de Lisboa, OAL, Tapada da Ajuda, 1349-018 Lisboa, Portugal

Received: 10 November 2022
Accepted: 25 February 2023

Abstract

In this work we present the highest spatial and spectral resolution integral field observations to date of the bipolar jet from the Orion proplyd 244–440 using Multi-Unit Spectroscopic Explorer (MUSE) narrow-field mode (NFM) observations on the Very Large Telescope (VLT). We observed a previously unreported chain of six distinct knots in a roughly S-shaped pattern, and by comparing them with Hubble Space Telescope (HST) images we estimated proper motions in the redshifted knots of 9.5 mas yr⁻¹ with an inclination angle of 73°, though these quantities could not be measured for the blueshifted lobe. Analysis of the [Fe II] and [Ni II] lines suggests jet densities on the order of ~10⁵ cm⁻³. We propose that the observed S-shaped morphology originates from a jet launched by a smaller source with M_★ < 0.2 M_⊙ in orbital motion around a larger companion of M_★ ≃ 0.5 M_⊙ at a separation of 30–40 au. The measured luminosities of the knots using the [O I]λ6300 Å and [S II]λ6731 Å lines were used to estimate a lower limit to the mass-loss rate in the jet of 1.3 × 10⁻¹¹ M_⊙ yr⁻¹ and an upper limit of 10⁻⁹ M_⊙ yr⁻¹, which is typical for low-mass driving sources. While the brightness asymmetry between the redshifted and blueshifted lobes is consistent with external irradiation, further analysis of the [Ni II] and [Fe II] lines suggests that photoionization of the jet is not likely to be a dominant factor, and that the emission is dominated by collisional excitation. The dynamical age of the jet compared to the anticipated survival time of the proplyd demonstrates that photoevaporation of the proplyd occurred prior to jet launching, and that this is still an active source. These two points suggest that the envelope of the proplyd may shield the jet from the majority of external radiation, and that photoionization of the proplyd does not appear to impact the ability of a star to launch a jet.