Emission-line Data Cubes of the HH 32 Stellar Jet

Hartigan, Patrick; Hillenbrand, Lynne A.; Matuszewski, Matuesz; Borges, Arlindo Chan; Neill, James D.; Martin, D. Christopher; Morrissey, Patrick; Moore, Anna

doi:10.3847/1538-3881/abadfa

Cited by 3 publications

(1 citation statement)

References 38 publications

(62 reference statements)

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“…In our series of papers about the chemical content of HH objects, we find that gas-phase Fe/H and Ni/H abundances seem to be correlated with the propagation velocity (being HH 529 the slowest and HH 514 the fastest), which is consistent with studies of HH objects propagating in neutral environments (See Fig. 14 from Hartigan et al 2020). However, it is still not clear if this relation is simply linear or shows a more complex behaviour or even if the dust destruction efficiency reaches a maximum at a given velocity.…”

Section: Discussionsupporting

confidence: 84%

Photoionized Herbig-Haro objects in the Orion Nebula through deep high-spectral resolution spectroscopy III: HH514

Méndez-Delgado,

Esteban,

García-Rojas

et al. 2022

Preprint

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We analyze the physical conditions and chemical composition of the photoionized Herbig-Haro object HH 514, which emerges from the proplyd 170-337 in the core of the Orion Nebula. We use high-spectral resolution spectroscopy from UVES at the Very Large Telescope and IFU-spectra from MEGARA at the Gran Telescopio de Canarias. We observe two components of HH 514, the jet base and a knot, with 𝑛 e = (2.3 ± 0.1) × 10 5 cm −3 and 𝑛 e = (7 ± 1) × 10 4 cm −3 , respectively, both with 𝑇 e ≈ 9000 K. We show that the chemical composition of HH 514 is consistent with that of the Orion Nebula, except for Fe, Ni and S, which show higher abundances. The enhanced abundances of Fe and Ni observed in HH objects compared with the general interstellar medium is usually interpreted as destruction of dust grains. The observed sulphur overabundance (more than two times solar) is challenging to explain since the proplyd photoevaporation flow from the same disk shows normal sulphur abundance. If the aforementioned S-overabundance is due to dust destruction, the formation of sulfides and/or other S-bearing dust reservoirs may be linked to planet formation processes in protoplanetary disks, which filter large sulfide dust grains during the accretion of matter from the disk to the central star. We also show that published kinematics of molecular emission close to the central star are not consistent with either a disk perpendicular to the optical jet, nor with an outflow that is aligned with it.

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Section: Discussionsupporting

confidence: 84%

Photoionized Herbig-Haro objects in the Orion Nebula through deep high-spectral resolution spectroscopy III: HH514

Méndez-Delgado,

Esteban,

García-Rojas

et al. 2022

Preprint

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Photoionized Herbig–Haro objects in the Orion Nebula through deep high-spectral resolution spectroscopy – I. HH 529 II and III

Méndez-Delgado

Esteban

García‐Rojas

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present the analysis of physical conditions, chemical composition, and kinematic properties of two bow shocks – HH 529 II and HH 529 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 yr of Hubble Space Telescope imaging. We separate the emission of the high-velocity components of HH 529 II and III from the nebular one, determining ne and Te 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 and RLs. We find a good agreement between the predictions of the temperature fluctuation paradigm (t2) and the abundance discrepancy factor (ADF) in the main emission of the Orion Nebula. However, t2 cannot account for the higher ADF found in HH 529 II and III. We estimate 6 per cent of Fe in the gas phase of the Orion Nebula, while this value increases to 14 per cent in HH 529 II and between 10 and 25 per cent 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 and 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° ± 4° for HH 529.

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Photoionized Herbig–Haro objects in the Orion Nebula through deep high-spectral resolution spectroscopy – III. HH 514

Méndez-Delgado¹,

Esteban²,

García‐Rojas³

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We analyze the physical conditions and chemical composition of the photoionized Herbig-Haro object HH 514, which emerges from the proplyd 170-337 in the core of the Orion Nebula. We use high-spectral resolution spectroscopy from UVES at the Very Large Telescope and IFU-spectra from MEGARA at the Gran Telescopio de Canarias. We observe two components of HH 514, the jet base and a knot, with ne = (2.3 ± 0.1) × 105 cm−3 and ne = (7 ± 1) × 104 cm−3, respectively, both with Te ≈ 9000K. We show that the chemical composition of HH 514 is consistent with that of the Orion Nebula, except for Fe, Ni and S, which show higher abundances. The enhanced abundances of Fe and Ni observed in HH objects compared with the general interstellar medium is usually interpreted as destruction of dust grains. The observed sulphur overabundance (more than two times solar) is challenging to explain since the proplyd photoevaporation flow from the same disk shows normal sulphur abundance. If the aforementioned S-overabundance is due to dust destruction, the formation of sulfides and/or other S-bearing dust reservoirs may be linked to planet formation processes in protoplanetary disks, which filter large sulfide dust grains during the accretion of matter from the disk to the central star. We also show that published kinematics of molecular emission close to the central star are not consistent with either a disk perpendicular to the optical jet, nor with an outflow that is aligned with it.

show abstract

Emission-line Data Cubes of the HH 32 Stellar Jet

Cited by 3 publications

References 38 publications

Photoionized Herbig-Haro objects in the Orion Nebula through deep high-spectral resolution spectroscopy III: HH514

Photoionized Herbig-Haro objects in the Orion Nebula through deep high-spectral resolution spectroscopy III: HH514

Photoionized Herbig–Haro objects in the Orion Nebula through deep high-spectral resolution spectroscopy – I. HH 529 II and III

Photoionized Herbig–Haro objects in the Orion Nebula through deep high-spectral resolution spectroscopy – III. HH 514

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