Detection of knots in the supernova type Iax remnant Pa 30
Abstract
We present deep, narrowband Gemini North/GMOS images of the Pa 30 nebula that reveal rich small-scale structure in the ejecta filaments. In [S II], the number of detected filaments increases by about an order of magnitude compared to previous studies. The imaging further reveals that the filaments are not smooth radial streaks, but instead are composed of cascades of knots or clumps. The images in [O III] yield the first confirmation that previously detected diffuse [O III] emission in fact originates from the same [S II] filaments. We measure a nebula center consistent with the position of the central star, indicating that the remnant has not received a large transverse kick. The 3σ upper limit on the velocity of the stellar kick is ≲100 km/s. Cross-sectional profiles of the filaments in [S II] and [O III] show a central peak on top of a nebular background, the latter being likely due to diffuse emission or unresolved filaments. The median [S II] width of 0.7'' is slightly broader than the 0.50'' seeing, providing some evidence of partially resolved filaments and implying a characteristic knot diameter of ∼1016 cm. The ≈1'' widths measured in [O III] are consistent with the poorer seeing of the oxygen images. The discovery of this clumpy substructure provides a new observational constraint on models for the origin and evolution of the remarkable filamentary ejecta of Pa 30.
Versions
Related
- Detection of Knots in the Type Iax Supernova Remnant Pa 30
- Fermi-LAT Detection of Extended GeV Emission toward the Middle-aged Supernova Remnant G156.2+05.7
- Pulsar J1909+0749 and Supernova Remnant G42.1-0.2: A case of a pulsar that has exited the shell of its associated supernova remnant
- XRISM/Resolve Study of Large Scale Properties in Tycho's Supernova Remnant
- Identifying a jet-shaped point-symmetric morphology in the supernova remnant HB9
BibTeX
@misc{cunningham2026detection,
title = {{Detection of knots in the supernova type Iax remnant Pa 30}},
author = {Tim Cunningham and Ilaria Caiazzo and John C. Raymond and Scott J. Kenyon},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.06424},
eprint = {2610.06424},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.06424},
}
RIS
TY - UNPB
TI - Detection of knots in the supernova type Iax remnant Pa 30
AU - Tim Cunningham
AU - Ilaria Caiazzo
AU - John C. Raymond
AU - Scott J. Kenyon
PY - 2026
DA - 2026/10/05
PB - arXiv
DO - 10.48550/arxiv.2610.06424
UR - https://arxiv.org/abs/2610.06424
AB - We present deep, narrowband Gemini North/GMOS images of the Pa 30 nebula that reveal rich small-scale structure in the ejecta filaments. In [S II], the number of detected filaments increases by about an order of magnitude compared to previous studies. The imaging further reveals that the filaments are not smooth radial streaks, but instead are composed of cascades of knots or clumps. The images in [O III] yield the first confirmation that previously detected diffuse [O III] emission in fact originates from the same [S II] filaments. We measure a nebula center consistent with the position of the central star, indicating that the remnant has not received a large transverse kick. The 3σ upper limit on the velocity of the stellar kick is ≲100 km/s. Cross-sectional profiles of the filaments in [S II] and [O III] show a central peak on top of a nebular background, the latter being likely due to diffuse emission or unresolved filaments. The median [S II] width of 0.7'' is slightly broader than the 0.50'' seeing, providing some evidence of partially resolved filaments and implying a characteristic knot diameter of ∼10^16 cm. The ≈1'' widths measured in [O III] are consistent with the poorer seeing of the oxygen images. The discovery of this clumpy substructure provides a new observational constraint on models for the origin and evolution of the remarkable filamentary ejecta of Pa 30.
ER -