Kinematical investigation of possible fast collimated outflows in twelve planetary nebulae

Abstract

A significant fraction of planetary nebulae (PNe) exhibit collimated outflows, distinct narrow kinematical components with notable velocity shifts with respect to the main nebular shells typically associated with low-ionization compact knots and linear or precessing jet-like features. We present here a spatio-kinematical investigation of a sample of twelve PNe with morphologies in emission lines of low-ionization species suggestive of collimated outflows. Using archival narrow-band images and our own high-dispersion long-slit echelle spectra, we confirm the presence of collimated outflows in Hen 2-429, J 320, M 1-66, M 2-40, M 3-1, and NGC 6210 and possibly in NGC 6741, for which the spatio-kinematical data can also be interpreted as a pair of bipolar lobes. The presence of collimated outflows is rejected in Hen 2-47, Hen 2-115, M 1-26, and M 1-37, but their morphology and kinematics are indicative of the action of supersonic outflows that have not been able to pierce through the nebular envelope. In this sense, M 1-66 appears to have experienced a similar interaction between the outflow and nebular envelope, but, as opposed to these four PNe, the outflow has been able to break through the nebular envelope. It is suggested that the PNe without collimated outflows in our sample are younger or descend from lower mass progenitors than those that exhibit unambiguous collimated outflows.

Spin-orbit misalignment from triple-star common envelope evolution

“…The case of an AGB star that engulfs a tight binary system of two MSSs or of a white dwarf with a MSS is relevant to the formation of planetary nebulae, and in particular to planetary nebulae with 'messy' morphologies, i.e, that lack any kind of symmetry. 'Messy' planetary nebulae most like result from triple star interaction (e.g., Bear & Soker 2017;Danehkar et al 2018;Jones et al 2019;Miszalski et al 2019;Schreier et al 2019;Rechy-García et al 2020;Henney et al 2021). The spinning-up of the AGB envelope to have a rotation that is inclined to the triple star orbital angular momentum that I studied here adds to the 'messy' mass loss morphology.…”

Parasite common envelope evolution by triple-star systems

“…However, within ≈ 10 5 yr of total envelope ejection the system forms a planetary nebula. The triple is likely to leave a messy planetary nebulae, i.e., one that strongly depart from axial-symmetry, in particular if the orbital plane of the inner binary is not aligned with the triple orbital plane (e.g., Bear & Soker 2017;Jones et al 2019;Rechy-García et al 2020;Glanz & Perets 2021;Henney et al 2021). Else, the system might explode as a (peculiar) SN Ia.…”

Shaping Planetary Nebulae with Jets and the Grazing Envelope Evolution

“…The early recognition that jets play major roles in shaping planetary nebulae (PNe; e.g., Morris (1987); Soker (1990); Sahai & Trauger (1998)) has received great attention and support in recent years (e.g., Rechy-García et al (2017); Akashi & Soker (2018); Balick et al (2019); Derlopa et al (2019); Estrella-Trujillo et al (2019); Tafoya et al (2019); Balick et al (2020); Rechy-García et al (2020)). The binary system might launch jets before and/or after the common envelope evolution (CEE; e.g., Tocknell et al (2014)).…”