The messy death of a multiple star system and the resulting planetary nebula as observed by JWST

Marco, Orsola De; Akashi, Muhammad; Akras, S.; Alcolea, J.; Aleman, Isabel; Amram, P.; Balick, Bruce; Beck, E. De; Blackman, Eric G.; Boffin, H. M. J.; Boumis, P.; Bublitz, Jesse; Bucciarelli, B.; Bujarrabal, V.; Cami, J.; Chornay, Nicholas; Chu, You‐Hua; Corradi, R. L. M.; Frank, Adam; García-Hernández, D. A.; García‐Rojas, J.; Garcı́a-Segura, Guillermo; Gómez-Llanos, Veronica; Gonçalves, Denise R.; Guerrero, M. A.; Jones, David; Karakas, Amanda I.; Kastner, Joel H.; Kwok, Sun; Lykou, Foteini; Manchado, A.; Matsuura, M.; McDonald, Iain; Miszalski, B.; Mohamed, S.; Monreal-Ibero, A.; Monteiro, H.; Montez, Rodolfo; Moraga, Baez, Paula; Morisset, Charles; Nordhaus, Jason; Oliveira, C. Mendes de; Osborn, Zara; Otsuka, Masaaki; Parker, Quentin A.; Peeters, E.; Quint, Bruno; Quintana-Lacaci, G.; Redman, M. P.; Ruiter, Ashley J.; Sabin, L.; Sahai, Raghvendra; Contreras, C. Sánchez; Santander-García, M.; Seitenzahl, Ivo R.; Soker, Noam; Speck, A. K.; Stanghellini, Letizia; Steffen, W.; Toalá, J. A.; Ueta, Toshiya; Steene, G. C. Van de; Winckel, H. Van; Ventura, P.; Villaver, E.; Vlemmings, Wouter; Walsh, J. R.; Wesson, R.; Zijlstra, A. A.

doi:10.1038/s41550-022-01845-2

Cited by 20 publications

(22 citation statements)

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“…We have investigated the relationship between the CS and the A2V star as follows. First, there is little doubt that these two stars are a physical pair (De Marco et al 2022), given the close agreement in their Gaia-based proper motions (A2V star: PMra = −7.747 ± 0.027 mas yr −1 , PMdec = −0.125 ± 0.031 mas yr −1 ; CS: PMra = −7.677 ± 0.235 mas yr −1 , PMdec = 0.197 ± 0.28 mas yr −1 ) and radial velocities (A2V star: VLSR = −24.1 ± 1.6 km s −1 ; CS: VLSR = −25 ± 0.9 km s −1 ). We have therefore inferred a distance to NGC 3132 of 0.75 kpc by inverting the parallax of the A2V star companion 11 (1.3198 ± 0.0344mas) listed in the Gaia DR3 database (Gaia Collaboration 2022).…”

Section: A Central Binary and Orbital Motionmentioning

confidence: 99%

“…16 Models with a substantial fraction of large grains, e.g.,  a 1 max μm, produced radial intensity profiles that are significantly more compact than observed; in addition, the detailed shape of the SED between 7.7 and 18 μm (described above) cannot be reproduced-large grains produce a dust emission spectrum in which there is a smooth rise with increasing wavelength. De Marco et al (2022) present a simple large-grain (size ~100 μm) dust shell model, which suffers from these deficiencies. Keeping the grain-size distribution the same but allowing the grains to be cooler by decreasing T d results in a decrease in the 7.7 μm to 18 μm flux ratio-and simultaneously makes the model emission more extended due to an increase in R in .…”

Section: Dust Radiative Transfer Modelingmentioning

confidence: 99%

“…In the two-shell model, the mass in the inner shell is a small percentage (0.5%) of the total. For comparison, de Marco et al (2022) derive a dust mass of ~5 x 10 -2 M ⊕ from their simple model. For both the one-shell and two-shell model classes, models covering an appropriately large input parameter space were computed, allowing us to estimate rough uncertainties in the derived output parameters for a fixed value of T eff .…”

Section: Dust Radiative Transfer Modelingmentioning

confidence: 99%

“…Including the theoretical spectrum of such a companion (BT-NextGen (AGSS2009) model with T eff = 2500 K, log(g(cm s −2 )) = 5, extracted from http://svo2.cab.inta-csic.es/theory/newov2/ index.php; Allard et al 2011) increases the model SED flux in the F356W filter by 30%, well above the observed value (see inset of Figure 5(d)). De Marco et al (2022) propose that the CS has at least two, and maybe even three close companions, in order to explain the origin of the dust cloud and the morphological structure of the extended PN.…”

Section: Interaction With a Binary Companionmentioning

confidence: 99%

“…We focus in this study on the CS and its immediate surroundings; description and analysis of the full PN morphology are not within the scope of this paper, but has been reported by De Marco et al (2022).…”

Section: Introductionmentioning

confidence: 99%

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The Binary and the Disk: The Beauty is Found within NGC3132 with JWST

Sahai

Bujarrabal

Quintana-Lacaci

et al. 2023

ApJ

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The planetary nebula (PN) NGC 3132 is a striking example of the dramatic but poorly understood mass-loss phenomena that (1–8) M ⊙ stars undergo during their death throes as they evolve into white dwarfs (WDs). From an analysis of JWST multiwavelength (0.9–18 μm) imaging of NGC 3132, we report the discovery of an extended dust cloud around the WD central star (CS) of NGC 3132, seen most prominently in the 18 μm image, with a surface-brightness-limited radial extent of ≳2″. We show that the A2V star located 1.″7 to CS’s northeast (and 0.75 kpc from Earth) is gravitationally bound to the latter, as evidenced by the detection of relative orbital angular motion of 0.°24 ± 0.°045 between these stars over ∼20 yr. Using aperture photometry of the CS extracted from the JWST images, together with published optical photometry and an archival UV spectrum, we have constructed the spectral energy distribution (SED) of the CS and its extended emission over the UV to mid-IR (0.091–18 μm) range. We find that fitting the SED of the CS and the radial intensity distributions at 7.7, 12.8, and 18 μm with thermal emission from dust requires a cloud that extends to a radius of ≳1785 au, with a dust mass of ∼1.3 × 10−2 M ⊕ and grains that are 70% silicate and 30% amorphous carbon. We propose plausible origins of the dust cloud and an evolutionary scenario in which a system of three stars—the CS, a close low-mass companion, and a more distant A2V star—forms a stable hierarchical triple system on the main sequence but becomes dynamically unstable later, resulting in the spectacular mass ejections that form the current, multipolar PN.

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Section: A Central Binary and Orbital Motionmentioning

confidence: 99%

Section: Dust Radiative Transfer Modelingmentioning

confidence: 99%

Section: Dust Radiative Transfer Modelingmentioning

confidence: 99%

Section: Interaction With a Binary Companionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The Binary and the Disk: The Beauty is Found within NGC3132 with JWST

Sahai

Bujarrabal

Quintana-Lacaci

et al. 2023

ApJ

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Chemical tracers of a highly eccentric AGB–main-sequence star binary

Danilovich,

Malfait,

Van de Sande

et al. 2024

Nat Astron

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Morphokinematical study of the planetary nebula Me2-1: Unveiling its point-symmetric and unusual physical structure

Miranda,

Vázquez,

Olguín

et al. 2024

A&A

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Me\,2-1 is a high-excitation planetary nebula whose morphology and physical structure have not yet been investigated. We present narrow-band images in several emission lines, and high- and intermediate-resolution long-slit spectra aimed at investigating its morphology and 3D structure, and its physical parameters and chemical abundances. By applying deconvolution techniques to the images, we identified in Me\,2-1: an elliptical ring; two elongated, curved structures (caps) that contain three pairs of bright point-symmetric (PS) knots; a shell interior of the ring; and a faint halo or attached shell. The caps are observed in all images, while the PS knots are only observed in the low-excitation emission line ones. These structures are also identified in the high-resolution long-slit spectra, allowing us to study their morphokinematics. The 3D reconstruction shows that Me\,2-1 consists of a ring seen almost pole-on, and a virtually spherical shell, to which the caps and PS knots are attached. Caps and PS knots most probably trace the sites where high-velocity collimated bipolar outflows, ejected along a wobbling axis, collide with the spherical shell, are slowed down, and remain attached to it. Although the main excitation mechanism in Me\,2-1 is found to be photoionization, a contribution of shocks in the PS knots is suggested by their emission line ratios. The combination of collimated outflows and a ring with a spherical shell is unusual among planetary nebulae. We speculate that two planets, each with less than one Jupiter mass, could be involved in the formation of Me\,2-1 if both enter a common envelope evolution during the asymptotic giant branch phase of the progenitor. One planet is tidally disrupted, forming an accretion disk around the central star, from which collimated bipolar outflows are ejected; the other planet survives, causing wobbling of the accretion disk. The physical parameters and chemical abundances obtained from our intermediate-resolution spectrum are similar to those obtained in previous analyses, with the abundances also pointing to a low-mass progenitor of Me\,2-1.

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The messy death of a multiple star system and the resulting planetary nebula as observed by JWST

Cited by 20 publications

References 80 publications

The Binary and the Disk: The Beauty is Found within NGC3132 with JWST

The Binary and the Disk: The Beauty is Found within NGC3132 with JWST

Chemical tracers of a highly eccentric AGB–main-sequence star binary

Morphokinematical study of the planetary nebula Me2-1: Unveiling its point-symmetric and unusual physical structure

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