The early interaction of the planetary nebula NGC 40  
 with the interstellar medium

Martin, Jodie R.; Xilouris, K. M.; Soker, Noam

doi:10.1051/0004-6361:20020848

Cited by 15 publications

(24 citation statements)

References 24 publications

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“…5) of proper motion, similar to case B of Wareing et al (2007). The filamentary structure and the direction of the filaments suggests strong interaction of the stellar wind with ISM, as described by Martin et al (2002).…”

Section: Fuv Halo and Ismsupporting

confidence: 63%

“…5) and extends to about 4 arcmin from the star. The FUV halo is also filamentary and shows similarity with optical and IR halo features like the bent jet (Martin et al 2002) and bands denoted as A & B by Ramos-Larios et al (2011). (2) The axis of the FUV halo seems to point in the direction of the proper motion of the star.…”

Section: Fuv Halo and Ismmentioning

confidence: 99%

“…(2) The axis of the FUV halo seems to point in the direction of the proper motion of the star. Figure 5 (black contours) from Martin et al (2002) shows the proper motion vector (black arrow).…”

Section: Fuv Halo and Ismmentioning

confidence: 99%

“…The ISO and Spitzer spectra of the nebula show that it has 90 to 150 K cool dust, polycyclic aromatic hydrocarbon (PAH) features as well as some low-ionization ionic lines (Ramos-Larios et al 2011). Martin et al (2002) interpreted the bright filament in the north-east and other filaments and tongues as a result of the interaction of the nebula as it moves in the interstellar medium (ISM). The discovery of diffuse soft X-ray emission from NGC 40 confirmed the interaction of the fast stellar wind with slowmoving AGB envelope (Montez et al 2005).…”

Section: Introductionmentioning

confidence: 99%

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Planetary nebulae with UVIT: Far ultra-violet halo around the Bow Tie nebula (NGC 40)

Rao

Sutaria

Murthy

et al. 2018

A&A

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Context. NGC 40 is a planetary nebula with diffuse X-ray emission, suggesting an interaction of the high-speed wind from WC8 central star (CS) with the nebula. It shows strong C IV 1550 Å emission that cannot be explained by thermal processes alone. We present here the first map of this nebula in C IV emission using broad band filters on the Ultra-Violet Imaging Telescope (UVIT). Aims. We aim to map the hot C IV-emitting gas and its correspondence with soft X-ray (0.3-8 keV) emitting regions in order to study the shock interaction between the nebula and the ISM. We also aim to illustrate the potential of UVIT for nebular studies. Methods. We carry out a morphological study of images of the nebula obtained at an angular resolution of about 1.3 in four UVIT filter bands that include C IV 1550 Å and [C II] 2326 Å lines as well as UV continuum. We also make comparisons with X-ray, optical, and IR images from the literature. Results. The [C II] 2326 Å images show the core of the nebula with two lobes on either side of CS similar to [N II]. The C IV emission in the core shows similar morphology and extent to that of diffuse X-ray emission concentrated in nebular condensations. A surprising UVIT discovery is the presence of a large faint far UV (FUV) halo in an FUV filter with λ eff of 1608 Å. The UV halo is not present in any other UV filter. The FUV halo is most likely due to UV fluorescence emission from the Lyman bands of H 2 molecules. Unlike the optical and IR halo, the FUV halo trails predominantly towards the south-east side of the nebular core, opposite to the CS's proper motion direction. Conclusions. Morphological similarity of C IV 1550 Å and X-ray emission in the core suggests that it results mostly from the interaction of strong CS wind with the nebula. The FUV halo in NGC 40 highlights the extensive existence of H 2 molecules in the regions even beyond the optical and IR halos. Thus UV studies are important to estimate the amount of H 2 , which is probably the most dominant molecule and significant for mass-loss studies.

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Section: Fuv Halo and Ismsupporting

confidence: 63%

Section: Fuv Halo and Ismmentioning

confidence: 99%

Section: Fuv Halo and Ismmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Planetary nebulae with UVIT: Far ultra-violet halo around the Bow Tie nebula (NGC 40)

Rao

Sutaria

Murthy

et al. 2018

A&A

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“…The lack of X-ray emission associated with the apparent "blowouts" (interruptions in the rim) that are aligned along an axis running NNE-SSW in NGC 40 further suggests that this wind is more or less spherically symmetric, with a possible enhancement along the equatorial plane of the system rather than along the polar axis. We note that there is no kinematic evidence for the presence of collimated jets in NGC 40, despite the appearance of polar "blowouts" and jet-like features in this nebula (Meaburn et al 1996;Martin et al 2002).…”

Section: Discussionmentioning

confidence: 66%

X‐Ray Imaging of Planetary Nebulae with Wolf‐Rayet–type Central Stars: Detection of the Hot Bubble in NGC 40

Montez

Kastner

Marco

et al. 2005

ApJ

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We present the results of Chandra X-ray Observatory (CXO) observations of the planetary nebulae (PNs) NGC 40 and Hen 2-99. Both PNs feature late-type Wolf-Rayet central stars that are presently driving fast (∼ 1000 km s −1 ), massive winds into denser, slow-moving (∼10 km s −1 ) material ejected during recently terminated asymptotic giant branch (AGB) evolutionary phases. Hence, these observations provide key tests of models of wind-wind interactions in PNs. In NGC 40, we detect faint, diffuse X-ray emission distributed within a partial annulus that lies nested within a ∼ 40 ′′ diameter ring of nebulosity observed in optical and near-infrared images. Hen 2-99 is undetected. The inferred X-ray temperature (T X ∼ 10 6 K) and luminosity (L X ∼ 2 × 10 30 ergs s −1 ) of NGC 40 are the lowest measured thus far for any PN displaying diffuse X-ray emission. These results, combined with the ring-like morphology of the X-ray emission -2 -from NGC 40, suggest that its X-ray emission arises from a "hot bubble" that is highly evolved and is generated by a shocked, quasi-spherical fast wind from the central star, as opposed to AGB or post-AGB jet activity. In constrast, the lack of detectable X-ray emission from Hen 2-99 suggests that this PN has yet to enter a phase of strong wind-wind shocks.

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Interacting planetary nebulae III: verification and galactic population based on the measurements of Gaia EDR3

Mohery

Ali

Mindil

et al. 2022

Astrophys Space Sci

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The early interaction of the planetary nebula NGC 40 with the interstellar medium

Cited by 15 publications

References 24 publications

Planetary nebulae with UVIT: Far ultra-violet halo around the Bow Tie nebula (NGC 40)

Planetary nebulae with UVIT: Far ultra-violet halo around the Bow Tie nebula (NGC 40)

X‐Ray Imaging of Planetary Nebulae with Wolf‐Rayet–type Central Stars: Detection of the Hot Bubble in NGC 40

Interacting planetary nebulae III: verification and galactic population based on the measurements of Gaia EDR3

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