Planetary nebulae with UVIT: II. Revelations from far-UV vision of Butterfly nebula NGC 6302

N. Kameswara Rao; O. De Marco; S. Krishna; J. Murthy; A. Ray; F. Sutaria; R. Mohan

doi:10.1051/0004-6361/201833507

Planetary nebulae with UVIT: II. Revelations from far-UV vision of Butterfly nebula NGC 6302

N. Kameswara Rao, O. De Marco, S. Krishna, J. Murthy, A. Ray, F. Sutaria, R. Mohan

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Abstract

The high excitation planetary nebula, NGC 6302, has been imaged in two far-ultraviolet (FUV) filters, F169M (Sapphire; λ_eff : 1608 Å) and F172M (Silica; λ_eff : 1717 Å) and two near-UV (NUV) filters, N219M (B15; λ_eff : 2196 Å) and N279N (N2; λ_eff : 2792 Å) with the Ultra Violet Imaging Telescope (UVIT). The FUV F169M image shows faint emission lobes that extend to about 5 arcmin on either side of the central source. Faint orthogonal collimated jet-like structures are present on either side of the FUV lobes through the central source. These structures are not present in the two NUV filters or in the FUV F172M filter. Optical and infrared (IR) images of NGC 6302 show bright emission bipolar lobes in the east-west direction with a massive torus of molecular gas and dust seen as a dark lane in the north-south direction. The FUV lobes are much more extended and oriented at a position angle of 113°. They and the jet-like structures might be remnants of an earlier evolutionary phase, prior to the dramatic explosive event that triggered the Hubble type bipolar flows approximately 2200 years ago. The source of the FUV lobe and jet emission is not known, but is likely due to fluorescent emission from H₂ molecules. The cause of the difference in orientation of optical and FUV lobes is not clear and, we speculate, could be related to two binary interactions.

Original language	English
Article number	A138
Pages (from-to)	1-9
Number of pages	9
Journal	Astronomy and Astrophysics
Volume	620
DOIs	https://doi.org/10.1051/0004-6361/201833507
Publication status	Published - 1 Dec 2018

Bibliographical note

Reproduced with permission from Astronomy & Astrophysics, Copyright 2018 ESO. First published in Astronomy and Astrophysics, 620, A138, 2018, published by EDP Sciences. The original publication is available at https://doi.org/10.1051/0004-6361/201833507. Version archived for private and non-commercial use with the permission of the author/s and according to publisher conditions. For further rights please contact the publisher.

Keywords

Stars: winds, outflows
Planetary nebulae: general
Planetary nebulae: individual: NGC 6302
Stars: AGB and post-AGB

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10.1051/0004-6361/201833507

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Cite this

@article{7a17760b84e940ff9714e0fa01faf2e3,

title = "Planetary nebulae with UVIT: II. Revelations from far-UV vision of Butterfly nebula NGC 6302",

abstract = " The high excitation planetary nebula, NGC 6302, has been imaged in two far-ultraviolet (FUV) filters, F169M (Sapphire; λeff : 1608 {\AA}) and F172M (Silica; λeff : 1717 {\AA}) and two near-UV (NUV) filters, N219M (B15; λeff : 2196 {\AA}) and N279N (N2; λeff : 2792 {\AA}) with the Ultra Violet Imaging Telescope (UVIT). The FUV F169M image shows faint emission lobes that extend to about 5 arcmin on either side of the central source. Faint orthogonal collimated jet-like structures are present on either side of the FUV lobes through the central source. These structures are not present in the two NUV filters or in the FUV F172M filter. Optical and infrared (IR) images of NGC 6302 show bright emission bipolar lobes in the east-west direction with a massive torus of molecular gas and dust seen as a dark lane in the north-south direction. The FUV lobes are much more extended and oriented at a position angle of 113°. They and the jet-like structures might be remnants of an earlier evolutionary phase, prior to the dramatic explosive event that triggered the Hubble type bipolar flows approximately 2200 years ago. The source of the FUV lobe and jet emission is not known, but is likely due to fluorescent emission from H2 molecules. The cause of the difference in orientation of optical and FUV lobes is not clear and, we speculate, could be related to two binary interactions. ",

keywords = "Stars: winds, outflows, Planetary nebulae: general, Planetary nebulae: individual: NGC 6302, Stars: AGB and post-AGB",

author = "{Kameswara Rao}, N. and {De Marco}, O. and S. Krishna and J. Murthy and A. Ray and F. Sutaria and R. Mohan",

note = "Reproduced with permission from Astronomy & Astrophysics, Copyright 2018 ESO. First published in Astronomy and Astrophysics, 620, A138, 2018, published by EDP Sciences. The original publication is available at https://doi.org/10.1051/0004-6361/201833507. Version archived for private and non-commercial use with the permission of the author/s and according to publisher conditions. For further rights please contact the publisher.",

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AU - Ray, A.

AU - Sutaria, F.

AU - Mohan, R.

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PY - 2018/12/1

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N2 - The high excitation planetary nebula, NGC 6302, has been imaged in two far-ultraviolet (FUV) filters, F169M (Sapphire; λeff : 1608 Å) and F172M (Silica; λeff : 1717 Å) and two near-UV (NUV) filters, N219M (B15; λeff : 2196 Å) and N279N (N2; λeff : 2792 Å) with the Ultra Violet Imaging Telescope (UVIT). The FUV F169M image shows faint emission lobes that extend to about 5 arcmin on either side of the central source. Faint orthogonal collimated jet-like structures are present on either side of the FUV lobes through the central source. These structures are not present in the two NUV filters or in the FUV F172M filter. Optical and infrared (IR) images of NGC 6302 show bright emission bipolar lobes in the east-west direction with a massive torus of molecular gas and dust seen as a dark lane in the north-south direction. The FUV lobes are much more extended and oriented at a position angle of 113°. They and the jet-like structures might be remnants of an earlier evolutionary phase, prior to the dramatic explosive event that triggered the Hubble type bipolar flows approximately 2200 years ago. The source of the FUV lobe and jet emission is not known, but is likely due to fluorescent emission from H2 molecules. The cause of the difference in orientation of optical and FUV lobes is not clear and, we speculate, could be related to two binary interactions.

AB - The high excitation planetary nebula, NGC 6302, has been imaged in two far-ultraviolet (FUV) filters, F169M (Sapphire; λeff : 1608 Å) and F172M (Silica; λeff : 1717 Å) and two near-UV (NUV) filters, N219M (B15; λeff : 2196 Å) and N279N (N2; λeff : 2792 Å) with the Ultra Violet Imaging Telescope (UVIT). The FUV F169M image shows faint emission lobes that extend to about 5 arcmin on either side of the central source. Faint orthogonal collimated jet-like structures are present on either side of the FUV lobes through the central source. These structures are not present in the two NUV filters or in the FUV F172M filter. Optical and infrared (IR) images of NGC 6302 show bright emission bipolar lobes in the east-west direction with a massive torus of molecular gas and dust seen as a dark lane in the north-south direction. The FUV lobes are much more extended and oriented at a position angle of 113°. They and the jet-like structures might be remnants of an earlier evolutionary phase, prior to the dramatic explosive event that triggered the Hubble type bipolar flows approximately 2200 years ago. The source of the FUV lobe and jet emission is not known, but is likely due to fluorescent emission from H2 molecules. The cause of the difference in orientation of optical and FUV lobes is not clear and, we speculate, could be related to two binary interactions.

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KW - Planetary nebulae: general

KW - Planetary nebulae: individual: NGC 6302

KW - Stars: AGB and post-AGB

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SN - 0004-6361

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JF - Astronomy and Astrophysics

M1 - A138

ER -

Planetary nebulae with UVIT: II. Revelations from far-UV vision of Butterfly nebula NGC 6302

Abstract

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Keywords

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