Near-infrared [Fe II] and H2 emission-line study of Galactic supernova remnants in the first quadrant

Yong Hyun Lee; Bon Chul Koo; Jae-Joon Lee; Michael G. Burton; Stuart Ryder

doi:10.3847/1538-3881/ab0212

Near-infrared [Fe II] and H₂ emission-line study of Galactic supernova remnants in the first quadrant

Yong Hyun Lee, Bon Chul Koo, Jae-Joon Lee, Michael G. Burton, Stuart Ryder

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Abstract

We report the detection of near-infrared (NIR) [Fe ii] (1.644 μm) and H₂ 1-0 S(1) (2.122 μm) line features associated with Galactic supernova remnants (SNRs) in the first quadrant using two narrowband imaging surveys, UWIFE and UWISH2. Among the total of 79 SNRs fully covered by both surveys, we found 19 [Fe II]-emitting and 19 H₂ -emitting SNRs, giving a detection rate of 24% for each. Eleven SNRs show both emission features. The detection rate of [Fe II] and H₂ peaks at the Galactic longitude (l) of 40°-50° and 30°-40°, respectively, and gradually decreases toward smaller/larger l. Five out of the eleven SNRs emitting both emission lines clearly show an "[Fe II]-H₂ reversal," where H₂ emission features are found outside the SNR boundary in [Fe II] emission. Our NIR spectroscopy shows that the H₂ emission originates from collisionally excited H₂ gas. The brightest SNR in both [Fe ii] and H₂ emissions is W49B, contributing more than 70% and 50% of the total [Fe II] 1.644 μm (2.0 ×10⁴ L⊙) and H₂ 2.122 μm (1.2 ×10^{3 L}⊙) luminosities of the detected SNRs. The total [Fe II] 1.644 μm luminosity of our Galaxy is a few times smaller than that expected from the SN rate using the correlation found in nearby starburst galaxies. We discuss possible explanations for this.

Original language	English
Article number	123
Pages (from-to)	1-19
Number of pages	19
Journal	Astronomical Journal
Volume	157
Issue number	3
DOIs	https://doi.org/10.3847/1538-3881/ab0212
Publication status	Published - Mar 2019

Bibliographical note

Copyright 2019 The American Astronomical Society. First published in The Astronomical Journal, 157(3), 123, 2019. The original publication is available at http://www.doi.org/10.3847/1538-3881/ab0212, published by IOP Publishing. 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

infrared: ISM
ISM: clouds
ISM: supernova remnants
surveys

Access to Document

10.3847/1538-3881/ab0212

Publisher version (open access)Final published version, 13.5 MBLicence: Other

Cite this

@article{9c15d35583ae47bf8f837f036da225a6,

title = "Near-infrared [Fe II] and H2 emission-line study of Galactic supernova remnants in the first quadrant",

abstract = " We report the detection of near-infrared (NIR) [Fe ii] (1.644 μm) and H2 1-0 S(1) (2.122 μm) line features associated with Galactic supernova remnants (SNRs) in the first quadrant using two narrowband imaging surveys, UWIFE and UWISH2. Among the total of 79 SNRs fully covered by both surveys, we found 19 [Fe II]-emitting and 19 H2 -emitting SNRs, giving a detection rate of 24% for each. Eleven SNRs show both emission features. The detection rate of [Fe II] and H2 peaks at the Galactic longitude (l) of 40°-50° and 30°-40°, respectively, and gradually decreases toward smaller/larger l. Five out of the eleven SNRs emitting both emission lines clearly show an {"}[Fe II]-H2 reversal,{"} where H2 emission features are found outside the SNR boundary in [Fe II] emission. Our NIR spectroscopy shows that the H2 emission originates from collisionally excited H2 gas. The brightest SNR in both [Fe ii] and H2 emissions is W49B, contributing more than 70% and 50% of the total [Fe II] 1.644 μm (2.0 ×104 L⊙) and H2 2.122 μm (1.2 ×103 L⊙) luminosities of the detected SNRs. The total [Fe II] 1.644 μm luminosity of our Galaxy is a few times smaller than that expected from the SN rate using the correlation found in nearby starburst galaxies. We discuss possible explanations for this.",

keywords = "infrared: ISM, ISM: clouds, ISM: supernova remnants, surveys",

author = "Lee, {Yong Hyun} and Koo, {Bon Chul} and Jae-Joon Lee and Burton, {Michael G.} and Stuart Ryder",

note = "Copyright 2019 The American Astronomical Society. First published in The Astronomical Journal, 157(3), 123, 2019. The original publication is available at http://www.doi.org/10.3847/1538-3881/ab0212, published by IOP Publishing. 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.",

year = "2019",

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language = "English",

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T1 - Near-infrared [Fe II] and H2 emission-line study of Galactic supernova remnants in the first quadrant

AU - Lee, Yong Hyun

AU - Koo, Bon Chul

AU - Lee, Jae-Joon

AU - Burton, Michael G.

AU - Ryder, Stuart

N1 - Copyright 2019 The American Astronomical Society. First published in The Astronomical Journal, 157(3), 123, 2019. The original publication is available at http://www.doi.org/10.3847/1538-3881/ab0212, published by IOP Publishing. 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.

PY - 2019/3

Y1 - 2019/3

N2 - We report the detection of near-infrared (NIR) [Fe ii] (1.644 μm) and H2 1-0 S(1) (2.122 μm) line features associated with Galactic supernova remnants (SNRs) in the first quadrant using two narrowband imaging surveys, UWIFE and UWISH2. Among the total of 79 SNRs fully covered by both surveys, we found 19 [Fe II]-emitting and 19 H2 -emitting SNRs, giving a detection rate of 24% for each. Eleven SNRs show both emission features. The detection rate of [Fe II] and H2 peaks at the Galactic longitude (l) of 40°-50° and 30°-40°, respectively, and gradually decreases toward smaller/larger l. Five out of the eleven SNRs emitting both emission lines clearly show an "[Fe II]-H2 reversal," where H2 emission features are found outside the SNR boundary in [Fe II] emission. Our NIR spectroscopy shows that the H2 emission originates from collisionally excited H2 gas. The brightest SNR in both [Fe ii] and H2 emissions is W49B, contributing more than 70% and 50% of the total [Fe II] 1.644 μm (2.0 ×104 L⊙) and H2 2.122 μm (1.2 ×103 L⊙) luminosities of the detected SNRs. The total [Fe II] 1.644 μm luminosity of our Galaxy is a few times smaller than that expected from the SN rate using the correlation found in nearby starburst galaxies. We discuss possible explanations for this.

AB - We report the detection of near-infrared (NIR) [Fe ii] (1.644 μm) and H2 1-0 S(1) (2.122 μm) line features associated with Galactic supernova remnants (SNRs) in the first quadrant using two narrowband imaging surveys, UWIFE and UWISH2. Among the total of 79 SNRs fully covered by both surveys, we found 19 [Fe II]-emitting and 19 H2 -emitting SNRs, giving a detection rate of 24% for each. Eleven SNRs show both emission features. The detection rate of [Fe II] and H2 peaks at the Galactic longitude (l) of 40°-50° and 30°-40°, respectively, and gradually decreases toward smaller/larger l. Five out of the eleven SNRs emitting both emission lines clearly show an "[Fe II]-H2 reversal," where H2 emission features are found outside the SNR boundary in [Fe II] emission. Our NIR spectroscopy shows that the H2 emission originates from collisionally excited H2 gas. The brightest SNR in both [Fe ii] and H2 emissions is W49B, contributing more than 70% and 50% of the total [Fe II] 1.644 μm (2.0 ×104 L⊙) and H2 2.122 μm (1.2 ×103 L⊙) luminosities of the detected SNRs. The total [Fe II] 1.644 μm luminosity of our Galaxy is a few times smaller than that expected from the SN rate using the correlation found in nearby starburst galaxies. We discuss possible explanations for this.

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KW - ISM: clouds

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KW - surveys

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