A SEARCH FOR SUPERNOVA REMNANTS IN NGC 6946 USING THE [Fe II] 1.64 μm LINE

Bruursema, Justice; Meixner, Margaret; Long, Knox S.; Otsuka, Masaaki

doi:10.1088/0004-6256/148/3/41

Cited by 13 publications

(18 citation statements)

References 35 publications

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“…J84.906182-69.769472 is one of three sources that shows [Fe ii] 1.64 µm emission. Near-IR [Fe ii] emission is often assumed to be shock excited as it is seen in protostellar jets and supernova remnants (e.g., Giannini et al 2013;Bruursema et al 2014). However, significant FUV radiation in H ii regions may allow photoexcitation to dominate (e.g., Mouri et al 2000).…”

Section: Ysos In N159mentioning

confidence: 99%

“…Near-IR [Fe ii] emission lines are often assumed to be collisionally-excited in shocks given their prevalence in protostellar jets and supernova remnants (e.g., Hollenbach & McKee 1989;Morel et al 2002;Giannini et al 2013;Bruursema et al 2014). However, as with H 2 , in H ii regions where significant FUV radiation permeates the region, [Fe ii] may be photoexcited.…”

Section: [Fe Ii]mentioning

confidence: 99%

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Unveiling the nature of candidate high-mass young stellar objects in the Magellanic Clouds with near-IR spectroscopy

Reiter

Nayak

Meixner

et al. 2019

Monthly Notices of the Royal Astronomical Society

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As nearby neighbors to the Milky Way, the Large and Small Magellanic Clouds (LMC and SMC) provide a unique opportunity to study star formation in the context of their galactic ecosystems. Thousands of young stellar objects (YSOs) have been characterized with large-scale Spitzer and Herschel surveys. In this paper, we present new near-IR spectroscopy of five high-mass YSOs in the LMC and one in the SMC. We detect multiple hydrogen recombination lines, as well as He i 2.058 µm, H 2 , [Fe ii], and [S iii] in these highly excited sources. We estimate the internal extinction of each source and find that it is highest for sources with the youngest evolutionary classifications. Using line ratios, we assess the dominant excitation mechanism in the three sources where we detect both H 2 2.12 µm and [Fe ii] 1.64 µm. In each case, photoexcitation dominates over shock excitation. Finally, we detect CO bandhead absorption in one of our LMC sources. While this feature is often associated with evolved stars, this object is likely young with strong PAH and fine-structure emission lines tracing an H ii region detected at longer wavelengths. Compared to high-mass YSOs in the Galaxy, our sources have higher bolometric and line luminosities, consistent with their selection as some of the brightest sources in the LMC and SMC.

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Section: Ysos In N159mentioning

confidence: 99%

Section: [Fe Ii]mentioning

confidence: 99%

Unveiling the nature of candidate high-mass young stellar objects in the Magellanic Clouds with near-IR spectroscopy

Reiter

Nayak

Meixner

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…The 1D spectrum of Spot A in Slit 2 is shown inFigure 9. .-[Fe II] 1.644 µm luminosity of Galactic and extragalactic SNRs: Galactic SNRs (this paper), LMC SNRs(Oliva et al 1989), M33 SNRs(Morel et al 2002), NGC 1569 and NGC 5253 SNRs(Labrie & Pritchet 2006), NGC 6946 SNRs(Bruursema et al 2014), and M82 and NGC 253 SNRs (Alonso-Herrero et al 2003). For M82 and NGC 253, the upper and lower luminosities are presented.…”

mentioning

confidence: 82%

Near-infrared [Fe ii] and H₂ Emission-line Study of Galactic Supernova Remnants in the First Quadrant

Lee

Koo

Lee

et al. 2019

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We report the detection of near-infrared (NIR) [Fe II] (1.644 µm) and H 2 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 H 2 -emitting SNRs, giving a detection rate of 24% for each. Eleven SNRs show both emission features. The detection rate of [Fe II] and H 2 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]-H 2 reversal," where H 2 emission features are found outside the SNR boundary in [Fe II] emission. Our NIR spectroscopy shows that the H 2 emission originates from collisionally excited H 2 gas. The brightest SNR in both [Fe II] and H 2 emissions is W49B, contributing more than 70% and 50% of the total [Fe II] 1.644 µm (2.0 × 10 4 L ) and H 2 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.

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“…In any case, the elliptical ring is not a young supernova remnant, because there is no [Fe II] or X-ray emission, as follows from the data shown by Bruursema et al (2014). The Red Ellipse is ten times larger and much brighter than the MF 16, and this fact alone casts strong doubt on the identification of the Red Ellipse as a SNR.…”

Section: Archival Direct Imagingmentioning

confidence: 91%

Imaging and spectroscopic observations of a strange elliptical bubble in the northern arm of the spiral galaxy NGC 6946

Efremov¹,

Моисеев²

2016

Mon. Not. R. Astron. Soc.

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NGC 6946, known as the Fireworks galaxy because of its high supernova rate and high star formation, is embedded in a very extended HI halo. Its northern spiral arm is well detached from the galactic main body. We found that this arm contains a large (∼ 300 pc in size) Red Ellipse, named according to a strong contamination of the Hα emission line on its optical images. The ellipse is accompanied by a short parallel arc and a few others still smaller and less regular; a bright star cluster is seen inside these features. The complicated combination of arcs seems to be unique, it is only a bit similar to some SNRs. However, the long-slit spectral data obtained with the Russian 6-m telescope did not confirm the origin of the nebula as a result of a single SN outburst. The emission-line spectrum corresponds to the photoionization by young hot stars with a small contribution of shock ionization. The most likely explanation of the Red Ellipse is a superbbuble created by a collective feedback of massive stars in the star cluster located in the NE side of the Red Ellipse. However, the very regular elliptical shape of the nebulae seems strange.

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A SEARCH FOR SUPERNOVA REMNANTS IN NGC 6946 USING THE [Fe II] 1.64 μm LINE

Cited by 13 publications

References 35 publications

Unveiling the nature of candidate high-mass young stellar objects in the Magellanic Clouds with near-IR spectroscopy

Unveiling the nature of candidate high-mass young stellar objects in the Magellanic Clouds with near-IR spectroscopy

Near-infrared [Fe ii] and H₂ Emission-line Study of Galactic Supernova Remnants in the First Quadrant

Imaging and spectroscopic observations of a strange elliptical bubble in the northern arm of the spiral galaxy NGC 6946

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A SEARCH FOR SUPERNOVA REMNANTS IN NGC 6946 USING THE [Fe II] 1.64 μm LINE

Cited by 13 publications

References 35 publications

Unveiling the nature of candidate high-mass young stellar objects in the Magellanic Clouds with near-IR spectroscopy

Unveiling the nature of candidate high-mass young stellar objects in the Magellanic Clouds with near-IR spectroscopy

Near-infrared [Fe ii] and H2 Emission-line Study of Galactic Supernova Remnants in the First Quadrant

Imaging and spectroscopic observations of a strange elliptical bubble in the northern arm of the spiral galaxy NGC 6946

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Near-infrared [Fe ii] and H₂ Emission-line Study of Galactic Supernova Remnants in the First Quadrant