What Produced the Ultraluminous Supernova Remnant in NGC 6946?

Dunne, B. C.; Gruendl, R. A.; Chu, You‐Hua

doi:10.1086/301264

Cited by 30 publications

(41 citation statements)

References 31 publications

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“…In some ULXNe radial velocity gradients (∼100 km/s) were directly detected (Dunne et al(2000), Pakull et al(2006), Fabrika et al(2006) and references therein). We make an additional conclusion:…”

Section: Discussionmentioning

confidence: 92%

“…Dunne et al(2000) have resolved Hα, [N ii] and [O iii] lines in a narrow (FWHM∼20-40km s −1 ) component from unshocked material and a broad (FWHM∼250km s −1 ) from shocked material. Basing on the MPFS and SCORPIO spectra we performed a thoroughful analysis of the ionization and excitation sources of the nebula Abolmasov et al, 2007a), leading to a conclusion that most of the power of the nebula comes not from shock waves but from photoionizing ultraviolet source even more luminous than the central X-ray source.…”

Section: Ngc6946 X-1mentioning

confidence: 99%

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Spectroscopy of optical counterparts of ultraluminous X-ray sources

et al. 2007

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Abstract. Here we present the results of panoramic and long-slit observations of eight ULX nebular counterparts held with the 6m SAO telescope. In two ULXNe we detected for the first time signatures of high excitation ([O iii]λ5007 / Hβ > 5). Two of the ULXs were identified with young (T ∼ 5 − 10 M yr) massive star clusters. Four of the eight ULX Nebulae (ULXNe) show bright high-excitation lines. This requires existence of luminous (∼ 10 38 ÷ 10 40 ergs s −1 ) UV/EUV sources coinciding with the X-ray sources. Other 4 ULXNe require shock excitation of the gas with shock velocities of 20-100km s −1 . However, all the studied ULXN spectra show signatures of shock excitation, but even those ULXNe where the shocks are prevailing show presence of a hard ionizing source with the luminosity at least ∼ 10 38 ergs s −1 . Most likely shock waves, X-ray and EUV ionization act simultaneously in all the ULXNe, but they may be roughly separated in two groups, shock-dominated and photoionization-dominated ULXNe. The ULXs have to produce strong winds and/or jets powering their nebulae with ∼ 10 39 ergs s −1 . Both the wind/jet activity and the EUV source needed are consistent with the suggestion that ULXs are high-mass X-ray binaries with the supercritical accretion disks of the SS433 type.

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Section: Discussionmentioning

confidence: 92%

Section: Ngc6946 X-1mentioning

confidence: 99%

Spectroscopy of optical counterparts of ultraluminous X-ray sources

et al. 2007

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“…It is located near H ii regions, but does not encompass any massive stars. MF 33 resembles both the Type Ia SNR N103B in the LMC (Hughes et al 1995) and the core-collapse SNR MF 16 in NGC 6946 (Dunne et al 2000), so we cannot classify it as either Type Ia or core collapse.…”

Section: Discussionmentioning

confidence: 96%

Physical Structure and Nature of Supernova Remnants in M101

Franchetti

Gruendl

Chu

et al. 2012

The Astronomical Journal

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Supernova remnant (SNR) candidates in the giant spiral galaxy M101 have been previously identified from groundbased Hα and [S ii] images. We have used archival Hubble Space Telescope (HST) Hα and broadband images as well as stellar photometry of 55 SNR candidates to examine their physical structure, interstellar environment, and underlying stellar population. We have also obtained high-dispersion echelle spectra to search for shocked high-velocity gas in 18 SNR candidates, and identified X-ray counterparts to SNR candidates using data from archival observations made by the Chandra X-Ray Observatory. Twenty-one of these 55 SNR candidates studied have X-ray counterparts, although one of them is a known ultraluminous X-ray source. The multi-wavelength information has been used to assess the nature of each SNR candidate. We find that within this limited sample, ∼16% are likely remnants of Type Ia SNe and ∼45% are remnants of core-collapse SNe. In addition, about ∼36% are large candidates which we suggest are either superbubbles or OB/H ii complexes. Existing radio observations are not sensitive enough to detect the non-thermal emission from these SNR candidates. Several radio sources are coincident with X-ray sources, but they are associated with either giant H ii regions in M101 or background galaxies. The archival HST Hα images do not cover the entire galaxy and thus prevents a complete study of M101. Furthermore, the lack of HST [S ii] images precludes searches for small SNR candidates which could not be identified by ground-based observations. Such high-resolution images are needed in order to obtain a complete census of SNRs in M101 for a comprehensive investigation of the distribution, population, and rates of SNe in this galaxy.

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“…Though both searches detected a large number of sources (27 and 35, respectively), only two were in common (Lacey & Duric 2001): MF9 and MF16, using the notation from Matonick & Fesen (1997). MF16 is known to be an extremely luminous X-ray source with luminosity of approximately 10 39 erg per second: the true nature of this X-ray emission is still not known (Dunne et al 2000;Schlegel et al 2000). We adopted the optical diameters for these sources as listed by Matonick & Fesen (1997), assuming a distance to the galaxy of 5.5 Mpc (Tully 1988).…”

Section: Ngc 6946mentioning

confidence: 99%

The $\mathsf{\Sigma}$ – Drelation for supernova remnants in nearby galaxies

Urošević

Pannuti

Duric

et al. 2005

A&A

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Abstract. This paper examines relations between the radio surface brightness Σ and the diameter D (also known as Σ − D relations) for a sample of extragalactic supernova remnants (SNRs) as constructed from a combination of published data and data from our own surveys. Our sample of extragalactic SNRs is the largest ever devised for the purpose of analyzing Σ − D relations. The main results of this paper may be summarized as follows: (i) the empirical relations for SNRs in 10 of the 11 nearby galaxies studied have the approximately trivial Σ ∝ D −2 form, therefore limiting their interpretation as physically meaningful relations. In addition, these relations are subject to selection effects rendering them even less useful. Further Monte Carlo simulations suggest that the effect of survey sensitivity has the opposite effect of volume selection (e.g. Malmquist bias, a volume selection effect that shapes the Galactic sample) by tending to flatten the slopes toward a trivial relation. In this case, the true slopes may be steeper than the observed slopes; (ii) compact M 82 SNRs appear to follow a uniquely different Σ− D relation in comparison to the larger, older SNRs in the other 10 galaxies. Monte Carlo simulations suggest that the probability of this difference arising by chance is ≈1% to 10%, depending on what is assumed regarding the underlying SNR population; (iii) three candidate hypernova remnants were identified in our sample of 11 nearby galaxies.

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What Produced the Ultraluminous Supernova Remnant in NGC 6946?

Cited by 30 publications

References 31 publications

Spectroscopy of optical counterparts of ultraluminous X-ray sources

Spectroscopy of optical counterparts of ultraluminous X-ray sources

Physical Structure and Nature of Supernova Remnants in M101

The $\mathsf{\Sigma}$ – Drelation for supernova remnants in nearby galaxies

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