Supernova Remnants in the Magellanic Clouds. VII. Infrared Emission from Supernova Remnants

Williams, R. M.; Chu, You‐Hua; Gruendl, R. A.

doi:10.1086/507839

Cited by 32 publications

(35 citation statements)

References 41 publications

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“…With the exception of a weak detection in ULX-1, we have not detected the emission line [O iv] 25.91 mm, a strong feature in SNRs (e.g., Morris et al 2006;Williams et al 2006), supporting previous suggestions that ULX-1 is a SNR (e.g., based on radio and X-ray constraints; Roberts et al 2002).…”

Section: L24supporting

confidence: 85%

Constraints on Accretion in Ultraluminous X-Ray Sources fromSpitzerIRS Observations of NGC 4485/4490: Infrared Diagnostic Diagrams

Vázquez¹,

Hornschemeier²,

Colbert³

et al. 2007

ApJ

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Constraining the astrophysical nature of ultraluminous X-ray (ULX) sources, which have X-ray luminosities exceeding 10 39 ergs s Ϫ1 , has been elusive due to the optical faintness of any counterparts. With high spectral resolution observations in the ∼10-30 mm wavelength range we have conducted an experiment to study six ULX sources in the NGC 4485/4490 galaxy pair. We have found that five of the six ULXs, based on mid-infrared spectral diagnostics, show the characteristic higher ionization features that are found in AGNs. The sixth source, ULX-1, is consistent with being a supernova remnant. The chief infrared spectral diagnostics used are the ratiosIn two instances fits to the continuum and polycyclic aromatic hydrocarbon (PAH) features also indicate higher dust temperatures, which are characteristic of accreting sources. Overall, however, we find that the continuum is dominated by stellar processes, and the best diagnostic features are the emission lines. High spectral resolution studies in the mid-infrared thus appear to show great promise for determining the astrophysical nature of ULXs.

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Section: L24supporting

confidence: 85%

Constraints on Accretion in Ultraluminous X-Ray Sources fromSpitzerIRS Observations of NGC 4485/4490: Infrared Diagnostic Diagrams

Vázquez¹,

Hornschemeier²,

Colbert³

et al. 2007

ApJ

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“…Evidence for this quantity of dust forming in young SNe in the local Universe has been scant and controversial. Observations from mid‐/far‐infrared (IR) satellites ( IRAS , ISO and Spitzer ) detect only warm dust and find orders of magnitude less than predicted by theory (Dwek et al 1987; Lagage et al 1996; Douvion et al 2001; Borkowski et al 2006; Sugerman et al 2006; Williams, Chu & Gruendl 2006; Blair et al 2007; Meikle et al 2007), for example the maximum warm dust mass inferred for Cas A from Spitzer data is 0.03–0.05 M ⊙ (Rho et al 2008). Submillimetre (submm) observations of Cas A seemed to provide the first evidence for large (∼2 M ⊙ ) quantities of colder dust manufactured in the SN explosion (Dunne et al 2003, hereafter D03).…”

Section: Introductionmentioning

confidence: 93%

Cassiopeia A: dust factory revealed via submillimetre polarimetry

Dunne

Maddox

Ivison

et al. 2009

Monthly Notices of the Royal Astronomical Society

124

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If Type-II supernovae - the evolutionary end points of short-lived, massive stars - produce a significant quantity of dust (>0.1 M_sun) then they can explain the rest-frame far-infrared emission seen in galaxies and quasars in the first Gyr of the Universe. Submillimetre observations of the Galactic supernova remnant, Cas A, provided the first observational evidence for the formation of significant quantities of dust in Type-II supernovae. In this paper we present new data which show that the submm emission from Cas A is polarised at a level significantly higher than that of its synchrotron emission. The orientation is consistent with that of the magnetic field in Cas A, implying that the polarised submm emission is associated with the remnant. No known mechanism would vary the synchrotron polarisation in this way and so we attribute the excess polarised submm flux to cold dust within the remnant, providing fresh evidence that cosmic dust can form rapidly. This is supported by the presence of both polarised and unpolarised dust emission in the north of the remnant, where there is no contamination from foreground molecular clouds. The inferred dust polarisation fraction is unprecedented (f_pol ~ 30%) which, coupled with the brief timescale available for grain alignment (<300 yr), suggests that supernova dust differs from that seen in other Galactic sources (where f_pol=2-7%), or that a highly efficient grain alignment process must operate in the environment of a supernova remnant.Comment: In press at MNRAS, 10 pages, print in colou

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“…Now there are 74 SNRs and candidates. The sources were Dickel et al (2001), Lazendic, Dickel & Jones (2003), van der Heyden, Bleeker & Kaastra (2004), Blair et al (2006), Williams, Chu & Gruendl (2006), Bojicic et al (2007), and Chu et al (1997).…”

Section: The Updated Cataloguementioning

confidence: 99%

A general catalogue of extended objects in the Magellanic System

Bica

Bonatto

Dutra

et al. 2008

Monthly Notices of the Royal Astronomical Society

184

276

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We update the SMC, Bridge, and LMC catalogues of extended objects that were constructed by members of our group from 1995 to 2000. In addition to the rich subsequent literature for the previous classes, we now also include HI shells and supershells. A total of 9305 objects were cross-identified, while our previous catalogues amounted to 7900 entries, an increase of $\approx12%$. We present the results in subcatalogues containing 1445 emission nebulae, 3740 star clusters, 3326 associations, and 794 HI shells and supershells. Angular and apparent size distributions of the extended objects are analysed. We conclude that the objects, in general, appear to respond to tidal effects arising from the LMC, SMC, and Bridge. Number-density profiles extracted along directions parallel and perpendicular to the LMC bar, can be described by two exponential-disks. A single exponential-disk fits the equivalent SMC profiles. Interestingly, when angular-averaged number-densities of most of the extended objects are considered, the profiles of both Clouds do not follow an exponential-disk. Rather, they are best described by a tidally-truncated, core/halo profile, despite the fact that the Clouds are clearly disturbed disks. On the other hand, the older star clusters taken isolately, distribute as an exponential disk. The present catalogue is an important tool for the unambiguous identification of previous objects in current CCD surveys and to establish new findings.Comment: 15 pages, 10 figures, MNRAS, accepte

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Supernova Remnants in the Magellanic Clouds. VII. Infrared Emission from Supernova Remnants

Cited by 32 publications

References 41 publications

Constraints on Accretion in Ultraluminous X-Ray Sources fromSpitzerIRS Observations of NGC 4485/4490: Infrared Diagnostic Diagrams

Constraints on Accretion in Ultraluminous X-Ray Sources fromSpitzerIRS Observations of NGC 4485/4490: Infrared Diagnostic Diagrams

Cassiopeia A: dust factory revealed via submillimetre polarimetry

A general catalogue of extended objects in the Magellanic System

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