The relativistic ISM in M33: Role of the supernova remnants

Duric, N.; Gordon, S.; Goss, W. M.; Viallefond, F.; Lacey, C. K.

doi:10.1086/175683

Cited by 56 publications

(53 citation statements)

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“…The analysis of the synchrotron emission in the young supernova remnant Cas A showed the presence of electrons with energies up to 200 GeV with a magnetic field strength of about 500 µG. The interpretation of nonthermal radio emission from external galaxies proved that supernova remnants are the sites of acceleration of relativistic electrons with an efficiency similar to the one needed to provide the observed intensity of Galactic cosmic-ray electrons (Duric et al 1995).…”

Section: Supernova Remnants As Cr Accelerators and Gamma-ray Astronomymentioning

confidence: 97%

Cosmic Rays in Galactic and Extragalactic Magnetic Fields

et al. 2011

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We briefly review sources of cosmic rays, their composition and spectra as well as their propagation in the galactic and extragalactic magnetic fields, both regular and fluctuating. A special attention is paid to the recent results of the X-ray and gamma-ray observations that shed light on the origin of the galactic cosmic rays and the challenging results of Pierre Auger Observatory on the ultra high energy cosmic rays. The perspectives of both high energy astrophysics and cosmic-ray astronomy to identify the sources of ultra high energy cosmic rays, the mechanisms of particle acceleration, to measure the intergalactic radiation fields and to reveal the structure of magnetic fields of very different scales are outlined.

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Section: Supernova Remnants As Cr Accelerators and Gamma-ray Astronomymentioning

confidence: 97%

Cosmic Rays in Galactic and Extragalactic Magnetic Fields

et al. 2011

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“…27 to integrate via: (28) which is a better estimate of the total contribution of non-thermal emission from SNRs in the LMC. As in Duric et al (1993) we then B 0 (LMC) 1−α(LMC) (29) where τ e represents the residency time of electrons in the disk of the galaxy, τ snr is the lifetime of the remnant and S 20 is the non-thermal flux density at 20 cm. The equation has a similar form as in Duric et al (1993) with the α sign being the only difference.…”

Section: Radio Surface Brightness Evolutionmentioning

confidence: 99%

“…As in Duric et al (1993) we then B 0 (LMC) 1−α(LMC) (29) where τ e represents the residency time of electrons in the disk of the galaxy, τ snr is the lifetime of the remnant and S 20 is the non-thermal flux density at 20 cm. The equation has a similar form as in Duric et al (1993) with the α sign being the only difference. Duric et al (1993) used S ∝ ν −α while here we adopted the S ∝ ν α form.…”

Section: Radio Surface Brightness Evolutionmentioning

confidence: 99%

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Statistical Analysis of Supernova Remnants in the Large Magellanic Cloud

Bozzetto

Filipović

Vukotić

et al. 2017

ApJS

111

158

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We construct the most complete sample of supernova remnants (SNRs) in any galaxy -the Large Magellanic Cloud (LMC) SNR sample. We study their various properties such as spectral index (α), size and surface-brightness. We suggest an association between the spatial distribution, environment density of LMC SNRs and their tendency to be located around supergiant shells. We find evidence that the 16 known type Ia LMC SNRs are expanding in a lower density environment compared to the Core-Collapse (CC) type. The mean diameter of our entire population (74) is 41 pc, which is comparable to nearby galaxies. We didn't find any correlation between the type of SN explosion, ovality or age. The N (< D) relationship of a = 0.96 implies that the randomised diameters are readily mimicking such an exponent. The rate of SNe occurring in the LMC is estimated to be ∼1 per 200 yr. The mean α of the entire LMC SNR population is α=-0.52, which is typical of most SNRs. However, our estimates show a clear flattening of the synchrotron α as the remnants age. As predicted, our CC SNRs sample are significantly brighter radio emitters than the type Ia remnants. We also estimate the Σ − D relation for the LMC to have a slope ∼3.8 which is comparable with other nearby galaxies. We also find the residency time of electrons in the galaxy

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“…Optically selected SNRs: 98 sources, Gordon et al (1998); 5. Radio selected SNRs: 30 sources, Duric et al (1995), Gordon et al (1999); 6. PNe: 152 sources Ciardullo et al (2004).…”

Section: The Ir Emission Of Nebulae In M 33mentioning

confidence: 99%

Star formation in M 33: Spitzer photometry of discrete sources

Verley

Hunt²,

Corbelli

et al. 2007

A&A

132

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Aims. Combining the relative vicinity of the Local Group spiral galaxy M 33 with the Spitzer images, we investigate the properties of infrared (IR) emission sites and assess the reliability of the IR emission as a star formation tracer. Methods. The mid-and far-IR emission of M 33 was obtained from IRAC and MIPS images from the Spitzer archive. We compared the photometric results for several samples of three known types of discrete sources (Hii regions, supernovae remnants and planetary nebulae) with theoretical diagnostic diagrams, and derived the spectral energy distribution (from 3.6 to 24 µm) of each type of object. Moreover, we generated a catalogue of 24 µm sources and inferred their nature from the observed and theoretical colours of the known type sources. We estimated the star formation rate in M 33 both globally and locally, from the IR emission and from the Hα emission line.Results. The colours of the typical IR emissions of Hii regions, supernovae remnants and planetary nebulae are continuous among the different samples, with overlapping regions in the diagnostic diagrams. The comparison between the model results and the colours of Hii regions indicates a dusty envelope at relatively high temperatures ∼600 K, and moderate extinction A V < ∼ 10. The 24 µm sources IR colours follow the regions observationally defined by the three classes of known objects but the majority of them represent Hii regions. The derived total IR luminosity function is in fact very similar to the Hii luminosity function observed in the Milky Way and in other late type spirals. Even though our completeness limit is 5 × 10 37 erg s −1 , in low density regions we are able to detect sources five times fainter than this, corresponding to the faintest possible Hii region. The 8 and 24 µm luminosities within the central 5 kpc of M 33 are comparable and of order 4 × 10 28 erg s −1 Hz −1 (νL ν (8) = 1.5 × 10 42 and νL ν (24) = 4.4 × 10 41 erg s −1 ). We estimate the total IR emission in the same region of M 33 to be 10 9 L . The discrete sources account for about one third of the 24 µm emission while the rest is diffuse. From the IR emission, we derive a star formation rate for the inner disk equal to 0.2 M yr −1 , consistent with the star formation rate obtained from the Hα emission.

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The relativistic ISM in M33: Role of the supernova remnants

Cited by 56 publications

References 0 publications

Cosmic Rays in Galactic and Extragalactic Magnetic Fields

Cosmic Rays in Galactic and Extragalactic Magnetic Fields

Statistical Analysis of Supernova Remnants in the Large Magellanic Cloud

Star formation in M 33: Spitzer photometry of discrete sources

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