Rotation and Other Motions of the Magellanic Clouds from Radio Observations

Kerr, F. J.; Vaucouleurs, G. de

doi:10.1071/ph550508

Cited by 43 publications

(24 citation statements)

References 7 publications

(8 reference statements)

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“…The centroid of the 3·5 m distribution in the Large Cloud has been calculated by making reasonable estimates of the percentage of radiation originating in the outer regions and is probably accurate to about half a degree. Ignorance of the distribution of weak radiation far from the centre is the chief cause of" (1955a) and Kerr and de Vaucouleurs (1955). " All the centres differ in position, but in view of the uncertainties involved no definite conclusions can be drawn.…”

Section: Radiation From the Magellanic Oloudsmentioning

confidence: 99%

The Observation and Interpretation of Radio Emission from Some Bright Galaxies

Mills¹

1955

Aust. J. Phys.

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SummaryPreliminary attempts to observe 13 bright southern galaxies are described. Of these 10 were detected, including the Magellanic Clouds. The latter were studied in detail. Supplementary measurements on the Milky Way near the galactic centre were made and also some unsuccessful attempts to observe two globular clusters. Taking these results in conjunction with some observations of Brown and Hazard it is possible to derive a consistent picture of the radio emitting properties of " normal" galaxies.It is found that radio emission probably occurs with two markedly different distributions, one displaying characteristics of a type I population, the other having a very extensive, roughly spherical, spatial distribution quite unlike any known stellar population. Both distributions have a non-thermal spectrum, and the relative contributions of each appear to vary between different galaxy types. In general terms, although not altogether in detail, these results support the conclusions reached by Shklovskii concerning the distribution of radio emission in the Galaxy; also his interpretation of the spherical distribution as the result of relativistic electrons radiating in weak magnetic fields is examined, and found, with some modifications, to afford a plausible explanation of the observed differences between the radiating efficiencies of different types of galaxies.

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Section: Radiation From the Magellanic Oloudsmentioning

confidence: 99%

The Observation and Interpretation of Radio Emission from Some Bright Galaxies

Mills¹

1955

Aust. J. Phys.

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“…Because astrophysical factor D depends only in the amount of DM in the halo, and is less sensitive to profile shape, calculations for dIrr Galaxies, plus a combined analysis, can improve our limits for τ χ . As an example, the astrophysical factor D for IC10 is 4.1631 × 10 15 TeV cm −2 , comparable to the value for Triangulum II.…”

Section: Pos(icrc2017)897mentioning

confidence: 54%

“…With the proof that Large and Small Magellanic Clouds are rotating systems [14,15], measurements of the rotation curve of other dIrr Galaxies were performed. It was observed that the rotation curve for these galaxies flatten after about 2 disk scale lengths and no cases of declining curves were found, indicating that dIrr Galaxies have no bulge.…”

Section: The Dm Profile In Dirr Galaxiesmentioning

confidence: 99%

Searching for TeV DM evidence from Dwarf Irregular Galaxies with the HAWC Observatory

Hernández¹,

Alfaro²,

Sandoval³

et al. 2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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The dynamics of dwarf irregular (dIrr) galaxies are observed to be dominated by dark matter (DM). Recently, the DM density distribution has been studied for 31 dIrrs. Their extended DM halo (Burket type profile) makes these objects good candidates for DM searches. Located in Puebla (Mexico), the High Altitude Water Cherenkov (HAWC) Observatory is an optimal instrument to perform such DM searches, because of its large sky coverage (8.4 sr per day). We analyzed a set of two years of HAWC data and we found no significant DM signal from dIrr galaxies. We present the upper limits for DM annihilation cross-section with dIrr galaxies.

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“…4 The average value for the Clouds is approximately equal to the relative density in the solar neighborhood, but is much higher than the integrated figures for the Galaxy and M31. This difference conforms with the difference in galactic types, the Clouds being irregular, and presumably "younger" systems.…”

mentioning

confidence: 81%

Mass Distribution of Galactic Neutral Hydrogen

Kerr¹,

Hindman²

1957

PASP

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which was derived in part from the Leiden 21-cm observations of radial velocity. The hydrogen does not share the high concentration toward the center that is shown by the mass. Its density is relatively constant beyond 4-5 kpc from the center, but falls off rapidly in the inner regions. The radial variation in the proportion of hydrogen to total mass is shown in Figure 1. The upper curve gives the ratio of the space densities in the equatorial surface; the lower curve gives the ratio of the densities projected on to the principal plane (this is the distribution that would be seen 558

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Rotation and Other Motions of the Magellanic Clouds from Radio Observations

Cited by 43 publications

References 7 publications

The Observation and Interpretation of Radio Emission from Some Bright Galaxies

The Observation and Interpretation of Radio Emission from Some Bright Galaxies

Searching for TeV DM evidence from Dwarf Irregular Galaxies with the HAWC Observatory

Mass Distribution of Galactic Neutral Hydrogen

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