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        <dc:title>Detection of compact radio emission from Circinus X-1 with the first Southern hemisphere e-VLBI experiment</dc:title>
        <dc:creator>Phillips, CJ</dc:creator>
        <dc:creator>Dickey, JM</dc:creator>
        <dc:creator>Fender, RP</dc:creator>
        <dc:creator>Tudose, V</dc:creator>
        <dc:creator>Nicolson, GD</dc:creator>
        <dc:creator>Deller, A</dc:creator>
        <dc:creator>Amy, SW</dc:creator>
        <dc:creator>Tingay, SJ</dc:creator>
        <dc:creator>Tzioumis, AK</dc:creator>
        <dc:creator>Reynolds, JE</dc:creator>
        <dc:creator>Jauncey, DL</dc:creator>
        <dc:creator>Stevens, JB</dc:creator>
        <dc:creator>Ellingsen, S</dc:creator>
        <dc:subject>240101 Astronomy and Astrophysics</dc:subject>
        <dc:description>Circinus X-1 has recently returned to a state of strong radio flaring. Here we report on the first&#13;
VLBI observations, and detection, undertaken in the 25 years since the 1975–1985 period of&#13;
strong recurrent flaring activity.We detected Circinus X-1 with the first observations conducted&#13;
by a recently developed Southern hemisphere e-VLBI array, at both 1.6 and 8.4 GHz, over a&#13;
three-day period. At 1.6 GHz, the compact source has a total flux density of 11 mJy and a size of&#13;
60 ± 15 mas (Gaussian model full width at half maximum). At 8.4 GHz, the compact source is&#13;
less than 60 mas. The size variation with frequency is consistent with a broadened image&#13;
due to scattering in the turbulent, ionized interstellar medium of our Galaxy. However, these&#13;
size measurements appear inconsistent with the λ2.2 variation expected for strong interstellar&#13;
scattering and previous VLBI observations made at 2.3 GHz in the early 1980s. To explain this&#13;
apparent inconsistency, we suggest that Circinus X-1 supports a weak, non-varying component&#13;
of 35 mas extent (175 au at 5 kpc distance), corresponding to compact structure in the extended&#13;
radio nebula. No significant variation in the flux density at 1.6 GHz is evident between two&#13;
observations 24 h apart. No jet-like structures are evident on scales of tens of mas, simply a&#13;
scatter broadened source, presumably coincident with the suggested neutron star in the binary&#13;
system.</dc:description>
        <dc:publisher>Blackwell Publishing</dc:publisher>
        <dc:date>2007</dc:date>
        <dc:type>Article</dc:type>
        <dc:type>PeerReviewed</dc:type>
        <dc:format>application/pdf</dc:format>
        <dc:identifier>http://eprints.utas.edu.au/4065/1/4065.pdf</dc:identifier>
        <dc:relation>http://dx.doi.org/10.1111/j.1745-3933.2007.00339.x</dc:relation>
        <dc:identifier>Phillips, CJ and Dickey, JM and Fender, RP and Tudose, V and Nicolson, GD and Deller, A and Amy, SW and Tingay, SJ and Tzioumis, AK and Reynolds, JE and Jauncey, DL and Stevens, JB and Ellingsen, S (2007) Detection of compact radio emission from Circinus X-1 with the first Southern hemisphere e-VLBI experiment. Monthly Notices of the Royal Astronomical Society, 380 (1). L11-L14. ISSN 0035-8711</dc:identifier>
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