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September 28, 2014, at 03:03 PM by 121.45.161.42 -
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%lfloat width=215px text-align=center margin-top=5px margin-right=25px margin-bottom=5px margin-left=25px% Attach:news_aces3.jpg | BETA Band 1 (712- 1015 MHz) observation of the 1 Jy radio galaxy PKS2252-089. The (known) absorption line associated with HI gas intrinsic to PKS2252-089 can clearly be seen at 884 MHz. The inset shows a close-up of the detected absorption line, with the BETA spectrum in red and an earlier GBT observation in blue. ''[Figure courtesy of CSIRO]''\\\
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%lfloat width=255px text-align=center margin-top=5px margin-right=25px margin-bottom=5px margin-left=25px% Attach:news_aces3.jpg |
BETA Band 1 (712- 1015 MHz) observation of the 1 Jy radio galaxy PKS2252-089. The (known) absorption line associated with HI gas intrinsic to PKS2252-089 can clearly be seen at 884 MHz. The inset shows a close-up of the detected absorption line, with the BETA spectrum in red and an earlier GBT observation in blue. ''[Figure courtesy of CSIRO]''\\\
September 28, 2014, at 03:01 PM by 121.45.161.42 -
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%lfloat width=255px text-align=center margin-top=5px margin-right=25px margin-bottom=5px margin-left=25px% Attach:news_aces3.jpg | BETA Band 1 (712- 1015 MHz) observation of the 1 Jy radio galaxy PKS2252-089. The (known) absorption line associated with HI gas intrinsic to PKS2252-089 can clearly be seen at 884 MHz. The inset shows a close-up of the detected absorption line, with the BETA spectrum in red and an earlier GBT observation in blue. ''[Figure courtesy of CSIRO]'']]
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%lfloat width=215px text-align=center margin-top=5px margin-right=25px margin-bottom=5px margin-left=25px% Attach:news_aces3.jpg | BETA Band 1 (712- 1015 MHz) observation of the 1 Jy radio galaxy PKS2252-089. The (known) absorption line associated with HI gas intrinsic to PKS2252-089 can clearly be seen at 884 MHz. The inset shows a close-up of the detected absorption line, with the BETA spectrum in red and an earlier GBT observation in blue. ''[Figure courtesy of CSIRO]''\\\
September 28, 2014, at 02:59 PM by 121.45.161.42 -
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%lfloat width=255px text-align=center margin-top=5px margin-right=25px margin-bottom=5px margin-left=25px% Attach:news_aces3.jpg | ''[Figure courtesy of CSIRO]''
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%lfloat width=255px text-align=center margin-top=5px margin-right=25px margin-bottom=5px margin-left=25px% Attach:news_aces3.jpg | BETA Band 1 (712- 1015 MHz) observation of the 1 Jy radio galaxy PKS2252-089. The (known) absorption line associated with HI gas intrinsic to PKS2252-089 can clearly be seen at 884 MHz. The inset shows a close-up of the detected absorption line, with the BETA spectrum in red and an earlier GBT observation in blue. ''[Figure courtesy of CSIRO]'']]
September 28, 2014, at 02:54 PM by 121.45.161.42 -
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%lfloat width=255px text-align=center margin-top=5px margin-right=25px margin-bottom=5px margin-left=25px% Attach:2col_final2.jpg|Radio colour-colour plot (from Murphy et al. 2010) for a set of 3763 AT20G sources with near-simultaneous observations at 20, 8 and 5 GHz (crosses). Open circles show a newly-identifed class of ''Ultra-Inverted Spectrum (UIS)'' sources with a spectral index of α(5, 20) > +0.7.\\\
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%lfloat width=255px text-align=center margin-top=5px margin-right=25px margin-bottom=5px margin-left=25px% Attach:2col_final2.jpg|
Radio colour-colour plot (from Murphy et al. 2010) for a set of 3763 AT20G sources with near-simultaneous observations at 20, 8 and 5 GHz (crosses). Open circles show a newly-identifed class of ''Ultra-Inverted Spectrum (UIS)'' sources with a spectral index of α(5, 20) > +0.7.\\\
September 28, 2014, at 02:53 PM by 121.45.161.42 -
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%lfloat width=320px text-align=center margin-top=5px margin-right=25px margin-bottom=5px margin-left=25px% Attach:2col_final2.jpg|Radio colour-colour plot (from Murphy et al. 2010) for a set of 3763 AT20G sources with near-simultaneous observations at 20, 8 and 5 GHz (crosses). Open circles show a newly-identifed class of ''Ultra-Inverted Spectrum (UIS)'' sources with a spectral index of α(5, 20) > +0.7.\\\
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%lfloat width=255px text-align=center margin-top=5px margin-right=25px margin-bottom=5px margin-left=25px% Attach:2col_final2.jpg|Radio colour-colour plot (from Murphy et al. 2010) for a set of 3763 AT20G sources with near-simultaneous observations at 20, 8 and 5 GHz (crosses). Open circles show a newly-identifed class of ''Ultra-Inverted Spectrum (UIS)'' sources with a spectral index of α(5, 20) > +0.7.\\\
September 28, 2014, at 02:52 PM by 121.45.161.42 -
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[[<<]]
September 28, 2014, at 02:51 PM by 121.45.161.42 -
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%lfloat width=255px text-align=center margin-top=5px margin-right=25px margin-bottom=5px margin-left=25px% Attach:news_aces.3jpg | ''[Figure courtesy of CSIRO]''
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%lfloat width=255px text-align=center margin-top=5px margin-right=25px margin-bottom=5px margin-left=25px% Attach:news_aces3.jpg | ''[Figure courtesy of CSIRO]''
September 28, 2014, at 02:49 PM by 121.45.161.42 -
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%lfloat width=255px text-align=center margin-top=5px margin-right=25px margin-bottom=5px margin-left=25px% Attach:news_aces_11072014_full.jpg |
37). ''[Figure courtesy of CSIRO]''
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%lfloat width=255px text-align=center margin-top=5px margin-right=25px margin-bottom=5px margin-left=25px% Attach:news_aces.3jpg | ''[Figure courtesy of CSIRO]''
September 28, 2014, at 02:43 PM by 121.45.161.42 -
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We are currently carrying out a series of ''demonstration science'' observations with the BETA test array which links six ASKAP antenas with Mk1 Phased Array Feeds (see [[http://www.atnf.csiro.au/projects/askap/BETA_results.html | here]] for more details).

%lfloat width=255px text-align=center margin-top=5px margin-right=25px margin-bottom=5px margin-left=25px% Attach:news_aces_11072014_full.jpg |
37). ''[Figure courtesy of CSIRO]''
September 28, 2014, at 02:37 PM by 121.45.161.42 -
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We recently completed the first high-frequency radio survey of the southern sky, the Australia Telescope 20 GHz (AT20G) survey, using a wide-band analogue correlator on the Australia Telescope Compact Array (ATCA). More details of the survey, as well as the public data catalogue released in late 2009, are available [[http://www.atnf.csiro.au/research/AT20G/ | here.]]\\\
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We recently completed the first high-frequency radio survey of the southern sky, the Australia Telescope 20 GHz (AT20G) survey, using a wide-band analogue correlator on the Australia Telescope Compact Array (ATCA). More details of the survey, as well as the public data catalogue released in 2010, are available [[http://www.atnf.csiro.au/research/AT20G/ | here.]]\\\
September 28, 2014, at 02:36 PM by 121.45.161.42 -
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!!! 21cm HI absorption studies with ASKAP
I lead the ASKAP-FLASH survey (see http://www.physics.usyd.edu.au/sifa/Main/FLASH/), which will carry out the first blind survey for HI in individual galaxies at 0.5 < z < 1.0 by detecting the HI line in absorption against background continuum sources.


!!! HI in nearby E/S0 galaxies
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I am also PI for the ASKAP-FLASH survey (see http://www.physics.usyd.edu.au/sifa/Main/FLASH/), which will carry out the first blind survey for HI in individual galaxies at 0.5 < z < 1.0 by detecting the HI line in absorption against background continuum sources.

!!! HI in nearby E/S0 galaxies
January 03, 2010, at 11:36 AM by ems -
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!! 'Radio galaxies and their evolution
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!! Radio galaxies and their evolution
December 16, 2009, at 07:13 AM by ems -
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Welcome to my home page, I'm an ARC Australian Professorial Fellow (and Professor of Astrophysics) in the School of Physics at the University of Sydney. I work within the Sydney Institute for Astronomy (SIfA).
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[+Welcome to my home page, I'm an ARC Australian Professorial Fellow (and Professor of Astrophysics) in the School of Physics at the University of Sydney. I work within the Sydney Institute for Astronomy (SIfA). +]
December 15, 2009, at 11:24 PM by ems -
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December 15, 2009, at 10:15 PM by ems -
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December 15, 2009, at 10:12 PM by ems -
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December 15, 2009, at 10:12 PM by ems -
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Welcome to my home page, I'm an ARC Australian Professorial Fellow (and Professor of Astrophysics) in the School of Physics at the University of Sydney. I work within the Sydney Institute for Astronomy (SIfA).