Parkes observations for project P1066 semester 2021APRS_22
We propose 36 hrs of Parkes observations to continue our successful Deeper, Wider, Faster (DWF) program to detect fast transients and fast radio burst (FRB) counterparts and help resolve their nature. DWF coordinates over 80 observatories worldwide at all wavelengths, from radio to gamma-ray to dete...
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Online Access: | https://doi.org/10.25919/fe7x-2q11 https://researchdata.edu.au/parkes-observations-project-semester-2021aprs22/1769898 https://data.csiro.au/collection/csiro:52469 http://hdl.handle.net/102.100.100/429691?index=1 |
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ftands:oai:ands.org.au::1769898 2024-09-09T20:09:07+00:00 Parkes observations for project P1066 semester 2021APRS_22 Temporal: From 2021-04-01 to 2021-09-30 https://doi.org/10.25919/fe7x-2q11 https://researchdata.edu.au/parkes-observations-project-semester-2021aprs22/1769898 https://data.csiro.au/collection/csiro:52469 http://hdl.handle.net/102.100.100/429691?index=1 unknown Commonwealth Scientific and Industrial Research Organisation https://researchdata.edu.au/parkes-observations-project-semester-2021aprs22/1769898 https://data.csiro.au/collection/csiro:52469 http://hdl.handle.net/102.100.100/429691?index=1 https://doi.org/10.25919/fe7x-2q11 Commonwealth Scientific and Industrial Research Organisation transients Astronomical sciences not elsewhere classified Astronomical sciences PHYSICAL SCIENCES dataset ftands https://doi.org/10.25919/fe7x-2q11 2024-08-13T00:21:48Z We propose 36 hrs of Parkes observations to continue our successful Deeper, Wider, Faster (DWF) program to detect fast transients and fast radio burst (FRB) counterparts and help resolve their nature. DWF coordinates over 80 observatories worldwide at all wavelengths, from radio to gamma-ray to detect and follow-up FRBs and other elusive fast (millisecond-to-hours duration) transients. Crucially, we coordinate simultaneous deep, fast-cadenced, wide-field observations at all wavelengths to observe the same field at the same time as Parkes, enabling multi-wavelength detection before, during, and after the radio detection. Little to no multi-wavelength observations to any significant depth have been done on these timescales, leaving this parameter space underexplored. DWF coordinates major facilities to observe with Parkes, such as South Pole Telescope (mm/sub-mm), GROND (infrared), CTIO Dark Energy Camera (optical), Astrosat (UV/X-ray), HXMT (X-ray), HESS (gamma-ray), and Pierre Auger (high-energy). We perform realtime data processing and transient identification at all wavelengths that enables triggering our deep, rapid-response (within minutes) follow up programs for deep spectroscopy and imaging using the world's largest telescopes (e.g., Keck, VLT, Gemini, SALT, ATCA). Dataset South pole Research Data Australia (Australian National Data Service - ANDS) Gemini ENVELOPE(-62.500,-62.500,-66.133,-66.133) Hess ENVELOPE(-65.133,-65.133,-67.200,-67.200) South Pole |
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Open Polar |
collection |
Research Data Australia (Australian National Data Service - ANDS) |
op_collection_id |
ftands |
language |
unknown |
topic |
transients Astronomical sciences not elsewhere classified Astronomical sciences PHYSICAL SCIENCES |
spellingShingle |
transients Astronomical sciences not elsewhere classified Astronomical sciences PHYSICAL SCIENCES Parkes observations for project P1066 semester 2021APRS_22 |
topic_facet |
transients Astronomical sciences not elsewhere classified Astronomical sciences PHYSICAL SCIENCES |
description |
We propose 36 hrs of Parkes observations to continue our successful Deeper, Wider, Faster (DWF) program to detect fast transients and fast radio burst (FRB) counterparts and help resolve their nature. DWF coordinates over 80 observatories worldwide at all wavelengths, from radio to gamma-ray to detect and follow-up FRBs and other elusive fast (millisecond-to-hours duration) transients. Crucially, we coordinate simultaneous deep, fast-cadenced, wide-field observations at all wavelengths to observe the same field at the same time as Parkes, enabling multi-wavelength detection before, during, and after the radio detection. Little to no multi-wavelength observations to any significant depth have been done on these timescales, leaving this parameter space underexplored. DWF coordinates major facilities to observe with Parkes, such as South Pole Telescope (mm/sub-mm), GROND (infrared), CTIO Dark Energy Camera (optical), Astrosat (UV/X-ray), HXMT (X-ray), HESS (gamma-ray), and Pierre Auger (high-energy). We perform realtime data processing and transient identification at all wavelengths that enables triggering our deep, rapid-response (within minutes) follow up programs for deep spectroscopy and imaging using the world's largest telescopes (e.g., Keck, VLT, Gemini, SALT, ATCA). |
format |
Dataset |
title |
Parkes observations for project P1066 semester 2021APRS_22 |
title_short |
Parkes observations for project P1066 semester 2021APRS_22 |
title_full |
Parkes observations for project P1066 semester 2021APRS_22 |
title_fullStr |
Parkes observations for project P1066 semester 2021APRS_22 |
title_full_unstemmed |
Parkes observations for project P1066 semester 2021APRS_22 |
title_sort |
parkes observations for project p1066 semester 2021aprs_22 |
publisher |
Commonwealth Scientific and Industrial Research Organisation |
url |
https://doi.org/10.25919/fe7x-2q11 https://researchdata.edu.au/parkes-observations-project-semester-2021aprs22/1769898 https://data.csiro.au/collection/csiro:52469 http://hdl.handle.net/102.100.100/429691?index=1 |
op_coverage |
Temporal: From 2021-04-01 to 2021-09-30 |
long_lat |
ENVELOPE(-62.500,-62.500,-66.133,-66.133) ENVELOPE(-65.133,-65.133,-67.200,-67.200) |
geographic |
Gemini Hess South Pole |
geographic_facet |
Gemini Hess South Pole |
genre |
South pole |
genre_facet |
South pole |
op_source |
Commonwealth Scientific and Industrial Research Organisation |
op_relation |
https://researchdata.edu.au/parkes-observations-project-semester-2021aprs22/1769898 https://data.csiro.au/collection/csiro:52469 http://hdl.handle.net/102.100.100/429691?index=1 https://doi.org/10.25919/fe7x-2q11 |
op_doi |
https://doi.org/10.25919/fe7x-2q11 |
_version_ |
1809943242778607616 |