Parkes observations for project P1066 semester 2021APRS_14
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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ftands:oai:ands.org.au::1767888 2024-09-15T18:36:48+00:00 Parkes observations for project P1066 semester 2021APRS_14 Temporal: From 2021-04-01 to 2021-09-30 https://doi.org/10.25919/gt9x-4950 https://researchdata.edu.au/parkes-observations-project-semester-2021aprs14/1767888 https://data.csiro.au/collection/csiro:52434 http://hdl.handle.net/102.100.100/429477?index=1 unknown Commonwealth Scientific and Industrial Research Organisation https://researchdata.edu.au/parkes-observations-project-semester-2021aprs14/1767888 https://data.csiro.au/collection/csiro:52434 http://hdl.handle.net/102.100.100/429477?index=1 https://doi.org/10.25919/gt9x-4950 Commonwealth Scientific and Industrial Research Organisation transients Astronomical sciences not elsewhere classified Astronomical sciences PHYSICAL SCIENCES dataset ftands https://doi.org/10.25919/gt9x-4950 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) |
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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_14 |
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_14 |
title_short |
Parkes observations for project P1066 semester 2021APRS_14 |
title_full |
Parkes observations for project P1066 semester 2021APRS_14 |
title_fullStr |
Parkes observations for project P1066 semester 2021APRS_14 |
title_full_unstemmed |
Parkes observations for project P1066 semester 2021APRS_14 |
title_sort |
parkes observations for project p1066 semester 2021aprs_14 |
publisher |
Commonwealth Scientific and Industrial Research Organisation |
url |
https://doi.org/10.25919/gt9x-4950 https://researchdata.edu.au/parkes-observations-project-semester-2021aprs14/1767888 https://data.csiro.au/collection/csiro:52434 http://hdl.handle.net/102.100.100/429477?index=1 |
op_coverage |
Temporal: From 2021-04-01 to 2021-09-30 |
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-2021aprs14/1767888 https://data.csiro.au/collection/csiro:52434 http://hdl.handle.net/102.100.100/429477?index=1 https://doi.org/10.25919/gt9x-4950 |
op_doi |
https://doi.org/10.25919/gt9x-4950 |
_version_ |
1810480508252979200 |