Animation of the Pulsar Surveys

This single 46'' (1.7 pc) beam, centered on the position of the Sgr A* radio source, is a targeted search for undiscovered pulsars orbiting the supermassive black hole candidate. These pulsars could enable the best tests of gravitational theories. The Galactic Centre (GC) search with the Effelsberg telescope started in January 2012, observing at a frequency of 18.95 GHz. Since then, the GC survey capabilities led to the first radio detection of a magnetar in the Galactic Centre likely less than half a light year from Sgr A* [Eatough et al., Nature, August 14, 2013]. Zoom Image
This single 46'' (1.7 pc) beam, centered on the position of the Sgr A* radio source, is a targeted search for undiscovered pulsars orbiting the supermassive black hole candidate. These pulsars could enable the best tests of gravitational theories. The Galactic Centre (GC) search with the Effelsberg telescope started in January 2012, observing at a frequency of 18.95 GHz. Since then, the GC survey capabilities led to the first radio detection of a magnetar in the Galactic Centre likely less than half a light year from Sgr A* [Eatough et al., Nature, August 14, 2013]. [less]
The Parkes Multi Beam Pulsar Survey (PMPS) is the most successful pulsar search of the last generation. And in fact re-analyses of the observational data are still producing new pulsar discoveries up to now. One re-analysis project is currently conducted with EINSTEIN@HOME (E@H) (http://einstein.phys.uwm.edu/),  a volunteer distributed computing project, designed to find pulsars in the most extreme binary systems. Zoom Image
The Parkes Multi Beam Pulsar Survey (PMPS) is the most successful pulsar search of the last generation. And in fact re-analyses of the observational data are still producing new pulsar discoveries up to now. One re-analysis project is currently conducted with EINSTEIN@HOME (E@H) (http://einstein.phys.uwm.edu/),  a volunteer distributed computing project, designed to find pulsars in the most extreme binary systems. [less]
The limit of the survey is 3.5°<|b|<5° and ~74°-150° in longiude. SPAN 512 („Survey Pulsar à Nançay”, http://arxiv.org/abs/1211.3936) started in January 2012 and is expected to be complete in late 2014. Observation is taken with the Nançay telescope in France at 1.2-1.7 GHz with a bandwidth of 512 MHz. Zoom Image
The limit of the survey is 3.5°<|b|<5° and ~74°-150° in longiude. SPAN 512 („Survey Pulsar à Nançay”, http://arxiv.org/abs/1211.3936) started in January 2012 and is expected to be complete in late 2014. Observation is taken with the Nançay telescope in France at 1.2-1.7 GHz with a bandwidth of 512 MHz.
The PALFA [http://www.naic.edu/alfa/pulsar/] survey is ongoing at the Arecibo telescope and uses the seven-pixel ALFA receiver recording data at 1.4 GHz. PALFA observes at low galactic latitudes in two survey regions 32°&lt; l&lt;77° and 168°&lt;l&lt;214°. PALFA began in 2004 and is the most sensitive pulsar survey ever done. Zoom Image
The PALFA [http://www.naic.edu/alfa/pulsar/] survey is ongoing at the Arecibo telescope and uses the seven-pixel ALFA receiver recording data at 1.4 GHz. PALFA observes at low galactic latitudes in two survey regions 32°< l<77° and 168°
[less]
The Arecibo 327-MHz drift scan survey (http://www.naic.edu/~deneva/drift-search/) has been focusing on the declination range -1° to +28°  North. Eventually the survey will cover the entire Arecibo sky (from -1° to +37°). Zoom Image
The Arecibo 327-MHz drift scan survey (http://www.naic.edu/~deneva/drift-search/) has been focusing on the declination range -1° to +28°  North. Eventually the survey will cover the entire Arecibo sky (from -1° to +37°). [less]
The LOFAR Tied-Array All-Sky Survey (LOTAAS) began in early December 2012 and will eventually cover the whole northern sky. Observations are taken with the LOFAR HBA Core Stations tied-array at observing frequency between 119-151 MHz. At these low observing frequencies LOTAAS is well-suited to find weak pulsars. Zoom Image
The LOFAR Tied-Array All-Sky Survey (LOTAAS) began in early December 2012 and will eventually cover the whole northern sky. Observations are taken with the LOFAR HBA Core Stations tied-array at observing frequency between 119-151 MHz. At these low observing frequencies LOTAAS is well-suited to find weak pulsars. [less]
The High Time Resolution Universe (HTRU) survey is a blind survey of the northern sky with the 100-m Effelsberg radio telescope in Germany and a twin survey of the southern sky with the 64-m Parkes radio telescope in Australia. The survey is split into three regions of sky, the low-latitude, medium-latitude and high-latitude regions, with varying integration times for different discovery aims at each region. Zoom Image
The High Time Resolution Universe (HTRU) survey is a blind survey of the northern sky with the 100-m Effelsberg radio telescope in Germany and a twin survey of the southern sky with the 64-m Parkes radio telescope in Australia. The survey is split into three regions of sky, the low-latitude, medium-latitude and high-latitude regions, with varying integration times for different discovery aims at each region.

[less]
All pulsar surveys as displayed in the animation at the top are displayed in Galactic coordinates centred at l=0°, b=0°. Zoom Image
All pulsar surveys as displayed in the animation at the top are displayed in Galactic coordinates centred at l=0°, b=0°. [less]
 
loading content
Go to Editor View