Knowing the primary beam shape of a radio telescope is critical for deriving accurate fluxes away from the beam center. In the case of PAFs, the primary beam response, also known as the compound beam shape, must be independently measured for each compound beam as they are not constrained to have the same shape. Generally, formed beams further from the pointing center of the PAF will have more elongated shapes. 

Full characterization of the Apertif primary beam is ongoing work. In this documentation we describe the methods used to measure the compound beam shapes (drift scan measurements and Gaussian process regression); describe the first release of primary beam images and plans for near-term updates; and offer an initial characterization of these released primary beam images.

We wish to emphasize that the use of the classic WSRT primary beam correction is not appropriate for Apertif. In addition to the fact that the compound beams can have non circularly symmetric shapes (see Figure 1), the sizes of the primary beams are different from the classic WSRT. The Apertif front-ends fill the focal plane more efficiently than the old MFFE frontends, leading to a smaller primary beam shape. Figure 2 shows one set of measured compound beam shapes divided by the classic WSRT primary beam shape. In addition to the elongated shapes (and offsets) visible in outer beams, the Apertif primary beam value is generally smaller than the classic WSRT primary beam value, confirming the smaller primary beam shape for Apertif.

Figure 1. Beam maps for all 40 apertif beams reconstructed from drift scans. Contour levels are: 0.1, 0.2, 0.4, 0.5, 0.6, 0.8. Red contours highlight the 10% and the 50% sensitivity level. These drift scans were measured in September 2019 and channel 7 corresponds to a frequency of ~ 1.363 GHz.

 

Figure 2. Compound beam shapes derived from drift scans divided by the classic WSRT primary beam. Contours are: 0.2, 0.4, 0.6, 0.8, 1.0.

Latest tweets

Daily image of the week

On June 13-17, the LOFAR Family Meeting took place in Cologne. After two years LOFAR researchers could finally meet in person again. The meeting brings together LOFAR users and researchers to share new scientific results.
https://www.astron.nl/dailyimage/main.php?date=20220621

Our renewed ‘Melkwegpad’ (Milky Way Path) is finished! The new signs have texts in Dutch on the one side and in English on the other side. The signs concerning planets have a small, 3D printed model of that planet in their centre.
https://www.astron.nl/dailyimage/
#Melkwegpad @RTVDrenthe

Daily image of the week

The background drawing shows how the subband correlator calculates the array correlation matrix. In the upper left the 4 UniBoard2s we used. The two ACM plots in the picture show that the phase differences of the visibilities vary from 0 to 360 degrees.

Daily image of the week: Testing with the Dwingeloo Test Station (DTS)
One of the key specifications of LOFAR2.0 is measuring using the low- and the highband antenna at the same time. For this measurement we used 9 lowband antenna and 3 HBA tiles.
https://www.astron.nl/dailyimage/main.php?date=20220607

searchtwitter-squarelinkedin-squarebarsyoutube-playinstagramfacebook-officialenvelopecrosschevron-right