LOFAR: first international fringes
Please note the press release
of the MPIfR and
one of ASTRON.
Our findings are also featured by the EVN newsletter.
Some more details are shown in a presentation.
Fringes between the first international LOFAR station in Effelsberg and
stations near Exloo in the Netherlands have now been detected after several
The long-awaited signal was finally found in observations of the source 3C196
taken with the low-band system (LBA) on 20 August 2009 for the "First
Imaging Busy Week" (George Heald et al).
Neal Jackson and James Anderson
were the first to claim seeing hints of a weak signal in this data but were
not sure about its true nature. This motivated me (Olaf
Wucknitz) to have a closer look.
First delay spectra (28 August 2009)
There were indeed consistent (but noisy) phases visible in parts of the data
(frequency averaged over subbands), but these alone could also be
caused by other effects.
One week after the observations I produced the first delay
spectra of NL-NL and DE-NL baselines (one subband around 45MHz, about one hour
of data 11:15 to 12:15):
Higher resolution delay spectra (30 August 2009)
It is rather obvious that there is a signal at zero delay on both baselines,
but it is much stronger on the shorter Dutch baseline.
However, it is suspicious that the maximum signal is located at a delay of
almost exactly zero, since we would expect some ionospheric delay that is not
corrected during the correlation.
This can be investigated further with the following plots that have been
prepared with higher resolution in delay-space (again for NL-NL and DE-NL
Please click on the images to see a postscript version that also shows some other
subbands of the same observations.
These plots (as the ones above) were produced by taking one subband (195kHz total, 256 channels of
763Hz each), coherently averaging 1 to 32 of the 5sec integrations, Fourier-transforming to translate into delay
space and subsequent incoherent averaging of the power as function of delay.
Again the international LOFAR signal is considerably weaker than the Dutch
one. More importantly we see that the delay is not exactly zero but around -1
micro-sec, about the value expected from the ionosphere and clock offsets.
We also see that the signal gets weaker for longer coherent averaging
intervals (the lower curves) because the non-zero phase rates cause
decorrelation. Still it is good to see that the signal is still clearly
visible even after averaging over 160sec. The ionosphere seems to behave well
even during daytime.
Delay/rate spectra (31 August 2009)
We can take the rates into account by producing two-dimensional delay/rate
spectra. In these plots a peak should appear at the corresponding delay and
rate, while its strength would automatically be corrected for the two effects.
The movies below show these spectra as a function of time. Each time-interval
consists of 64 of the original 5sec integrations. A different subband around
69MHz was now used.
A postscript plot with flux, delay and rate as function of time for this NL-NL baseline can be found here.
A postscript plot with flux, delay and rate as function of time for this DE-NL baseline can be found here.
It is rather obvious that we do indeed see an astronomical signal. The
variation of flux with time is also consistent with the structure of the
source 3C196. Once we take into account delays and rates, we even find that
the signal on the international baseline is not that much weaker than the pure
NL-NL signal as we originally thought.
Later results: multi-band fits
Later I produced movies and plots in which I either averaged incoherently over
all bands or fitted for consistent multi-band delays to all subbands
The latter also provides much higher resolution in delay and even allows to
distinguish between dispersive (ionosphere) and non-dispersive (clock errors,
position errors of target or station) delays and rates. The parameter space
gets quite large when fitting for everything, so the computations take
Here is a movie of coherent multi-band delay/rate for a DE-NL baseline:
Note that the scale in delay (but also rate) is now very different from the
We also see that the response is slightly dirty in the delay direction. This
is partly due to the fact that I only fitted for a non-dispersive delay in
By varying all four parameters (dispersive/non-dispersive delay/rate), I
produced the following plot:
Please click on the image to see the postscript
What do we learn? The flux curve does now actually look like a part of a
sinusoidal beating pattern.
The delay has two contributions, a constant non-dispersive part due to a clock
offset and a time-variable dispersive one due to the ionosphere. Both are at
the expected levels.
The rate, on the other hand, is clearly dominated by the dispersive
ionospheric part. The clock offset is pretty much constant.
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This document last modified Wed Feb 10 15:42:45 UTC 2010