projects:jupiter:intercont-2023-12-27 [Fundamental Physics in Radio Astronomy]

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====== Observations 2023-12-27 20:30-22:30 UTC ======

This time was chosen because of a good chance to see DAM signals from both hemispheres of Jupiter, so that that could be calibration relative to each other. We observed with NenuFAR, the LWA (LWA1, LWA-SV), KAIRA, GLOW, and other international LOFAR stations (FIXME). It is very sad that our Ukrainian friends cannot participate with UTR2 anymore. 

All LOFAR(-like) stations observed in RCU mode 3 (band 10_90) with 8-bit recording of 244 subbands (40-283, 8-55 MHz). Beamforming was done in direction ''0.5826639,0.2118205,J2000'' or ''0,0,JUPITER''.



===== Individual stations =====

Diagnostic plots for all participating LOFAR stations (and eventually NenuFAR, FIXME) can be found {{:projects:jupiter:jupiter_2023_12_27_stat.pdf|here.}} They all show clear signatures from Jupiter in the dynamic spectra even at this very low resolution.


==== KAIRA ====

Here are beamlet statistics (dynamic spectrum) just before the observations: \\
{{:projects:jupiter:kaira_kmb.png?direct&300|KAIRA BST plot}}

This plot was taken from the realtime display at [[https://www.sgo.fi/KAIRA/bst.php]]. It shows nice DAM signals (possibly  Io-B, north).

**People involved: Derek McKay**


==== NenuFAR ====

Beamlet statistics (dynamic spectra for XX and YY) from NenuFAR show the great performance of this telescope: \\
{{:projects:jupiter:20231227_202900_bst_sum_up_glisse_s_.pdf}}

These plots show the strong (Io-B?) arc, but unfortunately not the expected (Io-D) counterpart from the southern hemisphere that we had hoped for. The exact nature of these signals needs to be investigated. In any case the signal is clearly strong enough for a VLBI analysis.

Here are plots from data taken before our observation (kindly provided by Laurent Lamy):\\
{{:projects:jupiter:20231227_140000_20231227_202900_jupiter_tracking.pdf}}\\
He writes: "(1) It confirmes that the prominent vertex-early arcs are RH polarized (white on the bottom panel) and therefore consistent with Io-B emission (2) at the lowest frequencies, LH emission (black on the bottom panel) is seen continuously after 16:30, including what might be a signature of Io-D emission after 18:00".

This means we have a good chance to see emission from both hemispheres at least at the beginning of our observation.

**People involved: Laurent Lamy, Jean-Mathias Griessmeier, Philippe Zarka, Louis Bondonneau**



==== LWA ====

The [[https://leo.phys.unm.edu/~lwa/|LWA]] participated with the stations LWA1 and LWA-SV with director's time in project DW005.
The schedule file [[projects:jupiter:2023-12-27_idf|DW005_231227_2230_0001.idf]] was used. It defines two tunings with 19.6 MHz bandwidth each, one centred on 16.078125000 MHz, one on 31.390625000 MHz.

**People involved: Greg Taylor, Jayce Dowell**



==== GLOW ====

The German LOFAR stations DE601,602,603,604,605,609 observed using the standard scheduling system in mode ''UDP2lanesRCU3''. They all produced data, but DE601 had strong noise and dropped out too early. They all have their own RFI. I also recorded subband statistics (SST) and beamlet statistics (BST) with 1-sec time resolution for all stations, as well as 1-sec TBB dumps with DE604 and DE605 every about 8 minutes.

Plots of the BST files (dynamic spectra) can be found {{:projects:jupiter:glow_bst.pdf|here.}}

**People involved: Olaf Wucknitz, Francesco Angelo Iraci, Sai Chaitanya Susarla, Krishnakumar Moochickal Ambalappat**


==== PL612 ====

**People involved: Tomasz Sidorowicz**


==== IE613 ====

**People involved: Joe McCauley, Corentin Louis**

==== LV614 ====

LV614 started a bit late, but also continued for a bit longer.

**People involved: Janis Steinbergs**
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