The LOFAR radio environment

A. R. Offringa (1) , A. G. de Bruyn (1) , S. Zaroubi (1) , G. van Diepen , O. Martinez-Ruby , P. Labropoulos , M. A. Brentjens (2) , B. Ciardi (3) , S. Daiboo , G. Harker , V. Jelić , S. Kazemi (4) , L. V. E. Koopmans , G. Mellema , V. N. Pandey (5) , R. F. Pizzo (2) , J. Schaye (6) , H. Vedantham , V. Veligatla , S. J. Wijnholds (2) , S. Yatawatta (1) , P. Zarka (7) , A. Alexov (2) , J. Anderson (3) , A. Asgekar (2) , M. Avruch , R. Beck (8) , M. Bell (9) , M. R. Bell (9) , M. Bentum (2) , G. Bernardi (10) , P. Best (11) , L. Birzan (6) , A. Bonafede (12) , F. Breitling (13) , J. W. Broderick (9) , M. Brüggen (12) , H. Butcher (2) , J. Conway , M. de Vos , R. J. Dettmar (14) , J. Eisloeffel , H. Falcke (2, 15, 16) , R. Fender (9) , W. Frieswijk (2) , M. Gerbers (2) , Jean-Mathias Griessmeier (2, 17) , A. W. Gunst (2) , T. E. Hassall (18) , G. Heald (2) , J. Hessels (19) , M. Hoeft (20) , A. Horneffer (3) , A. Karastergiou (21) , V. Kondratiev (2) , Y. Koopman , M. Kuniyoshi (15) , G. Kuper (2) , P. Maat (2) , G. Mann (13) , J. Mckean (2) , H. Meulman (2) , M. Mevius (2) , J. D. Mol (22) , R. Nijboer , J. Noordam (2) , M. Norden , H. Paas (23) , M. Pandey , R. Pizzo (2) , A. Polatidis (2) , D. Rafferty (24) , S. Rawlings (25) , W. Reich (15) , H. J. A. Röttgering (6) , A. P. Schoenmakers (2) , J. Sluman (2) , O. Smirnov (26) , C. Sobey (15) , B. Stappers (18) , M. Steinmetz (13) , J. Swinbank (27) , Michel Tagger (17) , Y. Tang (2) , C. Tasse (7) , A. van Ardenne , W. van Cappellen (28) , A. P. van Duin , M. van Haarlem (2) , J. van Leeuwen (19) , R. J. van Weeren (2) , R. Vermeulen (2) , C. Vocks , R. A. M. J. Wijers (27) , M. Wise (27, 2) , O. Wucknitz (29)

1 Kapteyn Astronomical Institute [Groningen]
2 ASTRON - Netherlands Institute for Radio Astronomy
3 Max Planck Institute for Astrophysics
4 Department of process and energy
5 NRAO - National Radio Astronomy Observatory [Charlottesville]
6 Leiden Observatory [Leiden]
7 Observatoire de Paris
8 LCPM - Laboratoire de Chimie Physique Moléculaire
9 University of Southampton
10 CfA - Harvard-Smithsonian Center for Astrophysics
11 Edin. - University of Edinburgh
12 Jacobs University = Constructor University [Bremen]
13 AIP - Leibniz-Institut für Astrophysik Potsdam
14 Astronomisches Institut der Ruhr-Universität Bochum
15 MPIFR - Max-Planck-Institut für Radioastronomie
16 Radboud University [Nijmegen]
17 LPC2E - Laboratoire de Physique et Chimie de l'Environnement et de l'Espace
18 Jodrell Bank Centre for Astrophysics
19 UvA - University of Amsterdam [Amsterdam] = Universiteit van Amsterdam
20 TLS - Thüringer Landessternwarte Tautenburg
21 Oxford Astrophysics
22 Center for Agricultural Research in Suriname CELOS and Department of Biology
23 Center for Information Technology CIT
24 Department of Astronomy and Astrophysics [PennState]
25 Oxford Astrophysics
26 Rhodes University, Grahamstown
27 AI PANNEKOEK - Astronomical Institute Anton Pannekoek
28 Department of Reproduction and Development
29 AlfA - Argelander-Institut für Astronomie

Aims: This paper discusses the spectral occupancy for performing radio astronomy with the Low-Frequency Array (LOFAR), with a focus on imaging observations. Methods: We have analysed the radio-frequency interference (RFI) situation in two 24-h surveys with Dutch LOFAR stations, covering 30-78 MHz with low-band antennas and 115-163 MHz with high-band antennas. This is a subset of the full frequency range of LOFAR. The surveys have been observed with a 0.76 kHz / 1 s resolution. Results: We measured the RFI occupancy in the low and high frequency sets to be 1.8% and 3.2% respectively. These values are found to be representative values for the LOFAR radio environment. Between day and night, there is no significant difference in the radio environment. We find that lowering the current observational time and frequency resolutions of LOFAR results in a slight loss of flagging accuracy. At LOFAR's nominal resolution of 0.76 kHz and 1 s, the false-positives rate is about 0.5%. This rate increases approximately linearly when decreasing the data frequency resolution. Conclusions: Currently, by using an automated RFI detection strategy, the LOFAR radio environment poses no perceivable problems for sensitive observing. It remains to be seen if this is still true for very deep observations that integrate over tens of nights, but the situation looks promising. Reasons for the low impact of RFI are the high spectral and time resolution of LOFAR; accurate detection methods; strong filters and high receiver linearity; and the proximity of the antennas to the ground. We discuss some strategies that can be used once low-level RFI starts to become apparent. It is important that the frequency range of LOFAR remains free of broadband interference, such as DAB stations and windmills.

Mots clés: Instrumentation: interferometers - Methods: data analysis - Techniques: interferometric - Telescopes - Radio continuum: general

Domaines: Planète et Univers [physics]

A. R. Offringa, A. G. de Bruyn, S. Zaroubi, G. van Diepen, O. Martinez-Ruby, et al.. The LOFAR radio environment. Astronomy and Astrophysics - A&A, 2013, 549, 15 p. ⟨10.1051/0004-6361/201220293⟩. ⟨insu-01289809⟩