Abstract. We present the final data release of the high sensitivity λ 21-cm neutral hydrogen survey of the sky south of δ ≤ −25• . A total of 50 980 positions lying on a galactic coordinate grid with points spaced by (∆l, ∆b) = (0.• 5/cos b, 0.• 5) were observed with the 30-m dish of the Instituto Argentino de Radioastronomía (IAR). The angular resolution of the survey is HPBW = 0.• 5 and the velocity coverage spans the interval −450 km s −1 to +400 km s −1 (LSR). The velocity resolution is 1.27 km s −1 and the final rms noise of the entire database is 0.07 K. The data are corrected for stray radiation and converted to brightness temperatures.

Abstract. This paper reports on a high sensitivity λ 21-cm neutral hydrogen survey of the sky south of δ ≤ −25• . A total of 50980 positions lying on a galactic coordinate grid with points spaced by ( l, b) = (0.• 5/cos b, 0.• 5), were observed with the 30 m dish of the Instituto Argentino de Radioastronomía (IAR). The angular resolution of the survey is HPBW = 30 , and the velocity coverage spans the interval −450 km s −1 to +400 km s −1 (LSR). The velocity resolution is 1.27 km s −1 and the final rms noise of the entire database is ∼ 0.07 K. The brightness temperature scale is accurate to 5%.

Abstract. We describe the equipment, observational method and reduction procedure of an absolutely calibrated radio continuum survey of the South Celestial Hemisphere at a frequency of 1420 MHz. These observations cover the area 0 h ≤ RA ≤ 24 h for declinations less than −10• . The sensitivity is about 50 mK TB (full beam brightness) and the angular resolution (HP BW ) is 35. 4, which matches the existing northern sky survey at the same frequency.

We present briefly the LLAMA sub-mm radiotelescope, a joint project of Argentina and Brazil, being mounted in the Andes, Argentina, at 4800 m altitude. Here we focus on the activities that are going on mostly under the responsibility of Brazil, like the high frequency receivers, parts of the back-end and electronics, the optical system of the telescope to bring the radiation to the receivers, the equipment needed for the integration and verification phase (optical telescope and holography) and the computation system.The main scientific applications that are planned are dscribed. We also report on a joint program with BRICS countries approved in 2019, which will involve the use of LLAMA for testing high-frequency receivers.

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