Medicina Radiotelescopes : Photo Gallery

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Radio image of the moon Polarized emission map of the Moon at 8300MHz. Observed by 32m parabolic antenna.

 

Quattro grafici con frangia di interferenza

 

 

For the first time interference fringes were found in a real time e-VLBI experiment involving Medicina station.

The experiment with signals roued via a fiber optic connection was conducted on March 9, 2006 at 5GHz, on source 2007+777 (extragalactic radio sources, catalogued as BLLac, redshift z=0.342)., using a bit rate of 128Mbit/s.

The plots shown the results relative to the Westerbork-Medicina baseline.

 

 

 

 

Graph with spectral lines

 

Spectral line C252a  observed on CassiopeiaA at 408.7MHz. Kelvin vs Spectrum Channels. Observed by Northern Cross.

 

 

Radio pulses

 

New millisecond pulsar discovered by Northern Cross 1999, J0030+0600 (J0030+0452) at 408MHz. Impulse period 4.86msec. More pulsars at http://pulsar.ca.astro.it/pulsar/bol_obs.html

 

 

Graph with spectral lines

 

H2O water maser line observed on W3OH (massive star forming region in the Perseus spiral arm, at a distance of 1.953 ±0.04 kpc) at 22235.079MHz. Kelvin vs Spectrum Channels. Integration time 2.1h. Observed by 32m parabolic antenna.

 

 

 

Graph with spectral lines

H2O water maser emission at 22235.079MHz coming from the impact of the Shoemaker-Levy comet and Jupiter atmosphere, 1994. Observed by the 32m parabolic antenna.

Reference: C.B. Cosmovici, S. Montebugnoli, A. Orfei, S. Pogrebenko, P. Colom

“First evidence of water maser emission induced by a catastrophic impact” Planetary and Space Science, vol. 44, No. 8, pp. 735-739,1996

 

 

Graph with spectral line and high noise superimposed

C2S spectral line observed on L1544 (core of a dense, compact pre-stellar region in Taurus) at 22234.033MHz. Kelvin vs Spectrum Channels. Integration time 3.4h. Very bad weather conditions. Observed by 32m parabolic antenna.

 

Radio map, total intensity Radio map, polarized intensity

 

5o x 5o linear polarization map of the galactic diffuse emission at 5070MHz. 80MHz bandwidth, september 2004. Pixel dimension, 8 x 8 arcmin. Integration time per pixel, 1 min. RMS noise per pixel, 1mK. Total observing time, 24h. Observed by 32m parabolic antenna.

I(mK)= total power, Q,U(mK)= Stokes components of the linear polarization, L(mK)= total linear polarization power.

 

 
Radio map, horizonthal polarization Radio map, vertical polarization

 

Graph with spectral lines

 

NH3(1,1)  spectral line observed on L483 (deeply embedded low-mass protostar) at 23694.495MHz. Kelvin vs Spectrum Channels. Integration time 691sec. Observed by 32m parabolic antenna.

 

 

 

Three graphs with spectral lines

H92a recombination line observed on three different Rosetta Nebula  positions (vast cloud of dust and gas, extending over an area of more than 1 degree across, or about 3 times the area covered by the full moon, its parts have been assigned different NGC numbers) at 8309.4MHz. Kelvin vs Spectrum Channels. Total observed time 23.5h. Observed by 32m parabolic antenna.

Reference: Tsivilev et al.,2002,New Astronomy,7,449

 
   
 

 

 

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