FDWAVE Pixels without photomultipliers removed to be installed

FDWAVE Pixels without photomultipliers (removed to be installed in HEAT (*)) 220 pixels available (not considering the columns adjacent to pmts) Use LL 1 & LL 6 to detect microwave radiation equipping the empty pixels with microwave radio receivers (*) dopo che i tedeschi avevano fatto l’ordine per HEAT 3 la Photonis ha interrotto la produzione --> usare i pmt che hanno davanti poche tanks

FDWAVE Use the standard FD trigger and readout the radio receivers every FD shower candidate Use the profile reconstructed with pmts to estimate the energy deposit seen by radio receivers LL 6 No pmts ?

OPTICS LL mirror are of aluminium kind --> good reflectivity Reflector Spherical FD Parabolic microwave telescope spherical aberration in the focus all rays have the same phase! BUT: the parabolic dish is not suitable for track imaging purposes because of the strong aberrations for inclined rays the best reflector is spherical !!!

SIGNAL / BACKGROUND 1÷ 2 Expected flux density P. W. Gorham et al. , Phys. Rew. D 78, 032007 (2008) ≈ 100 K + penalty factor (100 K? ) staying within FD building (diaphragm, …) Background bandwidth

OPTICS SIMULATION GRASP www. ticra. com Radio receivers in the camera center at 1. 657 m from the mirror ~ 7 GHz - HP=600 Auger mirror R = 3. 4 m waves only in one plane Diaphragm 2. 2 m Camera shadow ≈1 m

OPTICS SIMULATION Gain (G) with respect to isotropy emission factor 10 secondary lobes due mainly to camera shadow viewing angle

ANTENNA Conical Horn in the frequency range [9 -11] GHz (0. 70 -0. 80) connector for output signal (can be put in another position) circular aperture 42 mm (<a) support (can be removed) waveguide 24. 5 mm (<b) camera holes b=40 mm maximum aperture a=45. 6 mm Contacts with SATIMO experts to lower the frequency

TELESCOPE APERTURE aperture from Gain constant within 1% efficiency factor

SIGNAL / BACKGROUND quadratic scaling linear scaling 10 km 15 km Rate in LL 6 above 1018. 5 e. V: 50 events/year Possibility to increase I/ t > 100 ns averaging over more showers and FADC traces

FE ELECTRONIC & DAQ power detector FADC Log-power detector AD 8317 up to 10 GHz 55 d. B dyn. range amplifier ANTENNA typical signals very low I Aeff f ≈ -90 d. Bm (1 p. W) we need 50 d. B amplification with low noise to match the power detector dynamic range AMF-5 F-07100840 -08 -13 P 7. 1 -8. 4 GHz Gain 53 d. B use the FD FADCs Tnoise = 58. 7 K a trigger signal is needed radio signals will be available in a friendly format and this makes easier the access for all Auger people

quadratic scaling linear scaling 10 km 15 km

OPTIMAL WAVELENGHT pixel field of view Half Power Beam Width inserting antenna in camera holes lower limit on camera body antenna optimal 1. 50: 4. 56 cm 5 GHz 6 cm > 6. 6 GHz

RECOVERING PMT PULSE SHOWER DATA pulse of pixels close to SDP pulse of 1 pixel detecting the halo averaging over many events background dominates

6 LL 1