No abstract

No abstract

42The Rosetta flyby geometry at Lutetia on 10 July 2010 was suboptimal 43 because of the large flyby distance d=3168 +/-7.5 km, the high relative 46 Frequency Prediction 47The received carrier frequency from the actual flyby is compared with a 61The frequency prediction is routinely computed for radio science data 151The Doppler contributions from the HGA slew are evident in Figure 2b. 152The increase in frequency shortly before closest approach contrasts 174The rotation rates and angles were provided via the spacecraft housekeeping 175 telemetry data. 177 Filtering and adjustment 178The frequency residuals in Figure 2d were filtered at an integration time 179 of 18 seconds for noise reduction. 226The error of each parameter is derived from the diagonal terms of the 227 covariance matrix. 229The value of GM from the above described fitting procedure and 230 considering further error sources is determined to be GM = (11.34 ± 2311 The SPICE Kernel ORHR_______________00109.BSP is available from ssols01.esac.esa.int for all Rosetta experiment teams and is considered as a long term planning orbit file for experimental purposes. Comparison and discussion 246The values for GM and ∆f agree within the error with the analytical of Lutetia from astrometry (Baer et al., 2011; Fienga et al., 2008; Fienga 258 et al., 2010; Folkner et al., 2009 decreased by little more than a factor of 2. 294The volume leads to a bulk density of (3.4 ± 0.

No abstract

No abstract