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ICARUS 14,187-191(1971)MicrowaveRadiation of Uranus and NeptuneC. Hulburt Center for Space Re.eearch, Naval Research Laboratory, Washington, D.C. 20390 Received October 7, 1970; revised October 30, 1970 Observations of Uranus and Neptune at wavelengths of 1.65, 2.7, and 6 cm further clarify their radio emission spectra and atmospheric temperatures. Measurements made at the same time of Jupiter and Mars at the I.65 and 2.7-cm wavelengths are presented.I. INTRODUCTION The weak radio radiation from Uranus and Neptune has been observed only relatively recently with the availability of improved radiometers and large radio telescopes. The radio emission of Uranus was first observed by Kellermann (1966) and that of Neptune by Kellermann and Pauliny-Toth (1966).
Since then, several additional observations have been reported (Klein and Seling, 1966; Berge, 1968; Gerard, 1969; Pauliny-Toth and Kellermann, 1970). These observations showed the radio brightness temperatures of both planets to be much higher than the predicted equilibrium temperatures from solar heating, and suggested the possibility of maxima in the brightness temperature spectra near 2-cm wavelength. The observations presented here were made in 1969 at the 1.65cm wavelength and in 1968 (except Neptune), 1969, and 1970 (except Mars) at the 2.7-cm wavelength using the 85-ft reflector at the Naval Research Laboratory, Maryland Point Observatory and wide-bandwidth tunnel diode radiometers, and in 1970 at the 6-cm wavelength using the 140-ft reflector at the National Radio Astronomy Observatory1 and the NRA0 cooled parametric amplifier radiometer.
The observations were made at night and in good 1 The National Radio Astronomy Observatory is operated by Associated Universities, Incorporated, under contract with the National Science Foundation. 7weather using beam-switching to minimize the effect of atmospheric fluctuations and the beam-to-beam comparison method to increase the observed signal (Kellermann and Pauliny-Toth, 1966). The tunnel-diode amplifiers at the 1.65 and 2.7-cm wavelengths had bandwidths of 2 GHz and were followed by tunnel diode detectors, video amplifiers, and coherent detectors switched synchronously with the beam-switching between oppositely, linearly-polarized beams separated by 12’ in right ascension. The noise temperatures of the radiometers were 1150°K at the 1.65-cm and 750°K at the 2.7-cm wavelength, and the rms fluctuations in the radiometer outputs with a lo-second time constant were 0.02”K and 0.015”K respectively.
The corresponding signal-to-noise ratios were approximately 4.5 and 2 for Uranus at the 1.65- and 2.7-cm wavelengths and 1.3 and 1 for Neptune with 10 seconds integration time. The signal-to-noise ratio for Mars varied over the period of observations from 3 to 43 at 1.65 cm and from 2 to 37 at 2.7 cm. The observations at 1.65- and 2.7cm wavelengths were made by integrating the source radiation for 1.3 minute intervals alternating between the two beams. A noise tube calibration signal was applied after a set of five comparisons. The data set was reduced by differencing the responses of one beam with the average of the two adjacent alternate beam responses to compensate for linear base level changes, and taking the ratio of the average of the I 87188C.
MCCUL&OUC)Hfive source differences to the calibration signal difference for normalization of radiometer gain. Several data sets were taken around the meridian each night, and observing periods were spaced far enough that the planets had moved in the sky by more than several beamwidths. An additional check for background radiation confusion of the weak radiation from Neptune at the 2.7-cm wavelength was made by re-observing the position of Neptune after Neptune had moved to another part of the sky and gave negative results. The pointing corrections were determined from Jupiter which was near Uranus in the sky and Mars which was near Neptune during 1969. The cooled-parametric amplifier radiometer at the 6-cm wavelength had a bandwidth of 200 MHz and a system noise temperature of 130°K.
The rms fluctuation in the radiometer output with a 10 second time constant was 0.006”K and the corresponding signal-to-noise ratios were approximately 4 for Uranus and 1.5 for Neptune. The radiometer input was switched between oppositely, linearlypolarized beams separated by 1515 in declination. The observing method was similar to that used for the shorter wavelengths except that ten one-minute integrations were accumulated in a set. In order to correct for background radiation confusion, the measurements were repeated at the same positions a month later when Uranus and Neptune had moved by more than a beamwidth in the sky and the observed small background responses were subtracted from the responses for Uranus and Neptune. The pointing of the telescope was calibrated using Jupiter and radio sources with accurately known positions.
The measurements were calibrated against the standard source Virgo A which was near Jupiter and Uranus in the sky and which was observed with the same technique but fewer integrations. The 6-cm peak flux density for Virgo A of 65.75 rt 0.6 x 1O-26 W mm2 Hz-l given by Pauliny-Toth and Kellermann (1968) for the 140-ft reflector beam was used. For the shorter wavelengths, a linear fit to the logarithmic flux density spectrum forVirgo A was found using the flux densities at 2.7 and 5 GHz from Kellermann, Pauliny-Toth, and Williams (1969), at 8.25 and 15.45 GHz from Allen, Barrett and Crowther (1968), at 8 and 14.5 GHz from Baars, Mezger, and Wendker (1965), and at 20.5, 23.7, 25.5, and 35.5 GHz from Welch (Dr. Welch, private communication). The flux density from this spectrum at the 2.7-cm wavelength was 38.5 x 1O-26 W rnw2 Hz-l, and at the 1.65-cm wavelength was 26 x 10Az6 W mm2 Hz-l. These flux densities were corrected for the finite size of the source in the reflector beam using corrections derived from the observed beam broadening in both principal planes of 1.06 at the 1.65-cm and 1.03 at the 2.7-cm wavelength and the assumption of a gaussian brightness distribution. The corrected peak flux densities for Virgo A in the reflector beam at the 2.7- and 1.65cm wavelengths were 36.2 x 1O-26 W rnw2Hz-l and 23.1 x 1O-26 W mm2 Hz-l.
The uncertainty in the calibration of the planetary flux was estimated to be 5.5% at the 6-cm wavelength, 6.5% at 2.7 cm, and 7% at 1.65 cm. The flux densities observed by this method using two oppositely-polarized beams are independent of linear polarization of the radiation if the gains of the two was beams are equal. This condition satisfied at the 6-cm wavelength where the beams were oriented symmetrically with respect to the reflector axis. At the shorter wavelengths, where one beam was aligned with the reflector axis while the other was off-axis resulting in a lower gain for the off-axis beam (15% less at 2.7 and 25% less at 1.65 cm), the possible error due to source linear polarization was not eliminated but was effectively reduced. The resultant error in the calibrations using Virgo A is less than 1%.
The observed flux densities for the planets were corrected for differential atmospheric absorption and reflector efficiency between the pointing directions for the planets and for the calibration source Virgo A using the experimentally determined dependence of these quantities on zenith angle. The corrections determined by Pauliny-Toth and Kellermann (1968)URABNTJS AND NEPTUNERADIO EMISSION were used for the observations at the 6-cm wavelength, and corrections determined at Maryland Point during these and other observations where used at the 1.65- and 2.7-cm wavelengths. Since Virgo A, Uranus, and Jupiter were near each other in the sky at the time of the observations, the differential corrections were small for these planets and contributed an uncertainty estimated at less than 1% to the measurements of these planets. Neptune and Mars were at lower declination and the uncertainties in the differential corrections added an uncertainty estimated at less than 2% to the measured flux densities of these planets at the 1.65-cm wavelength and of less than 1% for Neptune and Mars at the 2.7-cm wavelength and for Neptune at the 6-cm wavelength.II. RESULTS The measured flux densities varied with the apparent diameters of the planets over the time covered by the observations. Representative values in units of 1O-26 W m-’ Hz-l are: At 1.65 cm, Jupiter 31 to 43, Mars 1 to 12.4, Uranus 0.5, Neptune 0.2; at 2.7 cm, Jupiter 13.5 to 22.6, Mars 0.24 to 4.5, Uranus 0.22, Neptune 0.09; at 6 cm, Uranus 0.046, Neptune 0.018.
The brightness temperatures of the planets were derived from the observed flux densities using solid angles calculated from the semidiameters tabulated in the American Ephemeris and Nautical Almanac, except for Neptune where the ephemeris values were corrected to be consistent with the smaller diameter recently determined from occultation measurements by Taylor (1970) and Bixby and van Flandern ( 1969). The diameter for Neptune from the American Ephemeris and Nautical Almanac was corrected by a factor of 0.945. The observed brightness temperatures are listed in Table I where the values for Mars have been adjusted to mean solar distance assuming T cc (,/r)l/. The results of the different nights of observation were averaged with greater weight given to nights with smaller scatter and to the189TABLE I OBSERVED PLANETARY BRIGHTNESS TEMPERATURES Wavelength Jupiter Mel-8 Uranus NeptuneI.65cm 165 f 196 & 201 f 194 f12 16 16 242.7cm 201 186 212 225i & f f13 12 16 206cm210 & 17 227 f 23observations of Mars at the times of high flux density, although the results at the times of low flux density agreed well. The averages for Uranus and Neptune included more than 70 minutes of integration on each beam.
The measurement errors were estimated from the scatter of the observations and were higher than predicted from the signal-to-noise ratio; the additional scatter presumably being introduced by such factors at atmospheric fluctuations and possibly small errors in telescope pointing. The measurement errors were combined quadratically with the calibration errors to give the mean errors listed in Table I. The measured brightness temperatures for Jupiter and Mars agree well with recent observations at nearby wavelengths, and for Mars are reasonably consistent with the expected average temperature over the planet from solar heating, when estimates of the surface emissivity are applied. The measurements of Mars are not sufficiently comprehensive to define a systematic dependence of brightness temperature on the phase of solar illumination or on the longitude of the central meridian, but are compatible with such systematic effects of up to a few percent. The brightness temperatures for Uranus and Neptune at the 1.65-, 2.7-, and 6-cm wavelengths are all near the high level observed previously at 2-cm wavelength by Kellermann and Pauliny-Toth.
The new measurements are compared in Fig. 1 with the measurements at 0.35-, 0.95-, and 1.95cm wavelength (Pauliny-Toth and Kellermann, 1970, at 3.12 cm (Berge, 1968), at 3.75 cm (Klein and Seling, 1966),190C. ICICCULLOUOH300URANUSI0B e co300-200-IIINEPTUNEloo-f00.1IIII0.31.03.010.0WAVELENGTH30.0(CM)Fm.
Brightness temperature spectra of Uranus and Neptune. Circled data points are measurements from this paper. References for the other data points are given in the text.at 11 cm (Kellermann, 1966) and at 11 cm (Gerard, 1969). The brightness temperatures for Neptune reported by PaulinyToth and Kellermann are computed using the new smaller diameter for Neptune as were those in this paper.
The brightness temperature at 3.12 cm reported by Berge was computed for the ephemeris diameter but was corrected by us to correspond with the new diameter for comparison with the other observations. The standard error bars include both measurement scatter and calibration error.
The new measurements appear to disagree significantly with the interferometer observations of both Uranus and Neptune at 3.12-cm and the single dish measurement of Uranus at 3.75-cm wavelength. The discrepancy may be due at least in part to differences in absolute calibration between observers. If further measurements confirm the discrepancies, a spectral feature in common with both planetary atmospheres may be indicated.
The measurements of the radio radiation from Uranus and Neptune now define the gross features of their spectra. The general form of increasing radio brightness temperature with increasing wavelength from temperatures near the predicted equilibrium temperatures at short millimeter wavelengths is in common with theother planets with extensive atmospheres, Venus, Jupiter, and Saturn. This is the qualitatively expected form of spectrum for a planet for which the atmospheric transmission increases with wavelength and the atmospheric temperature increases with depth beneath the visible cloud surface. The present spectra for Ura.nus and Neptune interpreted as atmospheric thermal radiation imply an increasing atmospheric transmission from 3-mm to at least 3-cm wavelength and a temperature increase with depth in the atmosphere to a temperature near 200’K. The present spectra do not support the suggestion from previous observations of a maximum near the ammonia inversion spectrum at 1.25cm wavelength. ACKNOWLEDGMENTS We wish to thank J. Boland for his assistance with the apparatus and observations at Maryland Point, S.
Mango for preparing ephemerides, Professor W. Welch for use of his data prior to publication, Dr.
Kellermann and Dr. Pauliny-Toth for helpful discussions and use of their data prior to publication, and the staff of the National Radio Astronomy Observatory for their assistance and for providing the excellent apparatus at Green Bank.URANUS AND NEPTUNE RADIO EMISSION191emission from Mercury, Venus, Mars, Saturn, and Uranus. I., ANDPAULINY-TOTH, I.
J., BARRE=, A. H., AND CROWTHER, KELTZRMANN, (1966). Observations of the radio emission of P. Observationsof the radio sources Uranus, Neptune, and other planets at 1.9 cm. 3C 34, 3C 273, 3C 274, and 3C 279 at short Astrophya.
M., MEZUER,P. G., ANDWENDKER, KELLERMANN,K. I., PAULINY-TOTE,I. K., ANDWILLIAMS,P. The spectra of H. The spectra of the strongest non, radio sources in the revised 3C Catalogue. Thermal radio sources in the oentimeterAstrophy& J.
Wavelength range. Recent observations of PAULINY-TOTE,I. K., AND KELLERMANN, K. Measurementsof the flux density Saturn, Uranus, and Neptune at 3.12 cm. And spectra of discrete radio sourcesat centiAetrophy8. Meter wavelengths.
The observations at BIXBY, J. E., ANDVAN FLANDERN,T.
5 GHz (6 cm). The diameter of Neptune.
K., AND KELLERMANN, GERARD, E. Observations of Saturn, PAULINY-TOTF, K. Millimeter-wavelengthmeasureUrsnus, and Neptune at 11.13 cm. Ments of Uranus and Neptune. Lett., 6, 185. J., AND SELING,T. Radio TAYLOR,G.
The occultation of B.D. Emissionfrom Ursnus at 8 Gc/s.17’4388 by Neptune on 1968 April 7. IVotices Roy. KELLERMANN, K. The thermal radio REFERENCES.
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