Class that defines the possible metadata queries specific to the CEDAR data archive. CCEDAR Metadata Service ERROR FOR Photon counts error counts -2490 ERROR FOR Potassium [K] number density error [K] -906 ERROR FOR Additional increment to neutral Vlos error vnlui -801 vnlui Additional increment to Neutral Vlos 801 Potassium [K] number density Potassium [K] number density 906 Photon counts Photon counts (per range,altitude bin) 2490 JRO W beam chisquare JRO West beam reduced chisquare 3109 JRO E beam chisq JRO East beam reduced chisquare 3110 JRO W beam chisquare JRO West beam reduced chisquare 32000 JRO E beam chisq JRO East beam reduced chisquare 32001 150 G Circ Dst Horiz great crcl dist from ref lat/lon 890 log10 (HE number density) lg([HE]) Positive One Electric Charge St. Santin data quality code 4 STS Dat QC4 469 525 lg(HtIntNe) log10 (Vert. integrated electron den.) Time Series Plot of parameter values vs time coordinate St. Santin data quality code 3 468 STS Dat QC3 467 St. Santin data quality code 2 STS Dat QC2 502 Raw Ne Uncorrected electron density 466 STS Dat QC1 St. Santin data quality code 1 DDX OPeNDAP DDX (Data descriptor in XML) data file OPeNDAP DDX (Data descriptor in XML) data file Millstone Hill data quality code 5 MLH Dat QC5 465 MLH Dat QC4 Millstone Hill data quality code 4 464 MLH Dat QC3 463 Millstone Hill data quality code 3 SBZERO sp4d_sourcefunction Radiative transfer source function Uncorrected electron density increment Raw Ne Inc 501 462 MLH Dat QC2 Millstone Hill data quality code 2 lg([H]) log10 (H number density) 900 Arecibo data quality code 5 460 ARO Dat QC5 470 STS Dat QC5 St. Santin data quality code 5 ASCII OPeNDAP Ascii Response Negative One Electric Charge 404 Pulse Len Pulse length 341 aa aa index Tab delimited data file TAB STREAM Stream binary file 522 Line integrated electron density Lin Int Ne Variation in elevation (end El-beg El) 145 El Change log10 (integrated electron density) lg(Int Ne) 523 http://www.haystack.mit.edu/homepage.html The Millstone Hill Observatory, located in Westford, Massachusetts, is a broad-based atmospheric sciences research facility owned and operated by the Massachusetts Institute of Technology. Millstone Hill IDL IDL Script Data File Beginning additional increment to hhmm 29 Beg TimeInc Zero Electric Charge Chatanika/Sondrestrom data qual code 2 472 CHT/SON QC2 Emery intersat adjust hourly composite elec Hp 175_31200 Chatinika/Sondrestrom data qual code 5 CHT/SON QC5 475 JRO Dat QC5 455 Jicamarca data quality code 4 Height vs Time A contour plot of the selected variable versus Height (Y axis) and Time (X axis) A contour plot of the selected variable versus Height (Y axis) and Time (X axis) lg(RawNmax) log10 (max uncorrected Ne in m-3) 536 The Arecibo Observatory is located in Arecibo, Puerto Rico on the north coast of the island. It is operated by Cornell University under cooperative agreement with the National Science Foundation. The observatory works as the National Astronomy and Ionosphere Center (NAIC) although both names are officially used to refer to it. The observatory's radio telescope is the largest single-aperture telescope ever to be constructed. (Compare "multiple aperture telescope".) It collects radio astronomy, terrestrial aeronomy, and planetary radar data for scientists around the world. Usage of the telescope is gained by submitting proposals to an independent board of referees. Although it has been given many usages, the observatory's main purpose is to detail and observe stellar objects. Arecibo http://www.naic.edu/ http://en.wikipedia.org/wiki/Arecibo_Observatory EISCAT data quality code 2 EIS Dat QC2 477 EIS Dat QC3 478 EISCAT data quality code 3 EISCAT data quality code 4 479 EIS Dat QC4 DAS OPeNDAP DAS (Data Attribute Structure) data file OPeNDAP NetCDF Data Return NetCDF Local solar time at conjugate point 47 SLT@Conj INFO OPeNDAP information data file lg([AR]) log10 (AR number density) 880 Positive Electric Charge SP4D_StokesI StokesI Stokes I Polarization Parameter F10.7 solar flux qualifier observed 355 F10.7q 354 F10.7 Obs F10.7 solar flux observed (Ottawa) OPeNDAP data file OPeNDAP 356 Avg Typ 356's avg code: 1=>81day ; 2=13mon 357 Peach Mountain is the home of the 24 inches McMath Telescope and is part of Stinchfield Woods. Stinchfield Woods is owned by the University of Michigan and used by several university departments including the Astronomy Department and the School of Natural Resources and Environment. http://www.umich.edu/~lowbrows/theclub/mcmath.html Peach Mountain F10.7a F10.7 Multiday average observed 356 Ne Inc 511 Additional increment to code 510 (Ne) 66 Time increment between rows DT rows FLAT Flat space-delimited data file Precision Solar Photometric Telescope H PSPT_MLSO 480 EIS Dat QC5 EISCAT data quality code 5 135 Variation in azimuth (end Az - beg Az) Az Change OPeNDAP DDS (Data Descriptor Structure) data file DDS Negative Electric Charge 531 Max Raw Ne Maximum uncorrected electron density Poker Flat Alaska MST Radar Vn hrly aves, vertical beam PKR QC Avg of Galactic Noise 4003 PF Gal Nois lg(S/N) log10 (signal to noise ratio) 412 ERROR FOR PKR QC Avg of Galactic Noise error PF Gal Nois -4003 Vnlos Line of sight neutral vel (pos = away) 803 Pulse Len 402 Pulse length ERROR FOR PKR QC log10 (signl pwr in spectrm) error lg(SgnlPwr) -4005 1140_20003 PF NR Noise PKR QC No records in noise avg 4002 415 Smpl Tm Usd No smpls in time avg; or 414 incremnt error Vnlos -803 ERROR FOR Line of sight neutral vel (pos = away) -4004 ERROR FOR PKR QC log10 (noise pwr in spectrm) error lg(NoisPwr) 4004 lg(NoisPwr) PKR QC log10 (noise pwr in spectrm) No samples available in time average 413 Smpl T Aval Altitude Altitude (height) 110 Elevation angle (0=horizontal,90=vert) 140 El lg(SgnlPwr) PKR QC log10 (signl pwr in spectrm) 4005 111 Alt Inc Additional increment to altitude PFQC 4001 PKR QC 0=Okay -806 error Vn Spread ERROR FOR Neutral velocity spread error lg(S/N) ERROR FOR log10 (signal to noise ratio) -412 Az Mean azimuth angle (0=geog N,90=east) 130 Vn Spread Neutral velocity spread 806 Vn hrly aves, combined E/N winds Vn2 Direction 2 Neutral wind (northward) 1422 ERROR FOR Direction 2 Neutral wind (northward) -1422 error Vn2 ERROR FOR Direction 1 Neutral wind (eastward) -1412 error Vn1 1140_20004 1412 Direction 1 Neutral wind (eastward) Vn1 1140 http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:pkr PKR The Poker Flat MST radar was located at the Poker Flat Rocket range about 200 m above mean sea level in Alaska at (65.13N, 145.46W), and operated between 1979 and 1987. The last 2 years are not in the CEDAR Data Base. The inclination angle is about 77 degrees, and the declination is about 29 degrees to the east of north. The Poker Flat radar was a high power radar, with three narrow beams. One beam looked vertically (kindat=20003) and the other two were inclined at 15 degrees to vertical, or at an elevation angle of 75 degrees. The 'east' beam had an azimuth 26 degrees north of east (kindat=20001) while the 'north' beam had an azimuth 26 degrees west of north (kindat=20002). Most of the data were taken using all three beams but some, especially in the early days, were taken with only the vertical beam or with only the oblique beams. During an experiment one or more beams were sometimes inactivated. The cycle time for a complete set of vertical and oblique records seldom exceeded 10 min and was typically 1 min. When available, velocity measurements from the two oblique beams were combined to give eastward and northward components of the neutral wind (kindat=20004). The velocity spread is twice the square root of the second moment of the power spectrum and is a measure of shear or turbulence in the measurement volume. Data quality below 5 km is definitely dubious and below 8 km should be treated with suspicion due to recovery problems. The more obviously false data have been removed from this data set but consistently false data are hard to distinguish from the real thing and may be included. The original Poker Flat data set has been subjected to an extensive set of checks to remove various interference modes, outliers and otherwise non-atmoshperic data. The parameters for the remaining data have been averaged for all appropriate records that commenced within a one hour interval. Note that these are averages of the derived parameters and not parameters derived from an average velocity spectrum. In the absence of any signal echo the main contribution to noise is the radio noise from our galaxy. Hence there is a siderial variation (of about 4 db) in the noise level. Atmospheric absorption events reduce the level of noise. Receiver gain and cable attenuation fluctuations may have a small influence. Operator modification of gain controls are rare. Strong signals can corrupt the computation through their sidelobes. The errors given are the root mean square values of the deviation from the mean for that hour. ERROR FOR Neutral velocity spread -805 error Vn Spread -802 error Vnlos ERROR FOR Line of sight neutral vel (pos = away) Vn hrly aves, north beam Vn Spread Neutral velocity spread 805 1140_20002 Vnlos Line of sight neutral vel (pos = away) 802 1140_20001 Vn hrly aves, east beam CEDAR http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:arm Arecibo P.R. MST Radar Tsys System temperature 482 1040_2002 407 IPP Interpulse Period 484 Cal Temp Calibration temperature Cod baud l Code baud length 431 No samples used in Fourier transform 417 N Smpl/FFT No incoherent integrations 434 N Inc Int Reduced-chi square of fit Chi Sqr 420 Cod baud n 432 No. bauds in code 433 Cod type Code type (0=non,1=cmplmntry) Vn Transmitted frequency 490 Xmit Freq 1040 ARM The ST (strato/troposphere) radar at the National Astronomy and Ionosphere Center (NAIC) at Arecibo, Puerto Rico (18.3N, 66.75W), made measurements during the AIDA (Arecibo Initiative in Dynamics of the Atmosphere) campaign of March-May, 1989, an international multi-instrument campaign which was conducted to compare wind measurements in the mesosphere taken by various radar and optical devices. The tropo- and stratosphere data taken by the Arecibo ST radar during this period were largely decoupled from the main objectives and the observations of the other instruments. Data are available for both day and night times. Integration time per profile varies and is on the order of 30 sec to 1 min. However, because the mesosphere observations were interleaved with this data set, there are many gaps between profiles on the order of a few minutes. During AIDA, the altitude range sampled was from about 5 to 20 km, and the resolution was about 0.3 km. For this data set, the antenna azimuth scan pattern was very roughly as follows: 1.5 hrs at 14 or 32 deg, 10 min at -76 or -58 deg, 10 min at 194 or 212 deg, 30 min at 104 or 122 deg, 10 min at 194 or 212 deg, and 10 min at -76 or -58 deg, then repeat. Beware that the times do appear to vary. Elevation angle was fixed at about 79 degrees. Results from AIDA have been published in J. Atmos. Terr. Phys., 55, 1993, a special issue dedicated to the campaign. H. Mario Ierkic was responsible for the operation of the Arecibo ST radar during AIDA, and John Cho put this data set into the CEDAR Data Base. This program extracts the following data from the Doppler spectra of the Arecibo ST radar: (1) Line-of-sight velocity of the clear air, (2) signal spectral width, and (3) SNR. Item (1) is self-explanatory. Items (2) and (3) yield information about the actual radar scattering mechanism. If the mechanism is turbulence, then (1) and (3) yield the turbulence intensity. For further information see Gage and Balsley [1980]. MLH33 The incoherent scatter transmitter station at Millstone Hill, Massachusetts (42.6N, 71.5W) has been in operation since 1960. The facility is part of and operated by the Massachusetts Institute of Technology. ISR data comes from the fixed zenith antenna, the steerable antenna, or both. The electron densities from the power profile were calibrated with an on-site ionosonde, where recently, this ionosonde has been the University of Massachusetts at Lowell digisonde. Since the Coast Guard uses some of the frequencies needed to properly scan the ionosphere, calibration can sometimes be difficult. The calibrated electron density is then corrected for Te and Ti effects, where Te and Ti come from auto-correlation fits. The calibration and auto-correlation fits now have the same height resolution, although in the past, the auto-correlation fits had lower height resolution. The ion composition changes from mostly O2+ and NO+ at lower altitudes, to mostly O+, and then to H+ and some He+ at higher altitudes. Above 400 km, the percent H+ is computed along with the major ion O+. At lower altitudes, the ratio of molecular ions to the total number of ions is modeled as specified by the FORTRAN code segment below. REAL FUNCTION PMF(Z) Z1=AMIN1(-(Z-120.)/40.,50.) H=10.-6.*EXP(Z1) Z2=AMIN1(-(Z-180.)/H, 50.) Millstone Hill: steerable L-band ant. 33 http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:mlh 24-h northwrd neutral wind amplitude 24h Vnn Amp 941 12-h max northward neutrl wind phase 956 12h Vne Phs 24h Vne Phs 24-h max eastward neutral wind phase 945 error 12h Vnu Phs ERROR FOR 12-h max upward neutral wind phase -989 12-h upward neutral wind amplitude 12h Vnu Amp 985 error 12h Vne Phs -955 ERROR FOR 12-h max eastward neutral wind phase 24-h max northwrd neutral wind phase 946 24h Vnn Phs Day No Day number of year (universal time) 21 935 Mean eastward neutral wind Mean Vne error Mean Vne ERROR FOR Mean eastward neutral wind -935 Mean upward neutral wind 934 Mean Vnu ERROR FOR Mean northward neutral wind error Mean Vnn -936 Vn tides 4-day CEDAR/TIMED analysis 12-h northward neutrl wind amplitude 12h Vnn Amp 951 -950 error 12h Vne Amp ERROR FOR 12-h eastward neutral wind amplitude 24h Vnu Phs 987 24-h max upward neutral wind phase 989 12h Vnu Phs 12-h max upward neutral wind phase Integration time for these data 62 Int Time Mean northward neutral wind 936 Mean Vnn Reference geodetic longitude 156 Ref Gd Lon 926 Eastwd Residual Sqrt[1/N*sum(ui-uf)**2] Vne resid 12h Vne Amp 12-h eastward neutral wind amplitude 950 Reference geod latitude (N hemi=pos) Ref Gd Lat 153 ERROR FOR 24-h northwrd neutral wind amplitude error 24h Vnn Amp -941 ERROR FOR 24-h max eastward neutral wind phase -945 error 24h Vne Phs error 12h Vnu Amp -985 ERROR FOR 12-h upward neutral wind amplitude 1750_17100 -951 error 12h Vnn Amp ERROR FOR 12-h northward neutrl wind amplitude 940 24h Vne Amp 24-h eastward neutral wind amplitude 12-h max eastward neutral wind phase 955 12h Vne Phs 984 24h Vnu Amp 24-h upward neutral wind amplitude error 12h Vne Phs ERROR FOR 12-h max northward neutrl wind phase -956 927 Vnn resid Northwd Residual Sqrt[1/N*sum(vi-vf)**2] Vnu resid Upwd Residual Sqrt[1/N*sum(wi-wf)**2] 928 Number of hours filled in harm anal 925 No hr filld error Mean Vnu -934 ERROR FOR Mean upward neutral wind ERROR FOR 24-h max upward neutral wind phase -987 error 24h Vnu Phs error 24h Vne Amp ERROR FOR 24-h eastward neutral wind amplitude -940 42 Local solar time diff (=SLT-UT) +E lon SLT-UT error 24h Vnn Phs -946 ERROR FOR 24-h max northwrd neutral wind phase -984 error 24h Vnu Amp ERROR FOR 24-h upward neutral wind amplitude The Obninsk, Russia (55.11N, 36.51E; ~172 m above msl) 33.3 MHz meteor radar has been in operation since 1964. On day 359 of 2001 at 89 km altitude, the apex magnetic coordinates were (51.2, 111.0) degrees. The magnetic inclination and declination angles were 70.5 deg and 8.3 deg. The magnetic local time at 0 Universal Time (UT) is about 0219 MLT. The solar local time (SLT) is UT plus 2 hours and 26 minutes (36.51/15=2.434). With no height ranging, the observations come approximately from 95 km. Obninsk Russia Meteor Wind Radar OBN 1750 http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:mltr MLH31 121 Range Inc Additional increment to range ERROR FOR Electron temperature -560 error Te Nu Ne Ni Te Ti Tr Vi error [H+]/Ne ERROR FOR Ion Composition - [H+]/Ne -660 3318 Power NrmK MLH D.P. Power Normalization constant -550 error Ti ERROR FOR Ion temperature 411 S/N Signal to noise ratio Ion Composition - [H+]/Ne 660 [H+]/Ne Beg El 142 Beginning elevation angle 3303 NNSAMP MLH Number of noise samples in profile NRSWP MLH Number of Radar Sweeps for Record 3308 Ti 550 Ion temperature 170 Geodetic longitude of measurement Geod Lon Beginning azimuth (0=geog N,90=east) Beg Az 132 PNRMMP MLH Mean power prof Normalizatn Const 3310 MLH Mode Letter (65-80 = A-P) 3300 MLH Mode ERROR FOR log10 (Ne in m-3) error lg(Ne) -520 3319 Additnl P. MLH Additional increment to DP Pwr Nrm C lg(Ne) 520 log10 (Ne in m-3) Ending elevation angle End El 143 MLH Number profile Noise level samples 3306 NPNSWP Geod Lat Geodetic latitude of measurement 160 error Vilos -580 ERROR FOR Line of sight ion velocity (pos = away) 3309 NNRSWP MLH Number noise gates in radar sweep -505 error lg(RawNe) ERROR FOR log10 (uncorrected electron density) 133 End Az Ending azimuth (0=geog N,90=east) 31_3304 NCSAMP 3304 MLH Number calibration samples in prof Peak Power Peak power 486 560 Te Electron temperature -570 error Te/Ti ERROR FOR Temperature ratio (Te/Ti) Vilos 580 Line of sight ion velocity (pos = away) log10 (uncorrected electron density) 505 lg(RawNe) Range Range 120 570 Temperature ratio (Te/Ti) Te/Ti 3302 NRP MLH Number of signal samples in profile The incoherent scatter transmitter station at Millstone Hill, Massachusetts (42.6N, 71.5W) has been in operation since 1960. The facility is part of and operated by the Massachusetts Institute of Technology. ISR data comes from the fixed zenith antenna, the steerable antenna, or both. The electron densities from the power profile were calibrated with an on-site ionosonde, where recently, this ionosonde has been the University of Massachusetts at Lowell digisonde. Since the Coast Guard uses some of the frequencies needed to properly scan the ionosphere, calibration can sometimes be difficult. The calibrated electron density is then corrected for Te and Ti effects, where Te and Ti come from auto-correlation fits. The calibration and auto-correlation fits now have the same height resolution, although in the past, the auto-correlation fits had lower height resolution. The ion composition changes from mostly O2+ and NO+ at lower altitudes, to mostly O+, and then to H+ and some He+ at higher altitudes. Above 400 km, the percent H+ is computed along with the major ion O+. At lower altitudes, the ratio of molecular ions to the total number of ions is modeled as specified by the FORTRAN code segment below. REAL FUNCTION PMF(Z) Z1=AMIN1(-(Z-120.)/40.,50.) H=10.-6.*EXP(Z1) Z2=AMIN1(-(Z-180.)/H, 50.) 426 Additional increment to wide chi square Wide ChiSqi error Col Freq -710 ERROR FOR Ion-neutral collision frequency error Vilos Inc ERROR FOR Additional increment to code 580 -581 95 Cyc No Cycle sequence number (e.g., 5th cycle) Position number within cycle 96 Pos No MLH par 54 MLH parameter 54 3353 -3313 error ACF Norm ERROR FOR MLH ACF Normalization Factor 581 Additional increment to code 580 Vilos Inc 3324 MLH par 25 MLH parameter 25 Scan Type Scan type (0=any,1=fixed,2=az,3=el) 94 3325 MLH par 26 MLH parameter 26 Wide Chi Sq Wide reduced-chi square of fit 425 -3352 error MLH par 53 ERROR FOR MLH parameter 53 -690 error [N-0]/Ne ERROR FOR Ion Composition - [mol wt 28 to 32]/Ne 461 MLH Dat QC1 Millstone Hill data quality code 1 error Dopp Vel -3350 ERROR FOR MLH Line of sight Doppler V(pos = away) MLH parameter 52 3351 MLH par 52 MLH parameter 29 MLH par 29 3328 MLH parameter 53 3352 MLH par 53 MLH parameter 30 3329 MLH par 30 -3320 error MLH par 21 ERROR FOR MLH parameter 21 Col Freq Ion-neutral collision frequency 710 MLH parameter 24 MLH par 24 3323 3313 ACF Norm MLH ACF Normalization Factor Goodness of fit Goodnes Fit 430 Ion Composition - [mol wt 28 to 32]/Ne 690 [N-0]/Ne 3346 MLH lag MLH Lag spacing ERROR FOR MLH parameter 52 -3351 error MLH par 52 31_3410 3350 Dopp Vel MLH Line of sight Doppler V(pos = away) Nu Ni Ti Tr Vi MIDAS-W anal MLH parameter 23 3322 MLH par 23 Tsys Inc 483 Additional increment to system temp 3320 MLH par 21 MLH parameter 21 3321 MLH par 22 MLH parameter 22 MLH par 6 MLH parameter 6 3305 500 Raw Ne Uncorrected electron density (Te/Ti=1) 31_3001 MLH par 8 3307 MLH parameter 8 Power NrmK MLH Power Normalization constant 3301 Nu Ne Te Ti Tr Vi Millstone Hill: steerable UHF antenna error E5 ERROR FOR Direction 5 electric field (perp north) -1650 Vi Ef 1250 Vi5 Direction 5 Ion velocity (perp north) Direction 5 electric field (perp north) E5 1650 1640 E4 Direction 4 electric field (perp east) 31_13002 error E4 ERROR FOR Direction 4 electric field (perp east) -1640 Max Alt Maximum altitude 108 1020 Rot angl-mg Magnetic unit vector rotation angle error Vi4 ERROR FOR Direction 4 Ion velocity (perp east) -1240 106 Minimum altitude Min Alt Direction 4 Ion velocity (perp east) Vi4 1240 Bmag Geomagnetic field strength 210 ERROR FOR Direction 5 Ion velocity (perp north) -1250 error Vi5 31_3302 Nu Ne Ni Te Ti Tr Vi http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:mlh 31_3071 Nu Ne Ni Te Ti Tr Vi 125 Width of range gate Rng Gate Rng GateInc Additional increment to rnge gate width 126 31_3408 Nu Ni Ti Tr Vi -1420 error Vn2 ERROR FOR Direction 2 Neutral wind (northward) 3568 lg(fit(Ne)) SON log10 (ne-parabolic fit to ln(ne)) 353 352 Avg Typ 352's avg code: 1=>81day ; 2=13mon 3574 SON Neutral atmosphere model code Neut Atm 3510 SON Derivative of Ti with altitude DTi/DHt Upar SON Portion of Umerid due to Vpar 3512 SON Amount subtracted from Vlos 3567 Vbias SON Uambi from DNe/DH fit to ne 3514 Uden1 3504 V Src SON Source of velocity Vi6 Direction 6 Ion velocity (antiparallel) 1260 620 [O+]/Ne Ion Composition - [O+]/Ne Ugrav SON portion of Uambi from gravity 3517 31_15100 340 AP AP index (daily) Vn2 1420 Time > 0UT 34 Time past 0000 UT Direction 2 Neutral wind (northward) 870 lg([O]) log10 (O number density) ERROR FOR Direction 6 Ion velocity (antiparallel) error Vi6 -1260 T Src 3503 SON Source of temperature ERROR FOR SON Portion of Umerid due to Vpar -3512 error Upar Geographic unit vector rotation angle 1010 Rot angl-gg Ni Nn Te Ti Tn Vi Vn lg([O2]) 860 log10 (O2 number density) log10 (N2 number density) 850 lg([N2]) Tinf Exospheric temperature 820 Neutral temperature 810 Tn Utemp SON portion of Uambi from dTp/dH 3516 F10.7 Multiday average 352 F10.7a(Sa) 3511 DTe/DHt SON Derivative of Te with altitude 3513 Uambi SON Umerid from ambipolar diffusn SON Uambi from DNe/DH fit to ln(ne) 3515 Uden2 Den src 3505 SON Source of density profile -3513 ERROR FOR SON Umerid from ambipolar diffusn error Uambi 31_3303 Nu Ne Ni Te Ti Tr Vi 31_3301 Nu Ne Te Ti Tr Vi 31 31_13001 Vi Ef Davis, Antarctica MF radar http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:dav 1215 1215_17100 Vn tides 4-day CEDAR/TIMED analysis 1421 Vn2 Direction 2 Neutral wind (northward) Vn 1215_17001 Int Time 61 Integration time for these data error Vn1 ERROR FOR Direction 1 Neutral wind (eastward) -1411 error Vn2 ERROR FOR Direction 2 Neutral wind (northward) -1421 SLT 44 Local solar time Vn1 Direction 1 Neutral wind (eastward) 1411 DAV The Davis, Antarctica (68.60S, 77.97E; ~1 m alt) 1.94 MHz MF radar has been in operation since April 1994. On day 359 of 2001 at 89 km altitude, the apex magnetic coordinates were (64.1, 152.4) degrees. The magnetic inclination and declination angles were 81.7 deg and 21.7 deg. The magnetic local time at 0 Universal Time (UT) is about 0505 MLT. The solar local time (SLT) is UT plus 5 hours and 12 minutes (77.97/15.=5.198). Code 42 (LST-UT) was corrected from 1.E-03 hr to hhmm in Sep 2004. The original data files are hourly averages of the zonal and meridional velocity in Local Time (LT), which is 5 hours later than UT. Smaples are taken every 2 min, so a possible 30 samples can be had between 05:00:00 LT and 06:00:00 LT. The midpoint is 05:30:00 LT or 0:30:00 UT, or 5:42:00 SLT. Local times have been converted to the mid-point SLT, or 42 min (0.618 hr) are added to the beginning LT hour. The MF operating frequency is 1.94 MHz, with a peak transmitter power of 25 kW, 40 kW starting in 2004. The radar operates as a spaced-antenna system (Vincent, 1986), relying on coherent echo signals from middle atmosphere ionization. The inter-pulse period is 12.5 and 25 millisec, respectively during the day and night. There are usually 32 coherent integrations during the day and 16 at night, using 256 samples in the full correlation analysis (FCA) of Briggs [1984] with built-in rejection criteria. [ie, want about 2 min or 102.4 sec integration day or night, or 12.5x10-3sec * 32 integ * 256 samples = 102.4 sec and 25x10-3sec * 16 integ * 256 samples = 102.4 sec.] The height coverage is 50-100 km during the day or night at Davis. The pulse width is 30 microsec, giving a height resolution of 4.5 km assuming a simple rectangular wave pulse [range of heights illuminated by the wave pulse = velocity of light * pulse-width / 2 = 3x10**8 m/s * 30x10-6s / 2 = 4.5 km]. However, the height range provided is every 2 km between 50 and 100 km starting in 2003, and 50 and 98 km earlier. 20 mmdd Month/day (universal time) Yr 10 Year (universal time) 368 Estimated Hemispheric Pwr Corr. Factor Hem PwrFctr Estimated Hemispheric Power Qualifier 367 Hem PwrQual 175_31012 366 Estimated Hemispheric Power Index Hem PwrIndx Hour/min (universal time) hhmm 30 DMSP sat electron hemispheric power in GW el Hem Pwr 365 Estim. Electron Hemispheric Power Input 175 Estimated Hemispheric Power EHP original estim. Ion Hp input EHP origHpi 4164 364 Estim. Ion Hemispheric Power Input ion Hem Pwr Estim. Total Hemispheric Power Input tot Hem Pwr 363 EHP origHPe EHP original estim. Electron Hp input 4165 Emery intersat adjust elec,SEM-2 ion Hp (GW) 175_31100 EHP original estim. Total Hp input EHP origHpt 4163 The total hemispheric power input is computed from NOAA/TIROS and DMSP satellite measurements of high latitude precipitating energy flux carried by ions and electons with energies between 300 eV and 20 keV (NOAA/TIROS), or carried by electrons with energies between 460 eV and 30 keV (DMSP). The satellite orbits are sun synchronous around 850 km altitude. Times given are the center of the polar pass used to make the estimate where a typical polar pass takes about 25 minutes. Often there are two satellites operating simultaneously providing coverage at 30 to 60 minute intervals between auroral latitude crossings. The energy flux observations made during a single pass over the polar regions (above about 45 degrees of magnetic latitude) are used to estimate the total precipitating power input to a single hemisphere at that time. This power index was devised by David Evans for the NOAA/TIROS satellites, and adapted for the DMSP satellites by Frederick Rich and William Denig. http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:ehp -364 ERROR FOR Estim. Ion Hemispheric Power Input error ion Hem Pwr EHP maximum estim. Ion Hp input EHP max HPi 4168 4167 EHP med HPi EHP median estim. Ion Hp input -365 error el Hem Pwr ERROR FOR Estim. Electron Hemispheric Power Input 28 Beginning hour/min (universal time) Beg hhmm No Smpl usd No samples used 419 4162 EHP maximum estim. Electron Hp input EHP max HPe EHP median estim. Electron Hp input EHP med HPe 4161 EHP # w HPi 4166 EHP # of samples used for SEM-2 Hpi EHP NOAA sat tot, elec and proton hem power in GW 175_31021 http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:rfp cloudcov10 Cloud cover in tenths (0=clr,10=ovcst) 442 RFP avlosh RFP ave hourly zero los wind 4172 -1431 error Vn3 ERROR FOR Direction 3 Neutral wind (up) Vn1 Direction 1 Neutral wind (eastward) 1410 ERROR FOR Line of sight neutral vel (pos = away) -800 error Vnlos 813 relativ Tn Relative neutral temperature Relative background radiance 2555 RelBkgRadnc 4173 RFP losbf0 RFP los wind before zero rm (+away) ERROR FOR log10 (Relative line/band brightness) -2506 error lg(rel br) Direction 3 Neutral wind (up) Vn3 1431 180 Sol Zenith Solar zenith angle in measurement vol 2506 lg(rel br) log10 (Relative line/band brightness) -4173 error RFP losbf0 ERROR FOR RFP los wind before zero rm (+away) 800 Vnlos Line of sight neutral vel (pos = away) Wavelength Wavelength 2400 -1410 error Vn1 ERROR FOR Direction 1 Neutral wind (eastward) error relativ Tn ERROR FOR Relative neutral temperature -813 -2555 ERROR FOR Relative background radiance error RelBkgRadnc 4171 RFP mdlos0 RFP median nightly zero los wind 5535_17001 Vn Red line (~250 km), rel Tn The Fabry-Perot Interferometer at Resolute Bay, Canada (74.73N, -94.89E, 87 m ASL) has been operated since 2003 by the High Altitude Observatory of the National Center For Atmospheric Research. The apex magnetic coordinates of Resolute Bay at 250 km height in 2004 were (83.1, -39.0) with a magnetic declination of -24.4 deg, an inclination of 88.0 deg, and 0 UT at 16.31 MLT. The dispersing element of the interferometer is an air-spaced, 10 cm diameter effective clear-aperture Fabry-Perot etalon. It has a fixed gap of 2.0 cm. The etalon is housed in a temperature controlled chamber (Wu et al. 2004). The instrument detector is a back illuminated CCD camera with 1024x1024 pixels and 1x1 inch size. The CCD temperature is set at -55 C. The readout noise of the CCD is 4 electrons. The interferometer has an 8-position filter wheel. The wavelengths used at Resolute Bay are: 1. The red line (630.0 nm, kindat=17001) of atomic oxygen (OI) with a typical emission height peak in the range 210 to 300 km. 2. The green line (557.7 nm, kindat=17002) of atomic oxygen (OI), with a typical emission height peak range near 94-98 km. 3. The [OH] line (892.0 nm, kindat=17003) of the nightglow excited hydroxyl [OH*] with an emission peak between about 87 and 91 km. 5535 RFP Resolute Bay Fabry-Perot Interf Sp Global Positioning System Receivers GPS http://cedarweb.hao.ucar.edu/ 110 0.0 Global Positioning System Receivers 0.0 Qparth Particle energy heat rate height int. 2140 2142 Qparthe Particle energy heat rate hemisph.int. 1220 Direction 2 Ion velocity (northward) Vi2 Ee0 2155 Average electron energy 2310 Elect Pot Electric Potential Vi Ep Qp SH,NH 23-26 Sep 1986 for TIGCM 1230 Vi3 Direction 3 Ion velocity (up) 311_30020 Polar cap potential difference 2301 PC Pot Dif Direction 1 Ion velocity (eastward) 1210 Vi1 -2050 error HtInt HallC ERROR FOR Height integral hall conductivity 226 Apex Lat Apex latitude in measurement volume Pot Max Potential maximum 2303 Ef Ep Qp Sg new NH 23-26 Sep 1986 2050 HtInt HallC Height integral hall conductivity 320 Ae Index (1 or 2.5 min sample) Ae 311_30018 Magnetic local time 54 Mag Local Qjouhe 2152 Joule heat rate hemisphere integrated HtInt Ped C 2040 Height integral pedersen conductivity error HtInt Ped C ERROR FOR Height integral pedersen conductivity -2040 2302 Potential minimum Pot Min 311_30011 Ef Ep Qp Sg old NH 23-26 Sep 1986 311_30010 Ef Ep Sg NH 18-19 Jan 1984 311 AMI By GSM 2206 Interplanetary Mag Field By GSM SON Reduced chi square of Ne 3566 chi sq Ne Int Time Integration time for these data 60 Interplanetary Mag Field Bz GSM Bz GSM 2208 Ef Ep Qp Sg SH 20-21 Mar 1990 330 Dst index Dst 2204 Interplanetary Mag Field Bx GSM Bx GSM Au Au Index (1 or 2.5 min sample) 322 311_30022 Al Index (1 or 2.5 min sample) 321 Al http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:are AMIE Model Output Ep SH assumed 23-26 Sep 1986 311_30019 Ef Ep Qp Sg NH for several AMIE campaigns 311_30021 The Assimilative Mapping of Ionospheric Electrodynamics (AMIE) procedure is an NCAR model. A subset of the list of AMIE campaigns has been put into the CEDAR Database. These campaigns are: * 18-19 January 1984 * 23-26 September 1986 * 12-16 January 1988 * 20-21 March 1990 * 8-9 November 1991 * 27-29 January 1992 * 28-29 March 1992 * 20-21 July 1992 Most of these campaigns do not have plots on the CEDAR Database. But the input Goose Bay and Halley HF ion drifts are available for some of these campaigns. These are model lunar semidiurnal tides calculated in the Earth's atmosphere. The lunar day is 24 hr 50.47 min. The phases vary between 0.00 and 12.00 hours in lunar time, where 0 lunar time refers to the time of lower transit. This is when the moon is 180 degrees opposite one's position on Earth, and is entirely analogous to solar local time. The calculations were done for each month, where the day assumed was the 15th of each month. The results are independent of solar cycle, so the year is arbitrary. The year 1993 was chosen because this was the year that the model runs were made. The semidiurnal amplitudes and phases of the eastward neutral wind, the northward neutral wind, the neutral temperature, and the geopotential are given for 12 altitudes between about 78 and 102 km. The altitudes are slightly for each month. The original results were southward winds, so the phases were shifted by 6 hours to make them northward. The maximum amplitudes are just below 20 m/s for the winds, about 6 degrees K for the temperature, and nearly 2500 m2/s2 in geopotential. Some temperature amplitudes are shown as 0 near the pole but with some phase. This is the result of truncating amplitudes less than 0.005 K. 321 SDL http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:sdl Tn Vn tides 12-h neutral temperature amplitude 952 12h Tn Amp 12h Tn Phs 957 12-h max neutral temperature phase 953 lg(12h Gp) log10 (12-h geopotential amplitude) 12-h max geopotential phase 958 12h Gp Phs 321_20001 Vial/Forbes Model Lunar Tides The Aerospace 4 channel filter photometer at Fort Yukon, Alaska (66.57N, 214.73E) was developed to estimate the energy flux of auroral electrons, their average energy Eo (usually from 0.1 to 30 keV using a modified Gaussian or Maxwellian shape), and a scale factor fo for the atomic oxygen densities [O] from an MSIS model atmosphere. The [O] densities using the scaling factor fo can be compared to GUVI/TIMED estimates. The technique is only valid for clear night conditions where the solar zenith angle (sza) is greater than 102 deg (code 4102=1), and there is enough auroral emission (427.8 nm brightness, code 2421). Fort Yukon apex magnetic coordinates are (67.3, -94.7) at 110 km in 2001, with 0 UT corresponding to 12:36 MLT. The magnetic inclination and declination angles are 78.7 deg and 25.6 deg. The photometer looks up the magnetic field line with a field of view (fov) of about 1 deg. The data rate can be programmed, but typically each channel is integrated for 1 sec, where the whole cycle including filter moves takes about 8 sec. The 4 channels correspond to: 1. N2+ (427.8 nm, blue) first negative group (1NG) 0,1 molecular band 2. OI (630.0 nm, red) forbidden 3. OI (844.6 nm, eight) permitted 4. N2 (871.0 nm or 871.4 nm) first positive group (1PG) 2,1 molecular band http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:y4p 4473 Fort Yukon Alaska 4 Channel Photometer 2156 Aur Flx Typ Auroral flux type: maxwellian=1,gauss=2 4473_18002 -350 ERROR FOR F10.7 solar flux (Sa) error F10.7 (Sa) ERROR FOR log10 (N2 number density) error lg([N2]) -850 Ht Scl Chap Scale ht of Chapman model electron den 541 Hecht 4ch Ph. Model no. (eg MSIS90) 4101 H4P mod no Model Neutral temperature Tn Model 811 530 Maximum electron density Max Ne Modl Day No Model Day number of year (UT, 1=Jan 1) 22 error AP ERROR FOR AP index (daily) -340 F10.7 (Sa) F10.7 solar flux (Sa) 350 error SLT ERROR FOR Local solar time -44 error lg([O]) -870 ERROR FOR log10 (O number density) error lg([O2]) ERROR FOR log10 (O2 number density) -860 Ne Nn Strickland transport model inputs w 2 locs -540 error Ht Max Ne ERROR FOR Height of maximum electron density Ht Max Ne Height of maximum electron density 540 ERROR FOR Maximum electron density -530 error Max Ne scale factor to model [O] profile 871 [O] mod scl UT of Nautical sunrise (szen=102 deg) 77 Tsris Naut Channel 2 Wavelength Ch2 Wavelen 2422 78 Tsset Astr UT of Astronomical sunset (szen=108 deg) Ch4 Bkg Cor Channel 4 Background correction 2574 Hecht 4ch Ph. 1=ok (sza>102;flux;Eo;fo) 4102 H4P SZ flg Ne Nn Em optical obs/calcs and transp model input 2523 Ch3 Cal Channel 3 Calibration (cnt/s over R) Particle energy heat rate height int. 2139 Qparth Ch1 Bright Channel 2 line/band brightness 2512 Channel 4 line/band brightness 2514 Ch1 Bright 76 Tsset Naut UT of Nautical sunset (szen=102 deg) 2573 Ch3 Bkg Cor Channel 3 Background correction Ch1 Wavelen Channel 1 Wavelength 2421 Channel 4 Wavelength Ch4 Wavelen 2424 Ch1 Bright 2511 Channel 1 line/band brightness Channel 3 line/band brightness 2513 Ch1 Bright 4473_17002 2522 Ch2 Cal Channel 2 Calibration (cnt/s over R) Ch4 Cal Channel 4 Calibration (cnt/s over R) 2524 Tmonnrise 73 UT of Moonrise (from US Naval Obs) UT of Civil sunrise (szen=96 deg) 75 Tsris Civil Channel 2 Background correction 2572 Ch2 Bkg Cor 4103 H4P Moonflg Hecht 4ch Ph. 1=moon down; 0=moonlit Channel 1 Calibration (cnt/s over R) 2521 Ch1 Cal 2423 Channel 3 Wavelength Ch3 Wavelen Tsris Astr 79 UT of Astronomical sunrise (szen=108deg) Dif Aur Rat 2600 Diffuse aurora ratio (Ch1/Ch4) Tmoonset 72 UT of Moonset (from US Naval Obs) H4P nitflg 4104 Hecht 4ch Ph. 1=good night, 0=so-so Tsset Civil UT of Civil sunset (szen=96 deg) 74 Normalized Brightness ratio (Ch1/Ch4) 2601 NorBritnRat Ch1 Bkg Cor Channel 1 Background correction 2571 Y4P 41 http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:sts Bisector ion vel (bistatic sys,pos=up) 590 Vi Bisect Bn Northward component of geomagnetic fld 204 Ne Ni Te Ti Vi 41_4205 720 lg(ColF) log10 (ion-neutral collision frequency) 208 Bd Downward component of geomagnetic field error Vi Bisect ERROR FOR Bisector ion vel (bistatic sys,pos=up) -590 Electron density Ne 512 -512 error Ne ERROR FOR Electron density error lg(ColF) ERROR FOR log10 (ion-neutral collision frequency) -720 Eastward component of geomagnetic field 206 Be The incoherent scatter transmitter station at St. Santin, France (44.6N, 2.2E) operated between 1963 and 1987. The CEDAR Data Base holds all the data taken from 1966 until the end. Up until June 1973 and after July of 1986, the only receiver station operating was located at Nancay (47.4N, 2.2E). Between 1973 and 1986, 2 other receivers also operated at Montpazier (44.7N, 0.8E) and at Mende (44.5N, 3.45E). In general, the daytime height range is 105 to 350 km, while the nighttime height range is 200 to 500 km. Before January 1, 1969, the faraday correction is not taken into account in the computation. The spectrum are analysed following the scheme described in Waldteufel (1970). The ion drift component is quasi parallel to the magnetic field as measured by the Nancay receiving station. Because the transmitter is not located at the receiving location, the bisector velocity is plotted for the period when only Nancay data were received. When all 3 receivers were on, then the data are 30 minute averages and the ion drifts in the geomagnetic coordinate system are calculated. There are 4 areas in the summary plots. There are image plots as a function of height and time of the electron density, electron temperature, and ion temperature. Bin sizes are 40 minutes in time and 40 km in height. For the Nancay period alone there is also an image plot of the bisector velocity, while this is replaced by line plots of the ion drift in the perpendicular east, north and parallel directions at the altitude closest to 300 km. when there are 3 receivers. Ne Te Ti Vi 41_4206 Saint Santin: Nancay receiver STS41 41_4207 Ne Te Ti Vi Tn 41_30004 ERROR FOR Exospheric temperature error Tinf -820 650 [HE+]/Ne Ion Composition - [HE+]/Ne error Raw Ne ERROR FOR Uncorrected electron density (Te/Ti=1) -500 ERROR FOR Ion Composition - [HE+]/Ne error [HE+]/Ne -650 Nu Ne Ni Te Ti Faraday rot data > 1995 w coh echoes 10_1800 Direction 7 Elevation angle 1040 El(dir 7) 454 JRO Dat QC4 Jicamarca data quality code 4 Az(dir 8) Direction 8 Azimuth angle 1050 -1270 error Vi7 ERROR FOR Direction 7 Ion velocity JRO Dat QC3 Jicamarca data quality code 3 453 10_1051 Jicamarca data quality code 2 452 JRO Dat QC2 No samples used in time average 414 Smpl Tm usd 1270 Vi7 Direction 7 Ion velocity El(dir 8) 1060 Direction 8 Elevation angle -1280 error Vi8 ERROR FOR Direction 8 Ion velocity Direction 8 Ion velocity 1280 Vi8 Az(dir 7) 1030 Direction 7 Azimuth angle Spectral sampling time Spct Smpl T 406 Vi JRO Dat QC1 Jicamarca data quality code 1 451 Vi 10_1050 10_1101 Nu Ne Faraday rot data 1984 Nu Ni Te Ti 10_1802 JRO The 50 MHz incoherent scatter radar at Jicamarca, Peru (11.95 S, 76.87 W; 520 m alt) has been operating since 1963. On day 359 of 2001 at the ground, the apex magnetic lat,lon were (0.58, -5.12) deg. The magnetic inclination and declination angles were 1.145 deg and 0.367 deg. The magnetic local time at 0 UT is ~1835 MLT. There are three basic types of operating modes for the incoherent scatter radar: 1. Faraday rotation to obtain electron densities (Ne) and electron (Te) and ion temperatures (Ti) 2. the drift mode 3. the bistatic coherent radar mode (E-region Ne above Paracas) The drift mode, which finds perpendicular east and north (near vertical) ion drifts, has data from 1984 to the present. The analysis scheme to derive the drifts was changed starting in September of 1994 with a resulting increase in the data quality. Hard copies of time series plots of the older ion drifts are available upon request from NCAR. The bistatic coherent radar experiment involves the 50 MHz transmitter at Jicamarca and a reciever at Paracas (13.85 S, 76.25 W), which is about 200 km south of Jicamarca. E region (~95-110 km) electron density data are available using a 4 microsecond (~0.6 km) pulse length from Mar 2004. This experiment can run concurrently with either the Faraday rotation or the drift mode. http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:jro Jicamarca Peru I.S. Radar 10_1040 Vi Ne Te Ti Faraday rot data 1966-1969 (Te>Ti forced) 10_30003 Receiver bandwidth 494 Rec Bandw No Lags No ACF lags calculated 418 3100 T Norm Fctr JRO normalizing factor (JRO661111A) Vi 4 ht avs kindat 1910 w/o coh echoes -1252 error Vi5 ERROR FOR Direction 5 Ion velocity (perp north) Direction 4 Ion velocity (perp east) 1241 Vi4 Alt AvgNtvl 115 Altitude averaging interval 10_1911 Direction 5 Ion velocity (perp north) Vi5 1252 -1241 error Vi4 ERROR FOR Direction 4 Ion velocity (perp east) JRO W beam log10(1+RxA coher. pwr/noise) 3102 PwrC RxA W JRO parameter 17 JRO par 17 3116 JRO E beam log10(1+RxC coher. pwr/noise) 3106 PwrC RxC E 10_1910 3113 JRO par 14 JRO parameter 14 Vi 5mn aves func(alt) new w coh echoes PwrI RxB W JRO W beam log10(1+RxB incoh. pwr/noise) 3103 ERROR FOR Direction 8 Ion velocity error Vi8 -1282 3107 PwrI RxD E JRO E beam log10(1+RxD incoh. pwr/noise) PwrC RxB W 3104 JRO W beam log10(1+RxB coher. pwr/noise) 3114 JRO parameter 15 JRO par 15 error Vi7 ERROR FOR Direction 7 Ion velocity -1272 3101 JRO W beam log10(1+RxA incoh. pwr/noise) PwrI RxA W Direction 8 Ion velocity Vi8 1282 PwrC RxD E 3108 JRO E beam log10(1+RxD coher. pwr/noise) PwrI RxC E JRO E beam log10(1+RxC incoh. pwr/noise) 3105 3115 JRO par 16 JRO parameter 16 1272 Direction 7 Ion velocity Vi7 10 Nu Ni Te Ti Faraday rot data > 2000 w coh echoes 10_1801 http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:aei 211 Geophysical indices from NGDC: AE The CEDAR Database contains 1 min and hourly values of the magnetic indices AE, AL AU and AO from 1 January 1978 to 30 June 1988, and provisional AE indices from 1 January 1990 to 31 December 1994. The provisional AE indices came from http://swdcdb.kugi.kyoto-u.ac.jp/aedir, where one can get recent estimated AE plots also. The older AE came from World Data Center in Boulder where one can get: * hourly AE, AL, AU, AO (1 July 1957 - 30 June 1988) * 1 min AE, AL, AU, AO (1 Jan 1986 - 30 June 1988). Previous years of 1 min data must be ordered from NGDC, or taken from the CEDAR Database. When the Assimilative Mapping of Ionospheric Electrodynamics (AMIE) procedure uses ground magnetometers, it can calculate the AE at usually 5 minute intervals. AE is thus usually available for the list of AMIE campaigns. 31 Beg TimeInc Centiseconds (UT, increment to hhmm) Ao (hr) Ao Index (hourly mean) 327 Ao 323 Ao Index (1 or 2.5 min sample) 324 Ae (hr) Ae Index (hourly mean) Sampling interval (time between sampls) Sampl Ntvl 70 211_30008 Al Index (hourly mean) Al (hr) 325 Au (hr) Au Index (hourly mean) 326 AE (AU,AL,AO) gnd magnetic index (1m,hrly) AEI The Saskatoon HF radar is located in central Saskatchewan (52.16 deg N, -106.53 deg E) and looks over a section of ionosphere poleward of 53 deg N that covers north-central Canada including Hudson Bay and the Canadian arctic archipelago. It has operated since 1993. The facility is part of the SuperDARN network of HF radars that extends from western North America to Scandinavia in the Northern hemisphere and covers much of Antarctica in the Southern hemisphere. The SuperDARN radar for the most direct 2-D merging of Saskatoon velocity data is located at Kapuskasing, Canada. The radar forms and steers its beam by the phasing of transmissions from 16 elements in a linear antenna array. A second 4-element array provide the capability to measure elevation angle. The basic radar operation consists of the following steps: i) selection of a beam position (0-15), ii) search for the quietest 5-kHz channel about the assigned transmitting frequency (8-20 MHz), iii) repeated transmission of a multi-pulse sequence over the selected integration period and reception of backscattered signal with gating in range (1-70), and iv) calculation of the auto-correlation functions (ACFs). These operations are usually carried out in sequence for the 16 beam positions, which collectively constitute 1 scan. The beam integration period is typically 6 or 7 sec, and the scan repeat time is 96 sec or 120 sec. Within a scan, beam 0 corresponds to the most westward beam position and beam 15 to the most eastward. The azimuth sector scanned is approximately 50 deg wide and is centered on 23.1 deg E of N. http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:shf Saskatoon HF Radar 861 PACE Lat 225 PACE magnetic latitude of meas volume Lag1 Lag to the first range gate 401 610 Vel El Velocity direction - local elevation Vel Az Velocity direction - local azimuth 600 GBF GScat F GBF QC Groundscatter flag (0:n, 1:y) 4035 585 Vi Spread Ion Velocity spread (spectral width) Rng Gate No 127 Range gate number 861_7001 GBF SkyNois 4031 GBF QC Skynoise (A/D convertor units) 496 Rec Delay Receiver delay time PACE magnetic longitude of meas volume 245 PACE Lon GBF QC XCF flag (0=Off, 1=On) 4032 GBF XCF Flg Vi 230 PACE Az PACE magnetic azimuth error Vi Spread ERROR FOR Ion Velocity spread (spectral width) -585 SHF JUL 840 For the JULIA coherent scatter radar: The Jicamarca Radio Observatory is a facility of the Instituto Geofisico del Peru and is operated with support from the National Science Foundation Cooperative Agreement ATM-0432565 through Cornell University. These data are proxy measurements of F-region ExB ion drifts derived from the 150-km echoes measured with the Jicamarca (11.95 S, 76.87 W; 520 m alt) Unattended Long-Term studies of the Ionosphere and Atmosphere (JULIA) system. On day 359 of 2001 at the ground, the apex magnetic lat,lon were (0.58,-5.12) deg. The magnetic inclination and declination angles were 1.145 deg and 0.367 deg. The magnetic local time at 0 UT is ~1835 MLT. Jicamarca is the site of a 50 MHz incoherent scatter radar (ISR, kinst=10) in operation since the 1960s. The JULIA system is a coherent scatter radar (kinst=840) that uses two low-power 50 MHz transmitters which are phased together to excite the transmission antennas as a single unit. The JULIA system was intended for uninterrupted observations of ionospheric and atmospheric irregularities. JULIA shares the antenna, receiving system, processing, etc. with the ISR, but uses different transmitters. The coherent and incoherent scatter radar transmitters can operate at the same time for intercomparisons [e.g. Chau and Woodman, 2004]. The JULIA data are divided into 3 categories based on their altitude range and local time of occurrance. Observations of the E region electrojet (EEJ) are made between altitudes of 85 and 140 km in the morning and evening. The equatorial spread F (ESF) region irregularities are sampled between 95 and more than 850 km at night. For the valley region and so-called "150 kilometer" echoes, altitudes between 130 and 180 km are sampled during the day. The present 150-km echoes are averages between 140 and 170 km. JULIA ionospheric irregularity data have been collected beginning in August 1996. Signal-to-noise ratios are shown as intensities. Horizontal zonal drifts are deduced with radar intererometry. Vertical drifts refer to Doppler phase speeds where positive values imply upward phase propagation in the EEJ and ESF modes. Echoes from 150-km irregularities were first observed in the early 1960's over Jicamarca using the ISR [Balsley, 1964]. These echoes occurr only during the daytime and show very little seasonal dependence. The 150-km echoes have been observed at Jicamarca with the ISR on a campaign basis [e. g., Kudeki and Fawcett, 1993]. Sucessful low power observations of 150-km echoes have been performed since 2001 with the JULIA radar using two different antenna beam configurations (a single vertical beam, and an east-west beam pair). Using the vertical beam, only the vertical ion Doppler velocities are obtained, while using the east-west beam position both the vertical and zonal ion velocities are measured. In the latter case, two beams are used at the same time using diffent antenna sections. An important finding from the study of these 150-km echoes is that the daytime vertical Doppler velocities of the 150-km irregularities averaged over the altitudinal region of the irregularities were in excellent agreement with the mean F region (200-500 km) ISR vertical drifts [Chau and Woodman, 2004]. Vertical is perpendicular north at the magnetic equator where the B field is horizontally directed from the south to the north. The zonal ion Doppler velocities from the east-west JULIA beam are in reasonable agreement with the ISR zonal ion velocities. Although 150-km echoes have been observed and studied for many years, the physical mechanism which causes them is still unknown. This JULIA database of representative zonal and vertical (perpendicular north) ion drifts could contribute in providing very precise proxy measurements of F region drifts using less powerful and more economical radar. http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:jul JULIA Jicamarca Peru Coherent Radar -110 error Altitude ERROR FOR Altitude (height) The Kauai, Hawaii (22.0N, 159.3W; 2 m alt) 1.98 MHz MF radar has been in operation since 1990. On day 359 of 2001 at 89 km altitude, the apex magnetic coordinates were (22.6, -91.5) degrees. The magnetic inclination and declination angles were 38.6 deg and 10.1 deg. The magnetic local time at 0 Universal Time (UT) is about 1249 MLT. The solar local time (SLT) is UT minus 10 hours and 37 minutes (-159.3/15.=-10.620). Kauai, Hawaii MF RADAR 1270 http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:mltr KAU Vn tides 4-day CEDAR/TIMED analysis 1270_17100 1254 http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:tir TIR The Tirunelveli, India (8.67N, 77.82E; 30 m alt) 1.98 MHz MF radar has been in continuous operation since December 1992. On day 359 of 2001 at 89 km altitude, the apex magnetic coordinates were (6.8, 149.8) degrees. The magnetic inclination and declination angles were 1.4 deg and -2.6 deg. The magnetic local time at 0 Universal Time (UT) is about 0554 MLT. The solar local time (SLT) is UT plus 5 hours and 11 minutes (77.82/15.=5.188). The original data files are hourly averages of the zonal and meridional velocity in Indian Standard Time (IST), which is 5 hours and 30 minutes later than UT. Samples are taken every 2 min, so a possible 30 samples can be had between IST 0:00:00 and IST 0:59:00, which is labelled as hour 1:00:00 IST. These times have been converted to the mid-point solar local time (or 0:11 SLT or 0.188 SLT for this example). The MF radar system is identical to the one operating at Christmas island (2E,158W) and designed by Robert Vincent (robert.vincent@adelaide.edu.au) of the University of Adelaide in Australia (Vincent, 1991). The operating frequency is 1.98 MHz, with a peak transmitter power of 25 kW. The radar operates as a spaced-antenna system (Vincent, 1986), relying on coherent echo signals from middle atmosphere ionization. The inter-pulse period is 12.5 millisec during the day and 25 millisec during the night. There are 32 coherent integrations during the day and 16 at night, using 256 samples in the full correlation analysis (FCA) of Briggs [1984] with built-in rejection criteria. [ie, want about 2 min or 102.4 sec integration during day and night, or 12.5x10-3sec * 32 integ * 256 samples = 102.4 sec and 25x10-3sec * 16 integ * 256 samples = 102.4 sec.] The height coverage is 68-98 km during the day and 70-98 km during the night. The pulse width is 30 microsec, giving a height resolution of 4.5 km assuming a simple rectangular wave pulse [range of heights illuminated by the wave pulse = velocity of light * pulse-width / 2 = 3x10**8 m/s * 30x10-6s / 2 = 4.5 km]. However, neutral velocities are given every 2 km between 80 and 98 km since the ionization is less below 80 km. Tirunveli India MF radar Vn 1254_17001 1245 1245_17100 Vn tides 4-day CEDAR/TIMED analysis http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:mltr RTG Rarotonga Cook Islands MF RADAR The Rarotonga, Cook Islands (21.21S, 159.77W; 2 m alt) 1.98 MHz MF radar has been in operation since 2000. On day 359 of 2001 at 89 km altitude, the apex magnetic coordinates were (-22.9, -84.9) degrees. The magnetic inclination and declination angles were -39.5 deg and 13.5 deg. The magnetic local time at 0 Universal Time (UT) is about 1316 MLT. The solar local time (SLT) is UT minus 10 hours and 39 minutes (-159.77/15.=-10.651). 70_6210 Vi 70 Vi 70_6122 EIS70 EISCAT I.S. Radar The EISCAT (European Incoherent SCATter) facility in Scandinavia consists of a transimitter/receiver station at Tromso, Norway (69.6N, 19.2E), and receiver stations at Kiruna, Sweden (67.9N, 20.4E) and Sodankyla, Finland (67.4N, 26.6E). The facility has been in operation since 1981. The power profiles are calibrated with an on-site ionosonde, and are then corrected for Te and Ti effects which are deduced from the auto-correlation functions (ACFs). The collision frequency model used is the CIRA 1972 model atmosphere in Banks and Kockarts (1973), in Aeronmy Part A. The NO+ composition is assumed zero above 300 km. Perpendicular and parallel ion velocities were calculated routinely beginning in March, 1990. 70_6208 Vi Vi 70_6312 Vi 70_6118 http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:eis Vi 70_6314 Vi 70_6120 Syowa Antarctica HF Radar The Syowa South HF radar is located in Antarctica (69.00 S, 39.58 E) and looks over a section of ionosphere poleward (southward) of 70 deg S that includes central Antarctica. It has operated since 1995. The facility is part of the SuperDARN network of HF radars that extends from western North America to Scandinavia in the Northern hemisphere and covers much of Antarctica in the Southern hemisphere. The SuperDARN radar for the most direct 2-D merging of Syowa velocity data is located at SANAE (South African National Antarctic Expedition), Antarctica. The radar forms and steers its beam by the phasing of transmissions from 16 elements in a linear antenna array. A second 4-element array provide the capability to measure elevation angle. The basic radar operation consists of the following steps: i) selection of a beam position (0-15) ii) search for the quietest 5-kHz channel about the assigned transmitting frequency (8-20 MHz) iii) repeated transmission of a multi-pulse sequence over the selected integration period and reception of backscattered signal with gating in range (1-70) iv) calculation of the auto-correlation functions (ACFs). These operations are usually carried out in sequence for the 16 beam positions, which collectively constitute 1 scan. The beam integration period is typically 6 or 7 sec, and the scan repeat time is 96 sec or 120 sec. Within a scan, beam 0 corresponds to the most westward beam position and beam 15 to the most eastward. The azimuth sector scanned is approximately 50 deg wide and is centered on 159 deg E of N, or about 52 degrees west of the general scan position of Syowa East. http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:syf 830_7001 Vi 830 SYF These experiments are a compilation of Irkutsk ISR data available in October 2002 from http://62.76.21.18/cgi-bin/madrigal/madInvent.cgi This is the first contribution from the Irkutsk IS radar, Geographic: 52.9N 103.3E 502m-msl Magnetic: 41.06N 104.75E which started full operation in 1996, although there are some single measurements from 1988. These data (for 1999 to 2002) have 50km spatial resolution, typically starting at 250-300 km height and with time resolution 20 minutes. The data are in the vertical direction. Higher resolution is available on request with as little as 10 km height intervals, starting at 170-200 km, and 2 minutes time resolution. The data can be used under the 'Rules of the Road' - ie, informing us at an early stage of the work and offering us a cooperation request at the publication stage. IST 53 http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:ist Nu Te Ti Vi 53_9801 Irkutsk Russia I.S. Radar Ref 1/2-wid Refernce rel 1/2-width (arb press unit) 2455 Direction 3 Neutral wind (up) 1430 Vn3 4056-7Error AFP QC Error in 4056/4057 per 1000 km 4058 ERROR FOR Relative 1/2-width deviation from 2455 error 1/2-wid Dev -2456 4050 AFP Zen Flg AFP QC Zenith ref flag (1=use ; 0=no) 4051 AFP QC Free spectral range(arb p unit) AFP SpctRng Em Vn vertical meas in zero vel ref 5160_17011 AFP QC D(Vnn)/Dy per 1000 km (y +Nwrd) 4057 DVnn/Dx/mkm error Vn3 ERROR FOR Direction 3 Neutral wind (up) -1430 4055 AFP No Harm AFP QC No Harmonics in Fourier Anal 4056 DVne/Dx/mkm AFP QC D(Vne)/Dx per 1000 km (x +Ewrd) AFP I Cal F AFP QC Intensity Calibration Factor 4053 2456 1/2-wid Dev Relative 1/2-width deviation from 2455 1456 Direction 5 Neutral wind horizontl comp Vn5h AFP Et Th 4052 AFP QC Etalon Thickness rel Bright Relative line/band brightness 2505 Arecibo P.R. Fabry-Perot The Arecibo Observatory Fabry-Perot interferometer (18.35N, 66.75W) has been in operation since 1972. The data reported here (1980-1988), are atomic oxygen measurements at 630.0 nm. According to the IGRF model, the magnetic declination angle at Arecibo varied between -9.4 and -10.4 degrees between February 1980 and July 1988, while the inclination angle varied between 48.8 and 47.9 degrees. All nights are clear, or had cloudy periods removed. The approximate emission height is assumed to be 300 km. Scans in azimuth were done at a 30 degree elevation height, with usually one zenith measurment per scan. The intensities are relative, (Code 2505) but are approximately correct to within a factor of two of the true emission intensities in Rayleighs. The Doppler half-width is related to the square root of the neutral temperature assuming a Gaussian emission shape. The instrument was not optimized to measure Doppler widths, but was broadened to increase the signal throughput in order to make better measurements of the Doppler shift, which is related to the neutral velocity. Because of uncertainties in the half-width, the conversion to temperature was not made. In some of the data files the zenith observations were used as a zero reference in the analysis (Code 4050=1), while for others, all of the measurements for a given night were used (Code 4050=0) by assuming that each component of the horizontal neutral wind velocity can be represented by a second order Taylor expansion (constant horizontal velocity gradients) about a point directly above the station. A harmonic analysis gives the zonal (Ue) and meridional (Un) velocities, and two parameters related to the deformation of the flow, d(Ue)/dx and d(Un)/dy, where x and y are the eastward and northward directions, respectively. The vertical wind velocity (Uz) is thus not measured directly, but is derived from the DC term of the expansion. Values of Uz are inferred as the product of the horizontal divergence of the horizontal wind velocity, Uh, and the neutral scale height H: i.e., Uz = H del(Uh) where H = 50 km. 5160 Em Vn 5160_17020 5160_17010 Em Vn combined meas in zero vel ref 5160_17001 Em Vn older submissions AFP http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:afp DVS The Davis, Antarctica (68.48S, 77.97E; 25 m alt) Czerny-Turner (CZT) scanning spectrophotometer obtains mesosphere temperatures from ratios of the hydroxyl (OH) (6-2) band during nighttime hours. The spectrophotometer was in campaign operation March to October 1990 and April to August 1994, and has had continuous winter operations since March 1995. (See Greet et al., 1998; French et al., 2000; Burns et al., 2002.) Hydroxyl (6-2) band rotational temperatures are derived using Langhoff et al. (1986) transition probabilities, which are approximately 2 K higher than the temperatures derived by French et al. (2000) using experimentally derived P1 branch ratios with a slit width of 100 microns. The hydroxyl layer is centered at a mean height of 87+/-4 km with a mean thickness of 8 km. WINDII data showed that the hydroxyl layer often (up to 25% of the the time) has 2 peaks between 83 and 93 km (She and Lowe, 1998). The brightness of this layer usually decreases during the night. The spectrophotometer has a 6 degree field-of-view (fov) that was aligned 30-degrees above the horizon in a direction +130 E from Davis away from auroral precipitation in 1990 (Greet et al., 1998). An order separating filter was not used in 1990. Starting in 1994, the optical axis was aligned in the zenith, with a resultant area of about 8 km x 8 km at 87 km. In practice the field of view is defined by the diffraction grating. The diffraction grating rotates about the vertical axis as it scans, so that the area of the grating directly viewing the sky decreases with wavelength (when the grating is at vertical the fov is zero). Thus the fov corresponding to the grating vertical axis varies with grating rotation angle and consequently with wavelength. The instrument is aligned towards the SE (+130 E), but rotates about the vertical as the spectrum is sampled, so these observations are considered to be in the vertical. 3010 http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:dvs Beginning wavenumber Beg Wavenum 2411 Beg Wavelen 2401 Beginning wavelength End Wavenum 2412 Ending wavenumber 2402 Ending wavelength End Wavelen Tn Em 812 Tn1 Neutral temperature 4132 DVS cloud c DVS Cloud cover (0-3=clr-ovcst;4=snow) 3010_17001 ERROR FOR Neutral temperature error Tn1 -812 DVS QC Counting error 4131 DVS cnt err 2507 LinEmisRat Relative line emission rate Davis Antarctica Spectrometer JBR Jicamarca: Paracas Peru antenna 11 error Ne -510 ERROR FOR Electron density Ne Bistatic daytime E-region 510 Electron density Ne 11_1850 http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:jro Vi 825_7001 SAN The SANAE (South African National Antarctic Expedition) HF radar is located in Antarctica (71.68 deg S, -2.85 deg E) and looks over a section of ionosphere poleward of 65 deg S that covers much of East Antarctica. It has operated since 1997. The facility is part of the SuperDARN network of HF radars that extends from Alaska to Scandinavia in the Northern hemisphere and covers much of Antarctica in the Southern hemisphere. The SuperDARN radar for the most direct 2-D merging of SANAE velocity data is located at Halley Station. The radar forms and steers its beam by the phasing of transmissions from 16 elements in a linear antenna array. It has no second array for deriving elevation angle information. The basic radar operation consists of the following steps: i) selection of a beam position (0-15) ii) search for the quietest 5-kHz channel about the assigned transmitting frequency (8-20 MHz) iii) repeated transmission of a multi-pulse sequence over the selected integration period and reception of backscattered signal with gating in range (1-70) iv) calculation of the auto-correlation functions (ACFs). These operations are usually carried out in sequence for the 16 beam positions, which collectively constitute 1 scan. The beam integration period is usually 7 sec, and the scan repeat time is then 120 sec (2 min). Within a scan, beam 0 corresponds to the most westward beam position and beam 15 to the most eastward. The azimuth sector scanned is approximately 50 deg wide and is centered on 107.0 deg E of N. 825 SANAE Antarctica HF Radar http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:san Vn tides LTCS period analysis 1320_17999 http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:cof COF Collm LF Radar Vn tides d/sd func(altitude) > 5/98 1320_17013 Vn hourly winds > 5/98 117 Virtual height Virt Ht 1320_17012 4070 COF ts wnd COF QC Mean sampling density for winds 1320_17003 COF ts hts 4071 COF QC Mean sampling density for hts Vn tides d/sd func(altitude) 1320 Beginning month/day (universal time) 19 Beg mmdd 1320_17011 Vn tides mean and sd f(v alt) > 5/98 The Collm Geophysical Observatory (51.31 N 13.003 E) uses the closely spaced receiver method at 177, 225, and 270 kHz. Two receivers are used to the geographic north and east of the radar so the center of the reflection point triangle is near (52 N, 15 E). The measurements of the nighttime neutral winds and virtual heights are averaged over half-hour intervals from measurements of about 3/minute for winds and about 300/minute for virtual heights. The virtual height of the half-hour means is converted to true height using an empirical relation with linear height reduction (Kurschner et al, 1987). Then the half-hour means of the zonal and meridional winds are put through a multiple regression analysis to determine the altitude dependance of the prevailing and semi-diurnal tidal winds. To improve the spectral sensitivity, it proved useful to assume a circularly polarized tidal wind, which is acceptable for mid-latitudes. Therefor, the amplitude of the zonal and meridional semi-diurnal tidal wind is equal, and the phase of the meridional wind is 3 hours earlier than that of the zonal wind. Similarly, the amplitude of the zonal and meridional diurnal tidal wind is equal, and the phase of the meridional wind is 6 hours earlier than that of the zonal wind. However, the 24 hour component is normally only computed for the height of 95 km where the signal is a maximum. The result should be treated with some caution considering the fact that the observations are nighttime only. The phases are in mean local solar time (SLT). There is 1 hour between SLT and UT since the measurements are near 15E. Most of the calculations are for the period of a month. Extra information of interest such as seasonal transitions and the quasi two-day wave are in catalogue records. The data in the CEDAR Data Base are from January 1993 to January 1997, with selected Lower Thermosphere Coupling Study (LTCS) periods earlier. Vn tides hourly winds 1320_17002 Vn tides mean and semi-diurnal (sd) 1320_17001 Sondre Stromfjord Fabry-Perot The Sondre Stromfjord Fabry Perot interferometer, operated by the Space Physics Research Laboratory, Department of Atmospheric, Oceanic and Space Sciences of the University of Michigan is located at latitude 66.99N and longitude 50.95W. The invariant latitude is 74 degrees, the inclination of the magnetic field is 80 degrees and the declination of the field is -39 degrees (39 degrees to the west). Midnight local solar time at the site occurs at 03:24 UT, while midnight magnetic local time is 01:57 UT at the equinoxes. Magnetic midnight varies with season, being 15 minutes earlier at the winter solstice and 15 minutes later at the summer solstice compared to the equinox value. Currently, the interferometer observes the line profiles of the forbidden emissions OI (557.7nm) and OI (630.0nm). Most of the data in the CEDAR Database are 630.0nm (code 7001), with additional 557.7nm (code 7002) data starting in 2002. The filter wheel was changed in 2002, resulting in brighter relative emissions. http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:sfp -810 ERROR FOR Neutral temperature error Tn Reduced-chi square of fit Chi Sqr 421 5480_7002 440 Cloud Cover Cloud cover (0-8=clr-ovcst;9=obscured) Tn Em Vn ERROR FOR Relative line emission rate -2507 error LinEmisRat Tn Em Vn (some Vn only line-of-sight) 5480_7001 SFP 5480 A near infrared (NIR) BOMEM MB160 Michelson interferometer (MI) has operated at South Pole Station (90.00S, 2835 m) in Antarctica since January 1992. The MI scans the dark sky NIR airglow emissions between ~5000-10000 cm-1. A periscope directs the airglow into the MI sequentially from three locations at an elevation angle of 25 deg at azimuth angles of 0 (0 E), 120 (120 E), and 240 (240 E) deg. The periscope dwells at each position for about 4-15 min. Airglow hydroxyl Meinel (OH-M) band emissions peak at 87 km and are located between about 83 and 89 km for an elevation angle of 25 deg, the 87 km peak is located at a latitude spacing of 1.6 degrees, or at 88.4 S. http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:spm 2501 lg(Bright) log10 (line/band brightness) 5700_17031 Tn ERROR FOR log10 (line/band brightness) -2501 error lg(Bright) 5700 Tn 5700_17001 5700_17042 Tn South Pole, Antarctica Michelson Inter. SPM The Vostok ground magnetometer station is located in Antarctica (-78.463 S, 106.826 E) and has been operated by the Arctic and Antarctic Research Institute of St. Petersburg since 1958. The analog data have been digitized for 1978 and 1979, and for 1983-1995. A 1-sec digital magnetometer was installed in 1996. The station is part of the former Soviet Union's scientific exploration of Antarctica, which started in 1957 during the International Geophysical Year (IGY). It is located near the center of the Antarctic ice sheet, about 3488 m above mean sea level, and about 1250 km from McMurdo and about 1500 km from Mirny on the coast. Vostok is located in the polar cap at a high magnetic latitude. In 1978, the magnetic field at the surface was about 60950 nT, with an inclination angle of -77.682 degrees, a declination angle of -11.835 degrees, and an apex magnetic location of (-83.30, 53.56). In 2001, the magnetic field at the surface was about 59470 nT, with an inclination angle of -76.807 degrees, a declination angle of -12.019 degrees, and an apex magnetic location of (-83.31, 55.11). The apex magetic location of -83.3 is very close to the corrected geomagnetic (cgm) location of -83.4 cgmlat used for Vostok. http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:pcv 220_17001 PCI Vostok 1 min polar cap index 319 PC Index Polar Cap Index PCI Vostok 60 min polar cap index 220_17060 Polar Cap Geomagnetic Index: Vostok 220 PCV PCI Vostok 15 min polar cap index 220_17015 http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:kgf The Kerguelen Island HF radar is located in the southern Indian Ocean (49.35 deg S, 70.28 deg E; 58.9 mag S) and looks poleward. It has operated since 2000. The facility is part of the SuperDARN network of HF radars that extends from Alaska to Scandinavia in the Northern hemisphere and covers much of Antarctica in the Southern hemisphere. The SuperDARN radar for the most direct 2-D merging of SANAE velocity data is located at Syowa-East station. The radar forms and steers its beam by the phasing of transmissions from 16 elements in a linear antenna array. It has no second array for deriving elevation angle information. The basic radar operation consists of the following steps: i) selection of a beam position (0-15) ii) search for the quietest 5-kHz channel about the assigned transmitting frequency (8-20 MHz) iii) repeated transmission of a multi-pulse sequence over the selected integration period and reception of backscattered signal with gating in range (1-70) iv) calculation of the auto-correlation functions (ACFs). These operations are usually carried out in sequence for the 16 beam positions, which collectively constitute 1 scan. The beam integration period is usually 7 sec, and the scan repeat time is then 120 sec (2 min). Within a scan, beam 0 corresponds to the most westward beam position and beam 15 to the most eastward. The azimuth sector scanned is approximately 50 deg wide and is centered on 107.0 deg E of N. KGF Kerguelen Is. HF radar 835 835_7001 Vi Halley Antarctica Fabry-Perot HFP 5020_17002 Vn 1994-1998 cubic spline fits 5020_17001 Time past 0000 UT 36 Time > 0UT Vn 1988-1993 cubic spline fits A Fabry Perot Interferometer is operated by the British Antarctic Survey at Halley, Antarctica. The station is sited on a floating ice shelf that drifts westward at around 800 m per year, requiring a new station to be built further to the east about every 10 years or so. The geographic coordinates are 75.5 deg S, 26.6 deg W, and the invariant geomagnetic coordinates are 61.5 deg S, 28.9 deg E. The magnetic inclination is 64 deg and magnetic north is 2 deg west of geographic north. The mean local time is 1 hour and 46 minutes (-26.6/15.) before Universal Time. The station was closed in 1998. http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:hfp 5020 5015 1475 Vn7h Direction 7 Neutral wind horizontl comp 5015_17011 Tn Vn Red line (~240 km), multi-directions error Vn7h -1475 ERROR FOR Direction 7 Neutral wind horizontl comp http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:ahf AHF The Fabry-Perot Spectrometer at Arrival Heights, Antarctica (77.8296 S, 166.6627 E, 190.3 m ASL) has been operated since 2002 by the Department of Earth and Space Sciences, University of Washington. The apex magnetic coordinates of Arrival Heights at 250 km height in 2002 were (-80.1, -34.3) with a magnetic declination of 142.6 deg, an inclination of -81.3 deg, and 0 UT at 17.15 MLT. The dispersing element of the spectrometer is an air-spaced, 14 cm diameter effective clear-aperture Fabry-Perot etalon, which is both self-aligning and self-stabilizing. It is operated near the optimum operational point (2.0 cm spacer) for kinetic temperature determinations (Hernandez, 1988). The spectrometer operates simultaneously at two wavelengths, which are arbitrarily selected by the use of dichroic mirrors and narrow (0.3 nm wide) interference filters. The inherent stability of the spectrometer is about 0.5 m/s (632.8 nm) for periods of months, because of its self-stabilizing properties. The instrumental internal stability calibration is updated every 9 s. Arrival Heights Fabry-Perot Interf Sp EQB DMSP sat auroral midnight equatorward boundary 370 MlatEqBndry Est mag lat 0MLT equatorwd aurora bndry 180_17002 Midnight Equatorward Boundary 180 The Defense Meteorological Satellite Program (DMSP) has launched DMSP satellites since the mid 1970s. All the satellites have had precipitating particle spectrometer sensors (SSJ2-J4) on board. The SSJ4 sensor was first flown on DMSP-F6 in late 1982, so 1983 is the start of the automatically computed equivalent boundary data set. The official name of the index is "The Air Force Research Laboratory Auroral Boundary Index" and should be acknowledged as being provided by the USAF Research Laboratory, Hanscom AFB, MA. A courtesy copy of any publications using the index should also be sent to Dr. M. Susan Gussenhoven-Shea or her replacement, Dr. Katharine Kadinsky-Cade, at Air Force Research Laboratory, VSBXS, 29 Randolph Road, Hanscom Air Force Base, MA 01731-3010. For most of the DMSP orbits on a given day, the auroral oval is crossed twice in each hemisphere, once on the ascending leg, and once on the descending leg. The auroral oval expands during increased auroral or magnetic activity and the equtorward boundary is strongly related to Kp (Gussenhoven et al., 1981). The poleward boundary is more difficult to detect than the equatorward boundary, so only the equatorward boundary is found automatically. Hand selection of the equatorward boundary is described in Gussenhoven et al. [1981, 1983]. The magnetic latitude of the equatorward boundary of the aurora is found for a particular orbit at a particular MLT. Then the magnetic latitude of the equivalent equatorward boundary at midnight magnetic local time (0 MLT) can be estimated by statistically determining the position of the auroral oval for every local time sector as a function of some magnetic activity index, such as Kp. A computer algorithm was written to select the boundaries imitating the rules for hand selection with a quality flag of: 'best', 'good', 'not good'. Only those flagged as 'best' are released. Determination of the quality depends on a variety of factors. Generally,the clearest boundaries occur premidnight, that is, on the evening side, but not prior to 17 MLT. The next best are on the dawn side. Here, however, the flux levels are decreasing and the boundaries are not sharp. The worst boundaries are on the dayside, and near midnight when the oval is cut obliquely. Therefore, the preponderance of boundaries with the 'best' flag are on the evening side. Only 1/3 of the total are 'best' boundaries. The equivalent equatorward boundary determined for 0 MLT is always defined positive, regardless of the hemisphere of the satellite. These data are also available as yearly files from the contact persons. The ftp and web sites at AFRL have been disconnected. Publically available plots from 1983 are at /instruments/eqb.html. http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:eqb 43 43_30004 Tn The incoherent scatter transmitter station at St. Santin, France (44.6N, 2.2E) operated between 1963 and 1987. The CEDAR Data Base holds all the data taken from 1966 until the end. Up until June 1973 and after July of 1986, the only receiver station operating was located at Nancay (47.4N, 2.2E). Between 1973 and 1986, 2 other receivers also operated at Montpazier (44.7N, 0.8E) and at Mende (44.5N, 3.45E). In general, the daytime height range is 105 to 350 km, while the nighttime height range is 200 to 500 km. Before January 1, 1969, the faraday correction is not taken into account in the computation. The spectrum are analysed following the scheme described in Waldteufel (1970). The ion drift component is quasi parallel to the magnetic field as measured by the Nancay receiving station. Because the transmitter is not located at the receiving location, the bisector velocity is plotted for the period when only Nancay data were received. When all 3 receivers were on, then the data are 30 minute averages and the ion drifts in the geomagnetic coordinate system are calculated. There are 4 areas in the summary plots. There are image plots as a function of height and time of the electron density, electron temperature, and ion temperature. Bin sizes are 40 minutes in time and 40 km in height. For the Nancay period alone there is also an image plot of the bisector velocity, while this is replaced by line plots of the ion drift in the perpendicular east, north and parallel directions at the altitude closest to 300 km. when there are 3 receivers. Saint Santin: Montpazier receiver STS43 http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:sts Ne Ni Te Ti 410 S/N Signal to noise ratio 20_30008 ARO Dat QC4 459 Arecibo data quality code 4 Vi 922 No Dirs Number of directions in analysis 20_2011 20_30016 Nu Ne log10 (max Ne in m-3) 535 lg(MaxNe) 20_2021 Vn LTCS Additional increment to max alt 109 Max Alt Inc 107 Min Alt Inc Additional increment to min alt Ne 20_2015 Alt Avg Inc Additional increment to ht avgng intrvl 116 20_30002 Ne 310 Geomagnetic Index Kp: low geomagnetic activity Low geomagnetic activity (as measured by index Kp) 3.0 9.0 3.0 Kp: medium geomagnetic activity Medium geomagnetic activity (as measured by index Kp) 9.0 High geomagnetic activity (as measured by index Kp) Kp: high geomagnetic activity Kp Kp Index Nu 20_30014 20 Ti Vn tides LTCS error Ti ERROR FOR Ion temperature -552 20_12999 -954 error 12h Ti Amp ERROR FOR 12-h ion temperature amplitude 954 12-h ion temperature amplitude 12h Ti Amp 939 Mean Ti Mean ion temperature error Mean Ti ERROR FOR Mean ion temperature -939 552 Ion temperature Ti 12-h max ion temperature phase 959 12h Ti Phs error 12h Ti Phs -959 ERROR FOR 12-h max ion temperature phase Ne Ni Ti Tr Vi 20_2002 Arecibo data quality code 2 457 ARO Dat QC2 Nu Ne Ni Ti Tr Vi 20_2001 -1230 error Vi3 ERROR FOR Direction 3 Ion velocity (up) 458 ARO Dat QC3 Arecibo data quality code 3 Nu Ne Te Ti Tr Vi Bdec 213 Geomagnetic field east declination Geomagnetic field downward inclination Binc 216 20_30015 20_30005 Nu No Coeffs 921 Number of coefficients in analysis Ne Ni Te Ti Vi 20_2010 ARO Arecibo P.R. I.S. Radar 20_30009 Ne Te Ti Tr Vi Ne Ni Ti Tr Vi 20_2003 The incoherent scatter radar at the National Astronomy and Ionosphere Center (NAIC) at Arecibo, Puerto Rico (18.3N, 66.75W), has made ionospheric measurements since 1963. The radar facilities are shared with radio astronomers. The most recent analysis solves between 3 (Ne, Ti, Ti) and 5 parameters (Ne, Ti, Te, H+/Ne, He+/Ne) simultaneously. The line-of-sight velocity is found in a separate fit to the slope of the auto-correlation function (ACF). There are several corrections that are applied to the data. These include a chirp correction for the velocities, eliminating bad data records due to satellites or ground based radio communication (some outliers remain), and calibration of electron densities with ionosonde data in post processing. In the lower altitudes, a molecular ion model is assumed. The model was determined by looking for consistency in the other parameters. The molecular ion mass is assumed to be 30 amu and the assumed molecular ion composition is: Alt(km) 145 182 219 256 > 293. [M. ion]/[Ne] 1. 0.3 0.2 0.07 0. Te Ti Tn Vi Vn F10.7q(Sa) F10.7 solar flux qualifier 351 20_15100 http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:aro 20_30001 ERROR FOR Ion Composition - [O+]/Ne error [O+]/Ne -620 ARO Dat QC1 Arecibo data quality code 1 (IFIT) 456 Ni Te Ti Vi Ef Nu 72_6117 1/2 Scat A Half scattering angle (bistatic system) 190 EIS72 Nu Ne Ni Te Ti Vi EISCAT data quality code 1 476 EIS Dat QC1 R Dop Foff 492 Received doppler frequency offset 72_7310 72_6111 Nu 3906 ACFin6 Normalized imaginary ACF at lag 6 ACFin8 Normalized imaginary ACF at lag 8 3908 3925 Normalized imaginary ACF at lag 25 ACFin25 ACFrs0 Scaled real ACF at zero lag 3800 3814 ACFrn14 Normalized real ACF at lag 14 Normalized real ACF at lag 9 3809 ACFrn9 Normalized imaginary ACF at lag 16 3916 ACFin16 ACFin15 3915 Normalized imaginary ACF at lag 15 Normalized imaginary ACF at lag 24 3924 ACFin24 3817 Normalized real ACF at lag 17 ACFrn17 ACFrn16 Normalized real ACF at lag 16 3816 3819 Normalized real ACF at lag 19 ACFrn19 Normalized real ACF at lag 20 3820 ACFrn20 Normalized real ACF at lag 22 3822 ACFrn22 ACFin1 3901 Normalized imaginary ACF at lag 1 3900 ACFsf0 Scale factor for ACF at zero lag Nu Ne Ni Te Ti Vi CF ACFrn7 Normalized real ACF at lag 7 3807 3929 ACFin29 Normalized imaginary ACF at lag 29 ACFrn26 3826 Normalized real ACF at lag 26 ACFrn10 Normalized real ACF at lag 10 3810 3917 ACFin17 Normalized imaginary ACF at lag 17 Normalized imaginary ACF at lag 10 3910 ACFin10 ACFin26 Normalized imaginary ACF at lag 26 3926 ACFin19 Normalized imaginary ACF at lag 19 3919 Normalized real ACF at lag 11 3811 ACFrn11 Normalized real ACF at lag 25 3825 ACFrn25 3927 ACFin27 Normalized imaginary ACF at lag 27 3802 Normalized real ACF at lag 2 ACFrn2 3801 Normalized real ACF at lag 1 ACFrn1 Normalized real ACF at lag 28 3828 ACFrn28 ACFin30 3930 Normalized imaginary ACF at lag 30 Normalized real ACF at lag 31 3831 ACFrn31 Normalized imaginary ACF at lag 3 ACFin3 3903 ACFin12 3912 Normalized imaginary ACF at lag 12 3921 Normalized imaginary ACF at lag 21 ACFin21 Normalized real ACF at lag 18 3818 ACFrn18 ACFrn4 Normalized real ACF at lag 4 3804 Normalized real ACF at lag 27 ACFrn27 3827 ACFrn21 Normalized real ACF at lag 21 3821 3932 Normalized imaginary ACF at lag 32 ACFin32 ACFrn30 Normalized real ACF at lag 30 3830 3902 ACFin2 Normalized imaginary ACF at lag 2 ACFin11 3911 Normalized imaginary ACF at lag 11 ACFrn3 Normalized real ACF at lag 3 3803 72_6210 Normalized real ACF at lag 12 3812 ACFrn12 Normalized imaginary ACF at lag 5 ACFin5 3905 Normalized imaginary ACF at lag 28 3928 ACFin28 3914 ACFin14 Normalized imaginary ACF at lag 14 Normalized imaginary ACF at lag 7 ACFin7 3907 Normalized real ACF at lag 13 3813 ACFrn13 ACFrn29 Normalized real ACF at lag 29 3829 3808 ACFrn8 Normalized real ACF at lag 8 3931 Normalized imaginary ACF at lag 31 ACFin31 3832 ACFrn32 Normalized real ACF at lag 32 Normalized imaginary ACF at lag 4 3904 ACFin4 ACFin13 3913 Normalized imaginary ACF at lag 13 3805 Normalized real ACF at lag 5 ACFrn5 Normalized real ACF at lag 6 3806 ACFrn6 3920 ACFin20 Normalized imaginary ACF at lag 20 3909 Normalized imaginary ACF at lag 9 ACFin9 3923 ACFin23 Normalized imaginary ACF at lag 23 ACFin22 3922 Normalized imaginary ACF at lag 22 3918 ACFin18 Normalized imaginary ACF at lag 18 ACFrn15 Normalized real ACF at lag 15 3815 Normalized real ACF at lag 24 ACFrn24 3824 3823 Normalized real ACF at lag 23 ACFrn23 Nu 72_6311 Nu Ne Ni Te Ti Vi CF 72_6714 72_6501 Nu Nu Ne Ni Te Ti Vi 72_7206 Nu Ne Ni Te Ti Vi 72_7112 72_6306 Nu Ne Ni Te Ti Vi CF 72_7116 Nu Ne Ni Te Ti Vi 72_7402 Nu Ne Ni Te Ti Vi Nu Ne Ni Te Ti Vi CF 72_7000 72_6305 Nu 72_6120 Nu Ne Ni Te Ti Vi CF Nu Ne Ni Te Ti Vi CF 72_6502 Nu Ne Ni Te Ti Vi 72_7118 72_6112 Nu Ne Ni Te Ti Vi CF http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:eis 72_8000 Nu Ne Ni Te Ti Vi Nu Ne Ni Te Ti Vi 72_7312 The EISCAT (European Incoherent SCATter) facility in Scandinavia consists of a transimitter/receiver station at Tromso, Norway (69.6N, 19.2E), and receiver stations at Kiruna, Sweden (67.9N, 20.4E) and Sodankyla, Finland (67.4N, 26.6E). The facility has been in operation since 1981, and recently expanded to include a facility at Svalbard, which will have its own web page when data are included in the CEDAR Data Base. 72_6205 Nu 72_6118 Nu Ne Ni Te Ti Vi CF 72_6119 Nu 72_6207 Nu Nu Ne Ni Te Ti Vi CF 72_6312 Nu 72_6313 Nu 72_6121 72_7208 Nu Ne Ni Te Ti Vi Nu 72_6209 Nu 72_6999 Nu Ne Ni Te Ti Vi 72_7314 72_6115 Nu 72_7306 Nu Ne Ni Te Ti Vi 72_6309 Nu Nu Ne Ni Te Ti Vi 72_7210 Nu Ne Ni Te Ti Vi CF 72_6122 Nu Ne Ni Te Ti Vi CF 72_6206 Nu Ne Ni Te Ti Vi 72_7120 72_6310 Nu Ne Ni Te Ti Vi CF Nu Ne Ni Te Ti Vi CF 72_6314 EISCAT: Tromso antenna Nu Ne Ni Te Ti Vi CF 72_6208 Nu Ne Ni Te Ti Vi 72_7122 72_7502 Nu Ne Ni Te Ti Vi 72_6116 Nu Ne Ni Te Ti Vi CF 72 72_6402 Nu Ne Ni Te Ti Vi CF http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:gcm 310 NCAR TGCM/TIGCM Model Output The NCAR TIGCM models output neutral winds and temperature. Specific TIGCM results are shown for the storm of March 22, 1979. The other results are of generic runs with the TIGCM which are described in Fesen (1997, JASTP, 785). The TIGCM model solves and saves 16 parameters: ht, Tn, un, vn, wn, N2, O2, O, N(4S), N(2D), NO, Te, Ti, Ne, O+, and O2+. The O+-O collision frequency was increased by a factor of 1.7 in the model over the laboratory value, as recommended by Burnside et al (1988, JGR, 8642) and Salah (1993, GRL, 1543). The model has 36 latitudes between -87.5 and +87.5 degrees geographic every 5 degrees apart, 72 longitudes between -180 and +175 geographic every 5 degrees apart, and 25 pressure levels between 97.5 km and approximately 500 km. This data set has interpolated (or extrapolated) values of the neutral zonal and meridional wind and neutral temperature at 22 heights between 100 and 500 km for all 36 latitudes at 24 longitudes every 15 degrees apart between -165 and +180 degrees. The diurnally reproducible results were saved for 25 UTs, and then harmonic analyses of these parameters were computed. Eighteen generic runs were made in 1993 for solar minimum (1976, with an assumed solar flux (350) of 75) and solar maximum (1979 with an assumed solar flux of 195), for three seasons (days 80, 172, and 355), and for three levels of activity (5 GW + 30 kV, 11 GW + 60 kV, and 33 GW + 90 kV). The activity is based on the hemispheric power and the polar cap potential drop. The IMF By was assumed to be 0 nT in the parameterizations. The 1989 Forbes and Vial semidiurnal tides appropriate for March, June and December were put at the lower boundary (97 km). Another version of these runs was for 70W only. The summary plots show the wind fields on the temperature over the globe at 300 and 140 km every 4 UT hours on March 22, 1979, and at 0 and 12 UT for the generic runs. Only the 60 kV case was plotted for the generic runs in solar minimum (sflux=75) and solar maximum (sflux=195) for March, June and December. The tidal fields for the neutral temperature and neutral zonal and meridional wind are shown at 140 and 300 km for the generic runs as a function of longitude and latitude. The 4 plots show the mean and the 24, 12 and 8-hr tidal amplitudes. Only the 60 kV case was plotted for the generic runs in solar minimum (sflux=75) and solar maximum (sflux=195) for March, June and December. The Fesen (JASTP, 1997) reference shows the tidal variations also as a function of height and magnetic activity for 70W. 943 24h Vne Amp 24-h eastward neutral wind amplitude 8h Tn Phs 967 8-h max neutral temperature phase 937 Mean Tn Mean neutral temperature 24-h max neutral temperature phase 947 24h Tn Phs 6h Vnn Phs 6-h max northward neutral wind phase 996 24h Tn Amp 24-h neutral temperature amplitude 942 Tn Vn Ep tides 90kV 6-h neutral temperature amplitude 6h Tn Amp 992 24-h northward neutral wind amplitude 948 24h Vnn Amp 961 8h Vnn Amp 8-h northward neutral wind amplitude 8h Vnn Phs 8-h max northward neutral wind phase 966 990 6h Vne Amp 6-h eastward neutral wind amplitude 965 8h Vne Phs 8-h max eastward neutral wind phase 962 8h Tn Amp 8-h neutral temperature amp 8h Vne Amp 960 8-h eastward neutral wind amplitude 991 6h Vnn Amp 6-h northward neutral wind amplitude 310_11092 6-h max neutral temperature phase 6h Tn Phase 997 995 6h Vne Phs 6-h max eastward neutral wind phase 310_11031 Tn Vn Ep 30kV Tn Vn Ep 60kV 310_11061 log10 (NO number density) 901 lg([NO]) lg([N(2D)]) log10 (N(2D) number density) 903 log10 (part energy heat rate ht. int.) 2141 lg(Qparth) 902 lg([N(4S)]) log10 (N(4S) number density) 640 [O2+]/Ne Ion Composition - [O2+]/Ne Vi1(F) 1211 Direction 1 F-region ion velocity 310_10034 1221 Vi2(F) Direction 2 F-region ion velocity Ne Ni Nn Te Ti Tn Vn Ep 22 March 1979 310_11091 Tn Vn Ep 90kV 310_11032 Tn Vn Ep tides 30kV 310_11062 Tn Vn Ep tides 60kV GCM MUI MU I.S. Radar, Shigaraki Japan 25 The Incoherent Scatter routine measurement with the MU (Middle and Upper atmosphere) radar (34.8N, 136.1E) uses 4 beam directions simultaneously, with the first 15 minutes of each hour devoted to single-pulse measurements (for electron density), and the last 45 minutes devoted to two-pulse (for ion drift velocity) or four-pulse (for ion/electron temperature) measurements. The radar operates at a frequency of 46.5 MHz and uses a beam width of 3.7 degrees. Measurements have been taken about 2 days per month starting on September 17, 1986. The 4 beams are at an elevation angle of 70 degrees pointing towards magnetic north, east, south and west, assuming a declination angle of -5 degrees. The inclination angle is about 48 degrees, and the corrected magneitc latitude of the MU radar is about 25 degrees. The initial range resolution of the velocities is 38 km. Velocities are averaged between 220 and 455 km, where the altitude of the measurement is defined to be 338, the midpoint of the 235 km range. A running 3-hour average of the ACF is computed as well as the height average before the line of sight (los) ion drift velocity is computed, so there are no error bars. The UT time is the midpoint of the 45 minutes of the middle hour. http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:mui 1090 El(dir 10) Direction 10 Elevation angle Direction 10 Azimuth angle 1085 Az(dir 10) Direction 9 Elevation angle 1080 El(dir 9) Direction 10 Ion velocity 1300 Vi10 MUI QC (0-3 <=> ok-bad) MUI qc 4092 MUI Vi3-ns 4090 MUI QC Ion velocity (up from NS dirs) 4091 MUI Vi3-ew MUI QC Ion velocity (up from EW dirs) 25_17000 Vi9 Direction 9 Ion velocity 1290 1070 Az(dir 9) Direction 9 Azimuth angle Vi http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:tfp 5540 Tn Vn 5540_7001 The Thule Fabry Perot interferometer, operated by the Space Physics Research Laboratory, Department of Atmospheric, Oceanic and Space Sciences of the University of Michigan is located at latitude 76.53N and longitude 68.44W. TFP Thule Greenland Fabry-Perot KHA The Wisconsin H-alpha Mapper (WHAM) Fabry-Perot Interferometer is operated at the Kitt Peak National Observatory by the Wisconsin Galactic Astronomy Group with support from the National Science Foundation. The Wisconsin H-alpha Mapper (WHAM) Fabry-Perot is located at the Kitt Peak Observatory (31.98N, 111.60W; alt 2120.0 m), and has been operated remotely by the University of Wisconsin Galactic Astronomy Group since 1997 [Reynolds, 1997; Haffner et al., 2003]. The geocoronal atomic hydrogen is studied using the H-alpha (656.274 nm) and H-beta (486.1 nm) emissions. The WHAM instrument is a double-etalon Fabry-Perot coupled to a Charge Coupled Device (CCD) camera where the optics are designed to image the Fabry-Perot annular interference pattern onto the CCD. Hence, the CCD images are spectral and not spatial. The geocoronal atomic hydrogen can be observed both at H-alpha (6563 A, ~1-10 Rayleighs), and H-beta (4861 A, ~0.25-1 R). The terrestrial H-alpha emission is primarily excited by the line center portion of the solar Lyman-beta emission and thus depends on both the solar excitation flux and the density distribution of upper atmospheric hydrogen. To first order, the column of H-alpha emissions (code 2502) observed by the Fabry-Perot comes from the sunlit portion of the geocorona above the Earth's shadow. Since density falls off with height, the shadow height (code 186) is roughly just below the peak emission height. However, a portion of the signal (~1-2 R) is also due to multiple scattering of Lyman-beta radiation below the Earth's shadow height in darkness. This contribution becomes increasingly significant for observations at higher shadow altitudes. The solar zenith angle (code 180) for all observations is below the horizon (e.g. nighttime conditions). The semi-raw spectral images are saved in FITS (.fts) format where only a portion of the chip was used and the read noise was reduced using 4 x 4 on-chip binning [Haffner et al., 2003]. The CEDAR Database FITS files include additional header information on the observing geometry, wavelength (H-alpha set at 6564 A in the original .fits headers starting in 2001), kinst (5190) and kindat (7001 for H-alpha or 7101 for H-beta). The kindat 17000 series files contain information from the H-alpha spectral profile (.spe) where the annular interference pattern in the .fts file is summed. Equal area annuli correspond to equal spectral intervals (measured in wavenumber, so the arbitrary pixel intensities are summed in equal area annuli to produce a spectral profile of relative emission as a function of wavenumber expressed as spectral displacement in velocity units km/s with an arbitrary zero (code 2416). The relative emission is divided by the exposure time (code 60) from the .coors file to create a relative emission rate (codes 4145 for NAN calibration files and 4146 for other files). Hot pixels due to cosmic rays, dark counts, reflections and a constant average bias have been removed. The standard deviation of the relative pixel intensity in each annuli divided by the exposure time is reported as the 'error bar' for the data point (codes -4145 and -4146). Codes 2507 and 2509 are the relative annular emission after the data have been normalized with a white light flat field (from the .dat files) divided by the exposure time to make an emission rate. The initial 31 spectral displacement points (below the arbitrary value of -50 km/s) are outside the aperture and are removed in the original .dat file and also in kindats 17000-3,17100-3. Additional information in nightly catalog files come from the headers from the FITS files and from shadow altitude calculations. This information is listed in the nightly .shad and .coors files. The UT times in the names (codes 4142 and 4143) of the original FITS files (.fts) are from .log file UTs that are contained in companion nightly catalog files. The actual UT start times listed in the FITS headers are a few seconds later than the UT start times in the .log file and reflect when the commands were started by the WHAM instrument. Astronomical locations are given in two coordinate systems: (1) galactic coordinates with galactic longitude b in degrees (code 193) and galactic latitude l in degrees (code 195), and (2) equatorial coordinates with right ascension (RA) in hours (code 192) and declination in degrees (code 194). The hour angle (code 191) is defined as the difference between the Local Siderial Time and the Right Ascension of the object. The hour angle is zero when the target transits the Local Meridian, which passes through the zenith direction. Hour angles are negative when the object is rising, and are positive when the object is setting. Atmospheric extinction is minimized when zenith angles are restricted to 50 degrees or less (ZA<50), which are equivalent to elevation angles (code 142) of 40 degrees or more (el>40). Typically, WHAM locks onto a given astronomical location for integration times (code 60) of 30 to 600 seconds, so the azimuth and elevation angles (codes 132 and 142) are initial values, while RA and DEC (codes 192 and 194) remain constant. All observations of H-alpha column emissions from the thermosphere plus exosphere are made at night during moonless conditions. All observations reported to the CEDAR Database are also made during clear sky conditions, since even high cirrus clouds can affect the H-alpha signal. Acceptable values of the quality code 4144 are: 1. =A Excellent conditions 2. =A- Clouds sighted much later or earlier in the night 3. =B Clouds sighted within a few hours of the observation OR spectrum close to sunset or sunrise at the observatory OR ZA>50 (el<40) -32767 Missing (consider ZA<50 or el>40 as best data) If the wing of a spectrum is truncated, then its grade is reduced. Sometimes a grade is given for each spectrum, sometimes for a single night, and sometimes grades are missing (-32767). Single nightly grades show as text in the nightly catalog record, and are marked as missing for each spectrum without an individual grade. Spectra with ZA>50 (el<40) are of lower quality. For ZA>80 (el<10), the data can be so compromised (e.g. very low emissions rates) that they were not included in this database. The regions of low galactic emission are useful for geocoronal observations because uncertainty in the retrieval of the geocoronal emission due to the presence of galactic emission is minimized. The fitting does not require removing the galactic emission in the low galactic region of observations. Geocoronal observations are also available from zenith and other directions, especially in survey runs. The analysis for survey data may include one or two Gaussians in the fit, while the cleaner low galactic emission regions are usually analyzed using two Gaussians to account for fine structure. The absolute intensities (code 2502) are calibrated using the bright H-alpha emission at (RA 20.97, DEC 44.6 or l,b 85.60 -0.72) of 800 R +/-10% from the North American Nebula (NAN). There is an additional ~5% uncertainty in the relative calibration due to night-to-night variability in the transmittance of the atmosphere. These uncertainties are larger than the standard deviation (codes -4145 and -4146) of pixel intensity in the annuli divided by the exposure time. Locations (code 4141) used for geocoronal observations or calibrations combined with the H-alpha kindats are: * -1/17001 = NAN (North Amercian Nebula calibration source) * 0/17000 = zenith (geoz, useful to compare with some models) * 1/17003 = surveys or other at all different (non-zenith) directions * 7/17002 = Lockman (low galactic emission region at l,b 148.5 53) * 8/17002 = Newoff (low galactic emission region at l,b 163.5 53.5) * 9/17002 = HD93521 (low galactic emission region at l,b 183.14 62.15) * 10/17002 = Off01 (low galactic emission region at l,b 166.7 26.31) * 11/17002 = Off02 (low galactic emission region at l,b 140.97 50.07) Further details of the procedure are in the references, in the generic kindat catalog records, and are available from the contact persons. Shadow Ht 186 Earth's Shadow altitude (height) ERROR FOR KHA rel annr emis rate w/o flatfld norm -4145 error KHA relert1 Hour angle HA=LSidT-RA (equatorial coor) 191 Hr Angle Spec disp V 2416 Spectral displ. in vel units w arb 0 KHA quality 4144 KHA quality code (1=A, 2=A-, 3=B, ...) 194 Declination angle (equatorial coords) Declin A KHA blgUTcs KHA beginning centisec (UT) from log 4143 2502 Bright line/band brightness Sol Azimuth 181 Solar azimuth angle 193 Galact Lon Galactic longitude b (galactic coords) KHA rel annr emis rate w/o flatfld norm 4145 KHA relert1 Local standard of rest velocity (VLSR) 2415 VLSR rest V Shadow Dist 188 Shadow distance (l-o-s terminator dist) 195 Galactic latitude l (galactic coords) Galact Lat 192 Right ascension RA (equatorial coords) Rt Asc A KHA astrnam 4141 KHA observation loc (astronomical name) KHA beginning hour/min (UT) from log 4142 KHA blgUThm ERROR FOR KHA rel annr emis rate w/o flatfld norm error KHA relert3 -4146 KHA relert3 KHA rel annr emis rate w/o flatfld norm 4146 RelEmisRt3 Relative emission rate 2509 http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:kha Kitt Pk H-alpha Fabry-Perot 5190 Vn tides LTCS period analysis 1210_17999 http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:sbf SBF The Scott Base MF radar (78 S, 167 E) in Antarctica is operated by the Physics Department of the University of Canterbury, Christchurch, New Zealand. It uses the partial-reflection, spaced antenna method (Fraser, 1984b) and has contributed to mean wind and tidal studies (Avery et al, 1989; Fraser 1984a, 1989; Fraser et al 1989; Manson et al., 1989, 1990, 1991). The mean solar local time (SLT) is about 11 hours and 8 minutes ahead of Universal Time (UT) (i.e., 167 E / 15 deg/hr = 11.13 hours = 11 hrs 8 min). The phases are in SLT. Scott Base Antarctica MF Radar 1210 5240 http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:fpf The dispersing elements of the spectrometers are air-spaced, 14 cm diameter effective clear-aperture Fabry-Perot interferometers, which are self-aligning and self-stabilizing (Hernandez and Mills, 1973). The instruments were operated at the optimum point for kinetic temperature determinations (Hernandez, 1979; 1988). The spectrometers operated with narrow (<0.3 nm wide) interference filters -a necessity, in particular, for the 630.0 nm emission, in order to avoid contamination from the nearby OH emission lines (Hernandez, 1974). The inherent stability of the spectrometers is about 0.5 m/s (632.8 nm) for periods of months, because of their self-stabilizing properties. The instrumental internal stability calibration is updated every 9 s throughout the day, year round. The spectrometer observed wavelengths with these Fritz Peak instruments have been the so-called red line (630.0 nm, kindat=17001, 1973-1985) and green line (557.7 nm, kindat=17002, 1969-1985) of atomic oxygen (OI) with typical emission height peaks in the range 210 to 300 km and 94-98 km, respectively. Each spectrometer observed a different wavelength. The spectrometers observed the night-sky at the 4 cardinal directions at 20-degree elevation above the horizon, as well as zenith. Since the instruments are light-limited, the time spent in observing this 5-direction cycle can be as short as 5 minutes during auroral activity. The instrument is internally time-limited to spend no less that one-minute and no more than 15 minutes in any given direction. Other observing protocols, such as two orthogonal directions and zenith, have also been used. The observations were made every evening and only those with clear weather -as reported by an observer on site- are reported here. Because of the narrow filters used, operation of the instrument is not affected by moonlight. Typically, about 30% of the nights observed were clear. FPF Fritz Peak CO Fabry-Perot Interf Sp Tn Em Vn -1440 error Vn4 ERROR FOR Direction 4 Neutral wind (perp east) Insert here description of the 5430/17001 operating mode Vn4 Direction 4 Neutral wind (perp east) 1440 Direction 5 Neutral wind horizontl comp 1455 Vn5h ERROR FOR Relative line/band brightness error rel Bright -2505 ERROR FOR Direction 5 Neutral wind horizontl comp error Vn5h -1455 5460_17001 4025 CFP QC No coefficients CFP N Coefs http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:cfp 5460 CFP The College, Alaska Fabry-Perot interferometer was located on the roof of the Geophysical Institute in the years reported here (1981-1983). This is at 64.7N and 148.1W in geographic coordinates, where the corrected geomagnetic coordinates are 64.9N and 100.3W. This is relatively close to the Chatanika incoherent scatter radar site at 65.1N and 147.4W, which operated between 1971 and 1982. The IGRF model gives a magnetic declination angle of about 25 degrees and inclination angle of 76 degrees for the measurement period. However, the measurements were made relative to the magnetic field direction where the declination was assumed to be 30 degrees. This is not significantly different from the true declination, so the derived horizontal results are reported as being in the magnetic directions. The measurements are all at 630.0 nm. All nights included are clear, or had cloudy periods removed. The zenith measurements are assumed to be on average zero throughout the night. All other measurements were taken in directions relative to the magnetic E, N, W and S directions at elevations angles between 20 and 45 degrees, and were converted to horizontal directions assuming an emission layer centered at 225 km. The intensities are relative, (Code 2505) but are approximately within 25% of the true intensities in Rayleighs. College Fabry-Perot 3320 http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:wup Wuppertal Germany OH Spectrometer 3320_17004 Tn nightly averages The Wuppertal, Germany (51.3N, 7.2E) Czerny-Turner grating spectrometer scans in the near infrared between 1.05 - 1.74 um with a spectral resolution of about 450. It has been operated by the University of Wuppertal since 1980. The instrument measures the nightglow hydroxyl [OH*]. The [OH*] emission layer is centered near 87 km (+/-2 km) with a thickness of about 9 km. Measured parameters are the hydroxyl Meinel band rotational temperature (Code 812) in tenths of Kelvin. To reduce NLTE effects as much as possible, the (3,1) transition lines P1(2), P1(3) and P1(4) near 1.5 um are chosen for the measurements. More than 3100 average nightly mean temperatures are available continously from July 1980 until now with a gap in 1985/86. The instrument field-of-view in the zenith has a horizontal resolution of 20x20 km^2 (with respect to 86 km altitude). One spectrum is measured in 90 s. Rotational temperatures are derived from the relative intensities of the three lines. Hence, if there should be changes of spectrometer sensitivity, atmospheric transmission, or other factors the derived temperatures would not be affected unless such changes are wavelength dependent. Even in that case, influences would be small because the three line are close together (1.524 um, 1.533 um, 1.543 um). The relative error of nightly mean temperature values is estimated to be 1-2 K. This is derived from measurements during the whole night, and therefore, it still contains some atmospheric variability. Thus, the value must be considered as an upper limit for the relative error. The absolute temperature error is of the same magnitude. Spectral and absolute intensity calibrations are performed about once per year. WUP Vn tides LTCS period analysis 2090_17999 2-dy northward neutrl wind amplitude 2dy Vnn Amp 971 2-dy eastward neutral wind amplitude 970 2dy Vne Amp -971 ERROR FOR 2-dy northward neutrl wind amplitude error 2dy Vnn Amp 2-day component period 2dy Period 980 -976 ERROR FOR 2-dy max northward neutrl wind phase error 2dy Vnn Phs ERROR FOR 2-dy max eastward neutral wind phase -975 error 2dy Vne Phs Vn tides normal analysis 976 2-dy max northward neutrl wind phase 2dy Vnn Phs error 2dy Vne Amp ERROR FOR 2-dy eastward neutral wind amplitude -970 2-dy max eastward neutral wind phase 2dy Vne Phs 975 2090_17001 982 BegUT 2dcal UT at start of 2-day comp calc UT day no rel to 2-dy comp phase 981 d# 2d Phase Christmas Island ST (MEDAC) Radar http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:cia CIA The Christmas Island ST (MEDAC) radar is located at (1.95N, 157.30W). The MEDAC (Meteor Echo Detection And Collection) sytem added to the ST (STratospheric) radar makes observations of winds measured from the backscatter off meteor trails. The system is described in Avery et al. (1990). The observations are described in solar local time, which is defined to be 10 hours and 32 minutes after UT (-158/15 = -10.53 or 10 hours and 32 minutes, where the longitude used was 158 W instead of 157.30 W). These are monthly means corresponding to the day numbers given. The days are counted from Hawaiian Standard Time (= UT-10h). Hence, data starting on the first of the month actually starts at 10 UT on the first of the month, and data ending at the end of the month ends on the first day of the next month at 0959 UT. This data set is two years of data from September 1988 to August 1989, and for all of 1991. The analysis will be revised in the future. 2090 Syowa East (Antarctica) HF Radar The Syowa East HF radar is located in Antarctica (69.00 deg S, 39.58 deg E) and looks over a section of ionosphere poleward of 70 deg S that includes the east Antarctica ice cap and the southern ocean. It has operated since 1997. The facility is part of the SuperDARN network of HF radars that extends from Alaska to Scandinavia in the Northern hemisphere and covers much of Antarctica in the Southern hemisphere. The SuperDARN radar for the most direct 2-D merging of Syowa velocity data is located at Kerguelen. The radar forms and steers its beam by the phasing of transmissions from 16 elements in a linear antenna array. A second 4-element array provide the capability to measure elevation angle. The basic radar operation consists of the following steps: i) selection of a beam position (0-15) ii) search for the quietest 5-kHz channel about the assigned transmitting frequency (8-20 MHz) iii) repeated transmission of a multi-pulse sequence over the selected integration period and reception of backscattered signal with gating in range (1-70) iv) calculation of the auto-correlation functions (ACFs). These operations are usually carried out in sequence for the 16 beam positions, which collectively constitute 1 scan. The beam integration period is usually 7 sec, and the scan repeat time is then 120 sec (2 min). Within a scan, beam 0 corresponds to the most westward beam position and beam 15 to the most eastward. The azimuth sector scanned is approximately 50 deg wide and is centered on 107.0 deg E of N, or about 52 degrees east of the look direction for Syowa South. http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:sye SYE 831 Vi 831_7001 The Stockholm, Sweden (59.5N, 18.2E) IR Michelson Interferometer (IRMI) scans in the near infrared between wavenumbers 6000 to 10,000 cm-1 (or in the range of 1000-1667 nm in wavelength), with a 4 cm-1 resolution (or 0.1% resolution, about 0.3 nm). The instrument is operated by Utah State University with support from Stockholm University. The instrument measures the nightglow hydroxyl [OH]. The [OH] emission layer is centered near 87 km with a thickness of about 8 km. The center of the layer can vary between about 86 and 89 km, giving an error bar in the altitude of about +/6 km considering the thickness also. The rotational temperatures reflect the neutral temperatures in this altitude region. The measured parameters are the hydroxyl Meinel band rotational temperature in Kelvin and the hydroxyl Meinel integrated band radiance in kR and in log10(R). http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:stm STM 5860 Stockholm Sweden IR Michelson Interfer. Tn ERROR FOR STM QC Solar scaling factor -4080 error STM sol scl 5860_17001 STM QC Solar scaling factor 4080 STM sol scl Log10 (background noise, residual) 2560 lg(BkgNois) http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:pkf PKF PKF QC perp (left) compon. to code 4111 4112 PKF fitpvnl 4111 PKF fithlos PKF QC neut horiz wind fit los to az dir 2561 lg(BkgCnts) log10 (background counts) -2561 error lg(BkgCnts) ERROR FOR log10 (background counts) 5465_17001 Tn Em Vn error lg(Counts) ERROR FOR log10 (Counts) -2491 lg(Counts) log10 (Counts) 2491 Poker Flat AK Scanning Imaging F-P Spec 5465 The all-sky scanning imaging Fabry-Perot Spectrometer (ASIFPS) at Poker Flat, Alaska (65.12N, 147.43W) is also known as a Scanning Doppler Instrument (SDI). It is an extremely high resolution optical imaging spectrometer. It measures the angular distribution of Doppler shifts and of Doppler broadening of optical airglow and auroral light emitted from the Earth's upper atmosphere, across the entire sky scene that is visible to the gorund-based instrument, down to a zenith angle of ~75 deg. The distributions of Doppler shifts and of Doppler broadening across the sky are used to infer geographic maps of the wind and temperature distributions prevailing within the emission layer. The instrument is located on a ridge-top, 50 km ENE from Fairbanks and at 440 m above mean sea level. It has been operated since November 1994 by the Geophysical Institute of the University of Alaska as part of the optical diagnostic instruments at the Poker Flat Research Range. The building is aligned in the magnetic north direction at 28.5 degrees azimuth to NE. The apex magnetic coordinates of Poker Flat in December 2001 at 240 km were (65.25, -95.41), with a magnetic declination of 23.56 deg to NE, an inclination of 77.36 deg to SW, and 0 UT at 1231 MLT. At 96 km, apex coordinates are (65.23, -95.45), with a magnetic declination of 24.28 deg, an inclination of 77.37 deg, and 0 UT at 1231 MLT. The observations are reported in approximate local magnetic coordinates, rotated 28.5 degrees clockwise from geographic, and also in geographic coordinates. The magnetic skew angle (code 1020) is about 4.6 deg, which is negligible. The instrument is based on a 100-mm aperture capacitance-stabilized Fabry-Perot etalon, the plates of which are piezoelectrically scannable in spacing over approximately 1.5 orders of interference (at 630-nm) about a nominal 20-mm gap. Skylight is coupled into the etalon through an all-sky lens and optical relay system which maps an approximately 75-degree half-angle field-of-view onto 6 orders of interference at the etalon. Interference fringes formed by the etalon are conjugate with the sky. The sky, modulated by this fringe pattern, is re-imaged onto an intensified CCD detector, after first passing through a narrow-band interference filter. http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:whf 910_7001 Vi 910 The Stokkseyri HF radar is located in western Iceland (63.86 deg N, -22.02 deg E) and looks to the west over a section of ionosphere that includes southern Greenland and northeastern Canada. It has operated since 1994. The facility is part of the SuperDARN network of HF radars that extends from western North America to Scandinavia in the Northern hemisphere and covers much of Antarctica in the Southern hemisphere. The SuperDARN radar for the most direct 2-D merging of Stokkseyri velocity data is located at Goose Bay in Canada. The radar forms and steers its beam by the phasing of transmissions from 16 elements in a linear antenna array. A second 4-element array provides the capability to measure elevation angle. The basic radar operation consists of the following steps: i) selection of a beam position (0-15), ii) search for the quietest 5-kHz channel about the assigned transmitting frequency (8-20 MHz), iii) repeated transmission of a multi-pulse sequence over the selected integration period and reception of backscattered signal with gating in range (1-70), and iv) calculation of the auto-correlation functions (ACFs). These operations are usually carried out in sequence for the 16 beam positions, which collectively constitute 1 scan. The beam integration period is typically 6 or 7 sec, and the scan repeat time is 96 sec or 120 sec. Within a scan, beam 0 corresponds to the most westward beam position and beam 15 to the most eastward. The azimuth sector scanned is westward approximately 50 deg wide and is centered on -59 deg E of N. Stokkseyri (Iceland West) HF Radar WHF Ascension Island Meteor RADAR 1539 http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:mltr The Ascension Island (7.96 S, 14.38 W; alt 170 m) 43.50 MHz meteor radar has been in operation since August 1999. On day 359 of 2001 at 89 km altitude, the apex magnetic coordinates were (-19.6, 55.0) degrees. The magnetic inclination and declination angles were -39.3 deg and -16.8 deg. The magnetic local time at 0 Universal Time (UT) is about 2235 MLT. The solar local time (SLT) is UT minus 58 minutes (14.38/15=0.959). Vn tides 4-day CEDAR/TIMED analysis 1539_17100 ASC SON Mean azimuth position 1 Azm pos 1 3518 Elm pos 2 SON Mean elevation position 2 3521 SON Mean azimuth position 2 Azm pos 2 3520 80_15413 Invariant latitude in measurement vol Inv Lat 222 Ne Te Ti Vi Ef LTCS F reg long pulse 3519 SON Mean elevation position 1 Elm pos 1 2150 Joule energy heat rate height integral Qjoulh error Qjoulh -2150 ERROR FOR Joule energy heat rate height integral Ln int J5 Line int (1 hemi): dir 5 current den 1950 80_15022 Vi Ef Je Qj -1950 error Ln int J5 ERROR FOR Line int (1 hemi): dir 5 current den axis of sym 3597 SON Azimuth of axis of symmetry -1940 ERROR FOR Line int (1 hemi): dir 4 current den error Ln int J4 Ln int J4 1940 Line int (1 hemi): dir 4 current den 3599 SON Direction 4 F Region ion velocity Vi4F 830 lg(Mn) log10 (neutral mass density) error Vn6 -1460 ERROR FOR Direction 6 Neutral wind 840 lg(Nn) log10 (neutral number density) ERROR FOR SON Direction 4 F Region ion velocity -3599 error Vi4F 3600 Vi5F SON Direction 5 F Region ion velocity lg(Hl Cond) log10 (Hall Conductivity) 2021 error Vi5F ERROR FOR SON Direction 5 F Region ion velocity -3600 -1850 error J5 ERROR FOR Direction 5 electric current density 3576 SON Cross correlation coefficient Uxy xccof Uxy 80_15116 Direction 6 Neutral wind Vn6 1460 SON Correlation coefficient vxy c cof xy 3571 J5 1850 Direction 5 electric current density Ne Nn Tn Vi Vn Ef Je Sg LTCS E reg electrodyn ERROR FOR Direction 4 electric current density error J4 -1840 log10 (Pedersen Conductivity) 2011 lg(Pd Cond) 3596 SON Ion gyro frequency ion g freq 1450 Vn5 Direction 5 Neutral wind (perp north) SON Relative error in neutral atmos 3595 signeut SON Correlation coefficient Exy 3575 c cof Exy Direction 4 electric current density 1840 J4 error Vn5 ERROR FOR Direction 5 Neutral wind (perp north) -1450 949 24h Ti Phs 24-h max ion temperature phase 944 24h Ti Amp 24-h ion temperature amplitude 80_15999 Ti Vn tides LTCS error 24h Ti Amp ERROR FOR 24-h ion temperature amplitude -944 ERROR FOR 24-h max ion temperature phase -949 error 24h Ti Phs 3592 SON Error on Un from signeut unneute xccof Uenn SON Cross correlatn on Une from signeut 3580 uxneute SON Error on Ux from signeut 3587 uyneute SON Error on Uy from signeut 3588 uxcorr 3585 SON Correction term = Ux-Vx 3591 ueneute SON Error on Ue from signeut ERROR FOR SON Correction term = Uy-Vy error uycorr -3586 3579 xccof Uxyt SON Total cross correlation for Uxy SON Horizontal magn neutral wind 3582 Umerid siguztot SON Total error on Uzum (code 1460) 3584 log10 (joule energy spec. heat rate) 2121 lg(Qjoulv) SON Total error on Uy siguytot 3590 SON Cross correlatn on Uxy from signeut 3578 xccof Uxyn Ne Nn Te Ti Tn Vi Vn Ef LTCS E reg neu dyn 3583 Uzneute SON Alternate error on Uzum (code 1460) siguetot SON Total error on Ue 3593 80_15115 3581 xccof Uent SON Total cross correlatn for Ue and Un 3586 uycorr SON Correction term = Uy-Vy 3589 siguxtot SON Total error on Ux ERROR FOR SON Horizontal magn neutral wind -3582 error Umerid -3585 ERROR FOR SON Correction term = Ux-Vx error uxcorr 3594 siguntot SON Total error on Un 3577 SON Cross correlation coefficient Une xccof Uen CHT/SON QC1 Chatanika/Sondrestrom data qual code 1 471 Nu Ne Ni Te Ti Vi 473 Fit Code MUSCOX Fit Code 80_5502 Field line integral(1 hemi) Hall Cond 2080 LnInt HallC 80_15620 Ef Je Sg 2070 LnInt Ped C Field line integral(1 hemi) Ped Cond 80_9003 Nu End pos flg 97 End of event flag (0=off, 1=on) Ne Ni Te Ti Vi LTCS 80_15014 c cof xz SON Correlation coefficient vxz 3572 3573 SON Correlation coefficient vyz c cof yz 80_9002 Nu Ne Te Ti Vi Ef cwinds 3-pos long pulse 80_15613 80_5523 Nu Ne Ni Te Ti Vi acport ac elscans 80_19120 Vi Ef Je Sg 80_5100 Ne 80_5526 Nu Ne Ni Te Ti Vi 80_5152 Ne 80_15013 Ne Ni Te Ti Vi Ef LTCS F region The incoherent scatter transmitter station at Kangerlussuaq (Sondrestrom), Greenland (66.99N, 50.95W, 185m ASL) has been in operation since February, 1983. It was moved from Chatanika, Alaska in 1982-1983, where it operated from July 1971 to March 1982. On day 359 of 2001 at 110 km altitude, the apex magnetic coordinates were (73.0, 40.5) degrees. The magnetic inclination and declination angles were 80.1 deg and -35.2 deg. The magnetic local time at 0000 Universal Time (UT) is about 2137 MLT. The solar local time (SLT) is UT minus 3 hours and 24 minutes (-50.95/15.=-3.397). 80_9001 Nu 80_15100 Te Ti Tn Vi Vn 80_5521 Nu Ne Ni Te Ti Vi XY |Vel.| 3626 SON Vector Velocity Magnitude (XY plane) Vi Ef Viperp(ht,mlat), Vipar=0 80_15610 -3627 ERROR FOR SON CW angle from GM North for 3626-XY error nangle 474 RV Pair CD Res. Vel. Pairing Code ERROR FOR SON Vector Velocity Magnitude (XY plane) -3626 error XY |Vel.| 3627 SON CW angle from GM North for 3626-XY nangle SON 80_5124 Te Ti