A Directory containing Daily FTP downloadable Files containing Readout-by-Readout Listings of the Counts accumulated in the H1-H27 Spin-Averaged Counting Rates. The Rates H10-H13 are Coincidence Counting Rates corresponding primarily to Heavy Nuclei (Z>2) with Penetrating Power equivalent to Carbon-12 Nuclei in the approximate Energy Ranges 26-36, 44-127, 127-173, and >173 MeV/n, respectively. H14-H27 are single Detector Counting Rates giving, in order, the total Number of Counts above the lowest level Discriminator Thresholds of Detectors D1-D6, K1-K6 (or D7-D12), A (or D13), and the Anti-Coincidence Scintillator S. The single Detector Counting Rates are provided simply to assess the Health of the Detectors and are of little use scientifically. The Naming Convention for the Daily Files is uly_het_full_rat_omni2_YYYDDD.txt, where YYY indicates the three digit Year since 1900 (e.g. YYY=090 for 1990, and YYY=102 for 2002) and DDD indicates the three digit Day of Year (January 1 = 1). In each File, following a detailed Description of the Format, the Data consist of a Listing of Counts accumulated in the H10-H27 Spin-Averaged Counting Rates during the Intervals between successive Readouts, organized into Columns as described below. The first four Columns give the Start Time of the Counting Rate Accumulation Period as Fractional Year (to 12 Decimal Places) and as Year since 1900, Day of Year, and Milliseconds of Day at the Start of the Accumulation, followed by one Column giving the Duration of the Accumulation Period in Milliseconds (it is the same for all Rates except H13, which is read out twice in each Accumulation Period, and is thus represented as H13a and H13b, see below and embedded Documentation in each Daily File), and 19 Columns giving the Counts accumulated in that Period for each Rate. All Fields except for the Fractional Year are in Integer Format. The Start Time for H13a is the Time given as the Start Time for the Line, but (to sufficient accuracy) its Accumulation Period is half the Period given under "Coverage". Again, to sufficient accuracy, the Start Time for H13b is the Time given plus half the Accumulation Period, and the Accumulation Period for H13b is half the Period given under "Coverage". Each Line contains Data for one single Readout of the Rates H10-H12, H13a, H13b, and H14-H27. All Readouts where at least one of the Rates has a Non-fill Value are included. Where Fill does occur it is indicated by -1. Since the Accumulation Period for each Readout is forced to include an Integral Number of Spacecraft Spins in order to produce pure Spin-Averaged Measurements, the Lengths of the Accumulation Periods vary in a Cyclic Manner as the Period of the Telemetry Cycle beats with the Spacecraft Spin Period. At the most common Science Telemetry Rate, 2048 bps, each Rate in this File is Readout on average once every 128 s, except for H13 which is Readout on average twice in every 128 s. At 2048 bps, the Cycle of Accumulation Periods is 132, 132, 120, 132, 132,, 120, 132, etc., seconds. No Noise Removal or Despiking has been done, so Caution must be used in interpreting isolated large Increases or Decreases in the Counting Rates.
Version:2.2.9
A Directory containing Daily FTP downloadable Files containing Readout-by-Readout Listings of the Counts accumulated in the H1-H27 Spin-Averaged Counting Rates. The Rates H10-H13 are Coincidence Counting Rates corresponding primarily to Heavy Nuclei (Z>2) with Penetrating Power equivalent to Carbon-12 Nuclei in the approximate Energy Ranges 26-36, 44-127, 127-173, and >173 MeV/n, respectively. H14-H27 are single Detector Counting Rates giving, in order, the total Number of Counts above the lowest level Discriminator Thresholds of Detectors D1-D6, K1-K6 (or D7-D12), A (or D13), and the Anti-Coincidence Scintillator S. The single Detector Counting Rates are provided simply to assess the Health of the Detectors and are of little use scientifically. The Naming Convention for the Daily Files is uly_het_full_rat_omni2_YYYDDD.txt, where YYY indicates the three digit Year since 1900 (e.g. YYY=090 for 1990, and YYY=102 for 2002) and DDD indicates the three digit Day of Year (January 1 = 1). In each File, following a detailed Description of the Format, the Data consist of a Listing of Counts accumulated in the H10-H27 Spin-Averaged Counting Rates during the Intervals between successive Readouts, organized into Columns as described below. The first four Columns give the Start Time of the Counting Rate Accumulation Period as Fractional Year (to 12 Decimal Places) and as Year since 1900, Day of Year, and Milliseconds of Day at the Start of the Accumulation, followed by one Column giving the Duration of the Accumulation Period in Milliseconds (it is the same for all Rates except H13, which is read out twice in each Accumulation Period, and is thus represented as H13a and H13b, see below and embedded Documentation in each Daily File), and 19 Columns giving the Counts accumulated in that Period for each Rate. All Fields except for the Fractional Year are in Integer Format. The Start Time for H13a is the Time given as the Start Time for the Line, but (to sufficient accuracy) its Accumulation Period is half the Period given under "Coverage". Again, to sufficient accuracy, the Start Time for H13b is the Time given plus half the Accumulation Period, and the Accumulation Period for H13b is half the Period given under "Coverage". Each Line contains Data for one single Readout of the Rates H10-H12, H13a, H13b, and H14-H27. All Readouts where at least one of the Rates has a Non-fill Value are included. Where Fill does occur it is indicated by -1. Since the Accumulation Period for each Readout is forced to include an Integral Number of Spacecraft Spins in order to produce pure Spin-Averaged Measurements, the Lengths of the Accumulation Periods vary in a Cyclic Manner as the Period of the Telemetry Cycle beats with the Spacecraft Spin Period. At the most common Science Telemetry Rate, 2048 bps, each Rate in this File is Readout on average once every 128 s, except for H13 which is Readout on average twice in every 128 s. At 2048 bps, the Cycle of Accumulation Periods is 132, 132, 120, 132, 132,, 120, 132, etc., seconds. No Noise Removal or Despiking has been done, so Caution must be used in interpreting isolated large Increases or Decreases in the Counting Rates.
| Role | Person | StartDate | StopDate | Note | |
|---|---|---|---|---|---|
| 1. | PrincipalInvestigator TeamLeader | spase://SMWG/Person/R.Bruce.McKibben | |||
| 2. | DataProducer | spase://SMWG/Person/Clifford.Lopate | |||
| 3. | CoInvestigator | spase://SMWG/Person/James.Connell |
Published Description of the COSPIN Instrumentation, J.A. Simpson et al., Astron. Astrophys. Suppl. Ser. 92, 365-399, 1992. See especially Section 4.3 for a detailed Description of the High Energy Telescopes, HET. An electronic Copy of this Paper is available at http://adsbit.harvard.edu/cgi-bin/nph-iarticle_query?1992A%26AS...92..365S&defaultprint=YES&filetype=.pdf.
The User Notes File at the Ulysses Final Archive (UFA) describes the Format of the ASCII Data Files for the COSPIN High Energy Telescope, HET
Top Level Descriptions of Formats and Contents of the six File Types that make up the COSPIN HET Full Resolution Data Set. Detailed Descriptions of the Formats and Contents are found in Header Lines at the Start of each downloaded Data File. The Data covered by this SPASE Description are described in the ReadMe under the Heading omni2. (*** Note ***: During the Build-up of this Data Set, a few Errors and Omissions have been found in the Header Lines for some of the File Types. These Errors and Omissions are listed in this ReadMe File. Upon Completion of the Data Set, all Errors and Omissions discovered will be corrected in all of the Header Lines of all of the File Types at which time this Note will be removed).
Parent Directory containing FTP downloadable Daily Files with the Format described below
Nominal Start Time for the average given in decimal year, integer year, Day of Year, and Milliseconds of Day.
Length of the accumulation period in milli-seconds.
Counts accumulated by counting rate H10 during the period of coverage (column 5) starting at the time defined in columns 1-4. The H10 counting rate normally responds primarily to nuclei with Z>2 with penetrating power equivalent to 26-36 MeV/n Carbon-12 nuclei. Protons, helium nuclei, and electrons are excluded by discriminators requiring an energy deposit in at least one detector greater than can be produced by a Z=2 nucleus.
Counts accumulated by counting rate H11 during the period of coverage (column 5) starting at the time defined in columns 1-4. The H11 counting rate normally responds primarily to nuclei with Z>2 with penetrating power equivalent to 44-127 MeV/n Carbon-12 nuclei. Protons, helium nuclei, and electrons are excluded by discriminators requiring an energy deposit in at least one detector greater than can be produced by a Z=2 nucleus.
Counts accumulated by counting rate H12 during the period of coverage (column 5) starting at the time defined in columns 1-4. The H12 counting rate normally responds primarily to nuclei with Z>2 with penetrating power equivalent to 127-173 MeV/n Carbon-12 nuclei. Protons, helium nuclei, and electrons are excluded by discriminators requiring an energy deposit in at least one detector greater than can be produced by a Z=2 nucleus.
Counts accumulated by counting rate H13a during the first half of the period of coverage (column 5) starting at the time defined in columns 1-4. The H13a counting rate normally responds primarily to nuclei with Z>2 with penetrating power equivalent to Carbon-12 nuclei with energies greater than 173 MeV/n. Such nuclei completely penetrate the telescope. Therefore, the H13 is also sensitive, above a poorly known energy threshold, to nuclei going backward through the HET after penetrating the spacecraft structures and other instruments that lie behind the HET on the spacecraft. Protons, helium nuclei, and electrons are excluded by discriminators requiring an energy deposit in at least one detector greater than can be produced by a Z=2 nucleus.
H13b is identical to H13a except that it accumulates counts during the second half of the period of coverage (column 5) starting at the time defined in columns 1-4. Thus the start time for the H13b accumulation is the time in columns 1-4 plus half coverage interval listed in column 5. All other considerations described for H13a apply equally to H13b.
H14 registers the total number of counts above the lowest level threshold in detector D1 of the HET during the accumulation period (column 5) starting at the time defined in columns 1-4. No coincidence conditions are applied, so no particle identification can be made, nor can any energy range be defined other than that the particle (or gamma ray) must be able to reach the detector either through the telescope aperture and overlying detector stack, or through the side of the telescope and any spacecraft or instrument structure in its path. Consequently, the counting rate is most often dominated by high energy cosmic rays and by electrons produced by Gamma Rays in the telescope.
H15 registers the total number of counts above the lowest level threshold in detector D2 of the HET during the accumulation period (column 5) starting at the time defined in columns 1-4. No coincidence conditions are applied, so no particle identification can be made, nor can any energy range be defined other than that the particle (or gamma ray) must be able to reach the detector either through the telescope aperture and overlying detector stack, or through the side of the telescope and any spacecraft or instrument structure in its path. Consequently, the counting rate is most often dominated by high energy cosmic rays and by electrons produced by Gamma Rays in the telescope.
H16 registers the total number of counts above the lowest level threshold in detector D3 of the HET during the accumulation period (column 5) starting at the time defined in columns 1-4. No coincidence conditions are applied, so no particle identification can be made, nor can any energy range be defined other than that the particle (or gamma ray) must be able to reach the detector either through the telescope aperture and overlying detector stack, or through the side of the telescope and any spacecraft or instrument structure in its path. Consequently, the counting rate is most often dominated by high energy cosmic rays and by electrons produced by Gamma Rays in the telescope.
H17 registers the total number of counts above the lowest level threshold in detector D4 of the HET during the accumulation period (column 5) starting at the time defined in columns 1-4. No coincidence conditions are applied, so no particle identification can be made, nor can any energy range be defined other than that the particle (or gamma ray) must be able to reach the detector either through the telescope aperture and overlying detector stack, or through the side of the telescope and any spacecraft or instrument structure in its path. Consequently, the counting rate is most often dominated by high energy cosmic rays and by electrons produced by Gamma Rays in the telescope.
H18 registers the total number of counts above the lowest level threshold in detector D5 of the HET during the accumulation period (column 5) starting at the time defined in columns 1-4. No coincidence conditions are applied, so no particle identification can be made, nor can any energy range be defined other than that the particle (or gamma ray) must be able to reach the detector either through the telescope aperture and overlying detector stack, or through the side of the telescope and any spacecraft or instrument structure in its path. Consequently, the counting rate is most often dominated by high energy cosmic rays and by electrons produced by Gamma Rays in the telescope.
H19 registers the total number of counts above the lowest level threshold in detector D6 of the HET during the accumulation period (column 5) starting at the time defined in columns 1-4. No coincidence conditions are applied, so no particle identification can be made, nor can any energy range be defined other than that the particle (or gamma ray) must be able to reach the detector either through the telescope aperture and overlying detector stack, or through the side of the telescope and any spacecraft or instrument structure in its path. Consequently, the counting rate is most often dominated by high energy cosmic rays and by electrons produced by Gamma Rays in the telescope.
H20 registers the total number of counts above the lowest level threshold in detector K1 (D7) of the HET during the accumulation period (column 5) starting at the time defined in columns 1-4. No coincidence conditions are applied, so no particle identification can be made, nor can any energy range be defined other than that the particle (or gamma ray) must be able to reach the detector either through the telescope aperture and overlying detector stack, or through the side of the telescope and any spacecraft or instrument structure in its path. Consequently, the counting rate is most often dominated by high energy cosmic rays and by electrons produced by Gamma Rays in the telescope.
H21 registers the total number of counts above the lowest level threshold in detector K2 (D8) of the HET during the accumulation period (column 5) starting at the time defined in columns 1-4. No coincidence conditions are applied, so no particle identification can be made, nor can any energy range be defined other than that the particle (or gamma ray) must be able to reach the detector either through the telescope aperture and overlying detector stack, or through the side of the telescope and any spacecraft or instrument structure in its path. Consequently, the counting rate is most often dominated by high energy cosmic rays and by electrons produced by Gamma Rays in the telescope.
H22 registers the total number of counts above the lowest level threshold in detector K3 (D9) of the HET during the accumulation period (column 5) starting at the time defined in columns 1-4. No coincidence conditions are applied, so no particle identification can be made, nor can any energy range be defined other than that the particle (or gamma ray) must be able to reach the detector either through the telescope aperture and overlying detector stack, or through the side of the telescope and any spacecraft or instrument structure in its path. Consequently, the counting rate is most often dominated by high energy cosmic rays and by electrons produced by Gamma Rays in the telescope.
H23 registers the total number of counts above the lowest level threshold in detector K4 (D10) of the HET during the accumulation period (column 5) starting at the time defined in columns 1-4. No coincidence conditions are applied, so no particle identification can be made, nor can any energy range be defined other than that the particle (or gamma ray) must be able to reach the detector either through the telescope aperture and overlying detector stack, or through the side of the telescope and any spacecraft or instrument structure in its path. Consequently, the counting rate is most often dominated by high energy cosmic rays and by electrons produced by Gamma Rays in the telescope.
H24 registers the total number of counts above the lowest level threshold in detector K5 (D11) of the HET during the accumulation period (column 5) starting at the time defined in columns 1-4. No coincidence conditions are applied, so no particle identification can be made, nor can any energy range be defined other than that the particle (or gamma ray) must be able to reach the detector either through the telescope aperture and overlying detector stack, or through the side of the telescope and any spacecraft or instrument structure in its path. Consequently, the counting rate is most often dominated by high energy cosmic rays and by electrons produced by Gamma Rays in the telescope.
H25 registers the total number of counts above the lowest level threshold in detector K6 (D12) of the HET during the accumulation period (column 5) starting at the time defined in columns 1-4. No coincidence conditions are applied, so no particle identification can be made, nor can any energy range be defined other than that the particle (or gamma ray) must be able to reach the detector either through the telescope aperture and overlying detector stack, or through the side of the telescope and any spacecraft or instrument structure in its path. Consequently, the counting rate is most often dominated by high energy cosmic rays and by electrons produced by Gamma Rays in the telescope.
H26 registers the total number of counts above threshold in detector A (D13) of the HET during the accumulation period (column 5) starting at the time defined in columns 1-4. No coincidence conditions are applied, so no particle identification can be made, nor can any energy range be defined other than that the particle (or gamma ray) must be able to reach the detector either through the telescope aperture and overlying detector stack, or through the side of the telescope and any spacecraft or instrument structure in its path. Consequently, the counting rate is most often dominated by high energy cosmic rays and by electrons produced by Gamma Rays in the telescope.
H27 registers the total number of counts above threshold in the Anti-Coincidence plastic scintillator, S, that surrounds the HET detector stack during the accumulation period (column 5) starting at the time defined in columns 1-4. No coincidence conditions are applied, so no particle identification can be made, nor can any energy range be defined other than that the particle (or gamma ray) must be able to reach the detector either through the telescope aperture and overlying detector stack, or through the side of the telescope and any spacecraft or instrument structure in its path. Consequently, the counting rate is most often dominated by high energy cosmic rays and by electrons produced by Gamma Rays in the telescope.