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FIGURES 368–375. Pinodytes setosus. 368. Male right antenna, dorsal. 369. Male right protibia and protarsus. 370. Male right mesotibia. 371. Male right metafemur and metatibia. 372. Aedeagus, lateral. 373. Aedeagus, dorsal. 374. Spermatheca. 375 in Systematics, distributions and bionomics of the Catopocerini (eyeless soil fungivore beetles) of North America (Coleoptera: Leiodidae: Catopocerinae) 3077
FIGURES 368–375. Pinodytes setosus. 368. Male right antenna, dorsal. 369. Male right protibia and protarsus. 370. Male right mesotibia. 371. Male right metafemur and metatibia. 372. Aedeagus, lateral. 373. Aedeagus, dorsal. 374. Spermatheca. 375. Mesoventrite, lateral; dotted line indicates area of setal patch. Scale bar = 0.1 mm (Fig. 374), 0.3 mm (Figs. 372, 373, 375), 0.4 mm (Figs. 368–371).
FIGURES 233–240. Pinodytes spinus. 233. Male right antenna, dorsal. 234. Male right protibia and protarsus. 235. Male right mesotibia. 236. Male right metafemur and metatibia. 237. Aedeagus, lateral. 238. Aedeagus, dorsal. 239. Spermatheca. 240 in Systematics, distributions and bionomics of the Catopocerini (eyeless soil fungivore beetles) of North America (Coleoptera: Leiodidae: Catopocerinae) 3077
FIGURES 233–240. Pinodytes spinus. 233. Male right antenna, dorsal. 234. Male right protibia and protarsus. 235. Male right mesotibia. 236. Male right metafemur and metatibia. 237. Aedeagus, lateral. 238. Aedeagus, dorsal. 239. Spermatheca. 240. Mesoventrite, lateral. Scale bar = 0.15 mm (Fig. 239), 0.3 mm (Figs. 233–238, 240).
FIGURES 216–223. Pinodytes sequoia. 216. Male right antenna, dorsal. 217. Male right protibia and protarsus. 218. Male right mesotibia. 219. Male right metafemur and metatibia. 220. Aedeagus, lateral. 221. Aedeagus, dorsal. 222. Spermatheca. 223 in Systematics, distributions and bionomics of the Catopocerini (eyeless soil fungivore beetles) of North America (Coleoptera: Leiodidae: Catopocerinae) 3077
FIGURES 216–223. Pinodytes sequoia. 216. Male right antenna, dorsal. 217. Male right protibia and protarsus. 218. Male right mesotibia. 219. Male right metafemur and metatibia. 220. Aedeagus, lateral. 221. Aedeagus, dorsal. 222. Spermatheca. 223. Mesoventrite, lateral. Scale bar = 0.2 mm (Fig. 222), 0.3 mm (Fig. 223), 0.5 mm (Figs. 216–221).
FIGURES 376–383. Pinodytes shoshone. 376. Male right antenna, dorsal. 377. Male right protibia and protarsus. 378. Male right mesotibia. 379. Male right metafemur and metatibia. 380. Aedeagus, lateral. 381. Aedeagus, dorsal. 382. Spermatheca. 383 in Systematics, distributions and bionomics of the Catopocerini (eyeless soil fungivore beetles) of North America (Coleoptera: Leiodidae: Catopocerinae) 3077
FIGURES 376–383. Pinodytes shoshone. 376. Male right antenna, dorsal. 377. Male right protibia and protarsus. 378. Male right mesotibia. 379. Male right metafemur and metatibia. 380. Aedeagus, lateral. 381. Aedeagus, dorsal. 382. Spermatheca. 383. Mesoventrite, lateral. Scale bar = 0.15 mm (Fig. 382), 0.3 mm (Figs. 381, 383), 0.4 mm (Figs. 377–380), 0.45 mm (Fig. 376).
FIGURES 96–103. Pinodytes chandleri. 96. Male right antenna, dorsal. 97. Male right protibia and protarsus. 98. Male right mesotibia. 99. Male right metafemur and metatibia. 100. Aedeagus, lateral. 101. Aedeagus, dorsal. 102. Spermatheca. 103 in Systematics, distributions and bionomics of the Catopocerini (eyeless soil fungivore beetles) of North America (Coleoptera: Leiodidae: Catopocerinae) 3077
FIGURES 96–103. Pinodytes chandleri. 96. Male right antenna, dorsal. 97. Male right protibia and protarsus. 98. Male right mesotibia. 99. Male right metafemur and metatibia. 100. Aedeagus, lateral. 101. Aedeagus, dorsal. 102. Spermatheca. 103. Mesoventrite, lateral. Scale bar = 0.2 mm (Fig. 102), 0.3 mm (Figs. 96–101, 103).
FIGURES 112–119. Pinodytes contortus. 112. Male right antenna, dorsal. 113. Male right protibia and protarsus. 114. Male right mesotibia. 115. Male right metafemur and metatibia. 116. Aedeagus, lateral. 117. Aedeagus, dorsal. 118. Spermatheca. 119 in Systematics, distributions and bionomics of the Catopocerini (eyeless soil fungivore beetles) of North America (Coleoptera: Leiodidae: Catopocerinae) 3077
FIGURES 112–119. Pinodytes contortus. 112. Male right antenna, dorsal. 113. Male right protibia and protarsus. 114. Male right mesotibia. 115. Male right metafemur and metatibia. 116. Aedeagus, lateral. 117. Aedeagus, dorsal. 118. Spermatheca. 119. Mesoventrite, lateral. Scale bar = 0.1 mm (Fig. 118), 0.3 mm (Figs. 112–117, 119).
FIGURES 37–42. Hydnobius laticeps. 37. Right antenna, dorsal view. 38. Mandibles, dorsal view. 39. Male right metafemur. 40. Aedeagus, dorsal view. 41. Female sternite 8, ventral view. 42 in Review of the Sogdini of North and Central America (Coleoptera: Leiodidae: Leiodinae) with descriptions of fourteen new species and three new genera
FIGURES 37–42. Hydnobius laticeps. 37. Right antenna, dorsal view. 38. Mandibles, dorsal view. 39. Male right metafemur. 40. Aedeagus, dorsal view. 41. Female sternite 8, ventral view. 42. Female coxites and styli, ventral view. Scale bar = 0.3 mm (Figs. 40–42), 0.4 mm (Figs. 37, 38), 0.5 mm (Fig. 39).
FIGURE6. Telsimia pygmaea Poorani, sp. n.: a. head; b. antenna; c. maxilla; d. labium; e. abdomen, male; f. terminal ventrite, female; g–i. male genitalia: g. tegmen, inner view; h. penis, lateral view; i. penis, dorsal view; j. coxites in --A--brief--review--of--the--tribe--Telsimiini--(Coleoptera:--Coccinellidae)--of--the--Indian-subcontinent,--including--three--new--species--of--Telsimia Casey--from--South--India
FIGURE6. Telsimia pygmaea Poorani, sp. n.: a. head; b. antenna; c. maxilla; d. labium; e. abdomen, male; f. terminal ventrite, female; g–i. male genitalia: g. tegmen, inner view; h. penis, lateral view; i. penis, dorsal view; j. coxites
FIGURE4. Telsimia flavomaculata Poorani: a. dorsal view; b. lateral view; c. frontal view; d. antenna; e. prosternal process; f. abdomen, male; g–i. male genitalia: g. tegmen, lateral view; h. tegmen, inner view; i. penis, inner view in --A--brief--review--of--the--tribe--Telsimiini--(Coleoptera:--Coccinellidae)--of--the--Indian-subcontinent,--including--three--new--species--of--Telsimia Casey--from--South--India
FIGURE4. Telsimia flavomaculata Poorani: a. dorsal view; b. lateral view; c. frontal view; d. antenna; e. prosternal process; f. abdomen, male; g–i. male genitalia: g. tegmen, lateral view; h. tegmen, inner view; i. penis, inner view
Bulk gene expression profiles of adult and pupal antennae in wild-type and orco mutant Harpegnathos saltator
GEO Series GSE236793. Harpegnathos saltator. 39 samples. Type: Expression profiling by high throughput sequencing.
Chromatin profiling of the Harpegnathos saltator antennae
GEO Series GSE280477. Harpegnathos saltator. 11 samples. Type: Genome binding/occupancy profiling by high throughput sequencing.
ROSETTA RF ANTENNA ENGINEERING DATA
This CODMAC level 3 data set contains the output of the Antenna Communication System Housekeeping placed in Tabular form. It covers the period from launch in 2004, through the 3 Earth and 1 Mars flyby, plus the hibernation phases, plus the asteroid flybys and finally covers the Prelanding, comet escort & Extension phases of the prime target of the mission. The prime target is comet 67P/Churyumov-Gerasimenko 1 (1969 R1). This version V1.0 is the first version of this dataset.
PSP FIELDS Digital Fields Board (DFB) AC-coupled Differential Voltage, V1-V2, V3-V4 Antennae, Dipole Mode, Cross Spectra, High Gain, Sensor coordinates, Level 2 (L2), 0.873813 s Data
PSP FIELDS Digital Fields Board (DFB), XXX ⨯ YYY cross spectra data:The DFB is the low frequency, less than 75 kHz, component of the FIELDS experiment on the Parker Solar Probe spacecraft, see reference [1] below. For a full description of the FIELDS experiment, see reference [2]. For a description of the DFB, see reference [3].DFB AC cross spectra data for a pair of input channels consist of:* 1) Power spectral densities (auto spectra, e.g. FT₁ ⨯ FT₁*)* 2) Real and imaginary parts of the spectral cross term (FT₁ ⨯ FT₂*)* 3) Coherence* 4) Phasewhere all as a function of frequency and time. The last two terms are describedcoherence and phase are defined in [3].These cross spectra are averaged in both frequency and time as described in [3]. The cross spectra have either 56 or 96 bins (selectable) with the bin central frequencies reported in the metadata. The AC cross spectra are duty-cycled such that spectral averaging takes place over the first 1/8 of any given NYs (assuming a 1 NYs data cadence). Less data are averaged by 2^N for cadences faster than 1 NYs by 2^N. For cadences slower than 1 NYs, the first 1/8 of each NYs of data included are averaged together to form the reported data.The Level 2 data products contained in this data file have been calibrated for:* 1) The Hanning window used in the spectral calculation* 2) DFB in-band gain* 3) DFB analog filter gain response* 4) DFB digital filter gain response* 5) The search coil preamplifier response, when applicable* 6) The bandwidth of each spectral binNote that compensation for the DFB digital filters will introduce a non-physical positively sloped power trend at high frequencies when the non-corrected signal is dominated by noise. This effect should be examined carefully when determining spectral slopes and features at the highest frequencies. Calibrations for the FIELDS preamplifiers have not been implemented as the preamplifier response is flat and equal to one through the DFB frequency range. Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor signals. These corrections will be applied in the Level 3 DFB data products. Therefore, all voltage sensor quantities when present in these Level 2 data products are expressed by using units of Volts squared per Hertz. Likewise, all magnetic field quantities when present in these Level 2 data product are expressed by using units of nanoTesla squared per Hertz. The units for phase are degrees.The Level 2 voltage data products contained in this data file are expressed in sensor coordinates: e.g. dV12, dV34 for voltage measurements. For solar orbits 1 and 2, the search coil magnetometer cross spectra data are rotated into a non-intuitive coordinate system with components [d,e,f]. For solar orbits 3 and beyond, the magnetic field cross spectra data are expressed by using search coil magnetometer sensor coordinates with components [u,v,w].To rotate from [d,e,f] coordinates to [u,v,w] search coil sensor coordinates, use the following matrix, written in IDL notation, and the following equation: spectra_uvw_vector = R ## spectra_def_vector.R = [[ 0.46834856, -0.81336422 , 0.34509170] [ -0.66921924, -0.071546954, 0.73961249] [ -0.57688408, -0.57733845 , -0.57782790]]For some orbits, sufficient spectral information exists in the auto spectra and cross spectra to determine wave ellipticity, planarity, and wave normal angles. One method for accomplishing this is presented in reference [4].Time resolution of the DFB AC cross spectral data can vary by multiples of 2^N. During encounter (when PSP is within 0.25 AU of the Sun), cadence for the DFB AC cross spectra is typically 1 NYsecond [2]. Timestamps correspond to the center time of each window.References:* 1) Fox, N.J., Velli, M.C., Bale, S.D. et al., Space Sci Rev (2016) 204:7. https://doi.org/10.1007/s1121401502116* 2) Bale, S.D., Goetz, K., Harvey, P.R. et al., Space Sci Rev (2016) 204:49. https://doi.org/10.1007/s1121401602445* 3) Malaspina, D.M., Ergun, R.E., Bolton, M. et al., JGR Space Physics (2016), 121, 5088-5096. https://doi.org/10.1002/2016JA022344* 4) Santolik, O., Parrot, M., Lefeuvre, F. Radio Science (2003), 38, 1010. https://doi.org/10.1029/2000RS002523
PSP FIELDS Digital Fields Board (DFB) DC-coupled Differential Voltage, V1-V2 Antennae, Dipole Mode, Spectra, High Gain, Sensor coordinates, Level 2 (L2), 6.99054 s Data
PSP FIELDS Digital Fields Board, DFB, dV12hg data:The DFB is the low frequency, less than 75 kHz, component of the FIELDS experiment on the Parker Solar Probe spacecraft, see reference [1] below. For a full description of the FIELDS experiment, see reference [2]. For a description of the DFB, see reference [3].DFB DC spectra data consist of power spectral densities as a function of frequency and time. These spectra are averaged over both frequency and time as described in [3]. The spectra have pseudo-logarithmically spaced frequency bins with the bin central frequencies reported in the metadata.The Level 2 data products contained in this data file have been calibrated for:* 1) The Hanning window used in the spectral calculation* 2) DFB in-band gain* 3) DFB analog filter gain response* 4) DFB digital filter gain response* 5) The search coil preamplifier response, when applicable* 6) The bandwidth of each spectral binNote that compensation for the DFB digital filters will introduce a non-physical positively sloped power trend at high frequencies when the non-corrected signal is dominated by noise. This effect should be examined carefully when determining spectral slopes and features at the highest frequencies. Calibrations for the FIELDS preamplifiers have not been implemented as the preamplifier response is flat and equal to one through the DFB frequency range. Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor signals. These corrections will be applied in the Level 3 DFB data products. Therefore, all voltage sensor quantities when present in these Level 2 data products are expressed by using units of Volts squared per Hertz. Likewise, all magnetic field quantities when present in these Level 2 data product are expressed by using units of nanoTesla squared per Hertz.The Level 2 data products contained in this data file are expressed in sensor coordinates: e.g. dV12, dV34 for voltage measurements. For solar orbits 1 and 2, the search coil magnetometer spectral data are rotated into a non-intuitive coordinate system with components [d,e,f]. For solar orbits 3 and beyond, the magnetic field spectral data are in expressed in search coil magnetometer sensor coordinates with components [u,v,w].To rotate from [d,e,f] coordinates into [u,v,w] search coil sensor coordinates, use the following matrix, written in IDL notation, and the following equation: spectra_uvw_vector = R ## spectra_def_vector.R = [[ 0.46834856, -0.81336422 , 0.34509170] [ -0.66921924, -0.071546954, 0.73961249] [ -0.57688408, -0.57733845 , -0.57782790]]The time resolution of the DFB DC spectral data can vary by multiples of 2^N. During encounter when PSP is within 0.25 AU of the Sun, the DFB DC spectra data cadence is typically 30 NYseconds NYsecond [2]. Timestamps correspond to the center time of each window.References:* 1) Fox, N.J., Velli, M.C., Bale, S.D. et al., Space Sci Rev (2016) 204:7. https://doi.org/10.1007/s1121401502116* 2) Bale, S.D., Goetz, K., Harvey, P.R. et al., Space Sci Rev (2016) 204:49. https://doi.org/10.1007/s1121401602445* 3) Malaspina, D.M., Ergun, R.E., Bolton, M. et al., JGR Space Physics (2016), 121, 5088-5096. https://doi.org/10.1002/2016JA022344
PSP FIELDS Digital Fields Board (DFB) AC-coupled V5 Antenna Voltage, Monopole Mode, Auto Spectra, High Gain, Sensor coordinates, Level 2 (L2), 0.873813 s Data
PSP FIELDS Digital Fields Board, DFB, V5 data:The DFB is the low frequency, less than 75 kHz, component of the FIELDS experiment on the Parker Solar Probe spacecraft, see reference [1] below. For a full description of the FIELDS experiment, see reference [2]. For a description of the DFB, see reference [3].DFB AC spectra data consist of power spectral densities as a function of frequency and time. These spectra are averaged over both frequency and time as described in [3]. The spectra have pseudo-logarithmically spaced frequency bins with the bin central frequencies reported in the metadata. The AC spectra are duty-cycled such that spectral averaging takes place over the first 1/8 of any given NYsecond when the data cadence is equal to one NYsecond. Less data are averaged by a factor of 2^N for data cadences that are faster than one NYsecond by 2^N. For cadences slower than one NYsecond, the first 1/8 of each NYsecond of data included are averaged together to construct the reported data.The Level 2 data products contained in this data file have been calibrated for:* 1) The Hanning window used in the spectral calculation* 2) DFB in-band gain* 3) DFB analog filter gain response* 4) DFB digital filter gain response* 5) The search coil preamplifier response, when applicable* 6) The bandwidth of each spectral binNote that compensation for the DFB digital filters will introduce a non-physical positively sloped power trend at high frequencies when the non-corrected signal is dominated by noise. This effect should be examined carefully when determining spectral slopes and features at the highest frequencies. Calibrations for the FIELDS preamplifiers have not been implemented as the preamplifier response is flat and equal to one through the DFB frequency range. Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor signals. These corrections will be applied in the Level 3 DFB data products. Therefore, all voltage sensor quantities when present in these Level 2 data products are expressed by using units of Volts squared per Hertz. Likewise, all magnetic field quantities when present in these Level 2 data product are expressed by using units of nanoTesla squared per Hertz.The Level 2 data products contained in this data file are expressed in sensor coordinates: e.g. dV12, dV34 for voltage measurements. For solar orbits 1 and 2, the search coil magnetometer spectral data are rotated into a non-intuitive coordinate system with components [d,e,f]. For solar orbits 3 and beyond, the magnetic field spectral data are in expressed in search coil magnetometer sensor coordinates with components [u,v,w].To rotate from [d,e,f] coordinates into [u,v,w] search coil sensor coordinates, use the following matrix, written in IDL notation, and the following equation: spectra_uvw_vector = R ## spectra_def_vector.R = [[ 0.46834856, -0.81336422 , 0.34509170] [ -0.66921924, -0.071546954, 0.73961249] [ -0.57688408, -0.57733845 , -0.57782790]]The time resolution of the DFB AC spectral data can vary by multiples of 2^N. During encounter when PSP is within 0.25 AU of the Sun, the DFB AC spectra data cadence is typically NYsecond NYsecond [2]. Timestamps correspond to the center time of each window.References:* 1) Fox, N.J., Velli, M.C., Bale, S.D. et al., Space Sci Rev (2016) 204:7. https://doi.org/10.1007/s1121401502116* 2) Bale, S.D., Goetz, K., Harvey, P.R. et al., Space Sci Rev (2016) 204:49. https://doi.org/10.1007/s1121401602445* 3) Malaspina, D.M., Ergun, R.E., Bolton, M. et al., JGR Space Physics (2016), 121, 5088-5096. https://doi.org/10.1002/2016JA022344
PSP FIELDS Digital Fields Board (DFB) DC-coupled Differential Voltage, V3-V4 Antennae, Dipole Mode, Bandpass filtered, High Gain, Sensor coordinates, Level 2 (L2), 0.873813 s Data
PSP FIELDS Digital Fields Board, DFB, dV34 data:The DFB is the low frequency, less than 75 kHz, component of the FIELDS experiment on the Parker Solar Probe spacecraft, see reference [1] below. For a full description of the FIELDS experiment, see reference [2]. For a description of the DFB, see reference [3].DFB DC bandpass data consist of peak and average values of the absolute value of bandpassed time series waveform data over a time interval equal to the reporting cadence. The DC bandpass data have the peak response frequency of each bin reported in the metadata. The frequency response curves for these bins are given in [3].The Level 2 data products contained in this data file have been calibrated for:* 1) The ~6.3 dB loss associated with forming the bandpass signal, see reference [3]* 2) DFB in-band gain* 3) The search coil preamplifier response, when applicable* 4) DFB digital filter time delays, the DFB filter time delays become significant in the lowest frequency DC bandpass binsCalibrations for the DFB digital filter gains and analog filter gains have not been implemented as it was determined that these could not be applied accurately to single numerical values representing a broadband signal response and because all bins except the highest frequency bin have a flat gain response equal to one due to these filters. Calibrations for the FIELDS preamplifiers have not been implemented as the preamplifier response is flat and equal to one through the DFB frequency range. Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor signals. These corrections will be applied in the Level 3 DFB data products. Therefore, all voltage sensor quantities when present in these Level 2 data products are expressed by using units of Volts. Likewise, all magnetic field quantities when present in these Level 2 data products are expressed by using units of nanoTelsas.The Level 2 data products contained in this data file are expressed in sensor coordinates: e.g. dV12, dV34 for voltage measurements and [u,v,w] for the searchcoil magnetometer.The time resolution of the DFB DC bandpass filtered data can vary by multiples of 2^N. During encounter when PSP is within 0.25 AU of the Sun, the DFB DC bandpass filtered data cadence is typically 1 NYsecond [2]. Timestamps correspond to the center time of each window.References:* 1) Fox, N.J., Velli, M.C., Bale, S.D. et al., Space Sci Rev (2016) 204:7. https://doi.org/10.1007/s1121401502116* 2) Bale, S.D., Goetz, K., Harvey, P.R. et al., Space Sci Rev (2016) 204:49. https://doi.org/10.1007/s1121401602445* 3) Malaspina, D.M., Ergun, R.E., Bolton, M. et al., JGR Space Physics (2016), 121, 5088-5096. https://doi.org/10.1002/2016JA022344
PSP FIELDS Digital Fields Board (DFB) AC-coupled Differential Voltage, V1-V2 Antennae, Dipole Mode, Spectra, High Gain, Sensor coordinates, Level 2 (L2), 0.873813 s Data
PSP FIELDS Digital Fields Board, DFB, dV12hg data:The DFB is the low frequency, less than 75 kHz, component of the FIELDS experiment on the Parker Solar Probe spacecraft, see reference [1] below. For a full description of the FIELDS experiment, see reference [2]. For a description of the DFB, see reference [3].DFB AC spectra data consist of power spectral densities as a function of frequency and time. These spectra are averaged over both frequency and time as described in [3]. The spectra have pseudo-logarithmically spaced frequency bins with the bin central frequencies reported in the metadata. The AC spectra are duty-cycled such that spectral averaging takes place over the first 1/8 of any given NYsecond when the data cadence is equal to one NYsecond. Less data are averaged by a factor of 2^N for data cadences that are faster than one NYsecond by 2^N. For cadences slower than one NYsecond, the first 1/8 of each NYsecond of data included are averaged together to construct the reported data.The Level 2 data products contained in this data file have been calibrated for:* 1) The Hanning window used in the spectral calculation* 2) DFB in-band gain* 3) DFB analog filter gain response* 4) DFB digital filter gain response* 5) The search coil preamplifier response, when applicable* 6) The bandwidth of each spectral binNote that compensation for the DFB digital filters will introduce a non-physical positively sloped power trend at high frequencies when the non-corrected signal is dominated by noise. This effect should be examined carefully when determining spectral slopes and features at the highest frequencies. Calibrations for the FIELDS preamplifiers have not been implemented as the preamplifier response is flat and equal to one through the DFB frequency range. Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor signals. These corrections will be applied in the Level 3 DFB data products. Therefore, all voltage sensor quantities when present in these Level 2 data products are expressed by using units of Volts squared per Hertz. Likewise, all magnetic field quantities when present in these Level 2 data product are expressed by using units of nanoTesla squared per Hertz.The Level 2 data products contained in this data file are expressed in sensor coordinates: e.g. dV12, dV34 for voltage measurements. For solar orbits 1 and 2, the search coil magnetometer spectral data are rotated into a non-intuitive coordinate system with components [d,e,f]. For solar orbits 3 and beyond, the magnetic field spectral data are in expressed in search coil magnetometer sensor coordinates with components [u,v,w].To rotate from [d,e,f] coordinates into [u,v,w] search coil sensor coordinates, use the following matrix, written in IDL notation, and the following equation: spectra_uvw_vector = R ## spectra_def_vector.R = [[ 0.46834856, -0.81336422 , 0.34509170] [ -0.66921924, -0.071546954, 0.73961249] [ -0.57688408, -0.57733845 , -0.57782790]]The time resolution of the DFB AC spectral data can vary by multiples of 2^N. During encounter when PSP is within 0.25 AU of the Sun, the DFB AC spectra data cadence is typically NYsecond NYsecond [2]. Timestamps correspond to the center time of each window.References:* 1) Fox, N.J., Velli, M.C., Bale, S.D. et al., Space Sci Rev (2016) 204:7. https://doi.org/10.1007/s1121401502116* 2) Bale, S.D., Goetz, K., Harvey, P.R. et al., Space Sci Rev (2016) 204:49. https://doi.org/10.1007/s1121401602445* 3) Malaspina, D.M., Ergun, R.E., Bolton, M. et al., JGR Space Physics (2016), 121, 5088-5096. https://doi.org/10.1002/2016JA022344
PSP FIELDS Digital Fields Board (DFB) DC-coupled Differential Voltage, V1-V2 Antennae, Dipole Mode, Bandpass filtered, High Gain, Sensor coordinates, Level 2 (L2), 0.873813 s Data
PSP FIELDS Digital Fields Board, DFB, dV12 data:The DFB is the low frequency, less than 75 kHz, component of the FIELDS experiment on the Parker Solar Probe spacecraft, see reference [1] below. For a full description of the FIELDS experiment, see reference [2]. For a description of the DFB, see reference [3].DFB DC bandpass data consist of peak and average values of the absolute value of bandpassed time series waveform data over a time interval equal to the reporting cadence. The DC bandpass data have the peak response frequency of each bin reported in the metadata. The frequency response curves for these bins are given in [3].The Level 2 data products contained in this data file have been calibrated for:* 1) The ~6.3 dB loss associated with forming the bandpass signal, see reference [3]* 2) DFB in-band gain* 3) The search coil preamplifier response, when applicable* 4) DFB digital filter time delays, the DFB filter time delays become significant in the lowest frequency DC bandpass binsCalibrations for the DFB digital filter gains and analog filter gains have not been implemented as it was determined that these could not be applied accurately to single numerical values representing a broadband signal response and because all bins except the highest frequency bin have a flat gain response equal to one due to these filters. Calibrations for the FIELDS preamplifiers have not been implemented as the preamplifier response is flat and equal to one through the DFB frequency range. Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor signals. These corrections will be applied in the Level 3 DFB data products. Therefore, all voltage sensor quantities when present in these Level 2 data products are expressed by using units of Volts. Likewise, all magnetic field quantities when present in these Level 2 data products are expressed by using units of nanoTelsas.The Level 2 data products contained in this data file are expressed in sensor coordinates: e.g. dV12, dV34 for voltage measurements and [u,v,w] for the searchcoil magnetometer.The time resolution of the DFB DC bandpass filtered data can vary by multiples of 2^N. During encounter when PSP is within 0.25 AU of the Sun, the DFB DC bandpass filtered data cadence is typically 1 NYsecond [2]. Timestamps correspond to the center time of each window.References:* 1) Fox, N.J., Velli, M.C., Bale, S.D. et al., Space Sci Rev (2016) 204:7. https://doi.org/10.1007/s1121401502116* 2) Bale, S.D., Goetz, K., Harvey, P.R. et al., Space Sci Rev (2016) 204:49. https://doi.org/10.1007/s1121401602445* 3) Malaspina, D.M., Ergun, R.E., Bolton, M. et al., JGR Space Physics (2016), 121, 5088-5096. https://doi.org/10.1002/2016JA022344
PSP FIELDS Digital Fields Board (DFB) AC-coupled Differential Voltage, V3-V4 Antennae, Dipole Mode, Spectra, High Gain, Sensor coordinates, Level 2 (L2), 0.873813 s Data
PSP FIELDS Digital Fields Board, DFB, dV34hg data:The DFB is the low frequency, less than 75 kHz, component of the FIELDS experiment on the Parker Solar Probe spacecraft, see reference [1] below. For a full description of the FIELDS experiment, see reference [2]. For a description of the DFB, see reference [3].DFB AC spectra data consist of power spectral densities as a function of frequency and time. These spectra are averaged over both frequency and time as described in [3]. The spectra have pseudo-logarithmically spaced frequency bins with the bin central frequencies reported in the metadata. The AC spectra are duty-cycled such that spectral averaging takes place over the first 1/8 of any given NYsecond when the data cadence is equal to one NYsecond. Less data are averaged by a factor of 2^N for data cadences that are faster than one NYsecond by 2^N. For cadences slower than one NYsecond, the first 1/8 of each NYsecond of data included are averaged together to construct the reported data.The Level 2 data products contained in this data file have been calibrated for:* 1) The Hanning window used in the spectral calculation* 2) DFB in-band gain* 3) DFB analog filter gain response* 4) DFB digital filter gain response* 5) The search coil preamplifier response, when applicable* 6) The bandwidth of each spectral binNote that compensation for the DFB digital filters will introduce a non-physical positively sloped power trend at high frequencies when the non-corrected signal is dominated by noise. This effect should be examined carefully when determining spectral slopes and features at the highest frequencies. Calibrations for the FIELDS preamplifiers have not been implemented as the preamplifier response is flat and equal to one through the DFB frequency range. Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor signals. These corrections will be applied in the Level 3 DFB data products. Therefore, all voltage sensor quantities when present in these Level 2 data products are expressed by using units of Volts squared per Hertz. Likewise, all magnetic field quantities when present in these Level 2 data product are expressed by using units of nanoTesla squared per Hertz.The Level 2 data products contained in this data file are expressed in sensor coordinates: e.g. dV12, dV34 for voltage measurements. For solar orbits 1 and 2, the search coil magnetometer spectral data are rotated into a non-intuitive coordinate system with components [d,e,f]. For solar orbits 3 and beyond, the magnetic field spectral data are in expressed in search coil magnetometer sensor coordinates with components [u,v,w].To rotate from [d,e,f] coordinates into [u,v,w] search coil sensor coordinates, use the following matrix, written in IDL notation, and the following equation: spectra_uvw_vector = R ## spectra_def_vector.R = [[ 0.46834856, -0.81336422 , 0.34509170] [ -0.66921924, -0.071546954, 0.73961249] [ -0.57688408, -0.57733845 , -0.57782790]]The time resolution of the DFB AC spectral data can vary by multiples of 2^N. During encounter when PSP is within 0.25 AU of the Sun, the DFB AC spectra data cadence is typically NYsecond NYsecond [2]. Timestamps correspond to the center time of each window.References:* 1) Fox, N.J., Velli, M.C., Bale, S.D. et al., Space Sci Rev (2016) 204:7. https://doi.org/10.1007/s1121401502116* 2) Bale, S.D., Goetz, K., Harvey, P.R. et al., Space Sci Rev (2016) 204:49. https://doi.org/10.1007/s1121401602445* 3) Malaspina, D.M., Ergun, R.E., Bolton, M. et al., JGR Space Physics (2016), 121, 5088-5096. https://doi.org/10.1002/2016JA022344
ROSETTA HIGH GAIN ANTENNA ENGINEERING DATA
This CODMAC level 3 data set contains the key parameters of the HGA Housekeeping. In particular, it provides information on the measured Azimuth & Elevation angles, as well as different pointing errors and displacement errors. It covers the period from launch in 2004, through the 3 Earth and 1 Mars flyby, plus the hibernation phases, plus the asteroid flybys and finally covers the Prelanding, comet escort & Extension phases of the prime target of the mission. The prime target is comet 67P/Churyumov-Gerasimenko 1 (1969 R1). This version V1.0 is the first version of this dataset.
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Allen Brain Atlas
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DANDI Archive for NWB datasets
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International Brain Laboratory public data
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OpenNeuro
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