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284 results for “telescope”
Recording of the STEREO-A space weather beacon with the Allen Telescope Array
<p>This dataset contains an IQ recording of the X-band 8443.5 MHz space weather beacon from STEREO-A, done with one of the antennas of the Allen Telescope Array. The recording was made as part of a demo for some GNU Radio tutorials for the Breakthrough Listen REU program.</p> <p>The recording was done with the spacecraft at around 9 million km from Earth, so the SNR is very good. Only one linear polarization (X, or horizontal) was recorded, using antenna 4g from the array.</p> <p>The hardware configuration was as follows: the antenna was connected to RFCB LO d, which was tuned to a frequency of 8443.54 MHz and used an output IF of 512 MHz. A USRP N321 digitized the X polarization. The USRP used an external 10 MHz reference and PPS coming from the observatory distribution system. The IQ sample rate of the USRP was 480 ksps, and a GNU Radio flowgraph was used to record IQ data to disk. The GNU Radio flowgraph stored the IQ data for each channel as 16-bin integers in the <a href="https://wiki.gnuradio.org/index.php/Metadata_Information">GNU Radio metatata file format</a>, with detached headers.</p> <p>After recording, the data was formatted using <a href="https://github.com/gnuradio/SigMF">SigMF</a>.</p>
Quick RFI Survey at the Allen Telescope Array
<p>This dataset contains some recordings done as a proof of concept of a radio frequency interference (RFI) scan at the Allen Telescope Array with an ADALM Pluto running <a href="https://maia-sdr.org/">Maia SDR</a>, a small monopole antenna for ~450 MHz, and a smartphone. The proof of concept consisted in showing how this hand-held equipment can be used to obtain a quick overview of strong RFI signals. IQ recordings in <a href="https://github.com/sigmf/SigMF">SigMF format</a> were done for all the signals between 70 MHz and 6 GHz visually detected on a spectrum plot. The 6 recordings are contained in this dataset. See <a href="https://destevez.net/2023/08/a-very-quick-rfi-survey-at-the-allen-telescope-array/(opens in a new tab)">this blog post</a> for more details and a short description of each recording.</p>
Jupiter's ground-based observations on 2018 May 24th-27th from the Very Large Telescope Imager and Spectrometer instrument
<p>The Very Large Telescope Imager and Spectrometer (VISIR) instrument on ESO's Very Large Telescope (VLT) has been used to support the NASA's Juno mission since 2016. The present dataset was collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme 0101.C-0073(A)). The 2018 May 24th-27th dataset provides a comprehensive view of Jupiter's pole-to-pole thermal, chemical, and aerosol structure ; including the Great Red Spot; and the auroral-related heating in the southern polar stratosphere; after retrieval calculations.</p> <p>Here, we provide the destriped, cleaned, calibrated and projected data of 2018 May 24h to 27th dataset.</p> <p> </p> <p>For the 7.9µm filter, we have added the radial Doppler velocities files.</p>
Recording of OSIRIS-REx with the Allen Telescope Array during SRC reentry
<p>This dataset contains an IQ recording of the X-band 8445.8 MHz telemetry signal from OSIRIS-REx as it passed over California during the sample return capsule reentry. Antennas 1a and 5c from the Allen Telescope Array were used in dual XY (linear) polarization.</p> <p>The hardware configuration was as follows: the antennas were connected to RFCB LO d, which was tuned to a frequency of 8425 MHz and used an output IF of 512 MHz. A USRP N321 and N320 digitized both polarizations of each antenna. The USRPs used an external 10 MHz reference and PPS coming from the observatory distribution system, and LO sharing was set up among the four channels. The IQ sample rate of the USRPs was 61.44 Msps and a GNU Radio flowgraph was used to record IQ data to disk. The GNU Radio flowgraph stored the IQ data for each channel as 16-bin integers in the <a href="https://wiki.gnuradio.org/index.php/Metadata_Information">GNU Radio metatata file format</a>, with detached headers.</p> <p>After recording, the data was downsampled to 2.048 Msps centered around 8445.8 MHz and formatted using <a href="https://github.com/gnuradio/SigMF">SigMF</a> using the script do_sigmf.py.</p>
Does Using a 5 mm Telescope in Laparoscopic Cholecystectomy Reduce the Incidence of Trocar Site Hernia?
ClinicalTrials.gov study NCT04279223. IPD Sharing: UNDECIDED. Countries: 1. Publications: 3.
Comparison of Tele-Critical Care Versus Usual Care On ICU Performance (TELESCOPE)
ClinicalTrials.gov study NCT03920501. IPD Sharing: YES. Countries: 1. Publications: 3.
A Prospective Study Comparing Telescopic vs. Balloon Dissection in Single Incision Laparoscopic Inguinal Herniorraphy (SILTELESCOPIC)
ClinicalTrials.gov study NCT01883115. IPD Sharing: Not stated. Countries: 1. Publications: 4.
Effectiveness of Telescopic Magnification in the Treatment of Amblyopia
ClinicalTrials.gov study NCT00970554. IPD Sharing: Not stated. Countries: 1. Publications: 1.
Tranexamic Acid During Telescoping Nail Application In Osteogenesis Imperfecta
ClinicalTrials.gov study NCT05321199. IPD Sharing: Not stated. Countries: 1. Publications: 10.
TELESCOPE- TELEhealth Shared Decision-making COaching
ClinicalTrials.gov study NCT05491213. IPD Sharing: NO. Countries: 1. Publications: 2.
Data from: A search for technosignatures from 14 planetary systems in the Kepler field with the Green Bank Telescope at 1.15–1.73 GHz
Open the record for dataset details and reuse information.
Data from: A Search for Technosignatures Around 31 Sun-like Stars with the Green Bank Telescope at 1.15–1.73 GHz
Open the record for dataset details and reuse information.
SolSysELTs2022 Part II: Investigating the Ice Giants with Extremely Large Telescopes
<p>Invited talk: presentation and video recording</p>
The m-Dimensional Spatial Nyquist Limit Using the Wave Telescope for Larger Numbers of Spacecraft Dataset
<p>Dataset for: The m-Dimensional Spatial Nyquist Limit Using the Wave Telescope for Larger Numbers of Spacecraft. Includes model results of 2D and 3D modelling. </p>
Hobby-Eberly Telescope Spectra of Planetary-Nebula Nuclei with O VI Emission
<p>HET spectra (.fits format) of 6 central stars of planetary nebulae showing O VI emission lines. Obtained with the LRS2 spectrograph of the Hobby-Eberly Telescope at McDonald Observatory. For each observation there are 2 spectra, one in the UV arm, and one in the Orange arm, of the LRS2 spectrograph. Absolute calibrations have been applied. These spectra are discussed in a forthcoming paper "Spectroscopic survey of faint planetary-nebula nuclei. I. Six new O VI} central stars," by H. E. Bond, K. Werner, G. Jacoby, and G. Zeimann, submitted to Monthly Notices of the Royal Astronomical Society.</p>
Patient Satisfaction and Retention in Implant Supported Telescopic Overdenture With Different Copings
ClinicalTrials.gov study NCT04032223. IPD Sharing: UNDECIDED. Countries: 0. Publications: 1.
Data from: A search for technosignatures from TRAPPIST-1, LHS 1140, and 10 planetary systems in the Kepler field with the Green Bank Telescope at 1.15–1.73 GHz
Open the record for dataset details and reuse information.
Allen Telescope Array Galileo E31 RF recording with 2 antennas and 2 polarizations
<p>This is a short recording of Galileo satellite GSAT0218 (E31) done with two antennas at Allen Telescope Array in the E1 (1575.42 MHz) frequency band, using a sample rate of 30.72 Msps.</p> <p>The recording was done with antennas 1h and 4g, and both polarizations X and Y from each antenna. The recording lasts approximately 15 seconds and was done on 2020-10-04.</p> <p>The hardware configuration was as follows: antennas 1h and 4g were connected to RFCB LO d, which was tuned to a frequency of 1475.42 MHz and used an output IF of 629 MHz. Two USRPs N32x were connected to the IF output of the RFCB. The first USRP digitized signals from both polarizations of antenna 1h, while the second USRP digitized signals from both polarizations of antenna 4g. The USRPs used external 10 MHz reference and PPS coming from the observatory distribution system.</p> <p>This dataset contains the baseband IQ recordings for each antenna and polarization in <a href="https://github.com/gnuradio/SigMF">SigMF</a> format.</p> <p>More information about the dataset can be found in the blog post "<a href="https://destevez.net/2020/10/gnss-interferometry-at-allen-telescope-array/">GNSS Interferometry at Allen Telescope Array</a>" by the first author.</p> <p><strong>Note:</strong> during the recording there was a problem with caused phase-modulation of the signals at 60 Hz and harmonics. The phase-modulation effect is common to all the channels, so interferometry applications of this data are not affected by it. However, this problem makes it somewhat difficult to perform tracking of the GNSS signals in the usual manner.</p>
Allen Telescope Array polarimetric observation of GNSS satellites
<p>This dataset contains polarimetric observations of several GNSS satellites done with two antennas at Allen Telescope Array in the E1 (1575.42 MHz) frequency band. The dataset consists of power spectra and cross-spectra for the X and Y linear polarizations of each antenna. A total of 1024 FFT channels are used with an input sample rate of 24.576Msps (IQ sampling) to give a frequency resolution of 24kHz. The |X|^2, |Y|^2 and X*conjugate(Y) cross-spectra are coherently averaged in windows of 0.1 seconds.</p> <p><strong>Note:</strong> only one out of every four 1024 IQ sample vectors was processed in order to reduce the CPU load during data recording, so the effective averaging of each spectrum is only 25ms.</p> <p>The recording was done with antennas 1h and 4g on 2020-10-24, and it includes several minutes of measurements for the Galileo satellites E01, E13, E26, E31, E33, and the GPS satellite G05.</p> <p>The hardware configuration was as follows: the antennas were connected to RFCB LO d, which was tuned to a frequency of 1475.42 MHz and used an output IF of 512 MHz. A USRPs N321 and a USRP N320 were connected to the IF output of the RFCB. Each of the USRPs was used to digitized both polarizations from one of the antenna. The USRPs used external 10 MHz reference and PPS coming from the observatory distribution system. LO sharing was configured between all of the USRPs channels.</p> <p>The dataset contains a flat .tar.xz archive with several files having names such as E01_2020-10-24T11:37:38.353705_0xx. The beginning of the filename indicates the target of the observation, then there is the UTC timestamp corresponding to the beginning of the observation, and finally a code that indicates the measurement channel. The first character of the code is either 0 or 1 to indicate antenna 1h or antenna 4g respectively. The remaining characters can be either xx or yy for the power spectra of polarizations X and Y respectively or xy for the cross-spectra of polarizations X and Y.</p> <p>The timestamp for the data is only approximate, because it refers to the instant at which the data collection script started. The USRPs take some 10 to 30 seconds to initialize after this.</p> <p>The format for the xx and yy power spectra files is raw binary in IEEE 754 32 bit floats, with every 1024 elements of the file constituting a power spectra. The format for the xy cross spectra files is raw binary in IEEE 754 32 bit floats. Each pair of floats represents the real and imaginary parts of a complex number. Every 1024 pairs of floats constitute a cross-spectra. Consecutive spectra are separated 0.1 seconds apart in both cases.</p> <p>More information about the dataset can be found in the blog post "<a href="https://destevez.net/2020/10/ata-polarimetry-test-with-gnss-satellites/">ATA polarimetry test with GNSS satellites</a>" by the first author.</p>
Allen Telescope Array polarimetric observation of 3C286
<p>This dataset contains a polarimetric interferometry observation of the quasar 3C286 done with two dishes from Allen Telescope Array on 2020-10-31. The observation was done during two hours around transit, so it has large parallactic angle coverage. Eight different frequency bands between 1 and 8 GHz were observed in turns. Scans of 100 seconds were done with a frequency change between each scan.</p> <p>The frequency bands observed are 1413 MHz, 1665 MHz, 2675 MHz, 4820 MHz, 6663 MHz, and 8665 MHz. A total of 30.72 MHz of spectrum divided in 256 frequency bins were observed in each band. This data set contains the same data in two formats: the raw measurements produced with GNU Radio, and the observations in UVFITS format.</p> <p>The raw measurements consists of power spectra and cross-spectra for the X and Y linear polarizations of each antenna, using a coherent averaging interval of 0.1 seconds.</p> <p>The observation was done with antennas 1h and 4g from the array, using two USRP N32x to digitize the signals, and GNU Radio to perform the digital signal processing. Both of the antennas were connected to LO d in the RF converter board, which downconverted the signals to a 512 MHz IF. The two channels of each USRP were used to digitize the two polarization channels of each antenna. The USRPs were configured to share the LO between all the channels, and were synchronized to the 10 MHz and 1PPS signals from the telescope timing distribution system.</p> <p>The raw measurements are not phased to the source: instrumental and geometric delays are not corrected in any way.</p> <p>All the raw measurements are stored in GNU Radio Metdata files with detached headers, contained in a flat .tar.xz archive. These files have names such as 3c286_2020-10-31T17:47:32.114581_cross_0. The beginning of the filename indicates the target of the observation, then there is the UTC timestamp corresponding to the beginning of the observation, and finally a code that indicates the measurement channel.</p> <p>Measurement channels are divided in "power" for (real-valued) PSD and "cross" for (complex-valued) cross spectra. The "power" channels are numbered 0 through 3 and correspond to |X1|^2, |Y1|^2, |X2|^2 and |Y2|^2, where Xj and Yj denote the X and Y polarizations of antenna j (here j = 1 corresponds to antenna 1h and j = 2 corresponds to antenna 4g). The "cross" channels are numbered 0 through 5 and correspond to <X1,Y1>, <X1,X2>, <X1,Y2>, <Y1,X2>, <Y1,Y2>, <X2,Y2>.</p> <p>Each file corresponds to one channel and one scan. The metadata detached header contains useful information, such as the precise timestamping of the samples and the observation frequency. Note that some of the files have invalid timestamps in the metadata (they are easy to distinguish because their first timestamp is zero). The timestamp in the filename is only a coarse estimate, and is typically within 1 second error of the precise timestamp in the metadata.</p> <p>The UVFITS files contain only the cross-spectra between different antennas (correlations XX, YY, XY and YX). The data is phased to the source, but the same number of frequency channels and integration interval is maintained. There is one UVFITS file per frequency band.</p> <p>More information about this observation and dataset can be found in the post "<a href="https://destevez.net/2020/11/polarimetric-observation-of-3c286-with-allen-telescope-array/">Polarimetric observation of 3C286 with Allen Telescope Array</a>" by the first author.</p>
ScienceDex guides
Understand access before you commit
These curated guides explain access requirements, typical timelines, costs, and reuse considerations for widely used research datasets.
Allen Brain Atlas
Allen Brain Atlas is an Allen Institute collection of brain map atlases, datasets, APIs, and analysis tools covering mouse, human, and non-human primate brain resources.
Annotated Behaviour and Observability Dataset (ABODe)
ABODe is a University of Edinburgh DataShare dataset for behavior classification in group-housed mice using home-cage video, identities, bounding boxes, ground-plate positions, and annotator labels.
DANDI Archive for NWB datasets
DANDI is a BRAIN Initiative archive for publishing and sharing neurophysiology data, including electrophysiology, optophysiology, and behavioral data packaged as NWB and related standards.
International Brain Laboratory public data
The International Brain Laboratory public data releases expose standardized mouse decision-making experiments, including Neuropixels recordings, widefield calcium imaging, behavior, and session metadata accessed through the ONE API.
OpenNeuro
OpenNeuro is a free, open platform for sharing neuroimaging datasets, with public search, dataset pages, and download paths for web, S3, DataLad, and the OpenNeuro CLI.