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284 results for “telescope”
Refracting telescope
The presented object is a telescope with variable magnification. Carl Zeiss – manufactory 1920s, Jena Jagiellonian University Museum Collegium Maius Inventory number: 4187; 187/V https://muzea.malopolska.pl/en/objects-list/2801 Source: Objaverse 1.0 / Sketchfab
Crab giant pulse detected with the Dwingeloo radio telescope on 2024-07-30
<p>This is a 0.2 second recording of a giant pulse of the Crab Pulsar, recorded with the Dwingeloo Radio Telescope. The data format is SigMF: the metadata file contains all metadata, while the data file contains raw 16-bit IQ samples. The recorded bandwidth is 400-420 MHz.</p>
Raw simulation data of response of the PATE particle telescope to electrons
<p>The dataset consists of multiple files, one incident energy per file. The electron distribution is spherically symmetric, the simulated particles are radiated from the inner surface of a sphere with a radius of 10 cm which encloses the entire telescope assembly. The initial angular distribution of the electrons is Lambertian uniform. </p> <p><strong>File naming schema</strong>: e_MONO_{ENERGY, MeV}_MeV_{COUNT, pcs}_count_{SERIAL NUMBER}.dat </p> <p>For example, a file with a serial number <strong>665</strong> which contains data for <strong>2.4E+8</strong> simulated electrons with <strong>70 keV</strong> energy is named "e_MONO_<strong>00.07</strong>_MeV_<strong>240000000</strong>_count_<strong>665</strong>.dat"</p> <p><strong>The data structure is the following:</strong></p> <p>Each line represents a detected particle. The detection means that a particle (including secondaries) deposited at least 50 keV at least in one of the sensitive silicon volumes. From the particle telescope view, there is no means to distinguish between particle flavors at the time of ionization and readout, thus no secondaries are treated separately.</p> <p>The particle record has 11 fields with signed decimal floating point values. The fields are separated by a single tab character ('\t'). There is no tab at the end of the line, the line ending is UNIX ('\n')</p> <p>The first eight floats are deposited energies in the sensitive silicon volumes of the detectors in the detector stack of the PATE instrument. They come in the following order: D1a D1b D1c D2a D2b D3 AC1 AC2. The next is the angle between the telescope axis and the incident particle momentum as seen by the D1 plate, or <strong>-888.0</strong> in case D1 has less than 50 keV of deposited energy. The next field is the angle between the telescope axis and the incident particle momentum at the starting point. <strong>All angles are in degrees</strong>. The last field is redundant, it contains the incident particle energy in <strong>MeV</strong>.</p> <p><strong>Example:</strong></p> <p>0 0 0.050963 0 0 0 0 0 12.728 8.9272 0.055</p> <p>This line represents a 55 keV particle detection, which has deposited 50.963 keV in the D1c detector. The particle was shot at 8.9272 degrees to the telescope axis, at the time it crossed the border of the sensitive volume it had a momentum direction at 12.728 degrees to the telescope axis.</p>
MAGIC Telescope Weather Station Data (2003-2023)
<p>The dataset consist of one file with contains measurement data from the weather station of the MAGIC telescope from the year 2003 until 2023. Due to the long series of measurements, various quality assurance measures were carried out, such as removing obviously incorrect values from an individual measurement sensor. The format of the file is HDF5 and contains various columns as described by the metadata file.</p>
"Filaments in and between galaxy clusters at low and mid-frequency with the SKA telescope" (Figures 6 to 13, B.1 and B.2)
<p>This file contains Figures 6 to 13, B.1 and B.2, from the paper "Filaments in and between galaxy clusters at low and mid-frequency with the SKA telescope", Vacca et al., accepted for publication on A&A on 25 September 2024.</p>
Recording of Europa Clipper X-band telemetry with the Allen Telescope Array shortly after launch
<p>This dataset contains an IQ recording of the X-band 8424.3 MHz telemetry signal from the Europa Clipper spacecraft done with the Allen Telescope Array starting 1 hour and 30 minutes after launch. Antenna 1a from the ATA was used in dual linear polarization (X and Y polarizations).</p> <p>The hardware configuration was as follows: the antenna was connected to RFCB LO d, which was tuned to a frequency of 8424.5 MHz and used an output IF of 512 MHz. A USRP N321 digitized both polarizations of each antenna. The USRP used an external 10 MHz reference and PPS coming from the observatory distribution system, and LO sharing was set up among the two channels. The IQ sample rate of the USRP was 6.144 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 96 ksps centered around 8424.3 MHz and formatted using <a href="https://github.com/gnuradio/SigMF">SigMF</a> with the script do_sigmf.py. This reduced bandwidth is sufficient to decode the low data rate (2 kbps) telemetry signal. In addition to this signal, there are sequential ranging tones throughout much of the recording, but they are outside the 96 kHz bandwidth contained in this dataset.</p>
Recording of Hera X-band telemetry with the Allen Telescope Array shortly after launch (part 1/2)
<p>This dataset contains an IQ recording of the X-band 8435.8 MHz telemetry signal from the Hera spacecraft done with the Allen Telescope Array starting 1 hour and 30 minutes after launch. Antenna 1a from the ATA was used in dual linear polarization (X and Y polarizations).</p> <p>The hardware configuration was as follows: the antenna was connected to RFCB LO d, which was tuned to a frequency of 8435 MHz for one of the recordings and 8435.75 MHz for the other one, and used an output IF of 512 MHz. A USRP N321 digitized both polarizations of each antenna. The USRP used an external 10 MHz reference and PPS coming from the observatory distribution system, and LO sharing was set up among the two channels. The IQ sample rate of the USRP was 6.144 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. The header files are included in the dataset as .hdr files. After recording, the data was formatted in <a href="https://github.com/gnuradio/SigMF">SigMF</a> with the script do_sigmf.py.</p> <p>Antenna pointing was done manually by trying to maximize the received signal power, since the ephemerides publicly available when the launch happened differed greatly from the true launch trajectory. As a consequence, there is signal fading when the antenna is not pointed correctly.</p> <p>This dataset is part 1/2. It contains two recordings of the low rate telemetry signal. <a href="https://zenodo.org/records/14060873">Part 2/2</a> contains a recording of the high rate telemetry signal.</p>
Optical polarimetric, photometric and spectroscopic observations of the TDE AT 2020mot with Nordic Optical Telescope
<p>The dataset contains:</p> <p>1. Polarization data from November 10th, 2020: raw FITS images of the tidal disruption event <a href="https://www.wis-tns.org/object/2020mot">AT 2020mot</a> (polAT2020mot.zip), master bias, master flat-fields (calibs.zip) and raw FITS images of a polarization standard stars (polstandards.zip) that can be used for the instrumental polarization correction.</p> <p>2. The imaging data from February 19th, 2021: raw fits images of the tidal disruption event <a href="https://www.wis-tns.org/object/2020mot">AT 2020mot</a> (imaging.zip) , master bias, master flat-fields (imagingcalibs.zip) and reduced and summed R+i image (TDEsum.fits) that was used to fit the host galaxy profile.</p> <p>3. The spectra from February 19th, 2021: raw fits of the spectra obtained using grisms #7 and #20 (spectroscopy.zip, includes calibration files) and the reduced spectra (TDE.fits).</p> <p>The dataset was obtained with the Nordic Optical Telescope (NOT).</p>
Spectroscopy of the Cosmic Web: a view beyond collisional ionisation equilibrium with future X-ray telescopes
<p>This is a special seminar I gave at the Goddard Space Flight Center of NASA about my Ph.D. research at the Leiden University and the Netherlands Institute for Space Research SRON. Here you can download the presentation slides as well as the recording of the seminar. </p> <p> </p> <p>Abstract:</p> <p>In this talk I will focus on the X-ray view of the cosmic web filaments, more specifically the warm-hot intergalactic medium (WHIM). Hitomi kick-started an upcoming era of X-ray microcalorimeters which offer an unprecedented spectral resolution of diffuse sources. Many spectral signatures that could not yet have been studied will become feasible for the detection, and my presentation will focus on two of these spectral effects.</p> <p><br> Firstly, I will discuss how galaxy cluster photons alter the ionization state of nearby WHIM and affect the column densities of e.g. O VI, O VII, C V, or Ne VIII. Secondly,<br> I will discuss the feasibility of detecting the circum- and intergalactic medium in X-ray absorption using the extended intracluster medium as a backlight. For this study we used the cosmological hydrodynamical simulations Hydrangea (based on EAGLE) and we reported the feasibility of the detection of cosmic web filaments in OVII and in OVIII absorption with the microcalorimeter arrays onboard Athena and LEM. Last but not least, I will discuss my contribution to updating the cooling curve in the photoionisation model of the plasma code SPEX, and show the comparison to other plasma codes (MEKAL, APEC, Cloudy) and other atomic databases (CHIANTI, ADAS).</p>
Demonstration of the Autonomous Precise Assembly of Segmented Mirror Tiles for a Space Telescope
<p>The video shows a complete sequence of the demonstration of the autonomous precise assembly of segmented mirror tiles for a space telescope. Within the EU project PULSAR, DLR, together with CSEM (Switzerland), Space Application Services (Belgium) and Magellium (France) developed the demonstrator of Precise Assembly of Mirror Tiles (dPAMT), focused on assembling a functional section of a primary mirror using an autonomous mobile robot. The demonstrator used a KUKA KMR robot, endowed with a KUKA iiwa arm, for manipulating the segmented mirror tiles through the HOTDOCK standard interface, and performing the assembly using compliant control.</p>
Sky model from the paper "Prospects for a survey of the Galactic plane with the Cherenkov Telescope Array" by the CTA Consortium
<p>The main source model definition file is provided in two formats.</p> <p>- models_gps.xml: readable using GammaLib/ctools, see http://cta.irap.omp.eu/ctools/users/user_manual/models.html</p> <p>- models_gps.yaml: readable using Gammapy, see https://docs.gammapy.org/1.1/tutorials/api/models.html#model-lists-and-serialisation</p> <p> </p> <p>We provide separately the three alternative interstellar emission models.</p> <p>- base: IEM_base.fits</p> <p>- varmin: IEM_varmin.fits.gz</p> <p>- varmin-rescaled: IEM_varmin_rescaled.fits.gz</p> <p>To use the interstellar models one can employ:</p> <p>- GammaLib/ctools, see http://cta.irap.omp.eu/ctools/users/user_manual/models_spatial.html#diffusemapcube</p> <p>- Gammapy, see https://docs.gammapy.org/1.1/tutorials/data/fermi_lat.html#galactic-diffuse-background</p> <p> </p> <p>This work was conducted in the context of the CTA Consortium. We gratefully acknowledge financial support from the agencies and organizations listed here: https://www.cta-observatory.org/consortium_acknowledgments/.</p>
Recording of Psyche with the Allen Telescope Array shortly after launch (decimated)
<p>This dataset contains an IQ recording of the X-band 8417.7 MHz telemetry signal from the Psyche spacecraft done with the Allen Telescope Array starting only 1 hour 30 minutes after launch. Antennas 1a and 5c from the ATA were used in dual linear polarization (X and Y polarizations).</p><p>The hardware configuration was as follows: the antennas were connected to RFCB LO d, which was tuned to a frequency of 8417 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 4.096 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 128 ksps centered around 8417.525 MHz and formatted using <a href="https://github.com/gnuradio/SigMF">SigMF</a> with the script do_sigmf.py. This reduced bandwidth is sufficient to decode the low data rate (2 kbps) telemetry signal. There is a higher data rate (61.1 kbps) signal, as well as sequential ranging tones, near the end of the recording for which this bandwidth is insufficient. The original 4.096 Msps data for this part of the recording has been published for a single antenna and polarization in 8-bit resolution in the dataset "<a href="https://zenodo.org/records/10023378">Recording of Psyche with the Allen Telescope Array shortly after launch (wideband)</a>".</p>
Recording of Psyche with the Allen Telescope Array shortly after launch (wideband)
<p>This dataset contains an IQ recording of the X-band 8417.7 MHz telemetry signal from the Psyche spacecraft done with the Allen Telescope Array starting only 1 hour 30 minutes after launch. Antennas 1a and 5c from the ATA were used in dual linear polarization (X and Y polarizations).</p> <p>The hardware configuration was as follows: the antennas were connected to RFCB LO d, which was tuned to a frequency of 8417 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 4.096 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 formatted using <a href="https://github.com/gnuradio/SigMF">SigMF</a> with the script do_sigmf.py. This dataset contains only the last part of the recording in the original 4.096 Msps sample rate, and only one antenna and polarization. During most of the recording the spacecraft signal is a low rate signal (2 kbps) that fits in a much smaller bandwidth, so another dataset "<a href="https://zenodo.org/records/10003647">Recording of Psyche with the Allen Telescope Array shortly after launch (decimated)</a>" has been published with 128 ksps centered at this signal for each antenna and polarization.</p>
Post-market Observational Study on JTIN Telescopic Nail in Osteogenesis Imperfecta Pediatric Patients
ClinicalTrials.gov study NCT05612139. IPD Sharing: NO. Countries: 1. Publications: 3.
Telescopic Dissection vs. Balloon Dissection During Laparoscopic TEP Inguinal Hernia Repair
ClinicalTrials.gov study NCT03276871. IPD Sharing: NO. Countries: 1. Publications: 5.
Data from: Evolution of cranial telescoping in echolocating whales (Cetacea: Odontoceti)
Open the record for dataset details and reuse information.
Data from: A Search for Technosignatures Around 11,680 Stars with the Green Bank Telescope at 1.15–1.73 GHz
Open the record for dataset details and reuse information.
FRB 121102 detections from the Lovell Telescope
<p>We provide data for FRB 121102 pulses detected with the Lovell telescope at Jodrell Bank, UK at 1.4 GHz. These detections were used in Rajwade et al. (2020). Each file is a single pulse from FRB 121102 in the standard SIGPROC filterbank format and can be read in by standard radio pulsar data processing software. The tarball contains all the filterbank files. The text file contains the name of each file in the first column and seconds into the file where the pulse is located in the second column. The start time of the pulse is with reference to the highest frequency channel i.e seconds into the file where the pulse was detected in the highest frequency channel.</p> <p> </p> <p>Citation:</p> <p>If you are planning to use these data in any publication, please do not forget to put in the following acknowledgement:</p> <p>"The data used in this manuscript have been downloaded from the Zenodo open access repository 'FRB 121102 detections from the Lovell Telescope' (10.5281/zenodo.3974768)." </p>
Data for "Martian oxygen and hydrogen upper atmospheres responding to solar and dust storm drivers: Hisaki space telescope observations"
<p>Data files (.npy) and python codes (.ipynb) to produce the figures in the paper.</p> <p>Download the zip file (dataforfigures_v2.zip), open plot_figX.ipynb with Jupyter notebook, and run it.</p> <p> </p>
Chang'e 5 RF recording at 8471.2 MHz with Allen Telescope Array during LOI-2
<p>This dataset contains a recording of X-band telemetry signals from the Chinese lunar sample retrieve mission Chang'e 5 done on 2020-11-29 before and during the LOI-2 (lunar orbit injection 2) manoeuvre that circularized the spacecraft's elliptical lunar orbit. The recording was done at Allen Telescope Array using antenna 1h in dual XY (linear) polarization.</p> <p>The hardware configuration was as follows: antenna 1h was connected to RFCB LO d, which was tuned to a frequency of 8475 MHz and used an output IF of 512 MHz. A USRP N321 was connected to the IF output of the RFCB and digitized both polarizations. The USRP used external 10 MHz reference and PPS coming from the observatory distribution system. The IQ sample rate of the USRP was 30.72 Msps and a GNU Radio flowgraph was used to channelize four frequencies from the spacecraft (8463.7, 8471.2, 8478.6 and 8486.2 MHz), using an IQ sample rate of 240 ksps for each channel.</p> <p>The GNU Radio flowgraph stored the IQ data for each channel as 32-bit floats in the <a href="https://wiki.gnuradio.org/index.php/Metadata_Information">GNU Radio metatata file format</a>, with detached headers. After recording, the data was converted to <a href="https://github.com/gnuradio/SigMF">SigMF</a> format.</p> <p>This dataset contains the IQ data for the channel at 8471.2 MHz, which corresponds to the orbiter, in SigMF format. Each polarization is in a different file. The original metadata headers are also provided.</p> <p><strong>Note:</strong> during the observation, the frequency of the RFCB LO was lowered by exactly 30 kHz in two occasions to prevent the signals from drifting out of the channel passband due to Doppler. The two LO jumps can be easily seen in the residual carrier of the signals and corrected.</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.