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Dataset results
126 results for “Photometry”
Synthetic J-H-K-W1-W2-W3-G-B-V photometry for random population of binary & single stars
<p>Table of synthetic photometry for ~800k stars, randomly distributed in the following ranges:</p> <ul> <li>mass_A = (0.2, 2.0)</li> <li>log10(age) = (8.0, 9.9)</li> <li>feh = N(0, 0.2)</li> <li>distance = (50, 2000) [pc]</li> <li>A_V = (0, 1)</li> <li>q (mass ratio) = (0.2, 1); mass_B = q * mass_A</li> </ul> <p>The table has columns for all the synthetic photometry as well as columns for the true properties and a boolean column for "is_binary"; the synthetic photometry is only a sum of the two stars if is_binary is True; otherwise the photometry is just for the primary star. Synthetic photometry is done using the MIST model grids, implemented by isochrones (github.com/timothydmorton/isochrones)</p> <p>The purpose of this table is to act a synthetic training set for single/binary classification algorithms.</p>
Gaia TGAS with 2MASS, WISE and Tycho2 photometry
<p>Crossmatch done taking the proper motions and epoch of the catalogues into account. This file should/will be replaced by one using the cross match tables provided by the Gaia Archive.</p> <p>Shared here by Ronald Drimmel for the Gaia Sprint NYC workshop, 2016.</p>
Color weight photometry
<p>Dataset relative to the following publication:</p> <p>Koenderink, J.J., van Doorn, A.& Gegenfurtner, K.R. (2016) Color weight photometry. Vision Research, in press.</p> <p>See the file README.txt for further information.</p>
Data and Software for: Resolved Near-infrared Stellar Photometry from the Magellan Telescope for 13 Nearby Galaxies: JAGB Method Distances
<p><strong>12/17/24 Update: I was made aware that the MRT files had the J-band and H-band column header labels incorrectly switched (this occured when converting the CSV files to MRT). I have fixed this mistake. The CSV files were correct the entire time. No data have been changed. Apologies for any inconvinence this may have caused. </strong></p> <p> </p> <p>Data for Resolved Near-infrared Stellar Photometry from the Magellan Telescope for 13 Nearby Galaxies: JAGB Method Distances</p> <p>The files are provided in two formats. A CSV format with a single line header, and a MRT files (zipped) written in the machine-readable format used by AAS & CDS: <a href="https://journals.aas.org/mrt-overview/" target="_blank" rel="noopener noreferrer">https://journals.aas.org/mrt-overview/</a></p> <p>Column descriptions in photometry catalogs:</p> <p>X/Y: Image coordinates from Fourstar camera</p> <p>J, J_err: J-band magnitudes and photometric errors returned from DAOPHOT/ALLFRAME</p> <p>H, H_er: H-band magnitudes and photometric errors returned from DAOPHOT/ALLFRAME</p> <p>K, K_err: K-band magnitudes and photometric errors returned from DAOPHOT/ALLFRAME</p> <p>chi: chi value returned from DAOPHOT/ALLFRAME</p> <p>sharp: sharpness value returned from DAOPHOT/ALLFRAME</p> <p>ra/dec: RA/Decl </p> <p>RGC: semi-major axis distance</p> <p> </p> <p>Notes on versions: all catalogs from all versions contain the same information, style was just adjusted to adhere to AAS standards. </p> <p> </p>
photometry
<p>Photometry catalogs</p>
CeA Psilocin fiber photometry study: Data and custom code from experiments looking at changes in calcium dynamics in response to an air puff events
<p>Psilocybin, and its active metabolite psilocin, have been shown to elicit rapid and long-lasting symptom improvements in a variety of affective psychiatric illnesses. However, the specific mechanisms behind these therapeutic effects remain relatively unknown. The central amygdala (CeA) is a primary output region within the extended amygdala that is heavily dysregulated in affective psychiatric disorders. Here, we utilized fiber photometry to measure changes in CeA reactivity to an aversive air puff stimulus after psilocin administration, both acutely and at varying prolonged time points. We found that administration of psilocin increased reactivity acutely in females, but not males. Additionally, we show that one dose of psilocin produced decreases in reactivity in males, but not females, 28-days post administration, with decreases seen as early as 2-days post administration. We further report stimulus-specific changes in CeA reactivity after psilocin with differential responsivity to an aversive air puff stimulus and an auditory stimulus. We also measured changes in behavioral response to the air puff stimulus and report sex differences in exploratory behavior but not threat responding or general locomotion. This study provides evidence that a single dose of psilocin can elicit sex-specific, dynamic, and enduring changes in CeA reactivity to an aversive stimulus. These data are an important step towards dissecting circuit-based mechanisms underlying the effects of psychedelics.</p>
SN2011fe late photometry dataset
<p>Dataset for doing late time photometry of SN2011fe published in http://adsabs.harvard.edu/abs/2017MNRAS.472.2534K. Please cite this paper when working with this dataset. </p>
Data from: Heterogeneous distribution of kinesin-streptavidin complexes revealed by mass photometry
<p>Kinesin-streptavidin complexes are widely used in microtubule-based active-matter studies. The stoichiometry of the complexes is empirically tuned but experimentally challenging to determine. Here, mass photometry measurements reveal heterogenous distributions of kinesin-streptavidin complexes. Our binding model indicates that heterogeneity arises from both the kinesin-streptavidin mixing ratio and the kinesin-biotinylation efficiency.</p>
Catalogues containing photometry in 22 passbands for 603311 LMC stars and 124578 SMC stars from Bellazzini & Pascale 2024, A&A,
<p>Catalogues from the paper "The RGB Tip in the SDSS, PS1, JWST, NGRST and Euclid photometric systems. Calibration in optical passbands using Gaia DR3 synthetic photometry" by M. Bellazzini (INAF - OAS Bo) & R. Pascale (INAF - OAS Bo), A&A, in press, (<a href="https://arxiv.org/abs/2406.04781" target="_blank" rel="noopener">arXiv:2406.04781</a>). Stars have been selected from the Gaia DR3 dataset and the magnitudes has been obtained from the Gaia GSPC catalogue of from GaiaXPy as described in Gaia Collaboration 2023.</p> <div>Each catalogue contains:</div> <div> </div> <div> <ul> <li>Column 1-15, parameters directly extracted from the Gaia DR3 source catalogue, namely: source_id, ra, dec, parallax, parallax_error, pmra, pmra_error, pmdec, pmdec_error, ruwe, phot_variable_flag, and non_single_star.</li> <li>Column 16: C⋆, a parameter that is derived from phot_bp_rp_excess_factor (that, in turn, has been extracted from the Gaia DR3 source catalogue) following (Riello et al. 2021).</li> <li>Column 17: colour excess E(B-V), derived from Skowronet al. (2021) and Schlegel et al. (1998); Schlafly & Finkbeiner (2011) as described in Sect. 2.</li> <li>Columns 18-27: standardised ugriz magnitudes in the SDSS system extracted from the Gaia DR3 GSPC (Gaia Collaboration et al. 2023a) and associated uncertainties.</li> <li>Columns 28-37: standardised UBVRI magnitudes in the JKCsystem extracted from the Gaia DR3 GSPC (Gaia Collaboration et al. 2023a) and associated uncertainties.</li> <li>Columns 38-47: standardised grizy magnitudes in the PS1 system computed with GaiaXPy and associated uncertainties.</li> <li>Columns 48-51: standardised F606W, F814W magnitudes in the HST ACS-WFC system extracted from the Gaia DR3 GSPC (Gaia Collaboration et al. 2023a) and associated uncertainties.</li> <li>Columns 52-55: non-standardised F070W and F090W magnitudes in the JWST-NIRCAM system computed with GaiaXPy and associated uncertainties.</li> <li>Columns 56-59: non-standardised R062 and Z087 magnitudes in the NGRST system computed with GaiaXPy and associated uncertainties .</li> <li>Columns 60-61: non-standardised I_E magnitude in the Euclid-VIS system computed with GaiaXPy and associated uncer-tainties (in this case, not corrected for the bias described in Sect. 2.1 of Gaia Collaboration et al. 2023a, hence slightly underestimated).</li> </ul> <p><strong>It is very important to remind </strong>that u_SDSS and U_JKC magnitudes from Gaia XPSP are significantly less accurate and pre-<br>cise than all the other magnitudes included in our catalogues (see Gaia Collaboration et al. 2023a, for detailed discussion).<br>Each star can lack some of the 22 magnitudes listed in the catalogues, depending on the signal-to-noise constraints applied to the original GSPC (S/N> 30 Gaia Collaboration et al. 2023a). For example, of the 603311 stars listed in the LMC sample only 83229(85338) have valid u_SDSS (U_JKC ) magnitudes. See Bellazzini & Pascale 2024 for further details and references.</p> </div> <p><strong>We cannot give any hint or guarantee on the behaviour of the completeness of the samples</strong> as a function of the various magnitudes and colours, as well as as a function of position in the sky (see Bellazzini & Pascale 2024 for details on the selections applied).</p>
Confronting sparse Gaia DR3 photometry with TESS for a sample of around 60,000 OBAF-type pulsators
<p>This listing contains the results produced as part of the paper "Confronting sparse Gaia DR3 photometry with TESS for a sample of around 60,000 OBAF-type pulsators" by Hey & Aerts, 2024.</p> <p>A description of the tables is as follows;</p> <ol> <li><strong>prewhiten_all.json</strong>: The frequencies, amplitudes, and phases of all targets in the sample prewhitened to a 1% false alarm level.</li> <li><strong>prewhiten_all_cleaned.json</strong>: The same as Table 1, where combination frequencies have been removed.</li> <li><strong>full_sample_prediction_paper.csv</strong>: The results of the classification for each variability class.</li> <li><strong>ranked_table_revised.csv:</strong> The final ranking of the targets for future studies.</li> </ol>
GRB 070306: Observing log and results from photometry
<p>Observation log and photometric results of GRB 070306 from Jaunsen et al. (2008), Ap.J. 681, p.453-461</p> <p> </p>
MACADAMIA Sloan Digital Sky Survey Asteroid Photometry, Measurements, and Images
<p>This dataset contains data from the Multi-Archive Catalog of Asteroid Detections And Measurements for Interactive Access (MACADAMIA), specifically of numbered asteroids observed serendipitously by the Sloan Digital Sky Survey (SDSS).</p> <p>photometry_archive_20201027.db is a SQLite database containing data corresponding to a search of the SDSS image archive conducted on 2020 May 1 of all numbered asteroids known at the time, which yielded 2.84 million search results, 1.98 million detections that were determined to actually be within the field of view of the identified image, and 993,777 successfully measured detections. Preview images of all detections and non-detections where the object was determined to be within the field of view of an identified image are collected in the detection_previews_*tar.gz files in this dataset, indexed by detection_id in the photometry database and listed under preview_image_file in the detection_data table.</p> <p>photometry_archive_20210927.db contains an update to the SDSS search, containing data corresponding to a search of the SDSS image archive conducted on 2021 July 2 of all numbered asteroids known at the time, which yielded 2.96 million search results, 2.06 million detections that were determined to actually be within the field of view of the identified image, and 1.02 million successfully measured detections. Previews of additional detections identified in this updated search may not be available due to data loss in a system failure in August 2023.</p> <p> </p>
Photometry and Spectroscopy of a z=9.51 galaxy in the RXJ2129 cluster field
<p>Reduced HST and JWST imaging, plus reduced JWST spectroscopy, of a redshift z=9.51 galaxy that is triply imaged and highly magnified by the RXJ2129 galaxy cluster. </p>
Photometry of outer Solar System objects from the Dark Energy Survey I: photometric methods, light curve distributions and trans-Neptunian binaries - data release
<p>This repository contains the full data release for the 814 outer Solar System objects found in the Dark Energy Survey.</p> <p>A full description of the object search is described in <a href="http://(https://ui.adsabs.harvard.edu/abs/2022ApJS..258...41B/abstract">Bernardinelli et al (2022)</a>, and a full description of the photometric processing is described in<a href="https://ui.adsabs.harvard.edu/abs/2023arXiv230403017B/abstract"> Bernardinelli et al (2023)</a>. If you use these files, we ask you to cite the corresponding papers.</p> <p>The FITS table `y6_des_tnos_color.fits` contains both the orbital elements and the colors for each object. The full description of the orbital element information is given in Table 3 of <a href="https://ui.adsabs.harvard.edu/abs/2022ApJS..258...41B/abstract">Bernardinelli et al (2022</a>). In addition to these, the table also includes the mean absolute magnitudes in each band, as well as mean <span class="math-tex">\((g-r, r-i, r-z)\)</span> colors and their corresponding covariance matrix, and the 68% confidence interval for the lightcurve amplitude.</p> <p>Inside the `fluxes` directory, the complete photometric record for each object is included in a `hdf5` file (for each object), and the MCMC chains for their fluxes and LCAs. The three Jupyter Notebooks included in the `notebooks` directory explains the columns and how to use these files to reproduce the results of the paper. Inside this directory there are also additional files needed to reproduce the code.</p> <p>The `binary` directory has the MCMC chains for their mutual orbits (in `.npy` files), as well as the astrometric and photometric record for the binary measurements. Another `README` file is included in that directory with a detailed explanation.</p>
Ages and metallicities of stellar clusters using S-PLUS narrow-band integrated photometry: the Small Magellanic Cloud
<p>These are the final photometric quantities measured in the work "Ages and metallicities of stellar clusters using S-PLUS narrow-band integrated photometry: the Small Magellanic Cloud". The raw S-PLUS images are available upon request to the corresponding author. Nevertheless, the complete S-PLUS data will become publicly available alongside the next data release, scheduled for 2023.</p>
Data from: Heterogeneous distribution of kinesin-streptavidin complexes revealed by mass photometry
Open the record for dataset details and reuse information.
Kisspeptin photometry recordings during pregnancy and lactation
Open the record for dataset details and reuse information.
CeA Psilocin fiber photometry study: Data and custom code from experiments looking at changes in calcium dynamics in response to an air puff events
Open the record for dataset details and reuse information.
NASA Sun Photometry Data at the Sevilleta National Wildlife Refuge, New Mexico (1994-present)
A sun photometer was installed at the Sevilleta Field Station in 1994.It is part of a network of such instruments deployed around the world within a program called AERONET (AErosol RObotic NETwork http://aeronet.gsfc.nasa.gov/new_web/system_descriptions.html) established by NASA to obtain a measure of atmospheric aerosols around the globe.  Individual photometer units are designed to view the sun and sky at preprogrammed intervals throughout the day for the measurement of aerosol optical thickness, water vapor amounts, ozone levels, particle size distribution, aerosol scattering, phase function, and single scattering albedo.  These measurements can also be used to radiometrically correct satellite imagery.  The unit consists of A) the photometer, B) a robot for directing the photometer at the sun, C) a CIMEL datalogger which directs the data collection and storage, D) a DCP (Data Collection Platform) which controls hourly data transmission to the GOES satellite and E) an antenna for facilitating this DCP to satellite link.  Solar measurements are made at 1021, 871, 669, 498, 437, 379, and 339 nm.  The Sevilleta LTER is responsible for maintenance of the unit on site while NASA takes care of data processing and and storage and annual re-calibration of the unit.  Data can be obtained from NASA via:http://aeronet.gsfc.nasa.gov/cgi-bin/type_piece_of_map_opera_v2_new.
Mitigating flicker noise in high-precision photometry. I - Characterization of the noise structure, impact on the inferred transit parameters, and predictions for CHEOPS observations
<p>This repository contains the publicly available artificial exoplanet transit light curves that has been generated in HMI observations.</p> <p>Descriptions of the data are encapsulated in the READme.dat file. For further details, please report to Sec. 3 of the paper (arXiV link: <a href="https://arxiv.org/abs/2003.07707">https://arxiv.org/abs/2003.07707</a>).</p> <p>If you find these synthetic data useful in your own research please cite the Sulis. et al., (2020) paper.</p> <p> </p> <p> </p> <p> </p> <p> </p>
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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)
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DANDI Archive for NWB datasets
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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.