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132 results for “Swift”
Assessment of Mandibular Bone Invasion With MRI Using SWIFT
ClinicalTrials.gov study NCT01817140. IPD Sharing: Not stated. Countries: 1. Publications: 0.
Implantation of the HeartMate 3 in Subjects With Heart Failure Using Surgical SWIFT HM3 PMS
ClinicalTrials.gov study NCT04548128. IPD Sharing: NO. Countries: 2. Publications: 0.
System-Wide Improvement for Transitions After Surgery: The SWIFT Post op Program
ClinicalTrials.gov study NCT02543190. IPD Sharing: Not stated. Countries: 1. Publications: 0.
Trial of Oligometastasis SBRT With Immediate, Simulation-Free Treatment Delivery (OLIGO-SWIFT)
ClinicalTrials.gov study NCT07079098. IPD Sharing: NO. Countries: 1. Publications: 0.
SASSIE Arctic Field Campaign L1 SWIFT Data Fall 2022
The Salinity and Stratification at the Sea Ice Edge (SASSIE) project is a NASA experiment that aims to understand how salinity anomalies in the upper ocean generated by melting sea ice affect sea surface temperature (SST), stratification, and subsequent sea-ice growth. SASSIE involved a field campaign that sampled the transition from summer melt to autumn ice advance in the Beaufort Sea during August-October 2022, making intensive in situ and remote sensing observations within ~200km of the sea ice edge. The Surface Wave Instrument Float with Tracking (SWIFT) drifter is a passive Lagrangian wave-following sensor platform. During the SASSIE deployment, five SWIFT drifters were deployed in September 2022, collecting measurements of salinity, sea surface temperature, waves, and meteorological data. SWIFT drifter buoys contain GPS, a pulse-coherent Doppler velocity profiler, an autonomous meteorological station, and a digital video recorder. Level 1 data are available as compressed files containing graphics of the measurements alongside MATLAB and NetCDF files.
Swift Induction of Human Spinal Lower Motor Neurons and Robust ALS Cell Screening via Single-Cell Imaging
GEO Series GSE229095. Homo sapiens. 15 samples. Type: Expression profiling by high throughput sequencing.
FIGURES 5‑9 in Parasitic On Swifts (Aves, Apodiformes, Apodidae) In Brazil
FIGURES 5‑9: Dennyus (D.) pichorimi sp. nov.: female head, in dorsal view (5); female gular, thoracic sternites, and abdominal sternites I and II (6); male genitalia (7); detail of the male genital sclerite (8); female subgenital, vulvar and ventral anal setae (9). lms = lateral marginal setae; mms = median marginal setae (both on the subgenital plate); gul = gular plate; pro = prosternal plate; mes = mesosternal plate; met = metasternal plate; strI = sternite I; strII = sternite II. Scale bars = 0.1 mm (Figs. 5-7, 9); = 0.05 mm (Fig. 8).
FIGURES 1‑4 in Parasitic On Swifts (Aves, Apodiformes, Apodidae) In Brazil
FIGURES 1‑4: Dennyus (D.) pichorimi sp. nov.: male holotype in dorsal (1) and ventral (2) views; female paratype in dorsal (3) and ventral (4) views. Scale bars = 0.2 mm
Swift, Certain, and Fair: Reducing Recidivism and Improving Outcomes for Alcohol and Drug Users on State Parole
ClinicalTrials.gov study NCT03826420. IPD Sharing: UNDECIDED. Countries: 0. Publications: 0.
Swift BAT Transient Monitoring Catalog
The SWBATMONTR database table records high-level information of the lightcurves from the sources monitored with the Burst Alert Telescope (BAT) on board of Swift. The Swift/BAT Monitoring Program is aimed at (1) the discovery of new transient X-ray sources, (2) the detection of outbursts or other changes in the flux of known X-ray sources, and (3) the generation of lightcurves of more than 1000 sources spanning the entire Swift lifetime. Swift is a NASA mission with international participation dedicated to the gamma-ray burst study. It carries three instruments. The BAT is the large field of view instrument and operates in the 10-300 keV energy band; and two narrow field instruments, XRT and UVOT, that operate in the X-ray and UV/optical regime, respectively. The BAT monitoring the sky in the field of view and provides alerts when detecting a burst of flux coming from a source in the field of view. The BAT monitoring lightcurves are generated by the BAT team over the course of the Swift mission. The HEASARC ingests these data in the archive and generates this database table by collecting high-level information from the data. The lightcurves are renamed to use a consistent naming convention, and the FITS header is updated by adding standard FITS keywords. This is a service provided by NASA HEASARC .
Swift Serendipitous Survey in Deep XRT GRB Fields (SwiftFT)
This table contains the SwiftFT catalog of point sources detected by the X-ray Telescope (XRT) on board the Swift satellite in observations centered on gamma-ray bursts (GRBs) during the first four years of operation (Jan 2005 - Dec 2008). Swift is a NASA mission with international participation dedicated to the gamma-ray burst study. It carries three instruments. The BAT is the large field of view instrument and operates in the 10-300 keV energy band; and two narrow field instruments, XRT and UVOT, that operate in the X-ray and UV/optical regime, respectively. The catalog was derived including pointing positions of the 374 fields centered on the GRBs covering a total area of ~32.55 square degrees. Since GRBs are distributed randomly in the sky, the survey covers totally unrelated parts of the sky, and is highly uniform courtesy of the XRT's stable point spread function and small vignetting correction factors. The observations for a particular field were merged together and the source search analysis was restricted to a circular area of 10 arcmin radius centered in the median of the individual observation aim points. The total exposure considering all the fields is of 36.8 Ms, with ~32% of the fields having more than 100 ks exposure time, and ~28% with exposure time in the range 50-100 ks. The catalog was generated by running the detection algorithm in the XIMAGE package version 4.4.1 that locates the point sources using a sliding-cell method. The average background intensity is estimated in several small square boxes uniformly located within the image. The position and intensity of each detected source are calculated in a box whose size maximizes the signal-to-noise ratio. The detect algorithm was run separately in the following three energy bands: 0.3-3 (Soft), 2-10 (Hard), and 0.3-10 (Full) keV. For each detections the three count rates in the soft, hard, and full bands are all corrected for dead times and vignetting using exposure maps and for the PSF. Hardness ratios are calculated using the three energy band and defined as HR = (c<sub>H</sub> - c<sub>S</sub>)/(c<sub>H</sub> + c<sub>S</sub>) where c<sub>S</sub> and c<sub>H</sub> are the count rates in the S(oft) and H(ard) bands, respectively. The catalog was cleaned of spurious and extended sources by visual inspection of all the observations. Count rates in the three bands were converted into flux in the 0.5-10, 0.5-2, and 2-10 keV energy bands, respectively. The flux was estimated using a power law spectrum with photon spectral index of 1.8 and a Galactic N<sub>H</sub> of 3.3 x 10<sup>20</sup> cm<sup>-2</sup>. Each row in the catalog is a unique source. The detections from the soft, hard, and full bands were merged into a single catalog using a matching radius of 6 arcsec and retaining detection with a significance level of being spurious <= 2 x 10<sup>-5</sup> in at least one band. There are 9387 total entries in the catalog. The SWIFTFT acronym honors both the Swift satellite and the memory of Francesca Tamburelli who made numerous crucial contributions to the development of the Swift-XRT data reduction software. This database table was created by the HEASARC in November 2021 based on the electronic version available from the ASI Data Center <a href="https://www.asdc.asi.it/xrtgrbdeep_cat/">https://www.asdc.asi.it/xrtgrbdeep_cat/</a> and published in the Astronomy and Astrophysics Journal. This catalog is also available as the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/528/A122">CDS catalog J/A+A/528/A122</a>. The HEASARC added the source_number parameter, a counter to numerically identify each source in the catalog, as well as Galactic coordinates and changed the source name from SWIFTFTJHHMMSS.s+DDMM.m to SWIFTFT JHHMMSS.s+DDMM.m, adding a space between the catalog prefix and the formatted J2000 coordinates. This is a service provided by NASA HEASARC .
Swift XRT Instrument Log
The XRT runs only one type of configuration mode/window in a given time interval. The table therefore contains for a given time interval a single record that describes one configuration. A new record is generated when the following is changing within an observation: new operating mode , new pointing mode, or new window configuration. This database table is generated by the Swift Data Center. During operation, it is updated on daily basis. This is a service provided by NASA HEASARC .
Swift-XRT Monitoring of Fermi-LAT Sources of Interest
The monitoring data shown on this site provides near real-time results from Swift observations of Fermi-LAT "sources of interest" and flaring sources. While this list is dominated by blazars, some X-ray binaries and Galactic transients are also included. The preliminary results on this page are intended to provide rapid feedback to the scientific community to aid in target of opportunity planning, multiwavelength campaigns, and planning of interesting scientific publications.
Swift-INTEGRAL X-Ray (SIX) Survey Catalog
The supermassive black holes at the center of active galactic nuclei (AGNs) are surrounded by obscuring matter that can block nuclear radiation. Depending on the amount of blocked radiation, the flux from the AGN can be too faint to be detected by currently operating hard X-ray (above 15 keV) missions. At these energies, only ~1% of the intensity of the cosmic X-ray background (CXB) can be resolved into point-like sources that are AGNs. In this work, the authors address the question of undetected sources contributing to the CXB with a very sensitive and new hard X-ray survey: the Swift-INTEGRAL X-ray (SIX) survey, which is obtained with the new approach of combining the Swift/BAT and INTEGRAL/IBIS X-ray observations. The authors merge the observations of both missions, which enhances the exposure time and reduces systematic uncertainties. As a result, they obtain a new survey over a wide sky area of 6200 deg<sup>2</sup> covering the region of the North Ecliptic Pole (NEP) and extending to the contiguous Coma region that is more sensitive than the surveys of Swift/BAT or INTEGRAL/IBIS alone. Their sample comprises 113 sources having S/N ratios of above 4.8 sigma: 86 AGNs (Seyfert-like and blazars), 5 galaxies, 2 clusters of galaxies, 3 Galactic sources, 3 previously detected unidentified X-ray sources, and 14 unidentified sources. The scientific outcome from the study of the sample has been properly addressed to study the evolution of AGNs at a redshift below 0.4. The authors do not find any evolution using the 1/V<sub>max</sub> method. Their sample of faint sources is a suitable target for the new generation of hard X-ray telescopes with focusing techniques. This table was created by the HEASARC in August 2012 based on an electronic version of Table 2 from the reference paper which was obtained from the ApJS web site. This is a service provided by NASA HEASARC .
Swift/UVOT Serendipitous Source Catalog, v1.1: Observations IDs
The first version of the Swift UVOT Serendipitous Source Catalog (UVOTSSC) provides positions and magnitudes, as well as errors and upper limits of confirmed sources, for observations taken from the start of operations in 2005 until October 1st of 2010. The first version of the UVOTSSC has been produced by processing the image data obtained from the Swift Ultraviolet and Optical Telescope (UVOT). The data processing was performed at the Mullard Space Science Laboratory (MSSL, University College London, U.K.) using Swift FTOOLS from NASA's High Energy Astrophysics Software package (HEASoft-6.11), with some customizing of the UVOT packages in order to get more complete source detection and to properly apply quality flags to those sources that were detected within the UVOT image artifacts. The total number of observations with 17'x17' images used for version 1 of the catalog is 23,059, giving 6,200,016 sources in total, of which 2,027,265 have multiple entries in the source table because they have been detected in more than one observation. Some sources were only observed in one filter. The total number of entries in the source table is 13,860,568. The S/N ratio for all sources exceeds 5 in at least one UVOT filter, the rest of the filters having a S/N greater than 3. One Swift ObsID can consist of one or more images, which for this catalog have been summed, yielding the quoted total exposure times. The original UVOT images can be found in the on-line archives at MAST, and in the Swift archives at <a href="http://swift.ac.uk/">http://swift.ac.uk/</a> and at the HEASARC (<a href="http://heasarc.gsfc.nasa.gov/W3Browse/all/swiftmastr.html">http://heasarc.gsfc.nasa.gov/W3Browse/all/swiftmastr.html</a>), using the ObsID as the search key. For higher temporal resolution, the original images need to be used because the catalog data herein are summed over all of the individual images within an ObsID. The upper limits per filter for the summed images are constructed for each ObsID because the sensitivity hardly varies over the detector. Usually the images within one ObsID share the same pointing, however, whereas the quoted upper limits always apply for sources near the pointing direction given, if the images had small offsets in pointing they may not apply to sources near the edge of the summed image, which is typically about 8 arcminutes from the quoted pointing direction. U, B, V, UVW2, UVM2 and UVW1 refer to the filter bandpasses defined in the UVOT Filterwheel section of the MSSL documentation at <a href="http://www.mssl.ucl.ac.uk/www_astro/uvot/uvot_instrument/filterwheel/filterwheel.html">http://www.mssl.ucl.ac.uk/www_astro/uvot/uvot_instrument/filterwheel/filterwheel.html</a>. This HEASARC table contains version 1.1 of the Swift UVOT table of observations in which the sources in the source table were detected and contains the details of 23,059 Swift UVOT observations. The HEASARC has changed the names of many of the parameters from those given in the original table. In such cases, we have listed the original names in parentheses at the end of the parameter descriptions given below. There is a related table which lists the 13,860,568 source detections that is available at the HEASARC as the SWUVOTSSC table. This table was created by the HEASARC in May 2017 based upon the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/II/339">CDS Catalog II/339</a> file summary.dat. This is a service provided by NASA HEASARC .
Swift TDRSS Messages
This database table is derived from the Swift TDRSS messages sent on ground soon after a BAT trigger occurs on-board. For each trigger there are associated up to 14 messages, however not all are always generated and sent on ground. The messages are generated on board by the BAT, XRT and UVOT instruments and the Figure of Merit part of the observatory's autonomy. The BAT and XRT can each have five different message types. The UVOT and FOM can each have two different message types. These TDRSS messages are the results of the on-board data processing of the three instruments and some contain data products. They are first distributed via the GCN and later archived. The BAT messages are: alert, 'ack' containing the position, or 'nack' if the position could not be calculated, a lightcurve and scaled map. The XRT messages are: centroid containing the position, an image (if the position has been calculated), centroid error if the position could not be calculated, spectra in Low Rate Photodiode and Windowed Timing modes, a lightcurve. The UVOT messages are: finding chart containing star positions and a subimage centered on the XRT position. The FOM messages are used to indicate if the FOM will or will not observe the new target and if the spacecraft will (or will not) request a slew for the new target. The parameters in this database table are a collection of high level information taken from the following messages : the BAT alert, 'ack' or 'nack' message, the FOM messages, the XRT position and image. If the information is not available the fields are left blank. All messages are provided as data products within this database table. This database table is generated at the Swift processing site. During operation, it is updated on daily basis. This is a service provided by NASA HEASARC .
Swift-BAT 157-Month All-Sky Hard X-Ray Survey
This catalog includes the hard X-ray sources detected in the first 157 months of observations with the Burst Alert Telescope (BAT) coded-mask imager on board the Swift observatory. The results of the 157 months survey catalog has been obtained using data from February 2007 to December 2017 and provide a uniform hard X-ray all-sky survey with a sensitivity of 8.40 x 10<sup>-12</sup> erg/s/cm<sup>2</sup> over 90% of the sky and 7.24 x 10<sup>-12</sup> erg/s/cm<sup>2</sup> over 50% of the sky in the 14-195 keV band. The exposure time in all sky ranges from ~ 15 Ms to ~ 35 Ms, where ~ 50% of the sky achieves an exposure time of ~ 22.8 Ms. The 157 months survey provides 1891 hard X-ray sources in the 14-195 keV band above the 4.8 sigma significance level, where 259 are new detections from the 105-month catalog of which 54 are previously known source in X-ray. The sources identification is mostly from NED and SIMBAD and the 157-month catalog reports for positive identification the counterpart R.A. and Dec and the alternative name. The sources are classified in 17 different classes as follows: <pre> Class Source Type Number of Sources 0 Unknown 221 1 Galactic 4 2 Galaxy 16 3 Galaxy Cluster 26 4 Seyfert I 446 5 Seyfert II 464 6 Other AGN 130 7 Beamed AGN (Blazar/FSRQ) 192 8 LINER 7 9 Cataclysmic Variable Star (CV) 81 10 Pulsar 27 11 Supernova Remnant (SNR) 7 12 Star 26 13 High Mass X-ray Binary (HMXB) 108 14 Low Mass X-ray Binary (LMXB) 118 15 Other X-ray Binary (XRB) 17 16 Tidal Disruption Event 1 Total 1891 </pre> The data reduction, analysis, and catalog generation of the Swift-BAT are conducted following the same procedures of the previous catalog survey (Tueller+ 2010, J/ApJS/1167/186, Baumgartner+ 2013, J/ApJS/207/19). The BAT survey data are collected into arrays (Detector Plane Histograms, DPHs) where the data are binned in ~ 300 s time interval and in 8 energy band channels (14-20, 20-24, 24-35, 35-50, 50-75, 75-100, 100- 197 150, and 150-195 keV) and 1 energy total band (14-195 keV). Three different mosaic images are created from the DPH dividing the sky in 6 regions. The first set has images created in 8 energy bands to span a contiguous time interval (snapshot). The second set has images co-adding data on a time period of a month. The third set is created in 8 energy bands by Crab-weighting the monthly images in each of the energy band with the following weights (Baumgartner+ 2013, J/ApJS/207/19): 27.000, 35.260, 22.700, 29.444, 21.272, 16.062, 8.449, 2.630. The benchmark Crab spectrum adopted is F(E) = 10.17E−2.15 photon cm2 s keV. The source detection algorithm uses the Crab-weighted mosaic images. For each source detected lightcurves and spectra are derived. The lightcurves are obtained from the snapshot images, the mosaic monthly images and the Crab-weighted mosaic images. The spectra are obtained from an additional set of mosaic images by adding all the snapshots for the 157 months period in 8-bands. All the analyses use HEASoft tools version 6.23, and the most recent BAT calibration database (updated on Oct. 3, 2017). Data products are generated for each source detected and these are: three different lightcurves in FITS format obtained from the snapshot, monthly and Crab-weighted monthly mosaic images and the equivalent plots as GIF images; an 8-channel average spectrum in FITS obtained using all 157 months; and a GIF file showing the spectrum with the fit to the best parameter of the power-law model. The snapshot lightcurves report rates for the 8-energy band, the monthly and Crab-weighted monthly mosaic lightcurves reports rated for the 8-energy band and the total band 14-195 keV. This table was ingested by the HEASARC in February 2025 based upon the published 157-month catalog. The catalog is also available at <a href="https://swift.gsfc.nasa.gov/results/bs157mon/">https://swift.gsfc.nasa.gov/results/bs157mon/</a>. This is a service provided by NASA HEASARC .
Swift BAT 100-Month Supergiant Fast X-Ray Transient Catalog
Supergiant Fast X-ray Transients (SFXTs) are High Mass X-ray Binaries (HMXBs) that are defined by their hard X-ray flaring behavior. During such flares they reach peak luminosities of 10<sup>36</sup> - 10<sup>37</sup> erg/s for a few hours (in the hard X-ray), i.e., much shorter timescales than those characterizing Be/X-ray binaries. The authors have investigated the characteristics of bright flares (detections in excess of 5 sigma) for a sample of SFXTs and their relation to the orbital phase. They have retrieved all Swift/BAT Transient Monitor light curves, and collected all detections in excess of 5 sigma from both daily- and orbital-averaged light curves in the time range from 2005 February 12 to 2013 May 31 (MJD 53413 - 56443). The authors also considered all on-board detections as recorded in the same time span and selected those within 4 arcminutes of each source in their sample and in excess of 5 sigma. This table contains the catalog of over a thousand Burst Alert Telescope (BAT) flares from 11 SFXTs, down to 15-150 keV fluxes of ~6 x 10<sup>-10</sup>erg/cm<sup>2</sup>/s (daily timescale) and ~1.5 x 10<sup>-9</sup>erg/cm<sup>2</sup>/s (orbital timescale, averaging ~800s) and spanning 100 months. The great majority of these flares are unpublished. This population is characterized by short (a few hundred seconds) and relatively bright (in excess of 100 milliCrab, 15-50 keV) events. In the hard X-ray, these flares last in general much less than a day. Clustering of hard X-ray flares can be used to indirectly measure the length of an outburst, even when the low-level emission is not detected. In their paper, the authors construct the distributions of flares, of their significance (in terms of sigma) and their flux as a function of orbital phase, to infer the properties of these binary systems. In particular, they observe a trend of clustering of flares at some phases as P_orb increases, as consistent with a progression from tight, circular or mildly eccentric orbits at short periods, to wider and more eccentric orbits at longer orbital periods. Finally, the authors estimate the expected number of flares for a given source for their limiting flux and provide the recipe for calculating them for the limiting flux of future hard X-ray observatories. The BAT observes 88% of the sky daily, on average, so it is ideally suited to detect flaring in hard X-ray sources. Since 2005-02-12, the BAT Transient Monitor (Krimm et al. 2013, ApJS, 209, 14) has been providing near real-time light curves in the 15-50 keV energy range of more than 900 sources with a mean variance for one-day mosaics of 5.3 milliCrab. Several flares from SFXTs are regularly caught every year by the BAT Transient Monitor (BATTM). The catalog contains a total of 1117 flares from 11 SFXT sources (the only other confirmed SFXT, IGR J11215-5952, never triggered the BAT: see Section 2.2 of the reference paper for more information about this source). They are divided into 46 BAT triggers (bat_subsample_flag = 'T', 43 in outbursts), 126 daily-averaged BATTM light curves (bat_subsample_flag = 'D'), 267 orbital-averaged BATTM light curves (bat_subsample_flag = 'O'), and 678 on-board detections (bat_subsample_flag = 'B'). For each flare, the time of the occurrence, duration, flux, and significance are reported. Given the cut in sigma applied to the available BATTM and on-board detections, this catalog is a flux-limited sample of flares. Assuming a Crab-like spectrum (power-law of photon index 2.15), 5 sigma detections for one day and an average orbit typically correspond to fluxes of 5.98 x 10<sup>-10</sup> and 1.46 x 10<sup>-9</sup> erg cm<sup>-2</sup> s<sup>-1</sup>, respectively, in the 15-150 keV band (or 3.38 x 10<sup>-10</sup> and 8.24 x 10<sup>-10</sup> erg cm<sup>-2</sup> s<sup>-1</sup> in the 15-50 keV band). This table was created by the HEASARC in August 2015 based on the union of <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/562/A2">CDS Catalog J/A+A/562/A2</a> files sample.dat (the properties of the confirmed SFXTs) and table4.dat (the catalog of the 1117 flares detected by the Swift BAT from 11 of the 12 confirmed SFXTs). This is a service provided by NASA HEASARC .
Swift-XRT Point Source Catalog (2SXPS)
This table contains the second Swift X-ray Point Source (2SXPS) catalog of detections by the Swift X-ray Telescope (XRT) used in Photon Counting (PC) mode in the 0.3-10 keV energy range. Swift is a NASA mission with international participation dedicated to the gamma-ray burst study. It carries three instruments. The BAT is the large field-of-view instrument and operates in the 10-300 keV energy band; and two narrow field instruments, XRT and UVOT, that operate in the X-ray and UV/optical regime, respectively. The overall 2SXPS catalog characteristics are as follows: <pre> Data included 2005 Jan 01 - 2018 August 01 Sky coverage 3,790 square degrees Typical Sensitivity (0.3-10 keV) 2x10<sup>-13</sup> erg cm<sup>-2</sup> s<sup>-1</sup> (observations) 4x10<sup>-14</sup> erg cm<sup>-2</sup> s<sup>-1</sup> (stacked images) Typical position error 5.6" (90% confidence radius, including systematics) Detections 1,091,058 Unique sources 206,335 Variable sources 82,324 Uncatalogued sources 78,100 False positive rate Flag=Good 0.3% Flag=Good/Reasonable 1% Flag=Good/Reasonable/Poor <10% </pre> This catalog enhances the 1SXPS catalogue (Evans, P. A., et al. 2014, ApJS, 210, 8) in different ways. The 2SXPS catalog uses an improved Point Spread Function (PSF) and pile-up models, a better source detection pipeline that includes a technique to model the effects of stray light, and tests to automatically avoid diffuse emission and ~six years more data. The results are that the 2SXPS catalog contains 50% more temporal coverage than 1SXPS, a sky coverage of 3790 square deg almost double compare to the 1SXPS (1905 square Degree) and ~30% more sources compared to the 1SXPS. The Swift XRT observations were filtered to remove times when: a) data were contaminated by scattered light from the daylight side of the Earth; b) the on-board astrometry derived from the images obtained by the Swift UV/Optical telescope was unreliable; and c) observations with less than 100s of PC mode. The 127519 observations included in the catalog provide a total usable exposure is 266.5 Ms. A Swift observation is a collection of snapshots and the source detection algorithm was run on individual observation as well as on stacked images. The latter were generated on a grid of 2,300x2,300 pixels (~ 90'x90') to ensure that every overlap between observations is in at least one stacked image. A total of 14628 stacked images were generated. Each record corresponds to a unique source which characteristics are described with 230 parameters. The catalog reports for each source rates in four energy band (0.3-10.keV, 0.3-1. keV, 1-2 keV and 3-10 keV), background rates, variability for each energy band, two hardness ratio, peak rate and several spectral parameters. The hardness ratios are defined as follows: <pre> HR1 = (M-S)/(M+S) where M and S are the medium (1-2 keV) and soft (0.3-1 keV) band count rates HR2 = (H-M)/(H+M) where H and M are the hard (2-10 keV) and medium (1-2 keV) band count rates </pre> and they are calculated using all observations. The peak rate is determined using three different timescale: the count rate considering all the observations (see parameters rates in this database), the count rate in each observation (not reported in this database) and the count rate in each snapshot (not reported in this database). The peak rate is the rate +/- error from the timescale which has the highest 1-sigma lower-limit on the count rate. Spectral parameters and source flux are estimated using three different methods for two spectral models, a power-law and APEC (see Smith et al., 2001, ApJL, 556, L91). Not all sources have values for all three methods. The parameters starting with "fix" are defined for every source and uses fixed spectral model parameters: a photon index of 1.7 for a power-law model, a temperature of kT=1keV for the APEC model and for both models uses the Galactic absorption listed in the parameter "nh". The parameters starting "intr" have been inferred from the hardness ratio. Look-up tables containing (HR1, HR2, NH, photon index) and (HR1, HR2, NH, kT) are pre-calculated for the power-law and APEC models. If the source HR1 and HR2 are close to the values in the table, spectral parameters are derived by interpolating the HR1 and HR2 in the look-up tables that are close to the HR1 and HR2 of the source. The parameters starting with "fit" have been derived from fitting an actual source spectrum in XSPEC and they are only available for the brightest sources (>50 net counts, and at least one detection in a single observation). The parameters fields starting with "pow" and "apec" report the values from the 'best' of these methods. The parameters "which_pow" and "which_apec" indicates which of the three methods are reported. The catalog also inclu
Swift Gamma Ray Burst Compilation by Burst Advocate
This database table includes the early results published in the Gamma-Ray Burst Coordinates Network (GCN) circulars on GRBs detected by the Swift observatory and GRBs detected first by other observatories and followed by Swift. The Swift observatory has a rapid (minute timescale) response to GRB detection and performs sensitive X-ray and optical afterglow observations of hundreds of GRBs on all timescales, from minutes to even months later. The instrumentation consists in a large field of view (FOV) instrument, the Burst Alert Telescope (BAT, 15-150 keV) and two narrow field of view instruments, the Ultraviolet/Optical Telescope (UVOT) and the X-ray Telescope (XRT). The BAT searches the sky for gamma-ray bursts (GRBs), determines their location with a precision of a few arcminutes, and triggers an autonomous spacecraft slew to place the burst in the FOV of the narrow field instruments. The first-look data from the three Swift instruments for a newly discovered GRB and its afterglow are transmitted to the ground via TDRSS. The complete telemetry (including the messages transmitted via TDRSS) is subsequently sent down via the Malindi ground station. The information transmitted via TDRSS are broadcast via the the Gamma-Ray Burst Coordinates Network (GCN) followed by subsequent GCN circular based on the early ground analysis of the data collected by Malindi. If the GRB is triggered by Swift , this table records the initial characteristic associated to a burst obtained with the data coming via TDRSS and initial data downloaded via Malindi which results are published via the GCN. In addition the table reports other burst characteristics as for redshift obtained by observations with ground observatories. If the GRB is detected first by other observatories, the table reports results obtained with the ground analysis of the Malindi data and published via the GCN. This database table is generated by compiling the results of the GCN circulars. It was added to the HEASARC database in March 2025. During operation, it is updated weekly and/or for any new trigger. This table is also available at <a href="https://swift.gsfc.nasa.gov/archive/grb_table/">https://swift.gsfc.nasa.gov/archive/grb_table/</a>. This is a service provided by NASA HEASARC .
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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)
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.