Neil Gehrels Swift Observatory

<h2 id="overview">Overview</h2>
Swift is a multi-<a href="/facts/Wavelength/kcJU0ymz">wavelength</a> <a href="/facts/Space_observatory/BtI46sDX">space observatory</a> dedicated to the study of <a href="/facts/Gamma-ray_burst/oRRU6Fhn">gamma-ray bursts</a>. Its three instruments work together to observe GRBs and their afterglows in the <a href="/facts/Gamma-ray/5Drf913J">gamma-ray</a>, <a href="/facts/X-ray/wseP79cN">X-ray</a>, <a href="/facts/Ultraviolet/kncBUqn5">ultraviolet</a>, and <a href="/facts/Optics/p0vq4S1T">optical</a> wavebands.
Based on continuous scans of the area of the sky with one of the instrument's monitors, Swift uses <a href="/facts/Momentum_wheel/m3M5RKGF">momentum wheels</a> to autonomously slew into the direction of possible GRBs. The name "Swift" is not a mission-related acronym, but rather a reference to the instrument's rapid <a href="/facts/Slew_(spacecraft)/8FvjQFUJ">slew</a> capability, and the nimble <a href="/facts/Swift_(bird)/VCEvAWuo">swift</a> (bird of the same name).<a class="footnote-ref" id="fnref:5" href="#fn:5">5</a> All of Swift's discoveries are transmitted to the ground and those data are available to other observatories which join Swift in observing the GRBs.
In the time between GRB events, Swift is available for other scientific investigations, and scientists from universities and other organizations can submit proposals for observations.
The Swift Mission Operation Center (MOC), where commanding of the satellite is performed, is located in <a href="/facts/State_College,_Pennsylvania/RFXIGMtX">State College, Pennsylvania</a> and operated by the <a href="/facts/Pennsylvania_State_University/WMQagtjM">Pennsylvania State University</a> and industry subcontractors. The Swift main ground station is located at the <a href="/facts/Broglio_Space_Center/0aNwJMSd">Broglio Space Center</a> near <a href="/facts/Malindi/bnbJLTq6">Malindi</a> on the coast of eastern <a href="/facts/Kenya/Y9Ko9pQu">Kenya</a>, and is operated by the <a href="/facts/Italian_Space_Agency/HNANQ521">Italian Space Agency</a> (ASI). The Swift Science Data Center (SDC) and archive are located at the Goddard Space Flight Center outside <a href="/facts/Washington,_D.C./enXPK156">Washington, D.C.</a> The United Kingdom Swift Science Data Centre is located at the <a href="/facts/University_of_Leicester/Q0vDtHV7">University of Leicester</a>.
The Swift <a href="/facts/Satellite_bus/UMlFYAUY">satellite bus</a> was built by <a href="/facts/Spectrum_Astro/vcPBvCul">Spectrum Astro</a>, which was later acquired by <a href="/facts/General_Dynamics_Mission_Systems/L8g4qvGA">General Dynamics Advanced Information Systems</a>,<a class="footnote-ref" id="fnref:6" href="#fn:6">6</a> which was in turn acquired by <a href="/facts/Orbital_Sciences_Corporation/WNB0SKlF">Orbital Sciences Corporation</a> (now <a href="/facts/Northrop_Grumman_Innovation_Systems/zwkJhWEe">Northrop Grumman Innovation Systems</a>).

<h2 id="instruments">Instruments</h2>
<h3>Burst Alert Telescope (BAT)</h3>

The BAT detects GRB events and computes its coordinates in the sky. It covers a large fraction of the sky (over one <a href="/facts/Steradian/PRCqT4n1">steradian</a> fully coded, three steradians partially coded; by comparison, the full sky solid angle is <a href="/facts/Solid_angle/se8IXufg">4π</a> or about 12.6 steradians). It locates the position of each event with an accuracy of 1 to 4 <a href="/facts/Minute_and_second_of_arc/tybs6YGC">arcminutes</a> within 15 <a href="/facts/Second/jtFxnJXx">seconds</a>. This crude position is immediately relayed to the ground, and some wide-field, rapid-slew ground-based telescopes can catch the GRB with this information. The BAT uses a <a href="/facts/Coded_aperture/5nc897I9">coded-aperture mask</a> of 52,000 randomly placed 5 mm (0.20 in) <a href="/facts/Lead/EYljasJN">lead</a> tiles, 1 m (3 ft 3 in) above a detector plane of 32,768 4 mm (0.16 in) <a href="/facts/Cadmium_zinc_telluride/yqG0NEUa">Cadmium zinc telluride</a> (CdZnTe) hard X-ray detector tiles; it is purpose-built for Swift. Energy range: 15–150 <a href="/facts/Electronvolt/YMT1fqX9">keV</a>.<a class="footnote-ref" id="fnref:7" href="#fn:7">7</a>

<h3>X-ray Telescope (XRT)</h3>

The XRT <a class="footnote-ref" id="fnref:8" href="#fn:8">8</a> can take images and perform <a href="/facts/Spectroscopy/mj71FuNK">spectral analysis</a> of the GRB afterglow. This provides more precise location of the GRB, with a typical error circle of approximately 2 <a href="/facts/Minute_and_second_of_arc/tybs6YGC">arcseconds</a> radius. The XRT is also used to perform long-term monitoring of GRB afterglow light-curves for days to weeks after the event, depending on the brightness of the afterglow. The XRT uses a <a href="/facts/Wolter_telescope/MxpwmMI5">Wolter Type I X-ray telescope</a> with 12 nested mirrors, focused onto a single MOS <a href="/facts/Charge-coupled_device/l6xffIcz">charge-coupled device</a> (CCD) similar to those used by the <a href="/facts/XMM-Newton/rXRB4WRM">XMM-Newton</a> EPIC MOS cameras. On-board software allows fully automated observations, with the instrument selecting an appropriate observing mode for each object, based on its measured count rate. The telescope has an energy range of 0.2–10 keV.<a class="footnote-ref" id="fnref:9" href="#fn:9">9</a>

<h3>Ultraviolet/Optical Telescope (UVOT)</h3>

After Swift has slewed towards a GRB, the <a href="/facts/Ultraviolet/Optical_Telescope/N4wdjRmL">UVOT</a> is used to detect an optical afterglow. The UVOT provides a sub-arcsecond position and provides optical and ultra-violet photometry through lenticular filters and low resolution spectra (170–650 nm) through the use of its optical and UV <a href="/facts/Grism/7SYQXuHj">grisms</a>. The UVOT is also used to provide long-term follow-ups of GRB afterglow lightcurves. The UVOT is based on the <a href="/facts/XMM-Newton/rXRB4WRM">XMM-Newton</a>'s Optical Monitor (OM) instrument, with improved optics and upgraded onboard processing computers.<a class="footnote-ref" id="fnref:10" href="#fn:10">10</a>
On 9 November 2011, UVOT photographed the asteroid <a href="/facts/(308635)_2005_YU55/7DmUBGK1">2005 YU55</a> as the <a href="/facts/Asteroid/g7Ulr1VB">asteroid</a> made a close flyby of the <a href="/facts/Earth/HLLmDfj0">Earth</a>.<a class="footnote-ref" id="fnref:11" href="#fn:11">11</a>
On 3 June 2013, UVOT unveiled a massive ultraviolet survey of the nearby <a href="/facts/Magellanic_Clouds/WEspxUJl">Magellanic Clouds</a>.<a class="footnote-ref" id="fnref:12" href="#fn:12">12</a>
In August 2017, UVOT imaged UV emissions from gravitational wave event <a href="/facts/GW170817/q78LSs5w">GW170817</a> detected by LIGO & Virgo detectors.<a class="footnote-ref" id="fnref:13" href="#fn:13">13</a><a class="footnote-ref" id="fnref:14" href="#fn:14">14</a>

<h2 id="experiments">Experiments</h2>

<h3>Burst Alert Telescope (BAT)</h3>
BAT (Burst Alert Telescope) is a gamma ray telescope, built by NASA's Goddard Space Flight Center, uses a coded aperture to locate the source. The software to locate the source is provided by the <a href="/facts/Los_Alamos_National_Laboratory/tlrLkV7r">Los Alamos National Laboratory</a> (LANL). The CdZnTe detector of 5,200 cm2 (810 sq in) area, consisting of 32,500 units of 4 × 4 × 2 mm (0.157 × 0.157 × 0.079 in), can pin-point the location of sources within 1.4 arcminutes. The energy range is 15-150 keV.<a class="footnote-ref" id="fnref:15" href="#fn:15">15</a>

<h3>Ultraviolet/Optical Telescope (UVOT)</h3>
UVOT (Ultraviolet/Optical Telescope) monitors the afterglow in ultraviolet and visible light, and locates the source at an accuracy of one arcsecond. Its aperture is 30 cm (12 in), with an f-number equal to 12.7, and is backed by 2048 x 2048 <a href="/facts/Photon/mFNhAEzA">photon</a> counting CCD <a href="/facts/Pixel/UzwBvXBV">pixels</a>. The source location accuracy is better than one arcsecond.<a class="footnote-ref" id="fnref:16" href="#fn:16">16</a>

<h3>X-Ray Telescope (XRT)</h3>
XRT (X-Ray Telescope) aims at the source more accurately, and monitors the afterglow in X-rays. It was built jointly by the <a href="/facts/Pennsylvania_State_University/WMQagtjM">Pennsylvania State University</a> (PSU), the <a href="/facts/Brera_Astronomical_Observatory/c4doIE7E">Brera Astronomical Observatory</a>, Italy, and the <a href="/facts/University_of_Leicester/Q0vDtHV7">University of Leicester</a>, United Kingdom. It has a detector of area 135 cm2 (20.9 sq in) consisting of 600 x 600 pixels, and covers the energy range of 0.2-10 keV. It can locate the afterglow source at an accuracy of four arcseconds.<a class="footnote-ref" id="fnref:17" href="#fn:17">17</a>

<h2 id="mission-goals">Mission goals</h2>
The Swift mission has four key scientific objectives:

<ul><li>To determine the origin of GRBs. There seem to be at least two types of GRBs, only one of which can be explained with a <a href="/facts/Hypernova/7f0l3sQB">hypernova</a>, creating a gamma-ray beam. More data is needed to explore other explanations</li>
<li>To use GRBs to expand understanding of the young <a href="/facts/Universe/XbfpnDmM">universe</a>. GRBs seem to take place at "cosmological distances" of many millions or billions of <a href="/facts/Light-years/IGc5NdQb">light-years</a>, which means they can be used to probe the distant, and therefore young, cosmos</li>
<li>To conduct an all-sky survey which will be more sensitive than any previous one, and will add significantly to scientific knowledge of astronomical X-ray sources. Thus, it could also yield unexpected results</li>
<li>To serve as a general purpose gamma-ray/X-ray/optical observatory platform, performing rapid "target of opportunity" observations of many transient astrophysical phenomena, such as <a href="/facts/Supernova/Pfo2J23l">supernova</a></li></ul>
<h2 id="mission-history">Mission history</h2>

Swift was launched on 20 November 2004, at 17:16:01 <a href="/facts/Coordinated_Universal_Time/2EnjfSyu">UTC</a> aboard a <a href="/facts/Delta_II/GoBa3Qch">Delta II</a> 7320-10C from <a href="/facts/Cape_Canaveral_Space_Force_Station/dwJ9MCPH">Cape Canaveral Air Force Station</a> and reached a near-perfect orbit of 585 × 604 km (364 × 375 mi) <a href="/facts/Altitude/B5eNVurK">altitude</a>, with an <a href="/facts/Orbital_inclination/TQCFWyfd">inclination</a> of 20.60°.<a class="footnote-ref" id="fnref:18" href="#fn:18">18</a>
On 4 December 2004, an anomaly occurred during instrument activation when the Thermo-Electric Cooler (TEC) Power Supply for the X-Ray Telescope did not turn on as expected. The XRT Team at University of Leicester and Pennsylvania State University were able to determine on 8 December 2004 that the XRT would be usable even without the TEC being operational. Additional testing on 16 December 2004 did not yield any further information as to the cause of the anomaly.
On 17 December 2004 at 07:28:30 UTC, the Swift Burst Alert Telescope (BAT) triggered and located on board an apparent gamma-ray burst during launch and early operations.<a class="footnote-ref" id="fnref:19" href="#fn:19">19</a> The spacecraft did not autonomously slew to the burst since normal operation had not yet begun, and autonomous slewing was not yet enabled. Swift had its first GRB trigger during a period when the autonomous slewing was enabled on 17 January 2005, at about 12:55 UTC. It pointed the XRT telescope to the on-board computed coordinates and observed a bright X-ray source in the field of view.<a class="footnote-ref" id="fnref:20" href="#fn:20">20</a>
On 1 February 2005, the mission team released the <a href="/facts/First_light_(astronomy)/pHI5o0r0">first light</a> picture of the UVOT instrument and declared Swift operational.
By May 2010, Swift had detected more than 500 GRBs.<a class="footnote-ref" id="fnref:21" href="#fn:21">21</a>
By October 2013, Swift had detected more than 800 GRBs.<a class="footnote-ref" id="fnref:22" href="#fn:22">22</a>
On 27 October 2015, Swift detected its 1,000th GRB, an event named GRB 151027B and located in the constellation <a href="/facts/Eridanus_(constellation)/cvtlSUun">Eridanus</a>.<a class="footnote-ref" id="fnref:23" href="#fn:23">23</a>
On 10 January 2018, NASA announced that the Swift spacecraft had been renamed the Neil Gehrels Swift Observatory in honor of mission PI <a href="/facts/Neil_Gehrels/1UK7tJ0I">Neil Gehrels</a>, who died in early 2017.<a class="footnote-ref" id="fnref:24" href="#fn:24">24</a><a class="footnote-ref" id="fnref:25" href="#fn:25">25</a>
Swift entered safe mode on March 15, 2024 (after the 2nd of 4 gyroscopes failed) and was not conducting science. A software patch for two-gyroscope mode was developed, uplinked and tested in April 2024, and Swift returned to nominal operations at that point.<a class="footnote-ref" id="fnref:26" href="#fn:26">26</a>

<h2 id="notable-detections">Notable detections</h2>

<ul><li>9 May 2005: Swift detected <a href="/facts/GRB_050509B/H65X46ew">GRB 050509B</a>, a burst of gamma rays that lasted one-twentieth of a second. The detection marked the first time that the accurate location of a short-duration gamma-ray burst had been identified and the first detection of X-ray afterglow in an individual short burst.<a class="footnote-ref" id="fnref:27" href="#fn:27">27</a><a class="footnote-ref" id="fnref:28" href="#fn:28">28</a></li>
<li>4 September 2005: Swift detected <a href="/facts/GRB_050904/q7YmwPrH">GRB 050904</a> with a <a href="/facts/Redshift/Qfl4VjDF">redshift</a> value of 6.29 and a duration of 200 seconds (most of the detected bursts last about 10 seconds). It was also found to be the most distant yet detected, at approximately 12.6 billion <a href="/facts/Light-year/IGc5NdQb">light-years</a>.</li>
<li>18 February 2006: Swift detected <a href="/facts/GRB_060218/95kfHCdx">GRB 060218</a>, an unusually long (about 2000 seconds) and nearby (about 440 million light-years) burst, which was unusually dim despite its close distance, and may be an indication of an imminent <a href="/facts/Supernova/Pfo2J23l">supernova</a>.</li>
<li>14 June 2006: Swift detected <a href="/facts/GRB_060614/tJDkpRgI">GRB 060614</a>, a burst of gamma rays that lasted 102 seconds in a distant galaxy (about 1.6 billion light-years). No supernova was seen following this event (and GRB 060505 to deep limits) leading some to speculate that it represented a new class of progenitors. Others suggested that these events could have been massive star deaths, but ones which produced too little radioactive <a href="/facts/Isotopes_of_nickel/3jPqldnR">56Ni</a> to power a supernova explosion.</li>
<li>9 January 2008: Swift was observing a supernova in <a href="/facts/NGC_2770/0y739nXn">NGC 2770</a> when it witnessed an X-ray burst coming from the same galaxy. The source of this burst was found to be the beginning of another supernova, later called <a href="/facts/SN_2008D/kP6I5hYe">SN 2008D</a>. Never before had a supernova been seen at such an early stage in its evolution. Following this stroke of luck (position, time, most appropriate instruments), astronomers were able to study in detail this <a href="/facts/Type_Ib_and_Ic_supernovae/UgGGLu6C">Type Ibc supernova</a> with the <a href="/facts/Hubble_Space_Telescope/NQeIf0vw">Hubble Space Telescope</a>, the <a href="/facts/Chandra_X-ray_Observatory/zU89xG3a">Chandra X-ray Observatory</a>, the <a href="/facts/Very_Large_Array/WqKH7Dq9">Very Large Array</a> in <a href="/facts/New_Mexico/wosJCGaW">New Mexico</a>, the <a href="/facts/Gemini_North/Yz6vJvms">Gemini North</a> telescope in <a href="/facts/Hawaii/ImxFefeK">Hawaii</a>, <a href="/facts/Gemini_South/Yz6vJvms">Gemini South</a> in Chile, the <a href="/facts/Keck_I/4yhJmNde">Keck I</a> telescope in Hawaii, the 1.3 m (4 ft 3 in) PAIRITEL telescope at <a href="/facts/Mount_Hopkins_(California)/lLGctIfn">Mount Hopkins</a>, the <a href="/facts/Hale_Telescope/NNgtWTV9">200-inch</a> and 60 in (1,500 mm) telescopes at the <a href="/facts/Palomar_Observatory/vRLjmDfr">Palomar Observatory</a> in <a href="/facts/California/zLW2vdQJ">California</a>, and the 3.5 m (11 ft) telescope at the <a href="/facts/Apache_Point_Observatory/UPJCGavT">Apache Point Observatory</a> in New Mexico. The significance of this supernova was likened by discovery team leader <a href="/facts/Alicia_Soderberg/9kTL3oBW">Alicia Soderberg</a> to that of the <a href="/facts/Rosetta_Stone/8JLFP1NN">Rosetta Stone</a> for egyptology.<a class="footnote-ref" id="fnref:29" href="#fn:29">29</a></li>
<li>8 and 13 February 2008: Swift provided critical information about the nature of <a href="/facts/Hanny%27s_Voorwerp/glw5Cfap">Hanny's Voorwerp</a>, mainly the absence of an ionizing source within the Voorwerp or in the neighboring <a href="/facts/IC_2497/tKMWyth0">IC 2497</a>.</li>
<li>19 March 2008: Swift detected <a href="/facts/GRB_080319B/7XcLcly2">GRB 080319B</a>, a burst of gamma rays amongst the brightest celestial objects ever witnessed. At 7.5 billion <a href="/facts/Light-year/IGc5NdQb">light-years</a>, Swift established a new record for the farthest object (briefly) visible to the naked eye. It was also said to be 2.5 million times intrinsically brighter than the previous <a href="/facts/SN_2005ap/ouMK2BzP">brightest accepted supernova (SN 2005ap)</a>. Swift observed a record four GRBs that day, which also coincided with the death of noted science-fiction writer <a href="/facts/Arthur_C._Clarke/2XJ6UGDB">Arthur C. Clarke</a>.<a class="footnote-ref" id="fnref:30" href="#fn:30">30</a></li>
<li>13 September 2008: Swift detected <a href="/facts/GRB_080913/4UxbTvxs">GRB 080913</a>, at the time the most distant GRB observed (12.8 billion light-years) until the observation of <a href="/facts/GRB_090423/jbvvdsK1">GRB 090423</a> a few months later.<a class="footnote-ref" id="fnref:31" href="#fn:31">31</a><a class="footnote-ref" id="fnref:32" href="#fn:32">32</a></li>
<li>23 April 2009: Swift detected <a href="/facts/GRB_090423/jbvvdsK1">GRB 090423</a>, the most distant cosmic explosion ever seen at that time, at 13.035 billion light-years. In other words, the universe was only 630 million years old when this burst occurred.<a class="footnote-ref" id="fnref:33" href="#fn:33">33</a></li>
<li>29 April 2009: Swift detected <a href="/facts/GRB_090429B/43HwdjeJ">GRB 090429B</a>, which was found by later analysis published in 2011 to be 13.14 billion light-years distant (approximately equivalent to 520 million years after the Big Bang), even farther than GRB 090423.<a class="footnote-ref" id="fnref:34" href="#fn:34">34</a></li>
<li>16 March 2010: Swift tied its record by again detecting and localizing four bursts in a single day.</li>
<li>13 April 2010: Swift detected its 500th GRB.<a class="footnote-ref" id="fnref:35" href="#fn:35">35</a></li>
<li>28 March 2011: Swift detected Swift J1644+57 which subsequent analysis showed to possibly be the signature of a star being disrupted by a black hole or the ignition of an active galactic nucleus.<a class="footnote-ref" id="fnref:36" href="#fn:36">36</a> "This is truly different from any explosive event we have seen before", said <a href="/facts/Joshua_Bloom/Cd2snGgu">Joshua Bloom</a> of the <a href="/facts/University_of_California,_Berkeley/MXVEjklr">University of California, Berkeley</a>, the lead author of the study published in the June issue of <a href="/facts/Science_(journal)/uTyzjkwD">Science</a>.<a class="footnote-ref" id="fnref:37" href="#fn:37">37</a></li>
<li>16 and 17 September 2012: BAT triggered two times on a previously unknown hard X-ray source, named <a href="/facts/Sw_J1745-26/FVPhh2Gc">Sw J1745-26</a>, a few degrees from the <a href="/facts/Galactic_Center/TI4MwWwM">Galactic Center</a>. The outburst, produced by a rare X-ray nova, announced the presence of a previously unknown stellar-mass black hole undergoing a dramatic transition from the low/hard to the high/soft state.<a class="footnote-ref" id="fnref:38" href="#fn:38">38</a><a class="footnote-ref" id="fnref:39" href="#fn:39">39</a><a class="footnote-ref" id="fnref:40" href="#fn:40">40</a></li>
<li>2013: Discovery of ultra-long class of gamma-ray bursts</li>
<li>24 April 2013: Swift detected an X-ray flare from the Galactic Center. This proved not to be related to <a href="/facts/Sgr_A*/5TWIRfgm">Sgr A*</a> but to a previously unsuspected <a href="/facts/Magnetar/By90KFyJ">magnetar</a>. Later observations by the <a href="/facts/NuSTAR/IfaBc33v">NuSTAR</a> and the <a href="/facts/Chandra_X-ray_Observatory/zU89xG3a">Chandra X-ray Observatory</a> confirmed the detection.<a class="footnote-ref" id="fnref:41" href="#fn:41">41</a></li>
<li>27 April 2013: Swift detected the "shockingly bright" Gamma-ray burst <a href="/facts/GRB_130427A/uqbjz7Y4">GRB 130427A</a>. Observed simultaneously by the <a href="/facts/Fermi_Gamma-ray_Space_Telescope/rwKktSFn">Fermi Gamma-ray Space Telescope</a>, it is one of the five closest GRBs detected and one of the brightest seen by either space telescope.<a class="footnote-ref" id="fnref:42" href="#fn:42">42</a></li>
<li>3 June 2013: Evidence for kilonova emission in short GRB</li>
<li>23 April 2014: Swift detected the strongest, hottest, and longest-lasting sequence of stellar flares ever seen from a <a href="/facts/DG_Canum_Venaticorum/FLrGn1Ds">nearby red dwarf star</a>. The initial blast from this record-setting series of explosions was as much as 10,000 times more powerful than the largest solar flare ever recorded.<a class="footnote-ref" id="fnref:43" href="#fn:43">43</a></li>
<li>3 May 2014: Detection of a UV Pulse from an iPTF discovered young Type Ia SN</li>
<li>June–July 2015: The <a href="/facts/Brown_dwarf/fa7kr9lH">brown dwarf</a> OGLE-2015-BLG-1319 was discovered using the <a href="/facts/Gravitational_microlensing/JL0fXQRC">gravitational microlensing</a> detection method in a joint effort between Swift, <a href="/facts/Spitzer_Space_Telescope/Ic1xXIYb">Spitzer Space Telescope</a>, and the ground-based <a href="/facts/Optical_Gravitational_Lensing_Experiment/FkmStM7p">Optical Gravitational Lensing Experiment</a>, the first time two space telescopes have observed the same microlensing event. This method was possible because of the large separation between the two spacecraft: Swift is in <a href="/facts/Low_Earth_orbit/rq1TwayJ">low Earth orbit</a> while Spitzer is more than one <a href="/facts/Astronomical_unit/gjsbu5xU">AU</a> distant in an Earth-trailing <a href="/facts/Heliocentric_orbit/b4zMv2jE">heliocentric orbit</a>. This separation provided significantly different perspectives of the brown dwarf, allowing for constraints to be placed on some of the object's physical characteristics.<a class="footnote-ref" id="fnref:44" href="#fn:44">44</a></li>
<li>27 October 2015: Swift detected its 1000th gamma-ray burst, GRB 151027B.<a class="footnote-ref" id="fnref:45" href="#fn:45">45</a></li>
<li>18 August 2017: Swift discovers UV emission from the <a href="/facts/Kilonova/okpV1akI">kilonova</a> <a href="/facts/AT_2017gfo/q78LSs5w">AT 2017gfo</a>, the electromagnetic counterpart to <a href="/facts/GW170817/q78LSs5w">GW170817</a>.<a class="footnote-ref" id="fnref:46" href="#fn:46">46</a></li>
<li>23 September 2017: Swift is the first to identify TXS 0506+056 as the possible source of the IceCube-170922A extremely high energy (EHE) <a href="/facts/Neutrino/yGWVfSg2">neutrinos</a>.<a class="footnote-ref" id="fnref:47" href="#fn:47">47</a></li>
<li>14 January 2019: Swift discovers the most powerful observed gamma-ray burst, <a href="/facts/GRB_190114C/h2wFr865">GRB 190114C</a>, reaching <a href="/facts/Teraelectronvolt/YMT1fqX9">teraelectronvolt</a> energies.<a class="footnote-ref" id="fnref:48" href="#fn:48">48</a></li>
<li>09 October 2022: Swift discovers, simultaneously with Fermi, <a href="/facts/GRB_221009A/CYxPkjrm">GRB 221009A</a>, one of the closest GRBs ever detected and the brightest ever detected.</li></ul>
<h2 id="see-also">See also</h2>
<ul>
<li>Spaceflight portal</li></ul>
<ul><li><a href="/facts/List_of_gamma-ray_bursts/aD5hFLbx">List of gamma-ray bursts</a></li>
<li><a href="/facts/List_of_X-ray_space_telescopes/0HK80fnv">List of X-ray space telescopes</a></li>
<li><a href="/facts/GRB_221009A/CYxPkjrm">GRB 221009A</a></li>
<li><a href="/facts/Space_Variable_Objects_Monitor/36Y0kqxh">Space Variable Objects Monitor</a> (SVOM), the planned successor of Swift</li></ul>

<h2 id="further-reading">Further reading</h2>
<ul><li>McKee, Maggie (6 April 2005). <a href="https://www.newscientist.com/article/dn7237">"Swift measures distance to gamma-ray bursts"</a>. New Scientist.</li></ul>
<h2 id="external-links">External links</h2>

Wikimedia Commons has media related to Swift Gamma-Ray Burst Mission.

<ul><li><a href="https://swift.gsfc.nasa.gov/">Swift website</a> by NASA/GSFC</li>
<li><a href="http://www.swift.ac.uk/">Swift website</a> by the UK Swift Science Data Centre</li>
<li><a href="http://www.swift.psu.edu/">Swift website</a> by Pennsylvania State University</li>
<li><a href="http://swift.sonoma.edu/">Swift website</a> by Sonoma State University</li>
<li><a href="http://grb.sonoma.edu/">Gamma-ray Burst Real-time Sky Map</a></li></ul>

<h2 id="references">References</h2>

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</ol>

Neil Gehrels Swift Observatory open-in-new

Neil Gehrels Swift Observatory