View source for Palermo scale

{{Short description|Logarithmic scale in astronomy}}
{{Use dmy dates|date=May 2019}}

The '''Palermo scale''' or '''Palermo technical impact hazard scale'''  is a [[logarithmic scale]] used by [[astronomer]]s to rate the potential hazard of impact of a [[near-Earth object]] (NEO). It combines two types of [[data]]&mdash;[[probability]] of impact and estimated [[kinetic energy|kinetic]] yield&mdash;into a single "hazard" value. A rating of 0 means the hazard is equivalent to the '''background hazard''' (defined as the average risk posed by objects of the same size or larger over the years until the date of the potential impact).<ref name="palermo"/> A rating of +2 would indicate the hazard is 100 times as great as a random background event. Scale values less than −2 reflect events for which there are no likely consequences, while Palermo scale values between −2 and 0 indicate situations that merit careful monitoring. A similar but less complex scale is the [[Torino scale]], which is used for simpler descriptions in the non-scientific media.

{{As of|2025|2|23}}, no asteroid has a cumulative rating for impacts above 0, and only two asteroids have ratings between −2 and 0. Historically, three asteroids had ratings above 0 and half a dozen more above −1, but most were downrated since.

== Scale ==

The Palermo scale was devised for astronomers to compare impact hazards at a technical level, rather than for the general public.<ref>{{cite journal |first1=Steven R. |last1=Chesley |first2=Paul W. |last2=Chodas |first3=Andrea |last3=Milani |first4=Giovanni B. |last4=Valsecchi |first5=Donald K. |last5=Yeomans |title=Quantifying the risk posed by potential Earth impacts |journal=[[Icarus (journal)|Icarus]] |volume=159 |issue=2 |pages=423––432 |date=October 2002 |doi=10.1006/icar.2002.6910 |bibcode=2002Icar..159..423C }}</ref> It was adopted at the meeting of the Working Group on Near-Earth Objects of the Scientific and Technical Subcommittee of the [[United Nations Committee on the Peaceful Uses of Outer Space]] which was held in [[Palermo]], Italy, on June 11–16, 2001.<ref>{{cite report |first1=David |last1=Morrison |first2=Andrea |last2=Milani |first3=Richard |last3=Binzel |display-authors=etal |title=Working group on near Earth objects |year=2003 |work=Transactions of the International Astronomical Union |volume=XXV A |pages=139–140 |publisher=IAU |editor-first=Hans |editor-last=Rickman |doi=10.1017/S0251107X00001358 }}</ref>

The scale compares the likelihood of the detected potential impact with the average risk posed by objects of the same size or larger over the years until the date of the potential impact. This average risk from random impacts is known as the background risk. The Palermo scale value, <math>P</math>, is defined by the equation:
:<math>P \equiv \log_{10} \frac {p_i} {f_B T}</math>
where
:*<math>p_i</math> is the impact probability
:*<math>T</math> is the time interval until the potential impact that is considered
:*<math>f_B</math> is the background impact frequency

The background impact frequency is defined for this purpose as:
:<math>f_B = 0.03\, E^{-\frac45} \text{ yr}^{-1}\;</math>
where the energy threshold <math>E</math> is measured in [[TNT equivalent|megatons]], and yr is the unit of <math>T</math> divided by one year.

For instance, this formula implies that the [[expected value]] of the time from now until the next impact greater than 1 megaton is 33 years, and that when it occurs, there is a 50% chance that it will be above 2.4 megatonnes. This formula is only valid over a certain range of <math>E</math>.

However, another paper<ref>{{cite journal |title=The flux of small near-Earth objects colliding with the Earth |author=P. Brown |display-authors=etal |journal=[[Nature (journal)|Nature]] |volume=420 |issue=6913 |pages=294–296 |date=November 2002 |bibcode=2002Natur.420..294B |doi=10.1038/nature01238 |pmid=12447433 |s2cid=4380864}}</ref> published in 2002 – the same year as the paper on which the Palermo scale is based – found a power law with different constants:

:<math>f_B = 0.00737 E^{-0.9} \;</math>

This formula gives considerably lower rates for a given <math>E</math>. For instance, it gives the rate for [[bolide]]s of 10 megatonnes or more (like the [[Tunguska explosion]]) as 1 per thousand years, rather than 1 per 210 years (or a 38% probability that it happens at least once in a century) as in the Palermo formula. However, the authors give a rather large uncertainty (once in 400 to 1800 years for 10 megatonnes), due in part to uncertainties in determining the energies of the atmospheric impacts that they used in their determination.

{| class="wikitable" style="text-align:center; font-size: 0.9em;"
|+Palermo Background Risk Chart
! rowspan="3" | Energy (MT)
! colspan="5" | Probability 
|-
! rowspan="2" | Once in<br/>this many years
! colspan="4" | At least once in one... 
|-
! decade
! century
! millennium
! million years
|-
| 0.1 || 5.28
| 87.73%
| >99.99%
| >99.99%
| >99.99%
|-
| 1 || 33.3
| 26.26%
| 95.24%
| >99.99%
| >99.99%
|-
| 10 || 210
| 4.65%
| 37.91%
| 99.15%
| >99.99%
|-
| 100  || 1,327
| 0.75%
| 7.26%
| 52.94%
| >99.99%
|-
| 1,000 || 8,373
| 0.12%
| 1.19%
| 11.26%
| >99.99%
|-
| 10,000 || 52,830
| 0.019%
| 0.19%
| 1.88%
| >99.99%
|-
| 100,000 || 333,333
| 0.003%
| 0.03%
| 0.3%
| 95.02%
|-
| 1,000,000 || 2,103,191
| 0.00048%
| 0.0048%
| 0.048%
| 37.84%
|-
| 10,000,000 || 13,270,239
| 0.000075%
| 0.00075%
| 0.0075%
| 7.26%
|-
| 100,000,000 || 83,729,548
| 0.000012%
| 0.00012%
| 0.0012%
| 1.19%
|-
| 1,000,000,000 || 528,297,731
| 0.0000019%
| 0.000019%
| 0.00019%
| 0.19%
|-
| <math>E</math> || <math>\frac{1}{f_B}=\frac{100}{3}E^{0.8}</math>
| <math>1-\left(1-f_B\right)^{10}</math>
| <math>1-\left(1-f_B\right)^{100}</math>
| <math>1-\left(1-f_B\right)^{1,000}</math>
| <math>1-\left(1-f_B\right)^{1,000,000}</math>
|}

For asteroids with multiple (<math>n</math>) potential impacts, the cumulative Palermo scale rating, <math>P_{cum}</math>, is the rating that can be calculated with the sum of the probability ratios of the individual potential impacts (each calculated with a <math>p_i</math> probability and a <math>T_i</math> time until potential impact), which can also be expressed as the logarithm of the sum of 10 raised to the <math>P_i</math> Palermo scale rating of the individual potential impacts:<ref name="palermo"/>

:<math>P_{cum} = \log_{10} \sum_{i=1}^{n} \frac {{p_i}} {f_B T_i} = log_{10}{\left(\sum_{i=1}^{n} 10^{P_i}\right)}</math>

== Risk calculation ==
{{multiple image
 |direction = vertical
 |align     = right
 |width1    = 300
 |width2    = 300
 |image1    = Apophis ellipse.svg
 |image2    = Impact probability of Apophis as function of uncertainty.jpg
 |footer    = ''Top:'' example of the shrinking and changing position of the 3-sigma uncertainty region relative to Earth in the B-plane<br>''Bottom:'' theoretical (blue and dashed red) and observational (crosses and triangles) evolution of impact probability as a function of uncertainty in the close approach distance for a bypass and an impact case, based on a planetary defense exercise using adapted real observations of [[99942 Apophis]]
}}

For [[NASA]], a unit of the [[Jet Propulsion Laboratory]] (JPL), the [[Center for Near-Earth Object Studies]] (CNEOS) calculates impact risks and assigns ratings in its [[Sentry (monitoring system)|Sentry Risk Table]],<ref name="sentry-list">{{cite web |title=Sentry: Earth Impact Monitoring. Impact Risk Data |publisher=NASA JPL CNEOS |url=https://cneos.jpl.nasa.gov/sentry/ |access-date=2025-02-08}}</ref> while another unit of JPL, Solar System Dynamics (SSD) provides orbital and close approach data.<ref name="sbdb">{{cite web |title=Small-Body Database Lookup |publisher=NASA JPL SSD |url=https://ssd.jpl.nasa.gov/tools/sbdb_lookup.html#/ |access-date=2025-02-08}}</ref> For [[European Space Agency|ESA]], similar services are provided by its [[Near-Earth Object Coordination Centre]] (NEOCC), which maintains its own Risk List<ref name="NEOCC-risk-list">{{cite web |title=Risk List |publisher=ESA NEOCC |url=https://neo.ssa.esa.int/risk-list |access-date=2025-02-08}}</ref> and Close Approaches List.<ref name="NEOCC-close-approach-list">{{cite web |title=Close Approaches |publisher=ESA NEOCC |url=https://neo.ssa.esa.int/close-approaches |access-date=2025-02-08}}</ref>

The basis for the risk evaluation is the most recent orbit calculation based on all known reliable observations. Along the calculated orbit, close approaches with Earth are determined. Due to measurement and model imprecision, the orbit calculation has an uncertainty, which can be quantified for the close approach distance. Assuming a two-dimensional [[normal distribution|Gaussian probability distribution]] in the plane perpendicular to the asteroid's orbit (the B-plane), the uncertainty can be characterised by the [[standard deviation]] (sigma) the close approach point in the directions along the asteroid's orbit and perpendicular to it, where the former is usually much larger. The one-sigma margin, which is used by ESA NEOCC one-sigma,<ref name="NEOCC-help">{{cite web |title=Help: Object |publisher=ESA NEOCC |url=https://neo.ssa.esa.int/objects/help |access-date=2025-02-08}}</ref> means that the close approach point is within those bounds with a 68.3% probability, while the 3-sigma margin, used by NASA JPL SSD, corresponds to 99.7% probability. The probability of an impact is the integral of the probability distribution over the cross section of Earth in the B-plane.

When the close approach of a newly discovered asteroid is first put on a risk list with a significant risk, it is normal for the risk to first increase, regardless whether the potential impact will eventually be ruled out or confirmed with the help of additional observations.<ref name="Smithsonian_no-panic">{{Cite news |first=Margherita |last=Bassi |title=Astronomers Raise Odds of Asteroid Impact in 2032 to 2.3 Percent—Here's Why You Shouldn't Panic |date=6 February 2025 |work=[[Smithsonian (magazine)|Smithsonian]] |url=https://www.smithsonianmag.com/smart-news/astronomers-raise-odds-of-asteroid-impact-in-2032-to-2-3-percent-heres-why-you-shouldnt-panic-180985949/ |access-date=2025-02-08 }}</ref> After discovery, Earth will be close to the center of the probability distribution, that is, the 3-sigma uncertainty margin will be much bigger than the nominal close encounter distance. With additional observations, the uncertainty will decrease, thus the 3-sigma uncertainty region will shrink, thus Earth will initially cover an increasing part of the probability distribution, resulting in increased risk, and an increasing rating. If the real orbit bypasses Earth, with further observations, Earth will only intersect the tail of the probability distribution (the 3-sigma region will shrink to exclude the Earth) and the impact risk will fall towards zero; while in case the asteroid will hit the Earth, the probability distribution will contract towards its intersection (the 3-sigma region will shrink into Earth's intersection in the B-plane) and the risk will rise towards 100%.<ref name="Reddy2022">{{cite journal |first1=Vishnu |last1=Reddy |first2=Michael S. |last2=Kelley |first3= Jessie |last3=Dotson |display-authors=etal |title=Apophis Planetary Defense Campaign |journal=[[The Planetary Science Journal]] |volume=3 |issue=5 |at=id. 123, 16 pp. |date=May 2022 |doi=10.3847/PSJ/ac66eb |doi-access=free |bibcode=2022PSJ.....3..123R }}</ref>

== Asteroids with high ratings ==
{{merge|section=yes|List of objects with non-zero Torino ratings|target=List of near-Earth objects with significant impact hazard ratings|discuss=Talk:List_of_objects_with_non-zero_Torino_ratings#Merge_proposal|date=February 2025}}
In 2002 the near-Earth asteroid {{mpl|(89959) 2002 NT|7}} reached a positive rating of 0.18 on the Palermo scale,<ref name="hohmanntransfer"/> indicating a higher-than-background threat. The value was subsequently lowered after more measurements were taken. {{mp|2002 NT|7}} is no longer considered to pose any risk and was removed from the [[Sentry (monitoring system)|Sentry Risk Table]] on 1 August 2002.<ref name="removed"/>

In September 2002, the highest Palermo rating was that of asteroid [[(29075) 1950 DA]], with a value of 0.17 for a possible collision in the year 2880.<ref name="NEO-1950DA_1"/> By March 2022, the rating had been reduced to −2.0.<ref name="SEIM29075"/><ref>{{cite web |title=Updated Calculations Refine the Impact Probability for (29075) 1950 DA |url=https://cneos.jpl.nasa.gov/news/news208.html |website=Center for NEO Studies (CNEOS) |publisher=JPL (NASA) |access-date=19 August 2022 |ref=Update}}</ref> In May 2024, a study that incorporated observations by the [[astrometry]] space observatory ''[[Gaia (spacecraft)|Gaia]]'' increased the impact risk, consequently, the rating was raised above −1 again.<ref>{{cite journal |first1=Oscar |last1=Fuentes-Muñoz |first2=Davide |last2=Farnocchia |first3=Shantanu P. |last3=Naidu |first4=Ryan S. |last4=Park |title=Asteroid Orbit Determination Using Gaia FPR: Statistical Analysis |journal=[[The Astronomical Journal]] |volume=167 |issue=6 |date=May 31, 2024 |page=290 |doi=10.3847/1538-3881/ad4291 |doi-access=free |bibcode=2024AJ....167..290F }}</ref>

For a brief period in late December 2004, with an [[observation arc]] of 190 days, asteroid {{mpl|99942 Apophis}} (then known only by its [[provisional designation]] {{mp|2004 MN|4}}) held the record for the highest Palermo scale value, with a value of 1.10 for a possible collision in the year 2029.<ref name="mirror"/> The 1.10 value indicated that a collision with this object was considered to be almost 12.6<ref name=Apophis-math>Math: 10<sup>1.10</sup>&nbsp;=&nbsp;12.589</ref> times as likely as a random background event: 1 in 37<ref name="predicting-Apophis"/> instead of 1 in 472. With further observations, the risk of impact during later close approaches was completely eliminated<ref>{{cite news |title=NASA Analysis: Earth Is Safe From Asteroid Apophis for 100-Plus Years |date=March 25, 2021 |work=News |publisher=NASA/JPL |url=https://www.jpl.nasa.gov/news/nasa-analysis-earth-is-safe-from-asteroid-apophis-for-100-plus-years |access-date=January 2, 2025 |url-status=live |archive-url=https://web.archive.org/web/20241212054436/https://www.jpl.nasa.gov/news/nasa-analysis-earth-is-safe-from-asteroid-apophis-for-100-plus-years/ |archive-date=December 12, 2024 }}</ref> and Apophis was removed from the Sentry Risk Table in February 2021.<ref name="removed"/>

{{As of|2025|2|28}}, on NASA's Sentry Risk Table,<ref name="cneos-sentry">{{cite web |title=Sentry: Earth Impact Monitoring - Impact Risk Data |url=https://cneos.jpl.nasa.gov/sentry/ |publisher=[[Jet Propulsion Laboratory]] |access-date=2025-02-23 |quote=Use unconstrained settings, sort by Palermo Scale (cum.) |archive-date=2025-01-31 |archive-url=https://web.archive.org/web/20250131135418/https://cneos.jpl.nasa.gov/sentry/ |url-status=live}}</ref> three asteroids have a cumulative Palermo scale value above −2: [[(29075) 1950 DA]] (−0.92), and [[101955 Bennu]] (−1.40). Four have cumulative Palermo scale values between −2 and −3: {{mpl|1979 XB|}} (−2.70), {{mpl|2000 SG|344}} (−2.77), {{mpl|2008 JL|3}} (−2.86) and {{mpl|2010 RF|12}} (−2.97). Of the 29 that have a cumulative Palermo scale value between −3 and −4, four were discovered in 2024: {{mpl|2024 BY|15}} (−3.30), {{mpl|2024 YR|4}} (−3.49), {{mpl|2024 JW|16}} (−3.63) and {{mpl|2024 TK|5}} (−3.76).<!-- This data should be checked by changing the default impact probability filter to "Any impact probability"-->

{{As of|2025|2|28}}, on the Risk List maintained by the [[Near-Earth Object Coordination Centre]] of the [[European Space Agency]] (ESA),<ref>{{Cite web |title=Risk List |url=https://neo.ssa.esa.int/risk-list |access-date=2025-02-20 |publisher=[[European Space Agency|ESA]] [[Near-Earth Object Coordination Centre|NEOCC]] }}</ref> one asteroid has a cumulative Palermo scale value above −2: 101955 Bennu (−1.41). Five have cumulative Palermo scale values between −2 and −3: 1950 DA (−2.13)<!-- According to email information from NEOCC, the big difference from the CNEOS figure is because CNEOS did an update including Gaia observations, while NEOCC has yet to update its software for that-->, {{mpl|2023 VD|3}} (−2.65), {{mp|1979 XB|}} (−2.72), {{mp|2000 SG|344}} (−2.78) and {{mp|2008 JL|3}} (−2.92). Of the 24 that have a cumulative Palermo scale value between −3 and −4, three were discovered in 2024 and three in 2025: {{mpl|2024 RF|10}} (−3.51), {{mp|2024 JW|16}} (−3.53), {{mp|2024 YR|4}} (−3.62), {{mpl|2025 DB|15}} (−3.70), {{mpl|2025 BA|1}} (−3.83) and {{mpl|2025 DT|2}} (−3.92).<!-- Sort by "PS cum". Note that Bennu & 1950 DA are listed separately under "Special Risk List". For those, no cumulative Palermo rating is given, it has to be calculated f.e. in an Excel table-->

{| class="wikitable" style="text-align:center; font-size: 0.9em;"
|+Historic cumulative Palermo ratings above &minus;1 in NASA's Sentry Risk Table
! rowspan=2 | Asteroid
! colspan=3 | Peak hazard
! colspan=3 | Hazard {{As of|2025|2|23|lc=y}}<ref name="cneos-sentry"/><ref name="removed"/>
|-
! Palermo rating
! Risk relative to<br>background risk
! Torino rating
! Palermo rating
! Risk relative to<br>background risk
! Torino rating

|-
| [[99942 Apophis]] || 1.10 || 12.6x greater (1260%) || 4 ||colspan="3"| ''removed from list on 21 February 2021''
|-
| {{mpl|(89959) 2002 NT|7}} || 0.18 || 1.51x greater (151%) || 1 ||colspan="3"| ''removed from list on 1 August 2002''
|-
| [[(29075) 1950 DA]] || 0.17 || 1.48x greater (148%) || - || −0.92 || 8.32x less (12.0%) || -
|--bgcolor=#c2c2c2
| background risk  || 0 || equal (100%) || - || 0 || equal (100%) || -
|-
| {{mpl|2024 YR|4}} || −0.18 || 1.51x less (66.1%) || 3  || −3.04 || 1096x less (0.09%) || 1
|-
| {{mpl|(144898) 2004 VD|17}} || −0.25 || 1.78x less (56.2%) || 2 ||colspan="3"| ''removed from list on 14 February 2008''
|-
| [[(410777) 2009 FD]] || −0.44 || 2.75x less (36.3%) || - ||colspan="3"| ''removed from list on 19 November 2020''
|-
| {{mpl|2022 AE|1}} || −0.66 || 4.57x less (21.9%) || 1 ||colspan="3"| ''removed from list on 20 January 2022''
|-
| {{mpl|2023 GQ|2}} || −0.70 || 5.01x less (20.0%) || 1 ||colspan="3"| ''removed from list on 1 May 2023''
|-
| {{mpl|2013 TV|135}} || −0.73 || 5.37x less (18.6%)  || 1||colspan="3"| ''removed from list on 8 November 2013''
|-
| {{mpl|(367789) 2011 AG|5}} || −1.00 || 10x less (10%) || 1 ||colspan="3"| ''removed from list on 21 December 2012''
|}

==See also==
*[[Asteroid impact avoidance]]
*[[Asteroid impact prediction]]
*[[Earth-grazing fireball]]
*[[Impact event]]
*[[List of asteroid close approaches to Earth]]
*[[List of Earth-crossing asteroids]]
*[[Time-domain astronomy]]

==References==
{{Reflist
| refs =

<ref name="palermo">{{cite web
  |title=Palermo Technical Impact Hazard Scale
  |publisher=NASA/JPL [[Center for Near-Earth Object Studies]]
  |url=https://cneos.jpl.nasa.gov/sentry/palermo_scale.html
  |access-date=2025-02-09
  |archive-date=14 November 2017
  |archive-url=https://web.archive.org/web/20171114131924/https://cneos.jpl.nasa.gov/sentry/palermo_scale.html
  |url-status=live
  }}</ref>

<ref name="removed">{{cite web
  |title=Sentry Risk Table - Removed Objects
  |publisher=NASA/JPL Near-Earth Object Program Office
  |url=https://cneos.jpl.nasa.gov/sentry/removed.html
  |access-date=2025-02-10
  |archive-date=17 October 2017
  |archive-url=https://web.archive.org/web/20171017180942/https://cneos.jpl.nasa.gov/sentry/removed.html
  |url-status=live
  }}</ref>

<ref name="hohmanntransfer">{{cite web
  |date=29 March 2003
  |title=How A/CC broke the 2002 NT7 story
  |publisher=hohmanntransfer
  |url=http://www.hohmanntransfer.com/sas/nt7/index.html
  |archive-url=https://web.archive.org/web/20201106104922/http://www.hohmanntransfer.com/sas/nt7/index.html
  |archive-date=2020-11-06 |url-status=dead
  |access-date=2019-04-25}}</ref>

<ref name="mirror">{{cite web
  |date=27 December 2004
  |title=2004 MN4 Earth Impact Risk Summary (computed 27 December 2004)
  |publisher=The Cosmic Mirror
  |author=Daniel Fischer
  |url=http://www.astro.uni-bonn.de/~dfischer/mirror/285neo041227.html
  |archive-url=https://web.archive.org/web/20050314032111/https://astro.uni-bonn.de/~dfischer/mirror/285neo041227.html
  |archive-date=14 March 2005
  |url-status=dead
  |access-date=2011-11-04}}</ref>

<ref name="predicting-Apophis">{{cite web
  |title=Predicting Apophis' Earth Encounters in 2029 and 2036
  |publisher=NASA/JPL Near-Earth Object Program Office
  |url=http://neo.jpl.nasa.gov/apophis/
  |archive-url=https://web.archive.org/web/20071118121950/http://neo.jpl.nasa.gov/apophis/
  |access-date=2007-12-28
  |archive-date=2007-11-18
  |url-status=dead}}</ref>

<ref name="SEIM29075">{{Cite web
  |title=Sentry: Earth Impact Monitoring: 29075
  |publisher=NASA/JPL Near-Earth Object Program Office
  |url=https://cneos.jpl.nasa.gov/sentry/details.html#?des=29075
  |archive-url=https://web.archive.org/web/20170402082636/https://cneos.jpl.nasa.gov/sentry/details.html
  |access-date=2017-06-20
  |archive-date=2017-04-02
  |url-status=live}}</ref>

<ref name="NEO-1950DA_1">{{cite web
  |title=Asteroid 1950 DA
  |publisher=NASA/JPL Near-Earth Object Program Office
  |url=http://neo.jpl.nasa.gov/1950da/
  |archive-url=https://web.archive.org/web/20021001185910/http://neo.jpl.nasa.gov/1950da/
  |access-date=2011-10-14
  |archive-date=2002-10-01
  |url-status=dead}}</ref>

<!--updated<ref name="NEO-1950DA_2">{{cite web
  |title=Asteroid 1950 DA Earth Impact Risk Summary
  |publisher=NASA/JPL Near-Earth Object Program Office
  |url=http://neo.jpl.nasa.gov/risk/a29075.html
  |archive-url=https://web.archive.org/web/20131226230040/http://neo.jpl.nasa.gov/risk/a29075.html
  |url-status=dead
  |archive-date=2013-12-26
  |access-date=2014-12-10}}</ref>-->

}}

== Further reading ==

* The primary reference for the Palermo scale is [https://dataverse.jpl.nasa.gov/dataset.xhtml?persistentId=hdl:2014/12844 "Quantifying the risk posed by potential Earth impacts"] by Chesley et al., [[Icarus (journal)|Icarus]] 159, 423-432 (2002).

==External links==
* [https://cneos.jpl.nasa.gov/sentry/palermo_scale.html Palermo Technical Impact Hazard Scale] at the [[Sentry (monitoring system)|Sentry]] monitoring system by [[Center for Near-Earth Object Studies|CNEOS]] at [[Jet Propulsion Laboratory|JPL]] from [[NASA]]

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