The debiased Near-Earth object population from ATLAS telescopes

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F25%3A10511170" target="_blank" >RIV/00216208:11320/25:10511170 - isvavai.cz</a>

Výsledek na webu

<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=KKcC4J9Hly" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=KKcC4J9Hly</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1016/j.icarus.2024.116316" target="_blank" >10.1016/j.icarus.2024.116316</a>

Jazyk výsledku

angličtina

Název v původním jazyce

The debiased Near-Earth object population from ATLAS telescopes

Popis výsledku v původním jazyce

This work is dedicated to debias the Near-Earth Object (NEO) population based on observations from the Asteroid Terrestrial-impact Last Alert System (ATLAS) telescopes. We have applied similar methods used to develop the recently released NEO model generator (NEOMOD), once debiasing the NEO population using data from Catalina Sky Survey (CSS) G96 telescope. ATLAS is composed of four different telescopes. We first analyzed observational data from each of all four telescopes separately and later combined them. Our results highlight main differences between CSS and ATLAS, e.g., sky coverage and survey power at debiasing the NEO population. ATLAS has a much larger sky coverage than CSS, allowing it to find bright NEOs that would be constantly &quot;hiding&quot;from CSS. Consequently, ATLAS is more powerful than CSS at debiasing the NEO population for H less than or similar to 19. With its intrinsically greater sensitivity and emphasis on observing near opposition, CSS excels in the debiasing of smaller objects. ATLAS, as an all sky survey designed to find imminent hazardous objects, necessarily spends a significant fraction of time looking at places on the sky where objects do not appear, reducing its power for debiasing the population of small objects. We estimate a NEO population completeness of approximate to 88%(+3%)(-2% ) for H &lt; 17.75 and approximate to 36%(+1%)(-1% ) for H &lt; 22.25. Those numbers are similar to previous estimates (within error bars for H &lt; 17.75) from CSS, yet, around 3% and 8% smaller at their face values, respectively. We also confirm previous finding that the V(6 )secular resonance is the main source of small and faint NEOs at H = 28, whereas the 3:1 mean motion resonance with Jupiter dominates for larger and brighter NEOs at H = 15.

Název v anglickém jazyce

The debiased Near-Earth object population from ATLAS telescopes

Popis výsledku anglicky

This work is dedicated to debias the Near-Earth Object (NEO) population based on observations from the Asteroid Terrestrial-impact Last Alert System (ATLAS) telescopes. We have applied similar methods used to develop the recently released NEO model generator (NEOMOD), once debiasing the NEO population using data from Catalina Sky Survey (CSS) G96 telescope. ATLAS is composed of four different telescopes. We first analyzed observational data from each of all four telescopes separately and later combined them. Our results highlight main differences between CSS and ATLAS, e.g., sky coverage and survey power at debiasing the NEO population. ATLAS has a much larger sky coverage than CSS, allowing it to find bright NEOs that would be constantly &quot;hiding&quot;from CSS. Consequently, ATLAS is more powerful than CSS at debiasing the NEO population for H less than or similar to 19. With its intrinsically greater sensitivity and emphasis on observing near opposition, CSS excels in the debiasing of smaller objects. ATLAS, as an all sky survey designed to find imminent hazardous objects, necessarily spends a significant fraction of time looking at places on the sky where objects do not appear, reducing its power for debiasing the population of small objects. We estimate a NEO population completeness of approximate to 88%(+3%)(-2% ) for H &lt; 17.75 and approximate to 36%(+1%)(-1% ) for H &lt; 22.25. Those numbers are similar to previous estimates (within error bars for H &lt; 17.75) from CSS, yet, around 3% and 8% smaller at their face values, respectively. We also confirm previous finding that the V(6 )secular resonance is the main source of small and faint NEOs at H = 28, whereas the 3:1 mean motion resonance with Jupiter dominates for larger and brighter NEOs at H = 15.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/GA23-04946S" target="_blank" >GA23-04946S: Studium vývojových drah asteroidů řízených negravitačními silami pomocí fotometrických pozorování</a><br>

Návaznosti

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Rok uplatnění

2025

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Icarus

ISSN

0019-1035

e-ISSN

1090-2643

Svazek periodika

425

Číslo periodika v rámci svazku

leden

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

17

Strana od-do

116316

Kód UT WoS článku

001327660500001

EID výsledku v databázi Scopus

2-s2.0-85204790725