Rogerio Deienno , Larry Denneau , David Nesvorný , David Vokrouhlický , William F. Bottke , Robert Jedicke , Shantanu Naidu , Steven R. Chesley , Davide Farnocchia , Paul W. Chodas
{"title":"来自 ATLAS 望远镜的去势近地天体群","authors":"Rogerio Deienno , Larry Denneau , David Nesvorný , David Vokrouhlický , William F. Bottke , Robert Jedicke , Shantanu Naidu , Steven R. Chesley , Davide Farnocchia , Paul W. Chodas","doi":"10.1016/j.icarus.2024.116316","DOIUrl":null,"url":null,"abstract":"<div><div>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 “hiding” from CSS. Consequently, ATLAS is more powerful than CSS at debiasing the NEO population for H <span><math><mo>≲</mo></math></span> 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 <span><math><msubsup><mrow><mo>≈</mo><mn>88</mn><mtext>%</mtext></mrow><mrow><mo>−</mo><mn>2</mn><mtext>%</mtext></mrow><mrow><mo>+</mo><mn>3</mn><mtext>%</mtext></mrow></msubsup></math></span> for H <span><math><mo><</mo></math></span> 17.75 and <span><math><msubsup><mrow><mo>≈</mo><mn>36</mn><mtext>%</mtext></mrow><mrow><mo>−</mo><mn>1</mn><mtext>%</mtext></mrow><mrow><mo>+</mo><mn>1</mn><mtext>%</mtext></mrow></msubsup></math></span> for H <span><math><mo><</mo></math></span> 22.25. Those numbers are similar to previous estimates (within error bars for H <span><math><mo><</mo></math></span> 17.75) from CSS, yet, around 3% and 8% smaller at their face values, respectively. We also confirm previous finding that the <span><math><msub><mrow><mi>ν</mi></mrow><mrow><mn>6</mn></mrow></msub></math></span> 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.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"425 ","pages":"Article 116316"},"PeriodicalIF":2.5000,"publicationDate":"2024-09-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":"{\"title\":\"The debiased Near-Earth object population from ATLAS telescopes\",\"authors\":\"Rogerio Deienno , Larry Denneau , David Nesvorný , David Vokrouhlický , William F. Bottke , Robert Jedicke , Shantanu Naidu , Steven R. Chesley , Davide Farnocchia , Paul W. Chodas\",\"doi\":\"10.1016/j.icarus.2024.116316\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"<div><div>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 “hiding” from CSS. Consequently, ATLAS is more powerful than CSS at debiasing the NEO population for H <span><math><mo>≲</mo></math></span> 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 <span><math><msubsup><mrow><mo>≈</mo><mn>88</mn><mtext>%</mtext></mrow><mrow><mo>−</mo><mn>2</mn><mtext>%</mtext></mrow><mrow><mo>+</mo><mn>3</mn><mtext>%</mtext></mrow></msubsup></math></span> for H <span><math><mo><</mo></math></span> 17.75 and <span><math><msubsup><mrow><mo>≈</mo><mn>36</mn><mtext>%</mtext></mrow><mrow><mo>−</mo><mn>1</mn><mtext>%</mtext></mrow><mrow><mo>+</mo><mn>1</mn><mtext>%</mtext></mrow></msubsup></math></span> for H <span><math><mo><</mo></math></span> 22.25. Those numbers are similar to previous estimates (within error bars for H <span><math><mo><</mo></math></span> 17.75) from CSS, yet, around 3% and 8% smaller at their face values, respectively. We also confirm previous finding that the <span><math><msub><mrow><mi>ν</mi></mrow><mrow><mn>6</mn></mrow></msub></math></span> 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.</div></div>\",\"PeriodicalId\":13199,\"journal\":{\"name\":\"Icarus\",\"volume\":\"425 \",\"pages\":\"Article 116316\"},\"PeriodicalIF\":2.5000,\"publicationDate\":\"2024-09-17\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"\",\"citationCount\":\"0\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"Icarus\",\"FirstCategoryId\":\"101\",\"ListUrlMain\":\"https://www.sciencedirect.com/science/article/pii/S0019103524003762\",\"RegionNum\":2,\"RegionCategory\":\"物理与天体物理\",\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"Q2\",\"JCRName\":\"ASTRONOMY & ASTROPHYSICS\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"Icarus","FirstCategoryId":"101","ListUrlMain":"https://www.sciencedirect.com/science/article/pii/S0019103524003762","RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"Q2","JCRName":"ASTRONOMY & ASTROPHYSICS","Score":null,"Total":0}
The debiased Near-Earth object population from ATLAS telescopes
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 “hiding” from CSS. Consequently, ATLAS is more powerful than CSS at debiasing the NEO population for H 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 for H 17.75 and for H 22.25. Those numbers are similar to previous estimates (within error bars for H 17.75) from CSS, yet, around 3% and 8% smaller at their face values, respectively. We also confirm previous finding that the 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.
期刊介绍:
Icarus is devoted to the publication of original contributions in the field of Solar System studies. Manuscripts reporting the results of new research - observational, experimental, or theoretical - concerning the astronomy, geology, meteorology, physics, chemistry, biology, and other scientific aspects of our Solar System or extrasolar systems are welcome. The journal generally does not publish papers devoted exclusively to the Sun, the Earth, celestial mechanics, meteoritics, or astrophysics. Icarus does not publish papers that provide "improved" versions of Bode''s law, or other numerical relations, without a sound physical basis. Icarus does not publish meeting announcements or general notices. Reviews, historical papers, and manuscripts describing spacecraft instrumentation may be considered, but only with prior approval of the editor. An entire issue of the journal is occasionally devoted to a single subject, usually arising from a conference on the same topic. The language of publication is English. American or British usage is accepted, but not a mixture of these.