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Discovery of Jupiter Family Comet 2011 UG104 Through AI Enhanced Citizen Science 通过人工智能增强公民科学发现木星家族彗星 2011 UG104
Research notes of the AAS Pub Date : 2024-05-22 DOI: 10.3847/2515-5172/ad4d9c
Jarod A. DeSpain, C. O. Chandler, Nima Sedaghat, William J. Oldroyd, C. Trujillo, William A. Burris, Henry H. Hsieh, Jay K. Kueny, Kennedy A. Farrell, Mark Jesus Mendoza Magbanua, Scott S. Sheppard, Michele T. Mazzucato, Milton K. D. Bosch, Tiffany Shaw-Diaz, Virgilio Gonano, Al Lamperti, José A. da Silva Campos, Brian L. Goodwin, Ivan A. Terentev, Charles J. A. Dukes
{"title":"Discovery of Jupiter Family Comet 2011 UG104 Through AI Enhanced Citizen Science","authors":"Jarod A. DeSpain, C. O. Chandler, Nima Sedaghat, William J. Oldroyd, C. Trujillo, William A. Burris, Henry H. Hsieh, Jay K. Kueny, Kennedy A. Farrell, Mark Jesus Mendoza Magbanua, Scott S. Sheppard, Michele T. Mazzucato, Milton K. D. Bosch, Tiffany Shaw-Diaz, Virgilio Gonano, Al Lamperti, José A. da Silva Campos, Brian L. Goodwin, Ivan A. Terentev, Charles J. A. Dukes","doi":"10.3847/2515-5172/ad4d9c","DOIUrl":"https://doi.org/10.3847/2515-5172/ad4d9c","url":null,"abstract":"\u0000 We report the discovery of cometary activity from minor planet 2011 UG104, which we classify as a Jupiter Family Comet (JFC). This discovery was aided by our Artificial Intelligence (AI) classification system: TailNet. JFC's, short-period comets with eccentric Jupiter-crossing orbits, originate from the Kuiper Belt and thus give us unique insight into the composition and distribution of volatiles in the outer solar system, past and present. Our AI assistant TailNet first classified 2011 UG104 as active, which was affirmed by Citizen Scientists on our NASA Partner Program Active Asteroids. Through further archival image searches our science team found evidence of activity on 2011 UG104 on three separate observations from 2021 February to 2021 April (81.°8 < f < 95.°0). ","PeriodicalId":74684,"journal":{"name":"Research notes of the AAS","volume":"63 21","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-05-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141110708","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Localizing Stellar Activity on Low-mass Stars with the Transiting Exoplanet Survey Satellite 利用凌日系外行星巡天卫星定位低质量恒星上的恒星活动
Research notes of the AAS Pub Date : 2024-05-22 DOI: 10.3847/2515-5172/ad4da0
Julie Moquin, Jordan Ealy, J. Schlieder, Christopher Johns-Krull
{"title":"Localizing Stellar Activity on Low-mass Stars with the Transiting Exoplanet Survey Satellite","authors":"Julie Moquin, Jordan Ealy, J. Schlieder, Christopher Johns-Krull","doi":"10.3847/2515-5172/ad4da0","DOIUrl":"https://doi.org/10.3847/2515-5172/ad4da0","url":null,"abstract":"\u0000 Magnetic reconnection is the underlying cause of stellar flares which are linked to regions of high magnetic activity, like star spots. To understand trends in stellar activity, we need to study how it is heightened by rapid rotation and deep convection in young low-mass stars. We analyze light curves of such stars observed by the Transiting Exoplanet Survey Satellite to investigate trends in flare timing with starspot modulation signals. Trends in flare properties and spot modulation can provide a means to “localize” which face of a star flares more frequently and better understand their association with active regions. We present an analysis of light curves from M and K dwarfs with no companions from five nearby and young moving groups spanning ages ∼20–150 Myr. We discuss a technique to analyze the distribution of flares and star spots and describe our results, which reveal a tentative correlation.","PeriodicalId":74684,"journal":{"name":"Research notes of the AAS","volume":"72 6","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-05-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141111827","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
A Python Project Template for Healthy Scientific Software 健康科学软件的 Python 项目模板
Research notes of the AAS Pub Date : 2024-05-21 DOI: 10.3847/2515-5172/ad4da1
Drew Oldag, Melissa DeLucchi, Wilson Beebe, Doug Branton, Sandro Campos, Colin Orion Chandler, Carl Christofferson, Andrew Connolly, Jeremy Kubica, Olivia Lynn, Konstantin Malanchev, Alex I. Malz, Rachel Mandelbaum, Sean McGuire and Chris Wenneman
{"title":"A Python Project Template for Healthy Scientific Software","authors":"Drew Oldag, Melissa DeLucchi, Wilson Beebe, Doug Branton, Sandro Campos, Colin Orion Chandler, Carl Christofferson, Andrew Connolly, Jeremy Kubica, Olivia Lynn, Konstantin Malanchev, Alex I. Malz, Rachel Mandelbaum, Sean McGuire and Chris Wenneman","doi":"10.3847/2515-5172/ad4da1","DOIUrl":"https://doi.org/10.3847/2515-5172/ad4da1","url":null,"abstract":"The creation of “healthy” scientific software is vital for its successful long-term adoption in scientific research. Here healthy code is defined to mean software that is usable, maintainable, and proffers consistently reproducible results. Incorporating tooling and practices to achieve these goals often leads to short-term, yet significant, overhead for new projects. We introduce the LINCC Frameworks Python Project Template, a configurable code template designed for scientific software projects that greatly simplifies adopting best practices by automating the setup and configuration of important tools locally and via a suite of GitHub workflows. Notably, the template does not include any application-specific code, thereby enabling users to focus on their scientific code rather than building or maintaining code infrastructure.","PeriodicalId":74684,"journal":{"name":"Research notes of the AAS","volume":"32 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-05-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141152041","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Ultracool Dwarf Absolute Magnitude Versus Spectral Type Relations for Euclid and Roman Near-infrared Filters 欧几里得和罗马近红外滤光片的超冷矮星绝对星等与光谱类型的关系
Research notes of the AAS Pub Date : 2024-05-21 DOI: 10.3847/2515-5172/ad4cec
A. Sanghi, Michael C. Liu, T. Dupuy, W. Best, R. Siverd, Zhoujian Zhang
{"title":"Ultracool Dwarf Absolute Magnitude Versus Spectral Type Relations for Euclid and Roman Near-infrared Filters","authors":"A. Sanghi, Michael C. Liu, T. Dupuy, W. Best, R. Siverd, Zhoujian Zhang","doi":"10.3847/2515-5172/ad4cec","DOIUrl":"https://doi.org/10.3847/2515-5172/ad4cec","url":null,"abstract":"\u0000 We synthesize Euclid Near Infrared Spectrometer and Photometer photometry for the Y\u0000 \u0000 E\u0000 \u0000 J\u0000 \u0000 E\u0000 \u0000 H\u0000 \u0000 E\u0000 filters and Roman Wide Field Instrument photometry for the F106, F129, F146, F158, F184 and F213 filters using SpeX prism spectra and parallaxes of 688 field-age and 151 young (≲200 Myr) ultracool dwarfs (spectral types M6–T9). For the above filters, we derive empirical absolute magnitude-spectral type polynomial relations that enable the calculation of photometric distances for ultracool dwarfs to be observed with Euclid and Roman, in the absence of parallax measurements. The synthesized photometry can also be used to generate color–color figures to distinguish high-redshift galaxies from brown dwarf interlopers.","PeriodicalId":74684,"journal":{"name":"Research notes of the AAS","volume":"23 3","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-05-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141113622","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Determination of the Abundance of Mercury from the Hg ii Line at 5677.10 Å in Late B-type Stars: Paper I—HD 35548 and HD 89822 通过 B 型晚期恒星中位于 5677.10 Å 处的 Hg ii 线确定汞的丰度：论文 I-HD 35548 和 HD 89822
Research notes of the AAS Pub Date : 2024-05-20 DOI: 10.3847/2515-5172/ad4c63
R. Monier
{"title":"Determination of the Abundance of Mercury from the Hg ii Line at 5677.10 Å in Late B-type Stars: Paper I—HD 35548 and HD 89822","authors":"R. Monier","doi":"10.3847/2515-5172/ad4c63","DOIUrl":"https://doi.org/10.3847/2515-5172/ad4c63","url":null,"abstract":"\u0000 The weak line of Hg ii located at 5677.10 Å is used to measure the mercury abundance in two mercury rich stars, HD 35548 and HD 89822. The synthesis of this line, using the current atomic parameters available in NIST, confirms that mercury is very abundant in both stars. The abundance derived from this line is in very good agreement with the abundance derived from the commonly used line at 3983.93 Å for HD 35548 but it is smaller for HD 89822.","PeriodicalId":74684,"journal":{"name":"Research notes of the AAS","volume":"74 14","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-05-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141123184","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
The Spectral ANalog of Dwarfs (SAND): New Model Atmospheres with Varying Chemistry for Galactic Archaeology with Ultracool Dwarfs 矮星光谱编目（SAND）：用于超冷矮星银河考古的不同化学性质的新大气模型
Research notes of the AAS Pub Date : 2024-05-17 DOI: 10.3847/2515-5172/ad4bd7
Efrain Alvarado, R. Gerasimov, A. Burgasser, Hunter Brooks, C. Aganze, C. Theissen
{"title":"The Spectral ANalog of Dwarfs (SAND): New Model Atmospheres with Varying Chemistry for Galactic Archaeology with Ultracool Dwarfs","authors":"Efrain Alvarado, R. Gerasimov, A. Burgasser, Hunter Brooks, C. Aganze, C. Theissen","doi":"10.3847/2515-5172/ad4bd7","DOIUrl":"https://doi.org/10.3847/2515-5172/ad4bd7","url":null,"abstract":"\u0000 The atmospheres of Ultracool Dwarfs (UCDs) are dominated by molecular chemistry, which makes their spectra and photometry particularly sensitive to elemental abundances. With lifespans in excess of the age of the universe, UCDs serve as chemical tracers in every component of the Milky Way. In this study, we present the Spectral ANalog of Dwarfs (SAND) grid of low-temperature model atmospheres that span T\u0000 eff from 700 to 4000 K, \u0000 \u0000\u0000\u0000 \u0000 log\u0000 (\u0000 g\u0000 )\u0000 \u0000 \u0000 from 4.0 to 6.0, [Fe/H] from −2.4 to +0.3, and a range of [α/Fe] that matches the Galactic distribution inferred from earlier spectroscopic surveys. The SAND grid primarily aims to model the spectra of brown dwarfs in the halo and thick disk of the Milky Way, and metal-poor UCDs in globular clusters.","PeriodicalId":74684,"journal":{"name":"Research notes of the AAS","volume":"63 8","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-05-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140965011","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Why the Laplace Resonant Angle is So Special 拉普拉斯谐振角为何如此特别
Research notes of the AAS Pub Date : 2024-05-17 DOI: 10.3847/2515-5172/ad4be8
D. Christodoulou, S. Laycock, D. Kazanas
{"title":"Why the Laplace Resonant Angle is So Special","authors":"D. Christodoulou, S. Laycock, D. Kazanas","doi":"10.3847/2515-5172/ad4be8","DOIUrl":"https://doi.org/10.3847/2515-5172/ad4be8","url":null,"abstract":"\u0000 We analyze adjacent local pairs of mean-motion resonances (MMRs) between three orbiting bodies designed to produce a Laplace resonant phase angle φ\u0000 L or one of its multiples N\u0000 φ\u0000 L, where integer N ≥ 2. This assumption yields a concrete pattern of Laplace resonances, very few of which (with angles φ\u0000 L and 2φ\u0000 L) have been observed in actual (extra)solar subsystems. All other MMRs face issues of proximity or remoteness of the orbits (they are too close or too far apart). We highlight one as yet unobservable MMR in each N-sequence for which these issues appear to be less acute.","PeriodicalId":74684,"journal":{"name":"Research notes of the AAS","volume":"57 11","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-05-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140964923","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Deep HST/UVIS Imaging of the Candidate Dark Galaxy CDG-1 候选暗星系 CDG-1 的 HST/UVIS 深度成像
Research notes of the AAS Pub Date : 2024-05-16 DOI: 10.3847/2515-5172/ad4be6
Pieter van Dokkum, Dayi David Li, Roberto Abraham, Shany Danieli, Gwendolyn M. Eadie, William E. Harris and Aaron J. Romanowsky
{"title":"Deep HST/UVIS Imaging of the Candidate Dark Galaxy CDG-1","authors":"Pieter van Dokkum, Dayi David Li, Roberto Abraham, Shany Danieli, Gwendolyn M. Eadie, William E. Harris and Aaron J. Romanowsky","doi":"10.3847/2515-5172/ad4be6","DOIUrl":"https://doi.org/10.3847/2515-5172/ad4be6","url":null,"abstract":"CDG-1 is a tight grouping of four likely globular clusters in the Perseus cluster, and a candidate dark galaxy with little or no diffuse light. Here we provide new constraints on the luminosity of any underlying stellar emission, using Hubble Space Telescope/UVIS F200LP imaging. No diffuse emission is detected, with a 2σ upper limit of F200LP > 28.1 mag arcsec−2 on the 5″ scale of CDG-1. This surface brightness limit corresponds to a 2σ lower limit of >0.5 for the fraction of the total luminosity that is in the form of globular clusters. The most likely alternative, although improbable, is that CDG-1 is a chance grouping of four globular clusters in the halo of the Perseus galaxy IC 312.","PeriodicalId":74684,"journal":{"name":"Research notes of the AAS","volume":"52 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-05-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141063082","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
Hidden Companions to Intermediate-mass Stars. XIX. Spin–Orbit Misalignment and a 0.26M ⊙, 1.8 au Companion in the Astrometric Binary Gamma Trianguli Australis* 中质量恒星的隐藏伴星。XIX.天体测量双星南三角伽马中的自旋-轨道错位和一个 0.26M ⊙, 1.8 au 伴星* .
Research notes of the AAS Pub Date : 2024-05-15 DOI: 10.3847/2515-5172/ad4a7b
I. Waisberg, Y. Klein, B. Katz
{"title":"Hidden Companions to Intermediate-mass Stars. XIX. Spin–Orbit Misalignment and a 0.26M\u0000 ⊙, 1.8 au Companion in the Astrometric Binary Gamma Trianguli Australis*","authors":"I. Waisberg, Y. Klein, B. Katz","doi":"10.3847/2515-5172/ad4a7b","DOIUrl":"https://doi.org/10.3847/2515-5172/ad4a7b","url":null,"abstract":"\u0000 Gamma Trianguli Australis is a nearby A-type star that was reported to be a 488 days astrometric binary in Gaia DR3. Here we report on a VLTI/GRAVITY observation of γ TrA in which we did not detect the companion down to a K band flux ratio of 0.5%. From the isochrone mass M\u0000 \u0000 A\u0000  = 3.04M\u0000 ⊙ of the subgiant primary, this implies a semimajor axis a\u0000 orb = 1.8 au and that the companion is a M\u0000 \u0000 B\u0000  = 0.26M\u0000 ⊙ M dwarf. The primary disk is partially resolved with an angular diameter θ\u0000 1 ≈ 1 mas ↔ 13.0R\u0000 ⊙. The differential visibility phases across the Brγ absorption line allowed us to measure the longitude of the ascending node of the primary’s rotational plane Ωrot = 212° ± 3°. This implies a spin–orbit misalignment of at least 27° ± 3° based on the Gaia astrometric solution.","PeriodicalId":74684,"journal":{"name":"Research notes of the AAS","volume":"76 2","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-05-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140975880","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
How Reliable are Rotation Period Determinations from TESS Data? 根据 TESS 数据确定自转周期的可靠性如何？
Research notes of the AAS Pub Date : 2024-05-15 DOI: 10.3847/2515-5172/ad4a7c
Mariel Lares-Martiz, Derek Buzasi, Terry Oswalt, Krystian Confeiteiro, Ahnika Gee, Luca Guida, Ryan Reynolds, Melinda Walls
{"title":"How Reliable are Rotation Period Determinations from TESS Data?","authors":"Mariel Lares-Martiz, Derek Buzasi, Terry Oswalt, Krystian Confeiteiro, Ahnika Gee, Luca Guida, Ryan Reynolds, Melinda Walls","doi":"10.3847/2515-5172/ad4a7c","DOIUrl":"https://doi.org/10.3847/2515-5172/ad4a7c","url":null,"abstract":"\u0000 Gyrochronology is the empirical relation between rotation and age. NASA's Transiting Exoplanet Survey Satellite (TESS), Kepler, and K2 missions have observed thousands of wide main sequence binaries. Since components of a binary are coeval, their rotation periods should be consistent with gyrochronology models. However, the usefulness of gyrochronology depends upon reliable rotation periods. We explore the reliability of rotation period determinations for a sample of wide binary components from the TESS cycle 3. Wide binaries with the most reliable rotation period determinations provide a strong basis for testing whether the gyrochronology empirical relation derived from open clusters is also valid for field stars.","PeriodicalId":74684,"journal":{"name":"Research notes of the AAS","volume":"133 34","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-05-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140976990","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
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