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The TESS-Keck Survey. XVII. Precise Mass Measurements in a Young, High-multiplicity Transiting Planet System Using Radial Velocities and Transit Timing Variations TESS-Keck 勘测。XVII.利用径向速度和凌日时间变化精确测量年轻高多倍性凌日行星系统的质量
The Astronomical Journal Pub Date : 2024-01-29 DOI: 10.3847/1538-3881/ad1330
C. Beard, Paul Robertson, F. Dai, R. Holcomb, J. Lubin, Joseph M. Akana Murphy, N. Batalha, S. Blunt, I. Crossfield, C. Dressing, B. Fulton, A. Howard, Dan Huber, H. Isaacson, S. R. Kane, G. Nowak, E. Petigura, Arpita Roy, R. Rubenzahl, L. Weiss, Rafael Barrena, A. Behmard, C. Brinkman, I. Carleo, A. Chontos, P. Dalba, T. Fetherolf, S. Giacalone, M. Hill, K. Kawauchi, J. Korth, R. Luque, M. MacDougall, A. Mayo, T. Močnik, Giuseppe Morello, F. Murgas, J. Orell-Miquel, E. Pallé, A. Polanski, M. Rice, N. Scarsdale, Dakotah B. Tyler, Judah Van Zandt
{"title":"The TESS-Keck Survey. XVII. Precise Mass Measurements in a Young, High-multiplicity Transiting Planet System Using Radial Velocities and Transit Timing Variations","authors":"C. Beard, Paul Robertson, F. Dai, R. Holcomb, J. Lubin, Joseph M. Akana Murphy, N. Batalha, S. Blunt, I. Crossfield, C. Dressing, B. Fulton, A. Howard, Dan Huber, H. Isaacson, S. R. Kane, G. Nowak, E. Petigura, Arpita Roy, R. Rubenzahl, L. Weiss, Rafael Barrena, A. Behmard, C. Brinkman, I. Carleo, A. Chontos, P. Dalba, T. Fetherolf, S. Giacalone, M. Hill, K. Kawauchi, J. Korth, R. Luque, M. MacDougall, A. Mayo, T. Močnik, Giuseppe Morello, F. Murgas, J. Orell-Miquel, E. Pallé, A. Polanski, M. Rice, N. Scarsdale, Dakotah B. Tyler, Judah Van Zandt","doi":"10.3847/1538-3881/ad1330","DOIUrl":"https://doi.org/10.3847/1538-3881/ad1330","url":null,"abstract":"\u0000 <jats:p>We present a radial velocity (RV) analysis of TOI-1136, a bright Transiting Exoplanet Survey Satellite (TESS) system with six confirmed transiting planets, and a seventh single-transiting planet candidate. All planets in the system are amenable to transmission spectroscopy, making TOI-1136 one of the best targets for intra-system comparison of exoplanet atmospheres. TOI-1136 is young (∼700 Myr), and the system exhibits transit timing variations (TTVs). The youth of the system contributes to high stellar variability on the order of 50 m s<jats:sup>−1</jats:sup>, much larger than the likely RV amplitude of any of the transiting exoplanets. Utilizing 359 High Resolution Echelle Spectrometer and Automated Planet Finder RVs collected as part of the TESS-Keck Survey, and 51 High-Accuracy Radial velocity Planetary Searcher North RVs, we experiment with a joint TTV-RV fit. With seven possible transiting planets, TTVs, more than 400 RVs, and a stellar activity model, we posit that we may be presenting the most complex mass recovery of an exoplanet system in the literature to date. By combining TTVs and RVs, we minimized Gaussian process overfitting and retrieved new masses for this system: (<jats:italic>m</jats:italic>\u0000 <jats:sub>\u0000 <jats:italic>b−g</jats:italic>\u0000 </jats:sub> =<jats:inline-formula>\u0000 <jats:tex-math>\u0000<?CDATA ${3.50}_{-0.7}^{+0.8}$?>\u0000</jats:tex-math>\u0000 <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" overflow=\"scroll\">\u0000 <mml:msubsup>\u0000 <mml:mrow>\u0000 <mml:mn>3.50</mml:mn>\u0000 </mml:mrow>\u0000 <mml:mrow>\u0000 <mml:mo>−</mml:mo>\u0000 <mml:mn>0.7</mml:mn>\u0000 </mml:mrow>\u0000 <mml:mrow>\u0000 <mml:mo>+</mml:mo>\u0000 <mml:mn>0.8</mml:mn>\u0000 </mml:mrow>\u0000 </mml:msubsup>\u0000 </mml:math>\u0000 <jats:inline-graphic xmlns:xlink=\"http://www.w3.org/1999/xlink\" xlink:href=\"ajad1330ieqn1.gif\" xlink:type=\"simple\" />\u0000 </jats:inline-formula>, <jats:inline-formula>\u0000 <jats:tex-math>\u0000<?CDATA ${6.32}_{-1.3}^{+1.1}$?>\u0000</jats:tex-math>\u0000 <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" overflow=\"scroll\">\u0000 <mml:msubsup>\u0000 <mml:mrow>\u0000 <mml:mn>6.32</mml:mn>\u0000 </mml:mrow>\u0000 <mml:mrow>\u0000 <mml:mo>−</mml:mo>\u0000 <mml:mn>1.3</mml:mn>\u0000 </mml:mrow>\u0000 <mml:mrow>\u0000 <mml:mo>+</mml:mo>\u0000 ","PeriodicalId":424210,"journal":{"name":"The Astronomical Journal","volume":"24 6","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-01-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140490116","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
Orbital and Absolute Magnitude Distribution of Jupiter Trojans 木星木马的轨道和绝对星等分布
The Astronomical Journal Pub Date : 2024-01-28 DOI: 10.3847/1538-3881/ad2200
D. Vokrouhlick'y, David Nesvorn'y, M. Brož, W. Bottke, R. Deienno, Carson Fuls, Frank C. Shelly
{"title":"Orbital and Absolute Magnitude Distribution of Jupiter Trojans","authors":"D. Vokrouhlick'y, David Nesvorn'y, M. Brož, W. Bottke, R. Deienno, Carson Fuls, Frank C. Shelly","doi":"10.3847/1538-3881/ad2200","DOIUrl":"https://doi.org/10.3847/1538-3881/ad2200","url":null,"abstract":"\u0000 Jupiter Trojans (JTs) librate about the Lagrangian stationary centers L4 and L5 associated with this planet on typically small-eccentricity and moderate-inclination heliocentric orbits. The physical and orbital properties of JTs provide important clues about the dynamical evolution of the giant planets in the early solar system, as well as populations of planetesimals in their source regions. Here we use decade-long observations from the Catalina Sky Survey (station G96) to determine the bias-corrected orbital and magnitude distributions of JTs. We distinguish the background JT population, filling smoothly the long-term stable orbital zone about L4 and L5 points and collisional families. We find that the cumulative magnitude distribution of JTs (the background population in our case) has a steep slope for H ≤ 9, followed by a moderately shallow slope until H ≃ 14.5, beyond which the distribution becomes even shallower. At H = 15 we find a local power-law exponent 0.38 ± 0.01. We confirm the asymmetry between the magnitude-limited background populations in L4 and L5 clouds characterized by a ratio 1.45 ± 0.05 for H < 15. Our analysis suggests an asymmetry in the inclination distribution of JTs, with the L4 population being tighter and the L5 population being broader. We also provide a new catalog of the synthetic proper elements for JTs with an updated identification of statistically robust families (9 at L4, and 4 at L5). The previously known Ennomos family is found to consist of two overlapping Deiphobus and Ennomos families.","PeriodicalId":424210,"journal":{"name":"The Astronomical Journal","volume":"343 5","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-01-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140490974","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 POKEMON Speckle Survey of Nearby M Dwarfs. III. The Stellar Multiplicity Rate of M Dwarfs within 15 pc POKEMON Speckle Survey of Nearby M Dwarfs.III.15 pc 范围内 M 矮星的恒星倍率
The Astronomical Journal Pub Date : 2024-01-26 DOI: 10.3847/1538-3881/ad267d
C. Clark, G. V. van Belle, E. Horch, D. Ciardi, K. von Braun, B. Skiff, J. Winters, M. Lund, M. Everett, Zachary D. Hartman, Joe Llama
{"title":"The POKEMON Speckle Survey of Nearby M Dwarfs. III. The Stellar Multiplicity Rate of M Dwarfs within 15 pc","authors":"C. Clark, G. V. van Belle, E. Horch, D. Ciardi, K. von Braun, B. Skiff, J. Winters, M. Lund, M. Everett, Zachary D. Hartman, Joe Llama","doi":"10.3847/1538-3881/ad267d","DOIUrl":"https://doi.org/10.3847/1538-3881/ad267d","url":null,"abstract":"\u0000 M dwarfs are ubiquitous in our Galaxy, and the rate at which they host stellar companions, and the properties of these companions, provide a window into the formation and evolution of the star(s), and of any planets that they may host. The Pervasive Overview of “Kompanions” of Every M dwarf in Our Neighborhood (POKEMON) speckle survey of nearby M dwarfs is volume limited from M0V through M9V out to 15 pc, with additional targets at larger distances. In total, 1125 stars were observed, and 455 of these are within the volume-limited, 15 pc sample of M-dwarf primaries. When we combine the speckle observations with known companions from the literature, we find that the stellar multiplicity rate of M dwarfs within 15 pc is 23.5% ± 2.0%, and that the companion rate is 28.8% ± 2.1%. We also find that the projected separation distribution for multiples that are known to host planets peaks at 198 au, while the distribution for multiples that are not yet known to host planets peaks at 5.57 au. This result suggests that the presence of close-in stellar companions inhibits the formation of M-dwarf planetary systems, similar to what has been found for FGK stars.","PeriodicalId":424210,"journal":{"name":"The Astronomical Journal","volume":"5 3-4","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-01-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140493631","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 Spatial Distribution of Type Ia Supernovae within Host Galaxies 宿主星系内 Ia 型超新星的空间分布
The Astronomical Journal Pub Date : 2024-01-24 DOI: 10.3847/1538-3881/ad234b
Christopher Pritchet, K. Thanjavur, Connor Bottrell, Yan Gao
{"title":"The Spatial Distribution of Type Ia Supernovae within Host Galaxies","authors":"Christopher Pritchet, K. Thanjavur, Connor Bottrell, Yan Gao","doi":"10.3847/1538-3881/ad234b","DOIUrl":"https://doi.org/10.3847/1538-3881/ad234b","url":null,"abstract":"\u0000 We study how type Ia supernovae (SNe Ia) are spatially distributed within their host galaxies, using data taken from the Sloan Digital Sky Survey (SDSS). This paper specifically tests the hypothesis that the SNe Ia rate traces the r-band light of the morphological component to which supernovae belong. A sample of supernovae is taken from the SDSS SN Survey, and host galaxies are identified. Each host galaxy is decomposed into a bulge and disk, and the distribution of supernovae is compared to the distribution of disk and bulge light. Our methodology is relatively unaffected by seeing. We find that, in galaxies dominated by disk light, SNe Ia trace light closely. The situation is less clear for bulges and ellipticals, because of resolution effects, but the available evidence is also consistent with the hypothesis that bulge/elliptical SNe Ia follow light.","PeriodicalId":424210,"journal":{"name":"The Astronomical Journal","volume":"78 2","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-01-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140498128","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
Large Interferometer For Exoplanets (LIFE). XII. The Detectability of Capstone Biosignatures in the Mid-infrared—Sniffing Exoplanetary Laughing Gas and Methylated Halogens 大型系外行星干涉仪(LIFE)。XII.中红外顶石生物特征的可探测性--探测系外行星笑气和甲基化卤素
The Astronomical Journal Pub Date : 2024-01-16 DOI: 10.3847/1538-3881/ad1f4b
D. Angerhausen, D. Pidhorodetska, Michaela Leung, Janina Hansen, E. Alei, F. Dannert, J. Kammerer, S. Quanz, E. Schwieterman
{"title":"Large Interferometer For Exoplanets (LIFE). XII. The Detectability of Capstone Biosignatures in the Mid-infrared—Sniffing Exoplanetary Laughing Gas and Methylated Halogens","authors":"D. Angerhausen, D. Pidhorodetska, Michaela Leung, Janina Hansen, E. Alei, F. Dannert, J. Kammerer, S. Quanz, E. Schwieterman","doi":"10.3847/1538-3881/ad1f4b","DOIUrl":"https://doi.org/10.3847/1538-3881/ad1f4b","url":null,"abstract":"\u0000 This study aims to identify exemplary science cases for observing N2O, CH3Cl, and CH3Br in exoplanet atmospheres at abundances consistent with biogenic production using a space-based mid-infrared nulling interferometric observatory, such as the Large Interferometer For Exoplanets (LIFE) mission concept. We use a set of scenarios derived from chemical kinetics models that simulate the atmospheric response of varied levels of biogenic production of N2O, CH3Cl, and CH3Br in O2-rich terrestrial planet atmospheres to produce forward models for our LIFEsim observation simulator software. In addition, we demonstrate the connection to retrievals for selected cases. We use the results to derive observation times needed for the detection of these scenarios and apply them to define science requirements for the mission. Our analysis shows that in order to detect relevant abundances with a mission like LIFE in its current baseline setup, we require: (i) only a few days of observation time for certain very nearby “golden target” scenarios, which also motivate future studies of “spectral-temporal” observations (ii) ∼10 days in certain standard scenarios such as temperate, terrestrial planets around M star hosts at 5 pc, (iii) ∼50–100 days in the most challenging but still feasible cases, such as an Earth twin at 5 pc. A few cases with very low fluxes around specific host stars are not detectable. In summary, the abundances of these capstone biosignatures are detectable at plausible biological production fluxes for most cases examined and for a significant number of potential targets.","PeriodicalId":424210,"journal":{"name":"The Astronomical Journal","volume":"32 7","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-01-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140505732","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
Circumstellar Disk Accretion Across the Lagoon Nebula: The Influence of Environment and Stellar Mass 礁湖星云的环状星盘吸积:环境和恒星质量的影响
The Astronomical Journal Pub Date : 2024-01-12 DOI: 10.3847/1538-3881/ad1f65
L. Venuti, A. Cody, G. Beccari, L. Rebull, M. J. Irwin, A. Thanvantri, S. Thanvantri, S. Alencar, C. O. Leal, G. Barentsen, J. E. Drew, S. B. Howell
{"title":"Circumstellar Disk Accretion Across the Lagoon Nebula: The Influence of Environment and Stellar Mass","authors":"L. Venuti, A. Cody, G. Beccari, L. Rebull, M. J. Irwin, A. Thanvantri, S. Thanvantri, S. Alencar, C. O. Leal, G. Barentsen, J. E. Drew, S. B. Howell","doi":"10.3847/1538-3881/ad1f65","DOIUrl":"https://doi.org/10.3847/1538-3881/ad1f65","url":null,"abstract":"\u0000 Pre-main-sequence disk accretion is pivotal for determining the final stellar properties and the early conditions for close-in planets. We aim to establish the impact of internal (stellar mass) and external (radiation field) parameters on the disk evolution in the Lagoon Nebula massive star-forming region. We employ simultaneous u, g, r, i, Hα time-series photometry, archival infrared data, and high-precision K2 light curves to derive the stellar, disk, and accretion properties for 1012 Lagoon Nebula members. We estimate that of all young stars in the Lagoon Nebula, 34%–37% have inner disks traceable down to ∼12 μm, while 38%–41% are actively accreting. We detect disks ∼1.5 times more frequently around G, K, and M stars than around higher-mass stars, which appear to deplete their inner disks on shorter timescales. We find tentative evidence for a faster disk evolution in the central regions of the Lagoon Nebula, where the bulk of the O/B population is located. Conversely, disks appear to last longer at the nebula outskirts, where the measured fraction of disk-bearing stars tends to exceed that of accreting and disk-free stars. The derived mass accretion rates show a nonuniform dependence on stellar mass between ∼0.2 and 5 M\u0000 ⊙. In addition, the typical accretion rates appear to differ across the Lagoon Nebula extension, with values twice lower in the core region than at its periphery. Finally, we detect tentative radial density gradients in the surface accretion shocks, leading to lags in the appearance of light curve brightness features as a function of wavelength that can amount to ∼7%–30% of the rotation period.","PeriodicalId":424210,"journal":{"name":"The Astronomical Journal","volume":"8 3","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-01-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140509341","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
JWST/NIRCam Transmission Spectroscopy of the Nearby Sub-Earth GJ 341b JWST/NIRCam 对近邻子地 GJ 341b 的透射光谱分析
The Astronomical Journal Pub Date : 2024-01-11 DOI: 10.3847/1538-3881/ad19df
James Kirk, Kevin B Stevenson, Guangwei Fu, J. Lustig-Yaeger, S. Moran, Sarah Peacock, M. Alam, N. Batalha, Katherine A. Bennett, Junellie Gonzalez-Quiles, Mercedes L'opez-Morales, J. Lothringer, R. MacDonald, E. M. May, L. C. Mayorga, Z. Rustamkulov, David K. Sing, K. Sotzen, J. Valenti, H. Wakeford
{"title":"JWST/NIRCam Transmission Spectroscopy of the Nearby Sub-Earth GJ 341b","authors":"James Kirk, Kevin B Stevenson, Guangwei Fu, J. Lustig-Yaeger, S. Moran, Sarah Peacock, M. Alam, N. Batalha, Katherine A. Bennett, Junellie Gonzalez-Quiles, Mercedes L'opez-Morales, J. Lothringer, R. MacDonald, E. M. May, L. C. Mayorga, Z. Rustamkulov, David K. Sing, K. Sotzen, J. Valenti, H. Wakeford","doi":"10.3847/1538-3881/ad19df","DOIUrl":"https://doi.org/10.3847/1538-3881/ad19df","url":null,"abstract":"\u0000 We present a JWST/Near Infrared Camera (NIRCam) transmission spectrum from 3.9 to 5.0 μm of the recently validated sub-Earth GJ 341b (R\u0000 P = 0.92 R\u0000 ⊕, T\u0000 eq = 540 K) orbiting a nearby bright M1 star (d = 10.4 pc, K\u0000 mag = 5.6). We use three independent pipelines to reduce the data from the three JWST visits and perform several tests to check for the significance of an atmosphere. Overall, our analysis does not uncover evidence of an atmosphere. Our null hypothesis tests find that none of our pipelines’ transmission spectra can rule out a flat line, although there is weak evidence for a Gaussian feature in two spectra from different pipelines (at 2.3 and 2.9σ). However, the candidate features are seen at different wavelengths (4.3 μm versus 4.7 μm), and our retrieval analysis finds that different gas species can explain these features in the two reductions (CO2 at 3.1σ compared to O3 at 2.9σ), suggesting that they are not real astrophysical signals. Our forward-model analysis rules out a low-mean-molecular-weight atmosphere (<350× solar metallicity) to at least 3σ, and disfavors CH4-dominated atmospheres at 1–3σ, depending on the reduction. Instead, the forward models find our transmission spectra are consistent with no atmosphere, a hazy atmosphere, or an atmosphere containing a species that does not have prominent molecular bands across the NIRCam/F444W bandpass, such as a water-dominated atmosphere. Our results demonstrate the unequivocal need for two or more transit observations analyzed with multiple reduction pipelines, alongside rigorous statistical tests, to determine the robustness of molecular detections for small exoplanet atmospheres.","PeriodicalId":424210,"journal":{"name":"The Astronomical Journal","volume":"53 6","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-01-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140510346","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
An Automatic Approach for Grouping Sunspots and Calculating Relative Sunspot Number on SDO/HMI Continuum Images 在 SDO/HMI 连续图像上对太阳黑子进行分组并计算相对太阳黑子数量的自动方法
The Astronomical Journal Pub Date : 2024-01-10 DOI: 10.3847/1538-3881/ad11e2
Cui Zhao, Shangbin Yang, Tingmei Wang, Haiyan Zhao, Shiyuan Liu, Fangyuan He, Zhengkun Hu
{"title":"An Automatic Approach for Grouping Sunspots and Calculating Relative Sunspot Number on SDO/HMI Continuum Images","authors":"Cui Zhao, Shangbin Yang, Tingmei Wang, Haiyan Zhao, Shiyuan Liu, Fangyuan He, Zhengkun Hu","doi":"10.3847/1538-3881/ad11e2","DOIUrl":"https://doi.org/10.3847/1538-3881/ad11e2","url":null,"abstract":"The relative sunspot number is one of the major parameters for the study of long-term solar activity. The automatic calculation of the relative sunspot number is more stable and accurate as compared to manual methods. In this paper, we propose an algorithm that can detect sunspots, and divide them into groups to automatically calculate the relative sunspot number. Mathematical morphology was adopted to detect sunspots then group them. The data set used were the continuum images from SDO/HMI. The process was carried out on the overall HMI data available on the timespan from 2022 January to 2023 May with a time cadence of one day. The experimental results indicated that the method achieved high accuracy of 85.3%. It was well fitted with the international relative sunspot number provided by Solar Influences Data Analysis Center (CC = 0.91). We calculated the conversion factor K value of SDO/HMI for calculating the relative sunspots number (K = 1.03).","PeriodicalId":424210,"journal":{"name":"The Astronomical Journal","volume":"38 6","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-01-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139441330","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
TESS Hunt for Young and Maturing Exoplanets (THYME). XI. An Earth-sized Planet Orbiting a Nearby, Solar-like Host in the 400 Myr Ursa Major Moving Group TESS Hunt for Young and Maturing Exoplanets (THYME).XI.400 Myr 大熊座移动星团中一颗环绕近邻类太阳宿主的地球大小的行星
The Astronomical Journal Pub Date : 2024-01-10 DOI: 10.3847/1538-3881/ad1039
Benjamin K. Capistrant, M. Soares-Furtado, A. Vanderburg, Alyssa Jankowski, A. Mann, Gabrielle Ross, G. Srdoč, N. Hinkel, J. Becker, C. Magliano, M. Limbach, A. Stephan, Andrew C. Nine, B. Tofflemire, A. Kraus, S. Giacalone, J. Winn, A. Bieryla, L. Bouma, D. Ciardi, Karen A. Collins, Giovanni Covone, Zoe L. de Beurs, Chelsea X. Huang, J. Jenkins, L. Kreidberg, D. Latham, S. Quinn, S. Seager, A. Shporer, J. Twicken, B. Wohler, R. Vanderspek, R. Yarza, C. Ziegler
{"title":"TESS Hunt for Young and Maturing Exoplanets (THYME). XI. An Earth-sized Planet Orbiting a Nearby, Solar-like Host in the 400 Myr Ursa Major Moving Group","authors":"Benjamin K. Capistrant, M. Soares-Furtado, A. Vanderburg, Alyssa Jankowski, A. Mann, Gabrielle Ross, G. Srdoč, N. Hinkel, J. Becker, C. Magliano, M. Limbach, A. Stephan, Andrew C. Nine, B. Tofflemire, A. Kraus, S. Giacalone, J. Winn, A. Bieryla, L. Bouma, D. Ciardi, Karen A. Collins, Giovanni Covone, Zoe L. de Beurs, Chelsea X. Huang, J. Jenkins, L. Kreidberg, D. Latham, S. Quinn, S. Seager, A. Shporer, J. Twicken, B. Wohler, R. Vanderspek, R. Yarza, C. Ziegler","doi":"10.3847/1538-3881/ad1039","DOIUrl":"https://doi.org/10.3847/1538-3881/ad1039","url":null,"abstract":"Young terrestrial worlds are critical test beds to constrain prevailing theories of planetary formation and evolution. We present the discovery of HD 63433 d—a nearby (22 pc), Earth-sized planet transiting a young Sun-like star (TOI-1726, HD 63433). HD 63433 d is the third planet detected in this multiplanet system. The kinematic, rotational, and abundance properties of the host star indicate that it belongs to the young (414 ± 23 Myr) Ursa Major moving group, whose membership we update using new data from the third data release of the Gaia mission and TESS. Our transit analysis of the TESS light curves indicates that HD 63433 d has a radius of 1.1 R ⊕ and closely orbits its host star with a period of 4.2 days. To date, HD 63433 d is the smallest confirmed exoplanet with an age less than 500 Myr, and the nearest young Earth-sized planet. Furthermore, the apparent brightness of the stellar host (V ≃ 6.9 mag) makes this transiting multiplanet system favorable to further investigations, including spectroscopic follow-up to probe the atmospheric loss in a young Earth-sized world.","PeriodicalId":424210,"journal":{"name":"The Astronomical Journal","volume":"76 2","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-01-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139440832","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 APO-K2 Catalog. I. ∼7500 Red Giants with Fundamental Stellar Parameters from APOGEE DR17 Spectroscopy and K2-GAP Asteroseismology APO-K2 目录。I. 从 APOGEE DR17 光谱和 K2-GAP 星震学中获得的带有基本恒星参数的 ∼7500 红巨星
The Astronomical Journal Pub Date : 2024-01-09 DOI: 10.3847/1538-3881/ad0b13
J. Schonhut-Stasik, J. C. Zinn, K. Stassun, M. Pinsonneault, Jennifer A. Johnson, J. Warfield, D. Stello, Y. Elsworth, Rafael A. García, S. Mathur, B. Mosser, M. Hon, J. Tayar, G. Stringfellow, R. Beaton, H. Jönsson, Dante Minniti
{"title":"The APO-K2 Catalog. I. ∼7500 Red Giants with Fundamental Stellar Parameters from APOGEE DR17 Spectroscopy and K2-GAP Asteroseismology","authors":"J. Schonhut-Stasik, J. C. Zinn, K. Stassun, M. Pinsonneault, Jennifer A. Johnson, J. Warfield, D. Stello, Y. Elsworth, Rafael A. García, S. Mathur, B. Mosser, M. Hon, J. Tayar, G. Stringfellow, R. Beaton, H. Jönsson, Dante Minniti","doi":"10.3847/1538-3881/ad0b13","DOIUrl":"https://doi.org/10.3847/1538-3881/ad0b13","url":null,"abstract":"We present a catalog of fundamental stellar properties for ∼7500 evolved stars, including stellar radii and masses, determined from the combination of spectroscopic observations from the Apache Point Observatory Galactic Evolution Experiment, part of the Sloan Digital Sky Survey IV, and asteroseismology from K2. The resulting APO-K2 catalog provides spectroscopically derived temperatures and metallicities, asteroseismic global parameters, evolutionary states, and asteroseismically derived masses and radii. Additionally, we include kinematic information from Gaia. We investigate the multidimensional space of abundance, stellar mass, and velocity with an eye toward applications in Galactic archaeology. The APO-K2 sample has a large population of low-metallicity stars (∼288 with [M/H] ≤ −1), and their asteroseismic masses are larger than astrophysical estimates. We argue that this may reflect offsets in the adopted fundamental temperature scale for metal-poor stars rather than metallicity-dependent issues with interpreting asteroseismic data. We characterize the kinematic properties of the population as a function of α enhancement and position in the disk and identify those stars in the sample that are candidate components of the Gaia-Enceladus merger. Importantly, we characterize the selection function for the APO-K2 sample as a function of metallicity, radius, mass, νmax , color, and magnitude referencing Galactic simulations and target selection criteria to enable robust statistical inferences with the catalog.","PeriodicalId":424210,"journal":{"name":"The Astronomical Journal","volume":"58 10","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-01-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139441871","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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