The Astronomical Journal最新文献

Grand Design versus Multiarmed Spiral Galaxies: Dependence on Galaxy Structure 大设计与多臂螺旋星系：取决于星系结构

The Astronomical Journal Pub Date : 2024-06-11 DOI: 10.3847/1538-3881/ad46fb

Beverly J. Smith, Matthew Watson, M. Giroux, C. Struck

{"title":"Grand Design versus Multiarmed Spiral Galaxies: Dependence on Galaxy Structure","authors":"Beverly J. Smith, Matthew Watson, M. Giroux, C. Struck","doi":"10.3847/1538-3881/ad46fb","DOIUrl":"https://doi.org/10.3847/1538-3881/ad46fb","url":null,"abstract":"We developed an algorithm to use Galaxy Zoo 3D spiral arm masks produced by citizen scientist volunteers to semiautomatically classify spiral galaxies as either multiarmed or grand design spirals. Our final sample consists of 299 multiarmed and 245 grand design galaxies. On average, the grand design galaxies have smaller stellar masses than the multiarmed galaxies. For a given stellar mass, the grand design galaxies have larger concentrations, earlier Hubble types, smaller half-light radii, and larger central surface mass densities than the multiarmed galaxies. Lower-mass galaxies of both arm classes have later Hubble types and lower concentrations than higher-mass galaxies. In our sample, a higher fraction of grand design galaxies have classical bulges rather than pseudo-bulges, compared to multiarmed galaxies. These results are consistent with theoretical models and simulations, which suggest that dense classical bulges support the development and/or longevity of two-armed spiral patterns. Similar specific star formation rates (sSFRs) are found in multiarmed and grand design galaxies with similar stellar masses and concentrations. This implies that the sSFRs in spiral galaxies are a function of concentration and stellar mass, but independent of the number of spiral arms. Our classifications are consistent with arm counts from the Galaxy Zoo 2 project and published m = 3 Fourier amplitudes.","PeriodicalId":424210,"journal":{"name":"The Astronomical Journal","volume":"37 5","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-06-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141358873","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

Masers and Star Formation Activities in W51A W51A 中的掩星器和恒星形成活动

The Astronomical Journal Pub Date : 2024-06-10 DOI: 10.3847/1538-3881/ad428d

Yan-Kun Zhang, Xi Chen, You-Xin Wang, Shijie Song, Jun-Ting Liu, Ying Lu

{"title":"Masers and Star Formation Activities in W51A","authors":"Yan-Kun Zhang, Xi Chen, You-Xin Wang, Shijie Song, Jun-Ting Liu, Ying Lu","doi":"10.3847/1538-3881/ad428d","DOIUrl":"https://doi.org/10.3847/1538-3881/ad428d","url":null,"abstract":"Concurrently with the maser flare observed in W51-North during the 3 month monitoring of H2O, NH3, and CH3OH maser variability from 2020 January to April using the Tianma 65 m Radio Telescope, we conducted Very Large Array mappings for these three maser species across the entirety of W51A region. After finding the ring-shaped H2O maser which might trace the disk surrounding the protostar residing in W51-North, the NH3 (9,6) maser delineated a jet which might be illuminated in the luminosity outburst possibly caused by the infalling streamer’s interaction with the protostar’s disk. An analysis of the comprehensive distribution of maser spots allowed us to affirm that W51N4 or ALMAmm31 serves as the primary source of the Lacy jet. Furthermore, we observed that class I methanol maser spots may extend beyond the locations of the H2O and NH3 (9,6) masers within the outflow. Additionally, emissions from other NH3 maser transitions coincided with specific 1.3 mm continuum sources. The arrangement of H2O maser spots in the vicinity of W51e2-E potentially indicates episodic accretions in this source. Combining the data from the Atacama Large Millimeter/submillimeter Array data archive for W51-North, W51e2, and W51e8, we have discovered that the H2O, NH3, and CH3OH masers, as well as the HC3N and SiO emissions are found to be good tools for tracing outflow in this work for W51A.","PeriodicalId":424210,"journal":{"name":"The Astronomical Journal","volume":" 78","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-06-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141365369","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

Host-star Properties of Hot, Warm, and Cold Jupiters in the Solar Neighborhood from Gaia Data Release 3: Clues to Formation Pathways 盖亚数据第3版显示的太阳近邻热木星、暖木星和冷木星的主星特性：形成途径的线索

The Astronomical Journal Pub Date : 2024-06-05 DOI: 10.3847/1538-3881/ad429f

Bihan Banerjee, M. Narang, P. Manoj, Thomas Henning, H. Tyagi, Arun Surya, P. K. Nayak, Mihir Tripathi

{"title":"Host-star Properties of Hot, Warm, and Cold Jupiters in the Solar Neighborhood from Gaia Data Release 3: Clues to Formation Pathways","authors":"Bihan Banerjee, M. Narang, P. Manoj, Thomas Henning, H. Tyagi, Arun Surya, P. K. Nayak, Mihir Tripathi","doi":"10.3847/1538-3881/ad429f","DOIUrl":"https://doi.org/10.3847/1538-3881/ad429f","url":null,"abstract":"Giant planets exhibit diverse orbital properties, hinting at their distinct formation and dynamic histories. In this paper, using Gaia Data Release 3 (DR3), we investigate if and how the orbital properties of Jupiters are linked to their host star properties, particularly their metallicity and age. We obtain metallicities for main-sequence stars of spectral type F, G, and K, hosting hot, warm, and cold Jupiters with varying eccentricities. We compute the velocity dispersions of the host stars of these three groups using kinematic information from Gaia DR3 and obtain average ages using a velocity dispersion–age relation. We find that the host stars of hot Jupiters are relatively metal rich ([Fe/H] = 0.18 ± 0.13) and young (median age of 3.97 ± 0.51 Gyr) compared to the host stars of cold Jupiters in nearly circular orbits, which are relatively metal poor (0.03 ± 0.18) and older (median age of 6.07 ± 0.79 Gyr). The host stars of cold Jupiters in high-eccentricity orbits, on the other hand, show metallicities similar to those of the hosts of hot Jupiters, but are older, on average (median age of 6.25 ± 0.92 Gyr). The similarity in metallicity between the hosts of hot Jupiters and the hosts of cold Jupiters in high-eccentricity orbits supports high-eccentricity migration as the potential origin of hot Jupiters, with the latter serving as the progenitors of hot Jupiters. However, the average age difference between them suggests that the older hot Jupiters may have been engulfed by their host star over timescales ∼ 6 Gyr. This allows us to estimate the value of stellar tidal quality factor, Q*′∼106±1 .","PeriodicalId":424210,"journal":{"name":"The Astronomical Journal","volume":"67 8","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-06-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141382742","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 Giants Transiting Giants. IV. A Low-density Hot Neptune Orbiting a Red Giant Star TESS 巨人 Transiting Giants.IV.一颗绕红巨星运行的低密度热海王星

The Astronomical Journal Pub Date : 2024-06-05 DOI: 10.3847/1538-3881/ad4149

S. Grunblatt, Nicholas Saunders, Dan Huber, D. Thorngren, S. Vissapragada, Stephanie Yoshida, K. Schlaufman, S. Giacalone, M. Macdougall, A. Chontos, E. Turtelboom, C. Beard, J. M. A. Murphy, M. Rice, H. Isaacson, R. Angus, Andrew W. Howard

{"title":"TESS Giants Transiting Giants. IV. A Low-density Hot Neptune Orbiting a Red Giant Star","authors":"S. Grunblatt, Nicholas Saunders, Dan Huber, D. Thorngren, S. Vissapragada, Stephanie Yoshida, K. Schlaufman, S. Giacalone, M. Macdougall, A. Chontos, E. Turtelboom, C. Beard, J. M. A. Murphy, M. Rice, H. Isaacson, R. Angus, Andrew W. Howard","doi":"10.3847/1538-3881/ad4149","DOIUrl":"https://doi.org/10.3847/1538-3881/ad4149","url":null,"abstract":"Hot Neptunes, gaseous planets smaller than Saturn (∼3–8 R ⊕) with orbital periods less than 10 days, are rare. Models predict this is due to high-energy stellar irradiation stripping planetary atmospheres over time, often leaving behind only rocky planetary cores. Using our TESS full-frame-image pipeline giants in conjunction with Keck/HIRES radial velocity measurements, we present the discovery of TIC365102760 b, a 6.2 R ⊕(0.55 R J), 19.2 M ⊕(0.060 M J) planet transiting a red giant star every 4.21285 days. The old age and high equilibrium temperature yet remarkably low density of this planet ( ρp=0.58−0.20+0.30ρJ ) suggest that its gaseous envelope should have been stripped by high-energy stellar irradiation billions of years ago. The present-day planet mass and radius suggest the atmospheric stripping was slower than predicted. Unexpectedly low stellar activity and/or late-stage planet inflation could be responsible for the observed properties of this system. Further studies of this system with more precise photometry in multiple passbands will be capable of revealing more details of this planet’s atmosphere.","PeriodicalId":424210,"journal":{"name":"The Astronomical Journal","volume":"295 8","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-06-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141386184","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

UV Cooling via O VI Emission in the Superwind of M82 Observed with the Far Ultraviolet Spectroscopic Explorer (FUSE) 远紫外线光谱探测器（FUSE）观测到的 M82 超风中通过 O VI 发射的紫外线冷却现象

The Astronomical Journal Pub Date : 2024-06-03 DOI: 10.3847/1538-3881/ad4887

Jin-A Kim, Haeun Chung, Carlos J. Vargas, E. Hamden

引用次数: 0

Simultaneous Photometric and Spectroscopic Analysis of V505 Lacertae, a Photospherically and Chromospherically Active Contact Binary Star 光球和色球活动接触双星 V505 Lacertae 的同步光度和光谱分析

The Astronomical Journal Pub Date : 2024-05-23 DOI: 10.3847/1538-3881/ad4293

M. Jeong, Chun-Hwey Kim, K. Hong, Hye-Young Kim, Mi-Hwa Song, Jang-Ho Park, Cheongho Han

{"title":"Simultaneous Photometric and Spectroscopic Analysis of V505 Lacertae, a Photospherically and Chromospherically Active Contact Binary Star","authors":"M. Jeong, Chun-Hwey Kim, K. Hong, Hye-Young Kim, Mi-Hwa Song, Jang-Ho Park, Cheongho Han","doi":"10.3847/1538-3881/ad4293","DOIUrl":"https://doi.org/10.3847/1538-3881/ad4293","url":null,"abstract":"\u0000 New BVR photometric and high-resolution spectroscopic observations of V505 Lac are presented with Transiting Exoplanet Survey Satellite (TESS) photometric data. The orbital period has experienced a secular decrease during the past 16 yr. A clear anticorrelation in the primary and secondary eclipse timing variation (PSETV) obtained from the TESS data is also identified. A double-lined radial velocity (RV) curve is secured, and the effective temperatures of the less- and more-massive stars (Stars 1 and 2, respectively) are measured. Using a spectral subtraction technique, excess emissions are detected in the time-series Ca ii H and K and Hα lines for Star 2. Simultaneous analysis of the light and RV curves using the Wilson–Devinney (WD) code reveals that V505 Lac is a photospherically and chromospherically active W-subtype contact binary system. The component-star masses and radii are determined to an accuracy of approximately 1%. The WD spot model is individually applied to 221 light curves segmented from the TESS data so as to derive the spot parameters of a cool spot on Star 2. The combined variations in both longitude and colatitude among the spot parameters appear to be strongly associated with those of both the anticorrelation in the PSETV and the O’Connell effect in the TESS light curves. Robust negative linear relationships between the PSETV anticorrelation size and the O’Connell effect magnitude are found for the first time. Mass–radius, mass–luminosity, and mass ratio–mass diagrams of contact binaries, along with the mass ratio frequency distribution, are presented in an attempt to elucidate the evolutionary characteristics of these systems.","PeriodicalId":424210,"journal":{"name":"The Astronomical Journal","volume":"17 22","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-05-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141104673","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 TESS-Keck Survey. VII. A Superdense Sub-Neptune Orbiting TOI-1824* TESS-Keck 勘测。VII.一颗环绕 TOI-1824* 的超密集亚海王星

The Astronomical Journal Pub Date : 2024-05-23 DOI: 10.3847/1538-3881/ad34d9

Sarah Lange, Joseph M. Akana Murphy, N. Batalha, I. Crossfield, C. Dressing, B. Fulton, A. Howard, Dan Huber, H. Isaacson, S. R. Kane, E. Petigura, P. Robertson, L. Weiss, A. Behmard, C. Beard, S. Blunt, C. Brinkman, A. Chontos, Fei Dai, P. Dalba, T. Fetherolf, S. Giacalone, M. Hill, R. Holcomb, J. Lubin, M. MacDougall, A. Mayo, T. Močnik, D. Pidhorodetska, A. Polanski, M. Rice, L. Rosenthal, R. Rubenzahl, N. Scarsdale, E. Turtelboom, Judah Van Zandt, D. Ciardi, A. Boyle

{"title":"The TESS-Keck Survey. VII. A Superdense Sub-Neptune Orbiting TOI-1824*","authors":"Sarah Lange, Joseph M. Akana Murphy, N. Batalha, I. Crossfield, C. Dressing, B. Fulton, A. Howard, Dan Huber, H. Isaacson, S. R. Kane, E. Petigura, P. Robertson, L. Weiss, A. Behmard, C. Beard, S. Blunt, C. Brinkman, A. Chontos, Fei Dai, P. Dalba, T. Fetherolf, S. Giacalone, M. Hill, R. Holcomb, J. Lubin, M. MacDougall, A. Mayo, T. Močnik, D. Pidhorodetska, A. Polanski, M. Rice, L. Rosenthal, R. Rubenzahl, N. Scarsdale, E. Turtelboom, Judah Van Zandt, D. Ciardi, A. Boyle","doi":"10.3847/1538-3881/ad34d9","DOIUrl":"https://doi.org/10.3847/1538-3881/ad34d9","url":null,"abstract":"\u0000 We confirm a massive sub-Neptune-sized planet on a P = 22.8 days orbit around the star TOI-1824 (T\u0000 eff = 5200 K, V = 9.7 mag). TESS first identified TOI-1824 b (formerly TOI-1824.01) as an object of interest in 2020 April after two transits in Sector 22 were matched with a single transit in Sector 21. TOI-1824 was subsequently targeted for ground-based Doppler monitoring with Keck-HIRES and APF-Levy. Using a joint model of the TESS photometry, radial velocities, and Ca ii H and K emission measurements as an activity indicator, we find that TOI-1824 b is an unusually dense sub-Neptune. The planet has a radius R\u0000 p = 2.63 ± 0.15 R\u0000 ⊕ and mass M\u0000 p = 18.5 ± 3.2 M\u0000 ⊕, implying a bulk density of 5.6 ± 1.4 g cm−3. TOI-1824 b's mass and radius situate it near a small group of “superdense sub-Neptunes” (R\u0000 p ≲ 3 R\u0000 ⊕ and M\u0000 p ≳ 20 M\u0000 ⊕). While the formation mechanism of superdense sub-Neptunes is a mystery, one possible explanation is the constructive collision of primordial icy cores; such giant impacts would drive atmospheric escape and could help explain these planets' apparent lack of massive envelopes. We discuss TOI-1824 b in the context of these overdense planets, whose unique location in the exoplanet mass–radius plane make them a potentially valuable tracer of planet formation.","PeriodicalId":424210,"journal":{"name":"The Astronomical Journal","volume":"109 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-05-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141105786","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

Motion Planning for the Robotic Fiber Positioners of the Large Sky Area Multiobject Fiber Spectrocopy Telescope 大天区多目标光纤光谱望远镜机器人光纤定位器的运动规划

The Astronomical Journal Pub Date : 2024-05-22 DOI: 10.3847/1538-3881/ad4353

Feifan Zhang, Baolong Chen, Yu Wang, Zhenwan Peng, Zengxiang Zhou, Jianping Wang

{"title":"Motion Planning for the Robotic Fiber Positioners of the Large Sky Area Multiobject Fiber Spectrocopy Telescope","authors":"Feifan Zhang, Baolong Chen, Yu Wang, Zhenwan Peng, Zengxiang Zhou, Jianping Wang","doi":"10.3847/1538-3881/ad4353","DOIUrl":"https://doi.org/10.3847/1538-3881/ad4353","url":null,"abstract":"\u0000 The Large Sky Area Multi-Object Fiber Spectroscopy Telescope (LAMOST) is one of the most effective multiobject spectroscopic instruments. Its survey efficiency is guaranteed by simultaneously positioning multiple fibers via 4000 robotic fiber positioners (RFPs). With the further updates to LAMOST, the new-generation RFPs will be smaller, and the number of RFPs will increase to 5000. The RFPs are densely packed with shared working space. Thus, they may collide with each other, leading to them damaged and reducing the survey speed. In this study, we propose a new motion planning algorithm that prevents the collision of RFPs. To simplify the collision avoidance problem, we transform the motion planning process from a dynamic one into a static one by selecting one of the RFPs in each collision pair as the waiting robot. Accordingly, we design a method for choosing the waiting robot, and use a rapidly exploring random tree to plan a collision-free path for the waiting robot. However, there may be blocks between the waiting robots and their neighbors. Therefore, we also design methods to resolve these blocks. Simulations suggest that the proposed algorithm can prevent 98.4% of the collisions. About 99.9% of the positioners can reach their targets without collisions. Although developed for LAMOST, we believe that our algorithm can also be used for other instruments with equal-arm theta-phi positioners, such as the Dark Energy Spectroscopic Instrument.","PeriodicalId":424210,"journal":{"name":"The Astronomical Journal","volume":"17 7","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-05-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141112475","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 MeerKAT Polarization Survey of Southern Calibration Sources MeerKAT 对南方校准源的偏振勘测

The Astronomical Journal Pub Date : 2024-05-07 DOI: 10.3847/1538-3881/ad4150

A. R. Taylor, L. S. Legodi

{"title":"A MeerKAT Polarization Survey of Southern Calibration Sources","authors":"A. R. Taylor, L. S. Legodi","doi":"10.3847/1538-3881/ad4150","DOIUrl":"https://doi.org/10.3847/1538-3881/ad4150","url":null,"abstract":"\u0000 We report on full-Stokes L-band observations of 98 MeerKAT calibration sources. Linear polarization is detected in 71 objects above a fractional level of 0.2%. We identify ten sources with strong fractional linear polarization and low Faraday rotation measure that could be suitable for wide-band absolute polarization calibration. We detect significant circular polarization from 24% of the sample down to a detection level of 0.07%. Circularly polarized emission is seen only for flat spectrum sources α > −0.5. We compare our polarized intensities and Faraday synthesis results to data from the NVSS at 1400 MHz and the ATCA SPASS survey at 2300 MHz. NVSS data exist for 54 of our sources and SPASS data for 20 sources. The percent polarization and rotation measures from both surveys agree well with our results. The residual instrumental linear polarization for these observations is measured at 0.16%, and the residual instrumental circular polarization is measured at 0.05%. These levels may reflect either instabilities in the relative bandpass between the two polarization channels with either time or antenna orientation, or atmospheric/ionospheric variations with pointing direction. Tracking of the hourly gain solutions on J0408-6545 after transfer of the primary gain solutions suggests a deterioration of the gain stability by a factor of several starting about 2 hr after sunrise. This suggests that observing during the nighttime could dramatically improve the precision of polarization calibration.","PeriodicalId":424210,"journal":{"name":"The Astronomical Journal","volume":" 33","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-05-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141129339","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

Surviving Tidal Tails Around the Milky Way Bulge Globular Cluster NGC 6355 银河系凸起球状星团 NGC 6355 周围幸存的潮汐尾迹

The Astronomical Journal Pub Date : 2024-05-02 DOI: 10.3847/1538-3881/ad4704

A. Piatti

{"title":"Surviving Tidal Tails Around the Milky Way Bulge Globular Cluster NGC 6355","authors":"A. Piatti","doi":"10.3847/1538-3881/ad4704","DOIUrl":"https://doi.org/10.3847/1538-3881/ad4704","url":null,"abstract":"\u0000 We present results of the analysis of a set of images obtained in the field of the Milky Way bulge globular cluster NGC 6355 using the Dark Energy Camera, which is attached to the 4 m Blanco telescope of the Cerro-Tololo Interamerican Observatory. We dealt with a heavy differential absorption across the observed field, a crowded field star population, and the superposition of field stars on to the cluster color–magnitude diagram main features to produce an intrinsic cluster stars density map. The resulting stellar density map reveals the presence of an extended envelope, a tidal tail, and scattered debris; the tidal tails pointing toward the Milky Way center. Such extra-tidal overdensities, detected above the mean star field density, resulted to be between four and six times larger that the local star field density fluctuation. They have also been recently generated by two independent studies which performed numerical simulations of synthetic tidal tails of Milky Way globular clusters. These results contrast with previous theoretical speculations about the possibility to detect tidal tails of globular clusters with chaotic orbits because they would be washed out after they were generated.","PeriodicalId":424210,"journal":{"name":"The Astronomical Journal","volume":" 4","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-05-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141129877","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