Stellar Population Astrophysics (SPA) with TNG Atmospheric parameters of members of 16 unstudied open clusters
R. Zhang, S. Lucatello, A. Bragaglia, R. Carrera, L. Spina, J. Alonso-Santiago, G. Andreuzzi, G. Casali, E. Carretta, A. Frasca4, X. Fu, L. Magrini, L. Origlia,… 展开作者
R. Zhang, S. Lucatello, A. Bragaglia, R. Carrera, L. Spina, J. Alonso-Santiago, G. Andreuzzi, G. Casali, E. Carretta, A. Frasca4, X. Fu, L. Magrini, L. Origlia, V. DOrazi, A. Vallenari
Thanks to modern understanding of stellar evolution, we can accurately measure the age of Open Clusters (OCs). Given their position, they are ideal tracers of the Galactic disc. Gaia data release 2, besides providing precise parallaxes, led to the detection of many new clusters, opening a new era for the study of the Galactic disc. However, detailed information on the chemical abundance for OCs is necessary to accurately date them and to efficiently use them to probe the evolution of the disc.Mapping and exploring the Milky Way structure %to combine accurate chemical information of OCs is the main aim of the Stellar Population Astrophysics (SPA) project. Part of this work involves the use of OCs and the derivation of their precise and accurate chemical composition.We analyze here a sample of OCs located within about 2 kpc from the Sun, with ages from about 50 Myr to a few Gyr.We used HARPS-N at the Telescopio Nazionale Gaileo and collected very high-resolution spectra (R = 115\,000) of 40 red giant/red clump stars in 18 OCs (16 never or scarcely studied plus two comparison clusters). We measured their radial velocities and derived the stellar parameters.We discussed the relationship between metallicity and Galactocentric distance, adding literature data to our results to enlarge the sample and taking also age into account. We compared the result of observational data with that from chemo-dynamical models. These models generally reproduce the metallicity gradient well. However, at young ages we found a large dispersion in metallicity, not reproduced by models. Several possible explanations are explored, including uncertainties in the derived metallicity. We confirm the difficulties in determining parameters for young stars (age < 200 Myr), due to a combination of intrinsic factors which atmospheric models can not easily reproduce and which affect the parameters uncertainty
Star clusters are key to understand the stellar and Galactic evolution. ASCC 123 is a little-studied, nearby and very sparse open cluster. We performed the first high-resolution spectroscopic study of this cluster in the framework of the SPA (Stellar Population Astrophysics) project with GIARPS at the TNG. We observed 17 stars, five of which turned out to be double-lined binaries. Three of the investigated sources were rejected as members on the basis of astrometry and lithium content. For the remaining single stars we derived the stellar parameters, extinction, radial and projected rotational…
Context. The Perseus complex in the outer disk of the Galaxy hosts a number of clusters and associations of young stars. Gaia is providing a detailed characterization of their kinematic structure and evolutionary properties. Aims. Within the SPA Large Programme at the TNG, we secured HARPS-N and GIANO-B high-resolution optical and near-infrared (NIR) spectra of the young red supergiant (RSG) stars in the Perseus complex, in order to obtain accurate radial velocities, stellar parameters and detailed chemical abundances. Methods. We used spectral synthesis to best-fit hundreds of atomic and mole…
Context. High-resolution spectroscopy in the near-infrared (NIR) is a powerful tool for characterising the physical and chemical properties of cool-star atmospheres. The current generation of NIR echelle spectrographs enables the sampling of many spectral features over the full 0.9-2.4 μm range for a detailed chemical tagging. Aims. Within the Stellar Population Astrophysics Large Program at the TNG, we used a high-resolution (R=50000) NIR spectrum of Arcturus acquired with the GIANO-B echelle spectrograph as a laboratory to define and calibrate an optimal line list and new diagnostic tools to…
The Scutum complex in the inner disk of the Galaxy hosts a number of young clusters and associations of red supergiant stars that are heavily obscured by dust extinction. These stars are important tracers of the recent star formation and chemical enrichment history in the inner Galaxy. Within the SPA Large Programme at the TNG, we secured GIANO-B high-resolution (R=50,000) YJHK spectra of 11 red supergiants toward the Alicante 7 and Alicante 10 associations near the RSGC3 cluster. Taking advantage of the full YJHK spectral coverage of GIANO in a single exposure, we were able to measure several…
In the framework of the Stellar Population Astrophysics (SPA) project, we present new observations and spectral analysis of four sparsely studied open clusters, namely Collinder 350, Gulliver 51, NGC 7044, and Ruprecht 171. We exploit the HARPS-N spectrograph at the TNG telescope to acquire high-resolution optical spectra for 15 member stars of four clusters. We derive stellar parameters using both the EW analysis and the spectral fitting technique. We compute elemental abundances for light, a-, iron-peak, and n-capture elements using the EW measurement approach. We investigate the origin of t…
Open clusters exquisitely track the Galactic disc chemical properties and its time evolution; a substantial number of studies and large spectroscopic surveys focus mostly on the chemical content of relatively old clusters (age $\gtrsim$ 1 Gyr). Interestingly, the less studied young counterpart populating the solar surrounding has been found to be solar (at most), with a notable surprising lack of young metal-rich objects. While there is wide consensus about the moderately above-solar composition of the Hyades cluster, the metallicity of Praesepe is still controversial. Recent studies suggest t…
The CAMELS project: Expanding the galaxy formation model space with new ASTRID and 28-parameter TNG and SIMBA suites
Harvard-Smithsonian Center for Astrophysics（哈佛-史密松天体物理中心）；Carnegie Mellon University（卡内基梅隆大学）；Flatiron Institute（弗莱提荣研究所）；Columbia University（哥伦比亚大学）；University of Connecticut（康涅狄格大学）；Princeton University（普林斯顿大学）；University of California, Riverside（加州大学河滨分校）
We analyze the velocity anisotropy of stars in real and energy space for a sample of Milky Way-like galaxies in the TNG50 simulation. We employ different selection criteria, including spatial, kinematic and metallicity cuts, and make three halo classes ($\mathcal{A}$-$\mathcal{C}$) which show mild-to-strong sensitivity to different selections. The above classes cover 48%, 16% and 36% of halos, respectively. We analyze the $β$ radial profiles and divide them into either monotonically increasing radial profiles or ones with peaks and troughs. We demonstrate that halos with monotonically increasi…
SAMI and TNG-Cluster: tracing galaxy spin and environmental transformation across cluster phase-space and cosmic time
Universidade Tecnológica Federal do Paraná（帕拉纳联邦技术大学）；European Southern Observatory（欧洲南方天文台）；Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo（圣保罗大学天文、地球物理与大气科学研究所）；University of Dodoma, College of Natural and Mathematical Sciences（多多马大学自然与数理科学学院）
Facultad de Matemática, Astronomía, Física y Computación, UNC（数学、天文学、物理与计算学院，科尔多瓦大学）；Instituto de Astronomía Teórica y Experimental, CONICET–UNC（理论与实验天体物理研究所，阿根廷国家科学研究委员会-科尔多瓦大学）；Observatorio Astronómico de Córdoba, UNC（科尔多瓦天文台，科尔多瓦大学）；Department of Physics and Astronomy, University of Victoria（物理学与天文学系，维多利亚大学）；Max-Planck-Institut für Astrophysik（马克斯·普朗克天体物理学研究所）
Exploring the Galactic chemical evolution and enrichment scenarios with open clusters allows us to understand the history of the Milky Way disk. High-resolution spectra of OCs are a crucial tool, as they provide precise chemical information, to combine with precise distances and ages. The aim of the Stellar Population Astrophysics project is to derive homogeneous and accurate comprehensive chemical characterization of a number of poorly studied OCs.Using the HARPS-N echelle spectrograph at the Telescopio Nazionale Galileo, we obtained high-resolution spectra of giant stars in 18 OCs, 16 of whi…
Stellar population astrophysics (SPA) with the TNG. Abundance analysis of nearby red giants and red clump stars: combining high resolution spectroscopy and asteroseismology
Stellar Population Astrophysics (SPA) with the TNG. CNO abundances in 28 open clusters
Vilnius University（维尔纽斯大学）；INAF - Osservatorio di Astrofisica e Scienza dello Spazio（意大利国家天体物理研究所-空间科学与天文观测台）；University of Rome Tor Vergata（罗马托尔维加塔大学）；INAF - Osservatorio Astronomico di Roma（意大利国家天体物理研究所-罗马天文台）；INAF - Ossevatorio Astronomico di Padova（意大利国家天体物理研究所-帕多瓦天文台）
Stock 2 is a little-studied open cluster that shows an extended main-sequence turnoff (eMSTO). In order to investigate this phenomenon and characterise the cluster itself we performed high-resolution spectroscopy in the framework of the Stellar Population Astrophysics (SPA) project. We employed the High Accuracy Radial velocity Planet Searcher in North hemisphere spectrograph (HARPS-N) at the Telescopio Nazionale Galileo (TNG). We completed our observations with additional spectra taken with the Catania Astrophysical Observatory Spectrograph (CAOS). In total we observed 46 stars (dwarfs and gi…
Magnetic fields in the intracluster medium with TNG-Cluster: properties, morphology, and tangential anisotropy
Universität Heidelberg, Zentrum für Astronomie（海德堡大学天文学中心）；Universität Heidelberg, Interdisziplinäres Zentrum für Wissenschaftliches Rechnen（海德堡大学跨学科科学计算中心）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；Centre de recherche en astrophysique du Quebec (CRAQ)（魁北克天体物理学研究中心）
Cool Embeddings: Predicting Galaxy Cluster Cooling Times in IllustrisTNG and TNG-Cluster with AstroCLIP
Université de Montréal（蒙特利尔大学）；Centre de recherche en astrophysique du Québec (CRAQ)（魁北克天体物理学研究中心）；Dragonfly Focused Research Organization（龙卷风重点研究组织）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；University of Michigan（密歇根大学）
Stellar Population Astrophysics (SPA) with the TNG. Beyond the iron peak: Galactic evolution of molybdenum, ruthenium and zirconium through open clusters
University of Rome Tor Vergata（罗马托尔维加塔大学）；INAF - Osservatorio Astronomico di Roma（罗马天文台意大利国家天体物理研究所）；Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange（蔚蓝海岸大学、蔚蓝海岸天文台、法国国家科学研究中心、拉格朗日实验室）；The University of Texas, Austin（德克萨斯大学奥斯汀分校）；Saint Mary’s University（圣玛丽大学）；INAF – Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（博洛尼亚空间天体物理学和科学研究所意大利国家天体物理研究所）；Astronomical Observatory, Odesa National University（敖德萨国立大学天文台）；Malmö University（马尔默大学）；Nordic Optical Telescope（北欧光学望远镜）
Cluster-green galaxy correlations: where do these galaxies live?
Instituto de Astronomía Teórica y Experimental, CONICET - UNC（理论与实验天体物理研究所，CONICET-科尔多瓦大学）；Facultad de Matemática, Astronomía, Física y Computación, Universidad Nacional de Córdoba（数学、天文学、物理与计算学院，科尔多瓦国立大学）；Observatorio Astronómico, Universidad Nacional de Córdoba（天文台，科尔多瓦国立大学）
ERGO-ML: A continuous organization of the X-ray galaxy cluster population in TNG-Cluster with contrastive learning
Max Planck Institut für Astronomie（马克斯·普朗克天文学研究所）；Universität Heidelberg, Zentrum für Astronomie, ITA（海德堡大学天文中心）；Argelander-Institut für Astronomie（阿根兰德天文学研究所）
A new classification of ex-situ and in-situ Galactic globular clusters based on a method trained on Milky Way analogues in the TNG50 cosmological simulations
Observatoire de Paris, Université PSL, Sorbonne Université, Université Paris Cité, CY Cergy Paris Université, CNRS（巴黎天文台，巴黎文理研究大学，索邦大学，巴黎西岱大学，塞吉-蓬图瓦兹大学，法国国家科学研究中心）；Lund Observatory, Division of Astrophysics, Department of Physics, Lund University（隆德大学天体物理系隆德天文台）；Leibniz-Institut für Astrophysik Potsdam (AIP)（波茨坦阿基米德天体物理研究所）；Kavli IPMU (WPI), UTIAS, The University of Tokyo（东京大学宇宙学国际研究前沿中心）；Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona（巴塞罗那大学宇宙科学研究所）；Université de Strasbourg, CNRS, Observatoire astronomique de Strasbourg（斯特拉斯堡大学，法国国家科学研究中心，斯特拉斯堡天文台）
Euclid preparation. Spatially resolved stellar populations of local galaxies with Euclid: a proof of concept using synthetic images with the TNG50 simulation
Puzzling Ultra-Diffuse Galaxy Evolution (PUDGE). II. A transformation pathway from ultra-diffuse galaxies to compact dwarfs in galaxy clusters
Faculty of Mathematics, University of Belgrade（贝尔格莱德大学数学系）；Astronomical Observatory（天文台）；Institute of Astrobiology, University Research and Innovation Center, University of Crete（克里特大学研究创新中心天体生物学研究所）
