J/A+A/658/A80       Red giants of NGC 1851                 (Tautvaisiene+, 2022)

Gaia-ESO Survey: Detailed elemental abundances in red giants of the peculiar globular cluster NGC 1851. Tautvaisiene G., Drazdauskas A., Bragaglia A., Martell S.L., Pancino E., Lardo C., Mikolaitis S., Minkeviciute R., Stonkute E., Ambrosch M., Bagdonas V., Chorniy Y., Sanna N., Franciosini E., Smiljanic R., Randich S., Gilmore G., Bensby T., Bergemann M., Gonneau A., Guiglion G., Carraro G., Heiter U., Korn A., Magrini L., Morbidelli L., Zaggia S. <Astron. Astrophys. 658, A80 (2022)> =2022A&A...658A..80T 2022A&A...658A..80T (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, globular ; Abundances ; Spectroscopy ; Optical Keywords: stars: abundances - stars: evolution - globular clusters: individual: NGC 1851 Abstract: NGC 1851 is one of several globular clusters for which multiple stellar populations of the subgiant branch have been clearly identified and a difference in metallicity detected. A crucial piece of information on the formation history of this cluster can be provided by the sum of A(C+N+O) abundances. However, these values have lacked a general consensus thus far. The separation of the subgiant branch can be based on age and/or A(C+N+O) abundance differences. Our main aim was to determine carbon, nitrogen, and oxygen abundances for evolved giants in the globular cluster NGC 1851 in order to check whether or not the double populations of stars are coeval. High-resolution spectra, observed with the FLAMES-UVES spectrograph on the ESO VLT telescope, were analysed using a differential model atmosphere method. Abundances of carbon were derived using spectral synthesis of the C 2 band heads at 5135 and 5635.5Å. The wavelength interval 6470-6490Å, with CN features, was analysed to determine nitrogen abundances. Oxygen abundances were determined from the [OI] line at 6300Å. Abundances of other chemical elements were determined from equivalent widths or spectral syntheses of unblended spectral lines. We provide abundances of up to 29 chemical elements for a sample of 45 giants in NGC 1851. The investigated stars can be separated into two populations with a difference of 0.07dex in the mean metallicity, 0.3dex in the mean C/N, and 0.35 dex in the mean s-process dominated element-to-iron abundance ratios [s/Fe]. No significant difference was determined in the mean values of A(C+N+O) as well as in abundance to iron ratios of carbon, α- and iron-peak-elements, and of europium. As the averaged A(C+N+O) values between the two populations do not differ, additional evidence is given that NGC 1851 is composed of two clusters, the metal-rich cluster being by about 0.6Gyr older than the metal-poor one. A global overview of NGC 1851 properties and the detailed abundances of chemical elements favour its formation in a dwarf spheroidal galaxy that was accreted by the Milky Way. Description: Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 188.B-3002 (The Gaia-ESO Public Spectroscopic Survey, PIs G. Gilmore and S. Randich). File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file table3.dat 529 45 Main atmospheric parameters and elemental abundances in stars of the globular cluster NGC 1851 -------------------------------------------------------------------------------- See also: J/MNRAS/442/3044 : Photometry and abundances of NGC1851 stars (Marino+, 2014) Byte-by-byte Description of file: table3.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 16 A16 --- Cname CNAME (HHMMSSss+DDMMSSs) 18- 21 I4 K Teff Effective temperature 23- 25 I3 K e_Teff Error of effective temperature 27- 30 F4.2 [cm/s2] logg Stellar surface gravity 32- 35 F4.2 [cm/s2] e_logg Error of stellar surface gravity 37- 41 F5.2 --- [Fe/H] Metallicity 43- 46 F4.2 --- e_[Fe/H] Error of metallicity 48- 51 F4.2 km/s vt Microturbulent velocity 53- 56 F4.2 km/s e_vt Error of microturbulent velocity 58- 62 F5.2 --- [AlI/H] Abundance [AlI/H] 64- 67 F4.2 --- e_[AlI/H] Error on AlI abundance 69 I1 --- o_[AlI/H] Number of AlI lines 71- 75 F5.2 --- [BaII/H] Abundance [BaII/H] 77- 80 F4.2 --- e_[BaII/H] Error on BaII abundance 82 I1 --- o_[BaII/H] Number of BaII lines 84- 88 F5.2 --- [BaII/H]NLTE Abundance [BaII/H]_NLTE 90- 93 F4.2 --- e_[BaII/H]NLTE Error on BaII_NLTE abundance 95 I1 --- o_[BaII/H]NLTE Number of BaII_NLTE lines 97-101 F5.2 --- [C/H] ? Abundance [C/H] 103-106 F4.2 --- e_[C/H] ? Error on C abundance 108 I1 --- o_[C/H] ? Number of C lines 110-114 F5.2 --- [CaI/H] Abundance [CaI/H] 116-119 F4.2 --- e_[CaI/H] Error on CaI abundance 121-122 I2 --- o_[CaI/H] Number of CaI lines 124-128 F5.2 --- [CaII/H] Abundance [CaII/H] 130-133 F4.2 --- e_[CaII/H] Error on CaII abundance 135 I1 --- o_[CaII/H] Number of CaII lines 137-141 F5.2 --- [CeII/H] Abundance [CeII/H] 143-146 F4.2 --- e_[CeII/H] Error on CeII abundance 148 I1 --- o_[CeII/H] Number of CeII lines 150-154 F5.2 --- [CoI/H] Abundance [CoI/H] 156-159 F4.2 --- e_[CoI/H] Error on CoI abundance 161-162 I2 --- o_[CoI/H] Number of CoI lines 164-168 F5.2 --- [CrI/H] Abundance [CrI/H] 170-173 F4.2 --- e_[CrI/H] Error on CrI abundance 175-176 I2 --- o_[CrI/H] Number of CrI lines 178-182 F5.2 --- [CrII/H] Abundance [CrII/H] 184-187 F4.2 --- e_[CrII/H] Error on CrII abundance 189-190 I2 --- o_[CrII/H] Number of CrII lines 192-196 F5.2 --- [CuI/H] Abundance [CuI/H] 198-201 F4.2 --- e_[CuI/H] Error on CuI abundance 203 I1 --- o_[CuI/H] Number of CuI lines 205-209 F5.2 --- [EuII/H] Abundance [EuII/H] 211-214 F4.2 --- e_[EuII/H] Error on EuII abundance 216 I1 --- o_[EuII/H] Number of EuII lines 218-222 F5.2 --- [LaII/H] ? Abundance [LaII/H] 224-227 F4.2 --- e_[LaII/H] ? Error on LaII abundance 229 I1 --- o_[LaII/H] ? Number of LaII lines 231-235 F5.2 --- A(LiI) ? A(LiI) abundance 237-240 F4.2 --- e_A(LiI) ? Error on A(LiI) abundance 242 I1 --- o_A(LiI) ? Number of LiI lines 244-248 F5.2 --- A(LiI)3DNLTE ? A(LiI)_3DNLTE abundance 250-253 F4.2 --- e_A(LiI)3DNLTE ? Error on A(LiI)_3DNLTE abundance 255 I1 --- o_A(LiI)3DNLTE ? Number of LiI lines 257-261 F5.2 --- [MgI/H] Abundance [MgI/H] 263-266 F4.2 --- e_[MgI/H] Error on MgI abundance 268 I1 --- o_[MgI/H] Number of MgI lines 270-274 F5.2 --- [MnI/H] Abundance [MnI/H] 276-279 F4.2 --- e_[MnI/H] Error on MnI abundance 281-282 I2 --- o_[MnI/H] Number of MnI lines 284-288 F5.2 --- [MoI/H] ? Abundance [MoI/H] 290-293 F4.2 --- e_[MoI/H] ? Error on MoI abundance 295 I1 --- o_[MoI/H] ? Number of MoI lines 297-301 F5.2 --- [N/H] ? Abundance [N/H] 303-306 F4.2 --- e_[N/H] ? Error on N abundance 308 I1 --- o_[N/H] ? Number of N lines 310-314 F5.2 --- [NaI/H] Abundance [NaI/H] 316-319 F4.2 --- e_[NaI/H] Error on NaI abundance 321 I1 --- o_[NaI/H] Number of NaI lines 323-327 F5.2 --- [NaI/H]NLTE ? Abundance [NaI/H]_NLTE 329-332 F4.2 --- e_[NaI/H]NLTE ? Error on NaI_NLTE abundance 334 I1 --- o_[NaI/H]NLTE ? Number of NaI_NLTE lines 336-340 F5.2 --- [NdII/H] Abundance [NdII/H] 342-345 F4.2 --- e_[NdII/H] Error on NdII abundance 347-348 I2 --- o_[NdII/H] Number of NdII lines 350-354 F5.2 --- [NiI/H] Abundance [NiI/H] 356-359 F4.2 --- e_[NiI/H] Error on NiI abundance 361-362 I2 --- o_[NiI/H] Number of NiI lines 364-368 F5.2 --- [OI/H] ? Abundance [OI/H] 370-373 F4.2 --- e_[OI/H] ? Error on OI abundance 375 I1 --- o_[OI/H] ? Number of OI lines 377-381 F5.2 --- [PrII/H] ? Abundance [PrII/H] 383-386 F4.2 --- e_[PrII/H] ? Error on PrII abundance 388 I1 --- o_[PrII/H] ? Number of PrII lines 390-394 F5.2 --- [ScI/H] Abundance [ScI/H] 396-399 F4.2 --- e_[ScI/H] Error on ScI abundance 401 I1 --- o_[ScI/H] Number of ScI lines 403-407 F5.2 --- [ScII/H] Abundance [ScII/H] 409-412 F4.2 --- e_[ScII/H] Error on ScII abundance 414-415 I2 --- o_[ScII/H] Number of ScII lines 417-421 F5.2 --- [SiI/H] Abundance [SiI/H] 423-426 F4.2 --- e_[SiI/H] Error on SiI abundance 428 I1 --- o_[SiI/H] Number of SiI lines 430-434 F5.2 --- [SmII/H] ? Abundance [SmII/H] 436-439 F4.2 --- e_[SmII/H] ? Error on SmII abundance 441 I1 --- o_[SmII/H] ? Number of SmII lines 443-447 F5.2 --- [TiI/H] Abundance [TiI/H] 449-452 F4.2 --- e_[TiI/H] Error on TiI abundance 454-455 I2 --- o_[TiI/H] Number of TiI lines 457-461 F5.2 --- [TiII/H] Abundance [TiII/H] 463-466 F4.2 --- e_[TiII/H] Error on TiII abundance 468-469 I2 --- o_[TiII/H] Number of TiII lines 471-475 F5.2 --- [VI/H] Abundance [VI/H] 477-480 F4.2 --- e_[VI/H] Error on VI abundance 482-483 I2 --- o_[VI/H] Number of VI lines 485-489 F5.2 --- [YII/H] Abundance [YII/H] 491-494 F4.2 --- e_[YII/H] Error on YII abundance 496-497 I2 --- o_[YII/H] Number of YII lines 499-503 F5.2 --- [ZnI/H] Abundance [ZnI/H] 505-508 F4.2 --- e_[ZnI/H] Error on ZnI abundance 510 I1 --- o_[ZnI/H] Number of ZnI lines 512-516 F5.2 --- [ZrI/H] ? Abundance [ZrI/H] 518-521 F4.2 --- e_[ZrI/H] ? Error on ZrI abundance 523-524 I2 --- o_[ZrI/H] ? Number of ZrI lines 526-529 F4.2 --- C/N ? C/N ratio -------------------------------------------------------------------------------- History: From Grazina Tautvaisiene, grazina.tautvaisiene(at)tfai.vu.lt Acknowledgements: Based on the Gaia-ESO Public Spectroscopic Survey data products from observations made with the ESO Very Large Telescope at the La Silla Paranal Observatory under programme ID 188.B-3002. These data products have been processed by the Cambridge Astronomy Survey Unit (CASU) at the Institute of Astronomy, University of Cambridge, and the FLAMES/UVES reduction team at INAF/Osservatorio Astrofisico di Arcetri. The Gaia-ESO Survey Data Archive is prepared and hosted by the Wide Field Astronomy Unit, Institute for Astronomy, University of Edinburgh, which is funded by the UK Science and Technology Facilities Council. The anonymous referee is thanked for helpful suggestions. S.L.M acknowledges support from the Australian Research Council through grant DP180101791 and from the UNSW Scientia Fellowship program. T.B. was funded by grant No. 2018-04857 from The Swedish Research Council. U.H. acknowledges support from the Swedish National Space Agency (SNSA/Rymdstyrelsen). This research has made use of SIMBAD (operated at CDS, Strasbourg), of VALD (Kupka et al. 2000), and of NASA's Astrophysics Data System. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.
(End) Patricia Vannier [CDS] 19-Nov-2021
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