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Fornax 3D project: Assessing the diversity of IMF and stellar population maps within the Fornax Cluster
Martin-Navarro, I.1,2; Pinna, F.3; Coccato, L.4; Falcon-Barroso, J.1,2; van de Ven, G.5; Lyubenova, M.4; Corsini, E. M.6,7; Fahrion, K.4; Gadotti, D. A.4; Iodice, E.8; McDermid, R. M.9,10; Poci, A.9; Sarzi, M.11,12; Spriggs, T. W.12; Viaene, S.12,13; de Zeeuw, P. T.14,15; Zhu, L.16
2021-10-11
Source PublicationASTRONOMY & ASTROPHYSICS
ISSN0004-6361
Volume654Pages:27
AbstractThe stellar initial mass function (IMF) is central to our interpretation of astronomical observables and to our understanding of most baryonic processes within galaxies. The universality of the IMF, suggested by observations in our own Milky Way, has been thoroughly revisited due to the apparent excess of low-mass stars in the central regions of massive quiescent galaxies. As part of the efforts within the Fornax 3D project, we aim to characterize the two-dimensional IMF variations in a sample of 23 quiescent galaxies within the Fornax cluster. For each galaxy in the sample, we measured the mean age, metallicity, [Mg/Fe], and IMF slope maps from spatially resolved integrated spectra. The IMF maps show a variety of behaviors and internal substructures, roughly following metallicity variations. However, metallicity alone is not able to fully explain the complexity exhibited by the IMF maps. In particular, for relatively metal-poor stellar populations ([M/H] less than or similar to -0.1), the slope of the IMF seems to depend on the (specific) star formation rate at which stars were formed. Moreover, metallicity maps have systematically higher ellipticities than IMF slope ones. At the same time, both metallicity and IMF slope maps have at the same time higher ellipticities than the stellar light distribution in our sample of galaxies. In addition we find that, regardless of the stellar mass, every galaxy in our sample shows a positive radial [Mg/Fe] gradient. This results in a strong [Fe/H]-[Mg/Fe] relation, similar to what is observed in nearby, resolved galaxies. Since the formation history and chemical enrichment of galaxies are causally driven by changes in the IMF, our findings call for a physically motivated interpretation of stellar population measurements based on integrated spectra that take into account any possible time evolution of the stellar populations.
Keywordgalaxies: formation galaxies: evolution galaxies: elliptical and lenticular, cD galaxies: stellar content
Funding OrganizationSpanish Ministry of Science and Innovation ; Spanish Ministry of Science and Innovation ; European Research Council (ERC) ; European Research Council (ERC) ; Australian Research Council Future Fellowship ; Australian Research Council Future Fellowship ; MIUR grant PRIN ; MIUR grant PRIN ; Padua University ; Padua University ; Spanish Ministry of Science and Innovation ; Spanish Ministry of Science and Innovation ; European Research Council (ERC) ; European Research Council (ERC) ; Australian Research Council Future Fellowship ; Australian Research Council Future Fellowship ; MIUR grant PRIN ; MIUR grant PRIN ; Padua University ; Padua University ; Spanish Ministry of Science and Innovation ; Spanish Ministry of Science and Innovation ; European Research Council (ERC) ; European Research Council (ERC) ; Australian Research Council Future Fellowship ; Australian Research Council Future Fellowship ; MIUR grant PRIN ; MIUR grant PRIN ; Padua University ; Padua University ; Spanish Ministry of Science and Innovation ; Spanish Ministry of Science and Innovation ; European Research Council (ERC) ; European Research Council (ERC) ; Australian Research Council Future Fellowship ; Australian Research Council Future Fellowship ; MIUR grant PRIN ; MIUR grant PRIN ; Padua University ; Padua University
DOI10.1051/0004-6361/202141348
WOS KeywordINITIAL-MASS FUNCTION ; EARLY-TYPE GALAXIES ; STAR-FORMATION HISTORIES ; SPATIALLY-RESOLVED SPECTROSCOPY ; MULTI-GAUSSIAN EXPANSION ; ABSORPTION-LINE SPECTRA ; TO-LIGHT RATIO ; SDSS-IV MANGA ; RADIAL GRADIENTS ; ELLIPTIC GALAXIES
Language英语
Funding ProjectSpanish Ministry of Science and Innovation[PID2019-107427GB-C32] ; European Research Council (ERC)[724857] ; Australian Research Council Future Fellowship[FT150100333] ; MIUR grant PRIN[20173ML3WW001] ; Padua University[DOR1885254/18] ; Padua University[DOR1935272/19] ; Padua University[DOR2013080/20]
Funding OrganizationSpanish Ministry of Science and Innovation ; Spanish Ministry of Science and Innovation ; European Research Council (ERC) ; European Research Council (ERC) ; Australian Research Council Future Fellowship ; Australian Research Council Future Fellowship ; MIUR grant PRIN ; MIUR grant PRIN ; Padua University ; Padua University ; Spanish Ministry of Science and Innovation ; Spanish Ministry of Science and Innovation ; European Research Council (ERC) ; European Research Council (ERC) ; Australian Research Council Future Fellowship ; Australian Research Council Future Fellowship ; MIUR grant PRIN ; MIUR grant PRIN ; Padua University ; Padua University ; Spanish Ministry of Science and Innovation ; Spanish Ministry of Science and Innovation ; European Research Council (ERC) ; European Research Council (ERC) ; Australian Research Council Future Fellowship ; Australian Research Council Future Fellowship ; MIUR grant PRIN ; MIUR grant PRIN ; Padua University ; Padua University ; Spanish Ministry of Science and Innovation ; Spanish Ministry of Science and Innovation ; European Research Council (ERC) ; European Research Council (ERC) ; Australian Research Council Future Fellowship ; Australian Research Council Future Fellowship ; MIUR grant PRIN ; MIUR grant PRIN ; Padua University ; Padua University
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000705838200002
PublisherEDP SCIENCES S A
Citation statistics
Document Type期刊论文
Identifierhttp://ir.bao.ac.cn/handle/114a11/74916
Collection中国科学院国家天文台
Corresponding AuthorMartin-Navarro, I.
Affiliation1.Inst Astrofis Canarias, C Via Lactea S-N, San Cristobal la Laguna 38205, Spain
2.Univ Laguna, Dept Astrofis, San Cristobal la Laguna 38205, Spain
3.Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany
4.European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany
5.Univ Vienna, Dept Astrophys, Turkenschanzstr 17, A-1180 Vienna, Austria
6.Univ Padua, Dipartimento Fis & Astron G Galilei, Vicolo Osservat 3, I-35122 Padua, Italy
7.INAF Osservat Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy
8.INAF Osservat Astron Capodimonte, Via Moiariello 16, I-80131 Naples, Italy
9.Macquarie Univ, Res Ctr Astron Astrophys & Astrophoton, Dept Phys & Astron, Sydney, NSW 2109, Australia
10.ARC Ctr Excellence All Sky Astrophys 3 Dimens AST, Sydney, NSW, Australia
11.Armagh Observ & Planetarium, Armagh BT61 9DG, North Ireland
12.Univ Hertfordshire, Ctr Astrophys Res, Coll Lane, Hatfield AL10 9AB, England
13.Univ Ghent, Sterrenkundig Observ, Krijgslaan 281, B-9000 Ghent, Belgium
14.Leiden Univ, Sterrewacht Leiden, Postbus 9513, NL-2300 RA Leiden, Netherlands
15.Max Planck Inst Fuer Extraterr Phys, Giessenbachstr, D-85741 Garching, Germany
16.Chinese Acad Sci, Shanghai Astron Observ, 80 Nandan Rd, Shanghai 200030, Peoples R China
Recommended Citation
GB/T 7714
Martin-Navarro, I.,Pinna, F.,Coccato, L.,et al. Fornax 3D project: Assessing the diversity of IMF and stellar population maps within the Fornax Cluster[J]. ASTRONOMY & ASTROPHYSICS,2021,654:27.
APA Martin-Navarro, I..,Pinna, F..,Coccato, L..,Falcon-Barroso, J..,van de Ven, G..,...&Zhu, L..(2021).Fornax 3D project: Assessing the diversity of IMF and stellar population maps within the Fornax Cluster.ASTRONOMY & ASTROPHYSICS,654,27.
MLA Martin-Navarro, I.,et al."Fornax 3D project: Assessing the diversity of IMF and stellar population maps within the Fornax Cluster".ASTRONOMY & ASTROPHYSICS 654(2021):27.
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