A1 Vertaisarvioitu alkuperäisartikkeli tieteellisessä lehdessä
Looking into the faintEst WIth MUSE (LEWIS): Exploring the nature of ultra-diffuse galaxies in the Hydra I cluster III. Untangling UDG 32 from the stripped filaments of NGC 3314A with multi-wavelength data
Tekijät: Hartke, Johanna; Iodice, Enrichetta; Gullieuszik, Marco; Mirabile, Marco; Buttitta, Chiara; Doll, Goran; D'Ago, Giuseppe; de la Casa, Clara C.; Hess, Kelley M.; Kotulla, Ralf; Poggianti, Bianca; Arnaboldi, Magda; Cantiello, Michele; Corsini, Enrico Maria; Falcon-Barroso, Jesus; Forbes, Duncan; Hilker, Michael; Mieske, S.; Rejkuba, Marina; Spavone, Marilena; Spiniello, C.
Kustantaja: EDP SCIENCES S A
Kustannuspaikka: LES ULIS CEDEX A
Julkaisuvuosi: 2025
Journal: Astronomy and Astrophysics
Tietokannassa oleva lehden nimi: ASTRONOMY & ASTROPHYSICS
Lehden akronyymi: ASTRON ASTROPHYS
Artikkelin numero: A91
Vuosikerta: 695
Sivujen määrä: 15
ISSN: 0004-6361
eISSN: 1432-0746
DOI: https://doi.org/10.1051/0004-6361/202452975
Verkko-osoite: https://doi.org/10.1051/0004-6361/202452975
Rinnakkaistallenteen osoite: https://research.utu.fi/converis/portal/detail/Publication/491571474
Context. UDG 32 is an ultra-diffuse galaxy (UDG) candidate in the Hydra I cluster that was discovered in the extended network of stellar filaments of the jellyfish galaxy NGC 3314A. This jellyfish galaxy is affected by ram pressure stripping and it is hypothesised that UDG 32 may have formed from this stripped material.
Aims. The aim of this paper is to address whether UDG 32 can be associated with the stripped material of NGC 3314A and to constrain its formation scenario in relation to its environment.
Methods. We use new integral-field spectroscopic data from the MUSE large programme 'LEWIS' in conjunction with deep multi-band photometry to constrain the kinematics of UDG 32 via spectral fitting and its stellar population properties with spectral energy distribution fitting.
Results. The new MUSE data allow us to reveal that the stripped material from NGC 3314A, traced by emission lines such as H alpha, extends much further from its parent galaxy than previously known, completely overlapping with UDG 32 in projection, and with ram pressure induced star formation. We determine the line-of-sight velocity of UDG 32 to be v(LOS) = 3080 +/- 120 km s(-1) and confirm that UDG 32 is part of the same kinematic structure as NGC 3314A, the Hydra I cluster south-east subgroup. By fitting the UV and optical spectral energy distribution obtained from deep multi-band photometry, we constrain the stellar population properties of UDG 32. We determine its mass-weighted age to be 7.7(-2.8)(+2.9) Gyr and its metallicity to be [M/H] = 0.07(-0.32)(+0.19) dex. We confirm the presence of two globular clusters (GCs) in the MUSE field of view, bound to the Hydra I cluster rather than to UDG 32, making them part of the Hydra I intracluster GC population.
Conclusions. The metal-rich and intermediate-age nature of UDG 32 points towards its formation from pre-enriched material in the south-east group of the Hydra I cluster that was liberated from a more massive galaxy via tidal or ram-pressure stripping, but we cannot establish a direct link to the ram-pressure stripped material from NGC 3314A.
Ladattava julkaisu This is an electronic reprint of the original article. |  |
Julkaisussa olevat rahoitustiedot:
J.H. and E.I. acknowledge the financial support from the visitor and mobility programme of the Finnish Centre for Astronomy with ESO (FINCA), funded by the Academy of Finland grant nr 306531. J.H. wishes to acknowledge CSC – IT Center for Science, Finland, for computational resources. This work is based on the funding from the INAF through the GO large grant in 2022, to support the LEWIS data reduction and analysis (PI E. Iodice). E.I. and M.C. acknowledge the support by the Italian Ministry for Education, University and Research (MIUR) grant PRIN 2022 2022383WFT “SUNRISE”, CUP C53D23000850006. G.D. acknowledges support by UKRI-STFC grants: ST/T003081/1 and ST/X001857/1. C.C.d.l.C. acknowledges financial support from the grant CEX2021-001131-S funded by MICIU/AEI/ 10.13039/501100011033, from the grant PID2021-123930OB-C21 funded by MICIU/AEI/ 10.13039/501100011033, by ERDF/EU and from the grant TED2021-130231B-I00 funded by MICIU/AEI/ 10.13039/501100011033 and by the European Union NextGenerationEU/PRTR. R.K. gratefully acknowledges financial support from the National Science Foundation under Grant No. AST-2150222. J.F.-B. acknowledges support from the PID2022-140869NB-I00 grant from the Spanish Ministry of Science and Innovation. D.F. thanks the ARC for support via DP220101863 and DP200102574. EMC is supported by the Istituto Nazionale di Astrofisica (INAF) grant Progetto di Ricerca di Interesse Nazionale (PRIN) 2022 C53D23000850006 and Padua University grants Dotazione Ordinaria Ricerca (DOR) 2020–2022. Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programmes 108.222P and 099.B-0560. Based on observations made with the NASA Galaxy Evolution Explorer. GALEX was operated for NASA by the California Institute of Technology under NASA contract NAS5-98034. This research made use of the following open-source software packages: ASTROPY (Astropy Collaboration 2013, 2018), ASTROQUERY (Ginsburg et al. 2019), BAGPIPES (Carnall et al. 2018), CORNER (Foreman-Mackey 2016), DER_SNR (Stoehr et al. 2008), EMCEE (Foreman-Mackey et al. 2013), MATPLOTLIB (Hunter 2007), MPDAF (Bacon et al. 2016; Piqueras et al. 2017), NEBULABAYES (Thomas et al. 2018), NUMPY (van der Walt et al. 2011), PHOTUTILS (Bradley et al. 2023), and PPXF (Cappellari 2023). This research has made use of the Astrophysics Data System, funded by NASA under Cooperative Agreement 80NSSC21M00561. We thank Gannon et al. (2024) for the compilation of their catalogue of UDG spectroscopic properties. The catalogue includes data from: McConnachie (2012), van Dokkum et al. (2015b), Beasley et al. (2016), Martin et al. (2016), Yagi et al. (2016), Martínez-Delgado et al. (2016), van Dokkum et al. (2016, 2017), Karachentsev et al. (2017), van Dokkum et al. (2018), Toloba et al. (2018), Gu et al. (2018), Lim et al. (2018), Ruiz-Lara et al. (2018), Alabi et al. (2018), Ferré-Mateu et al. (2018), Forbes et al. (2018), Martín-Navarro et al. (2019), Chilingarian et al. (2019), Fensch et al. (2019), Danieli et al. (2019), van Dokkum et al. (2019), Torrealba et al. (2019), Iodice et al. (2020), Collins et al. (2020), Müller et al. (2020), Gannon et al. (2020), Lim et al. (2020), Müller et al. (2021), Forbes et al. (2021), Shen et al. (2021), Ji et al. (2021), Huang & Koposov (2021), Gannon et al. (2021, 2022), Mihos et al. (2022), Danieli et al. (2022), Villaume et al. (2022), Webb et al. (2022), Saifollahi et al. (2022), Janssens et al. (2022), Gannon et al. (2023), Ferré-Mateu et al. (2023), Toloba et al. (2023), Iodice et al. (2023), Shen et al. (2023).
