Muestra métricas de impacto externas asociadas a la publicación. Para mayor detalle:
Departamento Gestión de Conocimiento, Monitoreo y Prospección
Consultas o comentarios: productividad@anid.cl
Consultas o comentarios: productividad@anid.cl
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
| Indexado |
|
||||
| DOI | 10.1051/0004-6361/202452975 | ||||
| Año | 2025 | ||||
| Tipo | artículo de investigación |
Citas Totales
Autores Afiliación Chile
Instituciones Chile
% Participación
Internacional
Autores
Afiliación Extranjera
Instituciones
Extranjeras
Abstract
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 Hα, 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 vLOS = 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.
| Ord. | Autor | Género | Institución - País |
|---|---|---|---|
| 1 | Hartke, J. | - |
Turun yliopisto - Finlandia
Tuorlan observatorio - Finlandia Univ Turku - Finlandia |
| 2 | Iodice, E. | Mujer |
Osservatorio Astronomico di Capodimonte - Italia
INAF - Italia |
| 3 | Gullieuszik, M. | - |
Osservatorio Astronomico di Padova - Italia
INAF Osservatorio Astron Padova - Italia |
| 4 | Mirabile, M. | - |
Istituto Nazionale Di Astrofisica, Rome - Italia
Observatorio Europeo Austral - Alemania Gran Sasso Science Institute - Italia INAF Osservatorio Astron Abruzzo - Italia European Southern Observ - Alemania Gran Sasso Sci Inst - Italia European Southern Observ - Chile INAF Osservatorio Astron Padova - Italia |
| 5 | Buttitta, C. | - |
Osservatorio Astronomico di Capodimonte - Italia
INAF - Italia |
| 6 | Doll, G. | - |
Osservatorio Astronomico di Capodimonte - Italia
Università Degli Studi di Napoli Federico II - Italia INAF - Italia Univ Naples Federico II - Italia |
| 7 | D'ago, G. | - |
Institute of Astronomy - Reino Unido
UNIV CAMBRIDGE - Reino Unido |
| 8 | De La Casa, C. C. | - |
CSIC - Instituto de Astrofísica de Andalucía (IAA) - España
Inst Astrofis Andalucia CSIC - España |
| 9 | Hess, K. M. | - |
Onsala Space Observatory - Suecia
Netherlands Foundation for Research in Astronomy - Países Bajos Chalmers Univ Technol - Suecia Netherlands Inst Radio Astron - Países Bajos |
| 10 | Kotulla, R. | - |
University of Wisconsin-Madison - Estados Unidos
Univ Wisconsin Madison - Estados Unidos |
| 11 | Poggianti, B. | Mujer |
Osservatorio Astronomico di Padova - Italia
INAF Osservatorio Astron Padova - Italia |
| 12 | Arnaboldi, M. | - |
Observatorio Europeo Austral - Alemania
European Southern Observ - Alemania European Southern Observ - Chile |
| 13 | Cantiello, M. | Mujer |
Istituto Nazionale Di Astrofisica, Rome - Italia
INAF Osservatorio Astron Abruzzo - Italia INAF Osservatorio Astron Padova - Italia |
| 14 | Corsini, E. M. | Hombre |
Osservatorio Astronomico di Padova - Italia
Università degli Studi di Padova - Italia INAF Osservatorio Astron Padova - Italia Univ Padua - Italia |
| 15 | Falcón-Barroso, J. | - |
Instituto Astrofisico de Canarias - España
Universidad de La Laguna - España Inst Astrofis Canarias - España UNIV LA LAGUNA - España |
| 16 | Forbes, D. A. | - |
Swinburne University of Technology - Australia
Swinburne Univ Technol - Australia |
| 17 | Hilker, M. | - |
Observatorio Europeo Austral - Alemania
European Southern Observ - Alemania European Southern Observ - Chile |
| 18 | Mieske, S. | - |
European Southern Observatory Santiago - Chile
European Southern Observ - Chile Observatorio Europeo Austral - Chile |
| 19 | Rejkuba, Marina | Mujer |
Observatorio Europeo Austral - Alemania
European Southern Observ - Alemania European Southern Observ - Chile |
| 20 | Spavone, M. | - |
Osservatorio Astronomico di Capodimonte - Italia
INAF - Italia |
| 21 | Spiniello, C. | - |
Osservatorio Astronomico di Capodimonte - Italia
University of Oxford - Reino Unido INAF - Italia UNIV OXFORD - Reino Unido |
| Fuente |
|---|
| National Science Foundation |
| China Scholarship Council |
| Spanish Ministry of Science and Innovation |
| Ministerio de Ciencia e Innovación |
| Australian Research Council |
| NASA |
| National Aeronautics and Space Administration |
| Ministerio de Ciencia, Innovacion y Universidades |
| Ministero dell’Istruzione, dell’Università e della Ricerca |
| ARC |
| Agencia Estatal de Investigación |
| California Institute of Technology |
| Academy of Finland |
| Istituto Nazionale di Astrofisica |
| European Organisation for Astronomical Research in the Southern Hemisphere under ESO |
| Università degli Studi di Padova |
| Italian Ministry for Education, University and Research (MIUR) |
| European Union NextGenerationEU/PRTR |
| PRTR |
| Finnish Centre for Astronomy |
| ERDF/EU |
| European Union NextGenerationEU |
| ESO (FINCA) |
| Dotazione Ordinaria Ricerca |
| Research Council of Finland |
| MICIU/AEI |
| UKRI-STFC |
| Istituto Nazionale di Astrofisica (INAF) grant Progetto di Ricerca di Interesse Nazionale (PRIN) 2022 |
| UKRISTFC |
| pPXF |
| INAF through the GO |
| Padua University grants Dotazione Ordinaria Ricerca (DOR) 2020-2022 |
| Agradecimiento |
|---|
| The authors wish to thank L. Buzzo, L. Coccato, E. Congiu, E. Emsellem, A. Ferr\u00E9-Mateu, C. Mondal, O. Gerhard, J. Gannon, F. Marleau, T. Puzia, and A. Werle for the useful comments and discussions on the work presented in this paper. We thank the anonymous referee for the careful reading of the manuscript and constructive comments. We thank the ESO Paranal Observatory staff for carrying out the observations used in this publication in service mode. 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 UKRISTFC 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. AST2150222. 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), Mart\u00EDnez-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), Ferr\u00E9-Mateu et al. (2018), Forbes et al. (2018), Mart\u00EDn-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), M\u00FCller et al. (2020), Gannon et al. (2020), Lim et al. (2020), M\u00FCller 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), Ferr\u00E9-Mateu et al. (2023), Toloba et al. (2023), Iodice et al. (2023), Shen et al. (2023). |
| The authors wish to thank L. Buzzo, L. Coccato, E. Congiu, E. Emsellem, A. Ferr\u00E9-Mateu, C. Mondal, O. Gerhard, J. Gannon, F. Marleau, T. Puzia, and A. Werle for the useful comments and discussions on the work presented in this paper. We thank the anonymous referee for the careful reading of the manuscript and constructive comments. We thank the ESO Paranal Observatory staff for carrying out the observations used in this publication in service mode. 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 UKRISTFC 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. AST2150222. 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), Mart\u00EDnez-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), Ferr\u00E9-Mateu et al. (2018), Forbes et al. (2018), Mart\u00EDn-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), M\u00FCller et al. (2020), Gannon et al. (2020), Lim et al. (2020), M\u00FCller 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), Ferr\u00E9-Mateu et al. (2023), Toloba et al. (2023), Iodice et al. (2023), Shen et al. (2023). |
| The authors wish to thank L. Buzzo, L. Coccato, E. Congiu, E. Emsellem, A. Ferre-Mateu, C. Mondal, O. Gerhard, J. Gannon, F. Marleau, T. Puzia, and A. Werle for the useful comments and discussions on the work presented in this paper. We thank the anonymous referee for the careful reading of the manuscript and constructive comments. We thank the ESO Paranal Observatory staff for carrying out the observations used in this publication in service mode. 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), Martinez-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), Ferre-Mateu et al. (2018), Forbes et al. (2018), Martin-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), Mueller et al. (2020), Gannon et al. (2020), Lim et al. (2020), Muller 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), Ferre-Mateu et al. (2023), Toloba et al. (2023), Iodice et al. (2023), Shen et al. (2023). |
