A1 Refereed original research article in a scientific journal
Narrow absorption lines from intervening material in supernovae: II. Galaxy properties
Authors: González-Gaitán, Santiago; Gutiérrez, Claudia P.; Martins, Goncalo; Müller-Bravo, Tomás E.; Duarte, João; Anderson, Joseph P.; Galbany, Lluis; Sullivan, Mark; Rino-Silvestre, João; Caixach, Mariona; Morales-Garoffolo, Antonia; Goswami, Sabyasachi; Mourão, Ana M.; Mattila, Seppo
Publisher: EDP SCIENCES S A
Publishing place: LES ULIS CEDEX A
Publication year: 2025
Journal: Astronomy and Astrophysics
Journal name in source: ASTRONOMY & ASTROPHYSICS
Journal acronym: ASTRON ASTROPHYS
Article number: A119
Volume: 700
Number of pages: 19
ISSN: 0004-6361
eISSN: 1432-0746
DOI: https://doi.org/10.1051/0004-6361/202554355
Web address : https://doi.org/10.1051/0004-6361/202554355
Self-archived copy’s web address: https://research.utu.fi/converis/portal/detail/Publication/499839067
The interstellar medium (ISM) has a number of tracers such as the NaI D lambda lambda 5890, 5896 absorption lines that are evident in the spectra of galaxies but also in those of individual astrophysical sources such as stars, novae, or quasars. Here, we investigate narrow absorption features in the spectra of nearby supernovae (SNe) and compare them to local (<0.5 kpc) and global host galaxy properties. With a large and heterogeneous sample of spectra, we are able to recover the known relations of ISM with galaxy properties: larger columns of ISM gas are found in environments that are more massive, more actively star-forming, younger, and viewed from a more inclined angle. Most trends are stronger for local properties than global properties, and we find that the ISM column density decreases exponentially with the offset from the host galaxy centre, as expected for a gas distribution following an exponential radial profile. We also confirm trends for the velocity of galactic outflows increasing with radius. The current study demonstrates the capability of individual light sources to serve as ubiquitous tracers of ISM properties across various environments and galaxies.
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We thank the anonymous referee for the comments and suggestions that have helped us to improve the paper. S.G.G thanks FCT for financial support through Project No. UIDB/00099/2020 and for support from the ESO Scientific Visitor Programme. C.P.G. acknowledges financial support from the Secretary of Universities and Research (Government of Catalonia) and by the Horizon 2020 Research and Innovation Programme of the European Union under the Marie Skłodowska-Curie and the Beatriu de Pinós 2021 BP 00168 programme, C.P.G. and L.G. recognise the support from the Spanish Ministerio de Ciencia e Innovaciôn (MCIN) and the Agencia Estatal de Investigación (AEI) 10.13039/501100011033 under the PID2023-151307NB-I00 SNNEXT project, from Centro Superior de Investigaciones Cientificas (CSIC) under the PIE project 20215AT016 and the program Unidad de Excelencia Maria de Maeztu CEX2020-001058-M, and from the Departament de Recerca i Universitats de la Generalitat de Catalunya through the 2021-SGR-01270 grant. A.M.G. acknowledges financial support from grant PID2023-152609OA-I00, funded by the Spanish Ministerio de Ciencia, Innovación y Universidades (MICIU), the Agencia Estatal de Investigación (AEI, 10.13039/501100011033), and the European Union’s European Regional Development Fund (ERDF). S.M. acknowledges support from the Research Council of Finland project 350458. This research has made use of the python packages hostphot (Müller-Bravo & Galbany 2022) for galaxy photometry and prospector (Johnson et al. 2021; Leja et al. 2017) for SED fitting. hostphot uses astropy (Astropy Collaboration 2013, 2018, 2022), photutils (Bradley et al. 2023), sep (Barbary 2016; Bertin & Arnouts 1996), ASTROQUERY (Ginsburg et al. 2019), REPROject, extinction (Barbary 2016), sfdmap, pyvo (Graham et al. 2014), ipywidgets and ipympl6. prospector also requires FSPS (Conroy et al. 2009; Conroy & Gunn 2010), PYTHON-FSPS (Johnson et al. 2023) and EMCEE (Foreman-Mackey et al. 2013). We also made use of: numpy (Harris et al. 2020), matplotlib (Hunter 2007), s cipy (Virtanen et al. 2020) and pandas (The pandas development team 2020; Wes McKinney 2010). We use the python implementations of KDA: key-driver-analysis (https://github.com/ bnriiitb/key-driver-analysis) and symbolic regression: PySR (Cranmer 2023) (https://github.com/MilesCranmer/PySR). Computations were performed at the cluster COIN, the CosmoStatistics Initiative, whose purchase was made possible due to a CNRS MOMENTUM 2018-2020 under the project “Active Learning for large scale sky surveys”. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is funded by the National Aeronautics and Space Administration and operated by the California Institute of Technology. This project used public archival data from the Dark Energy Survey (DES), the Sloan Digital Sky Survey (SDSS), the NASA Galaxy Evolution Explorer (GALEX), the Two Micron All Sky Survey (2MASS), the Visible and Infrared Survey Telescope for Astronomy (VISTA). Funding for the SDSS-V has been provided by the Alfred P. Sloan Foundation, the Heising-Simons Foundation, the National Science Foundation, and the Participating Institutions. SDSS acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. SDSS telescopes are located at Apache Point Observatory, funded by the Astrophysical Research Consortium and operated by New Mexico State University, and at Las Campanas Observatory, operated by the Carnegie Institution for Science. The SDSS web site is www.sdss.org. SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration, including Caltech, The Carnegie Institution for Science, Chilean National Time Allocation Committee (CNTAC) ratified researchers, The Flatiron Institute, the Gotham Participation Group, Harvard University, Heidelberg University, The Johns Hopkins University, L’Ecole polytechnique fédérale de Lausanne (EPFL), Leibniz-Institut für Astrophysik Potsdam (AIP), Max-Planck-Institut für Astronomie (MPIA Heidelberg), Max-Planck-Institut für Extraterrestrische Physik (MPE), Nanjing University, National Astronomical Observatories of China (NAOC), New Mexico State University, The Ohio State University, Pennsylvania State University, Smithsonian Astrophysical Observatory, Space Telescope Science Institute (STScI), the Stellar Astrophysics Participation Group, Universidad Nacional Autónoma de México, University of Arizona, University of Colorado Boulder, University of Illinois at Urbana-Champaign, University of Toronto, University of Utah, University of Virginia, Yale University, and Yunnan University. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desen-volvimento Cientifíco e Tecnológico and the Ministério da Ciência, Tecnolo-gia e Inovação, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are
Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambi-entales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Cièn-cies de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the OzDES Membership Consortium, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, and Texas A&M University. Based in part on observations at Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The Pan-STARRS1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the PanSTARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, the Queen’s University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation Grant No. AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation. GALEX is operated for NASA by the California Institute of Technology under NASA contract NAS5-98034. 2MASS, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. Based on data products created from observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme 179.A-2010 and made use of data from the VISTA Hemisphere survey (McMahon et al. 2013) with data pipeline processing with the VISTA Data Flow System (Irwin et al. 2004; Lewis et al. 2010; Cross et al. 2012). 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.
