| Title: | Probing gas and dust in the tidal tail of NGC 5221 with the type Ia supernova iPTF16abc |
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| Authors: | ID Ferretti, Raphael, Department of Physics, The Oskar Klein Centre, Stockholm University, Albanova, 106 92 Stockholm, Sweden (Author)
ID Amanullah, Rahman, Department of Physics, The Oskar Klein Centre, Stockholm University, Albanova, 106 92 Stockholm, Sweden (Author)
ID Goobar, Ariel, Department of Physics, The Oskar Klein Centre, Stockholm University, Albanova, 106 92 Stockholm, Sweden (Author)
ID Petrushevska, Tanja, Department of Physics, The Oskar Klein Centre, Stockholm University, Albanova, 106 92 Stockholm, Sweden (Author) |
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| Files: |
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| Language: | English |
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| Work type: | Not categorized |
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| Typology: | 1.01 - Original Scientific Article |
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| Organization: | UNG - University of Nova Gorica
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| Abstract: | Context. Type Ia supernovae (SNe Ia) can be used to address numerous questions in astrophysics and cosmology. Due to their well
known spectral and photometric properties, SNe Ia are well suited to study gas and dust along the lines-of-sight to the explosions.
For example, narrow Na I D and Ca II H&K absorption lines can be studied easily, because of the well-defined spectral continuum of
SNe Ia around these features.
Aims. We aim to study the gas and dust along the line-of-sight to iPTF16abc, which occurred in an unusual location, in a tidal arm,
80 kpc from centre of the galaxy NGC 5221.
Methods. Using a time-series of high-resolution spectra, we have examined narrow Na I D and Ca II H&K absorption features for
variations in time, which would be indicative for circumstellar (CS) matter. Furthermore, we have taken advantage of the well known
photometric properties of SNe Ia to determine reddening due to dust along the line-of-sight.
Results. From the lack of variations in Na I D and Ca II H&K, we determine that none of the detected absorption features originate
from the CS medium of iPTF16abc. While the Na I D and Ca II H&K absorption is found to be optically thick, a negligible amount
of reddening points to a small column of interstellar dust.
Conclusions. We find that the gas along the line-of-sight to iPTF16abc is typical of what might be found in the interstellar medium
(ISM) within a galaxy. It suggests that we are observing gas that has been tidally stripped during an interaction of NGC 5221 with
one of its neighbouring galaxies in the past ∼109 yr. In the future, the gas clouds could become the locations of star formation. On
a longer time scale, the clouds might diffuse, enriching the circum-galactic medium (CGM) with metals. The gas profile along the
line-of-sight should be useful for future studies of the dynamics of the galaxy group containing NGC 5221. |
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| Keywords: | supernovae: individual: iPTF16abc – galaxies: individual: NGC 5221 – galaxies: ISM – galaxies |
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| Publication version: | Version of Record |
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| Year of publishing: | 2017 |
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| Number of pages: | 8 |
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| Numbering: | A111, 606 |
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| PID: | 20.500.12556/RUNG-3574-a20b27a8-982d-00bd-cad8-60614008b938 |
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| COBISS.SI-ID: | 4998651 |
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| DOI: | 10.1051/0004-6361/201731409 |
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| NUK URN: | URN:SI:UNG:REP:PYZIJMIQ |
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| Publication date in RUNG: | 23.01.2018 |
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| Views: | 3007 |
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| Downloads: | 0 |
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