Time-varying sodium absorption in the Type Ia supernova 2013gh

Ferretti, R.; Amanullah, R.; Goobar, A.; Johansson, Joel; Vreeswijk, P. M.; Butler, R. Paul; Cao, Y.; Cenko, S. Bradley; Doran, Gary; Filippenko, A. V.; Freeland, Emily; Hosseinzadeh, G.; Howell, D. A.; Lundqvist, Peter; Mattila, S.; Nordin, J.; Nugent, P.; Petrushevska, T.; Valenti, S.; Vogt, Steven S.; Woźniak, P. R.

doi:10.1051/0004-6361/201628351

Cited by 19 publications

(19 citation statements)

References 67 publications

(91 reference statements)

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“…A larger sample of 14 SNe Ia with multi-epoch highresolution spectra (Sternberg et al 2014), did not reveal further examples of varying absorption lines. However, almost all existing time-series are taken at too late phases to probe for photoionisation of CS gas (see Ferretti et al 2016). Because of its low redshift, early discovery and a LOS seemingly clear of an ISM, the recently discovered SN 2017cbv (Hosseinzadeh et al 2017a) presents a good opportunity to search for photoionisation of CS gases.…”

Section: Introductionmentioning

confidence: 99%

No Evidence of Circumstellar Gas Surrounding Type Ia Supernova SN 2017cbv

Ferretti

Amanullah

Bulla

et al. 2017

ApJL

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Nearby type Ia supernovae (SNe Ia), such as SN 2017cbv, are useful events to address the question of what the elusive progenitor systems of the explosions are. Hosseinzadeh et al. (2017a) suggested that the early blue excess of the lightcurve of SN 2017cbv could be due to the supernova ejecta interacting with a nondegenerate companion star. Some SN Ia progenitor models suggest the existence of circumstellar (CS) environments in which strong outflows create low density cavities of different radii. Matter deposited at the edges of the cavities, should be at distances at which photoionisation due to early ultraviolet (UV) radiation of SNe Ia causes detectable changes to the observable Na I D and Ca II H&K absorption lines. To study possible narrow absorption lines from such material, we obtained a time-series of high-resolution spectra of SN 2017cbv at phases between −14.8 and +83 days with respect to B-band maximum, covering the time at which photoionisation is predicted to occur. Both narrow Na I D and Ca II H&K are detected in all spectra, with no measurable changes between the epochs. We use photoionisation models to rule out the presence of Na I and Ca II gas clouds along the line-of-sight of SN 2017cbv between ∼ 8 × 1016 -2 × 10 19 cm and Ca II within ∼ 10 15 -10 17 cm, respectively. Assuming typical abundances, the mass of a homogenous spherical CS gas shell with radius R must be limited to M CSM H I < 3 × 10 −4 × (R/10 17 [cm]) 2 M . The bounds point to progenitor models that deposit little gas in their CS environment.

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Section: Introductionmentioning

confidence: 99%

No Evidence of Circumstellar Gas Surrounding Type Ia Supernova SN 2017cbv

Ferretti

Amanullah

Bulla

et al. 2017

ApJL

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“…Thanks to the high lensing magnification we are able to study the structure and time evolution of interstellar absorption lines for z host = 0.4087 ± 0.0001 SNe Ia at cosmological distances, at a level previously only possible a small subset of very nearby SNe Ia (e.g. Goobar et al 2014;Ferretti et al 2016Ferretti et al , 2017. Similar to the lens galaxy, we also detect narrow emission lines from [O ] λ3727, H α , [N ] at the host galaxy redshift.…”

Section: The Host Galaxy Of Iptf16geumentioning

confidence: 78%

Spectroscopy of the first resolved strongly lensed Type Ia supernova iPTF16geu

Johansson

Goobar

Price

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We report the results from spectroscopic observations of the multiple images of the strongly lensed Type Ia supernova (SN Ia), iPTF16geu, obtained with ground-based telescopes and the Hubble Space Telescope (HST). From a single epoch of slitless spectroscopy with HST, we resolve spectra of individual lensed supernova images for the first time. This allows us to perform an independent measurement of the time-delay between the two brightest images, Δt = 1.4 ± 5.0 d, which is consistent with the time-delay measured from the light curves. We also present measurements of narrow emission and absorption lines characterizing the interstellar medium in the SN Ia host galaxy at z = 0.4087, as well as in the foreground lensing galaxy at z = 0.2163. We detect strong Na id absorption in the host galaxy, indicating that iPTF16geu belongs to a subclass of SNe Ia displaying ‘anomalously’ large Na id column densities compared to dust extinction derived from light curves. For the lens galaxy, we refine the measurement of the velocity dispersion, σ = 129 ± 4 km s−1, which significantly constrains the lens model. We use ground-based spectroscopy, boosted by a factor ∼70 from lensing magnification, to study the properties of a high-z SN Ia with unprecedented signal-to-noise ratio. The spectral properties of the supernova, such as pseudo-Equivalent widths of several absorption features and velocities of the Si ii-line, indicate that iPTF16geu is a normal SN Ia. We do not detect any significant deviations of the SN spectral energy distribution from microlensing of the SN photosphere by stars and compact objects in the lensing galaxy.

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“…For example, cases of slight variations in absorption line profiles (Patat et al 2007;Simon et al 2009;Patat et al 2013;Graham et al 2015;Ferretti et al 2016) hint at photoionisation or recombination of absorbers and predominantly blue-shifted Na I D profiles (Sternberg et al 2011;Maguire et al 2013) suggest outflowing gas.…”

Section: Absence Of Circumstellar Absorptionmentioning

confidence: 99%

Probing gas and dust in the tidal tail of NGC 5221 with the type Ia supernova iPTF16abc

Ferretti

Amanullah

Goobar

et al. 2017

A&A

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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 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 examine 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 take 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 ∼ 10 9 years. 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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Time-varying sodium absorption in the Type Ia supernova 2013gh

Cited by 19 publications

References 67 publications

No Evidence of Circumstellar Gas Surrounding Type Ia Supernova SN 2017cbv

No Evidence of Circumstellar Gas Surrounding Type Ia Supernova SN 2017cbv

Spectroscopy of the first resolved strongly lensed Type Ia supernova iPTF16geu

Probing gas and dust in the tidal tail of NGC 5221 with the type Ia supernova iPTF16abc

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