Direct distance measurements to SN 2009ip

Potashov, M. Sh.; Блинников, С. И.; Бакланов, П. В.; Dolgov, A. D.

doi:10.1093/mnrasl/slt016

Cited by 25 publications

(11 citation statements)

References 32 publications

(37 reference statements)

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“…In all of the following, we adopt the foreground reddening and distance towards SN 2009ip quoted by P13 and others μ = 31.55 mag, A R = 0.05 mag. The distance adopted is also in agreement with that found by Potashov et al (2013) from applying a geometric technique (the 'Dense Shell Method') to SN 2009ip itself.…”

Section: Introductionsupporting

confidence: 81%

SN 2009ip à la PESSTO: no evidence for core collapse yet★

Fraser

Inserra

Jerkstrand

et al. 2013

Monthly Notices of the Royal Astronomical Society

132

207

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We present ultraviolet, optical and near-infrared observations of the interacting transient SN 2009ip, covering the period from the start of the outburst in 2012 October until the end of the 2012 observing season. The transient reached a peak magnitude of M V = −17.7 mag, with a total integrated luminosity of 1.9 × 10 49 erg over the period of 2012 August-December. The light curve fades rapidly, dropping by 4.5 mag from the V-band peak in 100 d. The optical and near-infrared spectra are dominated by narrow emission lines with broad electron scattering wings, signalling a dense circumstellar environment, together with multiple components of broad emission and absorption in H and He at velocities in the range 0.5-1.2 × 10 4 km s −1 . We see no evidence for nucleosynthesized material in SN 2009ip, even in late-time pseudonebular spectra. We set a limit of <0.02 M on the mass of any possible synthesized 56 Ni from the late-time light curve. A simple model for the narrow Balmer lines is presented and used to derive number densities for the circumstellar medium in the range ∼10 9 -10 10 cm −3 . Our * Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile, as part of programme 188.D-3003 (PESSTO).

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Section: Introductionsupporting

confidence: 81%

SN 2009ip à la PESSTO: no evidence for core collapse yet★

Fraser

Inserra

Jerkstrand

et al. 2013

Monthly Notices of the Royal Astronomical Society

132

207

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“…Baklanov et al (2013) presents a LC model of SN 2009ip to demonstrate the dense shell method which is a newly-proposed method to use SNe IIn as a primary standard candle (cf. Potashov et al 2013). The CSM density slope is s = 3 and the average mass-loss rate is 10 −2 M⊙ yr −1 with vcsm = 100 km s −1 , which is consistent with our result.…”

Section: Sn 2009ipmentioning

confidence: 99%

Mass-loss histories of Type IIn supernova progenitors within decades before their explosion

Moriya

Maeda

Taddia

et al. 2014

Monthly Notices of the Royal Astronomical Society

113

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We present results of a systematic study of the mass-loss properties of Type IIn supernova progenitors within decades before their explosion. We apply an analytic light curve model to 11 Type IIn supernova bolometric light curves to derive the circumstellar medium properties. We reconstruct the mass-loss histories based on the estimated circumstellar medium properties. The estimated mass-loss rates are mostly higher than 10 −3 M ⊙ yr −1 and they are consistent with those obtained by other methods. The mass-loss rates are often found to be constantly high within decades before their explosion. This indicates that there exists some mechanism to sustain the high mass-loss rates of Type IIn supernova progenitors for at least decades before their explosion. Thus, the shorter eruptive mass loss events observed in some Type IIn supernova progenitors are not always responsible for creating their dense circumstellar media. In addition, we find that Type IIn supernova progenitors may tend to increase their mass-loss rates as they approach to the time of their explosion. We also show a detailed comparison between our analytic prediction and numerical results.

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“…The thick blue line is the adopted distance modulus in this work, µ = 32.00 ± 0.18, obtained as the weighted average of the PMM, SCM and PCM methods and the standard deviation is showed as a blue fill. We also show as a reference the distance measured to SN 2009ip in NGC 7259 (Potashov et al 2013).…”

Section: Distancementioning

confidence: 99%

The extraplanar type II supernova ASASSN-14jb in the nearby edge-on galaxy ESO 467-G051

Meza

Prieto

Clocchiatti

et al. 2019

A&A

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Aims. We present optical photometry and spectroscopy of the Type II supernova ASASSN-14jb, together with VLT MUSE IFU observations of its host galaxy and a nebular-phase spectrum. Methods. This supernova, in the nearby galaxy ESO 467-G051 (z = 0.006), was discovered and followed-up by the All Sky Automated Survey for SuperNovae (ASAS-SN). We obtained well-sampled LCOGTN BVgri and S wi f t w2m1w1ubv optical and near-UV/optical light curves and several optical spectra in the early photospheric phases. ASASSN-14jb exploded ∼ 2 kpc above the star-forming disk of ESO 467-G051, an edge-on disk galaxy. The large projected distance from the disk and non-detection of any H II region in a 1.4 kpc radius in projection are in conflict with the standard environment of core-collapse supernova progenitors and suggests the possible scenario that the progenitor received a kick in a binary interaction. Results. We present analysis of the optical light curves and spectra, from which we derive a distance of 25 ± 1 Mpc using state of the art empirical methods for Type II SNe, physical properties of the SN explosion ( 56 Ni mass, explosion energy, and ejected mass) and properties of the progenitor, namely the progenitor radius, mass and metallicity. Our analysis yields a 56 Ni mass of 0.0210 ± 0.0025 M , an explosion energy of ≈ 0.25 × 10 5 1 ergs and an ejected mass of ≈ 6 M . We also constrain the progenitor radius to be R * = 580 ± 28 R which seems to be consistent with the sub-Solar metallicity of 0.3 ± 0.1 Z derived from the supernova Fe II λ5018 line. The nebular spectrum constrains strongly the progenitor mass to be in the range 10-12 M . From Spitzer data archive we detect ASASSN-14jb ≈ 330 days past explosion and we derive a total dust mass of 10 −4 M from the 3.6 µm and 4.5 µm photometry. Using the FUV, NUV, BVgri,K s , 3.6 µm, and 4.5 µm total magnitudes for the host galaxy, we fit stellar population synthesis models which gives an estimate of M * ≈ 1 × 10 9 M , an age of 3.2 Gyr, and a SFR ≈ 0.07 M /yr. We also discuss the low oxygen abundance of the host galaxy derived from the MUSE data, having an average of 12 + log (O/H) = 8.27 +0.16 −0.20 using the O3N2 diagnostic, with strong line methods and compare it with the supernova spectra, which is also consistent with a sub-Solar metallicity progenitor. Following recent observations of extraplanar H II regions in nearby edge-on galaxies, we derive the metallicity offset from the disk, being positive (but consistent with zero at 2 σ), suggesting enrichment from disk outflows. We finally discuss the possible scenarios for the unusual environment for ASASSN-14jb and conclude that either the in-situ star formation or runaway scenario would imply a low mass progenitor, agreeing with our estimate from the supernova nebular spectrum. Regardless of the true origin of ASASSN-14jb we show in this work that the detailed study of the environment can roughly agree with the stronger constrains of the transient observations.

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Direct distance measurements to SN 2009ip

Cited by 25 publications

References 32 publications

SN 2009ip à la PESSTO: no evidence for core collapse yet★

SN 2009ip à la PESSTO: no evidence for core collapse yet★

Mass-loss histories of Type IIn supernova progenitors within decades before their explosion

The extraplanar type II supernova ASASSN-14jb in the nearby edge-on galaxy ESO 467-G051

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