Distribution of type Ib/c supernovae relative to galactic spiral arms

Mikhailova, G. A.; Bartunov, O. S.; Tsvetkov, D. Yu.

doi:10.1134/s1063773707110011

Cited by 8 publications

(15 citation statements)

References 15 publications

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“…These values show that, in contrast to d1, the distributions of d2 for all types of SNe are consistent with a Gaussian centred on the peaks of spiral arms. Therefore, the asymmetric distributions of SNe Ibc (obtained by Mikhailova et al 2007) and II with respect to the middle of spiral arm are just an effect of first normalization scheme of SNe distances, which does not take into account the intrinsic structure of spiral arms.…”

Section: Distribution Of Sne Relative To Spiral Armsmentioning

confidence: 99%

“…In the first approach, the distance 7 dSN of an SN from the inner edge (at galactocentric radius r = r−) of the spiral arm is normalized to the width W , defined as the distance between inner and outer edge (at galactocentric radius r+) of the arm (e.g. Maza & van den Bergh 1976;Bartunov et al 1994;Mikhailova et al 2007):…”

Section: Normalized Distances Along Arm Profilesmentioning

confidence: 99%

“…the second case. Most probably this effect is reflected in the results of Mikhailova et al (2007), who found that the distribution of SNe Ibc is skewed towards the inner edges of arms.…”

Section: Normalized Distances Along Arm Profilesmentioning

confidence: 99%

“…McMillan & Ciardullo (1996) and Petrosian et al (2005) found that CC SNe are more tightly concentrated to the arms than Ia. Finally, Mikhailova et al (2007) found that SNe Ibc 1 are concentrated to the inner edges of the spiral arms. They noted that there is a difference between the distribution of Ibc and II SNe, and conclude that the progenitors of Ibc SNe are younger.…”

Section: Introductionmentioning

confidence: 95%

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Supernovae and their host galaxies – IV. The distribution of supernovae relative to spiral arms

Aramyan

Hakobyan

Петросян

et al. 2016

Mon. Not. R. Astron. Soc.

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Using a sample of 215 supernovae (SNe), we analyze their positions relative to the spiral arms of their host galaxies, distinguishing grand-design (GD) spirals from non-GD (NGD) galaxies. We find that: (1) in GD galaxies, an offset exists between the positions of Ia and core-collapse (CC) SNe relative to the peaks of arms, while in NGD galaxies the positions show no such shifts; (2) in GD galaxies, the positions of CC SNe relative to the peaks of arms are correlated with the radial distance from the galaxy nucleus. Inside (outside) the corotation radius, CC SNe are found closer to the inner (outer) edge. No such correlation is observed for SNe in NGD galaxies nor for SNe Ia in either galaxy class; (3) in GD galaxies, SNe Ibc occur closer to the leading edges of the arms than do SNe II, while in NGD galaxies they are more concentrated towards the peaks of arms. In both samples of hosts, the distributions of SNe Ia relative to the arms have broader wings. These observations suggest that shocks in spiral arms of GD galaxies trigger star formation in the leading edges of arms affecting the distributions of CC SNe (known to have short-lived progenitors). The closer locations of SNe Ibc vs. SNe II relative to the leading edges of the arms supports the belief that SNe Ibc have more massive progenitors. SNe Ia having less massive and older progenitors, have more time to drift away from the leading edge of the spiral arms.

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Section: Distribution Of Sne Relative To Spiral Armsmentioning

confidence: 99%

Section: Normalized Distances Along Arm Profilesmentioning

confidence: 99%

“…the second case. Most probably this effect is reflected in the results of Mikhailova et al (2007), who found that the distribution of SNe Ibc is skewed towards the inner edges of arms.…”

Section: Normalized Distances Along Arm Profilesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 95%

See 2 more Smart Citations

Supernovae and their host galaxies – IV. The distribution of supernovae relative to spiral arms

Aramyan

Hakobyan

Петросян

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Although based on small number statistics, the early attempts to study the distribution of CC SNe within the framework of DW theory were performed by Moore (1973); McMillan & Ciardullo (1996) and Mikhailova et al (2007). In our recent paper (Aramyan et al 2016), we studied the distribution of 215 SNe relative to the spiral arms of their GD and non-GD (NGD) 1 host galaxies, using the Sloan Digital Sky Survey (SDSS) images.…”

Section: Introductionmentioning

confidence: 99%

The impact of spiral density waves on the distribution of supernovae

Karapetyan

Hakobyan

Barkhudaryan

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We present an analysis of the impact of spiral density waves (DWs) on the radial and surface density distributions of core-collapse (CC) supernovae (SNe) in host galaxies with different arm classes. For the first time, we show that the corotation radius normalized surface density distribution of CC SNe (tracers of massive star formation) indicates a dip at corotation in long-armed grand-design (LGD) galaxies. The high SNe surface density just inside and outside corotation may be the sign of triggered massive star formation by the DWs. Our results may support the large-scale shock scenario induced by spiral DWs in LGD galaxies, which predicts a higher star formation efficiency around the shock fronts, avoiding the corotation region.

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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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Distribution of type Ib/c supernovae relative to galactic spiral arms

Cited by 8 publications

References 15 publications

Supernovae and their host galaxies – IV. The distribution of supernovae relative to spiral arms

Supernovae and their host galaxies – IV. The distribution of supernovae relative to spiral arms

The impact of spiral density waves on the distribution of supernovae

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

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