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Title: Constraints on core-collapse supernova progenitors from explosion site integral field spectroscopy

Journal Article · · Astronomy and Astrophysics
ORCiD logo [1];  [2];  [3];  [4];  [5];  [6];  [7];  [8];  [8];  [9]
  1. Univ. of Turku, Piikkiö (Finland); Millennium Inst. of Astrophysics, Santiago (Chile); Univ. de Chile, Santiago (Chile)
  2. European Southern Observatory, Santiago (Chile)
  3. Univ. of Pittsburgh, Pittsburgh, PA (United States)
  4. Kyoto Univ., Kyoto (Japan); The Univ. of Tokyo, Chiba (Japan)
  5. Millennium Inst. of Astrophysics, Santiago (Chile); Univ. de Chile, Santiago (Chile)
  6. Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
  7. Seoul National Univ., Seoul (Korea); National Institutes of Natural Sciences, Hilo, HI (United States)
  8. Univ. of Tokyo, Tokyo (Japan)
  9. National Astronomical Observatory of Japan, Tokyo (Japan); SOKENDAI (The Graduate Univ. for Advanced Studies), Tokyo (Japan)
+ Show Author Affiliations

Observationally, supernovae (SNe) are divided into subclasses according to their distinct characteristics. This diversity naturally reflects the diversity in the progenitor stars. It is not entirely clear, however, how different evolutionary paths leading massive stars to become an SN are governed by fundamental parameters such as progenitor initial mass and metallicity. Furthermore, this paper places constraints on progenitor initial mass and metallicity in distinct core-collapse SN subclasses through a study of the parent stellar populations at the explosion sites. Integral field spectroscopy (IFS) of 83 nearby SN explosion sites with a median distance of 18 Mpc has been collected and analysed, enabling detection and spectral extraction of the parent stellar population of SN progenitors. From the parent stellar population spectrum, the initial mass and metallicity of the coeval progenitor are derived by means of comparison to simple stellar population models and strong-line methods. Additionally, near-infrared IFS was employed to characterise the star formation history at the explosion sites. No significant metallicity differences are observed among distinct SN types. The typical progenitor mass is found to be highest for SN type Ic, followed by type Ib, then types IIb and II. Type IIn is the least associated with young stellar populations and thus massive progenitors. However, statistically significant differences in progenitor initial mass are observed only when comparing SNe IIn with other subclasses. Stripped-envelope SN progenitors with initial mass estimates lower than 25 M⊙ are found; they are thought to be the result of binary progenitors. Confirming previous studies, these results support the notion that core-collapse SN progenitors cannot arise from single-star channels only, and both single and binary channels are at play in the production of core-collapse SNe. Near-infrared IFS suggests that multiple stellar populations with different ages may be present in some of the SN sites. As a consequence, there could be a non-negligible amount of contamination from old populations, and therefore the individual age estimates are effectively lower limits.

Research Organization:
Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States). National Energy Research Scientific Computing Center (NERSC)
Sponsoring Organization:
USDOE
OSTI ID:
1543824
Journal Information:
Astronomy and Astrophysics, Vol. 613; ISSN 0004-6361
Publisher:
EDP SciencesCopyright Statement
Country of Publication:
United States
Language:
English
Citation Metrics:
Cited by: 44 works
Citation information provided by
Web of Science

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Cited By (14)

A hybrid envelope-stripping mechanism for massive stars from supernova nebular spectroscopy journal March 2019
Relativistic supernova 2009bb exploded close to an atomic gas cloud journal October 2018
The extraplanar type II supernova ASASSN-14jb in the nearby edge-on galaxy ESO 467-G051 journal September 2019
A meta-analysis of core-collapse supernova 56 Ni masses journal July 2019
The diverse lives of progenitors of hydrogen-rich core-collapse supernovae: the role of binary interaction journal October 2019
Core-collapse supernovae ages and metallicities from emission-line diagnostics of nearby stellar populations journal October 2018
Investigating the properties of stripped-envelope supernovae; what are the implications for their progenitors? journal December 2018
The 50–100 pc scale parent stellar populations of Type II supernovae and limitations of single star evolution models journal October 2019
The radial distribution of supernovae compared to star formation tracers journal November 2019
A Long-duration Luminous Type IIn Supernova KISS15s: Strong Recombination Lines from the Inhomogeneous Ejecta–CSM Interaction Region and Hot Dust Emission from Newly Formed Dust journal February 2019
Core-collapse supernovae ages and metallicities from emission-line diagnostics of nearby stellar populations text January 2018
Relativistic supernova 2009bb exploded close to an atomic gas cloud text January 2018
Investigating the properties of stripped-envelope supernovae, what are the implications for their progenitors? text January 2018
The radial distribution of supernovae compared to star formation tracers text January 2019

Figures / Tables (16)

Fig. 1(p. 4)figure Fig. 1
Fig. 2(p. 4)figure Fig. 2
Table 1(p. 5)table Table 1
Fig. 3(p. 6)figure Fig. 3
Fig. 4(p. 7)figure Fig. 4
Fig. 5(p. 8)figure Fig. 5
Fig. 6(p. 8)figure Fig. 6
panel (i) represents the SINFONI FoV, and the white circle denotes the SN position within 1" radius. North is up and east is left in all maps. Cyan circles in panels (iii) and (iv) indicated with A and B have identical radii of 0.25". Panel (v) shows the SINFONI spaxels plotted according to the Br$$γ$$ and CO NCRs; these are shown as contours at 10%, 50%, and 90% levels, while for comparison, the VIMOS spaxels are plotted in red plus marks according to the H$$α$$ and [N ⅠⅠ] NCR. Panel (vi) shows the extracted spectra of regions A and B, in the Br$$γ$$ and CO spectral regions. The two lines are indicated with green-shaded regions. Wavelength is in the observer frame." data-ostiid="1543824">
Fig. 7(p. 9)figure Fig. 7
Table 2(p. 9)table Table 2
Fig. 8(p. 10)figure Fig. 8
Fig. 10(p. 12)figure Fig. 10
Fig. 9(p. 12)figure Fig. 9
Table A.1 Part 1(p. 15)table Table A.1 Part 1
Table A.1 Part 2(p. 16)table Table A.1 Part 2
Table A.2 Part 1(p. 17)table Table A.2 Part 1
Table A.2 Part 2(p. 18)table Table A.2 Part 2

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79 ASTRONOMY AND ASTROPHYSICS
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supernovae: general
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