Type Ibn Supernovae. Type Ibn Supernovae. Andrea Pastorello (INAF-OAPd) Andrea Pastorello (INAF-OAPd) Stockholm May 28 - June 1, 2018
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1 Type Ibn Supernovae Type Ibn Supernovae Andrea Pastorello (INAF-OAPd) Stockholm May 28 - June 1, 2018 Andrea Pastorello (INAF-OAPd)
2 Overview Introduction; SN 2006jc Heterogeneity of SN Ibn observables The progenitors of SNe Ibn: low or high mass stars? Conclusions
3 Timeline SN 1999cq, the first Ibn Matheson SN 2006jc & its pre-sn outburst Pastorello+ 2007; Foley SN Ibn designation Pastorello An SN Ibn in an E host Sanders Large SN Ibn samples Pastorello+ 2016; Hosseinzadeh The first SLSN Ibn Vallely+ 2018
4 Mass loss and interacting SNe Massive stars lose mass (via stellar winds, binary interaction, major outbursts), and form circumstaller cocoons. SN explosions in H-rich CSM produce SNe IIn (Schlegel 1990, MNRAS, 244, 269) SN explosions in H-poor and He-rich CSM produce SNe Ibn (Matheson+ 2000, AJ, 119, 2303; Pastorello+ 2008, MNRAS, 389, 113)
5 SN Ibn spectra Pastorello+ 2015, MNRAS, 449, 2921 Early Late
6 An outburts heralds the SN Ibn explosion Oct 2004 Oct 2006 Inserra & Smartt 2014 SN 2006jc Pastorello+ 2007, Nature, 447, 829 (also Foley+ 2007, ApJ, 657, L105) 2004 => Major outburst (MR = -14) 2006 => SN explosion as SE-SN interacting with He-rich CSM
7 Dust in a CDS Mattila et al. 2008, MNRAS, 389, 141 Late time optical deficit & NIR excess => old dust, and new dust in a CDS Smith+ 2008, Mattila+ 2008, Di Carlo+ 2008, Tominaga+ 2008
8 An homogeneous group? Luminous: MV ~ to -20 mag Extremely fast rise to maximum Fast optical decline (dust formation?) Spectra (almost) H-free, with narrow He I emissions and broad IME lines Pastorello+ 2008, MNRAS, 389, 113
9 An updated catalogue of SNe Ibn SN 1885A? (Ia-pec o Ibn? Pastorello+ 2008) SN 1999cq SN 2000er SN 2002ao SN 2005la (Ibn/IIn) SN 2006jc SN 2010al (Ibn/Ib) SN 2011hw (Ibn/IIn) PTF11rfh PS1-12sk (E-type galaxy) OGLE-2012-SN-006 (Ibn pec) LSQ12btw PTF12ldy iptf13beo LSQ13ccw (Ibn pec) SN 2014av iptf14aki/css140421: ASASSN-14dd OGLE-2014-SN-131 (Ibn pec) ASASSN-14ms (SL Ibn) ASASSN-15ed/PS15nk (Ibn/Ib) SN 2015G (Ibn/Ib) SN 2015U (reddened Ibn) iptf15ul (Ibn pec) iptf15akq (Ibn/IIn) PS15dpn SN 2016Q/PS16hy SN 2016cyj/ASASSN-16gn SN 2017ecp/ASASSN-17gi SN 2017fav/ATLAS17hrf (Ibn/IIn pec) SN 2017hyy/ASASSN-17os (Ibn/IIn pec) SN 2017iwp/Gaia17dgi (Ibn/IIn) SN 2017jfv/Gaia17dkl
10 SN Ibn variety: transitional Ibn/IIn events SN 2005la Pastorello+2008, MNRAS, 389, 131 Modjaz+ 2014, AJ, 147, 99 SN 2011hw Smith+ 2012, MNRAS, 426, 1905 Pastorello+ 2015, MNRAS, 449, 2921
11 SN Ibn variety: transitional Ibn/Ib events ASASSN-15ed Pastorello+ 2015b, 453, 3649
12 SN Ibn variety: transitional Ibn/Ib events SN 2015G Shivvers+ 2017, MNRAS, 471, 4381
13 SN Ibn photometric variety Broad light curve peak SN 2010al Pastorello+ 2015, MNRAS, 449, 2921
14 SN Ibn photometric variety Broad light curve peak OGLE-2014-SN-131 Karamehmetoglu+ 2017, A&A, 602, 93 With a 50d risetime!
15 SN Ibn photometric variety double-peak light curves iptf13beo Gorbikov+ 2014, MNRAS, 443, 671 SN 2011hw Pastorello+ 2015, MNRAS, 449, 2921
16 SN Ibn photometric variety slow-evolving late declines OGLE-2012-SN006 Pastorello+ 2015, MNRAS, 449, 1941
17 SN Ibn photometric variety fast-evolving light curves Highly reddened (Av > 1) Pastorello+ 2015, MNRAS, 454, 4293 Hosseinzadeh+ 2017, ApJ, 836, 158 SN 2015U Shivvers+ 2016, MNRAS, 461, 3057
18 SN Ibn photometric variety luminous lightcurve peak ASASSN-14ms Vallely et al. 2018, MNRAS, 475, 2344
19 hence, not so uniform... one heralded by an LBV-like ourburst (2006jc) transitioning to Type IIn SNe (2005la, 2011hw) transitioning to Type Ib (2010al, ASASN-15ed, 2015G) fast evolving (LSQ13ccw, iptf15ul, 2015U) slow-evolving at early phase (OGLE-2014-SN131) slow-evolving at late phases (OGLE-2012-SN-006) with double-peaked light curves (2011hw, iptf13beo) super-luminous (ASASSN-14ms, iptf15ul) one exploded in the outskirts of an E/S0 galaxy (PS1-12sk)
20 SN Ibn: photometric variety Pastorello+ 2016, MNRAS, 456, 853; See also Hosseinzadeh+ 2017, ApJ, 836, 158
21 SN Ibn: photometric variety SNe Ibn are more homogeneous than SNe IIn (Hosseinzadeh+ 2017, ApJ, 836, 158)
22 Type SN Ibn progenitors Methods: Characterization of the pre-sn wind SN site (progenitor, survived companion, local stellar population) Light curve modelling Suggestions are welcome
23 Line velocities Pastorello+ 2016, MNRAS, 456, 853 Immler+ 2008, ApJ, 674, L85
24 SN Ibn Progenitors What about SN 2006jc? MARRIED OR SINGLE LIFE? 1. High-velocity (10 3 km s -1 ) He rich pre-sn wind 2. Luminous Pre-SN outburst Single massive WR star that eruptively expelled He-rich CSM before core-collapse (Foley+ 2007, Pastorello+ 2007,Tominaga+ 2008) Binary: erupting LBV+exploding WR (Pastorello+ 2007, Nature, 447, 829) In either case, the progenitor of SN 2006jc was likely very massive Mej=4.9 M MZAMS 40 M Tominaga+ 2008, ApJ, 687, 1208
25 SN Ibn Progenitors SN 2006jc Location (Maund+ 2016, ApJ, 833, 128) A weak blue source detected in 3 bands at the SN location, (mags ) => MV ~ -5.6 No outbursts detected after the SN explosion No massive LBV companion (A-F supergiant with M < 10 M )
26 ASASSN-14ms SN Ibn Progenitors Pure radioactive decay (Mej<MNi! unphysical) Magnetar spin-down (Pin,spin=1 ms, Mej=3.3M ) CSM interaction model (with Mej=4.3M ; MCSM=0.5M ; 0.23 M of 56 Ni) => MZAMS>a few x10 M (host: 12+log(O/H) < 8.3) Vallely+ 2018, MNRAS, 475, 2344 SEE POSTER SECTION! OGLE-2014-SN-131 Fair fits with the (usual) magnetar, and CSM-interaction models; low-metallicity (SMC-like) host; MZAMS > 40 M Karamehmetoglu+ 2017, A&A, 602, 93
27 SN Ibn Progenitors From the non-detection of the progenitor in pre-sn HST images (MF555W > -6.4; MF814W > -7.1 mag) From the stellar environment analysis No pre-sn outbursts in ~20 yrs No single massive (>30 M ) star MZAMS < M in a binary system SN 2015G Shivvers+ 2017, 471, 4381
28 SN Ibn Progenitors In some cases, SNe Ibn are hardly reconciled with massive ejecta, e.g. some fast and furious SNe Ibn. Shivvers+ 2016, 461, 3057 Pastorello+ 2015, MNRAS, 449, 1954 SN 2015U, LSQ12btw, LSQ13ccw
29 SN Ibn variety Weird locations SNe Ibn are usually hosted in spiral galaxies/star-form. environments Sanders et al. 2013, ApJ, 769, 39 A SN Ibn apparently in a remote location of an early-type host! => an SN in a low-mass degenerate progenitor system? Alternatively, a dwarf host? => massive star precursor for PS1-12sk PS1-12sk
30 Conclusions SNe Ibn show a wide range of observational properties (in light curve shape, luminosity, spectral evolution, line profiles) Their peak luminosities span two orders of magnitude (10 42 to over10 44 erg s -1 ) From the CSM velocity (from the narrow line profiles) and the light curve modelling => different types of progenitor stars may produce SNe Ibn. SNe Ibn are rare: 5-6% of stripped-envelope SN discoveries; 2% of all CCSNe
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