THE HIGH-METALLICITY EXPLOSION ENVIRONMENT OF THE RELATIVISTIC SUPERNOVA 2009bb

Levesque, Emily M.; Söderberg, A. M.; Foley, R. J.; Berger, E.; Kewley, Lisa J.; Chakraborti, Sayan; Ray, Alak; Torres, M. A. P.; Challis, P.; Kirshner, R.; Barthelmy, S. D.; Bietenholz, M. F.; Chandra, Poonam; Chaplin, V.; Chevalier, Roger A.; Чугай, Н. Н.; Connaughton, V.; Copete, A.; Fox, O.; Fransson, Claes; Grindlay, Jonathan E.; Hamuy, M.; Milne, Peter; Pignata, G.; Stritzinger, M. D.; Wieringa, M.

doi:10.1088/2041-8205/709/1/l26

Cited by 36 publications

(30 citation statements)

References 45 publications

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“…Similar connections between low metallicity environments and GRBs are also presented in Levesque et al [15] and Stanek et al [16]. An interesting potential counter example is the high metallicity host galaxy of the relativistic supernova 2009bb [17,18]. Also, recent work by Savaglio et al [19] suggests that the low metallicity connection may be a selection effect since small metal poor galaxies are the most common galaxies in the universe but they are optically faint and thus only studied because they are host galaxies.…”

Section: Introductionsupporting

confidence: 76%

The identification and investigation of gamma-ray burst progenitors: A spectropolarimetric survey of Wolf-Rayet stars in the milky way and M33

Williams¹,

Smith

Schmidt

2012

AIP Conference Proceedings

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There is now irrefutable observational evidence that long duration gamma-ray bursts (GRBs) are linked to Type Ic core collapse supernovae (SNe Ic). This association has resulted in a wide acceptance of the collapsar model to explain the origin of GRBs. The collapsar model requires three physical characteristics: 1.) a massive core, 2.) a hydrogen free stripped envelope, and 3.) rapid rotation. These three characteristics are present in a rapidly rotating Wolf-Rayet (WR) star.We are conducting a spectropolarimetric survey of WR stars in the Milky Way and M33 using the CCD Imaging/Spectropolarimeter (SPOL) at the 1.6-m Kuiper, 2.3-m Bok and 6.5-m MMT telescopes. The objective of this work is to identify rapidly rotating WR stars and to study them as potential progenitors of long-duration GRBs. The identification is performed using spectropolarimetry to probe asymmetries in the structure of the mass loss envelopes. We will present results from our Galactic survey and provide motivation for and the initial results from a follow-up study of lower metallicity M33 WR stars.

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Section: Introductionsupporting

confidence: 76%

The identification and investigation of gamma-ray burst progenitors: A spectropolarimetric survey of Wolf-Rayet stars in the milky way and M33

Williams¹,

Smith

Schmidt

2012

AIP Conference Proceedings

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“…Apparently supporting this model, Stanek et al (2006) found that the isotropic prompt energy release of the GRB-SNe decreases steeply with metallicity, and other surveys have found observational evidence for the preferential occurrence of GRB-SNe in low-metallicity host galaxies (Fynbo et al 2003;Prochaska et al 2004;Sollerman et al 2005;Modjaz et al 2006;Wiersema et al 2007;Christensen et al 2008;Modjaz et al 2008;Levesque et al 2010a;Chornock et al 2010;Starling et al 2011). Challenging this view is the recent discovery of SN 2009bb, a broad-lined, engine-driven SN Ic found in a high-metallicity host environment (Soderberg et al 2010;Levesque et al 2010d;Pignata et al 2011). In SN 2010ay, we have found the opposite case-a broad-lined SN Ic found in a low-metallicity host environment, but without any indication (via either radio or gamma-ray emission) of a central engine.…”

Section: Discussionmentioning

confidence: 95%

“…First, there are two reported long-duration GRBs in solar or super-solar metallicity environments (GRB 020819, Levesque et al 2010c;GRB 051022, Graham et al 2009). Similarly, the luminous radio emission seen from SN Ic-BL 2009bb pointed unequivocally to the production of copious relativistic ejecta resembling a GRB afterglow (Soderberg et al 2010), while the explosion environment was characterized by a super-solar metallicity, Z ∼ 1-2 Z (Levesque et al 2010b). Together with the growing lack of evidence for massive progenitor stars for SNe Ic in pre-explosion Hubble Space Telescope images (Smartt 2009), a lower mass (M ∼ 10-20 M ) binary progenitor system model (with a gentler metallicity dependence) is gaining increasing popularity (Yoon et al 2010).…”

Section: Introductionmentioning

confidence: 93%

SN 2010ay IS A LUMINOUS AND BROAD-LINED TYPE Ic SUPERNOVA WITHIN A LOW-METALLICITY HOST GALAXY

Sanders¹,

Söderberg²,

Valenti³

et al. 2012

ApJ

Self Cite

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We report on our serendipitous pre-discovery detection and follow-up observations of the broad-lined Type Ic supernova (SN Ic) 2010ay at z = 0.067 imaged by the Pan-STARRS1 3π survey just ∼4 days after explosion. The supernova (SN) had a peak luminosity, M R ≈ −20.2 mag, significantly more luminous than known GRB-SNe and one of the most luminous SNe Ib/c ever discovered. The absorption velocity of SN 2010ay is v Si ≈ 19 × 10 3 km s −1at ∼40 days after explosion, 2-5 times higher than other broad-lined SNe and similar to the GRB-SN 2010bh at comparable epochs. Moreover, the velocity declines ∼2 times slower than other SNe Ic-BL and GRB-SNe. Assuming that the optical emission is powered by radioactive decay, the peak magnitude implies the synthesis of an unusually large mass of 56 Ni, M Ni = 0.9 M . Applying scaling relations to the light curve, we estimate a total ejecta mass, M ej ≈ 4.7 M , and total kinetic energy, E K ≈ 11 × 10 51 erg. The ratio of M Ni to M ej is ∼2 times as large for SN 2010ay as typical GRB-SNe and may suggest an additional energy reservoir. The metallicity (log(O/H) PP04 + 12 = 8.19) of the explosion site within the host galaxy places SN 2010ay in the low-metallicity regime populated by GRB-SNe, and ∼0.5(0.2) dex lower than that typically measured for the host environments of normal (broad-lined) SNe Ic. We constrain any gamma-ray emission with E γ 6 × 10 48 erg (25-150 keV), and our deep radio follow-up observations with the Expanded Very Large Array rule out relativistic ejecta with energy E 10 48 erg. We therefore rule out the association of a relativistic outflow like those that accompanied SN 1998bw and traditional long-duration gamma-ray bursts (GRBs), but we place less-stringent constraints on a weak afterglow like that seen from XRF 060218. If this SN did not harbor a GRB, these observations challenge the importance of progenitor metallicity for the production of relativistic ejecta and suggest that other parameters also play a key role.

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“…However, this sample can be further enlarged if we also consider those measurements computed with the PP04 N2 calibrator, and converted into O3N2 scale using the relation produced by Kewley & Ellison (2008). In this enlarged sample we used data from Stoll et al (2013), Sahu et al (2009), Levesque et al (2010), Milisavljevic et al (2013), Inserra et al (2013), Van Dyk et al (2012), Taddia et al (2013Taddia et al ( , 2015. We also added the metallicities of the SN Ia hosts Compilation of the oxygen abundances at the SN location measured in this work combined with previously published results from the literature.…”

Section: Differences Among Sn Subtypesmentioning

confidence: 99%

Nearby supernova host galaxies from the CALIFA survey

Galbany

Stanishev²,

Mourão³

et al. 2016

A&A

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The metallicity of a supernova progenitor, together with its mass, is one of the main parameters that can rule the progenitor's fate. We present the second study of nearby supernova (SN) host galaxies (0.005 < z < 0.03) using integral field spectroscopy (IFS) from the CALIFA survey. We analyze the metallicity of 115 galaxies, which hosted 132 SNe within and 10 SNe outside the field of view (FoV) of the instrument. Another 18 galaxies, which hosted only SNe outside the FoV, were also studied. Using the O3N2 calibrator that was described elsewhere, we found no statistically significant differences between the gas-phase metallicities at the locations of the three main SN types -Ia, Ib/c and II; they all have 12 + log (O/H) 8.50 within 0.02 dex. The total galaxy metallicities are also very similar, and we argue that the reason is that our sample only consists of SNe discovered in massive galaxies (log(M/M ) > 10 dex) by targeted searches. We neither found evidence that the metallicity at the SN location differs from the average metallicity at the galactocentric distance of the SNe. By extending our SN sample with published metallicities at the SN location, we are able to study the metallicity distributions for all SN subtypes split into SN discovered in targeted and untargeted searches. We confirm a bias toward higher host masses and metallicities in the targeted searches. By combining data from targeted and untargeted searches, we found a sequence from higher to lower local metallicity: SN Ia, Ic, and II show the highest metallicity, which is significantly higher than those of SN Ib, IIb, and Ic-BL. Our results support the scenario according to which SN Ib result from binary progenitors. Additionally, at least part of the SN Ic are the result of single massive stars that were stripped of their outer layers by metallicity-driven winds. We studied several proxies of the local metallicity that are frequently used in the literature and found that the total host metallicity allows estimating the metallicity at the SN location with an accuracy better than 0.08 dex and very small bias. In addition, weak AGNs that cannot be seen in the total spectrum may weakly bias (by 0.04 dex) the metallicity estimate that is derived from the galaxy-integrated spectrum.

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THE HIGH-METALLICITY EXPLOSION ENVIRONMENT OF THE RELATIVISTIC SUPERNOVA 2009bb

Cited by 36 publications

References 45 publications

The identification and investigation of gamma-ray burst progenitors: A spectropolarimetric survey of Wolf-Rayet stars in the milky way and M33

The identification and investigation of gamma-ray burst progenitors: A spectropolarimetric survey of Wolf-Rayet stars in the milky way and M33

SN 2010ay IS A LUMINOUS AND BROAD-LINED TYPE Ic SUPERNOVA WITHIN A LOW-METALLICITY HOST GALAXY

Nearby supernova host galaxies from the CALIFA survey

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