Stellar forensics with the supernova‐GRB connection – Ludwig Biermann Award Lecture 2010

Modjaz, M.

doi:10.1002/asna.201111562

Cited by 64 publications

(67 citation statements)

References 171 publications

(177 reference statements)

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“…recent review of metallicity measurements of CC SNe and those SNe accompanying Long duration Gamma Ray Bursts (LGRBs), was also presented in Modjaz (2011).…”

Section: H II Region Metallicitiesmentioning

confidence: 99%

Statistical Studies of Supernova Environments

Anderson

James

Habergham

et al. 2015

Publ. Astron. Soc. Aust.

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Mapping the diversity of supernovae (SNe) to progenitor properties is key to our understanding of stellar evolution and explosive stellar death. Investigations of the immediate environments of SNe allow statistical constraints to be made on progenitor properties such as mass and metallicity. Here we review the progress that has been made in this field. Pixel statistics using tracers of e.g. star formation within galaxies show intriguing differences in the explosion sites of, in particular SNe types II and Ibc (SNe II and SNe Ibc respectively), suggesting statistical differences in population ages. Of particular interest is that SNe Ic are significantly more associated with host galaxy Hα emission than SNe Ib, implying shorter lifetimes for the former. In addition, such studies have shown (unexpectedly) that the interacting SNe IIn do not explode in regions containing the most massive stars, which suggests that at least a significant fraction of their progenitors arise from the lower end of the core-collapse SN mass range. Host H ii region spectroscopy has been obtained for a significant number of core-collapse events, however definitive conclusions on differences between distinct SN types have to-date been elusive. Single stellar evolution models predict that the relative fraction of SNe Ibc to SNe II should increase with increasing metallicity, due to the dependence of mass-loss rates on progenitor metallicity. We present a meta-analysis of all current host H ii region oxygen abundances for CC SNe. It is concluded that the SN II to SN Ibc ratio shows little variation with oxygen abundance, with only a suggestion that the ratio increases in the lowest bin. Radial distributions of different SNe are discussed, where a central excess of SNe Ibc has been observed within disturbed galaxy systems, which is difficult to ascribe to metallicity or selection effects. Environment studies are also being undertaken for SNe Ia, where constraints can be made on the shortest delay times of progenitor systems. It is shown that 'redder' SNe Ia are more often found within star-forming regions. Environment studies are evolving to enable studies at higher spatial resolutions than previously possible, while in addition the advent of widefield integral field unit instruments allows galaxy-wide spectral analyses which will provide fruitful results to this field. Some example contemporary results are shown in that direction.

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“…recent review of metallicity measurements of CC SNe and those SNe accompanying Long duration Gamma Ray Bursts (LGRBs), was also presented in Modjaz (2011).…”

Section: H II Region Metallicitiesmentioning

confidence: 99%

Statistical Studies of Supernova Environments

Anderson

James

Habergham

et al. 2015

Publ. Astron. Soc. Aust.

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“…Ry, 97.60.Bw, 98.70.Rz Long gamma-ray bursts (GRBs) are believed to originate from relativistic jets launched at the death of massive stars. Associations with core-collapse supernovae (CCSNe) have provided strong evidence for the GRB-CCSN relationship [1]. But, there remain many important questions.…”

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confidence: 99%

“…Associations with core-collapse supernovae (CCSNe) have provided strong evidence for the GRB-CCSN relationship [1]. But, there remain many important questions.…”

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confidence: 99%

TeV–PeV Neutrinos from Low-Power Gamma-Ray Burst Jets inside Stars

2013

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We study high-energy neutrino production in collimated jets inside progenitors of gamma-ray bursts (GRBs) and supernovae, considering both collimation and internal shocks. We obtain simple, useful constraints, using the often overlooked point that shock acceleration of particles is ineffective at radiation-mediated shocks. Classical GRBs may be too powerful to produce high-energy neutrinos inside stars, which is consistent with IceCube nondetections. We find that ultralong GRBs avoid such constraints and detecting the TeV signal will support giant progenitors. Predictions for lowpower GRB classes including low-luminosity GRBs can be consistent with the astrophysical neutrino background that IceCube may detect, with a spectral steepening around PeV. The models can be tested with future GRB monitors.PACS numbers: 95.85. Ry, 97.60.Bw, 98.70.Rz Long gamma-ray bursts (GRBs) are believed to originate from relativistic jets launched at the death of massive stars. Associations with core-collapse supernovae (CCSNe) have provided strong evidence for the GRB-CCSN relationship [1]. But, there remain many important questions. What makes the GRB-CCSN connection? How universal is it? What is the central engine and progenitor of GRBs? How are jets launched and accelerated? Observationally, it is not easy to probe physics inside a star with photons until the jet breaks out and the photons leave the system. This is always the case if the jet is "chocked" rather than "successful" [2]; that is, the jet stalls inside the star, where the electromagnetic signal is unobservable. Such failed GRBs may be much more common than GRBs (whose true rate is ∼ 10 −3 of that of all CCSNe), and CCSNe driven by mildly relativistic jets may make up a few present of all CCSNe [3][4][5].Recent observations suggest interesting diversity in the GRB population. "Low-power GRBs" such as lowluminosity (LL) GRBs [3,6,7] and ultralong (UL) GRBs [8,9] have longer durations (∼ 10 3 -10 4 s) compared to that of classical long GRBs, suggesting different GRB classes and larger progenitors. While they were largely missed in previous observations, they are important for the total energy budget and the GRB-CCSN connection.Neutrinos and gravitational waves (GWs) can present special opportunities to address the above issues. In particular, IceCube is powerful enough to see high-energy (HE) neutrinos at 1 TeV [10] and has reported the first detections of cosmic PeV neutrinos [11]. Efficient HE neutrino production inside a star has been proposed assuming shock acceleration of cosmic rays (CRs) [12][13][14], and investigated by a lot of authors, since their detection allows us to study the GRB-CCSN connection [13,15], joint searches with GWs [16], neutrino mixing including the matter effect [17], the nature of GRB progenitors [18] and so on. However, IceCube has not detected neutrinos from GRBs, putting limits on this scenario as well as the classical prompt emission scenario [19,20]. It also constrains orphan neutrinos from a CCSN [21].In this work, we consider HE ne...

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“…Specifically, massive stars at different metallicities are expected to live and die differently, due to the metallicity dependence of mass loss and its subsequent link to rotation and angular momentum content of the stellar core (e.g., Crowther 2007). Since the early work on GRB host metallicities and their comparison with SDSS galaxies as well as with SN galaxies, the field of environmental metallicity studies has experienced a tremendous growth (see discussions in e.g., Levesque et al 2010b;Modjaz 2011; and references therein, as well as contributions in this volume).…”

Section: Measured Metallicities At the Explosion Sites Of Sne Ib/c Wimentioning

confidence: 99%

“…For the last 15 years, the exciting connection between long GRBs and SNe Ic-bl, the only type of SNe observed accompanying long GRBs (for reviews, see Woosley & Bloom 2006;Hjorth & Bloom 2011;Modjaz 2011), and the existence of many more SNe Ic-bl without GRBs raises the question of what distinguishes SN-GRB progenitors from those of ordinary SNe Ic-bl without GRBs. Viewing angle effects are probably not the reason why SNe Ic-bl do not show an accompanied GRB (Soderberg et al 2006).…”

Section: Introductionmentioning

confidence: 99%

Type Ib/c Supernovae with and without Gamma-Ray Bursts

Modjaz¹

2011

Proc. IAU

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Abstract. While the connection between Long Gamma-Ray Bursts (GRBs) and Type Ib/c Supernovae (SNe Ib/c) from stripped stars has been well-established, one key outstanding question is what conditions and factors lead to each kind of explosion in massive stripped stars. One promising line of attack is to investigate what sets apart SNe Ib/c with GRBs from those without GRBs. Here, I briefly present two observational studies that probe the SN properties and the environmental metallicities of SNe Ib/c (specifically broad-lined SNe Ic) with and without GRBs. I present an analysis of expansion velocities based on published spectra and on the homogeneous spectroscopic CfA data set of over 70 SNe of Types IIb, Ib, Ic and Ic-bl, which triples the world supply of well-observed Stripped SNe. Moreover, I demonstrate that a metaanalysis of the three published SN 1b/c metallicity data sets when including only values at the SN positions to probe natal oxygen abundances, indicates at very high significance that indeed SNe Ic erupt from more metal-rich environments than SNe Ib, while SNe Ic-bl with GRBs still prefer, on average, more metal-poor sites than those without GRBs.

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Stellar forensics with the supernova‐GRB connection – Ludwig Biermann Award Lecture 2010

Cited by 64 publications

References 171 publications

Statistical Studies of Supernova Environments

Statistical Studies of Supernova Environments

TeV–PeV Neutrinos from Low-Power Gamma-Ray Burst Jets inside Stars

Type Ib/c Supernovae with and without Gamma-Ray Bursts

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