INTERACTION BETWEEN THE BROAD-LINED TYPE Ic SUPERNOVA 2012ap AND CARRIERS OF DIFFUSE INTERSTELLAR BANDS

Milisavljevic, Dan; Margutti, R.; Crabtree, Kyle N.; Foster, Jonathan B.; Söderberg, A. M.; Fesen, Robert A.; Parrent, J.; Sanders, Nathan; Drout, M. R.; Kamble, A.; Chakraborti, Sayan; Pickering, T. E.; Cenko, S. Bradley; Silverman, J. M.; Filippenko, A. V.; Kirshner, R.; Mazzali, P. A.; Maeda, Keiichi; Marion, G. H.; Vinkó, J.; Wheeler, J. C.

doi:10.1088/2041-8205/782/1/l5

Cited by 22 publications

(29 citation statements)

References 41 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…One might thus infer a special fragility of its likely cation carriers. This could be confirmed by its early destruction in SN 2012ap (Milisavljevic et al 2014). We also note the extreme behaviour of the 5797 Å DIB in the sight line of SN 2014J in M82 .…”

Section: Interstellar Environment Dibs and Fullerenessupporting

confidence: 69%

Interstellar fullerene compounds and diffuse interstellar bands

Omont

2016

A&A

100

103

View full text Add to dashboard Cite

Recently, the presence of fullerenes in the interstellar medium (ISM) has been confirmed and new findings suggest that these fullerenes may possibly form from polycyclic aromatic hydrocarbons (PAHs) in the ISM. Moreover, the first confirmed identification of two strong diffuse interstellar bands (DIBs) with the fullerene, C + 60 , connects the long standing suggestion that various fullerenes could be DIB carriers. These new discoveries justify reassessing the overall importance of interstellar fullerene compounds, including fullerenes of various sizes with endohedral or exohedral inclusions and heterofullerenes (EEHFs). The phenomenology of fullerene compounds is complex. In addition to fullerene formation in grain shattering, fullerene formation from fully dehydrogenated PAHs in diffuse interstellar clouds could perhaps transform a significant percentage of the tail of low-mass PAH distribution into fullerenes including EEHFs. But many uncertain processes make it extremely difficult to assess their expected abundance, composition and size distribution, except for the substantial abundance measured for C + 60 . EEHFs share many properties with pure fullerenes, such as C 60 , as regards stability, formation/destruction and chemical processes, as well as many basic spectral features. Because DIBs are ubiquitous in all lines of sight in the ISM, we address several questions about the interstellar importance of various EEHFs, especially as possible carriers of diffuse interstellar bands. Specifically, we discuss basic interstellar properties and the likely contributions of fullerenes of various sizes and their charged counterparts such as C + 60 , and then in turn: 1) metallofullerenes; 2) heterofullerenes; 3) fulleranes; 4) fullerene-PAH compounds; 5) H 2 @C 60 . From this reassessment of the literature and from combining it with known DIB line identifications, we conclude that the general landscape of interstellar fullerene compounds is probably much richer than heretofore realized. EEHFs, together with pure fullerenes of various sizes, have many properties necessary to be suitably carriers of DIBs: carbonaceous nature; stability and resilience in the harsh conditions of the ISM; existing with various heteroatoms and ionization states; relatively easy formation; few stable isomers; spectral lines in the right spectral range; various and complex energy internal conversion; rich Jahn-Teller fine structure. This is supported by the first identification of a DIB carrier as C + 60 . Unfortunately, the lack of any precise information about the complex optical spectra of EEHFs and most pure fullerenes other than C 60 and about their interstellar abundances still precludes definitive assessment of the importance of fullerene compounds as DIB carriers. Their compounds could significantly contribute to DIBs, but it still seems difficult that they are the only important DIB carriers. Regardless, DIBs appear as the most promising way of tracing the interstellar abundances of various fullerene compounds if the breakthr...

show abstract

Section: Interstellar Environment Dibs and Fullerenessupporting

confidence: 69%

Interstellar fullerene compounds and diffuse interstellar bands

Omont

2016

A&A

100

103

View full text Add to dashboard Cite

show abstract

“…The doublet is far weaker in the Galactic foreground, consistent with the assumed low reddening from this contribution. We have also indicated in Figure 6 the presumed location from the host galaxy of the diffuse interstellar band (DIB) feature at 5780 Å, the strength of which can be used to infer visual extinction A V (Phillips et al 2013) and which can change over time in a subset of SNe Ib/c (Milisavljevic et al 2014). …”

Section: Spectroscopymentioning

confidence: 99%

SN 2017ein and the Possible First Identification of a Type Ic Supernova Progenitor

Dyk

Zheng

Brink

et al. 2018

ApJ

Self Cite

View full text Add to dashboard Cite

We have identified a progenitor candidate in archival Hubble Space Telescope (HST) images for the Type Ic supernova (SN Ic) SN 2017ein in NGC 3938, pinpointing the candidate's location via HST Target of Opportunity imaging of the SN itself. This would be the first identification of a stellar-like object as a progenitor candidate for any SN Ic to date. We also present observations of SN 2017ein during the first ∼49 days since explosion. We find that SN 2017ein most resembles the well-studied SN Ic SN 2007gr. We infer that SN 2017ein experienced a total visual extinction of A V ≈1.0-1.9 mag, predominantly because of dust within the host galaxy. Although the distance is not well known, if this object is the progenitor, it was likely of high initial mass, ∼47-48 M e if a single star, or ∼60-80 M e if in a binary system. However, we also find that the progenitor candidate could be a very blue and young compact cluster, further implying a very massive (>65 M e ) progenitor. Furthermore, the actual progenitor might not be associated with the candidate at all and could be far less massive. From the immediate stellar environment, we find possible evidence for three different populations; if the SN progenitor was a member of the youngest population, this would be consistent with an initial mass of ∼57 M e . After it has faded, the SN should be reobserved at high spatial resolution and sensitivity, to determine whether the candidate is indeed the progenitor.

show abstract

“…Temporal evolution of these lines could signify changes in ionization balance induced by the SN radiation field as shown for Na i D (Patat et al 2007;Blondin et al 2009;Simon et al 2009;Sternberg et al 2014), for K i (Graham et al 2015) and possibly for DIBs as well (Milisavljevic et al 2014). We investigate this by analyzing the temporal evolution of the pEW of these lines.…”

Section: Narrow Absorption Features Of Intervening Materialsmentioning

confidence: 95%

Supernova 2010ev: A reddened high velocity gradient type Ia supernova

Gutiérrez

González–Gaitán

Folatelli

et al. 2016

A&A

View full text Add to dashboard Cite

Aims. We present and study the spectroscopic and photometric evolution of the type Ia supernova (SN Ia) 2010ev.Methods. We obtain and analyze multiband optical light curves and optical/near-infrared spectroscopy at low and medium resolution spanning −7 days to +300 days from the B-band maximum.Results. A photometric analysis shows that SN 2010ev is a SN Ia of normal brightness with a light-curve shape of ∆m 15 (B) = 1.12 ± 0.02 and a stretch s = 0.94 ± 0.01 suffering significant reddening. From photometric and spectroscopic analysis, we deduce a color excess of E(B − V) = 0.25 ± 0.05 and a reddening law of R v = 1.54 ± 0.65. Spectroscopically, SN 2010ev belongs to the broad-line SN Ia group, showing stronger than average Si ii λ6355 absorption features. We also find that SN 2010ev is a high velocity gradient SN withv Si = 164 ± 7 km s

show abstract

INTERACTION BETWEEN THE BROAD-LINED TYPE Ic SUPERNOVA 2012ap AND CARRIERS OF DIFFUSE INTERSTELLAR BANDS

Cited by 22 publications

References 41 publications

Interstellar fullerene compounds and diffuse interstellar bands

Interstellar fullerene compounds and diffuse interstellar bands

SN 2017ein and the Possible First Identification of a Type Ic Supernova Progenitor

Supernova 2010ev: A reddened high velocity gradient type Ia supernova

Contact Info

Product

Resources

About