SN 1961V - an extragalactic ETA Carinae analog

Goodrich, Robert W.; Stringfellow, Guy S.; Penrod, G. D.; Filippenko, A. V.

doi:10.1086/167646

Cited by 83 publications

(141 citation statements)

References 0 publications

Supporting

Mentioning

135

Contrasting

Order By: Relevance

“…We note that an alternative distance estimate based on the Tully-Fisher relation has also been reported (10.6±1.3 Mpc; Terry et al 2002). The galaxy of SN 2007gr also hosted two prior supernovae, SN 1969L (A V = 0.17; Burstein & Heiles 1984) and SN 1961V (A V ∼ 2.2−4.1; Filippenko et al 1995a) with the latter possibly being the outburst of a luminous blue variable (Goodrich et al 1989).…”

Section: Sn 2007grsupporting

confidence: 50%

Extensive optical and near-infrared observations of the nearby, narrow-lined type Ic SN 2007gr: days 5 to 415

Hunter

Valenti

Kotak

et al. 2009

A&A

122

100

View full text Add to dashboard Cite

We present photometric and spectroscopic observations at optical and near-infrared wavelengths of the nearby type Ic supernova 2007gr. These represent the most extensive data-set to date of any supernova of this sub-type, with frequent coverage from shortly after discovery to more than one year post-explosion. We deduce a rise time to B-band maximum of 11.5 ± 2.7 d. We find a peak B-band magnitude of M B = −16.8, and light curves which are remarkably similar to the so-called "hypernova" SN 2002ap. In contrast, the spectra of SNe 2007gr and 2002ap show marked differences, not least in their respective expansion velocities. We attribute these differences primarily to the density profiles of their progenitor stars at the time of explosion i.e. a more compact star for SN 2007gr compared to SN 2002ap. From the quasi-bolometric light curve of SN 2007gr, we estimate that 0.076 ± 0.010 M of 56 Ni was produced in the explosion. Our near-infrared (IR) spectra clearly show the onset and disappearance of the first overtone of carbon monoxide (CO) between ∼70 to 175 d relative to B-band maximum. The detection of the CO molecule implies that ionised He was not microscopically mixed within the carbon/oxygen layers. From the optical spectra, near-IR light curves, and colour evolution, we find no evidence for dust condensation in the ejecta out to about +400 d. Given the combination of unprecedented temporal coverage, and high signal-to-noise data, we suggest that SN 2007gr could be used as a template object for supernovae of this sub-class.

show abstract

Section: Sn 2007grsupporting

confidence: 50%

Extensive optical and near-infrared observations of the nearby, narrow-lined type Ic SN 2007gr: days 5 to 415

Hunter

Valenti

Kotak

et al. 2009

A&A

122

100

View full text Add to dashboard Cite

show abstract

“…Indeed, other than the Smartt et al studies, progenitor masses for SNe II-P are virtually unconstrained by direct observation. 7 Although the progenitors of SN 1961V (Goodrich et al 1989;Filippenko et al 1995;Van Dyk, Filippenko, & Li 2002), SN 1978K (Ryder et al 1993), SN 1987A (e.g., White & Malin 1987;Walborn et al 1987), SN 1993J (Filippenko 1993;Aldering, Humphreys, & Richmond 1994;Cohen, Darling, & Porter 1995), and SN 1997bs (Van Dyk et al 1999a) have been identified, all of these SNe II were peculiar.…”

Section: Introductionmentioning

confidence: 99%

A Study of the Type II-Plateau Supernova 1999[CLC]gi[/CLC] and the Distance to its Host Galaxy, NGC 3184

Leonard

Filippenko

et al. 2002

The Astronomical Journal

Self Cite

151

View full text Add to dashboard Cite

We present optical spectra and photometry sampling the first 6 months after discovery of supernova (SN) 1999gi in NGC 3184. SN 1999gi is shown to be a Type II-plateau event with a photometric plateau lasting until about 100 days after discovery. Using the expanding photosphere method (EPM), we derive a distance to SN 1999gi of 11:1 þ2:0 À1:8 Mpc and an explosion date of 1999 December 5:8 þ3:0 À3:1 , or 4:1 þ3:0 À3:1 days prior to discovery. This distance is consistent with a Tully-Fisher distance recently derived to NGC 3184 (D % 11.59 Mpc), but it is somewhat closer than the Cepheid distances recently derived to two galaxies that have generally been assumed to be associated with the group containing NGC 3184 (NGC 3319, D = 13.30 AE 0.55 Mpc, and NGC 3198, D = 13.80 AE 0.51 Mpc). From many lines of evidence, we conclude that SN 1999gi is only minimally reddened. A comparison between the color of SN 1999gi at early times and that of an infinitely hot blackbody restricts the reddening to E(BÀV ) < 0.45 mag, while a comparison between the color evolution of SN 1999gi and the well-observed (and extensively modeled) Type II-P SN 1999em implies an even more restrictive upper reddening limit of E(BÀV ) < 0.3 mag. A variety of other, independent reddening estimates are consistent with these upper limits and yield a probable reddening of E(BÀV ) = 0.21 AE 0.09 mag. We reconsider the upper mass limit (9 þ3 À2 M ) recently placed on the progenitor star of SN 1999gi by Smartt et al. in light of these results. Following the same procedures, but using the new data presented here, we arrive at a less restrictive upper mass limit of 15 þ5 À3 M for the progenitor. The increased upper limit results mainly from the larger distance derived through the EPM than was assumed by the Smartt et al. analyses, which relied on less precise (and less recent) distance measurements to NGC 3184. Finally, we confirm the existence of '' complicated '' P Cygni line profiles in early-time and later photospheric-phase spectra of SN 1999gi. These features, first identified by Baron et al. in spectra of SN 1999em as high-velocity absorptions, in addition to the '' normal '' lower velocity component, are here verified to be true P Cygni profiles consisting of both an absorption trough and an emission peak at early times. In the earliest spectrum, taken less than a day after discovery, the features extend out to nearly À30,000 km s À1 , indicating the existence of very high velocity material in the outer envelope of SN 1999gi.

show abstract

“…It then rapidly declined about three magnitudes. It now has the spectrum of an M-type supergiant and a large infrared excess (Humphreys, Jones & Gehrz 1987 in NGC 1058 (Goodrich et al 1989;Filippenko et al 1995;van Dyk et al 2002)), V12 in NGO 2403 (SN 1954j, Tammann & Sandage 1968, and VI in NGC 2363…”

Section: Impostors In the H-r Diagram?mentioning

confidence: 99%

Luminous Blue Variables, cool hypergiants and some impostors in the H-R diagram

Humphreys¹

2003

Symp. - Int. Astron. Union

View full text Add to dashboard Cite

Abstract. Current observations of the S Dor/LBVs and candidates and the implications for their important role in massive star evolution are reviewed. Recent observations of the cool hypergiants are altering our ideas about their evolutionary state, their atmospheres and winds, and the possible mechanisms for their asymmetric high mass loss episodes which may involve surface activity and magnetic fields. Recent results for IRC+I0420, peas and VYC:rvla are highlighted. S Dor/LBVs in eruption, and the cool hypergiants in their high mass loss phases with their optically thick winds are not what their apparent spectra and temperatures imply; they are then 'impostors' on the H-R diagram. The importance of the very most massive stars, like 'f/ Carinae and the 'supernovae impostors' are also discussed.

show abstract

SN 1961V - an extragalactic ETA Carinae analog

Cited by 83 publications

References 0 publications

Extensive optical and near-infrared observations of the nearby, narrow-lined type Ic SN 2007gr: days 5 to 415

Extensive optical and near-infrared observations of the nearby, narrow-lined type Ic SN 2007gr: days 5 to 415

A Study of the Type II-Plateau Supernova 1999[CLC]gi[/CLC] and the Distance to its Host Galaxy, NGC 3184

Luminous Blue Variables, cool hypergiants and some impostors in the H-R diagram

Contact Info

Product

Resources

About