The Standard Candle Method for Type II Supernovae and the Hubble Constant

Hamuy, M.

doi:10.1017/s0252921100009635

Cited by 5 publications

(8 citation statements)

References 11 publications

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“…Due to the similarities between SN 2003gd and SN 1999em we take the weighted average of three independent measurements of v50 for SN 1999em and adopt this for SN 2003gd. The independent measurements are from Hamuy et al (2001), Leonard et al (2002a) and this paper, giving an adopted value of v50 = 3694 ± 981 km s −1 for SN 2003gd, where the error is the standard deviation of v50 in the sample of 22 SNe II-P from Hamuy (2004b). The two extreme SNe, 1992am and 1999br, were excluded in this standard deviation calculation due to their peculiarities.…”

Section: Distance Estimates To M74mentioning

confidence: 99%

“…We measured the expansion velocity of the ejecta of SN 2003gd from the minimum of the blue-shifted absorption trough of the Fe ii λ5169 line, as in Hamuy (2004b). This absorption line is asymmetric and shows signs of blending, possibly with Ti ii and Mg i λ5167 .…”

Section: Expansion Velocity Of Sn 2003gdmentioning

confidence: 99%

“…Hamuy in two further papers (Hamuy 2004a,b) firstly confirmed the SCM using a sample of 24 SNe II-P and then calibrated the Hubble diagram with known Cepheid distances to four of these supernovae. Hamuy (2004b) calculated the Hubble constant, using V and I data, to be H0(V ) = 75 ± 7 km s −1 Mpc −1 and H0(I) = 65 ± 12 km s −1 Mpc −1 . In this paper we use the weighted average of these results, H0 = 72 ± 6 km s −1 Mpc −1 , which is comparable to H0 = 71 ± 2 km s −1 Mpc −1 derived as part of the HST Key Project using SNe Ia (Freedman et al 2001).…”

Section: Distance Estimates To M74mentioning

confidence: 99%

“…The apparent magnitudes for SN 2003gd at day 50 were estimated using ∆m from the χ 2 -fitting results (Table 4) and V50 and I50 magnitudes for SN 1999em (Hamuy 2004b), giving V50 = 13.97 ± 0.50 and I50 = 13.27 ± 0.52 for SN 2003gd. The errors adopted are the following errors combined in quadrature:…”

Section: Distance Estimates To M74mentioning

confidence: 99%

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A study of the Type II-P supernova 2003gd in M74

Hendry

Smartt

Maund

et al. 2005

Monthly Notices of the Royal Astronomical Society

109

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We present photometric and spectroscopic data of the Type II‐P supernova (SN II‐P) 2003gd, which was discovered in M74 close to the end of its plateau phase. SN 2003gd is the first Type II supernova (SN) to have a directly confirmed red supergiant (RSG) progenitor. We compare SN 2003gd to SN 1999em, a similar SN II‐P, and estimate an explosion date of 2003 March 18. We determine a reddening towards the SN of E(B−V) = 0.14 ± 0.06, using three different methods. We also calculate three new distances to M74 of 9.6 ± 2.8, 7.7 ± 1.7 and 9.6 ± 2.2 Mpc. The former was estimated using the standard candle method (SCM), for Type II supernovae (SNe II), and the latter two using the brightest supergiants method (BSM). When combined with existing kinematic and BSM distance estimates, we derive a mean value of 9.3 ± 1.8 Mpc. SN 2003gd was found to have a lower tail luminosity compared with other normal Type II‐P supernovae (SNe II‐P) bringing into question the nature of this SN. We present a discussion concluding that this is a normal SN II‐P, which is consistent with the observed progenitor mass of 8+4−2 M⊙.

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Section: Distance Estimates To M74mentioning

confidence: 99%

Section: Expansion Velocity Of Sn 2003gdmentioning

confidence: 99%

Section: Distance Estimates To M74mentioning

confidence: 99%

Section: Distance Estimates To M74mentioning

confidence: 99%

See 2 more Smart Citations

A study of the Type II-P supernova 2003gd in M74

Hendry

Smartt

Maund

et al. 2005

Monthly Notices of the Royal Astronomical Society

109

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“…However, an estimate of the absorption is needed, and this is usually a thorny problem when dealing with SNe. The problem was faced by Hamuy (2003), where the absorption was estimated on the basis of observed (V − I) colors. Indeed, when it is assumed that the intrinsic end-of-the-plateau (V − I) color is the same for all the type IIP SNe and it is a function of the photospheric temperature only, a possible (V − I) color excess is due to the host galaxy extinction.…”

Section: Current Calibrations: An Overviewmentioning

confidence: 99%

Astronomical Distance Determination in the Space Age

et al. 2018

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The formal division of the distance indicators into primary and secondary leads to difficulties in description of methods which can actually be used in two ways: with, and without the support of the other methods for scaling. Thus instead of concentrating on the scaling requirement we concentrate on all methods of distance determination to extragalactic sources which are designated, at least formally, to use for individual sources. Among those, the Supernovae Ia is clearly the leader due to its enormous success in determina- tion of the expansion rate of the Universe. However, new methods are rapidly developing, and there is also a progress in more traditional methods. We give a general overview of the methods but we mostly concentrate on the most recent developments in each field, and future expectations.

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Cosmology with Type IIP Supernovae

Nugent¹,

Hamuy²

2016

Handbook of Supernovae

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We show how dense compact discrete shells of circumstellar gas immediately outside the red supergiants affect the optical light curves of type II-P/II-L SNe taking the example of SN 2013ej. The earlier efforts in the literature had used an artificial circumstellar medium (CSM) stitched to the surface of an evolved star which had not gone through a phase of late-stage heavy mass loss, which in essence, is the source of the CSM to begin with. In contrast we allow enhanced mass loss rate from the modeled star during the 16 O and 28 Si burning stages and construct the CSM from the resulting mass-loss history in a self-consistent way. Once such evolved pre-SN stars are exploded, we find that the models with early interaction between the shock and the dense CSM reproduce the light curves far better than those without that mass loss and hence having no dense, nearby CSM. The required explosion energy for the progenitors with a dense CSM is reduced by almost a factor of two compared to those without the CSM. Our model, with a more realistic CSM profile and presupernova and explosion parameters, fits observed data much better throughout the rise, plateau and radioactive tail phases compared to previous studies. This points to an intermediate class of supernovae between type II-P/II-L and type II-n SNe with the characteristics of simultaneous UV and optical peak, slow decline after peak and a longer plateau.

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The Standard Candle Method for Type II Supernovae and the Hubble Constant

Cited by 5 publications

References 11 publications

A study of the Type II-P supernova 2003gd in M74

A study of the Type II-P supernova 2003gd in M74

Astronomical Distance Determination in the Space Age

Cosmology with Type IIP Supernovae

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