Distances to extragalactic supernovae

Kirshner, R.; Kwan, John

doi:10.1086/153123

Cited by 274 publications

(213 citation statements)

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“…The expanding photosphere method (EPM) is a geometric distance measurement method that relates the angular size of the SN ejecta to its physical radius derived from the observed expansion velocity of the SN assuming homologous expansion (Kirshner & Kwan 1974;Dessart & Hillier 2005b). The angular radius of the photosphere in a homologously expanding ejecta is defined as…”

Section: Expanding Photosphere Methodsmentioning

confidence: 99%

Improved distance determination to M 51 from supernovae 2011dh and 2005cs

Vinkó

Takáts

Szalai

et al. 2012

A&A

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Aims. The appearance of two recent supernovae, SN 2011dh and 2005cs, both in M 51, provides an opportunity to derive an improved distance to their host galaxy by combining the observations of both SNe. Methods. We apply the Expanding Photosphere Method to get the distance to M 51 by fitting the data of these two SNe simultaneously. In order to correct for the effect of flux dilution, we use correction factors (ζ) appropriate for standard type II-P SNe atmospheres for 2005cs, but find ζ ∼ 1 for the type IIb SN 2011dh, which may be due to the reduced H-content of its ejecta. Results. The EPM analysis resulted in D M 51 = 8.4 ± 0.7 Mpc. Based on this improved distance, we also re-analyze the HST observations of the proposed progenitor of SN 2011dh. We confirm that the object detected on the pre-explosion HST-images is unlikely to be a compact stellar cluster. In addition, its derived radius (∼277 R ) is too large for being the real (exploded) progenitor of SN 2011dh. Conclusions. The supernova-based distance, D = 8.4 Mpc, is in good agreement with other recent distance estimates to M 51.

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Section: Expanding Photosphere Methodsmentioning

confidence: 99%

Improved distance determination to M 51 from supernovae 2011dh and 2005cs

Vinkó

Takáts

Szalai

et al. 2012

A&A

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“…THE EPM APPLIED TO SN 1999gi To derive the EPM distance to SN 1999gi we follow the procedure detailed by L02. Briefly, an EPM distance is calculated by comparing the linear radius of the expanding supernova photosphere, R, with the photosphere's angular size, h, to derive the distance to the SN, D (Kirshner & Kwan 1974). The radial velocity of the expanding photosphere, v, is found from the Doppler shifting of the spectral lines, so that R = v(t À t 0 ), where (t À t 0 ) is the time since explosion and the SN is assumed to be in free expansion.…”

Section: The Reddening Of Sn 1999gimentioning

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

151

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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.

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“…Rather than worry about what determines the properties of the atmosphere, one can use observed spectra to infer the properties, and then compute the luminosity. Early, primitive applications of this approach to SN Ia luminosities (Branch & Patchett 1973;Kirshner & Kwan 1974;Branch 1979) were referred to as the Baade, or Baade-Wesselink, method. For Type II Supernovae, this was succeeded by the more advanced Expanding Photosphere Method (Eastman & Kirshner 1989, Schmidt, Kirshner, & Eastman 1992.…”

Section: Physical Calibrationsmentioning

confidence: 99%

Type Ia Supernovae as Extragalactic Distance Indicators

Branch

Nugent

Fisher

1997

Thermonuclear Supernovae

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Abstract. Because Type Ia supernovae (SNe Ia) are not perfect standard candles, it is important to be able to use distance-independent observables (DIOs) to define subsets of SNe Ia that are "nearly standard candles" or to correct SN Ia absolute magnitudes to make them nearly homogeneous ("standardized candles"). This is not crucial for the measurement of H 0 , but it is for the measurement of q 0 and of parent-galaxy peculiar velocities. We discuss the use of various photometric and spectroscopic SN Ia DIOs, and a parent-galaxy DIO, for this purpose. We also discuss the status of the absolute-magnitude calibration of SNe Ia. We find that SNe Ia, whether calibrated by means of (1) Cepheids in their parent galaxies, (2) fitting their optical-ultraviolet spectra with detailed non-LTE model atmosphere calculations, or (3) by considering that the light curve is powered by the decay of radioactive 56 Ni, firmly indicate that the value of H 0 is low, less than or about 60 km s −1 Mpc −1 . Some issues regarding the determination of q 0 by means of SNe Ia are discussed briefly. Finally, we conjecture that even if q 0 =0.5, there probably is no cosmic age problem.

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Distances to extragalactic supernovae

Cited by 274 publications

References 0 publications

Improved distance determination to M 51 from supernovae 2011dh and 2005cs

Improved distance determination to M 51 from supernovae 2011dh and 2005cs

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

Type Ia Supernovae as Extragalactic Distance Indicators

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