(Q58603183)

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Nonlinear Decline‐Rate Dependence and Intrinsic Variation of Type Ia Supernova Luminosities

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Nonlinear Decline‐Rate Dependence and Intrinsic Variation of Type Ia Supernova Luminosities (English)

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Mark Strovink

2

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Saul Perlmutter

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6

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Saul Perlmutter

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Gerson Goldhaber

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4

object named as

Gerson Goldhaber

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James L. Siegrist

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7

object named as

James Siegrist

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author name string

Lifan Wang

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1

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Alexander Conley

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3

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Marek Kowalski

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5

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language of work or name

English

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publication date

10 April 2006

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full work available at URL

https://iopscience.iop.org/article/10.1086/500422/pdf

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published in

The Astrophysical Journal

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volume

641

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1

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page(s)

50–69

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cites work

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Cepheid calibration of the peak brightness of type Ia supernovae. IX. SN 1989B in NGC 3627

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The Reddening-Free Decline Rate Versus Luminosity Relationship for Type Ia Supernovae

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Optical and Near‐Infrared Photometry of the Type Ia Supernova 2000E in NGC 6951

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Optical and infrared photometry of the nearby type Ia supernova 2001el

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Constraints on Cosmological Models from [ITAL]Hubble Space Telescope[/ITAL] Observations of High-[CLC][ITAL]z[/ITAL][/CLC] Supernovae

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Photometric observations of the Type Ia SN 2002er in UGC 10743

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Absolute magnitudes of supernovae

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UBVRI Photometry of the Type IA SN 1994D in NGC 4526

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The Type Ia Supernova 2001V in NGC 3987

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Measurements of Ω and Λ from 42 High‐Redshift Supernovae

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Reddening, absorption, and decline rate corrections for a complete sample of type Ia supernovae leading to a fully corrected Hubble diagram to v < 30,000 km/s

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Dust around type Ia supernovae

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The Type I[CLC]a[/CLC] Supernova 1999[CLC]aw[/CLC]: A Probable 1999[CLC]aa[/CLC]-like Event in a Low-Luminosity Host Galaxy

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The High‐Z Supernova Search: Measuring Cosmic Deceleration and Global Curvature of the Universe Using Type Ia Supernovae

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Optical and Infrared Photometry of the Nearby Type Ia Supernovae 1999ee, 2000bh, 2000ca, and 2001ba

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(Q58603183)

Nonlinear Decline‐Rate Dependence and Intrinsic Variation of Type Ia Supernova Luminosities

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