The distance to Supernova 1998aq in NGC 3982

Stetson, P. B.; Gibson, Brad K.

doi:10.1046/j.1365-8711.2001.05005.x

Cited by 16 publications

(15 citation statements)

References 20 publications

(47 reference statements)

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“…We also used these observations to search for additional Cepheids in the hosts which previously had the smallest numbers of Cepheids: NGC 3021, NGC 3982, NGC 4536, and NGC 4639 (L. M. Macri et al 2011a, in preparation). The new observations, together with those from Riess et al (2009b), Saha et al (1996Saha et al ( , 1997Saha et al ( , 2001), Gibson et al (2000), Stetson & Gibson (2001), and Macri et al (2006), provide the position, period, and phase of 730 Cepheids in eight hosts with reliable SN Ia data as well as NGC 4258. The Cepheids in each host were typically imaged on 14 epochs in F 555W and 2-5 epochs with F 814W (except for NGC 4258, which has 12 epochs of F 814W data).…”

Section: Wfc3 Observations Of Cepheids In the Sh0es Programmentioning

confidence: 86%

A 3% SOLUTION: DETERMINATION OF THE HUBBLE CONSTANT WITH THEHUBBLE SPACE TELESCOPEAND WIDE FIELD CAMERA 3

Riess

Macri

Casertano

et al. 2011

ApJ

1,361

1,165

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We use the Wide Field Camera 3 (WFC3) on the Hubble Space Telescope (HST) to determine the Hubble constant from optical and infrared observations of over 600 Cepheid variables in the host galaxies of eight recent Type Ia supernovae (SNe Ia), providing the calibration for a magnitude-redshift relation based on 253 SNe Ia. Increased precision over past measurements of the Hubble constant comes from five improvements: (1) more than doubling the number of infrared observations of Cepheids in the nearby SN hosts; (2) increasing the sample size of ideal SN Ia calibrators from six to eight; (3) increasing by 20% the number of Cepheids with infrared observations in the megamaser host NGC 4258; (4) reducing the difference in the mean metallicity of the Cepheid comparison samples between NGC 4258 and the SN hosts from Δlog [O/H] = 0.08 to 0.05; and (5) calibrating all optical Cepheid colors with a single camera, WFC3, to remove cross-instrument zero-point errors. The result is a reduction in the uncertainty in H 0 due to steps beyond the first rung of the distance ladder from 3.5% to 2.3%. The measurement of H 0 via the geometric distance to NGC 4258 is 74.8 ± 3.1 km s −1 Mpc −1 , a 4.1% measurement including systematic uncertainties. Better precision independent of the distance to NGC 4258 comes from the use of two alternative Cepheid absolute calibrations: (1) 13 Milky Way Cepheids with trigonometric parallaxes measured with HST/fine guidance sensor and Hipparcos and (2) 92 Cepheids in the Large Magellanic Cloud for which multiple accurate and precise eclipsing binary distances are available, yielding 74.4 ± 2.5 km s −1 Mpc −1 , a 3.4% uncertainty including systematics. Our best estimate uses all three calibrations but a larger uncertainty afforded from any two: H 0 = 73.8 ± 2.4 km s −1 Mpc −1 including systematic errors, corresponding to a 3.3% uncertainty. The improved measurement of H 0 , when combined with the Wilkinson Microwave Anisotropy Probe (WMAP) 7 year data, results in a tighter constraint on the equation-of-state parameter of dark energy of w = −1.08 ± 0.10. It also rules out the best-fitting gigaparsec-scale void models, posited as an alternative to dark energy. The combined H 0 + WMAP results yield N eff = 4.2 ± 0.7 for the number of relativistic particle species in the early universe, a low-significance excess for the value expected from the three known neutrino flavors.

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Section: Wfc3 Observations Of Cepheids In the Sh0es Programmentioning

confidence: 86%

A 3% SOLUTION: DETERMINATION OF THE HUBBLE CONSTANT WITH THEHUBBLE SPACE TELESCOPEAND WIDE FIELD CAMERA 3

Riess

Macri

Casertano

et al. 2011

ApJ

1,361

1,165

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“…To account for possible differences in the Cepheid photometry measured with ACS and WFPC2, we compared the photometry of 8711 non-variable stellar sources in the field of NGC 3982 observed with both cameras through F 555W and F 814W . Using the master catalog of WFPC2 photometry used by Gibson et al (2000) and Stetson & Gibson (2001) we find the mean difference between our WFPC2 and ACS V − I colors of these sources to be 0.054 ± 0.005 mag (WFPC2 is bluer), with no dependence on source color or magnitude. The origin of this difference largely resides in the specific zeropoints adopted by Stetson & Gibson (2001) and those from Riess et al (2009) and Macri et al (2006Macri et al ( ,2009.…”

Section: Sky Determination and Bias Correctionmentioning

confidence: 80%

“…Using the master catalog of WFPC2 photometry used by Gibson et al (2000) and Stetson & Gibson (2001) we find the mean difference between our WFPC2 and ACS V − I colors of these sources to be 0.054 ± 0.005 mag (WFPC2 is bluer), with no dependence on source color or magnitude. The origin of this difference largely resides in the specific zeropoints adopted by Stetson & Gibson (2001) and those from Riess et al (2009) and Macri et al (2006Macri et al ( ,2009. Because our goal is limited to placing the WFPC2 Cepheid colors on the same photometric scale as the ACS data to measure distances relative to NGC 4258, we corrected the WFPC2 Cepheid data of Gibson et al (2000) for NGC 4639, NGC 4536, and NGC 3982 to the ACS color scale.…”

Section: Sky Determination and Bias Correctionmentioning

confidence: 80%

A REDETERMINATION OF THE HUBBLE CONSTANT WITH THEHUBBLE SPACE TELESCOPEFROM A DIFFERENTIAL DISTANCE LADDER

Riess

Macri

Casertano

et al. 2009

ApJ

807

920

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This is the second of two papers reporting results from a program to determine the Hubble constant to ∼ 5% precision from a refurbished distance ladder based on extensive use of differential measurements. Here we report observations of 240 Cepheid variables obtained with the Near Infrared Camera and Multi-Object Spectrometer (NIC-MOS) Camera 2 through the F 160W filter on the Hubble Space Telescope (HST). The Cepheids are distributed across six recent hosts of Type Ia supernovae (SNe Ia) and the "maser galaxy" NGC 4258, allowing us to directly calibrate the peak luminosities of the SNe Ia from the precise, geometric distance measurements provided by the masers. New features of our measurement include the use of the same instrument for all Cepheid measurements across the distance ladder and homogeneity of the Cepheid periods and metallicities thus necessitating only a differential measurement of Cepheid fluxes and reducing the largest systematic uncertainties in the determination of the fiducial SN Ia luminosity. In addition, the NICMOS measurements reduce the effects of differential extinction in the host galaxies by a factor of ∼5 over past optical data. Combined with a greatly expanded of 240 SNe Ia at z < 0.1 which define their magnitude-redshift relation, we find H 0 =74.2 ± 3.6 km s −1 Mpc −1 , a 4.8% uncertainty including both statistical and systematic errors. To independently test the maser calibration, we use the ten individual parallax measurements of Galactic Cepheids obtained with the HST Fine -2 -Guidance Sensor and find similar results. We show that the factor of 2.2 improvement in the precision of H 0 is a significant aid to the determination of the equation-of-state parameter of dark energy, w = P/(ρc 2 ). Combined with the Wilkinson Microwave Anisotropy Probe 5-year measurement of Ω M h 2 , we find w = −1.12 ± 0.12 independent of any information from high-redshift SNe Ia or baryon acoustic oscillations (BAO). This result is also consistent with analyses based on the combination of high-redshift SNe Ia and BAO. The constraints on w(z) now including high-redshift SNe Ia and BAO are consistent with a cosmological constant and are improved by a factor of 3 due to the refinement in H 0 alone. We show that future improvements in the measurement of H 0 are likely and should further contribute to multi-technique studies of dark energy.

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“…Using a P − L relation based on ∼650 Cepheids located in the Large Magellanic Cloud that were observed by the Optical Gravitational Lensing Experiment (OGLE) (Udalski et al 1999), the HKP team concluded that µ = 31.56 ± 0.08 (Stetson et al 2001). More recently Riess et al (2005) used the Advanced Camera for Surveys on the HST to obtain a Cepheid distance.…”

Section: Observational Data and Uvoir Light Curvesmentioning

confidence: 99%

Constraints on the progenitor systems of type Ia supernovae

Stritzinger

Leibundgut

Walch

et al. 2006

A&A

152

219

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Bolometric light curves provide a valuable insight into the nature of type Ia supernovae. We present an analysis of sixteen well-observed type Ia supernovae. Constraints are placed on several global parameters concerning the progenitor system, explosion mechanism, and subsequent radiation transport. By fitting a radioactive decay energy deposition function to the quasi-exponential phase (50 to 100 days after maximum light), it is found that the ejected mass varies by at least a factor of two. This result suggests that a sub Chandrasekhar mass white dwarf could be the progenitor system of some type Ia supernovae. We find that the range in the amount of synthesized 56 Ni indicates a significant variation in the burning mechanism. In order to explain a factor of ten range in the observed bolometric luminosity, more detailed modeling of the explosion mechanism is required.

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The distance to Supernova 1998aq in NGC 3982

Cited by 16 publications

References 20 publications

A 3% SOLUTION: DETERMINATION OF THE HUBBLE CONSTANT WITH THEHUBBLE SPACE TELESCOPEAND WIDE FIELD CAMERA 3

A 3% SOLUTION: DETERMINATION OF THE HUBBLE CONSTANT WITH THEHUBBLE SPACE TELESCOPEAND WIDE FIELD CAMERA 3

A REDETERMINATION OF THE HUBBLE CONSTANT WITH THEHUBBLE SPACE TELESCOPEFROM A DIFFERENTIAL DISTANCE LADDER

Constraints on the progenitor systems of type Ia supernovae

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