Cepheid Distances to SNe Ia Host Galaxies Based on a Revised Photometric Zero Point of the HST WFPC2 and New PL Relations and Metallicity Corrections

By A. Saha, F. Thim, G. Tammann, Bernd Reindl, A. S. Noao, A. Basel, Observatories of the Carnegie Institution of Washington. 2006

162 citations recorded by the source corpus.

With this paper we continue the preparation for a forthcoming summary report of our experiment with the HST to determine the Hubble constant using Type Ia supernovae as standard candles. Two problems are addressed. (1) We examine the need for, and determine the value of, the corrections to the apparent magnitudes of our program Cepheids in the 11 previous calibration papers due to sensitivity drifts and charge transfer effects of the HST WFPC2 camera over the life time of the experiment from 1992 to 2001. (2) The corrected apparent magnitudes are applied to all our previous photometric data from which revised distance moduli are calculated for the eight program galaxies that are parents to the calibrator Ia supernovae. Two different Cepheid P-L relations are used; one for the Galaxy and one for the LMC. These differ both in slope and zero point at a fixed period. The procedures for determining the absorption and reddening corrections for each Cepheid are discussed. Corrections for the effects of metallicity differences between the program galaxies and the two adopted P-L relations are derived and applied. The distance moduli derived here for the eight supernovae program galaxies, and for 29 others, average 0.20 mag fainter (more distant) than those derived by Gibson et al. and Freedman et al. in their 2000 and 2001 summary papers for reasons discussed in this paper. The effect on the Hubble constant is the subject of our forthcoming summary paper.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/406bdfe1d72d802ad0a25a6899786262c3ebc34e

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

Cepheid parallaxes and the Hubble constant (2007, background): “Sandage and his co-workers have recently completed a major programme of reanalysing HST data of Cepheids in galaxies in which supernovae have been observed (see S2006, Saha et al. 2006 and earlier papers in the series).”
The death of massive stars – I. Observational constraints on the progenitors of Type II-P supernovae (2008, background): “The most recent of these (Saha et al. 2006) found a distance of 14.2 ± 1.3 Mpc towards NGC 4527.”
X-ray emission from star-forming galaxies – I. High-mass X-ray binaries (2011, unknown): “Galaxy D Ref.a Hubble type ib RX c SFRd M⋆e SFR/M⋆ logLlim f NXRB g logLXRB h NCXB i logLCXB j (Mpc) (deg) (arcmin) (M⊙ yr−1) (1010 M⊙) (10−10 yr−1) (erg s−1) (erg s−1) (erg s−1) NGC 0278 11.8+2.4 −2.0 (2) SAB(rs)b 0 1.0 4.1 0.7 5.7 37.22 10 39.34 1.6 38.38 NGC 0520 27.8+5.6 −4.7 (2) Pec 69 1.8 11.6”
The Hubble Constant: A Summary of the Hubble Space Telescope Program for the Luminosity Calibration of Type Ia Supernovae by Means of Cepheids (2006, background): “Saha et al. (2006b) state that the current data are consistent withH0 anywhere between 60 and 80 at the 1 level depending on the mass model of the lens.”
ASTROPHYSICAL TESTS OF MODIFIED GRAVITY: CONSTRAINTS FROM DISTANCE INDICATORS IN THE NEARBY UNIVERSE (2012, methodology): “We use the normalization from Saha et al. (2006) to find the absolute magnitude.”
GHASP: an Hα kinematic survey of spiral and irregular galaxies – V. Dark matter distribution in 36 nearby spiral galaxies (2007, unknown): “Jam04=James et al. 2004 ; Kar04=Karachentsev et al. 2004 ; Koo06=Koopmann et al. 2006 ; Mou06=Moustakas & Kennicutt 2006 ; Saha06=Saha et al. 2006 ; Sha01=Shapley et al.2001 ; Sw02=Swaters & Balcells 2002.”