The Effect of Metallicity on Cepheid-based Distances

By S. Sakai, L. Ferrarese, Robert C. Kennicutt Jr., A. Saha. 2004

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We have used the Wide Field Planetary Camera 2 on board the Hubble Space Telescope to obtain V and I images of seven nearby galaxies. For each, we have measured a distance using the tip of the red giant branch (TRGB) method. By comparing the TRGB distances with published Cepheid distances, we investigate the metallicity dependence of the Cepheid period-luminosity relation. Our sample is supplemented by 10 additional galaxies for which both TRGB and Cepheid distances are available in the literature, thus providing a uniform coverage in Cepheid abundances between 1/20 and 2 (O/H)☉. We find that the difference between Cepheid and TRGB distances decreases monotonically with increasing Cepheid abundance, consistent with a mean metallicity dependence of the Cepheid distance moduli of δ(m - M)/δ[O/H] = -0.24 ± 0.05 mag dex-1.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/1aa383c456a0ff8e29d961a960970bdb79275e15

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Citations in the corpus

THE UNIVERSAL STELLAR MASS–STELLAR METALLICITY RELATION FOR DWARF GALAXIES (2013, background): “The extinction corrections were AV = 0.08 and AI = 0.05 (Sakai et al. 2004).”
Our Peculiar Motion Away from the Local Void (2007, methodology): “Individual TRGB distances are of comparable quality to the Cepheid values and are demonstrated to be on a consistent scale (Dolphin et al. 2003; Sakai et al. 2004; Rizzi et al. 2 2007).”
Tip of the Red Giant Branch Distances. I. Optimization of a Maximum Likelihood Algorithm (2006, methodology): “The current estimate of uncertainties in TRGBmeasurements if well above the photometric limit is 0.05 mag (Sakai et al. 2004).”
X-ray emission from star-forming galaxies – I. High-mass X-ray binaries (2011, unknown): “…(8) Sakai & Madore (1999), (9) Ismail et al. (2005), (10) Saviane, Hibbard, & Rich (2004), (11) Drozdovsky et al. (2002), (12) Seth, Dalcanton, & de Jong (2005), (13) Takáts & Vinkó (2006), (14) Sakai et al. (2004), (15) Drozdovsky & Karachentsev (2000), (16) Tully et al. (2009), (17) Wolter &…”
A 2.4% DETERMINATION OF THE LOCAL VALUE OF THE HUBBLE CONSTANT (2016, background): “We also see strong evidence of a metallicity term with a value of −0.20±0.05mag dex−1 for our preferred fit, also highly significant and consistent with the value from Sakai et al. (2004) of −0.24±0.05mag dex−1.”
Calibration of the Tip of the Red Giant Branch (2003, methodology): “…has been measured and successfully used by many independent groups to determine high-precision distances to large numbers of nearby galaxies (e.g., Sakai et al. 2004; Makarov et al. 2006; Rizzi et al. 2007; Dalcanton et al. 2009, 2012; Jang & Lee 2017a, 2017b; McQuinn et al. 2019; Freedman et al.…”
Cepheid parallaxes and the Hubble constant (2007, methodology): “Adopting the results of Andrievsky et al. (2002) and Sakai et al. (2004), as discussed by S2006 the LMC Cepheids are metal deficient by ∆[O/H ] = 0.26 on the “Te” abundance scale.”
The Hubble Constant (2010, methodology): “An extensive cross comparison of Cepheid and TRGB distances including highmetallicity systems is well summarized by Sakai et al. (2004).”
KECK HIRES SPECTROSCOPY OF EXTRAGALACTIC H ii REGIONS: C AND O ABUNDANCES FROM RECOMBINATION LINES (2009, methodology): “…et al. 2005), (3) the calibration of strongline methods for deriving H ii region abundances (Peimbert et al. 2007), (4) the possible metallicity dependence of the Cepheid period–luminosity relation (Sakai et al. 2004), (5) the metallicity dependence of the number ratios of the different types of W–”
CLUSTERING OF LOCAL GROUP DISTANCES: PUBLICATION BIAS OR CORRELATED MEASUREMENTS? III. THE SMALL MAGELLANIC CLOUD (2014, methodology): “In such cases, we homogenize the database by adding these differential values to the canonical LMC distance modulus adopted here (for similar approaches applied to a large number of nearby galaxies, see also Ferrarese et al. 2000; Sakai et al. 2004).”
Advanced Camera for Surveys Imaging of 25 Galaxies in Nearby Groups and in the Field (2005, methodology): “This method (Lee et al. 1993) has a precision comparable to the Cepheid method (Sakai et al. 1996, 2004; Ferrarese et al. 2000) but requires much less observing time.”
Cepheid Calibrations from the Hubble Space Telescope of the Luminosity of Two Recent Type Ia Supernovae and a Redetermination of the Hubble Constant (2004, methodology): “To obtain estimates, we followed the procedure established by Zaritsky et al. (1994) and subsequently utilized by Kennicutt et al. (1998) and Sakai et al. (2004).”
A 3% SOLUTION: DETERMINATION OF THE HUBBLE CONSTANT WITH THE HUBBLE SPACE TELESCOPE AND WIDE FIELD CAMERA 3 (2011, background): “Indeed, the metallicity correction empirically determined here, −0.10 ± 0.09 mag dex−1 (using all three calibrations), is less than half the value of ∼ − 0.25 mag dex−1 measured at optical wavelengths (Kennicutt et al. 1998; Sakai et al. 2004) and its absolute value is not significant.”
ASTROPHYSICAL TESTS OF MODIFIED GRAVITY: CONSTRAINTS FROM DISTANCE INDICATORS IN THE NEARBY UNIVERSE (2012, methodology): “Finally, the best fit value using the metallicity correction of Sakai et al. (2004) is also shown (Z-corr).”
H 0 revisited (2013, background): “At optical wavelengths, there is evidence for a metallicity dependence of ∼ −0.25 mag. dex−1 (Kennicutt et al. 1998; Sakai et al. 2004, Macri et al. 2006; Scowcroft et al. 2009).”