Calibrating Type Ia Supernovae Using the Planetary Nebula Luminosity Function. I. Initial Results

Feldmeier, John J.; Jacoby, George H.; Phillips, M. M.

doi:10.1086/510897

Cited by 37 publications

(46 citation statements)

References 71 publications

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“…However, even in the best case there is a non-negligible 0.2 mag offset between SBF and PNLF that implies ∼10% larger SBF distances. Again, this difference occurs mainly beyond ∼10 Mpc, and is similar to the 10% larger H 0 obtained when calibrating SNe Ia via PNLF instead of Cepheids (Feldmeier et al 2007).…”

Section: Discussionsupporting

confidence: 81%

“…In a recent review, Ciardullo (2012) finds that if one adopts the metallicity-dependent Cepeheid PL relations, the PNLF zero point brightens by 0.07 mag, going from M * = −4.46 ± 0.05 to M * = −4.53 ± 0.04 mag (external scatter σ = 0.16 mag). Feldmeier et al (2007) actually used M * = −4.47; thus their PNLF distance modulus for NGC 1316 becomes (m−M) = 31.32 +0.09 −0.12 mag 8 . Both PNLF distances given above agree within quoted uncertainties with the Str10 distance.…”

Section: Planetary Nebulae Luminosity Functionsmentioning

confidence: 99%

“…Both PNLF and SBF calibrations are tied to the same primary indicator, the period-luminosity relation of Cepheids, and to the same dataset, i.e., the Cepheids from Freedman et al (2001). However, the zero points of present SBF calibrations are tied to the Cepheid distances obtained with metallicity-dependent PL relations (D PLZ hereafter; Mei et al 2007;Blakeslee et al 2009Blakeslee et al , 2010, while the standard PNLF calibration relies on Cepheid distances with no dependence on metallicity (D PL ; Ciardullo et al 2002;Feldmeier et al 2007;Ciardullo 2012). Average (median) correction on the sample of nearby galaxies 0.06 ± 0.03 (0.085) Average correction on the complete sample of galaxies (assume zero for distant galaxies) 0.02 ± 0.01 in this work (SN 1981D, SN 2006dd, SN 2006mr).…”

Section: Appendix A: Some Musings On Pnlf and Sbf Distancesmentioning

confidence: 99%

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The distance to NGC 1316 (Fornax A): yet another curious case

Cantiello

Grado

Blakeslee

et al. 2013

A&A

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Aims. The distance of NGC 1316, the brightest galaxy in the Fornax cluster, provides an interesting test for the cosmological distance scale. First, because Fornax is the second largest cluster of galaxies within 25 Mpc after Virgo and, in contrast to Virgo, has a small line-of-sight depth; and second, because NGC 1316 is the single galaxy with the largest number of detected Type Ia supernovae (SNe Ia), giving the opportunity to test the consistency of SNe Ia distances both internally and against other distance indicators. Methods. We measure surface brightness fluctuations (SBF) in NGC 1316 from ground-and space-based imaging data. The sample provides a homogeneous set of measurements over a wide wavelength interval. The SBF magnitudes, coupled with empirical and theoretical absolute SBF calibrations, are used to estimate the distance to the galaxy. We also present the first B-band SBF measurements of NGC 1316 and use them together with the optical and near-IR SBF data to analyze the properties of field stars in the galaxy. Results. We obtain (m−M) = 31.59± 0.05(stat.)± 0.14(sys.) mag, or d = 20.8± 0.5(stat.)± 1.5(sys.) Mpc. When placed in a consistent Cepheid distance scale, our result agrees with the distances from other indicators. On the other hand, our distance is ∼17% larger than the most recent estimate based on SNe Ia. Possible explanations for this disagreement are the uncertain level of internal extinction, and/or calibration issues. Concerning the stellar population analysis, we confirm the results from other spectro-photometric indicators: the field stars in NGC 1316 are dominated by a component with roughly solar metallicity and intermediate age. A non-negligible mismatch exists between B-band SBF models and data. We confirm that such behavior can be accounted for by an enhanced percentage of hot horizontal branch stars. Conclusions. Our study of the SBF distance to NGC 1316, and the comparison with distances from other indicators, raises some concern about the homogeneity between the calibrations of different indicators. If not properly placed in the same reference scale, significant differences can occur, with dramatic impact on the cosmological distance ladder. Our results on the stellar populations properties show that SBF data over a broad wavelength interval are an efficient means of studying the properties of unresolved systems in peculiar cases like NGC 1316.

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Section: Discussionsupporting

confidence: 81%

Section: Planetary Nebulae Luminosity Functionsmentioning

confidence: 99%

Section: Appendix A: Some Musings On Pnlf and Sbf Distancesmentioning

confidence: 99%

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The distance to NGC 1316 (Fornax A): yet another curious case

Cantiello

Grado

Blakeslee

et al. 2013

A&A

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“…Feldmeier et al 2007;Stritzinger et al 2010;Cantiello et al 2013). For simplicity, we adopt a distance of 20 Mpc for NGC 1316, consistent with the various estimates given in the NASA Extragalactic Database (NED).…”

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confidence: 99%

Mid-infrared dust in two nearby radio galaxies, NGC 1316 (Fornax A) and NGC 612 (PKS 0131-36)

Asabere

Horellou

Jarrett

et al. 2016

A&A

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Context. Most radio galaxies are hosted by giant gas-poor ellipticals, but some contain significant amounts of dust, which is likely to be of external origin. Aims. In order to characterize the mid-IR properties of two of the most nearby and brightest merger-remnant radio galaxies of the Southern hemisphere, NGC 1316 (Fornax A) and NGC 612 (PKS 0131−36), we used observations with the Wide-field Infrared Survey Explorer (WISE) at wavelengths of 3.4, 4.6, 12 and 22 µm and Spitzer mid-infrared spectra. Methods. By applying a resolution-enhancement technique, new WISE images were produced at angular resolutions ranging from 2 . 6 to 5 . 5. Global measurements were performed in the four WISE bands, and stellar masses and star-formation rates were estimated using published scaling relations. Two methods were used to uncover the distribution of dust, one relying on two-dimensional fits to the 3.4 µm images to model the starlight, and the other one using a simple scaling and subtraction of the 3.4 µm images to estimate the stellar continuum contribution to the emission in the 12 and 22 µm bands. Results. The two galaxies differ markedly in their mid-IR properties. The 3.4 µm brightness distribution can be well represented by the superposition of two Sérsic models in NGC 1316 and by a Sérsic model and an exponential disk in NGC 612. The WISE colors of NGC 1316 are typical of those of early-type galaxies; those of NGC 612 are in the range found for star-forming galaxies. From the 22 µm luminosity, we infer a star-formation rate of ∼0.7 M yr −1 in NGC 1316 and ∼7 M yr −1 in NGC 612. Spitzer spectroscopy shows that the 7.7-to-11.3 µm PAH line ratio is significantly lower in NGC 1316 than in NGC 612. The WISE images reveal resolved emission from dust in the central 1 −2 of the galaxies. In NGC 1316, the extra-nuclear emission coincides with two dusty regions NW and SE of the nucleus seen in extinction in optical images and where molecular gas is known to reside. In NGC 612 it comes from a warped disk. This suggests a recent infall onto NGC 1316 and disruption of one or several smaller gas-rich galaxies, but a smoother accretion in NGC 612. While the nucleus of NGC 1316 is currently dormant and the galaxy is likely to evolve into a passive elliptical, NGC 612 has the potential of growing a larger disk and sustaining an active nucleus. Conclusions. NGC 1316 and NGC 612 represent interesting challenges to models of formation and evolution of galaxies and AGNs.

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“…The consistency of these results illustrates the robustness of the PNLF method. (Ciardullo et al 1989b(Ciardullo et al , 2002Feldmeier et al 1997), Virgo (Jacoby et al 1990;Feldmeier et al 2007), and Fornax (McMillan et al 1993;Teodorescu et al 2005;Feldmeier et al 2007) almost always place all galaxies comfortably within the typical group diameter of ∼ 1 Mpc. (The lone exception is in Virgo, where the PNLF clearly resolves the M84/M86 system which is now known to be in the background.)…”

Section: ) Leo Imentioning

confidence: 99%

The planetary nebula luminosity function

Ciardullo

2012

Proc. IAU

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Abstract. Although the method has no theoretical explanation, the [Oiii]λ5007Å planetary nebula luminosity function (PNLF) is an extremely valuable tool for obtaining accurate (< 10%) extragalactic distances out to ∼ 18 Mpc. Because the PNLF works in large galaxies of all Hubble types, it is one of the best tools we have for cross-checking the results of other methods and identifying systematic offsets between the Population I and Population II distance ladders. We review the PNLF's calibration and show that the method's Cepheid-derived zero point is virtually identical to that inferred from measurements of the tip of the red giant branch. We then compare the PNLF to the surface brightness fluctuations method and demonstrate that the latter's calibration yields a distance scale that is ∼ 15% larger than that of the PNLF. We argue that this offset is likely due to a number of factors, including the effects of reddening on both of the techniques. We conclude by discussing the use of the PNLF for supernovae Type Ia calibration and considering the outstanding problems associated with the method.

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Calibrating Type Ia Supernovae Using the Planetary Nebula Luminosity Function. I. Initial Results

Cited by 37 publications

References 71 publications

The distance to NGC 1316 (Fornax A): yet another curious case

The distance to NGC 1316 (Fornax A): yet another curious case

Mid-infrared dust in two nearby radio galaxies, NGC 1316 (Fornax A) and NGC 612 (PKS 0131-36)

The planetary nebula luminosity function

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