The Cepheid Period-Luminosity Relation (The Leavitt Law) at Mid-Infrared Wavelengths. Ii. Second-Epoch LMC Data

Madore, Barry F.; Freedman, Wendy L.; Rigby, J. Keith; Persson, S. E.; Sturch, Laura; Mager, Violet

doi:10.1088/0004-637x/695/2/988

Cited by 35 publications

(89 citation statements)

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“…This is the first such work primarily because the requisite observational data have not existed previously. Since the farther reach of (brighter) Cepheid PL relations makes their study potentially more influential, the Spitzer Space Telescope has been used to derive mid-infrared PL relations for Galactic (Marengo et al 2010) and Magellanic Clouds (Madore et al 2009) Cepheids (the latter making use of SAGE survey data: Meixner et al 2006;Madore et al 2009). These studies of Galactic (Magellanic Clouds) Cepheid midinfrared PL relations reported best-fit dispersions of ∼0.2 mag (∼0.12 mag).…”

Section: Introductionmentioning

confidence: 99%

MID-INFRARED PERIOD-LUMINOSITY RELATIONS OF RR LYRAE STARS DERIVED FROM THEWISEPRELIMINARY DATA RELEASE

Klein¹,

Richards²,

Butler³

et al. 2011

ApJ

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Interstellar dust presents a significant challenge to extending parallax-determined distances of optically observed pulsational variables to larger volumes. Distance ladder work at mid-infrared wavebands, where dust effects are negligible and metallicity correlations are minimized, has been largely focused on few-epoch Cepheid studies. Here we present the first determination of mid-infrared period-luminosity (PL) relations of RR Lyrae stars from phase-resolved imaging using the preliminary data release of the Wide-field Infrared Survey Explorer (WISE). We present a novel statistical framework to predict posterior distances of 76 well observed RR Lyrae that uses the optically constructed prior distance moduli while simultaneously imposing a power-law PL relation to WISE-determined mean magnitudes. We find that the absolute magnitude in the bluest WISE filter is M W1 = (−0.421 ± 0.014) − (1.681 ± 0.147) log 10 (P /0.50118 day), with no evidence for a correlation with metallicity. Combining the results from the three bluest WISE filters, we find that a typical star in our sample has a distance measurement uncertainty of 0.97% (statistical) plus 1.17% (systematic). We do not fundamentalize the periods of RRc stars to improve their fit to the relations. Taking the Hipparcos-derived mean V-band magnitudes, we use the distance posteriors to determine a new optical metallicity-luminosity relation. The results of this analysis will soon be tested by Hubble Space Telescope parallax measurements and, eventually, with the GAIA astrometric mission.

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Section: Introductionmentioning

confidence: 99%

MID-INFRARED PERIOD-LUMINOSITY RELATIONS OF RR LYRAE STARS DERIVED FROM THEWISEPRELIMINARY DATA RELEASE

Klein¹,

Richards²,

Butler³

et al. 2011

ApJ

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“…It is likely, as indicated in recent work from Spitzer data, that mid-infrared Cepheid PL relations are even superior to their near-infrared relations because of their even lower sensitivity to reddening, and lower intrinsic dispersions (Madore et al 2009). Yet, their dependence on metallicity has still to be investigated and they cannot be exploited from the ground making them exceedingly expensive to use.…”

Section: Discussionmentioning

confidence: 93%

Calibrating the Cepheid period-luminosity relation from the infrared surface brightness technique

Storm

Gieren

Fouqué

et al. 2011

A&A

109

111

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Context. The extragalactic distance scale builds directly on the Cepheid period-luminosity (PL) relation as delineated by the sample of Cepheids in the Large Magellanic Cloud (LMC). However, the LMC is a dwarf irregular galaxy, quite different from the massive spiral galaxies used for calibrating the extragalactic distance scale. Recent investigations suggest that not only the zero-point but also the slope of the Milky Way PL relation differ significantly from that of the LMC, casting doubts on the universality of the Cepheid PL relation. Aims. We want to make a differential comparison of the PL relations in the two galaxies by delineating the PL relations using the same method, the infrared surface brightness method (IRSB), and the same precepts. We furthermore extend the metallicity baseline for investigating the zero-point dependence, by applying the method to five SMC Cepheids as well. Methods. The IRSB method is a Baade-Wesselink type method to determine individual distances to Cepheids. We apply a newly revised calibration of the method as described in an accompanying paper (Paper I) to 36 LMC and five SMC Cepheids and delineate new PL relations in the V, I, J, & K bands as well as in the Wesenheit indices in the optical and near-IR. Results. We present 509 new and accurate radial velocity measurements for a sample of 22 LMC Cepheids, enlarging our earlier sample of 14 stars to include 36 LMC Cepheids. The new calibration of the IRSB method is directly tied to the recent HST parallax measurements to ten Milky Way Cepheids, and we find a LMC barycenter distance modulus of 18.45 ± 0.04 (random error only) from the 36 individual LMC Cepheid distances. In the J, K bands we find identical slopes for the LMC and Milky Way PL relations and only a weak letallicity effect on the zero points (consistent with a zero effect), metal poor stars being fainter. In the optical we find the Milky Way slopes are slightly shallower than the LMC slopes (but again consistent with no difference in the slopes) and small effects on the zero points. However, the important Wesenheit index in V, (V − I) shows a metallicity effect on the slope and on the zero point which is likely to be significant. Conclusions. We find a significant metallicity effect on the W VI index γ(W VI ) = −0.23 ± 0.10 mag dex −1 as well as an effect on the slope. The K-band PL relation on the other hand is found to be an excellent extragalactic standard candle being metallicity insensitive in both slope and zero-point and at the same time being reddening insensitive and showing the least internal dispersion.

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“…The expected MIR P-L slopes are represented as dashed lines in this Figure, and suggest that the P-L slopes approach these asymptotic values around ∼ 1.5µm. Empirical IRAC band P-L slopes from Madore et al (2009b) were included for comparison.…”

Section: The Empirical Mid-infrared P-l Relationsmentioning

confidence: 99%

Period-luminosity relations for Cepheid variables: from mid-infrared to multi-phase

Ngeow

Bellinger

Marconi

et al. 2012

Astrophys Space Sci

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This paper discusses two aspects of current research on the Cepheid period-luminosity (P-L) relation: the derivation of mid-infrared (MIR) P-L relations and the investigation of multi-phase P-L relations.The MIR P-L relations for Cepheids are important in the James Webb Space Telescope era for the distance scale issue, as the relations have potential to derive the Hubble constant within ∼ 2% accuracy -a critical constraint in precision cosmology. Consequently, we have derived the MIR P-L relations for Cepheids in the Large and Small Magellanic Clouds, using archival data from Spitzer Space Telescope. We also compared currently empirical P-L relations for Cepheids in the Magellanic Clouds to the synthetic MIR P-L relations derived from pulsational models.For the study of multi-phase P-L relations, we present convincing evidence that the Cepheid P-L relations in the Magellanic Clouds are highly dynamic quantities that vary significantly when considered as a function of pulsational phase. We found that there is a difference in P-L relations as a function of phase between the Cepheids in each of the Clouds; the most likely cause for this is the metallicity difference between the two galaxies. We also investigated the dispersion of the multi-phase P-L relations, and found that the minimum dispersions do not differ significantly from the mean light P-L dispersion.

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The Cepheid Period-Luminosity Relation (The Leavitt Law) at Mid-Infrared Wavelengths. Ii. Second-Epoch LMC Data

Cited by 35 publications

References 8 publications

MID-INFRARED PERIOD-LUMINOSITY RELATIONS OF RR LYRAE STARS DERIVED FROM THEWISEPRELIMINARY DATA RELEASE

MID-INFRARED PERIOD-LUMINOSITY RELATIONS OF RR LYRAE STARS DERIVED FROM THEWISEPRELIMINARY DATA RELEASE

Calibrating the Cepheid period-luminosity relation from the infrared surface brightness technique

Period-luminosity relations for Cepheid variables: from mid-infrared to multi-phase

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