A study on the universality and linearity of the Leavitt law in the LMC and SMC galaxies

García-Varela, A.; Sabogal, B. E.; Ramírez-Tannus, M. C.

doi:10.1093/mnras/stt325

Cited by 18 publications

(17 citation statements)

References 26 publications

(54 reference statements)

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“…This enables their apparent magnitudes to be converted into luminosities, which, along with the measured pulsation periods, provides an absolute calibration of the PLR. This is believed to be near-universal across the Cepheid population [81], although there is a weak dependence on metallicity [82]. Further constraining power for the PLR comes from Cepheids in the Large Magellanic Cloud (LMC) and M31 [83,84], the distances to which are measured independently with detached eclipsing binaries [85], and in N4258 whose distance is calibrated with a water maser [19].…”

Section: A Overviewmentioning

confidence: 99%

Local resolution of the Hubble tension: The impact of screened fifth forces on the cosmic distance ladder

2019

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The discrepancy between the values of the Hubble constant H 0 derived from the local distance ladder and the Cosmic Microwave Background provides a tantalising hint of new physics. We explore a potential resolution involving screened fifth forces in the local Universe, which alter the Cepheid calibration of supernova distances. In particular, if the Cepheids with direct distance measurements from parallax or water masers are screened but a significant fraction of those in other galaxies are not, neglecting the difference between their underlying period-luminosity relations biases the local H 0 measurement high. This difference derives from a reduction in the Cepheid pulsation period and possible increase in luminosity under a fifth force. We quantify the internal and environmental gravitational properties of the Riess et al. distance ladder galaxies to assess their degrees of screening under a range of phenomenological models, and propagate this information into the H 0 posterior as a function of fifth force strength. We consider well-studied screening models in scalar-tensor gravity theories such as chameleon, K-mouflage and Vainshtein, along with a recently-proposed mechanism based on baryon-dark matter interactions in which screening is governed by the local dark matter density. We find that a fifth force strength ∼ 5 − 30% that of gravity can alleviate the H 0 tension in many scenarios, around the sensitivity level at which tests based on other distance ladder data can constrain this strength. Our most successful models achieve consistency with Planck at the ∼1.5σ level. Although our analysis is exploratory and based on screening models that are not necessarily realised in full theories, our results demonstrate that new physics-based local resolutions of the H 0 tension are possible, supplementing those already known in the pre-recombination era. * harry.desmond@physics.ox.ac.uk

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Section: A Overviewmentioning

confidence: 99%

Local resolution of the Hubble tension: The impact of screened fifth forces on the cosmic distance ladder

2019

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“…Inno et al (2013) on the other hand find that their Magellanic Cloud Period-Wesenheit relations are linear. García-Varela et al (2013) observe non linear relations in the VI bands and that the Wesenheit function behaves exponentially.…”

Section: Introductionmentioning

confidence: 82%

THE M31 NEAR-INFRARED PERIOD-LUMINOSITY RELATION AND ITS NON-LINEARITY FOR δ Cep VARIABLES WITH 0.5 ⩽ log (P) ⩽ 1.7

Kodric

Riffeser

Seitz

et al. 2015

ApJ

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We present the largest M31 near-infrared (F110W (close to J band), F160W (H band)) Cepheid sample so far. The sample consists of 371 Cepheids with photometry obtained from the HST PHAT program. The sample of 319 fundamental mode Cepheids, 16 first overtone Cepheids and 36 type II Cepheids, was identified using the median absolute deviation (MAD) outlier rejection method we develop here. This method does not rely on priors and allows us to obtain this clean Cepheid sample without rejecting a large fraction of Cepheids.The obtained Period-Luminosity relations (PLRs) have a very small dispersion, i.e. 0.155 mag in F160W, despite using random phased observations. This remarkably small dispersion allows us to determine that the PLRs are significantly better described by a broken slope at ten days than a linear slope. The use of our sample as an anchor to determine the Hubble constant gives a 3.2% larger Hubble constant compared to the Riess et al. (2012) sample.

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“…The break in the PLRs at 10 days has also been observed for Cepheids in M31 (Kodric et al, 2015(Kodric et al, , 2018. Furthermore, possible non-linearities in Cepheid PLRs have been investigated using a number of independent methods including both parametric and non-parametric statistical tests (Kanbur et al, 2007;García-Varela, Sabogal & Ramírez-Tannus, 2013;Bhardwaj et al, 2016a). Bhardwaj et al (2016a) found evidence of a break at 10 days in optical Cepheid PLRs and around 18 days in the NIR PLRs in the LMC.…”

Section: Linear Versus Non-linear Period-luminosity Relationsmentioning

confidence: 91%

“…The application of Cepheid PLRs to the distance scale follows a basic assumption that these relations are linear over the entire period range. The nonlinearity of the PLRs has been a subject of many studies in the past decade (Tammann, Sandage & Reindl, 2003;Sandage, Tammann & Reindl, 2004;Ngeow et al, 2005;Ngeow & Kanbur, 2006a;Ngeow, Kanbur & Nanthakumar, 2008;García-Varela, Sabogal & Ramírez-Tannus, 2013;Bhardwaj et al, 2016a). The Cepheid PLRs in the LMC exhibit a change in the slope at 10 days for fundamental-mode Cepheids and at 2.5 days for first-overtone mode Cepheids at optical wavelengths (Bhardwaj et al, 2016a).…”

Section: Linear Versus Non-linear Period-luminosity Relationsmentioning

confidence: 99%

High-precision distance measurements with classical pulsating stars

Bhardwaj

2020

Preprint

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Classical Cepheid and RR Lyrae variables are radially pulsating stars that trace young and old-age stellar populations, respectively. These classical pulsating stars are the most sensitive probes for the precision stellar astrophysics and the extragalactic distance measurements. Despite their extensive use as standard candles thanks to their well-defined Period-Luminosity relations, distance measurements based on these objects suffer from their absolute primary calibrations, metallicity effects, and other systematic uncertainties. Here, I present a review of classical Cepheid, RR Lyrae, and type II Cepheid variables starting with a historical introduction and describing their basic evolutionary and pulsational properties. I will focus on recent theoretical and observational efforts to establish absolute scale for these standard candles at multiple wavelengths. The application of these classical pulsating stars to high-precision cosmic distance scale will be discussed along with observational systematics. I will summarize with an outlook for further improvements in our understanding of these classical pulsators in the upcoming era of extremely large telescopes.

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A study on the universality and linearity of the Leavitt law in the LMC and SMC galaxies

Cited by 18 publications

References 26 publications

Local resolution of the Hubble tension: The impact of screened fifth forces on the cosmic distance ladder

Local resolution of the Hubble tension: The impact of screened fifth forces on the cosmic distance ladder

THE M31 NEAR-INFRARED PERIOD-LUMINOSITY RELATION AND ITS NON-LINEARITY FOR δ Cep VARIABLES WITH 0.5 ⩽ log (P) ⩽ 1.7

High-precision distance measurements with classical pulsating stars

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