Young and Intermediate-Age Distance Indicators

Subramanian, Smitha; Marengo, Massimo; Bhardwaj, Anupam; Huang, Yang; Inno, L.; Nakagawa, Akiharu; Storm, J.

doi:10.1007/s11214-017-0427-8

Cited by 14 publications

(13 citation statements)

References 192 publications

(274 reference statements)

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“…where the color coefficient α is determined directly from the reddening law (α = A 1 /(A 2 − A 3 )). We adopt the reddening law from (Cardelli et al 1989), with R V = 3.1, but note that infrared PW relations are only weakly sensitive to variations in the dust parameter (Subramanian et al 2017). For the two-band combinations, M 1 = M 3 , and is the redder of the two bands.…”

Section: Wesenheit Magnitude Relationsmentioning

confidence: 99%

Standard Galactic field RR Lyrae II: a Gaia DR2 calibration of the period–Wesenheit–metallicity relation

Neeley

Marengo

Freedman

et al. 2019

Monthly Notices of the Royal Astronomical Society

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RR Lyrae stars have long been popular standard candles, but significant advances in methodology and technology have been made in recent years to increase their precision as distance indicators. We present multi-wavelength (optical UBV R c I c and Gaia G, BP, RP; near-infrared JHK s ; mid-infrared [3.6], [4.5]) period-luminosity-metallicity (PLZ), period-Wesenheit-metallicity (PWZ) relations, calibrated using photometry obtained from The Carnegie RR Lyrae Program and parallaxes from the Gaia second data release for 55 Galactic field RR Lyrae stars. The metallicity slope, which has long been predicted by theoretical relations, can now be measured in all passbands. The scatter in the PLZ relations is on the order of 0.2 mag, and is still dominated by uncertainties in the parallaxes. As a consistency check of our PLZ relations, we also measure the distance modulus to the globular cluster M4, the Large Magellanic Cloud (LMC) and the Small Magellanic Cloud (SMC), and our results are in excellent agreement with estimates from previous studies. † Hubble Fellow distances cannot be measured with the traditional distance scale.

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Section: Wesenheit Magnitude Relationsmentioning

confidence: 99%

Standard Galactic field RR Lyrae II: a Gaia DR2 calibration of the period–Wesenheit–metallicity relation

Neeley

Marengo

Freedman

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…In addition, there is a fourth subclass, the peculiar W Vir (pW Vir) stars which are brighter and bluer than the W Vir stars (Soszyński et al 2008). All these classi-cal pulsating stars follow well-defined Period-Luminosity relations (PLRs) which make them excellent distance indicators (Muraveva et al 2015;Bhardwaj et al 2016aBhardwaj et al , 2017aRipepi et al 2017;Subramanian et al 2017;Beaton & Carnegie-Chicago Hubble Program Team 2018).…”

Section: Introductionmentioning

confidence: 99%

“…cal pulsating stars follow well-defined Period-Luminosity relations (PLRs) which make them excellent distance indicators (Muraveva et al 2015;Bhardwaj et al 2016aBhardwaj et al , 2017aRipepi et al 2017;Subramanian et al 2017;Beaton & Carnegie-Chicago Hubble Program Team 2018).…”

mentioning

confidence: 99%

The stellar photosphere–hydrogen ionization front interaction in classical pulsators: a theoretical explanation for observed period–colour relations

Das

Bellinger

Bhardwaj

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Period-colour and amplitude-colour (PCAC) relations can be used to probe both the hydrodynamics of outer envelope structure and evolutionary status of Cepheids and RR Lyraes. In this work, we incorporate the PCAC relations for RR Lyraes, BL Her, W Vir and classical Cepheids in a single unifying theory that involves the interaction of the hydrogen ionization front (HIF) and stellar photosphere and the theory of stellar evolution. PC relations for RR Lyraes and classical Cepheids using OGLE-IV data are found to be consistent with this theory: RR Lyraes have shallow/sloped relations at minimum/maximum light whilst longperiod (P > 10 days) Cepheids exhibit sloped/flat PC relations at minimum/maximum light. The differences in the PC relations for Cepheids and RR Lyraes can be explained based on the relative location of the HIF and stellar photosphere which changes depending on their position on the HR diagram. We also extend our analysis of PCAC relations for type II Cepheids in the Galactic bulge, LMC and SMC using OGLE-IV data. We find that BL Her stars have sloped PC relations at maximum and minimum light similar to short-period (P < 10 days) classical Cepheids. W Vir stars exhibit sloped/flat PC relation at minimum/maximum light similar to long-period classical Cepheids. We also compute state-of-the-art 1D radiation hydrodynamic models of RR Lyraes, BL Her and classical Cepheids using the radial stellar pulsation code in MESA to further test these ideas theoretically and find that the models are generally consistent with this picture. We are thus able to explain PC relations at maximum and minimum light across a broad spectrum of variable star types.

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“…However, the metallicity effect on the near-IR PL relations is considered to be negligible (see e.g. Bono et al, 2010;Subramanian et al, 2017). Even a very conservative upper limit, 0.1 mag dex −1 , for the near-IR relations would lead to the small relative error of ∼0.1 mag, which is negligible as discussed above, when the most metal-rich ([Fe/H]∼ +0.5 dex) and the most metal-poor ([Fe/H]∼ −0.5 dex) Cepheids are compared.…”

Section: Metallicity Gradientmentioning

confidence: 99%

Impact of Distance Determinations on Galactic Structure. I. Young and Intermediate-Age Tracers

Matsunaga¹,

Bono²,

Chen³

et al. 2018

Space Sci Rev

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Young and Intermediate-Age Distance Indicators

Cited by 14 publications

References 192 publications

Standard Galactic field RR Lyrae II: a Gaia DR2 calibration of the period–Wesenheit–metallicity relation

Standard Galactic field RR Lyrae II: a Gaia DR2 calibration of the period–Wesenheit–metallicity relation

The stellar photosphere–hydrogen ionization front interaction in classical pulsators: a theoretical explanation for observed period–colour relations

Impact of Distance Determinations on Galactic Structure. I. Young and Intermediate-Age Tracers

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