Calibrating the Cepheid Period–Wesenheit Relation in the Gaia Bands Using Galactic Open-cluster Cepheids

Lin, Zuzhang; Xu, Ye; Hao, Chaojie; Liu, Dejian; Li, Yingjie; Bian, S. B.

doi:10.3847/1538-4357/ac9051

Cited by 3 publications

(4 citation statements)

References 49 publications

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“…We extended the list of magnitudes in anticipation of the vast and various data coming from the Vera Ru- bin and James Webb Space Telescope, which will also target classical Cepheids. The list of Wesenheit indices was extended due to the recent rise in popularity of the period-Wesenheit and period-Wesenheit-metallicity relations from the Gaia data (Lin et al 2022;Ripepi et al 2022), and due to the ongoing discussion about the precision and accuracy of the Hubble-Lemaître constant, H 0 , the value of which was calculated-among othersusing the W H index of classical Cepheids (Riess et al 2022).…”

Section: Extension Of the Synthetic Magnitudesmentioning

confidence: 99%

Synthetic Population of Binary Cepheids. II. The effect of companion light on the extragalactic distance scale

Karczmarek¹,

Hajdu²,

Pietrzyński³

et al. 2023

Preprint

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Because of their period-luminosity relation (PLR), classical Cepheids play a key role in the calibration of the extragalactic distance scale and the determination of the Hubble-Lemaître constant H 0 . Recent findings show that the majority of classical Cepheids should be in binary or multiple systems, which might undermine their accuracy, as the extra-and unaccounted for-light from the companions of Cepheids causes a shift in the PLR. We quantify this shift using synthetic populations of binary Cepheids that we developed for this purpose, as described in Paper I of this series. We find that while all PLRs are shifted toward brighter values due to the excess light from the companions, the bias in the relative distance modulus between two galaxies hosting binary Cepheids can be either positive or negative, depending on the percentage of binary Cepheids in them. If the binarity percentage in the two galaxies is similar, the effect of binarity is canceled. Otherwise, it introduces a shift in the distance modulus of the order of millimags in the near-infrared passbands and Wesenheit indices, and tens of millimags in the visual domain; its exact value depends on the variant of the synthetic population (a unique combination of metallicity, star formation history, shape and location of the instability strip, and initial parameter distributions). Such shifts in distance moduli to type Ia supernova host galaxies introduce an additional statistical error on H 0 , which however does not prevent measuring H 0 with a precision of 1%.

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Section: Extension Of the Synthetic Magnitudesmentioning

confidence: 99%

Synthetic Population of Binary Cepheids. II. The effect of companion light on the extragalactic distance scale

Karczmarek¹,

Hajdu²,

Pietrzyński³

et al. 2023

Preprint

View full text Add to dashboard Cite

show abstract

“…We extended the list of magnitudes in anticipation of the vast and various data coming from the Vera Rubin and James Webb Space Telescope, which will also target classical Cepheids. The list of Wesenheit indices was extended due to the recent rise in popularity of the period-Wesenheit and period-Wesenheitmetallicity relations from Gaia data (Lin et al 2022;Ripepi et al 2022), and due to the ongoing discussion about the precision and accuracy of the Hubble-Lemai ̂tre constant, H 0 , the value of which was calculated-among others-using the W H index of classical Cepheids (Riess et al 2022).…”

Section: Extension Of the Synthetic Magnitudesmentioning

confidence: 99%

Synthetic Population of Binary Cepheids. II. The Effect of Companion Light on the Extragalactic Distance Scale

Karczmarek

Hajdu

Pietrzyński

et al. 2023

ApJ

View full text Add to dashboard Cite

Because of their period–luminosity relation (PLR), classical Cepheids play a key role in the calibration of the extragalactic distance scale and the determination of the Hubble–Lemaître constant H 0. Recent findings show that the majority of classical Cepheids should be in binary or multiple systems, which might undermine their accuracy, as the extra—and unaccounted for—light from the companions of Cepheids causes a shift in the PLR. We quantify this shift using synthetic populations of binary Cepheids that we developed for this purpose, as described in Paper I of this series. We find that while all PLRs are shifted toward brighter values due to the excess light from the companions, the bias in the relative distance modulus between two galaxies hosting binary Cepheids can be either positive or negative, depending on the percentage of binary Cepheids in them. If the binarity percentage in the two galaxies is similar, the effect of binarity is canceled. Otherwise, it introduces a shift in the distance modulus of the order of millimagnitudes in the near-infrared passbands and Wesenheit indices, and tens of millimagnitudes in the visual domain; its exact value depends on the variant of the synthetic population (a unique combination of metallicity, star formation history, shape and location of the instability strip, and initial parameter distributions). Such shifts in the distance moduli to Type Ia supernova host galaxies introduce an additional statistical error on H 0, which however does not prevent measuring H 0 with a precision of 1%.

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“…This newly developed method takes advantage of the stars in the OCs all having a similar distance, extinction, age, and metallicity, as well as the fact that the age distribution of OCs (ranging from several million years to several billion years; Kharchenko et al 2013) partially overlaps with the age range of DECPSs. After parallax corrections (Lindegren et al 2021, hereafter L21), this method has been proven to eliminate residual parallax offset (Riess et al 2022;Cruz Reyes & Anderson 2023), resulting in more accurate PWRs and PWZRs (e.g., Breuval et al 2020;Zhou & Chen 2021;Lin et al 2022;Riess et al 2022;Cruz Reyes & Anderson 2023). For example, Riess et al (2022) used 17 OC-DCEPs with Hubble Space Telescope (HST) photometry to calibrate the PWZR in the HST photometric system and determine a precise Hubble constant of H 0 = 73.01 ± 0.99 km s −1 Mpc −1 .…”

Section: Introductionmentioning

confidence: 99%

“…The first OC-DCEPs was discovered by Doig (1925), and searches for OC DECPSs have been active in the past decade (Anderson et al 2013;Chen et al 2015;Clark et al 2015;Chen et al 2017;Lohr et al 2018;Alonso-Santiago et al 2020;Breuval et al 2020;Negueruela et al 2020;Medina et al 2021;Zhou & Chen 2021;Hao et al 2022;Lin et al 2022;Cruz Reyes & Anderson 2023). Recently, there have been new searches for OCs (e.g., Hunt & Reffert 2023) based on Gaia data release 3 (DR3; Collaboration et al 2023).…”

Section: Introductionmentioning

confidence: 99%

Search for Classical Cepheids in Galactic Open Clusters and Calibration of the Period–Wesenheit–Metallicity Relation in the Gaia Bands

Wang,

Xu,

Lin

et al. 2024

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It is beneficial to calibrate the period–Wesenheit–metallicity relation (PWZR) of Delta Cephei stars (DCEPs), i.e., classical Cepheids, using accurate parallaxes of associated open clusters (OCs) from Gaia data release 3 (DR3). To this aim, we obtain a total of 43 OC–DCEPs (including 33 fundamental mode, 9 first overtone mode, and 1 multimode DCEPs) and calibrate the PWZR as W G = ( − 3.356 ± 0.033 ) ( log P − 1 ) + ( − 5.947 ± 0.025 ) + (−0.285 ± 0.064)[Fe/H]. The concurrently obtained residual parallax offset in OCs, zp = −4 ± 5 μas, demonstrates the adequacy of the parallax corrections within the magnitude range of OC member stars. By comparing the field DCEPs’ DR3 parallaxes with their photometric parallaxes derived by our PWZR, we estimated the residual parallax offset in field DCEPs as zp = −15 ± 3 μas. Using our PWZR, we estimate the distance modulus of the Large Magellanic Cloud to be 18.482 ± 0.040 mag, which aligns well with the most accurate published value obtained through geometric methods.

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Calibrating the Cepheid Period–Wesenheit Relation in the Gaia Bands Using Galactic Open-cluster Cepheids

Cited by 3 publications

References 49 publications

Synthetic Population of Binary Cepheids. II. The effect of companion light on the extragalactic distance scale

Synthetic Population of Binary Cepheids. II. The effect of companion light on the extragalactic distance scale

Synthetic Population of Binary Cepheids. II. The Effect of Companion Light on the Extragalactic Distance Scale

Search for Classical Cepheids in Galactic Open Clusters and Calibration of the Period–Wesenheit–Metallicity Relation in the Gaia Bands

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