The M33 Synoptic Stellar Survey. II. Mira Variables

Yuan, Wenlong; He, Shiyuan; Macri, Lucas M.; Long, James P.; Huang, Jianhua Z.

doi:10.3847/1538-3881/aa63f1

Cited by 31 publications

(50 citation statements)

References 30 publications

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“…We based our study on NIR observations of M33 with: (1) the 3.8 m UK InfraRed Telescope (UKIRT, previously published by Javadi et al 2015), (2) the 4-m Mayall telescope at Kitt Peak National Observatory (KPNO, published here for the first time) and (3) the 8-m Gemini North telescope (also published here for the first time). We further make use of previously-published Iband time-series photometry obtained by the DIRECT project and follow-up observations Pellerin & Macri 2011), which were analyzed to search for Mira variables by Yuan et al (2017a). The sky coverage of the aforementioned NIR surveys are shown in Figure 1.…”

Section: Datamentioning

confidence: 99%

“…The sky coverage of the aforementioned NIR surveys are shown in Figure 1. We cross-matched stellar sources (including Mira candidates from Yuan et al 2017a) among these datasets by updating all their astrometry to a single reference frame (defined by the UKIRT catalog). In the rest of the section, we describe the observations, data reduction, photometry, and astrometric calibration for each dataset.…”

Section: Datamentioning

confidence: 99%

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Near-infrared Mira Period–Luminosity Relations in M33

Yuan

Macri

Javadi

et al. 2018

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We analyze sparsely-sampled near-infrared (JHK s ) light curves of a sample of 1781 Mira variable candidates in M33, originally discovered using I-band time-series observations. We extend our single-band semi-parametric Gaussian process modeling of Mira light curves to a multi-band version and obtain improved period determinations. We use our previous results on near-infrared properties of candidate Miras in the LMC to classify the majority of the M33 sample into Oxygen-or Carbon-rich subsets. We derive Period-Luminosity relations for O-rich Miras and determine a distance modulus for M33 of 24.80 ± 0.06 mag.

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Section: Datamentioning

confidence: 99%

Section: Datamentioning

confidence: 99%

Near-infrared Mira Period–Luminosity Relations in M33

Yuan

Macri

Javadi

et al. 2018

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“…-The H0 with two anchors and the slope fit using F160W (−3.35) is our preferred value. The linear PLR for NGC 4258 for the gold sample of Miras from H18 with the F160W slope derived from the OGLE LMC O-rich Mira data (left) and the H -band slope fromYuan et al (2017a). H18 originally used only a quadratic PLR.…”

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confidence: 99%

Hubble Space Telescope Observations of Mira Variables in the SN Ia Host NGC 1559: An Alternative Candle to Measure the Hubble Constant

Huang

Riess

Yuan

et al. 2020

ApJ

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We present year-long, near-infrared Hubble Space Telescope WFC3 observations used to search for Mira variables in NGC 1559, the host galaxy of the Type Ia supernova (SN Ia) 2005df. This is the first dedicated search for Miras, highly-evolved low-mass stars in a SN Ia host and subsequently the first calibration of the SN Ia luminosity using Miras in a role historically played by Cepheids. We identify a sample of 115 O-rich Miras with P < 400 day based on their light curve properties. We find that the scatter in the Mira Period-Luminosity Relation (PLR) is comparable to Cepheid PLRs seen in SN Ia supernova host galaxies. Using a sample of O-rich Miras discovered in NGC 4258 with HST F160W and its maser distance, we measure a distance modulus for NGC 1559 of µ 1559 = 31.41 ± 0.050 (statistical) ±0.052 (systematic) mag. Based on the light curve of the normal, well-observed, low-reddening SN 2005df, we obtain a measurement of the fiducial SN Ia absolute magnitude of M 0 B = −19.27 ± 0.13 mag. With the Hubble diagram of SNe Ia we find H 0 = 72.7 ± 4.5 km s −1 Mpc −1 . Combining the calibration from the NGC 4258 megamaser and the Large Magellanic Cloud detached eclipsing binaries gives a best value of H 0 = 73.3 ± 3.9 km s −1 Mpc −1 . This result is within 1σ of the Hubble constant derived using Cepheids and multiple calibrating SNe Ia. This is the first of four expected calibrations of the SN Ia luminosity from Miras which should reduce the error in H 0 via Miras to ∼ 3%. In light of the present Hubble tension and JWST, Miras have utility in the extragalactic distance scale to check Cepheid distances or calibrate nearby SNe in early-type host galaxies that would be unlikely targets for Cepheid searches.

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“…10). [33], [34] and [35] Figure 9. Application of the Gaussian Process to model simulated Mira light curves that are noisy and sparsely sampled (left) and success in recovering the known periods of the variables used to generate the simulations (right).…”

Section: Miras: New Techniques and Prospects For Lsstmentioning

confidence: 99%

“…9). We applied the technique to I-band observations of M33 ( [37,38]) and discovered over 1800 Mira candidates in this galaxy ( [35]). We matched our optical catalog with NIR and MIR observations from [39,40] and obtained PLRs that compare favorably to their LMC counterparts (see Fig.…”

Section: Miras: New Techniques and Prospects For Lsstmentioning

confidence: 99%

Pulsating stars and the distance scale

Macri

2017

EPJ Web Conf.

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Abstract. I present an overview of the latest results from the SH0ES project, which obtained homogeneous Hubble Space Telescope (HST) photometry in the optical and nearinfrared for ∼ 3500 and ∼ 2300 Cepheids, respectively, across 19 supernova hosts and 4 calibrators to determine the value of H 0 with a total uncertainty of 2.4%. I discuss the current 3.4σ "tension" between this local measurement and predictions of H 0 based on observations of the CMB and the assumption of "standard" ΛCDM. I review ongoing efforts to reach σ(H 0 ) = 1%, including recent advances on the absolute calibration of Milky Way Cepheid period-luminosity relations (PLRs) using a novel astrometric technique with HST. Lastly, I highlight recent results from another collaboration on the development of new statistical techniques to detect, classify and phase extragalactic Miras using noisy and sparsely-sampled observations. I present preliminary Mira PLRs at various wavelengths based on the application of these techniques to a survey of M33.

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The M33 Synoptic Stellar Survey. II. Mira Variables

Cited by 31 publications

References 30 publications

Near-infrared Mira Period–Luminosity Relations in M33

Near-infrared Mira Period–Luminosity Relations in M33

Hubble Space Telescope Observations of Mira Variables in the SN Ia Host NGC 1559: An Alternative Candle to Measure the Hubble Constant

Pulsating stars and the distance scale

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