<i>Wide-field Infrared Survey Explorer</i>
                    (
                    <i>WISE</i>
                    ) Catalog of Periodic Variable Stars

Chen, Xiaodian; Wang, Shu; Deng, Licai; Grijs, Richard de; Yang, Ming

doi:10.3847/1538-4365/aad32b

Cited by 118 publications

(91 citation statements)

References 56 publications

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“…They are affected by incompleteness for long periods (P > 10 days) and in crowded regions in the inner disk (because of the WISE observation model). The completeness of Cepheids in the WISE variables catalogue 8 is approximately 80% (with respect to the optical Cepheid catalogue 31 Our optical Cepheid sample is based on detections in optical passbands. The sample was compiled based on both Cepheid catalogues 30,31 and variable star catalogues [33][34][35][36][37] .…”

Section: Methodsmentioning

confidence: 98%

An intuitive 3D map of the Galactic warp’s precession traced by classical Cepheids

et al. 2019

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The Milky Way's neutral hydrogen (HI) disk is warped and flared 1, 2 . However, a dearth of accurate HI-based distances has thus far prevented the development of an accurate Galactic disk model. Moreover, the extent to which our Galaxy's stellar and gas disk morphologies are mutually consistent is also unclear. Classical Cepheids, primary distance indicators with distance accuracies of 3-5% 3 , offer a unique opportunity to develop an intuitive and accurate three-dimensional picture. Here, we establish a robust Galactic disk model based on 1339 classical Cepheids. We provide strong evidence that the warp's line of nodes is not oriented in the Galactic Center-Sun direction. Instead, it subtends a mean angle of 17.5 • ± 1 • (formal) ±3 • (systematic) and exhibits a leading spiral pattern. Our Galaxy thus follows Briggs' rule for spiral galaxies 4 , which suggests that the origin of the warp is associated with torques forced by the massive inner disk 5 . The stellar disk traced by Cepheids follows the gas disk in terms of their amplitudes; the stellar disk extends to at least 20 kpc 6,7 . This morphology provides a crucial, updated map for studies of the kinematics and archaeology of the Galactic disk.We have compiled samples of classical Cepheids from the Wide-field Infrared Survey Explorer (WISE) catalogue of periodic variables 8 (our 'WISE Cepheid sample') as well as from a number of optical surveys (collectively referred to as our 'optical Cepheid sample'). We will discuss both samples separately, because the catalogues' optical and infrared passbands are characterised by significantly different photometric and extinction sensitivities. Highly accurate Cepheid distances can be estimated using their well-established wavelength-dependent period-luminosity relations. To mitigate the influence of extinction in the Galactic plane and of photometric uncertainties at infrared wavelengths, we adopted the 'infrared multi-passband optimal distance method' 9 to determine accurate Cepheid distances. Contaminants, including Type-II Cepheids, long-period eclipsing binaries and quasi-periodic variables were removed using Gaia Data Release 2 parallaxes 10 .Cepheids located in areas centered on the Magellanic Clouds were also excluded. Careful sample selection resulted in a tally of 2330 classical Cepheids for further analysis.Distances were converted to 3D XY z and spherical Rφz coordinates by adopting a reference frame centered on the Galactic Center and a solar Galactocentric distance R 0 = 8.0 kpc. Here, φ is the Galactocentric angle in the anticlockwise direction (aligned with the disk's rotation axis) with respect to the solar position (φ = 0 • ). Since Gaia parallaxes are reliable within ∼5 kpc, we only selected Cepheids within the volume R < 20, |z| < 2 kpc to avoid significant contamination by Type-II Cepheids. Our downselection included 1459 Cepheids with distances accurate to <5%, corresponding to a distance modulus standard deviation <0.108 mag. Cepheids located clearly away from the best-fitting warp model (∆ > 1 kp...

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Section: Methodsmentioning

confidence: 98%

An intuitive 3D map of the Galactic warp’s precession traced by classical Cepheids

et al. 2019

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“…Although it is possible to derive periods based on the current data, the period search may be highly contaminated by the strong alias structures due to the very low sampling of WISE data as shown in Fig. 9; we only have twelve epochs spanning ∼3200 days and each epoch only covers about 5 to 10 days (we refer interested readers to Chen et al 2018 for the WISE catalog of periodic variable stars). In addition to MAD and SD, A91, page 6 of 17 the full amplitude (Amp = max mag − min mag ) was also calculated for each target.…”

Section: Multiwavelength Source Catalogmentioning

confidence: 99%

Evolved massive stars at low-metallicity

Yang

Bonanos

Jiang

et al. 2019

A&A

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We present a clean, magnitude-limited (IRAC1 or WISE1 ≤ 15.0 mag) multiwavelength source catalog for the Small Magellanic Cloud (SMC) with 45 466 targets in total, with the purpose of building an anchor for future studies, especially for the massive star populations at low-metallicity. The catalog contains data in 50 different bands including 21 optical and 29 infrared bands, retrieved from SEIP, VMC, IRSF, AKARI, HERITAGE, Gaia, SkyMapper, NSC, Massey (2002, ApJS, 141, 81), and GALEX, ranging from the ultraviolet to the far-infrared. Additionally, radial velocities and spectral classifications were collected from the literature, and infrared and optical variability statistics were retrieved from WISE, SAGE-Var, VMC, IRSF, Gaia, NSC, and OGLE. The catalog was essentially built upon a 1″ crossmatching and a 3″ deblending between the Spitzer Enhanced Imaging Products (SEIP) source list and Gaia Data Release 2 (DR2) photometric data. Further constraints on the proper motions and parallaxes from Gaia DR2 allowed us to remove the foreground contamination. We estimate that about 99.5% of the targets in our catalog are most likely genuine members of the SMC. Using the evolutionary tracks and synthetic photometry from MESA Isochrones & Stellar Tracks and the theoretical J − KS color cuts, we identified 1405 red supergiant (RSG), 217 yellow supergiant, and 1369 blue supergiant candidates in the SMC in five different color-magnitude diagrams (CMDs), where attention should also be paid to the incompleteness of our sample. We ranked the candidates based on the intersection of different CMDs. A comparison between the models and observational data shows that the lower limit of initial mass for the RSG population may be as low as 7 or even 6 M⊙ and that the RSG is well separated from the asymptotic giant branch (AGB) population even at faint magnitude, making RSGs a unique population connecting the evolved massive and intermediate stars, since stars with initial mass around 6 to 8 M⊙ are thought to go through a second dredge-up to become AGB stars. We encourage the interested reader to further exploit the potential of our catalog.

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“…Summarized refinement Criteria , the catalog of WISE variables (Chen et al 2018) and the variables from MACHO (Alcock et al 1997). Of the ∼220, 000 variables identified in this work, ∼131, 900 were previously discovered by other surveys, and ∼88, 300 are new discoveries, as also listed in Table 4.…”

Section: Classmentioning

confidence: 90%

The ASAS-SN catalogue of variable stars – V. Variables in the Southern hemisphere

Jayasinghe

Stanek

Kochanek

et al. 2019

Monthly Notices of the Royal Astronomical Society

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The All-Sky Automated Survey for Supernovae (ASAS-SN) provides long baseline (∼4 yrs) light curves for sources brighter than V 17 mag across the whole sky. As part of our effort to characterize the variability of all the stellar sources visible in ASAS-SN, we have produced ∼30.1 million V-band light curves for sources in the southern hemisphere using the APASS DR9 catalog as our input source list. We have systematically searched these sources for variability using a pipeline based on random forest classifiers. We have identified ∼220, 000 variables, including ∼88, 300 new discoveries. In particular, we have discovered ∼48, 000 red pulsating variables, ∼23, 000 eclipsing binaries, ∼2, 200 δ-Scuti variables and ∼10, 200 rotational variables. The light curves and characteristics of the variables are all available through the ASAS-SN variable stars database (https://asas-sn.osu.edu/variables). The pre-computed ASAS-SN Vband light curves for all the ∼30.1 million sources are available through the ASAS-SN photometry database (https://asas-sn.osu.edu/photometry). This effort will be extended to provide ASAS-SN light curves for sources in the northern hemisphere and for V 17 mag sources across the whole sky that are not included in APASS DR9.

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Wide-field Infrared Survey Explorer ( WISE ) Catalog of Periodic Variable Stars

Cited by 118 publications

References 56 publications

An intuitive 3D map of the Galactic warp’s precession traced by classical Cepheids

An intuitive 3D map of the Galactic warp’s precession traced by classical Cepheids

Evolved massive stars at low-metallicity

The ASAS-SN catalogue of variable stars – V. Variables in the Southern hemisphere

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