A Three-dimensional Map of the Milky Way Using 66,000 Mira Variable Stars

Iwanek, P.; Poleski, R.; Kozłowski, S.; Soszyński, I.; Pietrukowicz, P.; Ban, Makiko; Skowron, J.; Mróz, P.; Wrona, Marcin; Udalski, A.; Szymański, M. K.; Skowron, D. M.; Ulaczyk, K.; Gromadzki, M.; Rybicki, K.; Ratajczak, M.

doi:10.3847/1538-4365/acad7a

Cited by 12 publications

(13 citation statements)

References 123 publications

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“…Further, the lack of precise and accurate distance estimates, interstellar extinction, variability-related, and period-magnitude-relation uncertainties have an almost equally large impact, especially in the K s band. We note again that neither Gaia parallaxes nor the PLR-derived distance from Iwanek et al (2023) are well suited to these distant stars near the plane with significant envelopes.…”

Section: Error Budget Of Circumstellar Extinction Valuesmentioning

confidence: 69%

“…Of course this sample selection method depends on a different set of assumptions, namely that high velocity (>100 km s −1 ) Mira variables within 4 degrees of l,b=0,0 are at the distance of the GC, i.e., 8 kpc from the Sun (i.e., Gravity Collaboration et al 2019;Reid et al 2019;Do et al 2019;Iwanek et al 2023). We note that reliable Gaia data is sparse for this sample given the proximity to the Galactic plane and the large distances.…”

Section: Data and Sample Selectionmentioning

confidence: 99%

“…Further, Gaia parallaxes do not lead straightforwardly to accurate distances for Mira variables (Andriantsaralaza et al 2022); thus Gaia parallaxes are not employed. We also did not adopt the period-based distance estimates for OGLE Miras given by Iwanek et al (2023) as these are unlikely to be accurate for highly obscured stars. See Sect.…”

Section: Data and Sample Selectionmentioning

confidence: 99%

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Long-period maser-bearing Miras in the Galactic center

Lewis¹,

Bhattacharya²,

Sjouwerman³

et al. 2023

A&A

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We establish a sample of 370 Mira variables that are likely near the Galactic center (GC). The sources have been selected from the OGLE and BAaDE surveys based on their sky coordinates, OGLE classifications, and BAaDE maser-derived line-of-sight velocities. As the distance to the GC is known to a high accuracy, this sample is a test bed for reddening and extinction studies toward the GC and in Mira envelopes. We calculated separate interstellar-and circumstellar-extinction values for individual sources, showing that there is a wide range of circumstellar extinction values (up to four magnitudes in the K s band) in the sample, and that circumstellar reddening is statistically different from interstellar reddening laws. Further, the reddening laws in the circumstellar environments of our sample and the circumstellar environments of Large Magellanic Cloud (LMC) Miras are strikingly similar despite the different metallicities of the samples. Period-magnitude relations for the mid-infrared (MIR) WISE and MSX bands are also explored, and in the WISE bands we compare these to period-magnitude relationships derived from Miras in the LMC as it is important to compare these LMC relations to those in a higher metallicity environment. Emission from the envelope itself may contaminate MIR magnitudes altering the relations, especially for sources with thick envelopes.

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Section: Error Budget Of Circumstellar Extinction Valuesmentioning

confidence: 69%

Section: Data and Sample Selectionmentioning

confidence: 99%

Section: Data and Sample Selectionmentioning

confidence: 99%

See 1 more Smart Citation

Long-period maser-bearing Miras in the Galactic center

Lewis¹,

Bhattacharya²,

Sjouwerman³

et al. 2023

A&A

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“…Asymptotic giant branch (AGB) stars are in the late stages of stellar evolution and, due to their mass loss, are dominating contributors to the cosmic gas/dust cycle (e.g., Höfner & Olofsson 2018). With typical ages of a few gigayears (e.g., Sevenster 1999;Höfner & Olofsson 2018), AGB stars are found in all structures of the Milky Way 9 including the Galactic thin disk, thick disk, bulge, halo, and even the tidal stellar streams produced by the interaction of the Milky Way with its satellites (e.g., Li et al 2019;Suh 2021;Iwanek et al 2023). The three-dimensional (3D) motions of AGB stars located off the Galactic disk can provide a crucial clue on their nature, potentially shedding light on the formation history of our Galaxy.…”

Section: Introductionmentioning

confidence: 99%

Maser Investigation toward Off-Plane Stars (MIOPS): Detection of SiO Masers in the Galactic Thick Disk and Halo

Yang 杨,

Wu 吴,

Gong 龚

et al. 2024

ApJ

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Studying stars that are located off the Galactic plane is important for understanding the formation history of the Milky Way. We searched for SiO masers toward off-plane O-rich asymptotic giant branch (AGB) stars from the catalog presented by Mauron et al. in order to shed light on the origins of these objects. A total of 102 stars were observed in the SiO J = 1−0, v = 1 and 2 transitions with the Effelsberg 100 m and Tianma 65 m telescopes. SiO masers were discovered in eight stars, all first detections. The measured maser velocities allow for initial estimates of the host AGB stars’ radial velocities. We find that the radial velocities of three stars (namely G068.881−24.615, G070.384−24.886, and G084.453−21.863) significantly deviate from the values expected from Galactic circular motion. The updated distances and 3D motions indicate that G068.881−24.615 is likely located in the Galactic halo, while G160.648−08.846 is probably located in the Galactic thin disk, and the other six stars are probably part of the Galactic thick disk.

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“…Several previous studies have used SRVs and Miras to probe the structure of the Milky Way (Trabucchi et al 2017(Trabucchi et al , 2019(Trabucchi et al , 2021Iwanek et al 2023), and demonstrated that calibrated PL sequences can yield distances to within 15% precision (Tabur et al 2010;Auge et al 2020). However, sample sizes have so far remained limited and did not include pulsation amplitudes as an additional constraint (which increases the distance precision further; Rau et al 2019).…”

Section: Introductionmentioning

confidence: 99%

The Far Side of the Galactic Bar/Bulge Revealed through Semi-regular Variables

Hey,

Huber,

Shappee

et al. 2023

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The Galactic bulge is critical to our understanding of the Milky Way. However, due to the lack of reliable stellar distances, the structure and kinematics of the bulge/bar beyond the Galactic center have remained largely unexplored. Here, we present a method to measure distances of luminous red giants using a period–amplitude–luminosity relation anchored to the Large Magellanic Cloud, with random uncertainties of 10%–15% and systematic errors below 1%–2%. We apply this method to data from the Optical Gravitational Lensing Experiment to measure distances to 190,302 stars in the Galactic bulge and beyond out to 20 kpc. Using this sample, we measure a distance to the Galactic center of R 0 = 8108 ± 106stat ± 93sys pc, consistent with direct measurements of stars orbiting Sgr A*. We cross-match our distance catalog with Gaia DR3 and use the subset of 39,566 overlapping stars to provide the first constraints on the Milky Way’s velocity field (V R , V ϕ , V z ) beyond the Galactic center. We show that the V R quadrupole from the bar’s near side is reflected with respect to the Galactic center, indicating that the bar is bisymmetric and aligned with the inner disk. We also find that the vertical height V Z map has no major structure in the region of the Galactic bulge, which is inconsistent with a current episode of bar buckling. Finally, we demonstrate with N-body simulations that distance uncertainty plays a factor in the alignment of the major and kinematic axes of the bar, necessitating caution when interpreting results for distant stars.

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A Three-dimensional Map of the Milky Way Using 66,000 Mira Variable Stars

Cited by 12 publications

References 123 publications

Long-period maser-bearing Miras in the Galactic center

Long-period maser-bearing Miras in the Galactic center

Maser Investigation toward Off-Plane Stars (MIOPS): Detection of SiO Masers in the Galactic Thick Disk and Halo

The Far Side of the Galactic Bar/Bulge Revealed through Semi-regular Variables

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