A Very Long Baseline Array Trigonometric Parallax for RR Aql and the Mira Period–Luminosity Relation

Sun, Yan; Zhang, Bo; Reid, M. J.; Xu, Shuangjing; Wen, Shiming; Zhang, Jingdong; Zheng, Xingwu

doi:10.3847/1538-4357/ac69e0

Cited by 10 publications

(9 citation statements)

References 40 publications

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“…Maser sources present a path forward for studying Mira periodmagnitude relations in the MW, as distances to these stars can be measured via maser parallaxes (e.g., Sun et al 2022). We explore circumstellar extinction and period-magnitude relations in a sample of SiO-maser-bearing sources near the GC in order to understand the biases that maser-bearing sources may introduce as compared to the general Mira population, as well as the effects of the high-metallicity environment of the Galactic bulge as compared to previously explored low-metallicity LMC populations.…”

Section: Discussionmentioning

confidence: 99%

“…To estimate the effects of variability in the K s band, we first transform the I-band light curve to one in the K s band using a phase-shift of 0.08051 and an amplitude ratio of 0.368 (Iwanek et al 2021); for J and H bands we use phase shifts of 0.02818 and 0.05430, and amplitude ratios of 0.613 and 0.463 respectively. The 2MASS photometric point is used to anchor this transformed lightcurve, and then an average magnitude is extracted, similar to the method used by Sun et al (2022). Average magnitudes calculated in this way are very rough given the large amount of time between the 2MASS and OGLE photometry (often ten years), and we note again that we do not use these average magnitudes in our extinction estimates.…”

Section: Error Budget Of Circumstellar Extinction Valuesmentioning

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: Discussionmentioning

confidence: 99%

Section: Error Budget Of Circumstellar Extinction Valuesmentioning

confidence: 99%

Long-period maser-bearing Miras in the Galactic center

Lewis¹,

Bhattacharya²,

Sjouwerman³

et al. 2023

A&A

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“…Out of these, 3 are protoplanetary nebulae/post-AGB stars and 26 are AGB stars, according to the SIMBAD 4 database. Three additional VERA sources were published by Chibueze et al (2020) and Sun et al (2022). We also considered the maser-emitting AGB stars in the sample presented in Xu et al (2019) which was compiled from the results of Vlemmings et al (2003); Kurayama et al (2005); Vlemmings & van Langevelde (2007), and Zhang et al (2017).…”

Section: Vlbi Samplementioning

confidence: 99%

Distance estimates for AGB stars from parallax measurements

Andriantsaralaza

Ramstedt

Vlemmings

et al. 2022

A&A

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Context. Estimating the distances to asymptotic giant branch (AGB) stars using optical measurements of their parallaxes is not straightforward because of the large uncertainties introduced by their dusty envelopes, their large angular sizes, and their surface brightness variability. Aims. This paper aims to assess the reliability of the distances derived with Gaia DR3 parallaxes for AGB stars, and provide a new distance catalogue for a sample of ∼ 200 nearby AGB stars Methods. We compared the parallaxes from Gaia DR3 with parallaxes measured with maser observations with very long baseline interferometry (VLBI) to determine a statistical correction factor for the DR3 parallaxes using a sub-sample of 33 maser-emitting oxygen-rich nearby AGB stars. We then calculated the distances of a total of ∼ 200 AGB stars in the DEATHSTAR project using a Bayesian statistical approach on the corrected DR3 parallaxes and a prior based on the previously determined Galactic distribution of AGB stars. We performed radiative transfer modelling of the stellar and dust emission to determine the luminosity of the sources in the VLBI sub-sample based on the distances derived from maser parallaxes, and derived a new bolometric period-luminosity relation for Galactic oxygen-rich Mira variables. Results. We find that the errors on the Gaia DR3 parallaxes given in the Gaia DR3 catalogue are underestimated by a factor of 5.44 for the brightest sources (G < 8 mag). Fainter sources (8 ≤ G < 12) require a lower parallax error inflation factor of 2.74. We obtain a Gaia DR3 parallax zero-point offset of −0.077 mas for bright AGB stars. The offset becomes more negative for fainter AGB stars. After correcting the DR3 parallaxes, we find that the derived distances are associated with significant, asymmetrical errors for more than 40 % of the sources in our sample. We obtain a PL relation of the form M bol = (−3.31 ± 0.24) [log P − 2.5] + (−4.317 ± 0.060) for the oxygen-rich Mira variables in the Milky Way. A new distance catalogue based on these results is provided for the sources in the DEATHSTAR sample. Conclusions. The corrected Gaia DR3 parallaxes can be used to estimate distances for AGB stars using the AGB prior, but we confirm that one needs to be careful when the uncertainties on parallax measurements are larger than 20 %, which can result in model-dependent distances and source-dependent offsets. We find that a RUWE (re-normalised unit weight error) below 1.4 does not guarantee reliable distance estimates and we advise against the use of only the RUWE to measure the quality of Gaia DR3 astrometric data for individual AGB stars.

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“…Accurate measurements of 3D motions require high-accuracy astrometry and radial velocity information. Due to the large uncertainties caused by their dusty envelopes, their large angular sizes, and their surface brightness variabilities, AGB stars are problematic targets for astrometry at optical wavelengths (e.g., Reid & Honma 2014;Andriantsaralaza et al 2022;Sun et al 2022). Furthermore, optical spectroscopic measurements can be significantly affected by extinction at large distances.…”

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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A Very Long Baseline Array Trigonometric Parallax for RR Aql and the Mira Period–Luminosity Relation

Cited by 10 publications

References 40 publications

Long-period maser-bearing Miras in the Galactic center

Long-period maser-bearing Miras in the Galactic center

Distance estimates for AGB stars from parallax measurements

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

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