A New Catalog of Agb Stars Based on Infrared Two-Color Diagrams

Suh, Kwang Wook; Hong, Jinju

doi:10.5303/jkas.2017.50.4.131

Cited by 21 publications

(14 citation statements)

References 11 publications

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“…maserdb.net) with all the YSOs in 8 nearby low mass star forming regions. One source (D31) that is also listed in Suh & Hong (2017) was detected in the SiO maser emission (Deguchi et al 2010) while the source D1184 was detected in the OH maser emission (Eder et al 1988). Both sources are very bright in the WISE bands to produce large uncertainties (> 0.2 mag) in the photometry, so they were excluded from our initial analyses.…”

Section: Megeath Et Al 2012; Esplin and Luhman 2019mentioning

confidence: 99%

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AGB interlopers in YSO catalogues hunted out by NEOWISE

Lee,

Lee

et al. 2021

Preprint

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AGBs and YSOs often share the same domains in IR color-magnitude or color-color diagrams leading to potential mis-classification. We extracted a list of AGB interlopers from the published YSO catalogues using the periodogram analysis on NEOWISE time series data. YSO IR variability is typically stochastic and linked to episodic mass accretion. Furthermore, most variable YSOs are at an early evolutionary stage, with significant surrounding envelope and/or disk material. In contrast, AGBs are often identified by a well defined sinusoidal variability with periods of a few hundreds days. From our periodogram analysis of all known low mass YSOs in the Gould Belt, we find 85 AGB candidates, out of which 62 were previously classified as late-stage Class III YSOs. Most of these new AGB candidates have similar IR colors to O-rich AGBs. We observed 73 of these AGB candidates in the H 2 O, CH 3 OH and SiO maser lines to further reveal their nature. The SiO maser emission was detected in 10 sources, confirming them as AGBs since low mass YSOs, especially Class III YSOs, do not show such maser emission. The H 2 O and CH 3 OH maser lines were detected in none of our targets.

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Section: Megeath Et Al 2012; Esplin and Luhman 2019mentioning

confidence: 99%

“…Figure 2 shows the color-color diagram of our AGB candidates overlaid on the known AGBs from Suh & Hong (2017). The O-rich and C-rich AGB stars can be roughly distinguished on the MIR color-color diagram using photometric data including the ALLWISE data (Suh 2018).…”

Section: Megeath Et Al 2012; Esplin and Luhman 2019mentioning

confidence: 99%

AGB interlopers in YSO catalogues hunted out by NEOWISE

Lee,

Lee

et al. 2021

Preprint

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“…In addition to the Arecibo sample, we show in Fig. 8 the distribution of periods of almost 1500 O-rich AGBs compiled by Suh & Hong (2017), and the sample of 108 long-period Mira variables in the Galactic Disk presented by Urago et al (2020). All distributions were normalized to their maximum value.…”

Section: Variability Properties Of Lplavsmentioning

confidence: 99%

An infrared study of Galactic OH/IR stars. III. Variability properties of the Arecibo sample

Jiménez-Esteban,

Engels,

Aguado

et al. 2021

Preprint

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We present the results of a near-infrared (NIR) monitoring program carried out between 1999 and 2005 to determine the variability properties of the 'Arecibo sample of OH/IR stars'. The sample consists of 385 IRAS-selected Asymptotic Giant Branch (AGB) candidates, for which their O-rich chemistry has been proven by the detection of 1612 MHz OH maser emission. The monitoring data was complemented by data collected from public optical and NIR surveys. We fitted the light curves obtained in the optical and NIR bands with a model using an asymmetric cosine function, and derived a period for 345 sources (∼ 90% of the sample). Based on their variability properties, most of the Arecibo sources are classified as long-period large-amplitude variable stars (LPLAV), 4% as (candidate) post-AGB stars, and 3% remain unclassified although they are likely post-AGB stars or highly obscured AGB stars. The period distribution of the LPLAVs peaks at ∼ 400 days, with periods between 300 and 800 days for most of the sources, and has a long tail up to ∼ 2100 days. Typically, the amplitudes are between 1 and 3 mag in the NIR and between 2 and 6 mag in the optical. We find correlations between periods and amplitudes, with larger amplitudes associated to longer periods, as well as between the period and the infrared colours, with the longer periods linked to the redder sources. Among the post-AGB stars, the light curve of IRAS 19566+3423 was exceptional, showing a large systematic increase (> 0.4 mag yr −1 ) in K-band brightness over 7 years.

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“…We now test which population could be the contaminant in the previous subsections. We start with AGB stars using the catalog of Suh & Hong (2017) for oxygen-rich (O-AGB) and carbon rich (C-AGB) stars and we add the the S stars from Suh & Kwon (2011). We only select objects with 2MASS photometry with quality flag AAA and we divide the samples into two regions: the inner Galactic plane (IGP, defined as the region with |l | 90 o and |b| 5 o and composed mostly of high-extinction Galactic disc and bulge stars), where the sample should experience significant extinction, and the rest of the sky, where NIR extinction should be small for most of the sample.…”

Section: What Is the Contaminant Population?mentioning

confidence: 99%

“…Also, O-AGB stars are known to be much more abundant than C-AGB stars in the bulge and that explains the result from the previous subsection, in which we found more contaminants in the central (bulge+disc) that in the lateral (disc) regions. Furthermore, the Suh & Hong (2017) sample is obviously just the tip of the iceberg of all O-AGB stars in the Galaxy (as many are missing in regions with very high extinction or that are highly crowded) and their J magnitudes fall in the middle of the range of our global 2MASS sample, so many more other stars of the same type must be hidden in our sample there. Therefore, O-AGB stars appear to be a good candidate for the dominant contaminant population.…”

Section: What Is the Contaminant Population?mentioning

confidence: 99%

Galactic extinction laws: I. A global NIR analysis with 2MASS photometry

Apellániz,

González,

Barbá

et al. 2020

Preprint

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We have started an ambitious program to determine if the full diversity of extinction laws is real or if some of it is due to calibration or methodological issues. Here we start by analyzing the information on NIR extinction in a 2MASS stellar sample with good quality photometry and very red colours. We calculate the extinction at 1 µm, A 1 , and the power-law exponent, α (A λ = A 1 λ −α ), for the 2MASS stars located in the extinction trajectory in the H − K vs. J − H plane expected for red giants with A 1 > 5 mag. We test the validity of the assumption about the nature of those stars, whether a single or multiple values of α are needed, and the spatial variations of the results. Most (∼83%) of those stars can indeed be explained by high-extinction red giants and the rest is composed of extinguished AGB stars (mostly O-rich), blended sources, and smaller numbers of other objects, a contaminant fraction that can be reduced with the help of Gaia DR2 data. Galactic red giants experience a NIR extinction with α ∼ 2.27 and an uncertainty of a few hundredths of a magnitude. There is no significant spread in α even though our sample is widely distributed and has a broad range of extinctions. Differences with previous results are ascribed to the treatment of non-linear photometric effects and/or the contaminant correction. Future research should concentrate in finding the correct functional form for the NIR extinction law. In the appendix we detail the treatment of non-linear photometric effects in the 2MASS bands.

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A New Catalog of Agb Stars Based on Infrared Two-Color Diagrams

Cited by 21 publications

References 11 publications

AGB interlopers in YSO catalogues hunted out by NEOWISE

AGB interlopers in YSO catalogues hunted out by NEOWISE

An infrared study of Galactic OH/IR stars. III. Variability properties of the Arecibo sample

Galactic extinction laws: I. A global NIR analysis with 2MASS photometry

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