Three-dimensional Structure of the Milky Way Dust: Modeling of LAMOST Data

Li, Linlin; Shen, Shiyin; Hou, Jinliang; Yuan, Haibo; Xiang, Maosheng; Chen, Bingqiu; Huang, Yang; Liu, Xiaowei

doi:10.3847/1538-4357/aabaef

Cited by 33 publications

(20 citation statements)

References 64 publications

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“…The best-fit model has (N f b,0 [cm −2 ] = 10 22.08 , b 0N = −0.05 • , σ N = 0.66 • ) and (T f b,0 = 24.8K, b 0T = −0.17 • , σ T = 5.75 • ), notice that T f b is almost constant across the region. σ N = 0.66 • corresponds to a scale height of 97 pc, consistent with previous findings (Jones et al 2011;Li et al 2018).…”

Section: Fore/background Estimatessupporting

confidence: 91%

AzTEC Survey of the Central Molecular Zone: Increasing Spectral Index of Dust with Density

Tang,

Wang,

Wilson

2020

Preprint

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The Central Molecular Zone (CMZ) of our Galaxy hosts an extreme environment analogous to that found in typical starburst galaxies in the distant universe. In order to understand dust properties in environments like our CMZ, we present results from a joint SED analysis of our AzTEC/Large Millimeter Telescope survey, together with existing Herschel far-IR data on the CMZ, from a wavelength range of 160 µm to 1.1 mm. We include global foreground and background contributions in a novel Bayesian modeling that incorporates the Point Spread Functions (PSFs) of the different maps, which enables the full utilization of our high resolution (10.5 ′′ ) map at 1.1 mm and reveals unprecedentedly detailed information on the spatial distribution of dusty gas across the CMZ. There is a remarkable trend of increasing dust spectral index β, from 2.0 − 2.4, toward dense peaks in the CMZ, indicating a deficiency of large grains or a fundamental change in dust optical properties. This environmental dependence of β could have a significant impact on the determination of dust temperature in other studies. Depending on how the optical properties of dust deviate from the conventional model, dust temperatures could be underestimated by 10 − 50% in particularly dense regions.

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Section: Fore/background Estimatessupporting

confidence: 91%

AzTEC Survey of the Central Molecular Zone: Increasing Spectral Index of Dust with Density

Tang,

Wang,

Wilson

2020

Preprint

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“…For the single-disk model, we obtain an average scale-height of 205.5±1.5 pc. This value is slightly larger than reported in the literature (Li et al 2018;Jones et al 2011;Drimmel & Spergel 2001). This is mainly caused by the poor fitting in the current work.…”

Section: The Global Distribution Of the Milky Way Dustcontrasting

confidence: 81%

“…Jones et al (2011) studied the 3D dust distribution of the Milky Way from the spectroscopic data of SDSS and obtained a scale-height of 119 pc for the Solar neighbourhood. Most recently, Li et al (2018) presented a model of Galactic dust distribution that has a scalelength of 3,192 pc and a scale-height of 103 pc, based on the LAMOST spectroscopic data. All the above analyses assume that dust grains in the Milky Way are distributed in a single disk.…”

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confidence: 99%

Three-Dimensional Distribution of the Interstellar Dust in the Milky Way

Guo,

Chen,

Yuan

et al. 2020

Preprint

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We present a three-dimensional (3D) extinction map of the southern sky. The map covers the SkyMapper Southern Survey (SMSS) area of ∼ 14,000 deg 2 and has spatial resolutions between 6.9 and 27 arcmin. Based on the multi-band photometry of SMSS, the Two Micron All Sky Survey, the Wide-Field Infrared Survey Explorer Survey and the Gaia mission, we have estimated values of the r-band extinction for ∼ 19 million stars with the spectral energy distribution (SED) analysis. Together with the distances calculated from the Gaia data release 2 (DR2) parallaxes, we have constructed a three-dimensional extinction map of the southern sky. By combining our 3D extinction map with those from the literature, we present an all-sky 3D extinction map, and use it to explore the 3D distribution of the Galactic dust grains. We use two different models, one consisting a single disk and an other of two disks, to fit the 3D distribution of the Galactic dust grains. The data is better fitted by a two-disk model, yielding smaller values of the Bayesian Information Criterion (BIC). The best fit model has scale heights of 73 and 225 pc for the "thin" and "thick" dust disks, respectively.

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“…For the latter it is common practice not to correct for it, based on a number of arguments (Feldmeier et al 1997). In the case of the Milky Way, PNe have a higher vertical scale height (Bobylev & Bajkova 2017) than dust (Li et al 2018). If PNe are equally distributed in front of and behind the dust, we will observe about half of the sample with minimal extinction.…”

Section: Source Detection and Photometrymentioning

confidence: 94%

Planetary Nebula Luminosity Function distances for 19 galaxies observed by PHANGS-MUSE

Scheuermann,

Kreckel,

Anand

et al. 2022

Preprint

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We provide new planetary nebula luminosity function (PNLF) distances to 19 nearby spiral galaxies that were observed with VLT/MUSE by the PHANGS collaboration. Emission line ratios are used to separate planetary nebulae (PNe) from other bright [O ] emitting sources like compact supernovae remnants (SNRs) or H regions. While many studies have used narrowband imaging for this purpose, the detailed spectral line information provided by integral field unit (IFU) spectroscopy grants a more robust way of categorising different [O ] emitters. We investigate the effects of SNR contamination on the PNLF and find that we would fail to classify all objects correctly, when limited to the same data narrowband imaging provides. However, the few misclassified objects usually do not fall on the bright end of the luminosity function, and only in three cases does the distance change by more than 1𝜎. We find generally good agreement with literature values from other methods. Using metallicity constraints that have also been derived from the same IFU data, we revisit the PNLF zero point calibration. Over a range of 8.34 < 12 + log(O/H) < 8.59, our sample is consistent with a constant zero point and yields a value of 𝑀 * = −4.542 +0.103 −0.059 mag, within 1𝜎 of other literature values. MUSE pushes the limits of PNLF studies and makes galaxies beyond 20 Mpc accessible for this kind of analysis. This approach to the PNLF shows great promise for leveraging existing archival IFU data on nearby galaxies.

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Three-dimensional Structure of the Milky Way Dust: Modeling of LAMOST Data

Cited by 33 publications

References 64 publications

AzTEC Survey of the Central Molecular Zone: Increasing Spectral Index of Dust with Density

AzTEC Survey of the Central Molecular Zone: Increasing Spectral Index of Dust with Density

Three-Dimensional Distribution of the Interstellar Dust in the Milky Way

Planetary Nebula Luminosity Function distances for 19 galaxies observed by PHANGS-MUSE

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