A THREE-DIMENSIONAL MAP OF MILKY WAY DUST

By Gregory M. Green, Edward F. Schlafly, Douglas P. Finkbeiner, Hans-Walter Rix, N. Martin, W. Burgett, P. Draper, H. Flewelling, K. Hodapp, N. Kaiser and 6 more. 2015

351 citations recorded by the source corpus.

We present a three-dimensional map of interstellar dust reddening, covering three-quarters of the sky out to a distance of several kiloparsecs, based on Pan-STARRS 1 (PS1) and 2MASS photometry. The map reveals a wealth of detailed structure, from filaments to large cloud complexes. The map has a hybrid angular resolution, with most of the map at an angular resolution of 3 &farcm; 4 ?> – 13 &farcm; 7 ?> , and a maximum distance resolution of ∼ 25 % ?> . The three-dimensional distribution of dust is determined in a fully probabilistic framework, yielding the uncertainty in the reddening distribution along each line of sight, as well as stellar distances, reddenings, and classifications for 800 million stars detected by PS1. We demonstrate the consistency of our reddening estimates with those of two-dimensional emission-based maps of dust reddening. In particular, we find agreement with the Planck τ 353 GHz ?> -based reddening map to within 0.05 mag ?> in E ( B - V ) ?> to a depth of 0.5 mag ?> , and explore systematics at reddenings less than E ( B - V ) ≈ 0.08 mag ?> . We validate our per-star reddening estimates by comparison with reddening estimates for stars with both Sloan Digital Sky Survey photometry and Sloan Extension for Galactic Understanding and Exploration spectral classifications, finding per-star agreement to within 0.1 mag ?> out to a stellar E ( B - V ) ?> of 1 mag. We compare our map to two existing three-dimensional dust maps, by Marshall et al. and Lallement et al., demonstrating our finer angular resolution, and better distance resolution compared to the former within ∼ 3 kpc ?> . The map can be queried or downloaded at http://argonaut.skymaps.info. We expect the three-dimensional reddening map presented here to find a wide range of uses, among them correcting for reddening and extinction for objects embedded in the plane of the Galaxy, studies of Galactic structure, calibration of future emission-based dust maps, and determining distances to objects of known reddening.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/8aa6e54372c2eb9b7266478d13c6b50860ca8020

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In Astronomy and Astrophysics

1. Hans-Walter Rix
2. I. Minchev
3. Jo Bovy
4. C. Chiappini
5. M. Martig
6. D. Huber
7. S. Majewski
8. Timothy C. Beers

Citations in the corpus

• Confirming chemical clocks: asteroseismic age dissection of the Milky Way disc(s) (2017, methodology): “From the derived distance and coordinates of the target, we recompute the extinction value using the Green et al. (2015) reddening map.”
• The age–metallicity structure of the Milky Way disc using APOGEE (2017, background): “…for the Milky Way MNRAS 000, 1–21 (2017) derived by Marshall et al. (2006) for the inner disk plane, combined with those for a large majority of the APOGEE footprint by (Green et al. 2015), adopting conversions AH/AKS = 1.48 and AH/E(B − V) = 0.46 (Schlafly & Finkbeiner 2011; Yuan et al. 2013).”
• A compendium of distances to molecular clouds in the Star Formation Handbook (2020, methodology): “…(in the optical and near-infrared bands) as a function of distance, extinction, stellar type, and RV using a technique similar to that outlined in Green et al. (2014, 2015, 2018): m̂ = mint(Mr, [Fe/H]) + AV × (R + RV × R′) + µ (1) Here, mint is the set of intrinsic (un-reddened) magnitudes for…”
• Asteroseismology and Gaia: Testing Scaling Relations Using 2200 Kepler Stars with TGAS Parallaxes (2017, methodology): “To estimate AV,we used the 3D reddening map by Green et al. (2015), as implemented in the mwdust package by Bovy et al. (2016).”
• dustmaps: A Python interface for maps of interstellar dust (2018, methodology): “The left panel is a plot of dust reddening in Green et al. (2018) to a distance of 800 pc, while the right panel shows the correlation between Green et al. (2018) and Planck Collaboration et al. (2014).”
• Galactic reddening in 3D from stellar photometry – an improved map (2018, methodology): “These individual stellar inferences (which we here term the ‘raw’ inferences) are then used to infer the line-of-sight reddening, as described in Green et al. (2014, 2015).”
• Red Clump Stars from LAMOST II: the outer disc of the Milky Way (2017, background): “Indeed, Green et al. (2015) indicated that there are clouds with larger interstellar extinction located at a distance of 794–1995pc, in the region l ∼ 180◦ and below b = 0◦, which may be associated with the shallow dip.”
• Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18 (2019, methodology): “In principle, our results can thus be used to construct 3D extinction maps (e.g. Schlafly & Finkbeiner 2011; Green et al. 2015) and infer the three-dimensional dust distribution in the extended solar vicinity (e.g. Capitanio et al. 2017; Rezaei Kh. et al. 2018; Lallement et al. 2019; Zucker et al.…”
• Revised Radii of Kepler Stars and Planets Using Gaia Data Release 2 (2018, methodology): “We determined the latter by comparing the Green et al. (2015) map with the Green et al. (2018) map for our sample, yielding a median absolute deviation of ∼ 22%, which we adopt as a fractional uncertainty for our reported extinction values.”
• Mapping the Milky Way with LAMOST– III. Complicated spatial structure in the outer disc (2018, methodology): “D extinction model provided by Green et al. (2014, 2015) at a few lines-of-sight with high extinction in the GAC region.”
• Gaia-2MASS 3D maps of Galactic interstellar dust within 3 kpc (2019, methodology): “…the IPHAS Survey to simultaneously reconstruct stellar properties and extinction radial profiles at a 10′ resolution for -5≤b≤5◦ and 30≤l≤210◦ up to 5 kpc. Green et al. (2015, 2018) used 2MASS and PanSTARRS 1 and a refined Bayesian method to derive reddening radial profiles at very high angular…”
• THE STELLAR POPULATION STRUCTURE OF THE GALACTIC DISK (2015, methodology): “All mock data assume extinction according to the Green et al. (2015) map and properly take into account the variation of the density profile within each APOGEE field, therefore testing that this can be ignored in the calculation of the effective volume (see above).”
• Three-dimensional mapping of the local interstellar medium with composite data (2017, methodology): “…species (Marshall et al. 2006; Vergely et al. 2010; van Loon et al. 2013; Welsh et al. 2010; Lallement et al. 2014; Schlafly et al. 2014; Sale & Magor- rian 2014a; Kos et al. 2014; Schultheis et al. 2014; Zasowski et al. 2015; Green et al. 2015; Schlafly et al. 2015; Rezaei Kh. et al. 2016).”