A 3D Dust Map Based on Gaia, Pan-STARRS 1, and 2MASS

Abstract

We present a new three-dimensional map of dust reddening, based on Gaia parallaxes and stellar photometry from Pan-STARRS 1 and 2MASS. This map covers the sky north of a declination of −30 • , out to a distance of several kiloparsecs. This new map contains three major improvements over our previous work. First, the inclusion of Gaia parallaxes dramatically improves distance estimates to nearby stars. Second, we incorporate a spatial prior that correlates the dust density across nearby sightlines. This produces a smoother map, with more isotropic clouds and smaller distance uncertainties, particularly to clouds within the nearest kiloparsec. Third, we infer the dust density with a distance resolution that is four times finer than in our previous work, to accommodate the improvements in signal-to-noise enabled by the other improvements. As part of this work, we infer the distances, reddenings and types of 799 million stars. We obtain typical reddening uncertainties that are ∼30% smaller than those reported in the Gaia DR2 catalog, reflecting the greater number of photometric passbands that enter into our analysis. Our 3D dust map can be accessed at doi:10.7910/DVN/2EJ9TX or through the Python package dustmaps. Our catalog of stellar parameters can be accessed at

Gaia 18dvy: A New FUor in the Cygnus OB3 Association

“…Since Gaia18dvy is still surrounded by a circumstellar disk, and as the known precursors of most FUors are low-mass objects, we will adopt T eff =4330 K and A V =3 mag in the subsequent disk models. This choice is also supported by the fact that its extinction is broadly consistent with the value of A V 2 mag extracted from the 3D all-sky maps of Green et al (2019).…”

Time series of optical spectra of Nova V659 Sct

“…Applying the MMRD relation, we obtained an absolute visual magnitude for Nova V659 Sct of M V = − 8.8 mag and, thus, a distance of 7.5 kpc to it. In order to verify this result, we looked at the 3D Dust Mapping (http://argonaut.skymaps.info/) (Green et al 2019). In the direction of Nova V659 Sct, the distance of 7.5 kpc corresponds to an extinction of E ( g − r ) = 0.96, which roughly coincides with the aforementioned E ( B − V ) = 0.9.…”

FEDReD

“…Sale et al (2014) applied a hierarchical Bayesian method to infer stellar properties and extinction profiles with the IPHAS survey. Green et al (2014), also using a Bayesian method, derived an extinction map from Pan-STARRS data, later combined with Full Tables 1-5 and the extinction map are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/641/A79 2MASS data (Green et al 2015(Green et al , 2018 and the second Gaia data release (Gaia DR2; Green et al 2019) data. Capitanio et al (2017) and Lallement et al (2019) used a Bayesian inversion technique described in Vergely et al (2001) on composite dust proxies with Gaia DR1 parallax and on 2MASS crosmatched with Gaia DR2 respectively.…”