2014A&A...566A.120S


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.14CEST18:48:57

2014A&A...566A.120S - Astronomy and Astrophysics, volume 566A, 120-120 (2014/6-1)

Mapping the Milky Way bulge at high resolution: the 3D dust extinction, CO, and X factor maps.

SCHULTHEIS M., CHEN B.Q., JIANG B.W., GONZALEZ O.A., ENOKIYA R., FUKUI Y., TORII K., REJKUBA M. and MINNITI D.

Abstract (from CDS):

Three dimensional interstellar extinction maps provide a powerful tool for stellar population analysis. However, until now, these 3D maps were rather limited by sensitivity and spatial resolution. We use data from the VISTA Variables in the Via Lactea survey together with the Besancon stellar population synthesis model of the Galaxy to determine interstellar extinction as a function of distance in the Galactic bulge covering -10°<l<10° and -10°<b<5°. We adopted a recently developed method to calculate the colour excess. First we constructed the H-Ks vs. Ks and J-Ks vs. Ks colour-magnitude diagrams based on the VVV catalogues that matched 2MASS. Then, based on the temperature-colour relation for M giants and the distance-colour relations, we derived the extinction as a function of distance. The observed colours were shifted to match the intrinsic colours in the Besancon model as a function of distance iteratively. This created an extinction map with three dimensions: two spatial and one distance dimension along each line of sight towards the bulge. We present a 3D extinction map that covers the whole VVV area with a resolution of 6'x6' for J-Ks and H-Ks using distance bins of 0.5kpc. The high resolution and depth of the photometry allows us to derive extinction maps for a range of distances up to 10kpc and up to 30 mag of extinction in AV (3.0mag in AKs). Integrated maps show the same dust features and consistent values as other 2D maps. We discuss the spatial distribution of dust features in the line of sight, which suggests that there is much material in front of the Galactic bar, specifically between 5-7kpc. We compare our dust extinction map with the high-resolution 12CO maps (NANTEN2) towards the Galactic bulge, where we find a good correlation between 12CO and AV. We determine the X factor by combining the CO map and our dust extinction map. Our derived average value X=2.5±0.47x1020cm–2K–1km–1s is consistent with the canonical value of the Milky Way. The X-factor decreases with increasing extinction.

Abstract Copyright:

Journal keyword(s): Galaxy: bulge - dust, extinction - Galaxy: stellar content

VizieR on-line data: <Available at CDS (J/A+A/566/A120): table1jk.dat table1hk.dat>

Simbad objects: 10

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Number of rows : 10

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME NGP reg 12 51 26.275 +27 07 41.70           ~ 1020 0
2 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3027 0
3 NAME the Pipe Nebula DNe 17 30 -25.0           ~ 333 1
4 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11542 0
5 NAME Baade Window reg 18 03.5 -30 01           ~ 528 3
6 M 28 GlC 18 24 32.89 -24 52 11.4           ~ 662 0
7 NGC 6658 GiG 18 33 55.6323002609 +22 53 17.735096994   15.0       ~ 35 0
8 NAME Galactic Bar reg ~ ~           ~ 894 0
9 NAME Local Group GrG ~ ~           ~ 6973 0
10 NAME Galactic Bulge reg ~ ~           ~ 3391 0

    Equat.    Gal    SGal    Ecl

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2020.07.14-18:48:57

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