@article{PAR00011483,
  title = {3{D} maps of the local {ISM} from inversion of individual color excess measurements},
  author = {{L}allement, {R}. and {V}ergely, {J}. {L}. and {V}alette, {B}ernard and {P}uspitarini, {L}. and {E}yer, {L}. and {C}asagrande, {L}.},
  editor = {},
  language = {{ENG}},
  abstract = {{A}ims. {T}hree-dimensional (3{D}) maps of the {G}alactic interstellar matter ({ISM}) are a potential tool of wide use, but accurate and detailed maps are still lacking. {O}ne of the ways to construct the maps is to invert individual distance-limited {ISM} measurements, a method we have applied here to measurements of stellar color excess in the optical. {M}ethods. {W}e assembled color excess data together with the associated parallax or photometric distances to constitute a catalog of similar or equal to 23 000 sightlines for stars within 2.5 kpc. {T}he photometric data are taken from {S}tromgren catalogs, the {G}eneva photometric database, and the {G}eneva-{C}openhagen survey. {W}e also included extinctions derived towards open clusters. {W}e applied an inversion method based on a regularized {B}ayesian approach to this color excess dataset, a method previously used for mapping at closer distances. {R}esults. {W}e show the dust spatial distribution resulting from the inversion by means of planar cuts through the differential opacity 3{D} distribution, and by means of 2{D} maps of the integrated opacity from the {S}un up to various distances. {T}he mapping assigns locations to the nearby dense clouds and represents their distribution at the spatial resolution that is allowed by the dataset properties, i.e. similar or equal to 10 pc close to the {S}un and increasing to similar or equal to 100 pc beyond 1 kpc. {B}iases toward nearby and/or weakly extincted stars make this dataset particularly appropriate to mapping the local and neighboring cavities and to locating faint, extended nearby clouds, which are both goals that are difficult or impossible with other mapping methods. {T}he new maps reveal a similar or equal to 1 kpc wide empty region in the third quadrant in the continuation of the so-called {CM}a tunnel of the {L}ocal {C}avity, a cavity that we identify as the {S}uperbubble {GSH}238+00+09 detected in radio emission maps and that is found to be bounded by the {O}rion and {V}ela clouds. {T}he maps also show an extended narrower tunnel in the opposite direction (l similar or equal to 70 degrees) that also extends the {L}ocal {B}ubble further and together with it forms a conspicuous cavity bounded by the main {L}up, {S}co, {O}ph, {A}ql, {L}ac, {C}ep, and {T}au clouds and {OB} associations. {T}his chain of cavities and surrounding dense regions constitute the first computed representation of the well known {G}ould belt/{L}indblad ring structures. {F}inally, almost all off-plane faint features that appear in 2{D} dust maps have a counterpart in the 3{D} maps, providing the dust distribution in nearby tenuous clouds.},
  keywords = {local insterstellar matter ; dust, extinction ; {ISM}: bubbles ; {ISM}: clouds},
  booktitle = {},
  journal = {{A}stronomy and {A}strophysics},
  volume = {561},
  numero = {{A}91},
  pages = {17  [en ligne]},
  ISSN = {0004-6361},
  year = {2014},
  DOI = {10.1051/0004-6361/201322032},
  URL = {https://www.documentation.ird.fr/hor/{PAR}00011483},
}