A Parallactic Distance of \documentclassaastex \usepackageamsbsy \usepackageamsfonts \usepackageamssymb \usepackagebm \usepackagemathrsfs \usepackagepifont \usepackagestmaryrd \usepackagetextcomp \usepackageportland,xspace \usepackageamsmath,amsxtra \usepackage[OT2,OT1]fontenc \newcommand\cyr \renewcommand\rmdefaultwncyr \renewcommand\sfdefaultwncyss \renewcommand\encodingdefaultOT2 \normalfont \selectfont \DeclareTextFontCommand\textcyr\cyr \pagestyleempty \DeclareMathSizes10976 \begindocument \landscape 389⁺²⁴_-21 \enddocument Parsecs to the Orion Nebula Cluster from Very Long Baseline Array Observations

2007/06/15 by Karin Sandström, Karin M. Sandstrom, J. E. G. Peek +4 · 9 citations
Chemistry · Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Chemistry #Cluster (spacecraft) #Crystallography #Molecular Spectroscopy and Structure #Nebula #Open cluster #Orion Nebula #Parallax #Physics #Proper motion #Stars #Stellar, planetary, and galactic studies #astro-ph

paper · pdf · doi:10.1086/520922

10 pages, 4 figures, emulateapj, accepted to ApJ

arxiv created 2007/06/15 · openalex publication_date 2007/10/01 · arxiv updated 2009/12/01 · openalex created_date 2022/10/02 · openalex updated_date 2026/08/01

Abstract

We determine the parallax and proper motion of the flaring, nonthermal radio star GMR A, a member of the Orion Nebula Cluster, using Very Long Baseline Array observations. Based on the parallax, we measure a distance of 389 pc to the source. Our measurement places the Orion Nebula Cluster considerably closer than the canonical distance of 480 ± 80 pc determined by Genzel et al. A change of this magnitude in distance lowers the luminosities of the stars in the cluster by a factor of ~1.5. We briefly discuss two effects of this change—an increase in the age spread of the pre-main-sequence stars, and better agreement between the zero-age main sequence and the temperatures and luminosities of massive stars.

Citations

• Compact Radio Sources in Orion: New Detections, Time Variability, and Objects in OMC-1S
• Water Maser Motions in W3(OH) and a Determination of Its Distance
• Visual/infrared interferometry of Orion Trapezium stars: preliminary dynamical orbit and aperture synthesis imaging of theθ1 Orionis C system
• Rapid Formation of Molecular Clouds and Stars in the Solar Neighborhood

Cited by

• MASSIVE QUIESCENT CORES IN ORION. VI. THE INTERNAL STRUCTURES AND A CANDIDATE OF TRANSITING CORE IN NGC 2024 FILAMENT
• FIRST SCIENCE OBSERVATIONS WITH SOFIA/FORCAST: PROPERTIES OF INTERMEDIATE-LUMINOSITY PROTOSTARS AND CIRCUMSTELLAR DISKS IN OMC-2
• Millimeter- and Submillimeter-Wave Observations of the OMC-2/3 Region. IV Interaction between the Outflow and the Dense Gas in the Cluster Forming Region of OMC-2 FIR 6
• Probing the evolving massive star population in Orion with kinematic and radioactive tracers
• AN HST SURVEY FOR 100–1000 au COMPANIONS AROUND YOUNG STELLAR OBJECTS IN THE ORION MOLECULAR CLOUDS: EVIDENCE FOR ENVIRONMENTALLY DEPENDENT MULTIPLICITY
• AN ADAPTIVE OPTICS SURVEY FOR CLOSE PROTOSTELLAR BINARIES
• AHERSCHELAND APEX CENSUS OF THE REDDEST SOURCES IN ORION: SEARCHING FOR THE YOUNGEST PROTOSTARS
• Orders of magnitude (length) [wikipedia]
• Star formation [wikipedia]

Related

• A VLBI Resolution of the Pleiades Distance Controversy
• A PRECISE DISTANCE TO IRAS 00420+5530 VIA H2O MASER PARALLAX WITH THE VLBA
• Expansion Parallax for the Compact Planetary Nebula M2-43
• 3D shape of Orion A with Gaia DR2. An informed view on Star Formation Rates and Efficiencies
• The space distribution of nearby star-forming regions