2016/02/24 by Marina Kounkel, M. Kounkel, S. T. Megeath +5 · 1 citation
Physics and Astronomy · #Astro and Planetary Science #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Hubble Deep Field #Hubble Ultra-Deep Field #Hubble space telescope #Line-of-sight #Main sequence #Molecular cloud #Photometry (optics) #Physics #Protostar #Sigma #Star formation #Stars #Stellar density #Stellar, planetary, and galactic studies #Wide Field Camera 3 #Young stellar object #astro-ph.GA #astro-ph.SR
paper · pdf · doi:10.3847/0004-637x/821/1/52
20 pages, 7 tables, 22 figures Accepted to ApJ
arxiv created 2016/02/24 · openalex publication_date 2016/04/10 · arxiv updated 2016/04/27 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
ABSTRACT We present a near-infrared survey for the visual multiples in the Orion molecular clouds region at separations between 100 and 1000 au. These data were acquired at 1.6 μ m with the NICMOS and WFC3 cameras on the Hubble Space Telescope . Additional photometry was obtained for some of the sources at 2.05 μ m with NICMOS and in the L ′ band with NSFCAM2 on NASA’s InfraRed Telescope Facility. Toward 129 protostars and 197 pre-main-sequence stars with disks observed with WFC3, we detect 21 and 28 candidate companions between the projected separations of 100–1000 au, of which less than 5 and 8, respectively, are chance line-of-sight coincidences. The resulting companion fraction (CF) after the correction for the line-of-sight contamination is <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mn>14.4</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1.3</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>1.1</mml:mn> </mml:mrow> </mml:msubsup> <mml:mo>%</mml:mo> </mml:math> for protostars and <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mn>12.5</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.8</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>1.2</mml:mn> </mml:mrow> </mml:msubsup> <mml:mo>%</mml:mo> </mml:math> for the pre-main-sequence stars. These values are similar to those found for main-sequence stars, suggesting that there is little variation in the CF with evolution, although several observational biases may mask a decrease in the CF from protostars to the main-sequence stars. After segregating the sample into two populations based on the surrounding surface density of young stellar objects, we find that the CF in the high stellar density regions (Σ YSO > 45 pc −2 ) is approximately 50% higher than that found in the low stellar density regions (Σ YSO < 45 pc −2 ). We interpret this as evidence for the elevated formation of companions at 100–1000 au in the denser environments of Orion. We discuss possible reasons for this elevated formation.