High resolution near-infrared imaging of the trapezium: A stellar census

By M. McCaughrean, J. Stauffer. 1994

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

1. K. Luhman
2. B. Bowler
3. Eric Mamajek
4. Matthew R. Bate
5. A. Kraus
6. Pavel Kroupa
7. L. Hillenbrand
8. C. Lada

Citations in the corpus

• STELLAR AND PLANETARY PROPERTIES OF K2 CAMPAIGN 1 CANDIDATES AND VALIDATION OF 17 PLANETS, INCLUDING A PLANET RECEIVING EARTH-LIKE INSOLATION (2015, methodology): “…calibrated using dithered observations of the Trapezium cluster centered on 1q Ori C taken on 2015 February 3 UT. Based on the reference astrometry for pairs of stars in the field from McCaughrean & Stauffer (1994), we measure a plate scale of 25.2 ± 0.4 mas pixels−1 and north orientation of –0 ◦.”
• Accretion in stellar clusters and the collisional formation of massive stars (2002, background): “The core of the ONC is considerably more dense with n ≈ 2 × 104 star pc−3 (McCaughrean & Stauffer 1994).”
• Chandra Orion Ultradeep Project: Observations and Source Lists (2004, background): “…magnitudes for brighter stars were from other wide-field ONC catalogs and high spatial resolution studies of the inner core region as necessary (McCaughrean & Stauffer 1994; Hillenbrand 1997; Petr et al. 1998; Simon, Close, & Beck 1999; Lucas & Roche – 19 – 2000; Luhman et al. 2000; Muench et…”
• The VAST Survey - III. The multiplicity of A-type stars within 75 pc (2013, methodology): “These measurements were converted into an on-sky separation and position angle (ρ, θ) using the pixel scale and angle of North of the detector, estimated from observing an astrometric field (the Trapezium; McCaughrean & Stauffer 1994) or a calibration binary.”
• THE GALACTIC O-STAR SPECTROSCOPIC SURVEY. I. CLASSIFICATION SYSTEM AND BRIGHT NORTHERN STARS IN THE BLUE-VIOLET AT R ∼ 2500 (2011, methodology): “On the other hand, we searched the literature for results similar to those obtained with AstraLux (e.g. McCaughrean & Stauffer 1994; Duchêne et al. 2001; Mason et al. 1998; Turner et al. 2008; Bouy et al. 2008; Mason et al. 2009) and we plotted information from Simbad using Aladin images to ensure…”
• CH3OH and H2O masers in high-mass star-forming regions (2002, background): “Lada (1999) report a mean separation between stellar objects in clusters around 0.1 pc, and McCaughrean & Stauffer (1994) find mean separations in the center of the Orion Nebula Cluster of ∼0.03 pc.”
• On the origin of the o and b-type stars with high velocities II runaway stars and pulsars ejected from the nearby young stellar groups (2000, background): “Estimates for the stellar density are > 20 000 stars pc−3 for the inner 0.1–0.3 pc (e.g., McCaughrean & Stauffer 1994; Hillenbrand & Hartmann 1998).”
• The Initial Mass Function of Low-Mass Stars and Brown Dwarfs in Young Clusters (2000, background): “…& Walker 1988), optical images from the ground (Herbig & Terndrup 1986) and space (Prosser et al. 1994), wide-field infrared (IR) – 3 – images (Ali & DePoy 1995), and high-resolution ground-based IR images (McCaughrean & Stauffer 1994, hereafter MS; Petr et al. 1998; Simon, Close, & Beck 1999).”
• The Birth of High-Mass Stars: Accretion and/or Mergers? (2005, background): “…106 years old (Hillenbrand 1997; Hillenbrand & Hartmann 1998) The density of stars in the cluster core currently is in the range 5× 104 stars pc−3 (McCaughrean and Stauffer 1994) to 2 × 105 stars pc−3 (Henney & Arthur 1998), implying a nearest-neighbor distance between low-mass stars of only a…”
• Destruction of protoplanetary discs in the Orion Nebula Cluster (2000, background): “In the past decade, however, deep and high resolution studies at optical wavelengths (Prosser et al. 1994) and adaptive optical techniqes in the infrared (McCaughrean & Stauffer 1994) have greatly improved our understanding of the cluster’s size and composition.”
• The Origin of T Tauri X-Ray Emission: New Insights from the Chandra Orion Ultradeep Project (2005, background): “This star-forming region contains a massive cluster of young ( 106 yr) stars (cf. Herbig & Terndrup 1986; McCaughrean & Stauffer 1994; Hillenbrand 1997), which is known as the Orion Nebula Cluster (ONC).”
• The formation of a star cluster: predicting the properties of stars and brown dwarfs (2002, background): “The stellar densities in the centre of the Trapezium Cluster are 2−4×104 pc−3 (McCaughrean & Stauffer 1994; Hillenbrand & Hartmann 1998; Bate, Clarke & McCaughrean 1998) and the density falls off with radius as n ≈ 2 × 104(r/0.07 pc)−2 pc−3 (Bate et al. 1998).”
• DISCOVERY OF A PROBABLE 4–5 JUPITER-MASS EXOPLANET TO HD 95086 BY DIRECT IMAGING (2013, methodology): “The θ1 Ori C field data was reduced for detector calibrations by comparison with HST observations by McCaughrean & Stauffer (1994) (using the same set of stars TCC0051, 034, 029, and 026 at each epoch).”
• The Formation and Early Evolution of Low-Mass Stars and Brown Dwarfs (2012, background): “This approach was applied most extensively to the Trapezium Cluster at the center of the ONC because it is very compact and is located in front of a dense molecular cloud, reducing the contamination from background stars (Hillenbrand & Carpenter 2000; Lucas & Roche 2000; Lucas, Roche & Tamura 2005; ”
• The Luminosity and Mass Function of the Trapezium Cluster: From B Stars to the Deuterium-burning Limit (2002, methodology): “We list cross-references based on the most comprehensive or deep surveys; these include the Hillenbrand (1997), HC00, and Luhman et al. (2000) designations and McCaughrean & Stauffer (1994).”
• The formation of a bound star cluster: from the orion nebula cluster to the pleiades (2000, background): “The high central density of the Trapezium (McCaughrean & Stauffer 1994) was not known at the time of Lada et al. (1984), and they concluded that such high densities are not realistic, because this has not been observed in molecular clouds.”