The Supplemental IRAS Minor Planet Survey

By E. Tedesco, P. Noah, M. Noah, S. Price. 2002

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In Astronomy and Astrophysics

Citations in the corpus

PRELIMINARY RESULTS FROM NEOWISE: AN ENHANCEMENT TO THE WIDE-FIELD INFRARED SURVEY EXPLORER FOR SOLAR SYSTEM SCIENCE (2011, methodology): “This represents an advance of nearly two orders of magnitude over the IRAS Minor Planet Survey (Tedesco et al. 2002), allowing a correspondingly more detailed view of the size and albedo distributions throughout the Main Belt.”
The taxonomic distribution of asteroids from multi-filter all-sky photometric surveys (2013, methodology): “arvano’s inclusion of the u’ ﬁlter, which we exclude in our work (see Sec. 2.1). [Figure 6 about here.] Second, we retrieved the albedo of the asteroids as determined from IRAS, AKARI, and WISE data (Tedesco et al. 2002, Ryan and Woodward 2010, Usui et al. 2011, Masiero et al. 2011, 2012, Grav et al”
Binary asteroid population 1. Angular momentum content (2007, background): “Walsh and Richardson (2007) simulated a steady-state binary NEA population, and they found that tidal disruptions could account for only 1–2% of NEAs being binary.”
Evidence for asteroid space weathering from the Sloan Digital Sky Survey (2005, background): “Conversely, we were not able to identify any s nificant change as a function of time for asteroid alb values listed in the Supplementary IRAS Minor Planet S vey (SIMPS,Tedesco et al., 2002) and for the J/H and K/H near-IR band ratios listed in the 2-Micron All Sky Surv (2MASS, Sykes et al., 2000).”
MAIN BELT ASTEROIDS WITH WISE/NEOWISE. I. PRELIMINARY ALBEDOS AND DIAMETERS (2011, methodology): “Compositional gradients for the Main Belt have been shown in the past from both infrared and spectral surveys (e.g. Zellner 1979; Gradie & Tedesco 1982; Tedesco et al. 2002; Bus & Binzel 2002), but only for a limited number of objects.”
Asteroid Catalog Using AKARI: AKARI/IRC Mid-Infrared Asteroid Survey (2011, methodology): “…of the sky at 6 bands of 4.29, 4.35, 8.28, 12.13, 14.65, and 21.34 m; 160 asteroids were identified, for which the size and albedo were provided (Tedesco et al. 2002b).2 Also, the Infrared Space Observatory (ISO) launched in 1995 (Kessler et al. 1996) made yet-another part-of-sky survey, and…”
Absolute magnitudes of asteroids and a revision of asteroid albedo estimates from WISE thermal observations (2012, positive): “…Satellite (IRAS) , the Wide-ﬁeld Infrared Survey Explorer (WISE) , AKARI and the Spitzer Space Telescope resulted in estimates of diameters and albedos for thousands of asteroids (e.g., Tedesco et al., 2002; Mainzer et al., 2011a,b; Masiero et al., 2011; Usui et al., 2011; Ryan and Woodward, 2011).”
Bias-corrected population, size distribution, and impact hazard for the near-Earth objects (2004, methodology): “…NEATM m 1 The average albedos for main-belt asteroids in the A, R, and U onomic complexes were calculated as the geometric mean of the alb from IRAS(Tedesco et al., 2002)that have the appropriate taxonomic cla sification from the file Taxonomic Classifications, Version 3 in the Phys cal Data…”
Physical Properties of Kuiper Belt and Centaur Objects: Constraints from the Spitzer Space Telescope (2007, methodology): “The physical properties of Kuiper Belt Objects (KBOs) remain poorly known nearly 15 years after the discovery of (15760) 1992 QB1 (Jewitt and Luu, 1993).”
Density of asteroids (2012, background): “…sky at mid-infrared wavelengths (5 2 20 m m), so infrared satellites (IRAS, ISO, AKARI, Spitzer, and WISE) have been able to acquire observations of a vast number of these objects (see, Tedesco et al., 2002; Ryan and Woodward, 2010; Usui et al., 2011; Masiero et al., 2011; Mueller et al., 2011).”
INITIAL PERFORMANCE OF THE NEOWISE REACTIVATION MISSION (2014, positive): “…taxonomic classification, sizes, and shapes and rotational states are being determined for ∼100 additional NEOs each year (e.g. the MIT-UH-IRTF Joint Campaign for NEO Spectral Reconnaisance, Xu et al. 1995; Tedesco et al. 2002; Benner et al. 2008; Durech et al. 2010; Reddy 2010, and many others).”
Yarkovsky/YORP chronology of asteroid families (2006, methodology): “First, we examine Tedesco et al. (2002), who reanalyzed the IRAS (Infrared Astronomical Satellite) database of infrared observations for moving objects.”
The fossilized size distribution of the main asteroid belt (2003, methodology): “The best available estimates for asteroid diameters and albedos come from the Supplemental IRAS Minor Planet Survey (SIMPS), who used IRAS data to examine 2228 different multiply observed asteroids (Tedesco et al., 2002).”
NEAR-INFRARED SPECTROSCOPY OF TROJAN ASTEROIDS: EVIDENCE FOR TWO COMPOSITIONAL GROUPS (2008, methodology): “Albedos were taken from IRAS (Tedesco et al. 2002), a ground-based survey (Fernàndez et al. 2003), and Spitzer thermal emission measurements (Emery et al. 2006 and unpublished).”