The Flux Distribution and Sky Density of 25th Magnitude Main Belt Asteroids

@article{Heinze2019TheFD,
  title={The Flux Distribution and Sky Density of 25th Magnitude Main Belt Asteroids},
  author={Aren N. Heinze and Joseph Trollo and Stanimir A. Metchev},
  journal={The Astronomical Journal},
  year={2019},
  volume={158}
}
Digital tracking enables telescopes to detect asteroids several times fainter than conventional techniques. We describe our optimized methodology to acquire, process, and interpret digital tracking observations, and we apply it to probe the apparent magnitude distribution of main belt asteroids fainter than any previously detected from the ground. All-night integrations with the Dark Energy Camera (DECam) yield 95% completeness at R magnitude 25.0 and useful sensitivity to R = 25.6 mag when we… 

A re-assessment of the Kuiper belt size distribution for sub-kilometer objects

<p>In this work we combine several constraints provided by the crater records on Arrokoth and the worlds of the Pluto system to compute the size-frequency distribution (SFD) of the crater production

Interpreting the Cratering Histories of Bennu, Ryugu, and Other Spacecraft-explored Asteroids

Asteroid crater retention ages have unknown accuracy because projectile–crater scaling laws are difficult to verify. At the same time, our knowledge of asteroid and crater size–frequency

Space-Time Projection Optical Tomography: Search Space and Orbit Determination

In a companion article [1], we discussed the radiometric sensitivity and resolution of a new passive optical sensing technique, Space-Time Projection Optical Tomography(SPOT), to detect and track

Radiometric sensitivity and resolution of synthetic tracking imaging for orbital debris monitoring

We consider sampling and detection strategies for solar illuminated space debris. We argue that the lowest detectable debris cross section may be reduced by 10-100x by analysis of phase-space-pixels

A high-rate foreground of sub-second flares from geosynchronous satellites

The Weizmann Fast Astronomical Survey Telescope (W-FAST) is a 55 cm optical survey telescope with a high cadence (25 Hz) monitoring of the sky over a wide field of view (7 deg^2). The high frame rate

References

SHOWING 1-10 OF 37 REFERENCES

Collisional and dynamical evolution of the main belt and NEA population

Aims. In this paper, we analyze the collisional evolution of the Main Belt and NEA population taking into account the major dynamical features present in both populations. Methods. To do this, we

Evidence for a Color Dependence in the Size Distribution of Main-Belt Asteroids

We present the results of a project to detect small (∼1 km) main-belt asteroids with the 3.6 m Canada-France-Hawaii Telescope. We observed in two filters (MegaPrime g′ and r′) in order to compare the

Size and Spatial Distributions of Sub-km Main-Belt Asteroids ∗

This paper presents the result of the first systematic investigation of very small Main-Belt Asteroids (sub-km MBAs) using the Subaru Prime-Focus Camera (Suprime-Cam) with an 8K ×10K mosaic CCD array

On the asteroid belt's orbital and size distribution

HIGH ECLIPTIC LATITUDE SURVEY FOR SMALL MAIN-BELT ASTEROIDS

Main-belt asteroids have been continuously colliding with one another since they were formed. Their size distribution is primarily determined by the size dependence of asteroid strength against

GENERALIZED DERIVATION OF THE RRV METHOD AND ITS APPLICATION

Very recently, Heinze & Metchev proposed a novel method for calculating precise distances to the main-belt asteroids using only two nights of data from a single observatory. In this paper, we

PRECISE DISTANCES FOR MAIN-BELT ASTEROIDS IN ONLY TWO NIGHTS

We present a method for calculating precise distances to asteroids using only two nights of data from a single location—far too little for an orbit—by exploiting the angular reflex motion of the

DIGITAL TRACKING OBSERVATIONS CAN DISCOVER ASTEROIDS 10 TIMES FAINTER THAN CONVENTIONAL SEARCHES

We describe digital tracking, a method for asteroid searches that greatly increases the sensitivity of a telescope to faint unknown asteroids. It has been previously used to detect faint Kuiper Belt