G15

Kuiper Belt Plot

Fig. 24 A coarse and fine sweep acquired during SWAP ground calibration activities Fig. 24 A coarse and fine sweep acquired during SWAP ground calibration activities collected during a 32-s fine sweep in which the values related to pseudo-velocity, pseudo-density, and pseudo-temperature of a fine sweep are defined. For each of the summary values (angle, pseudo-density, pseudo-velocity, and pseudo-temperature), a running log of the sum, minimum, maximum, and variance are calculated. While the...

Frequency Hz

Kuiper Belt Plot

Such spectra the uplink signal strength is close to 105 dBm, somewhat stronger than the 110 dBm level expected at Pluto encounter. The noise floor at 171 dBm-Hz, is somewhat lower than pre-flight tests. At the same time the spectrum is free of spurious signals except for three features located near 50, 200, and 400 Hz and its harmonics. Finer analysis shows that in addition to these features there are also two symmetrically located responses near 30 Hz on either side of the carrier that are not...

Ralph A Visible Infrared Imager for the New Horizons Pluto Kuiper Belt Mission

Alan Stern John Scherrer Donald E. Jennings James W. Baer John Hanley Lisa Hardaway Allen Lunsford Stuart McMuldroch Jeffrey Moore Cathy Olkin Robert Parizek Harold Reitsma Derek Sabatke John Spencer John Stone Henry Throop Jeffrey Van Cleve Gerald E. Weigle Leslie A. Young Originally published in the journal Space Science Reviews, Volume 140, Nos 1-4, 129-154. DOI 10.1007 s11214-008-9375-7 Springer Science+Business Media B.V. 2008 Abstract The New Horizons instrument named...

Ralph MVIC and LEISA

Ralph has two focal planes, MVIC and LEISA. MVIC's prime purpose is to obtain the Group 1 panchromatic and color maps. It also supports the Group 1 goal of characterizing of haze properties, the Group 1 composition maps, and the Group 2 and 3 goals of time variability, stereo imaging, terminator imaging, bond albedos, bulk parameters, and satellite ring search. Both MVIC and LORRI take panchromatic images, with complementary observing techniques. Since MVIC operates its time-delay integration...

Conclusion

After five years of planning and revisions, the New Horizons mission design was finalized, and the spacecraft was launched successfully on January 19, 2006. The spacecraft was injected into the favorable JGA trajectory to Pluto, flew by Jupiter on February 28, 2007, and gained a significant speed boost well on its way to encounter Pluto on July 14, 2015. Using Jupiter's gravity assist in the trajectory design shortened the time of flight to Pluto by three years and provided a great opportunity...

Ion Wind Chamber Design

Ionic Winds Grain Surface

The Solar Wind Around Pluto (SWAP) instrument is designed to measure the tenuous solar wind out at 32 AU and its interaction with Pluto. SWAP directly addresses the Group 1 science objective for the New Horizons mission to characterize the neutral atmosphere of Pluto and its escape rate. In addition, SWAP makes measurements critical for the Group 2 objective of characterizing Pluto's ionosphere and solar wind interaction. Finally, SWAP makes observations relevant to...

The New Horizons Spacecraft

Kusnierkiewicz Christopher B. Hersman Timothy S. Herder Thomas B. Coughlin William C. Gibson Deborah A. Clancy Christopher C. DeBoy T. Adrian Hill James D. Kinnison Douglas S. Mehoke Geffrey K. Ottman Gabe D. Rogers S. Alan Stern James M. Stratton Steven R. Vernon Stephen P. Williams Originally published in the journal Space Science Reviews, Volume 140, Nos 1-4, 23-47. DOI 10.1007 s11214-008-9374-8 Springer Science+Business Media B.V. 2008 Abstract The New Horizons...

Gm

We note that the relative accuracy of the gravitational constant G is similar, 1.0 10-4. As comparisons of the values found in (6) and (8), with those of (7) show, the major determinant of the accuracy of GM is the uncertainty in the distance of closest approach, d. A potentially better accuracy in the determination of (Av)x would make the closest approach distance the sole driver of the GM accuracy. The reverse is also true, namely, any poorer knowledge of the closest...

Ccd

FPU board Primary mirror Secondary mirror with tolerance for easy coalignment. The two-axis gimbal was stepper motor-driven with a Unidex controller at 63 steps per arcsecond to scan LORRI across targets. A LORRI pixel subtends roughly one arcsecond. The reference photodiode was a Hamamatsu S1336-8BQ, whose responsivity was calibrated by the vendor at 10 nm intervals from 200 to 400 nm, and at 20 nm intervals from 400 to 1,180 nm. For thermal control during calibration, a shroud cooled by...

Column Index

Fig. 14 Plot of row 16 in the D2 spectral image shown in Fig. 13 (solid curve). A two Gaussian sum plus DC offset was fit to this profile (dashed line). The narrow emission on the right was used to calculate the filled slit spectral resolution is in the narrow slit segment and +2 is in the wide slit segment), and varied between 4.4 and 6.5 A FWHM, with an average of 5 A FWHM across the passband. The spatial PSF remained < 1.6 spatial pixels FWHM, but grew an average of 0.2 spatial pixels as...

Info

The early mission design work for the New Horizons mission began in late 2000, shortly after NASA terminated the Pluto-Kuiper Express program. A team at The Johns Hopkins University Applied Physics Laboratory (JHU APL), which was wrapping up NASA's Near-Earth Asteroid Rendezvous (NEAR) mission with an unprecedented soft landing on an asteroid, was assembled to put together a feasible mission implementation plan, including the early mission design concept. The team hoped to save the long-sought...

Data Analysis

When SDC data are received on Earth, they are sent to the New Horizons mission operations center at the Johns Hopkins University's Applied Physics Laboratory. The SDC data, as well as several ancillary spacecraft data packets, are also sent to SDCs home institution, LASP, via the Ground System Equipment Operating System (GSEOS). Simultaneously, it is also received at the Tombaugh Science Operations Center (TSOC) of the Southwest Research Institute (SwRI) in Boulder. The data are sent through...

What Object Has Gphs And

Fig. 9 The GPHS-RTG has 9.75 kg of plutonium dioxide distributed in 18 GPHS modules. The modules are designed to contain the plutonium in case of a launch accident. The aluminum outer assembly radiates the heat from the modules into space. The unicouples generate electricity based on temperature differential between the modules and the outer assembly. Prior to launch, the assembly is filled with an inert gas to keep the unicouples from oxidizing. Once in space, the gas pressure relief device...

Radio Occultation Sounding of Pluto and Charon

The reconnaissance of the Neptune system by Voyager 2 included a radio occultation experiment that successfully sounded the tenuous neutral atmosphere of Triton (Tyler et al. 1989). This experiment was conducted in the conventional downlink configuration, using radio signals transmitted by Voyager 2 and received by terrestrial tracking stations equipped with large-diameter antennas. The data at 3.6 cm-X had a fractional frequency stability Sf f of oAnan 2 10-12, where ffAllan is the Allan...

LORRI Requirements

Telescope Spectrometer Assembly

LORRI is a long focal length imager (see Fig. 1) designed for high resolution and respon-sivity at visible wavelengths. LORRI will perform its primary measurements while New Horizons approaches Pluto and its satellite Charon in July, 2015, obtaining images from a closest approach distance of 11,100 kilometers to Pluto, at a flyby speed of 13.77 kilometers per second. New Horizons performed a Jupiter flyby, with closest approach on February 28, 2007. During the Jupiter system flyby, LORRI imaged...

LORRI Instrument Description

The LORRI instrument was designed and fabricated by a combined effort of The Johns Hopkins University Applied Physics Laboratory (JHU APL) and SSG Precision Optronics Fig. 3 LORRI block diagram, showing subassemblies optics (OTA) and aperture door focal plane unit (FPU) and associated support electronics (ASE) with three slices, which are the low-voltage power supply, the event processing unit, and the imager input output board Fig. 3 LORRI block diagram, showing subassemblies optics (OTA) and...

Lorri

Panchromatic, narrow angle CCD imager, 0.30-0.95 microns, 5 microradians pixel. REX, an uplink radio science instrument with radiometer capabilities. LORRI, a long focal length panchromatic Charged Couple Device (CCD) camera to provide 4x higher resolution imaging than Ralph could accomplish. PAM, a plasma package consisting of both the high-sensitivity Solar Wind Around Pluto (SWAP) solar wind monitor to address Pluto atmospheric escape objectives and the Pluto Energetic Particle Sensor...

Differences from EPS on Messenger

The MESSENGER EPS unit was the first flight unit of this miniaturized hockey-puck design. PEPSSI presented different requirements with respect to available power and maximum count rates. While larger rates were anticipated for the encounter with Jupiter and could be used to good advantage for some calibration activities, PEPSSI requirements have always been focused at the conditions near Pluto. In addition, the launch of New Horizons over two years after that of MESSENGER allowed for some...

New Horizons Mission Design

Originally published in the journal Space Science Reviews, Volume 140, Nos 1-4, 49-74. DOI 10.1007 s11214-007-9242-y Springer Science+Business Media B.V. 2007 Abstract In the first mission to Pluto, the New Horizons spacecraft was launched on January 19, 2006, and flew by Jupiter on February 28, 2007, gaining a significant speed boost from Jupiter's gravity assist. After a 9.5-year journey, the spacecraft will encounter Pluto on July 14, 2015, followed by an extended mission to the Kuiper Belt...

Conjunction geometry

Occultation Observation Pluto Geometry

Fig. 9 Options for Pluto arrival time selection opportunity corresponds to the solar opposition geometry with Earth in between the Sun and Pluto, and the winter opportunity corresponds to the solar conjunction geometry with the Sun positioned in the center between Earth and Pluto. The summer arrival time was selected for the solar opposition geometry, which is more favorable for communications and the REX measurements. Inclusion of the Charon occultation in the flyby in addition to the Pluto...

I

PERSI John Scherrer (SwRI) RALPH MVIC Bob Parizek (BATC) RALPH LEISA Sfidhar Manthripragada (BATC) ALICE John Scherrer (SwRI) SWAP Scott Weidner (SwRI) PEPSSI Will Devereux (APL) REX Ivan Liriscott (Stanford) LORRI Kim Cooper (APL) SDC Gene Holland (LASP)_ Jim Stratton, Mark Perry, James Leary

Ta003274

Fig. 6 Simplified P-ALICE electronics block diagram redundant), an EMI filter board, a heater actuator board, and a motherboard. The LVPS electronics interfaces to the spacecraft via three links two links to the +30 V spacecraft power bus for (i) instrument power and (ii) actuator heater power the third link is a safing connector interface that prevents inadvertent HVPS and or actuator (i.e., launch latch, detector door, fail-safe door, SOCC door, and or detector vent valve) operations. The...