ASCAO - ASCA Proposals
ASCA (Advanced Satellite for Cosmology and Astrophysics; formerly Astro-D) is Japan's fourth x-ray astronomy mission and the second for which the U.S. is providing a significant part of the scientific payload. Its four large-area telescopes focus x-rays from a wide energy range onto a pair each of x-ray sensitive Charge-Coupled Devices (CCD's) and imaging Gas Scintillation Proportional Counters (GSPC's). ASCA is examining a variety of x-ray sources with moderate spatial resolution and spectral resolution, with particular emphasis on the iron K band.
Quoted from the PDMP:
The two identical x-ray CCD cameras on board ASCA are known as the Solid-state Imaging Spectrometers (SIS) and were provided by a hardware team from the Massachusetts Institute of Technology (MIT), Osaka University, and Japan's Institute of Space and Astronautical Science (ISAS). Each CCD camera head is based around four $420 \times 422$ pixel MIT Lincoln Laboratory CCD chips abutted side by side, with four preamplifiers, front-side illuminated. The field of view of each camera is $22 \times 22$ arcminutes. Since the SIS is the first x-ray CCD spectrometer on orbit, its resistance to radiation damage will be fully established as the mission progresses.
Each Gas Imaging Spectrometer (GIS) is a Xenon-filled imaging gas scintillation proportional counter; these two instruments were provided by the University of Tokyo and ISAS. The GIS complements the SIS: above the Xenon L edge ($\approx 5$ keV), the GIS has a detection efficiency that is both greater than the SIS and falls off less rapidly. The GIS, with a circular field of view of radius 25 arcminutes, observes about 4 times the area than covered by the SIS.
The high throughput X-Ray Telescopes (XRT's) utilize multiply-nested, thin foil, conical mirrors. The XRT's were supplied by GSFC, Nagoya University and ISAS, and provide a spatial resolution of $\sim$ 1.5 arc minutes (half-power radius) and a broad bandpass, 0.1-10 keV.
ASCA is the first x-ray imaging mission operating between 0.5 and 12 keV with high energy resolution (8 and 2 percent at 5.9 keV for the GSPC's and CCD's, respectively). It observes typically one or two sources per day. These combined capabilities enable a diverse and exciting program of astronomical research.
The sequence number.
The name of the target.
The Right Ascension of the target.
The Declination of the target.
The galactic longitude of the target.
The galactic latitude of the target.
The last name of the Principal Investigator.
The first name of the Principal Investigator.
The country of the PI's institution.
The proposal number.
The target number within the original proposal.
The AO number.
Total observing time in kiloseconds (ks): 1 ks = 1000 s.
Priority from the highest (1) to the lowest (3): notice that priority 3 targets are not guaranteed to actually be observed.
The last name of the co-PI.
The first name of the co-PI.
Proposal abstract filename
Holdover flag. (The parameter is deprecated and no longer populated.)