Engineering topics

Cominsky, L. R.

Publications and source records attributed to Cominsky, L. R..

11 records

DOE OSTI2020

Fermi Large Area Telescope Fourth Source Catalog

We present the fourth Fermi Large Area Telescope catalog (4FGL) of γ-ray sources. Based on the first eight years of science data from the Fermi Gamma-ray Space Telescope mission in the energy range from 50 MeV to 1 TeV, it is the deepest yet in this energy range. Relative to the 3FGL catalog, the 4FGL catalog has twice as much exposure as well as a number of analysis improvements, including an updated model for the Galactic diffuse γ-ray emission, and two sets of light curves (one-year and two-month intervals). The 4FGL catalog includes 5064 sources above 4σ significance, for which we provide localization and spectral properties. Seventy-five sources are modeled explicitly as spatially extended, and overall, 358 sources are considered as identified based on angular extent, periodicity, or correlated variability observed at other wavelengths. For 1336 sources, we have not found plausible counterparts at other wavelengths. More than 3130 of the identified or associated sources are active galaxies of the blazar class, and 239 are pulsars.

79 ASTRONOMY AND ASTROPHYSICS↗

NASA NTRS2004

The Swift Gamma Ray Burst Mission

The Swift mission: scheduled for launch in early 2004: is a multiwavelength observatory for gamma-ray burst (GRB) astronomy. It is the first-of-its-kind autonomous rapid-slewing satellite for transient astronomy and pioneers the way for future rapid-reaction and multiwavelength missions. It will be far more powerful than any previous GRB mission, observing more than 100 bursts per year and performing detailed X-ray and UV/optical afterglow observations spanning timescales from 1 minute to several days after the burst. The objectives are to: 1) determine the origin of GFU3s; 2) classify GRBs and search for new types; 3) study the interaction of the ultra-relativistic outflows of GRBs with their surrounding medium; and 4) use GRBs to study the early universe out to z greater than 10. The mission is being developed by a NASA-led international collaboration. It will carry three instruments: a new-generation wide-field gamma-ray (15-150 keV) detector that will detect bursts, calculate 1-4 arcmin positions: and trigger autonomous spacecraft slews; a narrow-field X-ray telescope that will give 5 arcsec positions and perform spectroscopy in the 0.2 to 10 keV band; and a narrow-field UV/optical telescope that will operate in the 170-600 nm band and provide 0.3 arcsec positions and optical finding charts. Redshift determinations will be made for most bursts. In addition to the primary GRB science, the mission will perform a hard X-ray survey to a sensitivity of approx. 1 mCrab (approx. 2 x l0(exp -11) erg/sq cm s in the 15-150 keV band), more than an order of magnitude better than HEAO A-4. A flexible data and operations system will allow rapid follow-up observations of all types of high-energy transients. with rapid data downlink and uplink available through the NASA TDRSS system. Swift transient data will be rapidly distributed to the astronomical community and all interested observers are encouraged to participate in follow-up measurements. A Guest Investigator program for the mission will provide funding for community involvement. Innovations from the Swift program applicable to the future include: 1) a large-area gamma-ray detector us- ing the new CdZnTe detectors; 2) an autonomous rapid slewing spacecraft; 3) a multiwavelength payload combining optical, X-ray, and gamma-ray instruments; 4) an observing program coordinated with other ground-based and space-based observatories; and 5) immediate multiwavelength data flow to the community. The mission is currently funded for 2 years of operations and the spacecraft will have a lifetime to orbital decay of approx. 8 years.

Gehrels, N.↗

NASA NTRS1996

Observations of 4U 1700-37 with BATSE

The eclipsing binary X-ray source 4U 1700-37 has been continually monitored by the BATSE experiment on the Compton Gamma Ray Observatory since the spring of 1991. Using source measurements at times of Earth occultation, we observe an average (uneclipsed) flux of 0.23 crab in the 20-120 keV band. The flux is highly variable, with occasional flaring behavior on timescales from hundreds of seconds to several hours and intensities as bright as 1 crab. The uneclipsed spectrum is well represented by an optically thin thermal bremsstrahlung model with a temperature of 25 keV independent of source intensity or orbital phase. An upper limit of 4% on the pulse fraction has been obtained for pulse periods between 2 and 700 s. Average orbital light curves from almost 1000 days of occultation measurements have been constructed. These profiles are used to measure: (1) the eclipse semiangle, Theta(sub E) = 28.6 deg +/- 2.1 deg in the 20-120 keV band, and (2) the decrease in orbital period, P(dot)/P = -(3.3 +/- 0.6) x 10(exp -7) 1/ yr. Estimates of system physical parameters are obtained using Monte Carlo simulations to propagate errors in measured and assumed parameters. For the X-ray source mass we find M(sub x) = 2.6(sub -1.4)(sup +2.3) solar mass, and for the mass and radius of the optical companion, M(sub 0) = 30(sub -7)(sup +11) solar mass and R(sub 0) = 18(sub -2)(sup +2) solar radius.

Rubin, B. C.↗

NASA NTRS1991

Multimission observations of 4U 1538 - 52

Archival data from the eclipsing binary X-ray pulsar 4U 1538 - 52 have been analyzed. These data were obtained from four different X-ray missions and span a baseline of 12 yr. Scanning observations were made using the Uhuru satellite during May 9-15, 1972 and using HEAO A1 during August 26-31, 1977 and February 22-28, 1978. Pointed observations were made using the Einstein Observatory during March 2, 1979 and Exosat during March 17, August 7-8 and 10-11, 1984. These data are used to improve the orbital period determination, to set a limit to the change in orbital period, and to improve the knowledge of the pulse period as a function of time. Exosat pulse profiles are presented and pulse-phase spectroscopy is performed. The pulsation observations of 4U 1538 - 52 are modeled geometrically, and parameters for magnetic beaming of the accretion column are derived.

Cominsky, L. R.↗

NASA NTRS1989

Further observations of the eclipsing X-ray burst source MXB 1659-29

An analysis is presented of data for MXB 1659-29 obtained during October 2-10, 1976 and June 6-11, 1977 using the SAS 3 X-ray Observatory (Lewin et al., 1976) and during September 8-13, 1978 using the A-1 experiment aboard HEAO 1 (Wood et al., 1984). The data confirm the 7.1 hr orbital period and provide evidence for the 15-min X-ray eclipse reported by Cominsky and Wood (1984). A total of 32 X-ray bursts are detected during the SAS 3 observations. By combining the data with previously published results, the orbital period is found to be about 0.29650474 days.

Cominsky, L. R.↗

NASA NTRS1984

Discovery of a 7.1 hour period and eclipses from MXB 1659-29

A 7.1 hr period has been discovered in the X-ray emission from the 'transient' X-ray burst source MXB 1659-29. Erratic variations in X-ray flux are seen during approximately 25 percent of the 7.1 hr cycle; at the end of this period, a stable dip in the flux occurs. Further analysis indicates that this dip is, in all probability, an eclipse by the companion star in the low-mass binary system. The short (about 15 minute) eclipse duration is used to refine the period determination (7.114104 + or - 0.000168 hr) and to constrain the companion star mass and binary system parameters. The companion star is found to be in the range 0.25-0.9 solar mass; probabilistic arguments and observations of cataclysmic variables with comparable periods indicate that the companion star is most likely less massive than the standard theories would indicate.

Cominsky, L. R.↗

NASA NTRS1984

X-ray observations of the burst source MXB 1728 - 34

Where sufficient information has been obtained, attention is given to the maximum burst flux, integrated burst flux, spectral hardness, rise time, etc., of 96 X-ray bursts observed from March 1976 to March 1979. The integrated burst flux and the burst frequency appear to be correlated; the longer the burst interval, the larger the integrated burst flux, as expected on the basis of simple thermonuclear flash models. The maximum burst flux and the integrated burst flux are strongly correlated; for low flux levels their dependence is approximately linear, while for increasing values of the integrated burst flux, the flux at burst maximum saturates and reaches a plateau.

Basinska, E. M.↗

NASA NTRS1983

Optical radiation associated with gamma-ray bursts

Calculations are made of the approximate characteristics of the reprocessed optical radiation resulting from the absorption of a gamma-ray burst by a nearby star. The overall reprocessing time scale, including contributions from gamma-ray transfer and diffusion of the optical radiation, is estimated. It is noted that diffusive cooling occurs by either a 'self-similar' or a 'transparency' wave of postabsorption stellar surface temperatures greater or less than 10,000 K, respectively. Depending on the combination of stellar and gamma-ray burst properties, the reprocessing time scale can vary from the duration of the gamma-ray burst (approximately 1 s) to the maximum calculated cooling time (approximately 1000 s). Calculations for close binary systems are made of the number of optical photons per square centimeter expected at earth as a function of the observed gamma-ray burst fluences and likely distances. It is predicted that, if all gamma-ray bursters are in close binaries, the number of detections per year by an all sky monitor of 200 photons per sq cm sensitivity will be about 100.

London, R. A.↗

NASA NTRS1983

X-ray burst observations of Serpens X-1

Fifty-seven X-ray bursts observed with SAS 3 in the period 1976 July to 1979 March are reported. Their general features (e.g., maximum burst flux, integrated burst flux, spectral hardness, and rise time) and the relations between them are discussed. Also a comparison is made between these burst features and the associated persistent X-ray flux. The latter appears to be correlated with the maximum burst flux; the temperature of the plasma that produces the persistent flux is roughly proportional to this flux.

Sztajno, M.↗

NASA NTRS1982

X-ray observations of the 1980 Cygnus X-1 'high state'

Observations of intensity transitions in the X-ray emission from the black-hole candidate Cygnus X-1 were made by the Hakucho satellite during the summer of 1980 and are reported here. In addition, the results of hard (20-120 keV) X-ray observations of Cyg X-1 are reported. These data were obtained during the 'high' intensity state by balloon-borne mercuric iodide detectors, and are compared with data obtained at similar energies approximately 1 month earlier (A. Sheepmaker et al., in preparation) during the 'low' intensity state.

Ogawara, Y.↗

NASA NTRS1980

Simultaneous IR and X-ray burst observation of Ser X-1

It has been suggested that the very bright IR bursts observed from the Rapid Burster (MXB 1730-335) are due to Type I X-ray bursts. If the suggestion is correct, similar bright IR bursts may, in general, accompany Type I X-ray bursts. This paper investigates this possibility for one specific case. During the 1977 coordinated worldwide burst watch, simultaneous X-ray and IR observations were made. On 00 h 00 min 25s June 17 UT, a Type I X-ray burst was observed, which was almost certainly emitted by Ser X-1 (MXB 1837+05, 4U1837+04). Simultaneous IR observations failed to detect any bursts.

Lewin, W. H. G.↗