OBSERVATION NOTES TABLES

TABLE 3A
OBSERVATION NOTES: ACCRETING GAMMA-RAY SOURCES
SourceInstrumentNotes
1A 0535+262...MIT76Exponential fit. Power-law fit is unacceptable
1A 0535+262...BATSE52 day outburst. Peak flux quoted. Extensive QPO and timing analysis presented
1A 0535+262...LEGSPulsations with P=103.79±0.01 s and double-peaked light curve
1A 0535+262...HEXEApr 8/9 combined data quoted here. Decrease in flux on the 14th. Shows pulse profiles. Fit included lower energy TTM data. Shows phase-resolved spectroscopy
1A 0535+262...Ariel 5Blackbody fit. Spectral fit is for Apr 27 – 28. Discusses light curve and spectral evolution
1A 0535+262...SIGNE 2MPAverage flux quoted is peak for the observation. Variability shown
1A 0535+262...TESRE/XG81Wien fit to pulse-averaged spectrum quoted. Also presents pulse-phase spectroscopy, null search for cyclotron lines, and study of short-term variability
1A 0535+262...POKERTotal emission quoted
1A 0535+262...HEAO A4Average flux assumes photon index 2.0
1A 0535+262...OSSEPower law modified by the factor e^{E/(17.8+5.4,-3.8 keV)×e^{-L(E)}, where L(E)=sum_{i=1,2} tau(nW)^2 (E/nEL)^{2}/[(E-nEL)^{2}+(nW)^{2}], where E(L)=55.0i, W is HWHM and equals 14.2 keV, tau is optical depth and is 0.10 for i=1, 1.8 for i=2. Average flux is quoted with variability shown
1A 0535+262...Marshall76 · · ·
1A 0535+262...SIGNE 2MP · · ·
1A 0535+262...MIFRASO2 sigma upper limit. Clearly detected below 56 keV
1A 1742-294...HEAO A4Average flux assumes photon index 2.0. Variable
1E 1740.7-2942...POKERHighly variable. Possibly some source confusion at low energies
1E 1740.7-2942...SIGMAComptonization model with optical depth 1.9(+0.7, -0.6). Possible line at 350 keV. See Churazov et al. 1993 regarding earlier SIGMA observations and Bouchet et al. 1991 regarding variable annihilation radiation
1E 1740.7-2942...HEXEBest-fit power law with exponential cutoff; cutoff energy 26.5 keV and folding energy 52.8 keV; spectral fit includes lower energy data
1E 1740.7-2942...GRIPAlso gives 2 sigma upper limit of 3.7×10-4 cm-2 s-1 for 511 keV line flux
1E 1740.7-2942...OSSE · · ·
1E 1740.7-2942...BATSEReduced flux during a 1992 Sep observation. Discusses comparison with SIGMA flare observations. Also detected in the 100 – 300 keV range. Some source confusion possible
1E 1740.7-2942...COMPTEL2 sigma upper limit. Limits at higher energies also listed
4U 0352+30...HEAO A4Spectral index is for a hard tail superposed on a 7 keV thermal fit. Also observed in 1977 Aug and 1978 Feb
4U 0115+63...OSSEExponential fit at peak of outburst. Shows flux and spectral development along with multiwavelength observations. Also describes BATSE 20 – 50 keV observations
4U 0115+63...Whipple85Also gives limit to pulsed emission
4U 1543-47...BATSEMonitoring of outburst
4U 1626-67...NRL · · ·
4U 1626-67...HEAO A4Average flux assumes a photon index 2.0
4U 1630-47...BATSEAverage low-level outburst flux quoted. Shows light curves and image
4U 1630-47...COMPTELUpper limits at higher energies also listed
4U 1700-377...BATSEOTTB fit with average flux. Presents light curves, analysis of binary orbit, and upper limits to pulsed flux
4U 1700-377...SIGMAValues listed are for flare spectrum. Light curves and spectral variability are shown and discussed. Thermal brehmstrahlung with kT 45 keV is a better fit
4U 1700-377...HEAO A4Average flux assumes photon index 2.0
4U 1700-377...SAS 2Quoted dates are mission duration
A0620-00...Ariel 5October numbers quoted here. Aug flux is smaller, which when combined with X-ray data shows anticorrelated hard/soft X-rays
A0620-00...COMPTELUpper limits at higher energies also listed
A1118-616...BATSESpectrum at the peak of outburst quoted
A1742-2942...SIGMAVariable. Upper limits or reduced flux for several other epochs
Aql X-1...BATSESeveral outbursts detected. Numbers here are for 1991 Aug 21 – 31. Also plots image and light curve
Aql X-1...HEAO A4Average flux assumes photon index 2.0
Cen X-3...Ariel 5Reduced flux during two other observations. Evans et al. 1980 give upper limits to cyclotron line emission
Cen X-3...HEAO A4Average flux assumes photon index 2.0
Cen X-3...SAS 2 · · ·
Cen X-3...EGRET · · ·
Cen X-3...Narrabri753 sigma upper limit
Cen X-3...JANZOSUpper limit to total emission (95%). No pulsed emission
Cen X-4...SIGNE 2MPProvides thermal brehmstrahlung fits at three epochs. Flux quoted is for peak outburst
Cyg X-1...HEAO A4Sunyaev & Titarchuk model fit. See also Nolan & Matteson 1983 regarding possible annihilation line and Levine et al. 1984. Evidence for an excess above 500 keV
Cyg X-1...POKERQPOs detected at 0.013 and 0.04 Hz
Cyg X-1...Saclay · · ·
Cyg X-1...OSO 8Numbers quoted are for 1976 Oct 27 – 31. Four other observations show a similar spectrum with a fifth showing softer high-state emission
Cyg X-1...MIFRASOAlso gives Comptonization fits. Makes comparisons with other observationss
Cyg X-1...MIT68 · · ·
Cyg X-1...BOEING · · ·
Cyg X-1...TESRE73"Normal" spectrum quoted, which does not include a 10 minute flare period which showed a softer spectrum
Cyg X-1...HEXECompton reflection model with covering fraction = 0.59±0.04. Average flux quoted. Shows results of timing analysis
Cyg X-1...LeidenSome possible contamination from Cyg X-2 and Cyg A
Cyg X-1...UCSD66 · · ·
Cyg X-1...MIT69May have some Cyg X-3 contamination
Cyg X-1...Tata71Extensive discussion of previous measurements. Variability analysis. Also describes a 1969 Apr 16 flight
Cyg X-1...LLL · · ·
Cyg X-1...MPI76No good reference for detector; X-ray burst experiment in development
Cyg X-1...UNH70 · · ·
Cyg X-1...BATSEQuoted spectrum is for a newly defined ultralow state detected over one 40 day period. Displays the light curve and describes spectral/flux changes over several other epochs. also see Crary et al. 1996
Cyg X-1...MISOMay values stated here. Oct values are representative of the "super-low state." Thermal and Comptonized fits also calculated. see Bassani et al. 1989 for a reanalysis
Cyg X-1...Ariel 5The spectral fit is for May 11 – 15 and includes lower energy data. Previously recorded flux is higher, which when combined with X-ray data shows anticorrelated hard/soft X-rays
Cyg X-1...PRLATime-averaged values shown. Variability discussed
Cyg X-1...SMM/JXRBSSunyaev & Titarchuk model with tau = 2.9±0.3. Peak flux quoted. Spectral values are for "quiescent" period from 1987 Feb 1 – Apr 3. Also presents light curves and outburst spectrum
Cyg X-1...Rice68Broken power law with break energy in parenthesis. Exponential fit is also quoted. Haymes & Harnden 1970 give details of a later flight (1969 Jun 4) with the same instrument which yielded similar results
Cyg X-1...SIGMAComptonizaton model fit with tau = 2.02±0.13
Cyg X-1...HEAO 3Numbers quoted are for the 1979 Sep data which define the "super-low state." Light curve and alternative fits and spectra for other states are shown. Further variability studies can be found in Ling et al. 1987
Cyg X-1...OSSEFit includes an exponential cutoff of the form e[-E/158+/-3(+/-12)]. Systematic errors are in parenthesis. No evidence of a broad MeV feature or annihilation radiation. Spectrum quoted is the average. Also addresses of curves, hardness ratios, alternative spectral forms, and spectral variability
Cyg X-1...MIT67Also seen at lower energies. See Overbeck, Womack, & Tananbaum (1967) regarding an earlier observation from 1966 Sep
Cyg X-1...CESRE76Flux values at higher energies plotted
Cyg X-1...CESR78Shows flux points up to 3 MeV
Cyg X-1...UNHDGTSpectral fit has reduced chi2 of 1.71. Apparent 2 – 9 MeV hard excess
Cyg X-1...COMPTELWien spectral fit shows no evidence for MeV excess. Flux and spectrum are for the August observation
Cyg X-1...Southampton732 sigma upper limit. Possible weak detection data if all data from 1 – 10 MeV are combined
Cyg X-1...UCR2 sigma upper limit. Limits at higher energies included
Cyg X-1...MPI732 sigma upper limit assumes power-law index 2.0
Cyg X-1...SMM/GRS3 sigma upper limit to steady flux from neutron capture line
Cyg X-1...Southampton2 sigma upper limit
Cyg X-1...SAS 2 · · ·
Cyg X-2...Saclay · · ·
Cyg X-2...NRL · · ·
Cyg X-2...TESRE/XG81Thermal brehmstrahlung and exponential fits also consistent with the data
Cyg X-2...UNH70Approximate 1 sigma upper limit. Detected at lower energies
Cyg X-2...MPI732 sigma upper limit assumes power-law index 2.0
Cyg X-2...Southampton2 sigma upper limit
Cyg X-2...SAS 2 · · ·
Cyg X-3...SaclayTotal spectrum ; 3 sigma upper limit
Cyg X-3...HEXEVariable. Values represent the brightest of the three observations (1988 Jul);
Cyg X-3...OSSEAlso see Matz et al. 1996. Evidence for flux decrease preceeding a radio flare. Spectrum in high emission state quoted here hardens at lower flux
Cyg X-3...HEAO A4Average flux assumes photon index 2.0
Cyg X-3...UNHDGTUpper limits at higher energies plotted
Cyg X-3...OSO 7Broken power-law fit quoted with break energy in parenthesis. No evidence for 4.8 hr periodicity. Other spectral fits quoted. Also see Ulmer 1975 for later observations
Cyg X-3...LeimitModulated at 4.8 hr period. Also discusses COS B limits
Cyg X-3...MPI/AITSome variability found over the 2 hr observation. Bremsstrahlung fit is slightly better
Cyg X-3...OSO 8Numbers quoted are for 1975 Nov 5 – 17. Weak above 50 keV for individual observations,
Cyg X-3...SIGMA · · ·
Cyg X-3...RiceFlux rising throughout the observation. Average spectrum quoted
Cyg X-3...UCR2 sigma upper limit. Also lists limits at higher energies
Cyg X-3...MPI732 sigma upper limit assumes power-law index 2.0
Cyg X-3...SMM/GRS3 sigma upper limit to steady flux from neutron capture line
Cyg X-3...EGRETPosition of detection consistent with Cyg X-3, but no pulsed emission; also see Thompson et al. 1995
Cyg X-3...COS B2 sigma upper limit to emission consistent with 4.8 hr periodicity
Cyg X-3...Southampton2 sigma upper limit
Cyg X-3...SAS 2Pulsed at 4.8 hr period
Cyg X-3...Whipple755 sigma upper limit,
Cyg X-3...Whipple903 sigma upper limit to steady emission. Also no evidence for 4.8 hr periodic emission. See Cawley et al. 1985a for earlier observations with possible detection
Cyg X-3...JPL TeV4.8 hr periodicity detected
EXO 2030+375...BATSESpectrum is for brightest outburst. Several observations tied to periastron passage with orbital solution given
EXS 1737.9-2952...EXITEPossible double – back-scattered annihilation line which accompanies an excess at hard X-ray energies
GRO J0422+32...SIGMAAverage flux quoted here. Light curves and other spectral models and spectral evolution are discussed. Also see Vikhlinin et al. 1995 for variability studies
GRO J0422+32...COMPTELTwo-bin detection with spectrum poorly constrained. Further observations reveal reduced intensity
GRO J0422+32...OSSEShows light curve and spectrum. Also see Grove et al. 1994 for timing properties
GRO J0422+32...BATSESpectrum and flux are near peak outburst. Sunyaev-Titarchuk model used. Also see Callanan et al. 1995 for a multiwavelength perspective
GRO J1008-57...BATSEOutbursts detected during four other epochs. Shows light curve and variability
GRO J1655-40...BATSEFlux is peak outburst. Spectrum is for initial outburst. Shows correlations with radio outbursts. Also see Zhang et al. 1997 for a multiinstrument analysis
GRO J1655-40...OSSE · · ·
GRO J1655-40...COMPTEL2 sigma upper limit. Limits at higher energies also listed
GRO J1719-24...BATSEFlux is during peak of the 80 day outburst. Shows spectral and flux evolution as well as power-spectral density evolution
GRO J1719-24...SIGMAComptonization model fit is for peak outburst with tau =2.3±0.1. Flux values are from the peak outburst from 1993 Sep 29 – 30. Shows light curves and extensive spectral fitting
GRO J1719-24...COMPTEL2 sigma upper limit with limits at higher energies also listed
GRO J1744-28...OSSEBurst spectrum is a power law with cutoff exponential of form e(-E/15 ± 3 keV). Shows burst and pulse profiles
GRO J1750-27...BATSESpectrum is for 1995 Aug 31 – Sep 7 with spectral form flux=A×(Ep/E)e-(E-Ep)/kT. Discusses orbit and pulse period changes
GRO J1849-03...BATSEAverage outburst spectrum listed here. Discovery of 241 day recurrence time and discussion of possible counterparts
GRO J1948+32...BATSEMonitoring of 33 day outburst. Spectrum and flux are for peak brightness. Shows flux history and folded light curves as a function of energy
GRO J2058+42...BATSEQuotes flux values for 20 – 50 keV and shows pulse profile and outburst light curve
GRS 1009-45...SIGMA · · ·
GRS 1724-308...SIGMANot detected at several other epochs
GRS 1730-312...SIGMAAverage spectrum quoted. A slightly better fit with thermal bremstrahlung. Variable flux with some evidence for spectral evolution;
GRS 1739-278...SIGMADiscusses possible counterparts
GRS 1758-258...POKER · · ·
GRS 1758-258...GRIPCook et al. 1991b present upper limits for a 1988 observation
GRS 1758-258...SIGMAComptonization model fit with tau =1.12(+0.35,-0.25). Numbers quoted are from average of Fall 1990 observations. Shows light curve and factor of 10 variability
GRS 1758-258...COMPTEL2 sigma upper limit with limits at higher energies also listed
GRS 1915+105...BATSEPeak numbers quoted here. Displays light curves
GRS 1915+105...SIGMA · · ·
GRS 1915+105...COMPTEL2 sigma upper limit with limits at higher energies also listed
GS 0834-43...BATSEPeak flux is quoted while the spectral index is an average value. Extensive pulse period and flux history are presented. Analysis of orbital parameters included. Shows energy dependence of pulse profiles
GS 0834-43...SIGMA · · ·
GS 1826-24...OSSEProvides alternative spectral fits with combined lower energy data
GS 1826-24...COMPTEL2 sigma upper limit with limits at higher energies also listed
GS 2000+25...HEXE/Pulsar X-1Bremstralung fit given here
GS 2000+25...COMPTEL2 sigma upper limit with limits at higher energies also listed
GX 1+4...UT/UCPaper includes pulse profiles and light curves. Greenhill et al. 1989a give more information on this flight
GX 1+4...Imperial/UT/IPEBlackbody fit
GX 1+4...NRLPossible line feature in the spectrum
GX 1+4...HEXEAlso gives alternative spectral fits. A second observation on 1988 Sep 23 – 27 is also described
GX 1+4...RICEDetection of pulsed emission
GX 1+4...NRLTiming analysis and pulse intensity variations
GX 1+4...BATSEThermal bremstrahlung fit. Shows pulse period history and relates flux history to torque changes. Discusses possibility of a retrograde accretion disk in this system. Spectrum consistent throughout monitoring
GX 1+4...Signe 2MPAverage flux quoted here. Variable = not detected for several weeks before stated dates. Light curves shown with estimated pulsed fraction of 37%±9%
GX 1+4...SIGMAShows light curve and pulse period history
GX 1+4...GRIP2 sigma upper limit
GX 1+4...HEAO A4Average flux assumes photon index 2.0
GX 1+4...IPEPulsed flux measured
GX 1+4...Narrabri753 sigma upper limit
GX 17+2...Ariel 52 sigma upper limit
GX 17+2...HEAO A4Average flux assumes photon index 2.0
GX 3+1...HEAO A4Average flux assumes photon index 2.0
GX 301-2...BATSEAnalysis of pulsed flux. Spectrum is calculated during periastron passage. Quotes other spectral fits during other orbital epochs. Extensive analysis of orbital variations in emission, pulse history, and orbital parameters
GX 301-2...Ariel 5Mean flux quoted here. Evans et al. 1980 give upper limits to cyclotron line emission
GX 301-2...HEAO A4Average flux assumes photon index 2.0
GX 304-1...HEAO A4Average flux assumes photon index 2.0
GX 339-4...HEAO A4Presents light curve. Not as bright during two 1978 observations. Spectral form is for high-energy tail beyond low-energy thermal component
GX 339-4...OSO 8Variable flux and spectrum. Quoted values are for first six days: hard state, transitions to soft state
GX 339-4...BATSEOptically thin thermal bremstrahlung fit. Monitoring of hard state outbursts. Shows light curves and spectral evolution. Spectrum and flux are for peak outburst
GX 339-4...EXITE · · ·
GX 339-4...SIGMAComptonized disk model quoted here. Detection of distinct spectral states and fluxes. Numbers shown are for the highest intensity state,
GX 339-4...MIT712 sigma upper limit to total emission
GX 339-4...OSSESunyaev & Titarchuk model with tau =2.39±0.09. Bright state flux listed here with significant variability detected
GX 339-4...Welcome-1Bright state flux listed. Paper includes alternate fits
GX 339-4...HEAO A4Flux assumes photon index 2.0. Not as bright at two other epochs
GX 339-4...COMPTEL2 sigma upper limit with limits at higher energies also listed
GX 340+0...HEAO A4Not as bright at two other epochs. Flux assumes photon index 2.0
GX 340+0...MIT712 sigma upper limit to total emission
GX 340+0...Narrabri753 sigma upper limit
GX 349+2...Ariel 5Average flux quoted. Somewhat weak at 50 keV. Lower fluxes reported for 1976 Feb/Mar and Dec observations
GX 349+2...HEAO A4Average flux assumes photon index 2.0
GX 354-0...SIGMABroken power-law fit with break energy in parenthesis. Light curve shown along with alternative fits
GX 354-0...BATSE · · ·
GX 354-0...HEAO A4Not as bright at two other epochs. Upper limit assumes index 2.0
GX 354-0...GRIPAlso detected at lower energies
GX 359+2...HEAO A4Average flux assumes photon index 2.0
GX 5-1...Imperial/UT/IPEBlackbody fit
GX 5-1...HEAO A4Average flux assumes photon index 2.0
GX 9+1...HEAO A4Average flux assumes photon index 2.0
H0614+091...HEAO A4Flux assumes photon index 2.0. Lower flux during two other observations
H0918-549...HEAO A4Average flux assumes photon index 2.0
H1145-619...HEAO A4Average flux assumes photon index 2.0
H1254-690...Ariel 5Mean flux quoted
H1417-624...BATSEPower-law fit with exponential cutoff energy 11.9 kev. Peak pulsed flux quoted here. Shows light curves and provides an orbital analysis
H1417-624...HEAO A4Average flux assumes photon index 2.0
H1538-522...HEAO A4Average flux assumes photon index 2.0
H1608-522...BATSEOptically thin thermal bremstrahlung fit. Peak flux and spectrum quoted. Shows light curves and spectral alternative spectral fits
H1624-490...HEAO A4Average flux assumes photon index 2.0
H1624-490...MIT712 sigma upper limit to total emission
H1636-536...HEAO A4Average flux assumes photon index 2.0
H1658-298...HEAO A4Average flux assumes photon index 2.0
H1705-250...HEAO A4Spectral fit is for hard power-law tail after subtracting thermal bremstrahlung
H1705-250...COMPTEL2 sigma upper limit with limits at higher energies also listed
H1705-440...BATSEBright outburst detected during this time. Average flux quoted
H1705-440...HEAO A4Not as bright at two other epochs. Flux assumes photon index 2.0
H1743-322...HEAO A4Not as bright during a 1977 Sep detection. Flux assumes index 2.0
H1745-203...HEAO A4Average flux which assumes photon index 2.0
H1755-338...HEAO A4Average flux which assumes photon index 2.0,
H1820-303...BATSEUpper limit to total emission for 10 day averages
H1820-303...HEAO A42 sigma upper limit
H1820-303...IPEDetection based upon epoch folding. No explicit flux given
H1822-000...HEAO A4 · · ·
H1907+097...TIFRNo pulsed emission. Also describes a 1991 March flight where the source was very weak
H1907+097...HEAO A4Average flux which assumes photon index 2.0
Her X-1...TESRE/XG81Fit includes line fixed at 52 keV with flux 3.5±1.9×10-3 cm-2 s-1 and fixed width 21 keV
Her X-1...PachmarhiPossible intense 30 minute flare
Her X-1...HEAO A4Spectral form is a power law with exponential break plus line. Spectral break is at 26.7±0.09 keV and the folding energy is 5.5±0.9 keV. Line intensity is 5.5±1.7×10-4 cm-2 s-1 with a centroid at 48±4 keV and FWHM 28±7 keV. Pulse-phase spectroscopy, pulse profile analysis and several alternative spectral fits are presented. Spectral feature around 50 keV could be emission or absorption. Levine et al. 1984 summarize all data
Her X-1...OSO 7Peak flux for the two weeks is quoted here. Light curve shows turnon of 35 day cycle
Her X-1...OSSEThermal bremstrahlung spectral fit. Light curve shows turnon of main high-state
Her X-1...BATSEThermal bremstrahlung spectral fit. Provides orbit determination
Her X-1...MPI/AITEither cyclotron emission line or lower energy absorption line. Values quoted are for emission line. Continuum emission is weak above 50 keV. Trumper et al. 1978 describe a 1976 flight
Her X-1...OSO 8 scintillator · · ·
Her X-1...Ariel 5Cyclotron line with significance 2.7 sigma . Gives upper limits to lines at higher harmonics
Her X-1...OSO 83 sigma upper limit to time-averaged line emission. Very weak continuum above 50 keV
Her X-1...LEGS2 sigma upper limit. Detected at energies below 70 keV
Her X-1...SAS 2Quoted dates are mission duration
Her X-1...HaleakelaPulsed, 15 minute, transient emission. Pulse period differs slightly from X-ray peroid
Her X-1...Whipple85/903 sigma upper limit to steady emission
KS 1731-260...SIGMANot detected during many other observations from 1989 Mar – 1991 Apr
LMC X-4...SIGMA3 sigma upper limit
LMC X-4...HEAO A4Average flux quoted assumes photon index 2.0
LMC X-4...MIT712 sigma upper limit to total emission
Nova Muscae 1991...SIGMAThe brightest flux level quoted here (Jan 9). Lists values for other epochsa and discusses a possible annihilation line feature at higher energies
OAO 1657-415...SIGMAEvidence for spin down
OAO 1657-415...HEAO A4Average flux which assumes photon index 2.0
PSR B1259+63...OSSEUnpulsed emission detected near periastron for this binary system
Sco X-1...MIT681 sigma upper limit to total emission
Sco X-1...Ariel 5Average flux listed. Reduced flux during a 1975 Mar observation
Sco X-1...Rice68 · · ·
Sco X-1...Imperial/UT/IPE1 sigma upper limit to total emission. Also not detected during a 1983 Mar 26 flight
Sco X-1...HEAO A4 · · ·
Sco X-1...OSO 82 sigma upper limit
Sco X-1...UNH70Approximate 1 sigma upper limit. Detected at lower energies
Sco X-1...POKER1 sigma upper limit. Clearly detected at lower energies
Sco X-1...MPI/AIT2 sigma upper limit. Detected below 50 keV
Sco X-1...SMM/GRS3 sigma upper limit to steady flux from neutron capture line
Sco X-1...SAS 2Quoted dates are mission duration
Sco X-1...Durham MkIIIDC signal. Null search for periodicity. Some observations in 1989 May revealing similar flux
Sco X-1...Whipple903 sigma upper limit to steady emission
Sco X-1...NRL2 sigma upper limit
Sct X-1...HEAO A4Average flux which assumes photon index 2.0
SGR 1806-20...SMMDates quoted are the detection of the first and last of six separate bursts. Lists durations and flux values for each of the bursts. Light curves shown for the four strongest. Flux is the peak flux (varies by a factor of about 20) and spectrum quoted is for the Nov 16 bursts
SGR 1900+14...BATSEThermal bremstrahlung model fit. Spectrum for the largest burst quoted. Lists the fluence and plots the light curve for each burst
SLX 1735-269...SIGMALittle sign of variability. Spectrum is averaged over all observations. Bremsstrahlung and Comptonization spectral forms also fit the data
SMC X-1...HEXEThermal bremstrahlung fit listed. Alternative fits and pulse period analysis included
SMC X-1...HEAO A4Average flux which assumes photon index 2.0
SMC X-1...Imperial/UT/IPE1 sigma upper limit to total emission
SMC X-3...HEAO A4Flux assumes photon index 2.0. Not detected at two other epochs
SS 433...HEAO 3Time-averaged fluxes. Possible interpretation as red and blue shifted 24Mg lines
SS 433...Imperial/UT/IPE1 sigma upper limit to total emission
SS 433...COMPTEL2 sigma upper limit with limits at higher energies also listed
SS 433...SMM3 sigma upper limit is for 9 day integrations
SS 433...Whipple903 sigma upper limit to steady emission
Tra X-1...SIGMANot redetected during a 1991 Jan 21 observation
Vela X-1...HEAO A4Power-law fit plus exponential cutoff e-(E-28.6)/14.0 above 28.6 keV. Numbers are for average of May observations. Pulse-phase spectroscopy and pulse timing included
Vela X-1...MPI/AITShows time-averaged light curves as a function of energy and looks at pulse-to-pulse variations. Many spectral forms quoted
Vela X-1...MIT712 sigma upper limit to total emission
Vela X-1...OSO 7Clearly detected at lower energies
Vela X-1...OSO 82 sigma upper limit. Observations at other dates also listed
Vela X-1...COS B2 sigma upper limit to pulsed emission
Vela X-1...SAS 2Date quoted is mission duration
Vela X-1...NarrabriPersistent, pulsed emission
Vela X-1...JANZOSUpper limit to total emission (95%). No pulsed emission
Vela X-1...NooitgedachtPersistent, pulsed emission
X 1732-304...SIGMANo significant variability. Spectrum fit equally well with a thermal bremstrahlung
TABLE 3B
OBSERVATION NOTES: GALAXIES, CLUSTERS, AND DIFFUSE
SourceInstrumentNotes
Coma Cluster...MIFRASOFit includes data from a lower energy detector
Coma Cluster...HXR 81 · · ·
Coma Cluster...OSO 8 · · ·
Coma Cluster...HEAO A4 · · ·
LMC...EGRET · · ·
NGC 253...OSSEAlso gives upper limits to line flux
NGC 253...EGRET · · ·
Perseus Cluster...HEAO A4 · · ·
Rho Oph...EGRET · · ·
Rho Oph...COS B · · ·
Virgo Cluster...HEAO A4 · · ·
TABLE 3C
OBSERVATION NOTES: PULSARS
SourceInstrumentNotes
Crab...MIFRASO · · ·
Crab...POKERNumbers are for total emission first then in parenthesis pulsed emission
Crab...UCSD72Total spectrum and flux values quoted. Also gives spectra on individual days
Crab...UCSD66Also includes data from a 1965 Sep 23 flight further discussed in Peterson, Jacobson, & Pelling 1966
Crab...HEAO A-4Values quoted are for a broken power law, first for total emission then pulsed emission. Break energies and indices are in parenthesis.
Crab...HEXEBroken power law with break values in parenthesis. Some pulse-phase spectroscopy. Upper limit to 77 keV line of 1.0×10-3 cm-2 s-1 (99%). Spectral fit relies upon combining with other data sets
Crab...LEGSPower-law fit with total emission followed by pulsed emission in parenthesis. Also gives 3 sigma upper limits to 0.073 and 0.40 MeV line emission of 6.2×10-4 cm-2 s-1 and 1.7×10-3 cm-2 s-1
Crab...GRISPower-law fit with total emission followed by pulsed emission in parenthesis. Sets upper limits on line emission and gives some pulse-phase spectroscopy
Crab...NRLPulsed spectrum quoted. Best-fit spectrum for nebular emission is a broken power law with a break at about 80 keV and index going from 1.99 to 2.42. 95% upper limits to 73.3 keV line emission of 1.5×10-3 cm-2 s-1. See Strickman, Kurfess & Johnson 1982 regarding transient line emission
Crab...HXR 79Composite nebular spectrum quoted. Spectral fit assumes possible line feature at 73 keV with strength 5±1.5×10-3 cm-2 s-1
Crab...MIT68 · · ·
Crab...SaclayTotal spectrum
Crab...GSFCTotal emission
Crab...OSO 8Time averaged. No spectral variability
Crab...UCSD/TokyoTotal emission. Also maps the size and shape of the hard X-ray nebula
Crab...MIT69Total emission
Crab...MISOComposite spectrum
Crab...MarshallPulsed emission. Provides pulse profile analysis. Pulsed flux values at higher energies available
Crab...Rice68Pulsed emission. Also see Haymes et al. 1968
Crab...SIGMAPulsed emission. See Gilfanov et al. 1994 regarding possible transient spectral feature
Crab...OSSEPhase averaged emission. Upper limits to line emission conflict with reported detections. Phase-dependent hardness ratios quoted. No evidence for time variability
Crab...HEAO 3Phase averaged emission. Also gives upper limits on 73 and 400 keV line emission of 2.8×10-4 and 1.8×10-4 cm-2 s-1. Includes some pulse-phase spectroscopy. See Ling & Dermer 1991 regarding possible MeV excess
Crab...Durham MK1Also shows evidence for variable emission at 78.9 keV
Crab...JPLComposite spectrum quoted. Spectral fit assumes possible line feature at 73±1 keV with strength 3.8±0.9×10-3 cm-2 s-1 with FWHM <4.9 keV
Crab...RICETotal emission and pulsed emission in parenthesis
Crab...Bell-SandiaTotal emission. Possible line feature at 400±1 keV with strength 2.24±0.65×10-3 cm-2 s-1 with line width <3 keV
Crab...NRL70 · · ·
Crab...UNHDGTPresents limits on line features
Crab...UCSD77Average pulsed power quoted. Not detected during two shorter flights. Gives some evidence for excess emission in the 1 – 10 MeV range
Crab...FIGARO IIPulsed emission. Includes pulse-phase spectroscopy.xxAlso see Massaro et al. 1991 for possible 440 keV line emission
Crab...UNH71Stated flux is for pulsed emission only
Crab...UCRPulse-shape analysis; no flux quoted
Crab...SMMFlux is a 3 sigma upper limit to single day transient in a search for line emission reported by other experiments
Crab...Bristol · · ·
Crab...COMPTELTotal pulsed spectrum.
Crab...Southampton2 sigma upper limit. Includes data up to 10 MeV. Possibly a weak detection if all data from 1 – 10 MeV combined
Crab...MPI ComptonTotal emission quoted
Crab...Case-WesternFlux is time-averaged pulsed emission
Crab...NRL emulsion · · ·
Crab...Saclay · · ·
Crab...SAS 2Total emission followed by pulsed in parenthesis
Crab...EGRETTotal (pulsar) ; some evidence for pulse shape variability; pulse-phase spectroscopy; see De Jager et al. 1996a for revised unpulsed spectrum
Crab...COS BPulsed emission quoted followed by unpulsed in parenthesis. Some evidence for pulse shape variability. Spectra for main peaks and interpulse shown
Crab...CornellFlux quoted is total flux, but see Greisen et al. 1975 regarding a later flight on 1973 Jul 23 where the reported flux is much weaker for the same instrument
Crab...Whipple72Unpulsed flux reported with possible variability. See Grindlay, Helmken, & Weekes 1976 for evidence for pulsed flux for the same instrument
Crab...Whipple90Unpulsed only. 99% level upper limit of 7×10-12 cm-2 s-1 to pulsed emission
Crab...Ootacamund · · ·
Crab...ASGATMeasured flux consistent with other TeV experiments. 99% level upper limit of 2.2×10-12 cm-2 s-1 (>600 GeV) for pulsed emission
Crab...HEGRAUnpulsed emission. Flux value also carries 30% systematic error. See Petry et al. 1996 for a reanalysis
Geminga...MISO2 sigma upper limit with limits at other energies available
Geminga...RiceUpper limit is 1 sigma with limits available over the rest of the energy range
Geminga...OSO 82 sigma upper limit. Lowest flux limit quoted. Lists upper limits in various bands at all epochs
Geminga...OSSE2 sigma upper limit to phase averaged flux which assumes power law of index 2.0. Also see Strickman et al. 1996b
Geminga...Ariel 52 sigma upper limit with upper limits at higher energies available
Geminga...MPI Compton · · ·
Geminga...COMPTEL2 sigma upper limit. Limit in 10 – 30 range of <3×10-7 cm-2 s-1 MeV-1
Geminga...EGRETTotal emission. Includes pulse-phase spectroscopy. No evidence for light curve variability
Geminga...SAS 2Also see Mattox et al. (1992) for a reanalysis including light curve
Geminga...COS B · · ·
Geminga...Whipple755 sigma upper limit
Geminga...Whipple903 sigma upper limit on steady emission. Also 5 sigma pulsed limit of <6.5×10-12 cm-2 s-1
Geminga...OotacamundAssociates count rate excesses with phase of COS B measured pulsations
PSR 0833-45...HEAO A43 sigma pulsed upper limit. Limits at higher energies available
PSR 0833-45...Rice71 · · ·
PSR 0833-45...HEAO A4Average flux which assumes photon index 2.0
PSR 0833-45...OSO 82 sigma upper limit
PSR 0833-45...OSSEPulsed emission analysis. Power-law and flux values are for total average pulsed flux. Also discusses multiinstrument fits. See De Jager, Harding, & Strickman 1996b regarding unpulsed spectrum
PSR 0833-45...Figaro II2 sigma pulsed upper limit
PSR 0833-45...UCR · · ·
PSR 0833-45...HEAO 32 sigma pulsed upper limit with limits at lower energies available
PSR 0833-45...Case-Western · · ·
PSR 0833-45...COMPTEL · · ·
PSR 0833-45...EGRETTotal emission measured. Extensive pulse-phase spectroscopy. Evaluates effects of a glitch on gamma-ray behavior
PSR 0833-45...SAS 2Should include 17% systematic uncertainty
PSR 0833-45...COS BPulsed emission measured. No unpulsed emission. Some sign of spectral changes at low and high energies. Pulse-phase spectroscopy presented
PSR 0833-45...Gamma-1 · · ·
PSR 0833-45...Narrabri753 sigma upper limit to total emission. Evidence for pulsed emission at a much lower flux
PSR 0833-45...BIGRAT95% confidence level upper limit to pulsed emission
PSR 1055-52...HEAO A43 sigma pulsed upper limit with limits at higher energies available
PSR 1055-52...SAS 22 sigma pulsed upper limit
PSR 1055-52...COS B3 sigma pulsed upper limit
PSR 1055-52...COMPTEL2 sigma upper limit to steady emission. No convincing evidence for pulsed emission
PSR 1055-52...EGRETNo evidence for unpulsed emission. Pulsations seen mainly above 500 MeV
PSR 1509-58...BATSEPlots flux values up to 1 MeV
PSR 1509-58...SIGMATotal flux quoted. Estimated to be 93%±30% pulsed based on a comparison with BATSE pulsed flux
PSR 1509-58...HEAO 32 sigma pulsed upper limit with limits at higher energies available
PSR 1509-58...OSSEPulsed component measured
PSR 1509-58...Welcome-1Pulsed flux
PSR 1509-58...COMPTEL · · ·
PSR 1509-58...SAS 22 sigma pulsed upper limit
PSR 1509-58...EGRET99.9% flux limit for pulsed emission
PSR 1706-44...OSSE2 sigma upper limit assuming power-law index 2.0
PSR 1706-44...COMPTEL2 sigma upper limit to steady emission. No convincing evidence for pulsed emission
PSR 1706-44...EGRETBroken power-law model with break values in parenthesis. See also Thompson et al. 1992 for an earlier analysis
PSR 1706-44...COS B · · ·
PSR 1706-44...CangarooUnpulsed emission measured. The quoted flux error represents a 30% systematic error
PSR B0656+14...EGRETPulsed emission; no dc excess found
PSR B1951+32...OSSE2s upper limit to phase averaged. Pulsed emission assumes a photon index of 2.0
PSR B1951+32...COMPTEL2 sigma upper limit to steady emission. Some weak evidence for pulsed emission
PSR B1951+32...EGRETPulsed emission measured with no evidence for unpulsed
TABLE 3D
OBSERVATION NOTES: BLAZARS
SourceInstrumentNotes
3C 273...HEAO A4Also see Levine et al. 1984. Flux values at lower energies also given
3C 273...MIFRASO · · ·
3C 273...TICALSpectral fit is poorly constrained
3C 273...MPI/AIT80 · · ·
3C 273...MPI/AITSee Pietsch et al. 1981 regarding an earlier observation in 1978 Nov by the same instrument
3C 273...HEXEOther spectral fits included
3C 273...SIGMAAverage numbers quoted. Not detected at two later epochs
3C 273...OSO 72 sigma upper limit
3C 273...OSO 82 sigma upper limit
3C 273...OSSEValues listed are from the 1991 Jun 15 – 28 observation. Detected at several other periods with variable flux but little spectral change
3C 273...COMPTELNot redetected in 1991 Oct
3C 273...UCR2 sigma upper limit with limits at higher energies available
3C 273...COS B · · ·
3C 273...EGRET · · ·
3C 273...SAS 22 sigma upper limit
3C 273...Narrabri753 sigma upper limit
3C 273...Whipple9099.9% conf. level upper limit. Higher limits for 1992 Feb – Apr and 1993 Jan observations
3C 279...SIGMA2 sigma upper limit
3C 279...OSSENot detected during several other observations through 1993 5 – 12
3C 279...COMPTELNot redetected in 1991 Oct
3C 279...EGRETSee Thompson et al. 1995 regarding other observations,
3C 279...SAS 22 sigma upper limit
3C 279...Whipple9099.9% conf. level upper limit. Also lists limit 1991 Dec – Apr observations
3C 454.3...OSSEUpper limits at higher energies listed. Not detected during other observations
3C 454.3...EGRETVariable by at least a factor of 3. Flux quoted is maximum. Also see Thompson et al. 1995
3C 454.3...Whipple903 sigma upper limit. Kerrick et al. 1995 give limits for a 1993 Oct – Nov observation
CTA 102...OSSEFluxes at higher energies listed. Mainly upper limits at two other epochs
CTA 102...EGRETWeak detections or upper limits at three other epochs. Also see Thompson et al. 1995
CTA 102...Whipple9099.9% conf. level upper limit
H1517+656...OSSEUpper limits at higher energies
MRK 421...HXR 81M · · ·
MRK 421...OSSE2 sigma upper limit with upper limits at higher energies also listed
MRK 421...OSO 82 sigma upper limit. Marginal detection in 25 – 60 keV band
MRK 421...HEGRAFlux value has large systematic errors,
MRK 421...EGRETAlso see Thompson et al. 1995 and Sreekumar et al. 1996 for more information
MRK 421...SAS 22 sigma upper limit
MRK 421...Whipple90Values are from the most intense outburst. See Kerrick et al. 1995, Punch et al. 1992, and Schubnell et al. 1996 for further analysis of a larger database
MRK 501...OSO 82 sigma upper limit
MRK 501...SAS 22 sigma upper limit
MRK 501...Whipple90Average flux quoted. Some evidence for variability
MRK 501...HEGRAFlux error is statistical. Add (+1.5,-0.6) systematic error
NRAO 190...EGRETLists several upper limits and detections for several other epochs. Describes multiwavelength observations for this flaring period
OJ 287...EGRETAlso describes multiwavelength observations
OJ 287...Whipple9099.9% conf. level upper limit. Also gives upper limit for a 1992 Mar – Apr observation
PG 1416-129...OSSETransient detection during 1/2 of a two week observation. Includes fit to data with nonsimultaneous Ginga data
PKS 0235+164...EGRETNot variable during this observation, but not detected during other epochs (Thompson et al. 1995)
PKS 0235+164...Whipple9099.9% conf. level upper limit
PKS 0446+112...EGRETAverage flux quoted; highly variable
PKS 0454-234...EGRET · · ·
PKS 0528+134...OSSEAverage values listed here. Fluxes at higher energies and light curve available
PKS 0528+134...COMPTELAverage spectrum quoted. Evidence for spectral changes given and discussions of variability and spectral changes
PKS 0528+134...EGRETAlso seen during two other epochs within ±1 month of this observation. Variable over a few days. See Thompson et al. 1995, Dingus et al. 1996, and Mukherjee et al. 1996 for other analyses
PKS 0528+134...Whipple9099.9% conf. level upper limit. Similar limit at an energy threshold of 500 GeV for a 1992 Mar observation
PKS 1622-297...OSSEBest-fit power law -1.87 when combined with EGRET data
PKS 1622-297...EGRETHighly variable light curve shown. Peak flux quoted here
PKS 2155-304...OSSEUpper limits at higher energies. Not detected during other observations
PKS 2155-304...EGRETNo variability during this observation although previous observations yielded only upper limits
QSO 1424-418...EGRET · · ·
QSO 0130-171...EGRET · · ·
QSO 0202+149...OSSE2 sigma upper limit and lists upper limits at higher energies
QSO 0202+149...EGRET · · ·
QSO 0202+149...Whipple9099.9% conf. level upper limit
QSO 0208-512...COMPTELNot detected during several epochs in 1991. Strange spectrum since not seen at energies directly above and below this range
QSO 0208-512...EGRETLower flux for several other observations within ±3 months
QSO 0420-014...EGRETNot redetected during a second observation in 1992 May/Jun
QSO 0458-020...EGRET · · ·
QSO 0521-365...EGRET · · ·
QSO 0537-441...EGRETUpper limits only for three subsequent observations
QSO 0716+714...OSSE2 sigma upper limit and lists upper limits at higher energies
QSO 0716+714...EGRETAverage spectrum quoted. Variable flux but no sign of spectral changes over six different observations. Also see Thompson et al. 1995 and Nolan et al. 1996
QSO 0716+714...Whipple9099.9% conf. level upper limit. Also gives upper limit at an energy threshold of 500 GeV for a 1992 Nov observation
QSO 0735+178...EGRET · · ·
QSO 0804+499...EGRET · · ·
QSO 0827+243...EGRET · · ·
QSO 0829+046...EGRET · · ·
QSO 0836+710...EGRET · · ·
QSO 0917+449...EGRETRelatively steady source
QSO 0954+556...EGRETNo evidence for variability. Also see Thompson et al. 1995
QSO 0954+658...EGRETNot detected during several other observations. See Thompson et al. 1995 or Sreekumar et al. 1996 for more information
QSO 1127-145...EGRETNot seen during other epochs. Flux value is from Thompson et al. 1995
QSO 1156+295...EGRETNot detected during many other epochs. Also see Thompson et al. 1995 (for flux)
QSO 1156+295...COS B2 sigma upper limit. Also lists limit in 50 – 150 MeV band
QSO 1156+295...Whipple9099.9% conf. level upper limit
QSO 1219+285...Ariel 52 sigma upper limit
QSO 1219+285...EGRETAverage flux and spectrum quoted. Later epoch described in Thompson et al. 1995 shows some variability
QSO 1219+285...COS B2 sigma upper limit and also lists limit in 50 – 150 MeV band
QSO 1219+285...Whipple9099.9% conf. level upper limit. Similar limit for a 1993 Mar – Apr observation
QSO 1222+216...COMPTELNot detected at energies above and below this. Possibly identified with 2EG J1224+2155
QSO 1222+216...EGRETFlux and spectrum variable. Seen during at least one other epoch at reduced flux. Also see Thompson et al. 1995
QSO 1222+216...Whipple9099.9% conf. level upper limit
QSO 1229-021...EGRET · · ·
QSO 1229-021...EGRET · · ·
QSO 1313-333...EGRET · · ·
QSO 1317+520...EGRET · · ·
QSO 1331+170...EGRET · · ·
QSO 1406-076...EGRETLong-term variability shown. Also see Thompson et al. 1995
QSO 1510-089...EGRETWeak flux. Little sign of variability. Also see Thompson et al. 1995
QSO 1604+159...EGRETLittle sign of variability. Also see Thompson et al. 1995
QSO 1604+159...Whipple9099.9% conf. level upper limit
QSO 1606+106...EGRETDetectable variability. Also see Thompson et al. 1995
QSO 1611+343...EGRETNot detected during other observations. Also see Thompson et al. 1995
QSO 1622-253...EGRET · · ·
QSO 1633+382...EGRETIncludes multiwavelength spectrum. See Thompson et al. 1995 or Sreekumar et al. 1996 for more observations
QSO 1633+382...Whipple9099.9% conf. level upper limit
QSO 1730-130...EGRETAverage flux and spectrum
QSO 1739+522...EGRETAverage flux and spectrum
QSO 1908-201...EGRETAverage flux and spectrum
QSO 1933-400...EGRETAverage flux and spectrum
QSO 2005-489...EGRETAverage flux quoted. Not claimed as a detection with inclusion of further data then reevaluated again by Lin et al. 1997
QSO 2022-077 6...EGRETAverage spectrum and flux quoted
QSO 2022-077 6...Whipple9099.9% conf. level upper limit
QSO 2052-474...EGRET · · ·
QSO 2200+420...EGRETAlso gives upper limits for many other observations from 1991 May to 1995 Jan
QSO 2200+420...Whipple90 · · ·
QSO 2209+236...EGRETAverage spectrum and flux quoted
QSO 2356+196...EGRET · · ·
TABLE 3E
OBSERVATION NOTES: SEYFERTS
SourceInstrumentNotes
3C 111...OSO 72 sigma upper limit during second epoch quoted
3C 111...EGRET2 sigma upper limit
3C 111...OSSE1991 values quoted. See Kurfess 1994 for more spectral information
3C 111...COMPTEL2 sigma upper limit. See Maisack, Mannhaim, & Collmar 1997 for 3 – 30 MeV limits
3C 111...SAS 22 sigma upper limit
3C 111...Whipple9099.9% conf. level upper limit
3C 120...MPI/AIT2 sigma upper limit. Limits at higher energies up to 200 keV also available
3C 120...EGRET2 sigma upper limit
3C 120...HEAO A4 · · ·
3C 120...OSSEAverage flux. See Kurfess 1994 for more spectral information
3C 120...COMPTEL2 sigma upper limit. See Maisack et al. 1997 for 3 – 30 MeV limits
3C 120...SAS 22 sigma upper limit
3C 390.3...HEAO A4 · · ·
3C 390.3...OSO 72 sigma upper limit estimate
3C 390.3...OSSEAverage flux. See Kurfess 1994 for more spectral information
Cen A...OSO 7High state of two observations. Also gives spectrum for 1972 Jul – Aug
Cen A...HEAO A4Composite spectrum quoted
Cen A...Poker · · ·
Cen A...UCBSpectral fit includes 1 – 10 keV data from a separate observation
Cen A...MPI/AIT · · ·
Cen A...HEXE1988 spectrum quoted. Other model fits included
Cen A...RICEPossible gamma-ray lines at 1.6 and 4.5 MeV
Cen A...Rice6895% conf. level. Upper limits at higher energies available
Cen A...SIGMABrightest of three observations quoted here. Variable flux but constant index
Cen A...SIGMASpectrum is average over all observations. See Bond et al. 1996 for a more recent analysis
Cen A...BATSEMean spectral index. Shows light curves and spectral development. Averages quoted
Cen A...OSSEBroken power law with break and reference energy the same. Spectral and flux information is for the average of the 1991 observations. Shows light curves and spectral evolution. Spectral index independent of intensity at low energies. Also see Johnson et al. 1994.
Cen A...LEGSGives upper limits to MeV line emission
Cen A...MPI Compton · · ·
Cen A...UCRUpper limits at higher energies and for line emission given
Cen A...SAS 22 sigma upper limit
Cen A...COS B2 sigma upper limit. Also lists limit in 50 – 150 MeV band
Cen A...Durham MKIII3 sigma upper limit
Cen A...Narrabri75 · · ·
Cen A...JANZOSUpper limit to total emission (95%)
ESO 141-G55...EGRET2 sigma upper limit
ESO 141-G55...HEAO A4 · · ·
ESO 141-G55...OSSE2 sigma upper limit
ESO 141-G55...COMPTEL2 sigma upper limit. See Maisack et al. 1997 for 3 – 30 MeV limits
IC 4329A...Imperial/UT/IPE1 sigma upper limit to total emission
IC 4329A...OSSEAverage flux quoted
IC 4329A...OSSEIncludes simultaneous ROSAT observation and combined spectral fits
IC 4329A...COMPTEL2 sigma upper limit. See Maisack et al. 1997 for 3 – 30 MeV limits
IC 4329A...SAS 22 sigma upper limit
IC 4329A...EGRET2 sigma upper limit. Also lists COMPTEL limits for several bands
IC 4329A...COS B2 sigma upper limit. Also lists limit in 50 – 150 MeV band
MCG +8-11-11...EGRET2 sigma upper limit
MCG +8-11-11...OSO 8Peak flux and highest spectrum in a 3 day period quoted. Variable but little change in spectrum
MCG +8-11-11...BolognaAverage flux over two transits
MCG +8-11-11...MIFRASO · · ·
MCG +8-11-11...OSSEAverage flux quoted. See Kurfess 1994 for more spectral information
MCG +8-11-11...MISOSpectral fit is for less than 1 MeV. Above this a break is needed
MCG +8-11-11...COMPTEL2 sigma upper limit. See Maisack et al. 1997 for 3 – 30 MeV limits
MCG +8-11-11...MPI ComptonLimit in 3 – 10 MeV band available
MCG +8-11-11...SAS 22 sigma upper limit
MCG -5-23-16...HEAO A4 · · ·
MCG -5-23-16...BATSEAverage flux quoted
MCG -5-23-16...OSSEAverage flux quoted. See Kurfess 1994 for more spectral information
MCG -5-23-16...SAS 22 sigma upper limit
MCG -5-23-16...COS B2 sigma upper limit. Also lists limit in 50 – 150 MeV band
MCG -6-30-15...OSSEAverage flux quoted. See Kurfess 1994 for more spectral information
MCG -6-30-15...COMPTEL2 sigma upper limit. See Maisack et al. 1997 for 3 – 30 MeV limits
MCG -6-30-15...EGRET2 sigma upper limit
MKN 463...BATSEAverage flux quoted
MRK 279...HEAO A4 · · ·
MRK 279...OSSESee Kurfess 1994 for more spectral information
MRK 279...SAS 22 sigma upper limit
MRK 279...EGRET2 sigma upper limit
MRK 509...HEAO A4Average flux and spectrum
MRK 509...OSSEAverage flux. See Kurfess 1994 for more spectral information
MRK 509...MPI/AIT2 sigma upper limit; limits at higher energies up to 200 keV also available
MRK 509...COMPTEL2 sigma upper limit; see also Maisack et al. 1997 for 3 – 30 MeV limits
MRK 509...SAS 22 sigma upper limit
MRK 509...EGRET2 sigma upper limit
NGC 1275...OSO 7Spectrum of hard tail calculated after subtracting 6.6 keV thermal bremstrahlung contribution
NGC 1275...HXR 81M · · ·
NGC 1275...TESRE/XG81NGC 1275 likely source of hard tail detected from the Perseus cluster. Flux includes small component due to thermal emission
NGC 1275...OSSE3 sigma upper limit. Much weaker than previously reported detections. Upper limits at higher energies shown
NGC 1275...EGRET2 sigma upper limit
NGC 1275...Whipple9099.9% conf. level upper limit. Also an upper limit for 1992 Dec observations at a 350 GeV energy threshold
NGC 3783...OSSESee Kurfess 1994 for more spectral information
NGC 3783...COMPTEL2 sigma upper limit; see also Maisack et al. 1997 for 3 – 30 MeV limits
NGC 3783...SAS 22 sigma upper limit
NGC 3783...HEAO A4 · · ·
NGC 3783...EGRET2 sigma upper limit
NGC 4151...OSO 7Average spectrum quoted
NGC 4151...UCSD · · ·
NGC 4151...Ariel 5 · · ·
NGC 4151...SIGMASpectrum is average over all observations
NGC 4151...MISOAlternative spectral model involves power law plus exponential tail. Perotti et al. 1981b gives results of a MISO measurement from 1979 Sep 30 showing reduced flux while Bassani et al. 1986 give upper limits for a 1980 observation
NGC 4151...HXR 76 · · ·
NGC 4151...EGRET2 sigma upper limit
NGC 4151...Whipple9099.9% conf. level upper limit
NGC 4151...HEAO A4Average spectrum and flux quoted. Variability detected. Possible intensity-spectrum correlation. Other model fits given
NGC 4151...HXR 81M · · ·
NGC 4151...BolognaAverage flux over two transits
NGC 4151...HEXESpectrum for highest flux quoted. Other model fits included. Discusses relevance of reflection component
NGC 4151...MIFRASOAlso discusses a 1986 Jul observation
NGC 4151...OSSEBroken power law with break energy and index in parenthesis. Other model fits included. Variability shown. Also see Johnson et al. 1997
NGC 4151...COMPTEL2 sigma upper limit. See Maisack et al. 1997 for 3 – 30 MeV limits
NGC 4151...UCR2 sigma upper limit. Limits at higher energies available
NGC 4151...SAS 22 sigma upper limit
NGC 4151...COS B2 sigma upper limit. Also lists limit in 50 – 150 MeV band
NGC 4388...HEAO A4Average flux and spectrum. Variability detected. Fluxes at lower energies available
NGC 4388...BATSEAverage flux quoted
NGC 4388...SIGMADetected during observations of the Virgo cluster. May account for the total emission from the cluster
NGC 4388...OSSESee Kurfess 1994 for more spectral information
NGC 4507...BATSEAverage flux quoted
NGC 4507...OSSEExponential fit. Extensive spectral modelling. Discusses implications for diffuse background
NGC 4507...COS B2 sigma upper limit. Also lists limit in 50 – 150 MeV band
NGC 5506...BATSEAverage flux quoted
NGC 5548...EGRET2 sigma upper limit
NGC 5548...HEAO A4 · · ·
NGC 5548...OSSEAverage flux. See Kurfess 1994 for more spectral information
NGC 5548...COMPTEL2 sigma upper limit. See also Maisack et al. 1997 for 3 – 30 MeV limits
NGC 5548...SAS 22 sigma upper limit
NGC 6814...HEAO A4 · · ·
NGC 6814...OSSE · · ·
NGC 6814...COMPTEL2 sigma upper limit. See also Maisack et al. 1997 for 3 – 30 MeV limits
NGC 6814...SAS 22 sigma upper limit
NGC 7582...OSSE2 sigma upper limit. See also Maisack et al. 1997 for 3 – 30 MeV limits
NGC 7582...COMPTELAverage flux. See Kurfess 1994 for more spectral information
TABLE 3F
OBSERVATION NOTES: SUPERNOVAE AND REMNANTS
SourceInstrumentNotes
Cas A...OSSEFit includes some lower energy data. Limits for lines also included
Cas A...COMPTELFlux from 44Ti line at 1.152±0.015 MeV nd r.m.s. width of 58±10 keV. Line is possibly Doppler broadened
SN 1987A...HEXEFlux on outburst day 407
SN 1987A...Pulsar X-1 · · ·
SN 1987A...SIGMA3 sigma upper limit with upper limits to line emission
SN 1987A...GRIPAlso gives continuum spectrum. Values at three other epochs also available. Also gives flux for 1.24 MeV line
SN 1987A...HEXAGONE2 sigma upper limit; includes upper limits several lines and continuum at higher energies up to 2 MeV
SN 1987A...Welcome 190% confidence level upper limit to all 57Co emission; sets limit to abundance ratio of 57Co/56Co
SN 1987A...LockheedObservation 250 days post supernova event
SN 1987A...GRIPValues at three other epochs also available
SN 1987A...SMM · · ·
SN 1987A...Kosmos 1870 · · ·
SN 1987A...SMM3 sigma upper limit based on 35 day sums
SN 1987A...UCRLine feature attributed to 1.238 MeV 56Co decay
SN 1987A...GRIPValues at three other epochs also available
SN 1987A...SMM · · ·
SN 1987A...Kosmos 1870 · · ·
SN 1987A...GRADAlso presents upper limits to 0.844 MeV emission
SN 1987A...GRISFlux on day 613. Flux available for day 433 as well. Also gives flux values for 1.24 MeV line
SN 1987A...JPLUpper limits to continuum and 847 keV emission
SN 1987A...SMM3 sigma upper limit based on 35 day sums
SN 1987A...Kosmos 16863 sigma upper limit
SN 1987A...UCRLine feature attributed to unresolved 1.77, 2.015, and 2.035 MeV lines from 56Co decay
SN 1987A...ADFA3 sigma upper limit
SN 1987A...Narrabri · · ·
SN 1987A...Potchefstroom · · ·
SN 1993J...OSSENot detected during a 1993 Jun obs. Some possibility of source confusion
SN 1993J...COMPTEL2 sigma upper limit. Also lists upper limits for other lines and for an earlier observation
TABLE 3G
OBSERVATION NOTES: UNIDENTIFIED SOURCES
SourceInstrumentNotes
2CG 006+00...Comptel3 sigma upper limit with limits at lower energies also given
2CG 006+00...COS B · · ·
2CG 006+00...EGRET · · ·
2CG 006+00...Potchefstroon95% upper limit for pulsed emission assuming the source is PSR 1802-23
2CG 010-31...COS B · · ·
2CG 013+00...COS B · · ·
2CG 036+01...OSO 82 sigma upper limit
2CG 036+01...COS B · · ·
2CG 054+01...OSO 82 sigma upper limit
2CG 054+01...COS B · · ·
2CG 065+00...OSO 8Possible 3.5 sigma detection over full energy range. Upper limit in this range for the first epoch
2CG 065+00...Ariel 52 sigma upper limit
2CG 065+00...COS B · · ·
2CG 065+00...EGRET · · ·
2CG 065+00...Whipple755 sigma upper limit
2CG 075+00...Ariel 52 sigma upper limit
2CG 075+00...COMPTEL3 sigma upper limit with limits at lower energies also given
2CG 075+00...COS B · · ·
2CG 075+00...EGRET · · ·
2CG 075+00...Whipple755 sigma upper limit
2CG 078+01...Ariel 52 sigma upper limit
2CG 078+01...COMPTEL3 sigma upper limit with limits at lower energies also given
2CG 078+01...COS B · · ·
2CG 078+01...EGRET · · ·
2CG 078+01...Whipple755 sigma upper limit. Hint of a detection but possible possible systematic error involved
2CG 095+04...OSO 82 sigma upper limit
2CG 095+04...COS B · · ·
2CG 121+04...OSO 82 sigma upper limit
2CG 121+04...Ariel 52 sigma upper limit
2CG 121+04...COS B · · ·
2CG 121+04...Whipple755 sigma upper limit
2CG 135+01...OSO 82 sigma upper limit
2CG 135+01...MISOUpper limits at lower and higher energies given. Requires a break to join with >100 MeV data
2CG 135+01...Ariel 53.2 sigma detection over full range
2CG 135+01...COMPTELNo sign of variability
2CG 135+01...UNHDGT2 sigma upper limits also quoted in many other energy bands
2CG 135+01...UCR2 sigma upper limit with limits at lower energies available
2CG 135+01...COS B · · ·
2CG 135+01...EGRET · · ·
2CG 135+01...Whipple755 sigma upper limit
2CG 135+01...Whipple902 sigma upper limit
2CG 218-00...COS B · · ·
2CG 235-01...OSO 82 sigma upper limit
2CG 235-01...COS B · · ·
2CG 284-00...OSO 82 sigma upper limit
2CG 284-00...COMPTEL3 sigma upper limit with limits at lower energies also given
2CG 284-00...COS B · · ·
2CG 284-00...EGRET · · ·
2CG 288-00...COMPTEL3 sigma upper limit with limits at lower energies also given
2CG 288-00...COS B · · ·
2CG 288-00...EGRET · · ·
2CG 311-01...OSO 8Possible 3.5 sigma detection over full energy range
2CG 311-01...Ariel 52 sigma upper limit
2CG 311-01...COS B · · ·
2CG 311-01...EGRET · · ·
2CG 333+01...OSO 82 sigma upper limit
2CG 333+01...Ariel 52 sigma upper limit
2CG 333+01...COS B · · ·
2CG 356+00...COS B · · ·
2CG 359-00...COS B · · ·
2CG 359-00...EGRETAverage flux quoted
2EG 0812-0648...EGRET · · ·
2EG J0008+7307...EGRET · · ·
2EG J0119+0312...EGRET · · ·
2EG J0159-3557...EGRET · · ·
2EG J0216+1107...EGRET · · ·
2EG J0220+4228...EGRET · · ·
2EG J0239+2818...EGRET · · ·
2EG J0323+5126...EGRET · · ·
2EG J0403+3357...EGRET · · ·
2EG J0406+1704...EGRET · · ·
2EG J0422+1414...EGRET · · ·
2EG J0426+6618...EGRET · · ·
2EG J0432+2910...EGRETAverage flux quoted
2EG J0432+2910...Whipple9099.9% conf. level upper limit
2EG J0437+1524...EGRET · · ·
2EG J0506+3424...EGRET · · ·
2EG J0511+5523...EGRET · · ·
2EG J0520+2626...EGRET · · ·
2EG J0521+2206...EGRET · · ·
2EG J0545+3943...COMPTEL3 sigma upper limit with limits at lower energies also given
2EG J0545+3943...EGRET · · ·
2EG J0617-0652...EGRET · · ·
2EG J0618+2234...EGRET · · ·
2EG J0635+0521...EGRET · · ·
2EG J0720-4746...EGRETAverage flux quoted
2EG J0744+5438...EGRETWeakr or not detected during several other observations. Proposed as a blazar candidate due to variability and possible association with radio source 87GB 073840.5+545138. Also see Thompson et al. 1995 and Nolan et al. 1996
2EG J0744+5438...EGRET · · ·
2EG J0809+5117...EGRET · · ·
2EG J0852-1237...EGRET · · ·
2EG J1054+5736...EGRET · · ·
2EG J1103-6106...EGRET · · ·
2EG J1136-0414...EGRETAlso see Sreekumar et al. 1996; extended source
2EG J1233-1407...EGRET · · ·
2EG J1233-1407...EGRET · · ·
2EG J1239+0441...EGRET · · ·
2EG J1239+0441...EGRET · · ·
2EG J1248-8308...EGRET · · ·
2EG J1324-4317...EGRET · · ·
2EG J1332+8821...EGRET · · ·
2EG J1346+2942...EGRETAlso see Sreekumar et al. 1996
2EG J1430+5356...EGRET · · ·
2EG J1443-6040...EGRET · · ·
2EG J1457-1916...EGRET · · ·
2EG J1528-2352...EGRET · · ·
2EG J1631-2845...EGRET · · ·
2EG J1635-1427...EGRET · · ·
2EG J1648-5042...EGRET · · ·
2EG J1709-0350...EGRET · · ·
2EG J1718-3310...EGRET · · ·
2EG J1731+6007...EGRET · · ·
2EG J1742-2250...EGRET · · ·
2EG J1746-0935...EGRET · · ·
2EG J1746-2852...EGRET · · ·
2EG J1747-3039...COMPTELPossible detection. Upper limits only at higher energies
2EG J1801-2312...COMPTEL3 sigma upper limit with limits at lower energies also given
2EG J1801-2312...EGRET · · ·
2EG J1811-2339...EGRET · · ·
2EG J1813-1229...EGRET · · ·
2EG J1815+2950...EGRET · · ·
2EG J1821-7915...EGRET · · ·
2EG J1825-1307...ComptelAlso seen at lower energies. Possible source confusion with 2EG J1813-1229
2EG J1825-1307...EGRET · · ·
2EG J1828+0145...EGRET · · ·
2EG J1834-2138...EGRET · · ·
2EG J1835+5919...EGRET · · ·
2EG J1835+5919...Whipple9099.9% conf. level upper limit
2EG J1847-3220...EGRET · · ·
2EG J1850-2638...EGRET · · ·
2EG J1857+0118...Comptel3 sigma upper limit with limits at lower energies also given
2EG J1857+0118...EGRET · · ·
2EG J1950-3503...EGRETSpectral index is from the sum of several observations from 1991 Apr – 1993 Sep
2EG J2006-2253...EGRET · · ·
2EG J2026+3610...EGRET · · ·
2EG J2027+1054...EGRET · · ·
2EG J2033+4112...EGRET · · ·
2EG J2039+1131...EGRETAverage flux and spectrum qoted
2EG J2227+6122...EGRET · · ·
2EG J2243+1545...EGRET · · ·
2EG J2354+3811...EGRET · · ·
2EGS J0426+1636...EGRET · · ·
2EGS J0500+5902...EGRET · · ·
2EGS J0552-1026...EGRETAverage flux
2EGS J0555+0408...EGRETAverage flux
2EGS J0724-5157...EGRETMost significant observation quoted here
2EGS J0852-4343...EGRETAverage flux
2EGS J0909+6558...EGRETNodata
2EGS J1050-7650...EGRETAverage flux
2EGS J1133+0037...EGRET · · ·
2EGS J1220-1510...EGRET · · ·
2EGS J1236-0416...EGRET · · ·
2EGS J1324+2210...EGRET · · ·
2EGS J1418-6049...EGRET · · ·
2EGS J1504-1537...EGRETMost significant observation quoted here
2EGS J1642-2659...EGRET · · ·
2EGS J1653-4604...EGRET · · ·
2EGS J1703-6302...EGRETMost significant observation quoted here
2EGS J1708-0927...EGRET · · ·
2EGS J1736-2904...EGRETAverage flux
2EGS J1800-4005...EGRETMost significant observation quoted here
2EGS J1833-2754...EGRETAverage flux
2EGS J1903+0529...EGRETAverage flux
2EGS J1905-1120...EGRETAverage flux
2EGS J1954-1419...EGRET · · ·
2EGS J2322-0321...EGRETMost significant observation quoted here
Briggs Source...HEAO A4Transient detection of anihilation radiation
GEV J0319+2407...EGRET · · ·
GEV J0508+0540...EGRET · · ·
GEV J0615+4200...EGRET · · ·
GEV J12026+4124...EGRET · · ·
GEV J1732-3130...EGRET · · ·
GEV J1837-0610...EGRET · · ·
GEV J1907-0557...EGRET · · ·
GEV J2035+1622...EGRET · · ·
GEV J2053+5644...EGRET · · ·
GRO J0435+25...EGRETAverage flux
GRO J0516-512...COMPTELNot detected during an observation in 1991 Jul/Aug. Interesting spectrum peaking in the few-MeV range
GRO J1040+48...COMPTELAlso detected up to 3.0 MeV. Average flux quoted. Some sign of variability;
GRO J1044-77...EGRETAverage flux
GRO J1214+06...COMPTELNot detected at energies above and below this
GRO J1753+57...COMPTELBroken power law is a better fit. Not seen at other epochs
GRO J1838-04...EGRETNot seen during many other observations
GRO J1940-12...EGRET · · ·
GRO J2303+44...EGRETAverage flux
GRS 1227+025...SIGMAVariable by a factor of 2
GRO J2250-13...EGRET · · ·
GRO J2254-30...EGRET · · ·