J/ApJS/154/585 BATSE earth occultation deep sample results (Harmon+, 2004)
The burst and transient source experiment (BATSE) earth occultation catalog of
low-energy gamma-ray sources.
Harmon B.A., Wilson C.A., Fishman G.J., Connaughton V., Henze W.,
Paciesas W.S., Finger M.H., McCollough M.L., Sahi M., Peterson B.,
Shrader C.R., Grindlay J.E., Barret D.
<Astrophys. J. Suppl. Ser., 154, 585-622 (2004)>
=2004ApJS..154..585H 2004ApJS..154..585H
ADC_Keywords: Gamma rays ; Occultations
Keywords: catalogs - gamma rays: observations - methods: data analysis -
occultations - surveys - X-rays: stars
Abstract:
The Burst and Transient Source Experiment (BATSE), aboard the Compton
Gamma Ray Observatory (CGRO), provided a record of the low-energy
gamma-ray sky (∼20-1000keV) between 1991 April and 2000 May (9.1yr).
We performed a deep-sampling of 58 objects, plus a selection of 121
more objects, combining data from the entire 9.1yr BATSE data set.
Source types considered were primarily accreting binaries, but a small
number of representative active galaxies, X-ray-emitting stars, and
supernova remnants were also included. The sample represents a
compilation of sources monitored and/or discovered with BATSE and
other high-energy instruments between 1991 and 2000, known sources
taken from the HEAO 1 A-4 (1984ApJS...54..581L 1984ApJS...54..581L) and Macomb & Gehrels
(1999ApJS..120..335M 1999ApJS..120..335M, Cat. J/ApJS/120/335) catalogs.
Flux data for the deep sample are presented in four energy bands:
2040, 4070, 70160, and 160430keV. The limiting average flux level
(9.1yr) for the sample varies from 3.5 to 20mcrab (5σ) between
20 and 430keV, depending on systematic error, which in turn is
primarily dependent on the sky location.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table4.dat 143 179 BATSE Earth Occultation Deep Sample Results
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See also:
IX/20 : The Fourth BATSE Burst Revised Catalog (Paciesas+ 1999)
J/ApJS/127/79 : BATSE occultation catalog of Gamma-Ray sources (Ling+, 2000)
J/ApJS/134/385 : Supplement to the BATSE gamma-ray burst catalogs
(Kommers+, 2001)
Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- Name Object name (1)
15 A1 --- n_Name [d] Indicates a firm detection
17- 32 A16 --- AName Alternative SIMBAD or well-known name
34- 48 A15 --- Type Object type
50- 53 A4 --- Cat Assigned category (2)
54 A1 --- n_Cat [t] Transient source (3)
56- 61 F6.2 deg RAdeg Right Ascension in decimal degrees (J2000) (4)
63- 68 F6.2 deg DEdeg Declination in decimal degrees (J2000) (4)
70- 75 F6.2 deg GLON Galactic longitude (4)
77- 82 F6.2 deg GLAT Galactic latitude (4)
84- 89 F6.1 --- SigAC Detection significance after correction
for systematic error
91- 96 F6.1 --- SigBC Detection significance before correction
for systematic error
98-103 F6.1 --- F1 ? The 20-40keV band flux in milliCrabs (5)
105-107 F3.1 --- e_F1 ? Uncertainty in F1 (5)
109 A1 --- Flag [u] Indicates uncorrected 4-band fluxes (6)
111-116 F6.1 --- F2 ? The 40-70keV band flux in milliCrabs (5)
118-120 F3.1 --- e_F2 ? Uncertainty in F2 (5)
122-127 F6.1 --- F3 ? The 70-160keV band flux in milliCrabs (5)
129-131 F3.1 --- e_F3 ? Uncertainty in F3 (5)
133-138 F6.1 --- F4 ? The 160-430keV band flux in milliCrabs (4)
140-143 F4.1 --- e_F4 ? Uncertainty in F4 (4)
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Note (1): Daily 4-band light curves in Crab units for the 83 category
A & B sources (definite detections) and FITS files containing daily
20-100keV fluxes and 16-channel spectra for all 179 sources are
available on http://gammaray.msfc.nasa.gov/batse/occultation/.
Note (2): category based on the significance of detection after and before
(in parentheses) correction for systematic error, as follows:
A. (Definite detections)
- Persistent sources have an average flux (9.1yr) that exceeded
a threshold of 0.01photons/cm2/s in the 20-100keV band.
- Transient sources exhibited at least one identifiable outburst
with an average daily flux exceeding a threshold of
0.01photons/cm2/s in the 20-100keV band.
- Typical category A sources show variability on timescales of
at least hours to a few days, have a readily identifiable
period by FFT, or variability that correlates well with
behavior in other wavelength bands.
B. (Definite detections)
Sources with a 9.1yr average flux that exceeded 10σ, but with
average flux less than 0.01photons/cm2/s in the 20-100keV band.
C. (Possible detections)
Sources with a 9.1yr average flux (20-100keV) with a
significance ≥3σ and <10σ.
N. (Nondetections)
Sources with a 9.1yr average flux (20-100keV) of significance
between ±3σ.
I. (Indeterminate)
Sources with a 9.1yr average flux (20-100keV) of significance
less than -3σ, indicating confusion with nearby sources,
or a poorly characterized systematic error in the surrounding
sky region.
Note (3): 'd' indicates a category A transient source, otherwise the
source is considered a persistent source.
Note (4): Listed positions should be used for reference only.
These positions were used in the analysis, and many are based on
historical measurements and are often only accurate to within a few
arcminutes. Location errors of a few arcminutes do not significantly
affect flux measurements with the BATSE Earth Occultation Technique (EOT).
Note (5): The Crab relative fluxes, we found, are the most accurate method
of displaying flux information for the deep sample in the absence of
precise spectral fitting information for each source. Conversion
factors from mCrab units to photon and energy fluxes are:
---------------------------------------------------------------------
HER Energy Band log Average Multiplier Multiplier
Channels (keV) (keV) (photons/cm2/s) (erg/cm2/s)
---------------------------------------------------------------------
7-11 20-40 28.3 8.508x10-6 7.567x10-12
11-18 40-70 52.9 2.323x10-6 5.830x10-12
18-36 70-160 105.8 5.514x10-7 8.079x10-12
36-75 160-430 262.3 6.261x10-8 6.887x10-12
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Note (6): Cases where the uncorrected flux was very small relative to
the systematic flux correction. In these cases the uncorrected 4-band
fluxes are reported because we believe they are closer to the true
9.1-year averages. See Section 2.4 for details
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Marianne Brouty [CDS] 07-Feb-2005