J/ApJS/73/781 X-ray observations of galactic Supernova Remnants (Seward, 1990)
EINSTEIN observations of galactic supernova remnants.
Seward F.D.
<Astrophys. J. Suppl. Ser. 73, 781 (1990)>
=1990ApJS...73..781S 1990ApJS...73..781S
ADC_Keywords: Supernova remnants ; X-ray sources
Mission_Name: Einstein
Keywords: nebulae: supernova remnants - X-rays: sources
Abstract:
This paper summarizes the observations of Galactic supernova remnants
with the imaging detectors of the Einstein Observatory. X-ray surface
brightness contours of 47 remnants are shown together with gray-scale
pictures. Count rates for these remnants have been derived and are
listed for the HRI, IPC, and MPC detectors.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
snr_ctrt.dat 114 61 SNR Count Rates in Einstein Detectors
snr_indx.dat 137 76 Index to FITS Images of SNR Available on Tape
snr_psrc.dat 87 62 Unresolved X-ray Sources Within or Nearby the SNR
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See also:
VII/211 : A Catalogue of Galactic Supernova Remnants
Byte-by-byte Description of file: snr_ctrt.dat
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Bytes Format Units Label Explanations
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2- 4 A3 --- SNR_no SNR assigned number (1)
6- 10 F5.1 deg GLON Galactic longitude from Green 1988 (2)
12- 15 F4.1 deg GLAT Galactic latitude from Green 1988 (2)
17- 28 A12 --- Name Common name of SNR (1)
30- 35 F6.2 ct/s IPCcr Corrected IPC count rate (3)
37- 41 F5.2 ct/s e_IPCcr Uncertainty on IPC count rate (3)
43- 46 A4 --- f_IPCcr Flag for IPC counts (4)
48- 54 F7.3 ct/s HRIcr Corrected HRI count rate (5)
56- 61 F6.3 ct/s e_HRIcr Uncertainty on HRI count rate (5)
63- 66 A4 --- f_HRIcr Flag for HRI counts (6)
68- 74 F7.2 ct/s MPCcr Corrected MPC count rate (7)
76- 80 F5.2 ct/s e_MPCcr Uncertainty on MPC count rate (7)
82- 84 A3 --- f_MPCcr Flag for MPC counts (8)
86- 92 A7 --- class Classification of the X-ray morphology (9)
94-118 A25 --- comments Miscellaneous comments (10)
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Note (1): The first column contains the SNR assigned number; a number
between 1 and 47, assigned in order of increasing right ascension. The
SNR_no has a letter following it when this refers to an unresolved
source (usually a pulsar) within the remnant. The common name for the
supernova remnant can be found in the 'Name' column.
Note (2): These columns give the galactic coordinates of the SNR from
Green, D.A., (1988Ap&SS.148....3G 1988Ap&SS.148....3G), except for the Vela SNR where the
position of the pulsar is used as the center of the remnant. For a
more precise position, the table snr_indx.dat contains the right
ascension and declination.
Note (3): These columns give the IPC (Imaging Proportional Counter) counts
per second and error, after background subtraction. The count rates
given are for the entire energy range of the IPC (pulse-height
channels 1 to 15), integrated over the entire IPC field of view (∼60'
diameter). They have been corrected for vignetting, dead time, and
scattering from the telescope mirror. A value of zero in the IPCcr
column indicates that the source was not resolved in the IPC (see
ipc_flag column).
Note (4): This column gives a flag for the IPC count rate. The following
flags are defined:
(3) = includes surrounding diffuse emission
> = count rate is a lower limit
NRS = not resolved from other parts of SNR
ave. = count rate is an average value
Note (5): These columns give the HRI (High Resolution Imager) counts per
second and error, after background subtraction. The count rates given
have been integrated over the entire HRI field of view (∼25' diameter)
and corrected for vignetting, scattering in the telescope, and dead
time. HRI rates have been corrected to January, 1979, the first use of
HRI #3, the detector used for all SNR observations, and the closest
time to the preflight calibration. A value of zero in the HRIcr column
indicates no data or incomplete data for this remnant (see f_HRIcr
column).
Note (6): This column gives a flag for the HRI count rate. The following
flags are defined:
(2) = estimated from partial HRI observation and HRI/IPC ratio
(3) = includes surrounding diffuse emission
INC = incomplete data, much of SNR not observed
ND = no data, not observed
ave. = count rate is an average value
Note (7): These columns give the MPC (Monitor Proportional Counter) counts
per second and error, after background subtraction in channels 1-6
(1-10 keV). A value of zero in the MPCcr indicates the source was not
resolved (see f_MPCcr column).
Note (8): This column gives a flag for the MPC count rate. The following
flags are defined:
(3) = includes surrounding diffuse emission
> = count rate is a lower limit
NRB = not resolved from nearby bright sources
NRS = not resolved from other parts of SNR
ave. = count rate is an average value
Note (9): This column gives the classification of the X-ray morphology.
More than one classification may be presented for a given supernova
remnant. The following classifications are used:
S = shell
F = filled center, plerionic
IR = irregular
CO = central object
NI = neutron star, isolated
NB = neutron star in binary system
Note (10): This column gives miscellaneous comments pertaining to the
supernova remnant. An "INC" indicates that there is incomplete data,
much of SNR was not observed.
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Byte-by-byte Description of file: snr_indx.dat
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Bytes Format Units Label Explanations
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2- 4 I3 --- File FITS tape file number (1)
6- 10 F5.1 deg GLON Galactic Longitude from Green 1988 (2)
11- 15 F5.1 deg GLAT Galactic Latitude from Green 1988 (2)
17- 46 A30 --- Name Common name (2)
48- 50 I3 --- ArrSize Number of pixels in array (3)
52- 55 F4.1 arcsec PixSize Pixel size (3)
57- 58 I2 h RAh Right Ascension (B1950) (hour)
60- 61 I2 min RAm Right Ascension (B1950) (min)
63- 64 I2 s RAs Right Ascension (B1950) (sec)
66 A1 --- DE- Declination sign (B1950)
67- 68 I2 deg DEd Declination (B1950) (deg)
70- 71 I2 arcmin DEm Declination (B1950) (arcmin)
73- 74 I2 arcsec DEs Declination (B1950) (arcsec)
76- 79 I4 arcsec width Width of the function used for smooth (4)
81- 85 A5 --- f_width Flag determining kind of smoothing (4)
87-123 A37 --- Seqno Einstein fields used to make the figure (5)
125-129 I5 --- max_val Maximum data value in the array (6)
131-137 A7 keV energy Energy range of IPC data included in the
figure (6)
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Note (1): This column contains the FITS tape file number on the tape. The
first 74 files contain smoothed images, with the smooth described in
the columns "width" and "f_width". Files 75 to 148 contain a set of
background-subtracted images which have not been smoothed, with which
the user can apply his or her own image-processing techniques. These
images were used to make those in files 1 - 74. For example: the image
of CTA 1 (smoothed file = #34) before smoothing is located in tape
file 74 + 34 = 108. The maximum value of array elements has usually
been set to be 32000 for files 75 - 148.
Note (2): The galactic coordinates from Green, D.A. (1988Ap&SS.148....3G 1988Ap&SS.148....3G),
are given in the columns GLON and GLAT. The "Name" column gives the
common name of the supernova remnant. Also given in this column is
information to distinguish the array from other arrays of the same
source. For instance, a given supernova remnant may have different
files for different energy bands. See the "energy" column for details
on the energy band used. See the "Seqno" column to determine which
instrument was used.
Note (3): These columns give the number of pixels in the image array, and
the pixel size in arcseconds.
Note (4): The "width" column gives the width of the Gaussian function, in
arcseconds, used to smooth the data. This column contains a 0 when the
smoothing was done by decon or when no smoothing was applied. The
"f_width" indicates what kind of smoothing was used. The following
flags are defined:
decon = maximum entropy deconvolution
gauss = Gaussian smoothing
none = no smoothing
Note (5): This column lists the Einstein fields used to make the figure.
The sequence numbers are The Einstein sequence number is a two to five
digit number which uniquely identifies the observation. The numbers
were assigned at the time of proposal submission. An "I" before the
sequence number indicates that the field was observed with the IPC; an
"H" before the sequence number indicates that the field was observed
with the HRI. When multiple sequence numbers are listed and were
observed with the same instrument, the leading letter was omitted for
the latter sequence numbers.
Note (6): The "max_val" column gives the maximum value of the array. The
"energy" column gives the range of IPC data included in the figure (in
keV). The HRI energy range is always 0.15-4 keV, with maximum response
at 0.2-2.0 keV; this is indicated by a (1) in the "energy" column.
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Byte-by-byte Description of file: snr_psrc.dat
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Bytes Format Units Label Explanations
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2- 3 I2 h RAh Right Ascension (B1950) (hour)
5- 6 I2 min RAm Right Ascension (B1950) (min)
8-11 F4.1 s RAs Right Ascension (B1950) (sec)
13 A1 --- DE- Declination sign (B1950)
14-15 I2 deg DEd Declination (B1950) (deg)
17-18 I2 arcmin DEm Declination (B1950) (arcmin)
20-22 F3.0 arcsec DEs Declination (B1950) (arcsec)
24-35 A12 --- Name Common name of the SNR
37-39 A3 --- Instr Instrument used in the observation (1)
41-45 I5 --- Seqno Sequence number of the observation (2)
47-51 F5.3 ct/s Ctrate Total counting rates (3)
53 A1 --- loc_flg Flag for where source is located in relation
to SNR (4)
55-89 A35 --- ID Identification of the source, when known (5)
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Note (1): The instrument used in the observation will either be the IPC
(Imaging Proportional Counter) or the HRI (High Resolution Imager).
Note (2): The sequence number is a two to five digit number which uniquely
identifies the observation. The numbers were assigned sequentially at
the time of proposal submission.
Note (3): This column gives the total counting rates (in units of counts
per second). All energy channels of the IPC (1-15) are included and
corrections have been made for mirror-scattering and dead time. For
the HRI, the energy range is always 0.15-4 keV, with maximum response
at 0.2-2.0 keV, and these corrections have also been made.
Note (4): This column gives a flag indicating where the source is located,
in relation to the SNR. The following flags are defined:
O = source lies outside the boundary of the SNR
I = source lies inside the boundary of the SNR
C = source lies at the approximate center of the SNR
Note (5): This columns gives the optical identification of the source,
when known. If no identification is known, "no ID" will appear in the
column, along with any miscellaneous comments such as "extended" or
"variable."
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History:
Prepared from the tables available at the "ADS Catalogue Service"
(CfA, Harvard-Smithsonian Center for Astrophysics, Cambrigde MA)
(End) Patricio Ortiz [CDS] 06-Apr-1999