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II/143A Guide Star Photometric Catalog, Updated Version 1 (Lasker+ 1988,1996)
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The Guide Star Photometric Catalog
Lasker B.M., Sturch C.R., Lopez C., Mallama A.D., McLaughlin S.F.,
Russell J.L., Wisniewski W.Z., Gillespie B.A., Jenkner H.,
Siciliano E.D., Kenny D., Baumert J.H., Goldberg A.M.,
Henry G.W., Kemper E., Siegel M.J.
<Astrophys. J. Suppl. Ser. 68, 1 (1988)>
=1988ApJS...68....1L
================================================================================
ADC_Keywords: Photometry, sequences ; Photometry, UBV ; Bibliography
Description:
The Guide Star Photometric Catalog (GSPC) is an all-sky set of 1477
photoelectrically determined BV sequences covering the magnitude range
from 9 to 15. The GSPC was created to provide photometric calibrators
for the HST Guide Star Catalog (GSC). Each sequence nominally contains
(at least) six stars, each with a photometric precision of 0.05 mag.
In practice, a small number of sequences contain fewer stars; and the
precisions achieved for the faintest stars are more nearly 0.1 mag.
For declinations greater than +3 degrees the sequences generally lie
near the centers of the original Palomar Observatory - National
Geographic Society Sky Atlas. Other sequences lie near the centers of
the ESO/SERC Southern Sky Atlas.
The catalog also includes a list of suspected variable stars, a
bibliography of literature sequences, and additional information which
was useful in the data reduction and for quality control of the final
catalog.
The full catalog is made of 7 FITS files: tables 1 to 5, references
(table 6 of the paper) and the actual catalogue (table 7 of the
paper). The ascii versions of Tables 1 to 5 are included in this file;
the ascii version of the references (refs.dat) and of the actual
catalogue (catalog.dat) are described here.
The updated version 1 was created by replacing photometric sequences
P040, P421, S335 and S742 in GSPC version 1. The updated sequences
have improved photometry and/or positions. In addition the sigma's
in V and B-V (here e_V and e_B-V) were replaced with the values
provided by the authors when we noted a discrepancy with the
published values.
Description of the Catalog:
The catalog is available both as ASCII tables as well as FITS files,
and originally appeared on the ADC CD-ROM, Vol. 1.
The table numberings refer to the original paper.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
catalog.dat 80 9525 Updated GSPC Catalog Version 1 (flat ascii)
table 7
refs.dat 119 150 References (flat ascii)
refs.fit 2880 11 References (FITS format)
table1.fit 2880 5 Breakdown of Original Sources of Photometric
Data (FITS format)
table2.fit 2880 6 Photometric reduction parameters (FITS format)
table3.fit 2880 5 Suspect Stars (FITS format)
table4.fit 2880 21 Statistics by letter/declination (FITS format)
table5.fit 2880 30 Observation statistics (FITS format)
--------------------------------------------------------------------------------
See also:
I/220 : The HST Guide Star Catalog
Breakdown of Original Sources of Photometric Data:
The GSPC Table 1, which describes the total numbers of
sequence fields and of sequence stars in the GSPC and summarizes the
observations made at CTIO, UAO, and SPO, together with the data taken
from the literature.
Please note that this breakdown is for the original sources. For this
updated version of the catalog the entirely new sequence P040 was
obtained from CCD observations at KPNO.
One notes in this Table the relatively greater number of GSPC fields
in the south; this is explained by the 5-degree centers used in the
southern survey, as opposed to 6-degree ones in the north. One also
notes that the number of southern observations exceeds the number of
southern stars by approximately a factor of two, thus affording a
measure of redundancy. In the north, where the same ratio is only
1.06, the redundancy that can be used to address reliability of the
observations and the presence of variable stars is minimal.
Table 1: Breakdown of original sources of photometric data
----------------------------------------------------------------
Item North South Total
----------------------------------------------------------------
Survey Plate Areas 583 894 1477
Sequence Stars 3760 5748 9508
Sacremento Peak Observations (SPO) 467 310 777
Cerro Tololo Observations (CTIO) 217 9452 9669
University of Arizona Observations (UAO) 3965 166 4131
Stars taken from Literature 328 554 882
----------------------------------------------------------------
Representative Parameters of the Photometric Reductions:
The representative values for epsilon and mu are presented which are
the color-coefficients of the V and B-V reductions, as well as values
for the standard extinctions, k. The notation follows that of the
printed paper (cf. Hardie 1962, equations 24) except that k' and k''
are written as K1 and K2, respectively.
For epsilon and mu, the UAO values, being based on equipment very
similar to that used to define the UBV system, are quite close to zero
and one, respectively, while the CTIO and SPO values, being based on
S-20 photomultipliers and red-blocked filters, represent more
significant color terms.
For the CTIO observations through July 1983, the reductions used the
standard extinctions given in the Facilities Manual (Hesser, Walker,
and Munoz 1980). Thereafter, extinction values derived from pairs of
Landolt standards (high airmass versus low) were obtained for
individual nights or observing runs whenever this analysis was
reliably supported by the data; otherwise, standard extinctions
continued to be used. For the UAO observations, extinctions derived
from pairs of Landolt standards (at high and low airmasses) were
similarly obtained for individual nights or observing runs whenever
this analysis was reliably supported by the data; otherwise, standard
extinctions were used. Mean extinctions were used throughout for the
SPO observations.
While the GSPC errors due to the use of standard extinctions are
probably small (relative to the 0.05 mag GSPC specification), the
potential for improvement by more detailed determinations of
extinction on a nightly, short-term, or seasonal basis is evident,
especially for the early CTIO data (e.g., Rufener 1986); and we expect
to include this improvement in a future revision of the GSPC.
Hardie, R. H., 1962, in Astronomical Techniques, ed. W. A. Hiltner,
vol 2 of "Stars and Stellar Systems," eds. G. P. Kuiper and
B. M. Middlehurst (Chicago: Univ. of Chicago Press), p. 178.
Hesser, J. E., Walker, A. R., and Munoz, J. 1980, The CTIO Facilities
Manual, (La Serena: CTIO).
Rufener, F. 1986, E. S. O. Messenger, No. 44, p. 32.
Table 2: Representative parameters of the photometric reductions
----------------------------------------------------
Source Tel. epsilon mu k(v) k'(bv) k"(bv)
----------------------------------------------------
CTIO 0.9m -0.103 1.203 0.140 0.090 -0.025
CTIO 0.6m -0.097 1.209 0.140 0.090 -0.025
SPO 1.2m -0.118 1.122 0.250 0.100 -0.020
UAO 1.0m +0.035 1.008 0.250 0.060 -0.033
UAO 1.5m -0.009 1.101 0.250 0.060 -0.033
----------------------------------------------------
Where:
SOURCE Observatory and Telescope
epsilon B-V Coefficient of V transformation
mu B-V Coefficient of B-V transformation
k_V Extinction coefficient in V
k1_BV First order extinction coefficient in B-V
k2_BV Second order extinction coefficient in B-V
----------------------------------------------------
The transformation and extinction coefficients are defined
in Hardie 1962, in "Stars and Stellar Systems", Vol.2
'Astronomical Techniques', p. 178.
Suspect Stars:
For stars having three or more observations with one discrepant by
0.20 mag or more, we assume the discrepant observation to be an error
and delete it from the average used in the GSPC; to allow for the
possibility that this procedure may incorrectly treat a variable star
as an observational error, we record the names of the stars so
processed in this table. Stars whose utility as
standards are suspect because their routine use in GSC production has
caused problems are also entered in this table.
Table 3: List of Suspect Stars
----------------------------------------------
P099-I P139-E P175-A P272-F P274-A P327-F
P328-D P330-B P331-E P382-F P438-C P445-F
P461-A P503-G P504-G P506-E P524-F P559-E
S099-F S137-B S208-C S214-B S326-E S496-C
S507-D* S556-A S694-G S707-E S808-F S810-F
S817-C S840-E S856-H S859-H
----------------------------------------------
S507-D: Definitely observed at CTIO but not present on
the SRC-J plate(J2340, 1976 May 29) used in the GSC.
Its image appears normal on the Palomar survey.
Catalog Statistics by Star-Letter and Declination Zone:
The GSPC has been divided into six zones of equal size (30 degrees) in
declination to collect the statistics which are presented in this
table, namely the average photometric properties of the
stars, the number of multiple observations, and the consistency of the
multiple observations. The average V magnitudes given in the Table
indicate the success of the fly-spanker technique in identifying stars
of approximately the correct magnitude from the survey prints and
films used for planning the program; on the average (over declination
zone and magnitude), the <V> values agree to approximately 0.1 mag
with the nominal values. As anticipated from Table 1, one can see the
general decrease in N(AV), the average number of observations per
star, with increasing declinations. This effect is especially serious
in the +75 degree declination zone, where the usual practical
limitations to rapid observing were incurred.
The standard deviations, s(V) and s(B-V), are measures of the
repeatability of the multiple observations. At the brighter
magnitudes, the results, which are typically more precise than the
0.05 magnitude specification which was initially set as the GSPC goal,
indicate that for the most part the catalog meets its design goal.
However, for the fainter stars and especially for the northern
declinations, where often we did not have adequate time to acquire
sufficient photon statistics, the achieved precision falls short of
the specification by a factor of 1.5 to 2. While this does not affect
the performance of the GSC for which the GSPC was built, users with
other applications should be aware of this limitation; one may expect
that the matter is especially serious when extrapolating from the
faint end of a sequence.
The 6 regions - one for each 30 degree declination zone, are
centered as follows: -75, -45, -15, +15, +45, +75.
Table 4: Statistics by star letter and declination zone.
This table gives the average photometric properties of the stars,
the average number of observations per star, the number of multiple
observations, and the consistency of the multiple observations.
------------------------------------------------------------------
Decl. Star <V> <B-V> Ntot N(AV) N(mult) s(V) s(B-V)
------------------------------------------------------------------
-75 A 8.18 +0.69 118 2.36 107 0.03 0.02
B 9.45 +0.66 116 2.19 104 0.03 0.02
C 10.79 +0.77 117 2.15 104 0.03 0.03
D 11.99 +0.80 117 2.21 104 0.04 0.03
E 13.01 +0.77 116 1.95 93 0.03 0.04
F 14.00 +0.81 114 1.81 76 0.05 0.06
G 14.74 +0.84 67 1.55 30 0.06 0.09
------------------------------------------------------------------
-45 A 8.49 +0.65 284 2.29 229 0.03 0.02
B 9.75 +0.69 285 2.00 226 0.03 0.02
C 11.03 +0.78 282 2.06 231 0.04 0.03
D 12.12 +0.77 283 2.06 229 0.03 0.03
E 13.14 +0.85 285 1.96 218 0.04 0.05
F 14.09 +0.79 275 1.72 155 0.05 0.07
G 14.64 +0.83 152 1.60 62 0.06 0.10
------------------------------------------------------------------
-15 A 8.98 +0.66 381 2.06 232 0.03 0.02
B 10.23 +0.77 366 1.78 216 0.04 0.03
C 11.43 +0.80 368 1.76 214 0.03 0.03
D 12.41 +0.80 367 1.74 212 0.04 0.05
E 13.65 +0.80 362 1.77 197 0.05 0.06
F 14.17 +0.85 280 1.66 127 0.05 0.08
G 14.60 +0.87 181 1.69 81 0.07 0.10
------------------------------------------------------------------
+15 A 8.91 +0.76 275 1.60 113 0.03 0.02
B 10.30 +0.79 273 1.47 104 0.03 0.03
C 11.54 +0.76 276 1.48 105 0.04 0.03
D 12.54 +0.77 269 1.48 102 0.04 0.03
E 13.82 +0.79 263 1.49 99 0.07 0.07
F 14.43 +0.84 262 1.45 89 0.07 0.09
G 14.86 +0.86 130 1.35 36 0.11 0.13
------------------------------------------------------------------
+45 A 9.10 +0.65 201 1.40 67 0.04 0.03
B 10.26 +0.76 195 1.36 64 0.04 0.03
C 11.54 +0.73 196 1.34 62 0.04 0.03
D 12.50 +0.74 203 1.33 63 0.05 0.04
E 13.74 +0.77 202 1.33 63 0.07 0.07
F 14.58 +0.79 199 1.35 62 0.10 0.09
G 14.77 +0.79 98 1.22 18 0.11 0.07
------------------------------------------------------------------
+75 A 9.02 +0.68 89 1.10 9 0.04 0.02
B 10.37 +0.68 86 1.07 6 0.04 0.02
C 11.45 +0.79 87 1.06 5 0.03 0.02
D 12.50 +0.84 86 1.05 4 0.03 0.01
E 13.88 +0.80 86 1.06 5 0.03 0.05
F 14.52 +0.87 86 1.06 5 0.02 0.07
G 14.47 +0.92 30 1.00 0 --- ---
------------------------------------------------------------------
Observation Statistics by Data Sources:
Comparisons made between the various possible pairs of data sources
are summarized in this table, which contains, for each
star-letter and observatory-pair, N, the number of multiple
observations, D(V) and D(B-V), the average differences
between (distinct) sites, and s(V) and s(B-V), the standard
deviations of the multiply-observed photometric values.
The practical development of the GSPC was such that the observations
are most extensive in the southern hemisphere, where 78 observations
of stars in the Graham E regions were made to test the external
accuracy of the GSPC. These observations, differenced against Graham's
standard values, are addressed in Section VI of the GSPC text, from
which one may conclude that our southern observations are an
acceptable representation of the BV system. In the northern
hemisphere, where practical limitations to the program prevented us
from getting a similar quantity of consistent test data, we
nevertheless did obtain 25 observations of standards adopted from our
literature sequences (P-T from P216; P-Y from P309; Q, R, and T from
P333; Q and S from S802; and P from P080, P093, P187, P188, and P331;
c.f. references in Table 6). From the differences of these against the
literature-values one may again conclude that our observations are an
acceptable representation of the BV system.
This argument is supported by the observatory-observatory comparisons
given in Table 5, from which one may verify that there are
no systematic trends as a function of magnitude. Note that, as no
reobservations of literature sequences are available for SPO, the
verification that the SPO data are also an acceptable representation
of the BV system is provided by the UAO-SPO and CTIO-SPO data given
here.
Table 5: Observation Statistics by data sources
For each star-letter and observatory-pair, this table lists
the number of multiple observations (N), the average
differences between (distinct) sites, and the standard
deviations of the multiply-observed photometric values.
----------------------------------------------------
Obs. Pair Star N D(V) D(B-V) s(V) s(B-V)
----------------------------------------------------
CTIO-CTIO A 1567 --- --- 0.03 0.02
B 883 --- --- 0.03 0.02
C 868 --- --- 0.04 0.03
D 885 --- --- 0.04 0.04
E 840 --- --- 0.04 0.05
F 599 --- --- 0.05 0.08
G 328 --- --- 0.06 0.10
----------------------------------------------------
UAO-UAO A 186 --- --- 0.03 0.03
B 135 --- --- 0.04 0.04
C 130 --- --- 0.05 0.03
D 132 --- --- 0.05 0.04
E 130 --- --- 0.07 0.08
F 131 --- --- 0.09 0.09
G 30 --- --- 0.10 0.08
----------------------------------------------------
SPO-SPO A 44 --- --- 0.02 0.01
B 42 --- --- 0.04 0.04
C 46 --- --- 0.04 0.02
D 35 --- --- 0.04 0.06
E 38 --- --- 0.05 0.05
F 37 --- --- 0.07 0.09
G 30 --- --- 0.12 0.12
----------------------------------------------------
CTIO-UAO A 64 -0.01 0.00 0.04 0.03
B 57 0.00 0.00 0.03 0.02
C 59 0.00 0.00 0.03 0.02
D 61 0.00 0.00 0.03 0.03
E 56 0.00 0.01 0.06 0.06
F 41 0.02 0.00 0.07 0.07
G 0 --- --- --- ---
----------------------------------------------------
CTIO-SPO A 16 0.01 0.01 0.02 0.02
B 16 0.03 0.01 0.05 0.02
C 13 -0.01 0.00 0.02 0.02
D 18 0.02 -0.03 0.03 0.08
E 16 0.00 -0.05 0.05 0.07
F 17 0.01 -0.01 0.03 0.07
G 8 0.03 0.00 0.06 0.09
----------------------------------------------------
UAO-SPO A 40 0.02 0.00 0.04 0.01
B 23 0.01 0.01 0.04 0.02
C 24 0.01 0.00 0.04 0.02
D 19 0.01 0.00 0.04 0.03
E 26 0.05 0.01 0.08 0.04
F 24 0.03 0.01 0.10 0.09
G 14 0.02 0.04 0.15 0.14
----------------------------------------------------
CTIO-Lit P 21 0.00 0.01 0.02 0.02
Q 13 -0.01 -0.02 0.02 0.02
R 4 -0.03 0.00 0.03 0.02
S 0 --- --- --- ---
T 0 --- --- --- ---
U 0 --- --- --- ---
----------------------------------------------------
UAO-Lit P 9 0.01 0.00 0.02 0.02
Q 3 -0.01 -0.01 0.04 0.02
R 3 0.01 -0.01 0.02 0.01
S 3 -0.01 -0.01 0.02 0.02
T 3 0.00 0.01 0.03 0.01
U 1 0.01 -0.01 0.01 0.01
----------------------------------------------------
SPO-Lit P 0 --- --- --- ---
Q 0 --- --- --- ---
R 0 --- --- --- ---
S 0 --- --- --- ---
T 0 --- --- --- ---
U 0 --- --- --- ---
----------------------------------------------------
The GSPC Catalog:
Please note that the catalog has been updated by the ADC with help
from the authors. Sequences P040, P421, S335, and S742 have been
replaced. The new catalog version number is still 1 since the authors
are working on version 2. Only the main catalog data file has been
updated. The errors in V and B-V were replaced with those in the
database maintained by the authors.
The organization of the GSPC is such that northern fields, listed by
increasing field number come first and are followed by the southern
fields, again listed by increasing field numbers; i.e., the catalog is
structured first by hemisphere and second by decreasing declination.
Some comments on specific fields of the catalog (Table 7 in the
publication) follow:
The field and star identifications are written in the form Hnnn-S,
where H takes on the values P or S, indicating Palomar or SRC centers,
nnn is a three digit field identification (with the range 1 through
583 for Palomar and 1 through 894 for SRC), and S is a letter
identifying an individual star.
A full discussion of the error indicators (ErrorInd), which are used
to indicate slightly blended literature stars and data for which no
formal error estimates are available, may be found in the GSPC text.
In sequences P040, P421, S335, and S742 the error indicator has
been replaced by an indicator flagging the update of the record for
GSPC Version 2.
For certain fields at zero hours right ascension, the survey-plate
overlap is sufficiently large that two fields may be calibrated by one
sequence; accordingly, the following pairs have "shared sequences"
which are flagged in the LIT field of the catalog and identified in
the LIT_REF field: P028 and P049, P149 and P191, P240 and P291, and
P348 and P403.
The coding of the literature citations (RefLit) used in this FILE
(GSPC Table 7) depend on the reference catalog from which we found the
data, as follows:
The Nicolet Catalog: citations are of the form Nn.k, where n
identifies a specific category in the Nicolet catalog and k is a
ten-digit context dependent string explained fully in Nicolet(1978)
and Mermilliod (1978); generally the first part of k identifies a
sequence and the second part identifies a specific star.
The catalogs by Argue and his colleagues and by Sharov and Yakimova:
citations are of the form Xn.k, where X takes the values A or S,
respectively, n identifies the specific catalog reference number and
k identifies a star within the sequence.
The Graham publications: citations are of the form Gn.k, where n is a
four character string identifying the Harvard E region and k is a four
character string identifying the star.
The Landolt publications: citations are of the form L7.nk, where n and
k are strings as above. Note that the Landolt citations in which k
contains no letters are generally valid Nicolet references. However,
for six sequences (S826, S853, S861, S870, S879, and S888) additional
photometry of stars fainter than V=13 was done after the publication
of the Nicolet catalog; Landolt (private communication) has furnished
citations for these stars, either as identifications from the original
Harvard publications or as his own letter designations, which we have
coded in the style of Nicolet (1978).
Mermilliod, J.-C. 1978, C. D. S. Info. Bull., 14, 32.
Nicolet, B. 1978, Astr. Ap. Suppl. 34, 1.
Byte-by-byte Description of file: catalog.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- Star Star identification (1)
9- 13 F5.2 mag Vmag V Magnitude
15- 19 F5.2 mag B-V B-V Color
22- 23 I2 h RAh 1950.0 Right Ascension - Hours
25- 26 I2 min RAm 1950.0 Right Ascension - Minutes
28- 31 F4.1 s RAs 1950.0 Right Ascension - Seconds
33 A1 --- DE- 1950.0 Declination - Sign
34- 35 I2 deg DEd 1950.0 Declination - Degrees
37- 38 I2 arcmin DEm 1950.0 Declination - Minutes
40- 41 I2 arcsec DEs 1950.0 Declination - Seconds
42 A1 --- u_DEs Uncertainty flag (:) on RA and DE (4)
45- 48 F4.2 mag e_Vmag *[0/]?=9.99 (sigma) Error in V Magnitude
50- 53 F4.2 mag e_B-V *[0/]?=9.99 (sigma) Error in B-V Color
54 A1 --- ErrorInd [*bu] Error/update indicator (2)
57 I1 --- o_Vmag ? Total Number of Observations
60 A1 --- CTIO [C] CTIO Observation Indicator
61 I1 --- o_CTIO ? Number of CTIO Observations
63 A1 --- SPO [S] SPO (Sacremento) Observation Indicator
64 I1 --- o_SPO ? Number of SPO Observations
66 A1 --- UAO [A] UAO (Arizona) Observation Indicator
67 I1 --- o_UAO ? Number of UAO Observations
69 A1 --- Lit [LM] Literature or Multiple Sequence (3)
70- 80 A11 --- RefLit Literature Reference
--------------------------------------------------------------------------------
Note (1): the Star is made of the Plate name, a slash, and an
alphabetic sequence number.
Note (2): the symbols have the following meaning:
b = star with faint blend (lit.)
* = no photometric statistics
: = questionable value
u = update from version 1
Note (3): this flag means the following:
L = sequence found in the literature
M = Multiply used sequence (shared)
Note (4): Coordinate Precision indicator
: - colon means approximate coordinates
- blank means accurate coordinates
Note on e_Vmag, e_B-V: errors in V and B-V
During error corrections and verification we discovered that these
values on the ADC CD-ROM Vol. 1 version were incorrect. They have
been updated with the values obtained from the authors' original
data base.
Bibliography of Literature Sequences:
Data not from UAO, SPO, or CTIO are taken from the literature. The
original sources of this data may be located directly from the
references in Table 6) which lists, for each literature-sequence,
the sequence name, the collection from which the sequence was
obtained, and a citation for the original data-source.
The collections of sequences are identified by the prefixes G, L, A,
S, and N, which respectively signify the publications by Graham
(1982), or by Landolt (1973, 1983), or the compilations by Argue and
his colleagues (Argue and Bok 1973a,b; Argue and Miller 1976; Argue,
Miller, and Warren 1983), by Sharov and Yakimova (1970), or by Nicolet
(1978). For example, S439 indicates reference 439 from Sharov and
Yakimova. The references for these collections are as follows:
Argue, A. N., and Bok, B. J. 1973a, A Catalog of Photometric
Sequences, (Tucson: Steward Observatory).
----- 1973b, A Catalog of Photometric Sequences, Supplement No. 1,
(Tucson: Steward Observatory).
Argue, A. N., and Miller, E. W. 1976, A Catalog of Photometric
Sequences, Supplement No. 2, (Cambridge: Cambridge University).
Argue, A. N., Miller, E. W., and Warren, W. H. 1983, A Catalog of
Photometric Sequences, Supplement No. 3, (Rexburg, Idaho: Ricks
College Press).
Graham, J. A. 1982, Publ. A.S.P., 94, 244.
Landolt, A. U. 1973, A. J., 78, 959.
----- 1983, A. J., 88, 439.
Nicolet, B. 1978, Astr. Ap., 34, 1.
Sharov, A. S., and Yakimova, N. N. 1970, Photometric Catalogs and
Standards, Trudy Sternberg Instit., 40, 106.
Journal references too long to fit into the allocated field of one
record are continued into the following records, with the first three
fields being blank and the fourth completing the reference. Note also
that the references in the FITS version of Table 6 have been prepared
without any attempt to code non-English characters; the reader is
referred to the printed table for the precise citations.
Byte-by-byte Description of file: refs.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- Plate Plate designation
8- 21 A14 --- Field Field designation
24- 29 A6 --- CatRef Catalog Reference
31-120 A90 --- LitRef Literature Reference
--------------------------------------------------------------------------------
Notes:
The GSPC Version 1 was published on the ADC CD-ROM Volume 1. In 1996
corrections were made to sequences P040, P421, S335, and S742. These
corrected sequences replace the sequences in GSPC Version 1.
Dr. Sturch provided the ADC with the revised sequences.
Acknowledgements:
The data for THE GUIDE STAR PHOTOMETRIC CATALOG were prepared
by Barry M. Lasker and Conrad R. Sturch, principal investigators; and
Carlos Lopez, Anthony D. Mallama, Steven F. McLaughlin, Jane L.
Russell, Wieslaw Z. Wisniewski, and Bruce A. Gillespie, principal
contributors to observing or data reduction; and Helmut Jenkner,
Elizabeth D. Siciliano, and Deborah Kenny, principal contributors to
preparation of the publication; and Alan M. Goldberg, Gregory W.
Henry, Edward Kemper, and Michael J. Siegel.
The documentation was standardized with contributions from Nancy Roman,
Francois Ochsenbein, Gail Schneider, Paul Kuin and the original
documentation in the ADC CD-ROM FITS files. We acknowledge the error
report by Mati Morel on S335. Conrad Sturch provided us with all the
corrections and updates.
================================================================================
(End) Paul Kuin (NASA/ADC) 21-Aug-1996