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The NLTT Catalogue and First Supplement
(Luyten 1979, 1980)
(Luyten and Hughes 1980)
Documentation for the Computer-Readable Version
Wayne H. Warren Jr.
National Space Science Data Center
Conrad R. Sturch
Computer Sciences Corporation
Space Telescope Science Institute
Barry M. Lasker
Space Telescope Science Institute
September 1988
Doc. No. NSSDCA/WDC-A-R&S 88-20
National Space Science Data Center (NSSDC)/
World Data Center A for Rockets and Satellites (WDC-A-R&S)
National Aeronautics and Space Administration
Goddard Space Flight Center
Greenbelt, MD 20771
Abstract
The machine-readable version of the catalog, prepared initially by reading
the published version with optical character recognition equipment and
transferring the data to a computer, is described. The First Supplement, as
computerized at the Astronomisches Rechen-Institut in Heidelberg, was
reformatted and merged into the main catalog to prepare a comprehensive and
uniform data file ordered by right ascension. The remarks, included with the
data in the published catalog, have been separated and placed into a second
file. Additional supplements will similarly be merged into the existing data
file if they become available.
Contents
1 Introduction 2
1.1 Description ................................................. 2
1.2 Source References ............................................. 2
2 Structure 3
2.1 File Summary ................................................. 3
2.2 Catalog (File 1 of 2) ........................................ 3
2.3 Notes (File 2 of 2) ......................................... 7
3 History 7
3.1 Remarks and Modifications ................................... 7
3.2 Acknowledgments ............................................... 12
3.3 References ................................................... 12
A Deletions and Addenda 13
List of Tables
1 Summary Description of Catalog Files ......................... 3
2 Data File Record Format ..................................... 5
3 Notes File Record Format ..................................... 7
4 Stars Deleted from the NLTT Catalogue ........................ 14
5 NLTT Addenda Stars ........................................... 15
1
1 Introduction
1.1 Description
The NLTT Catalogue (Luyten 1979, 1980) is a collection of stars on more than
800 Palomar Proper Motion Survey plates found to have relative annual proper
motions exceeding 0.18 arcsec. The motions have been determined by Luyten and
his coworkers by either hand blinking and measuring or with the automated-
computerized scanner and measuring machine built by Control Data Corporation
and located at the University of Minnesota. The new catalog replaces the LTT
Catalogues (Luyten 1957, 1961, 1962), wherein stars in the Bruce Proper Motion
Survey discovered to have motions exceeding 0.2 arcsec had been compiled. For
further information on the NLTT Catalogue itself, including discussions of
positional errors, estimation of magnitudes, star designations used in the
catalog, completeness, and accuracy of the measured motions, the introduction
to the published NLTT (see Volume I) should be consulted.
The First Supplement to the NLTT Catalogue (Luyten and Hughes 1980) is the
result of continued plate analysis and measurements during printing of the
NLTT. The Supplement contains data for 398 stars having motions larger than
0.179 arcsec annually.
A detailed discussion of the computerization of the catalog can be found in
Section 3 of this document. The document describes the machine-readable version
of the NLTT Catalogue and First Supplement as it is currently being distributed
from the Astronomical Data Center (ADC). It is only intended to facilitate the
processing and use of the data in the machine version. As mentioned above,
users should consult the source publication for additional details. A copy of
this document should be transmitted to any recipient of the machine-readable
catalog.
1.2 Source References
Luyten, W. J. 1979, 1980, New Luyten Catalogue of Stars with Proper Motions
Larger than Two Tenths of an Arcsecond (Minneapolis: University of
Minnesota).
Luyten, W. J. and Hughes, H. S. 1980, Proper Motion Survey with the
Forty-Eight Inch Schmidt Telescope. LV. First Supplement to the
NLTT Catalogue (Minneapolis: University of Minnesota).
2
2 Structure
2.1 File Summary
The machine version of the NLTT Catalogue and First Supplement consists of
two files. Table 1 gives the machine-independent file attributes. All logical
records are of fixed length, and, if the catalog is received on magnetic tape,
it will contain blocks of fixed length (as noted below) except that the last
block may be short. The first file contains the basic data of the catalog,
while the second contains the notes for particular stars, as flagged in the
individual records of the first file.
________________________________________________
| NLTT Catalogue and First Supplement |
|________________________________________________|
| | | Record | Record | Number of |
| File | Contents | Format | Length | Records |
|_______|__________|________|________|___________|
| 1 | Data | Fixed | 65 | 58845 |
| 2 | Notes | Fixed | 90 | 5843 |
|_______|__________|________|________|___________|
Table 1: Summary Description of Catalog Files
The information contained in the above table is sufficient for a user to
describe the indigenous characteristics of the machine-readable version of the
NLTT Catalogue and First Supplement to a computer. Information easily varied
from installation to installation, such as block size (physical record length),
blocking factor (number of logical records per physical record), total number
of blocks, density, number of tracks and character coding (ASCII, EBCDIC) for
tapes, is not included, but should always accompany secondary copies if any are
supplied to other users or installations.
2.2 Catalog (File 1 of 2)
This file contains the basic data of the catalog, which are the positions,
magnitudes, spectral or color classes, and proper motions of the cataloged
stars. The remarks flagged by asterisks in the star-identification field are
contained in the notes file described in Section 2.3.
Table 2 gives a byte-by-byte description of the contents of the data file. A
suggested Fortran format specification for reading each data field is included
and can be modified depending upon individual programming and processing
requirements (Fortran 77 character string-type formats are used); however,
caution is advised when substituting format specifications, since many data
3
fields contain character data and others are blank when data are absent.
Default (null) values are always blanks in data fields for which primary
suggested formats are given as A.
Star identification Star designation in one of a variety of other catalogs.
Identifiers from the Bonner and Cordoba Durchmusterungen
are used when they exist. Other miscellaneous
identifiers (Oxf = Oxford Astrographic Catalogue [AC];
Grw = Greenwich AC; U = Upgren; R = Ross, etc.) are
used for non-DM stars. Identifiers without prefixes are
DM or Luyten numbers from the Bruce Proper Motion
Survey (L numbers) or the Luyten-Palomar Survey (LP
numbers), the former in zones -45 to -89 deg and the
latter in zones +89 to -44 deg. Alternate identifiers
are sometimes given in the notes. An asterisk (*) in
the identification field indicates that a note will be
found in the "notes" file of the catalog. The mis-
cellaneous designations can be found in Fernandez et
al. (1983) and Lortet and Spite (1986).
Equatorial coordinates Positions are for equinox 1950 at epoch, with the
precision varying (bytes 21-22 and 38 sometimes
blank).
Right ascension flag Due to the varying precision of the reported positions
in the published catalog (right ascensions in the polar
caps [+90 to +80 deg; -45 to -90 deg] are reported to
minutes and tenths only, while other zones are given to
seconds of time) it was necessary to reformat the R.A.
data to make them uniform. Therefore, the right
ascensions were computed in both seconds of time and
minutes plus tenths for all stars. The flag denotes the
original format:
1 Original R.A. reported in minutes and tenths
of time
2 Original R.A. reported in seconds of time
4
___________________________________________________________________________
| | | Suggested | Default | |
| Bytes | Units | Format | Value | Data |
|_______|___________|___________|_________|_________________________________|
| 1-14 | --- | A14 | --- | Star identification |
| 15-16 | hours | I2 | --- | Right ascension |
| 17 | --- | 1X | --- | Blank |
| 18-19 | min | I2 | --- | R.A. |
| 20 | --- | 1X | --- | Blank |
| 21-22 | sec | I2 | blank | R.A. |
| 23 | --- | 1X | --- | Blank |
| 24-27 | min | F4.1 | --- | R.A. |
| 28 | --- | 1X | --- | Blank |
| 29 | --- | I1 | --- | Right ascension precision flag |
| 30 | --- | 1X | --- | Blank |
| 31 | --- | A1 | --- | Sign of declination |
| 32-33 | deg | I2 | --- | Dec. |
| 34 | --- | 1X | --- | Blank |
| 35-38 | arcmin | F4.1 | --- | Dec. |
| 39 | --- | 1X | --- | Blank |
| 40-43 | mag | F4.1 | blank | Red magnitude |
| 44 | --- | A1 | --- | Red magnitude flag |
| 45-48 | mag | F4.1 | blank | Photographic magnitude |
| 49 | --- | A1 | --- | Photographic magnitude flag |
| 50-52 | --- | A3 | --- | Spectral class or type |
| 53 | --- | 1X | --- | Blank |
| 54-58 | arcsec/yr | F5.3 | --- | Relative proper motion (annual) |
| 59 | --- | A1 | --- | Relative proper-motion |
| | | | | uncertainty flag |
| 60-62 | deg | I3 | --- | Position angle of proper motion |
| 63 | --- | A1 | --- | Position-angle uncertainty flag |
| 64 | --- | A1 | --- | Addenda flag |
| 65 | --- | A1 | --- | Supplement flag |
|_______|___________|___________|_________|_________________________________|
Table 2: Data File Record Format
5
Magnitudes Red and photographic magnitudes were estimated by
Luyten for stars fainter than 10m pg, but some
magnitude data fields are blank. Magnitudes for
brighter stars were evidently taken from the source
catalogs whose identifiers are given, or from a variety
of sources.
Magnitude flags A "+" indicates a magnitude fainter than the reported
value.
Spectral types Lower case letters represent estimated color classes or
ranges, while spectral types are reported where known.
All data are left justified in the field, not centered
as in the printed version.
Relative proper motion Total proper motion is reported. The proper-motion
vector is defined by the equation:
2 2 2 1/2
Mu = ( Mu_a cos(delta) + Mu_d )
where Mu_a and Mu_d are the right ascension and
declination components of the proper motion,
respectively, and delta is declination.
Proper-motion flag A colon (:) indicates uncertainty in the proper motion.
Position angle The direction of the proper-motion vector, as measured
in the usual way (north through east). The position
angle is defined by the following set of equations:
Mu_a = Mu sin(theta) ; Mu_d = Mu cos(theta)
where Mu_a is the right ascension component of the
proper motion, Mu_d is the declination component of the
proper motion, and theta is the position angle.
Position-angle flag A colon (:) indicates uncertainty.
Addenda flag The letter "A" indicates that data have been changed
for the machine-readable version, and the record does
not entirely match that of the published catalog. In
some cases, the star is entirely new and does not
appear in the published catalog. Deleted stars are
listed in a separate table in Appendix A of this
document - they have been removed from the machine
version entirely.
6
Supplement star flag A "1" denotes a star from the First Supplement (Luyten
and Hughes 1980). The supplement stars have been merged
into the main catalog entirely.
2.3 Notes (File 2 of 2)
This file contains the notes for stars flagged by an asterisk in the
identification field of the data file.
_____________________________________________________________
| | | Suggested | Default | |
| Bytes | Units | Format | Value | Data |
|________|________|___________|_________|_____________________|
| 1-16 | --- | A16 | --- | Star identification |
| 17 | --- | 1X | --- | Blank |
| 18-19 | hours | I2 | --- | Right ascension |
| 20 | --- | 1X | --- | Blank |
| 21-22 | min | I2 | --- | R.A. |
| 23 | --- | 1X | --- | Blank |
| 24-25 | sec | I2 | --- | R.A. |
| 26 | --- | 1X | --- | Blank |
| 27 | --- | A1 | --- | Sign of declination |
| 28-29 | deg | I2 | --- | Dec. |
| 30 | --- | 1X | --- | Blank |
| 31-34 | arcmin | F4.1 | --- | Dec. |
| 35 | --- | 1X | --- | Blank |
| 36-90 | --- | A55 | --- | Note(s) |
|________|________|___________|_________|_____________________|
Table 3: Notes File Record Format
Notes Notes in free text (upper and lower case) form. All notes are
contained in single records, i.e., no notes for one star extend to
additional records.
3 History
3.1 Remarks and Modifications
The desirability for a machine version of the NLTT was evident immediately
upon publication of the catalogs and, although the Palomar Proper Motion Survey
data for stars of large proper motions reside on magnetic tape in
7
Minneapolis, the tapes have not yet been processed to prepare a usable machine
version. A possible format for the NLTT was designed at the ADC in 1980 shortly
after the receipt of the final volume of the published catalog, and several
pages of volume I were keyed into a computer; however, the project was put
aside because of the great effort that it would have involved to key and check
the data manually. When interest in a machine version was expressed by Space
Telescope Science Institute personnel for use with the Guide Star Selection
System for the Hubble Space Telescope, an automatic method of computerizing the
catalog was contemplated and the present collaboration was formed. In 1981
March, we had received information on the Kurzweil Data Entry Machine (KDEM, an
optical scanning device) from Intermedia Digital Conversion, Inc. (IDC) in
Kensington, Maryland. A visit to the IDC was arranged and sample pages were
taken for a demonstration run. The results indicated that the machine would
perform satisfactorily as long as high quality source material were used,
although there were indications that some data records might be shifted because
of varying start positions in the left margin where the star identification
field begins each entry. However, we were informed that it might be possible to
avoid this problem if the machine could be set up and operated properly.
Because of the cost involved for processing of the entire catalog, we decided
to investigate other possibilities before making a final decision. A visit to
The Johns Hopkins University Applied Physics Laboratory was arranged to examine
an optical character recognition (OCR) machine located there, but this machine
turned out not to have the capabilities required. (It is restricted to text
prepared with a special font and, therefore, could be eliminated from
contention immediately.)
Professor Luyten kindly supplied us with an extra copy of the entire NLTT,
which was burst and set up for the job, and a contract was let to the IDC to
proceed with the work. A question arose about how to process the Greek letters
and double characters (e.g., 0.10 arcsec) included in the catalog, since they
could not be translated directly into established hexidecimal character codes.
The Kurzweil machine, however, has specific input capability for hexidecimal
codes to represent individual characters, and these can be inserted manually
when the machine stops at unrecognizable characters. Therefore, a table was
provided so that the Greek letters could be inserted manually, as represented
by extended EBCDIC codes now used to print on an extended chain printer. The
double (overstrike) characters were processed so that they merely followed one
another (e.g., 0".10), since this situation could be corrected globally via a
machine editor. (The hexidecimal-code insertion technique failed because the
codes turned out to be unrecognizable to the computer, but no attempt was
made to correct this situation after it was decided that three-letter
abbreviations should be substituted for the letters anyway.)
Careful checking and sample proofreading of the final catalog showed that
many problems were present:
1. Despite the indicated operational precautions, a significant number of
records had been shifted left or right to produce misalignment. This not
only occurred at the beginnings of records, but began at various points
in the records as well; i.e., the shifting seemed to be random and
occurrence was unpredictable.
8
2. Certain characters were frequently misread (not a significant percent-
age of the total, but enough to require that review and correction
procedures be undertaken). Fortunately, most of these involved the
substitution of "S" for "8" and "5", "I" or "L" for "1", and "K" for "k",
etc., occurrences that could be identified as out of context via general
editor search procedures.
3. A large number of commas had been substituted for decimal points, but
these also could be systematically identified as out of place.
4. The machine determined the left margin anew for each page; thus, if an
unusual identifier occurred as the first record on a page, groups of
records on that page were misaligned.
Attempts were made to write computer programs to find record shifts and
correct them automatically, first with a Fortran program, then with assembly
language code, but the shifts were so random and sometimes multiple within a
record that a universal algorithm could not be developed easily. Since other
types of errors also occurred, it was decided to use an editor to simply review
terminal screens full of records and fix them in a sequential fashion. This
initial editing was done at the ST ScI. No changes were made to the comments
fields at that time, however, because the comments were not required for use at
ST ScI. In fact, a second version was created there, in which the remarks
fields were removed. This short version was then refined by the detection and
correction of letters in numerical data fields, etc. The original and refined
versions were then processed through a special program that compared records
and indicated disagreements. This was not a simple compare program because
missing records had been detected and added at various places and because some
shifted fields had still not been detected and corrected in the full version.
The program was written and run at the ST ScI and the output sent to the ADC
for review and analysis.
The analysis was performed not only for the detection of individual errors
in the original version, but to formulate general rules for the systematic
global correction of cetain types of errors so that each would not require
specific editing. In fact, almost all errors occurred in a systematic fashion
and could be corrected by a set of predesigned global editing commands.
Since the KDEM read the data exactly as published, the hours of right
ascension were missing on all but the first entry of each page. A computer
program was written to add these data. The program also checked for the
agreement of asterisks in the star identification field for stars having
remarks and vice versa. This was done in preparation for separating the remarks
to make a second file for notes only. Disagreements in both directions were
found and corrected. The remarks themselves were then reviewed and made uniform
with regard to alignment, abbreviations for Greek letters, missing
punctuation, etc. This was a multistep process, with large numbers of changes
being made before printing, review, and final editing.
9
The First Supplement had been keypuched at the Astronomisches Rechen-
Institut in Heidelberg, and was kindly supplied on magnetic tape by H.
Jahreiss. The format was different, of course, and the remarks had not been
included. Therefore, another program was written to reformat the Supplement
data and the corresponding notes were edited in manually. A flag "1" to denote
"Supplement 1" was added to all Supplement records so that they can be
distinguished in the merged catalog.
During the course of the work, many errors were found in the original data.
Most of these had occurred as a result of misprints and were resolvable by
reference to context or to the LTT. Following the merging of the main catalog
and the Supplement, and sorting by right ascension (which was approved by
Professor Luyten), the remarks were stripped from the data and placed into a
separate data set. To simplify the location of particular remarks, the right
ascension and declination of each star are duplicated in the remarks file.
Since only one tenth of the stars in the catalog have notes, a considerable
amount of storage was saved by creating a separate file.
Another problem with the coordinates had to be solved to produce a uniformly
formatted data file. This difficulty occurred because of the varying
precision reported for stars in the polar and equatorial regions of the
published catalog. It would have been unacceptable to convert the lower
precision coordinates of the polar regions to equatorial format, and one
certainly wouldn't want to convert the seconds of time to fractions of a
minute for the equatorial stars. Yet, it is not at all desirable to have two
different forms for the coordinates within the catalog. Therefore, the right
ascensions are reported in both forms for the entire catalog. This was
accomplished by adding a data field to the machine version and computing the
alternate form. A flag was added to each record to indicate which form is used
in the original published catalog, since this is the accuracy that should be
adhered to when using the data.
Following the completion of the merged data file, the catalog was processed
through the ADC's General Validation Program to check for miscellaneous
problems. This program checks ordering and ranges for all specified values. Not
surprisingly, many additional letters were found in numerical fields, even
though careful checks were thought to have been made. Additional unresolvable
errors were found in position angles and positional data that fell outside the
allowable ranges. These problems were submitted to Professor Luyten, who kindly
returned to the original card file to resolve them. All entries of this nature,
including published addenda incorporated into the machine version, are flagged
by the letter "A" in each affected record. This is the case whenever a record
in the machine version does not agree with its corresponding entry in the
published catalog. All such records are listed in Appendix A so that a user can
either resolve a discrepancy or identify as an error any true disagreement
between the present machine version and the published catalog.
Additional possible and probable errors published by E. W. Weis (1987) where
checked and corrected where appropriate. Changes were made as a result of Notes
6, 8, 15-18, 24-25, 28, 39, and 46, while 7, 13, and 38 had been detected and
corrected independently; no action was taken for 10, 29, 31, and 33.
Although most of the hundreds of changes made to the published catalog
involved only the correction of certain data, some stars have actually been
removed from the catalog. These deletions were primarily the result of
10
duplicate entries and included stars that have later been found to display "no
motion" (defined as motion smaller than the lower cutoff for the catalog). The
deleted stars are listed in Appendix A so that users can determine immediately
if a star found to be missing in the machine version has been intentionally
removed.
3.2 Acknowledgments
The computerization of the NLTT Catalogue was a collaborative effort between
the Space Telescope Science Institute (ST ScI) and the Astronomical Data Center
of the National Space Science Data Center, with funding for the optical
scanning being provided by the former organization. The assistance of
Elizabeth D. Siciliano with programming and editing, Victoria G. Laidler and
Deborah Kenny with editing, and Karen Myers (all Computer Sciences Corp., ST
ScI) with proofreading selected pages, of Steven F. McLaughlin (Computer
Sciences Corp., ST ScI) with programming and comparison checks on partial
data computerized at the Astronomisches Rechen-Institut (ARI) in Heidelberg,
and of Joanne A. Sheridan (formerly of the ADC/NSSDC) with programming, is
appreciated.
We also gratefully acknowledge the help of Dr. Hartmut Jahreiss of the ARI
in providing machine-readable data from Volumes I and II of the NLTT and all of
the First Supplement keypunched in Heidelberg. Dr. Jahreiss also found and sent
several short lists of errors detected during the course of his own work with
the catalog.
The help of Professor Willem J. Luyten, who confirmed many of the errors
detected by returning to the original data and who cheerfully responded to
our many inquiries, was invaluable in preparing the corrected machine version.
We hope that the collaborative effort of these many persons has produced a
permanently useful addition to the long list of important machine-readable
astronomical catalogs.
3.3 References
Fernandez, A., Lortet, M.-C., and Spite, F. 1983, The First Dictionary of the
Nomenclature of Celestial Objects, Astron. Astrophys. Suppl. 52, No. 4.
Lortet, M.-C. and Spite, F. 1986, First Supplement to The First Dictionary of
the Nomenclature of Celestial Objects, Astron. Astrophys. Suppl. 64, 329.
Luyten, W. J. 1957, A Catalogue of 9867 Stars in the Southern Hemisphere with
Proper Motions Exceeding 0.2 arcsec Annually (LTT) (Minneapolis: The
Lund Press).
Luyten, W. J. 1961, A Catalogue of 7127 Stars in the Northern Hemisphere with
with Proper Motions Exceeding 0.2 arcsec Annually (LTT) (Minneapolis:
The Lund Press).
11
Luyten, W. J. 1962, First Supplement to the LTT Catalogue (Minneapolis: The
Observatory, University of Minnesota).
Luyten, W. J. 1979, 1980, New Luyten Catalogue of Stars with Proper Motions
Larger than Two Tenths of an Arcsecond (Minneapolis: University
of Minnesota).
Luyten, W. J. and Hughes, H. S. 1980, Proper Motion Survey with the
Forty-Eight Inch Schmidt Telescope. LV. First Supplement to the
NLTT Catalogue (Minneapolis: University of Minnesota).
Weis, E. W. 1987, Astron. J. 92, 451.
A Deletions and Addenda
Table 4 lists the stars (or entries) that have been removed from the machine
version of the NLTT catalog. Many of these deletions were circulated in a list
entitled "Errata to the NLTT Catalogue", distributed by Professor Luyten;
additional deletions were received from him via private communication,
forwarded to us by Dr. H. Jahreiss of the ARI, or discovered at the ADC during
the course of this work. The latter occurrences were in all cases confirmed by
Professor Luyten before they were removed. Where specific reasons are known for
the deletions, they are given in the table.
Table 5 lists all stars whose data differ in the machine and published
versions. These are all flagged with the letter "A" in byte 64 of the data file
records. The table has been printed separately and inserted into this document;
thus, it begins on the following page.
______________________________________________________________________
| Star | RA 1950 | Dec 1950 | Remarks |
|___________|__________|__________|____________________________________|
| | 1 10 48 | -01 59.5 | |
| 467- 86 | 1 12 40 | +14 20.9 | |
| 408- 1 | 1 29 08 | +20 33.5 | Duplicate entry |
| -69: 88 | 2 05 42 | -69 06. | No motion |
| | 2 56 44 | +48 49.2 | Duplicate entry |
| +34: 724 | 3 41 12 | +34 48.8 | Duplicate incorrect entry |
| 155-291 | 3 42 22 | +49 30.5 | |
| -60:1088 | 4 06 24 | -59 52. | No motion (10 observations) |
| 161- 75 | 6 52 39 | +47 03.5 | |
| | 10 44 58 | +34 59.2 | Duplicate entry |
| 794- 82 | 11 53 46 | -19 22.1 | |
| U38-101 | 12 23 12 | +38 02.0 | Same as LP266-50 at 12 22 55 |
| 320-583 | 12 25 45 | +31 28.0 | |
| U43-151 | 12 40 06 | +43 19.0 | Correct entry at 12 39 25 +43 19.1 |
| -63:1233 | 16 47 12 | -64 03. | No motion (6 observations) |
| | 17 40 15 | +01 38.0 | No motion |
| +45:2877 | 18 18 56 | +45 30.0 | |
| -74:1278 | 18 44 36 | -74 32. | No motion |
| +29:4321 | 20 05 06 | +29 34. | |
| 106-304 | 20 28 02 | +57 40.7 | Duplicate entry |
|___________|__________|__________|____________________________________|
Table 4: Stars Deleted from the NLTT Catalogue
14
______________________________________________________________________
| 1-157 0 17 54 17.9 1 +86 03.0 16.3 17.9 m 0.496 80 A |
| 405- 7 0 20 49 20.8 2 +19 33.6 11.3 12.9 m 0.287 124 A |
| 465- 65 0 37 52 37.9 2 +13 26.5 13.7 14.8 k 0.237 98 A |
| 241- 53 0 42 30 42.5 2 +39 02.0 13.9 15.4 m 0.342 229 A |
| 526- 48 0 58 27 58.5 2 + 8 02.9 17.3 18.4 k 0.245 122 A |
| +14:167B* 1 02 51 02.9 2 +15 07.4 9.6 10.9 k-m 0.199 175 A |
| 527- 20* 1 11 28 11.5 2 + 6 18.4 16.7 18.0 k-m 0.195 112 A |
| +30:206B* 1 18 38 18.6 2 +31 04.9 13.0 14.5 m 0.527 103 A |
| +30:206A 1 18 39 18.7 2 +31 04.9 9.5 10.6 k 0.527 103 A |
| 468- 99* 1 29 48 29.8 2 +14 02.1 16.9 18.5 m 0.220 125 A |
| 468- 98 1 29 48 29.8 2 +14 01.9 11.0 12.3 k-m 0.220 125 A |
| 939-117 1 38 04 38.1 2 -38 18.0 14.2 0.307 72 A |
| 768-453 1 43 52 43.9 2 -16 55.6 12.9 14.6 m 0.187 200 A |
| * 2 03 48 03.8 2 +44 57.3 10.5 11.8 K5 0.510 148 A |
| Pulk 22- 18 2 45 26 45.4 2 +44 32.8 13.0 14.5 m 0.281 125 A |
| 198-106 2 56 57 57.0 2 +44 06.5 18.4 21. +m 0.250 135 A |
| 471- 54 3 04 37 04.6 2 +12 33.9 12.7 13.6 g-k 0.328 142 A |
| 831- 38 3 10 13 10.2 2 -21 42.3 14.5 16.3 m 0.302 175 A |
| 831- 39* 3 10 13 10.2 2 -21 42.3 15.3 16.8 m 0.302 175 A |
| 198-289 3 10 15 10.3 2 +44 05.1 11.1 12.0 g-k 0.180 125 A |
| 198-290* 3 10 15 10.3 2 +44 05.1 11.5 12.6 k 0.180 125 A |
| -35:1111* 3 10 33 10.6 2 -34 59.7 10.2 11.3 k 0.182 186 A |
| +48:884* 3 15 49 15.8 2 +49 07.7 10.2 11.3 k 0.241 134 A |
| 155-231 3 29 02 29.0 2 +45 14.0 16.3 17.8 m 0.181 144 A |
| +34:724 3 41 18 41.3 2 +34 49.1 10.9 12.2 k-m 0.250 135 A |
| 474-233 3 56 00 56.0 2 + 9 28.0 12.6 13.7 k 0.183 103 A |
| 31-302* 4 00 30 00.5 2 +71 08.9 15.1 16.4 k-m 0.417 155 A |
| +11:570 4 03 08 03.1 2 +11 49.9 10.5 12.0 M1 0.200 88 A |
| 833- 51* 4 09 30 09.5 2 -26 10.2 13.1 14.4 k-m 0.195 139 A |
| 358- 60* 4 13 41 13.7 2 +24 39.9 14.5 15.6 k 0.398 85 A |
| 358-152 4 19 24 19.4 2 +22 49.0 18.3 20.8 m 0.182 169 A |
| 302- 49 4 19 59 20.0 2 +31 59.3 12.4 13.9 m 0.271 179 A |
| 415-254 4 33 54 33.9 2 +18 55.0 18.7 21.2 m 0.378 140 A |
| 358-501 4 37 26 38.4 2 +22 09.4 15.8 17.0 k 0.189 113 A |
| 358-499 4 37 33 38.6 2 +24 55.5 13.1 14.7 m 0.207 102 A |
| 891- 12* 4 43 17 43.3 2 -27 31.7 17.1 16.6 b 0.236 246 A |
| 891- 13 4 43 21 43.4 2 -27 31.4 15.1 16.4 k-m 0.236 246 A |
| 360- 9 5 18 44 18.7 2 +23 29.2 12.0 13.5 m 0.243 197 A |
| 119- 43 5 23 52 23.9 2 +55 12.8 14.8 16.8 m+ 0.228 228 A |
| 481- 6 6 42 34 42.6 2 + 9 38.9 10.0 11.1 k 0.220 129 A |
|______________________________________________________________________|
Table 5. NLTT Addenda Stars
15
______________________________________________________________________
| -43:2907* 7 02 27 02.5 2 -43 32.5 6.9 7.5 GO 0.412 343 A |
| -43:3260A* 7 27 39 27.7 2 -43 11.9 3.3 4.6 K5 0.200 340 A |
| 88-308* 7 40 40 40.7 2 +56 53.3 18.7 21.0 m+ 0.207 124 A |
| +68:518* 8 00 47 00.8 2 +68 31.6 7.6 8.0 F5 0.306 224 A |
| +45:1576 8 20 48 20.8 2 +45 06.8 7.7 8.6 g-k 0.201 202 A |
| - 9:2563* 8 30 32 30.5 2 - 9 23.4 10.7 12.2 m 0.199 217 A |
| 368- 36 8 38 24 38.4 2 +21 14.5 17.7 19.5 m 0.228 140 A |
| -18:2482* 8 45 15 45.3 2 -18 48.5 11.0 12.3 k-m 0.180 282 A |
| 18-173* 9 05 41 05.7 2 +78 57.0 18.2 20.0 m 0.319 221 A |
| + 6:2182 9 27 19 27.2 2 + 5 52.4 7.0 8.2 K2 0.523 282 A |
| 668- 59 9 48 00 48.0 2 - 4 43.6 9.5 10.8 k-m 0.193 291 A |
| +12:2149* 10 05 43 05.7 2 +12 12.7 1.4 1.2 B8 0.241 270 A |
| 489- 63 10 14 56 14.9 2 + 8 51.0 17.0 18.9 m 0.196 253 A |
| 670- 1 10 20 31 20.5 2 - 7 20.0 15.0 16.6 m 0.325 152 A |
| 490- 68 10 29 30 29.5 2 + 8 46.0 11.7 12.8 k 0.220 151 A |
| -18:3019* 10 43 19 43.3 2 -18 50.6 11.2 12.8 m 1.980 251 A |
| 791- 55* 10 43 19 43.3 2 -18 50.7 16.2 16.5 f 1.980 251 A |
| VBs 18* 10 54 26 54.4 2 +42 14.2 15.0 16.8 m 0.352 228 A |
| 102- 26* 10 56 12 56.2 1 -66 31. 12.9 14.4 m 0.24 305 A |
| 168- 47 10 56 28 56.5 2 +44 30.8 17.0 18.1 k 0.240 264 A |
| +56:1499 11 03 52 03.9 2 +55 59.0 9.2 9.8 GO 0.212 246 A |
| 318-129* 11 18 21 18.4 2 +30 02.5 13.0 14.5 m 0.237 171 A |
| 374- 54* 11 24 47 24.8 2 +23 06.3 12.3 14.5 k-m 0.635 217 A |
| -31:9083* 11 30 32 30.5 2 -31 34.8 3.7 4.6 G5 0.209 260 A |
| +36:2219 11 48 33 48.6 2 +35 32.9 10.6 11.9 k-m 0.350 321 A |
| 493- 60* 11 48 42 48.7 2 +13 10.6 19.0 19.0 f 0.210 182 A |
| 673- 42b* 11 50 44 50.7 2 - 7 05.5 19.0 19.4 f 0.538 198 A |
| 11 56 04 56.1 2 +59 50.0 10.7 12.2 m 0.699 271 A |
| Grw +68:4303 11 57 35 57.6 2 +68 05.7 11.5 12.8 k-m 0.192 242 A |
| -34:7900A* 12 02 42 02.7 2 -34 54.5 10.1 11.2 k 0.210 288 A |
| -34:7900B* 12 02 42 02.7 2 -34 54.5 13.2 14.3 k 0.210 288 A |
| 64-125* 12 07 28 07.5 2 +68 25.8 15.0 16.3 k-m 0.337 244 A |
| U 40- 83 12 09 57 10.0 2 +39 57.3 11.4 12.9 M2 0.239 130 A |
| 794- 49 12 16 03 16.1 2 -20 07.5 15.3 16.8 m 0.346 278 A |
| 495- 36 12 19 00 19.0 2 +14 38.5 14.8 16.3 m 0.273 261 A |
| 435- 46* 12 20 17 20.3 2 +17 41.6 14.9 16.4 m 0.323 224 A |
| U 43-151 12 39 25 39.4 2 +43 19.1 11.6 12.9 k-m 0.257 215 A |
| 436- 19* 12 47 13 47.2 2 +16 29.1 11.8 13.3 m 0.238 189 A |
| 39-231* 12 49 13 49.2 2 +71 34.1 16.2 17.7 m 0.263 286 A |
| 377- 90* 12 49 43 49.7 2 +23 00.4 11.9 13.0 k 0.203 292 A |
|______________________________________________________________________|
16
______________________________________________________________________
| 378-315 13 00 41 00.7 2 +24 14.2 14.4 16.0 m 0.420 268 A |
| +59:1488 13 07 16 07.3 2 +58 50.7 9.2 10.5 K2 0.294 225 A |
| 557- 17 13 09 36 09.6 2 + 4 45.6 15.0 15.9 g-k 0.219 260 A |
| * 13 11 38 11.6 2 + 6 34.6 15.5 16.6 k 0.334 216 A |
| 617- 43 13 20 21 20.4 2 - 0 35.2 18.7 19.0 f-g 0.192 304 A |
| 617- 46 13 21 16 21.3 2 + 0 07.2 19.0 21.0 m 0.193 259 A |
| 379- 57* 13 31 30 31.5 2 +21 24.7 13.0 14.7 m 0.305 245 A |
| 380- 7 13 45 49 45.8 2 +21 53.1 15.9 17.0 k 0.197 199 A |
| +24:2642* 13 46 12 46.2 2 +24 25.2 11.0 12.5 m 0.203 298 A |
| 324- 26 13 51 22 51.4 2 +27 00.1 18.7 20.7 m 0.185 194 A |
| 439-150 13 59 15 59.3 2 +16 26.5 18.3 21.0 m+ 0.304 175 A |
| 439-448 14 06 23 06.4 2 +17 46.2 12.1 13.0 g-k 0.265 214 A |
| 381- 41* 14 17 46 17.8 2 +22 55.9 12.0 12.2 f-g 0.429 248 A |
| + 2:2820A 14 24 04 24.1 2 + 2 21.2 9.7 10.8 k 0.198 308 A |
| 14 25 23 25.4 2 - 0 09.2 13.1 14.8 m 0.412 283 A |
| 500- 98 14 34 07 34.1 2 +11 15.7 13.4 14.9 m 0.292 118 A |
| 500- 99* 14 34 08 34.1 2 +11 15.9 13.5 15.0 m 0.292 118 A |
| -64:867B* 14 38 24 38.4 1 -64 46. 8.8 9.9 k 0.31 218 A |
| +14:2771* 14 39 07 39.1 2 +13 49.1 8.4 8.9 F8 0.397 257 A |
| 500- 80* 14 39 08 39.1 2 +13 50.4 12.8 14.3 m 0.397 257 A |
| +18:2917B* 14 40 40 40.7 2 +18 17.2 13.8 15.3 m 0.352 151 A |
| 682- 71 15 16 52 16.9 2 - 5 26.2 18.8 20.8 m 0.181 257 A |
| W 571 15 40 38 40.6 2 + 5 00.4 12.7 13.8 k 0.180 263 A |
| 177-118 15 47 48 47.8 2 +45 36.0 18.7 19.8 k 0.232 246 A |
| 100- 27* 15 49 53 49.9 2 +59 07.1 16.0 17.5 m 0.260 265 A |
| 384- 64 15 50 59 51.0 2 +22 59.9 13.5 15.0 m 0.276 236 A |
| 744- 19* 16 04 29 04.5 2 -14 14.7 11.9 13.2 k-m 0.180 192 A |
| 42-329* 16 15 51 15.9 2 +74 34.5 11.6 12.7 k 0.180 282 A |
| Grw +67:5226* 16 16 39 16.7 2 +67 22.6 11.1 12.7 M3 0.522 279 A |
| 686- 18* 16 48 14 48.2 2 - 8 47.1 12.6 13.5 g-k 0.322 228 A |
| -10:4463* 17 13 26 13.4 2 -10 48.9 10.3 11.5 K2 0.225 149 A |
| W 672A 17 16 05 16.1 2 + 2 00.2 14.9 14.7 DA 0.512 237 A |
| W 672B* 17 16 06 16.1 2 + 2 00.0 13.2 15.4 M3 0.512 237 A |
| L 485-9* 17 21 35 21.6 2 -35 26.1 14.5 15.6 k 0.316 186 A |
| 747- 27 17 23 40 23.7 2 -13 07.0 10.9 12.2 k-m 0.187 136 A |
| 24- 50* 17 40 48 40.8 2 +76 45.9 14.8 16.3 m 0.218 351 A |
| 748- 34* 17 47 22 47.4 2 -13 39.1 13.8 15.3 m 0.202 212 A |
| 748- 35 17 48 08 48.1 2 -12 29.5 13.5 14.8 k-m 0.349 224 A |
| + 4:3561a* 17 55 23 55.4 2 + 4 33.4 9.2 11.2 M5 0.310 356 A |
| 139- 42 18 02 27 02.5 2 +53 24.6 12.0 13.1 k 0.222 289 A |
|______________________________________________________________________|
17
______________________________________________________________________
| 449- 10 18 04 35 04.6 2 +17 20.3 14.7 15.8 k 0.234 3 A |
| 570- 18* 18 29 27 29.5 2 + 8 33.9 13.1 13.7 g 0.285 196 A |
| L 489-68 18 34 57 35.0 2 -39 07.8 14.0 0.188 73 A |
| 630- 16 18 36 09 36.2 2 + 1 56.5 13.5 15.0 m 0.232 186 A |
| 450- 12 18 39 00 39.0 2 +16 18.7 10.1 11.2 k 0.231 176 A |
| 867- 2* 18 43 59 44.0 2 -23 33.7 13.0 14.3 k-m 0.448 232 A |
| R 154* 18 46 45 46.8 2 -23 53.2 11.0 12.7 M6 0.720 107 A |
| 811- 16 18 50 13 50.2 2 -16 19.2 13.3 14.6 k-m 0.202 199 A |
| 336- 6* 19 05 45 05.8 2 +32 26.8 11.6 13.3 M3 1.635 49 A |
| +11:3777* 19 11 46 11.8 2 +11 43.5 10.5 11.6 k 0.251 228 A |
| 104-443 19 25 21 25.4 2 +58 06.5 16.0 17.5 m 0.356 222 A |
| +50:2848* 19 40 32 40.5 2 +50 24.0 6.4 7.0 GO 0.214 223 A |
| 925- 35* 19 40 36 40.6 2 -29 14.7 12.8 14.6 m 0.223 165 A |
| 869- 29 19 42 34 42.6 2 -24 11.3 17.8 20.5 m+ 0.240 213 A |
| 926- 4 19 47 28 47.5 2 -29 24.2 14.0 15.3 k-m 3.204 187 A |
| 870- 64 20 00 54 00.9 2 -23 48.5 13.2 13.8 g 0.185 237 A |
| L1573- 24 20 02 33 02.6 2 +38 00.1 13.8 14.9 k 0.320 202 A |
| 20 16 04 16.1 2 +23 09.4 10.7 12.2 m 0.258 4 A |
| 755- 36* 20 32 51 32.9 2 -13 06.8 14.5 15.6 k 0.322 134 A |
| R 764 20 40 31 40.5 2 +52 05.8 10.8 11.7 g-k 0.226 345 A |
| +45:3245A 20 40 39 40.7 2 +45 38.7 7.7 8.3 GO 0.205 200 A |
| +38:4344* 21 04 40 04.7 2 +38 29.8 5.8 7.2 K8 5.204 52 A |
| 186- 1* 21 07 00 07.0 2 +46 57.4 11.7 12.9 K3 0.497 120 A |
| 457- 11* 21 09 42 09.7 2 +18 10.1 15.7 16.8 k 0.195 179 A |
| 285- 11* 21 15 24 15.4 2 +34 33.7 14.3 15.8 m 0.240 50 A |
| 517- 35 21 17 42 17.7 2 +13 04.9 14.7 16.5 m 0.248 0 A |
| 21 26 53 26.1 2 +39 40.3 13.7 15.2 m 0.280 101 A |
| -68:2241* 21 34 18 34.3 1 -68 17. 8.5 10.0 m 0.22 101 A |
| 463- 20 21 34 40 34.7 2 +20 43.7 11.5 12.6 k 0.204 103 A |
| 398- 17 21 37 52 37.9 2 +21 32.6 18.9 20.6 m 0.202 48 A |
| + 5:4868 21 44 56 44.9 2 + 6 22.2 11.0 11.6 g 0.280 64 A |
| W 945 21 45 58 46.0 2 +50 00.3 13.7 15.2 m 0.823 58 A |
| * 21 51 55 51.9 2 +41 32.8 10.6 11.9 K8 0.533 133 A |
| R 263 21 54 17 54.3 2 +19 32.3 13.4 14.7 k-m 0.477 194 A |
| 283- 3 22 00 14 00.2 1 -50 51.7 11.9 13.4 m 0.58 148 A |
| Grw 65: * 22 04 25 04.4 2 +65 23.9 12.3 13.4 k 0.393 308 A |
| 1032-120 22 20 06 20.1 2 -43 42.5 14.0 0.863 117 A |
| 640- 76* 22 30 16 30.3 2 + 2 03.2 14.3 16.2 m 0.180 94 A |
| -28:17852* 22 34 37 34.6 2 -28 20.3 11.1 12.4 k-m 0.386 121 A |
| -28:17856* 22 34 50 34.8 2 -28 20.9 10.0 11.3 k-m 0.386 121 A |
|______________________________________________________________________|
18
______________________________________________________________________
| 27-403* 22 39 59 40.0 2 +75 31.4 15.7 17.0 k 0.180 71 A |
| +51:3485 22 48 37 48.6 2 +51 47.6 7.1 7.7 GO 0.220 36 A |
| 400- 70* 22 50 40 50.7 2 +27 10.9 17.1 19.4 m+ 0.181 91 A |
| 701- 84* 22 53 05 53.1 2 - 6 29.4 16.0 17.5 m 0.268 120 A |
| -26:16395A* 22 55 05 55.1 2 -26 22.3 7.4 8.0 GO 0.338 148 A |
| +11:4913 22 56 48 56.8 2 +11 55.6 8.5 9.1 GO 0.371 114 A |
| +40:4962 22 57 22 57.4 2 +40 47.2 11.0 12.5 m 0.260 224 A |
| 521- 59 22 59 10 59.2 2 +15 11.9 17.2 18.7 m 0.248 219 A |
| 985-108 23 09 22 09.4 2 -38 15.6 11.8 13.1 k-m 0.180 140 A |
| +20:5292 23 10 49 10.8 2 +20 40.4 9.9 10.8 G5 0.253 154 A |
| 23 15 00 15.0 2 +37 56.6 10.9 12.9 m 0.470 196 A |
| 643- 33* 23 37 23 37.4 2 - 1 43.7 18.5 21.0 m+ 0.210 214 A |
| +46:4175P 23 45 43 45.7 2 +46 48.4 9.3 10.4 k 0.236 125 A |
| +59: 68a 0 27 32 27.5 2 +59 54.5 9.1 9.5 F5 0.206 62 A |
| -57:395* 1 57 06 57.1 1 -57 07. 8.0 8.9 G0 0.20 45 A |
| -57:396* 1 57 06 57.1 1 -57 07. 8.3 9.2 G5 0.20 45 A |
| W 1059 7 57 23 57.4 2 +29 09.1 12.4 13.0 G0 0.481 184 A |
| 375- 23 11 39 43 39.7 2 +23 18.2 10.8 12.3 m 0.202 281 A |
| -48:7070 11 59 42 59.7 1 -48 27. 9.2 10.1 G5 0.23 268 A |
| -26:10310 14 25 48 25.8 2 -27 01.6 11.6 12.7 k 0.270 248 A |
| -73:1474* 19 48 42 48.7 1 -73 58. 9.6 9.7 K0 0.21 126 A |
| - 6:5663* 21 01 19 01.3 2 - 6 20.0 9.7 11.3 m 0.455 235 A |
| 290- 60 23 31 07 31.1 2 +32 17.7 13.7 14.8 k 0.261 95 A |
| 23 47 23 47.4 2 +29 17.8 15.2 15.8 g 0.531 191 A |
|______________________________________________________________________|
19
© UDS/CNRS