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CNS3 - Gliese Catalog of Nearby Stars, 3rd Edition

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Overview

The CNS3 catalog contains all known stars as of 1991 that are within 25 parsecs of the Sun. It depends mainly on a preliminary version (Spring 1989) of the new General Catalogue of Trigonometric Parallaxes (YPC) prepared by Dr. William F. van Altena (Yale University).

The catalog contains every then-known star with a trigonometric parallax greater than or equal to 0.0390 arcsec, even though it may be evident from photometry or for other reasons that the star has a larger distance. For red dwarf stars, new color-magnitude calibrations for broad-band colors were carried out and applied. For white dwarfs, the recipes of McCook and Sion in ApJS, 65, 603 (1987) were applied. Stroemgren photometry was used (not yet systematically) for early-type stars and for late dwarfs, the latter supplied by E. H. Olsen from Copenhagen Observatory (private communication).

In contrast to the CNS2 (Gliese 1969) catalog, trigonometric parallaxes and photometric or spectroscopic parallaxes were not combined in this version.

The resulting parallax in the present version is the trigonometric parallax if the relative error of the trigonometric parallax is smaller than 14 percent. The parallax may be the photometric or spectroscopic parallax only if no trigonometric parallax is available or if the standard error of the trigonometric parallax is considerably larger.


Catalog Bibcode

<V/70A/catalog.dat>

Caveats

The positions given for the stars in this table are (1) often not of high accuracy and (2) correspond to epoch 1950, and thus they do not include over a half-century of proper motions. Better quality positions for these stars are available in the GLIESE2MAS table.

References

Preliminary Version of the Third Catalogue of Nearby Stars, Wilhelm Gliese and Hartmut Jahreiss, Astronomisches Rechen-Institut, Heidelberg, Germany. (1991).

Provenance

The original catalog and the notes describing it were prepared by Wilhelm Gliese and Hartmut Jahreiss, Astronomisches Rechen-Institut, Moenchhofstrasse 12-14, D-6900 Heidelberg 1, Germany, in 1991. The CDS has made a number of formatting and documentation changes in the period 1994-1997, e.g., in December 1997 it added a running number to the name for 1388 stars which had all been given the same name of "NN" in the original version, starting with "NN 3001" (for the first "NN" star in order of 1950 RA), and ending with "NN 4388" (for the last "NN" star in order of 1950 RA). This revised version of the catalog (CDS/ADC Catalog V/70A) was used by the HEASARC to create this database in February 2001.

Nomenclature Note

All new nearby stars have not yet been given Gliese (Gl) or Gliese and Jahreiss (GJ) numbers and those stars were all given the name of "NN" in the original version of this catalog. It is recommended for such stars that one of the alternate designations (see the Giclas_Number, LHS_Number, Other_Name or Remarks parameter fields) be used if available. However, the usage found in the literature led the CDS in December 1997 to add a running number to the name for these "NN" stars, starting with "NN 3001" (for the first "NN" star in order of 1950 RA), and ending with "NN 4388" (for the last "NN" star in order of 1950 RA).

Parameters

Name
The name of the star in CNS3. Generally, the preferred designations are GL, e.g., GL 10, the Gliese number, or the designation given to the star in the 2nd version of the Gliese Catalog (Gliese 1969), or GJ, e.g., GJ 1001, also often called the Gliese number, and derived from a tabulation of Gliese and Jahreiss (1979, Astr. Ap. Suppl., 38, 423), or Wo, e.g., Wo 9006, the Woolley number, or the designation used to refer to stars in the Woolley Nearby Stars Catalog (Woolley et al., 1970, Royal Observatory Annals, No. 5). More recently added stars have simply been given the designation "NN ('No Name') #" where # is a running sequence number in increasing RA (1950). For stars which are multiple, the component designation (A, B, C ...) had been included in the name, e.g., GL 11A.

Component
The component designation (A, B, C ...) if in a visual binary system.

Distance_Code
The reliability of the distance, coded as follows:

   S  -  trig. parallax > 0.0390 and phot. parallax    <  0.0390
   X  -  trig. parallax > 0.0390 and phot. parallax    <  0.0190
   P  -  trig. parallax < 0.0390 and phot. parallax    >  0.0390
   Q  -  trig. parallax < 0.0390 and phot. parallax(:) >  0.0390
  

RA
The Right Ascension of the object in the selected equinox. In the original input table this was given in B1950 equinox with a precision of 1 second of time.

Dec
The Declination of the object in the selected equinox. In the original input table this was given in B1950 equinox with a precision of 0.1 arcminutes.

LII
The Galactic longitude of the object.

BII
The Galactic latitude of the object.

Tot_Proper_Motion
The total proper motion in seconds of arc per year.

Flag_Proper_Motion
Proper Motion Uncertainty Flag [:].

Dir_Proper_Motion
The direction angle of proper motion, in degrees, using the standard convention (N is 0, increasing eastwards).

Radial_Velocity
The heliocentric radial velocity in km/s.

Radial_Velocity_Code
Information regarding the radial velocity and possible close binary status is coded as follows:

   VAR  -  variable radial velocity
   SB?  -  suspected spectroscopic binary
   SB   -  spectroscopic binary
  

Spect_Type
The spectral type (e.g., G2 V) or Luyten color class (e.g., m).

Ref_Spect_Type
The reference code for the origin of the spectral type:

   K  -  Kuiper Type (see ApJS, 59, 197, 1985)
   L  -  San-Gak Lee (AJ 89, 702, 1984)
   O  -  objective prism MK type (but not Michigan type)
   R  -  Robertson type (AJ, 89, 1229, 1984)
   P  -  Stephenson type (AJ, 91, 144, 1985  and AJ, 92, 139, 1986)
   S  -  Smethells type (IAU Coll. No 76, p. 421, 1983)
   U  -  Upgren et al. (AJ, 77, 486, 1972)
   W  -  Mount Wilson type
  

App_Mag
The apparent magnitude.

App_Mag_Code
If blank, this means that the apparent magnitude is in the Johnson V band. Otherwise, one of the following codes for apparent magnitude is used:

   P  -  photographic
   M  -  photometric
   C  -  from 'Cape refractor system'
   L  -  calculated or transformed
   V  -  variable
   :  -  uncertain
  

App_Mag_Joint
If `J', this means that the quoted magnitude is a joint magnitude.

BV_Color
The B-V color.

BV_Color_Code
The reference code for the origin of the B-V color:

   P  -  photographic
   M  -  photometric
   C  -  from 'Cape refractor system'
   L  -  calculated or transformed
   V  -  variable
   :  -  uncertain
  

BV_Color_Joint
If `J', this means that the quoted color is a joint color.

UB_Color
The U-B color.

UB_Color_Code
The reference code for the U-B color:

   P  -  photographic
   M  -  photometric
   C  -  from 'Cape refractor system'
   L  -  calculated or transformed
   V  -  variable
   :  -  uncertain
  

UB_Color_Joint
If `J', this means that the quoted color is a joint color.

RI_Color
The R-I color.

RI_Color_Code
The reference code for the R-I color:

   C  -  in Cousins' system
   T  -  transformed from another system
   :  -  uncertain
  

RI_Color_Joint
If `J', this means that the quoted color is a joint color.

Trig_Parallax
The trigonometric parallax, TP, in milliseconds of arc. To calculate the distance D in parsecs based on this value, D = 1000/TP.

Trig_Parallax_Error
The standard error of the trigonometric parallax, in milliseconds of arc.

Result_Parallax
The resulting (adopted) parallax, RP, in milliseconds of arc. To calculate the distance D in parsecs based on this value, D = 1000/RP.

Result_Parallax_Error
The standard error of the resulting parallax, in milliseconds of arc.

Result_Parallax_Code
The reference code for the resulting parallax as follows:

  blank  parallax from trigonometric parallax
   R  -  parallax from spectral types and broad-band colours
   W  -  photom. parallax for white dwarfs
   S  -  photom. parallax from Stroemgren photometry
   O  -  photom. parallax from Stroemgren photometry calculated by
         E. H. Olsen
   P  -  photom. parallax from other colors
  

Abs_Vmag
The absolute visual magnitude, M(V) based on the apparent magnitude V and the resulting parallax, RP. The relation is M(V) = V + Log10(RP) -10.0, where RP is in milliarcsecs.

Abs_Vmag_Code
The quality of the absolute (visual) magnitude, coded as follows (where s.e. is the standard error):

   A  -             s.e.  <  0.10 mag
   B  -  0.11  <    s.e.  <  0.20
   C  -  0.21  <    s.e.  <  0.30
   D  -  0.31  <    s.e.  <  0.50
   E  -  0.51  <    s.e.  <  0.75
   F  -  0.76  <    s.e.
  

Uvel
The U space velocity component in the Galactic plane and directed to the Galactic center.

Vvel
The V space velocity component in the Galactic plane and in the direction of Galactic rotation.

Wvel
The W space velocity component perpendicular to the Galactic plane and in the direction of the North Galactic Pole.

HD_Number
The Henry Draper catalog entry number.

DM_Number
The Durchmusterung zone and number:

   BD  -  Bonner Durchmusterung
   CD  -  Cordoba Durchmusterung
   CP  -  Cape Photographic Durchmusterung
  

Giclas_Number
The Giclas catalog entry number.

LHS_Number
The LHS catalog entry number.

Other_Name
Alternative catalog designations:

   V  -  Vyssotsky number (CDS Cat. III/13)
   U  -  UGP number (see AJ, 77, 486, 1972)
   W  -  white dwarf  (EG or Gr number, see CDS Cat. III/129)
  

Remarks
Additional identifications (LTT, LFT, Wolf, Ross, etc.) and other remarks.

Class
The Browse object classification. This classification is based on the 'Spect_Type' parameter, if such information is available. The following points should be noted:

   -  Spectral types were always converted to EXOSAT class by truncation,
      for example M2.5 becomes M2 (class 2720).

   -  dMe stars were assigned classes in the 2800's.

   -  Unclassified stars and stars with only Luyten color classes were assigned
      classes in the 2900's.
  

Contact Person

Questions regarding the CNS3 database table can be addressed to the HEASARC User Hotline.

Page Author: Browse Software Development Team
Last Modified: 12-May-2011