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VII/203                 Las Campanas Redshift Survey (Shectman+ 1996)

The Las Campanas Redshift Survey Shectman S.A., Landy S.D., Oemler A., Tucker D.L., Lin H., Kirshner R.P., Schechter P.L. <Astrophys. J. 470, 172 (1996)> =1996ApJ...470..172S
ADC_Keywords: Redshifts ; Galaxy catalogs ; QSOs Keywords: cosmology: observations - galaxies: clusters: general - galaxies: distances and redshifts - surveys Abstract: The Las Campanas Redshift Survey (LCRS) consists of 26,418 redshifts of galaxies selected from a CCD-based catalog obtained in the R band. The survey covers over 700deg^2 in six strips, each 1.5x80deg, three each in the north and south Galactic caps. The median redshift in the survey is about 30,000km/s. Essential features of the galaxy selection and redshift measurement methods are described and tabulated here. These details are important for subsequent analysis of the LCRS data. Two-dimensional representations of the redshift distributions reveal many repetitions of voids, on the scale of about 5000km/s, sharply bounded by large walls of galaxies as seen in nearby surveys. Statistical investigations of the mean galaxy properties and of clustering on the large scale are reported elsewhere. These include studies of the luminosity function, power spectrum in two and three dimensions, correlation function, pairwise velocity distribution, identification of large-scale structures, and a group catalog. Description: In referencing individual galaxies within the LCRS, it is recommended that investigators adhere to the IAU-registered LCRS naming convention, as listed in the online "dictionary of nomenclature of celestial objects" (, which is: LCRS BHHMMSS.s-DDMMSS, in which the coordinates are equinox 1950.0, RA is truncated (* not rounded *) to a tenth of a second, and DEC is truncated (* not rounded *) to a whole arcsecond. See also: See also the LCRS home pages at: : Las Campanas Redshift Survey File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file fields.dat 123 327 LCRS spectroscopic fields (Table 2) catalog.dat 98 94959 Redshift catalog (Table 3)
Byte-by-byte Description of file: fields.dat
Bytes Format Units Label Explanations
1- 8 A8 --- Field Field designation (1) 10- 11 I2 h RA1h First boundary field right ascension (1950.0) 13- 14 I2 min RA1m First boundary field right ascension (1950.0) 16- 20 F5.2 s RA1s First boundary field right ascension (1950.0) 22- 23 I2 h RA2h Second boundary field right ascension (1950.0) 25- 26 I2 min RA2m Second boundary field right ascension (1950.0) 28- 32 F5.2 s RA2s Second boundary field right ascension (1950.0) 34 A1 --- DE1- First boundary field declination sign 35- 36 I2 deg DE1d First boundary field declination (1950.0) 38- 39 I2 arcmin DE1m First boundary field declination (1950.0) 41- 44 F4.1 arcsec DE1s First boundary field declination (1950.0) 46 A1 --- DE2- Second boundary field declination sign 47- 48 I2 deg DE2d Second boundary field declination (1950.0) 50- 51 I2 arcmin DE2m Second boundary field declination (1950.0) 53- 56 F4.1 arcsec DE2s Second boundary field declination (1950.0) 58- 62 F5.2 mag m1 Lower limit magnitude (2) 64- 68 F5.2 mag m2 Higher limit magnitude (2) 70- 74 F5.2 mag mcen Faint central magnitude limit at m2 (2) 76- 78 I3 --- Nfib Designates whether data was obtained with the 50- or 112-object spectrograph system 80- 82 I3 --- Ngal Number of galaxies, within the geometric and photometric limits of the field, which have redshifts. 84- 87 F4.2 --- f Sampling fraction (3) 89- 98 A10 "DD-MM-YYYY" Night Spectroscopic observations date 100-102 I3 --- Frame Spectroscopic exposure number 104-123 A20 --- plate Spectroscopic plate designation
Note (1): Field name from RA (HHMM), Dec (+DD) and a letter suffix "W", "E", or "M" which means west, east, or middle, Note (2): Photometric selection limits. Note the catalogs always contain objects outside the photometric limits. Isophotal magnitude m and central magnitudmc of each galaxy must meet the photometric selection criteria m1 ≤ m < m2 and mc < mcen - 0.5(m2-m) Note (3): Fraction of objects (galaxies plus stars) with velocities, among those objects meeting the photometric selection limits.
Byte-by-byte Description of file: catalog.dat
Bytes Format Units Label Explanations
1- 8 A8 --- Field Field designation 10- 15 F6.1 --- p Photometric catalog object number 17- 21 F5.2 mag mag Isophotal magnitude 23- 32 A10 --- Scan Designation of drift scan used to obtain object photometry 34- 38 F5.2 mag mc Central magnitude 40- 41 I2 h RAh Right Ascension (1950.0) 43- 44 I2 min RAm Right Ascension (1950.0) 46- 50 F5.2 s RAs [0,60] Right Ascension (may be 60.00) epoch 1950.0 52 A1 --- DE- Declination sign 53- 54 I2 deg DEd Declination (1950.0) 56- 57 I2 arcmin DEm Declination (1950.0) 59- 62 F4.1 arcsec DEs [0,60] Declination (may be 60.0) epoch 1950.0 64- 66 A3 --- s ? Spectroscopic fiber designation (1) 68- 69 A2 --- type ? Spectrum type (1) (2) 71- 75 I5 km/s cz ? Heliocentric velocity (1) 77- 80 I4 km/s e_cz ? rms uncertainty on cz 82- 86 F5.3 --- sf ? Product of sampling fraction, apparent magnitude completeness, and central surface brightness completeness factors (1) (3) 88- 92 F5.3 --- gsf ? Same as sf but sampling fraction is computed only in a 1000"-radius neighborhood of the galaxy (1) (4) 94- 98 I5 km/s cz55 ? Instrumental constraints prevent two object fibers from approaching closer than 55" on the sky (1) (5)
Note (1): Columns "s" to "cz55" are blank if not applicable to a particular object Note (2): Spectrum type: * c, e, b: galaxy - c: velocity from cross-correlation only - e: velocity from emission-line fitting only - b: velocity from both c and e * *: star * ?: spectrum failed to yield redshift * nh, tc, bl: same as no spectrum attempted (intended spectrum not observed) * QS: QSO * PN: planetary nebula Note (3): See Lin et al. (1996ApJ...464...60L) for more information; sf = f * F * G in the notation of that paper. Objects should be weighted by 1/sf in statistical analyses. Only those galaxies meeting the photometric selection limits have an entry. Note (4): This attempts to account for any variable geometric sampling effects, e.g. the reduced spectroscopic success at field corners (Shectman et al. 1995, in Wide-Field Spectroscopy and the Distant Universe, proceedings of the 35th Herstmonceux Conference (July 1994), eds. S. J. Maddox & A. Aragon-Salamanca (Singapore: World Scientific), p. 98.). Experience with the galaxy power spectrum (Lin et al., 1996ApJ...471..617L) shows that using gsf instead of sf makes little difference, but it does not hurt to check this for your own analyses. Note (5): For an object without a redshift, cz55 is the velocity of its closest neighbor within 55", if one exists, that has a velocity. Only objects within the photometric limits have an entry. To assess the significance of this selection effect for your particular analysis, you can try assigning fake velocities as described in Lin et al. (1996ApJ...471..617L).
Nomenclature note: In referencing individual galaxies within the LCRS, it is recommended that investigators adhere to the IAU-registered LCRS naming convention, as listed in the online "Dictionary of Nomenclature of Celestial Objects" (, which is: LCRS BHHMMSS.s-DDMMSS in which the coordinates are equinox 1950.0, RA is truncated (*** not rounded ***) to a tenth of a second, and Dec is truncated (*** not rounded ***) to a whole arcsecond. History: * 22-Oct-1996: AAS CD-ROM series, Volume 7, Lee Brotzman [ADS] * 03-Feb-1997: merged fields, Patricia Bauer, [CDS] * 18-Apr-2010: following a remark by H. Andernach: some fields were apparently missing in the merged catalog; the missing fields were added, and 4 duplicate records were removed (F. Ochsenbein)
(End) Patricia Bauer, [CDS] 03-Feb-1997
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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