# Where to find spectra from Las Campanas Redshift Survey?

We are searching data for your request:

Forums and discussions:
Manuals and reference books:
Data from registers:
Wait the end of the search in all databases.
Upon completion, a link will appear to access the found materials.

I am interested in the optical spectrum of a galaxy. In SIMBAD the reference for the redshift of my galaxy is the Las Campanas Redshift Survey. Hence I am looking for the optical spectrum from which the redshift was estimated.

LCRS catalog data should be accessible at VizieR:VII/203. The associated paper is Schectman et al. 1996.

## Las Campanas Redshift Survey

The Las Campanas Redshift Survey is considered the first attempt to map a large area of the universe out to a redshift of z = 0.2. It was begun in 1991 using the Las Campanas telescope in Chile to catalog 26418 separate galaxies. [1] It is considered one of the first surveys to document the so-called "end of greatness" where the Cosmological Principle of isotropy could be seen. Superclusters [2] [3] [4] [5] [6] [7] and voids are prominent features in the survey.

1. ^"The Las Campanas Redshift Survey". qold.astro.utoronto.ca. Archived from the original on 2012-06-30 . Retrieved 2016-12-26 .
2. ^
3. Shandarin, Sergei F. Yess, Capp (1998). "Detection of Network Structure in the Las Campanas Redshift Survey". The Astrophysical Journal. 505 (1): 12–17. arXiv: astro-ph/9705155 . Bibcode:1998ApJ. 505. 12S. doi:10.1086/306135.
4. ^
5. Bharadwaj, S. Gupta, A. K. Seshadri, T. R. (1999). "Nature of clustering in the Las Campanas redshift survey". Astronomy and Astrophysics. 351: 405–412. arXiv: astro-ph/9903252 . Bibcode:1999A&A. 351..405B.
6. ^
7. Einasto, J. Einasto, M. Hütsi, G. Saar, E. Tucker, D. L. Tago, E. Müller, V. Heinämäki, P. Allam, S. S. (2003). "Clusters and Superclusters in the Las Campanas Redshift Survey". Astronomy and Astrophysics. 410 (2): 425–443. arXiv: astro-ph/0304546 . Bibcode:2003A&A. 410..425E. doi:10.1051/0004-6361:20031105.
8. ^
9. Bharadwaj, S., Sahni, V., Sathyaprakash, B.S., Shandarin, Sergei F., Yess, Capp (2000). "Evidence for Filamentarity in the Las Campanas Redshift Survey". The Astrophysical Journal. 528 (1): 21–29. arXiv: astro-ph/9904406 . Bibcode:2000ApJ. 528. 21B. doi:10.1086/308163. CS1 maint: multiple names: authors list (link)
10. ^
11. Bharadwaj, Somnath Bhavsar, Suketu Sheth, Jatush V. (2004). "The Size of the Longest Filaments in the Universe". The Astrophysical Journal. 606 (1): 25–31. arXiv: astro-ph/0311342 . Bibcode:2004ApJ. 606. 25B. doi:10.1086/382140. ISSN0004-637X.
12. ^
13. Bharadwaj, Somnath Pandey, Biswajit (2004). "Using the filaments in the LCRS to test the LambdaCDM model". The Astrophysical Journal. 615 (1): 1–6. arXiv: astro-ph/0405059 . doi: 10.1086/424476 . ISSN0004-637X.

This astronomical catalog article is a stub. You can help Wikipedia by expanding it.

## Evidence for filamentarity in the Las Campanas Redshift Survey

We apply Shapefinders, statistical measures of "shape" constructed from two-dimensional partial Minkowski functionals, to study the degree of filamentarity in the Las Campanas Redshift Survey (LCRS). In two dimensions, three Minkowski functionals characterize the morphology of an object these are its perimeter (L), area (S), and genus. Out of L and S a single dimensionless Shapefinder statistic, Script F, can be constructed (0 ≤ Script F ≤ 1). The statistic Script F acquires extreme values on a circle (Script F = 0) and a filament (Script F = 1). Using Script F, we quantify the extent of filamentarity in the LCRS by comparing our results with a Poisson distribution having similar geometrical properties and the same selection function as the survey. Our results unambiguously demonstrate that the LCRS displays a high degree of filamentarity in both the northern and southern Galactic sections, in general agreement with the visual appearance of the catalog. It is well known that gravitational clustering from Gaussian initial conditions gives rise to the development of non-Gaussianity, reflected in the formation of a network-like filamentary structure on supercluster scales. Consequently, the fact that the smoothed LCRS catalog shows properties consistent with those of a Gaussian random field,whereas the unsmoothed catalog demonstrates the presence of filamentarity, lends strong support to the conjecture that the large-scale clustering of galaxies is driven by gravitational instability.

Item Type: Article Publication Published Physics and Astronomy Q Science > QB Astronomy IOP Publishing 0004-637X 04 Jun 2017 04:52 http://orca.cardiff.ac.uk/id/eprint/45938

## Loose groups of galaxies in the las campanas redshift survey

A "friends-of-friends" percolation algorithm has been used to extract a catalog of δn/n = 80 density enhancements (groups) from the six slices of the Las Campanas Redshift Survey (LCRS). The full catalog contains 1495 groups and includes 35% of the LCRS galaxy sample. A clean sample of 394 groups has been derived by culling groups from the full sample that either are too close to a slice edge, have a crossing time greater than a Hubble time, have a corrected velocity dispersion of zero, or contain a 55″ "orphan" (a galaxy with a mock redshift that was excluded from the original LCRS redshift catalog due to its proximity to another galaxy - i.e., within 55″). Median properties derived from the clean sample include a line-of-sight velocity dispersion σlos = 164 km s -1 , crossing time tcr = 0.10 H -1 0, harmonic radius Rh = 0.58 h -1 Mpc, pairwise separation Rp = 0.64 h -1 Mpc, virial mass Mvir = 1.90 × 10 13 h -1 M, total group R-band luminosity Ltot = 1.30 × 10 11 h -2 L, and R-band mass-to-light ratio M/L = 171 h M/L the median number of observed members in a group is three.

## Where to find spectra from Las Campanas Redshift Survey? - Astronomy

The SAO Telescope Data Center supports scheduling and astronomical observations on the optical telescopes of the Harvard-Smithsonian Center for Astrophysics: the Whipple and MMT Observatories on Mt. Hopkins in Arizona, and the Magellan Telescopes on Cerro Las Campanas in Chile.

We record and archive most observations on the telescopes on Mount Hopkins and reduce and analyze data from several spectrographs on those telescopes, producing redshifts for galaxies and radial velocities for stars. We also process and archive data from the f/5 MMIRS IR spectropgraph and Megacam imager on the Magellan Telescopes in Chile and archive data taken by CfA observers on other instruments on those telescopes. We develop and support computer software which helps scientists prepare for their observations, runs the instruments on the telescopes, reduces data to usable forms, and extracts star and galaxy velocities from spectra and positional information from images. Our web site provides full documentation of locally-developed software, access to some of our archived data, and results of some of the surveys we have supported.

The data we process is accessible through the CfA Optical/Infrared Science Archive.

For information on the services provided, click on one of the topics in the menu on the left.

## The deep abyss

A generous sprinkling of galaxies on an inky black sky is captured by the Victor M. Blanco four-metre telescope at Cerro Tololo Inter-American Observatory in Chile. Aside from a handful of foreground stars, distinguishable by their diffraction spikes, every object seen here is a galaxy, from the faintest splash of red to the dramatic ring of LEDA 14884.

Image: CTIO/NOIRLab/NSF/AURA.

The deep abyssThis region of sky is in the constellation Eridanus, the River, which is close to the galactic south pole, in the nearby constellation of Sculptor. The LEDA galaxy catalogue refers to the Lyon Extragalactic Database, which contains a list of galaxies and their properties from a variety of separate catalogues (LEDA 14884’s other designations are PGC01484 and ESO303-011.)

As can be seen in this mosaic assembled from images taken by the ‘Dark Energy Camera’ on the Victor M. Blanco telescope, there are hundreds if not thousands of galaxies visible in a patch of sky just 11.62 arcminutes by 7.48 arcminutes in area. The myriad galaxies seen here originally featured as part of the Las Campanas Redshift Survey in the late 1980s and 1990s, which measured the redshifts of 26,418 galaxies in six strips across the sky, covering 700 square degrees in total and focused on the galactic north and south poles. The purpose of the survey was to map the distribution of galaxies, looking for large-scale voids and great walls of galaxies that follow the cosmic web of matter.

## EDisCS

• Facilities:
• Frequency/Channel:
• Objects: galaxies in rich clusters.
• Distance: z

Objectives: “provide a large galaxy sample which permits detailed and accurate analyses of the properties of galaxies in the local universe” <Completed>

• Facilities:
• Frequency/Channel:
• Objects: Galaxies selected from a CCD-based catalog measured in a Kron-Cousins R-band
• Distance: Typical redshift is 30000 km/s
• Area: 700 square degrees in 6 strips, each 1.5 degrees * 80 degrees, three each in the North and South galactic caps.
• Resolution:
• Examinations: Clustering, luminosity, and spectral properties

Two dimensional representations of the redshift distribution

We can see voids and walls.

• Objectives: <Completed>
• Determination of the galaxy luminosity function in a volume with dimensions large enough to average over the large scale inhomogeneities.
• Study of the statistic of emission line galaxies in a large, unbiased sample of galaxies.
• Measure of the size distribution of inhomogeneities in the galaxy distribution over a large volume.
• Facilities: ESO 3.6m telescope
• Frequency/Channel:
• Objects: Limiting magnitude bJ=19.4
• Distance: Selection function peak at z=0.1
• Area: Over about 23 square degrees near the South Galactic Pole
• Resolution:

#### The CNOC1 Cluster Survey

• Facilities: CFHT Multi-Object-Spectrograph(MOS)
• Frequency/Channel:
• Objects: 16 rich X-ray selected galaxy clusters
• Distance: 0.17<z<0.55
• Area:
• Resolution:

### CNOC2 Field Galaxy Survey

• Facilities: CFHT MOS
• Frequency/Channel:
• Objects: 4 widely separated patches away from very bright stars and known rich low-z galaxy clusters
• Distance: To z=0.7
• Area: 1.5 square degrees
• Resolution:

## Keywords

• APA
• Standard
• Harvard
• Vancouver
• Author
• BIBTEX
• RIS

Research output : Contribution to journal › Review article › peer-review

T1 - The las campanas/AAT rich cluster survey

N2 - Some unsolved cosmological questions remain in relation to the formation of structure in the universe. One way of addressing such questions is to use rich galaxy clusters as tracers of the growth of large-scale structure. To date, studies of rich clusters of galaxies have concentrated on systems generally at either high redshift or in the local universe. The properties of clusters and their constituent galaxies at these extrema are becoming well understood. In particular, it is becoming clear that rich clusters have undergone considerable evolution both dynamically and in their galaxy populations over the last 5-8 Gyr. We are undertaking a detailed study of rich clusters of galaxies in the range 0·05 ≲ z ≲ 0·15. Our results will be directly comparable to those of previous studies both at high and low redshift and, for the first time, provide continuous coverage across this important and unexplored transitory epoch in terms of galaxy evolution and structure growth.

AB - Some unsolved cosmological questions remain in relation to the formation of structure in the universe. One way of addressing such questions is to use rich galaxy clusters as tracers of the growth of large-scale structure. To date, studies of rich clusters of galaxies have concentrated on systems generally at either high redshift or in the local universe. The properties of clusters and their constituent galaxies at these extrema are becoming well understood. In particular, it is becoming clear that rich clusters have undergone considerable evolution both dynamically and in their galaxy populations over the last 5-8 Gyr. We are undertaking a detailed study of rich clusters of galaxies in the range 0·05 ≲ z ≲ 0·15. Our results will be directly comparable to those of previous studies both at high and low redshift and, for the first time, provide continuous coverage across this important and unexplored transitory epoch in terms of galaxy evolution and structure growth.

## THE CENTER FOR ASTROPHYSICS REDSHIFT CATALOG

The CFA REDSHIFT CATALOG incorporates much of the latest velocity data from the Whipple Observatory and other sources as well as velocities from earlier compilations such as the Second Reference Catalogue of de Vaucouleurs, de Vaucouleurs and Corwin, the Index of Galaxy Spectra of Gisler and Friel, and the Catalogue of Radial Velocities of Galaxies of Palumbo, Tanzella-Nitti and Vettolani. It includes BT magnitudes, some UGC numbers and increased accuracy'' in the velocity source information.

The format for the catalog is:

A20,I2,I2,F5.2,A1,I2,I2,F4.1,F5.2,I7,I3,A1.

A more detailed description of the format can be found in Table 1. By definition, we are continually adding information and updates of the catalog will be made available at reasonable intervals.

The data presented here have primarily been assembled for the purpose of studying the large scale structure of the universe, and, as such, are nearly complete in redshift information, but are not necessarily complete in such categories as diameter, magnitude and cross-references to other catalogs. Additional information of that type will be added in later editions.

Much of the data in the northern hemisphere owe their origin to Zwicky's catalogues of galaxies (Zwicky et al. 1961-66 Zwicky 1971 Zwicky, Sargent and Kowal 1975). The authors of this catalog would like to express both their gratitute and reverence for Zwicky's monumental efforts.

The current public version of the CfA Redshift Catalog is available via anonymous ftp from:

The main data file is velocity.dat.gz (in compressed format) or velocity.dat (not compressed). Other useful data and programs can also be found there. Please read the README file first.

II. Velocities

Please note that the velocities quoted are heliocentric and that redshifts (z's) have been converted to velocity via v = zc, where c = 299,792.5 km s -1 . Redshift is defined as:

The use of velocity as cz without any special relativistic correction is important in reminding astronomers (and other folks!) that in the formula for proper, comoving distance, it is z (and not v) combined with that gives the distance:

from Mattig(1959) (c.f. Fairall 1992).

We quote heliocentric velocities to allow individual users to correct to their own favorite galactocentric or local groupocentric'' or Virgocentric'' or even the microwave background frame. We have endeavored to properly remove such corrections before entering data into the catalog, but confusion still remains in those cases where the authors do not explicitly state what corrections were made. In those cases we assume 300 sin(l) cos(b) km s -1 to be the galactocentric correction. Note also that now that velocities of precisions less than 30 km/sec are commonplace, the correction to heliocentic is mandatory! We strongly urge all other authors to follow this convention.

Basic radial velocity sources are listed in Table 2. Velocities with negative source designations are still in the private domain and cannot be used without the appropriate owner's consent. The additional source information in columns 51 and 52 is the number of the paper under the broader source categorization. Initially this was alphabetic, but as more recent papers are added, the numbering scheme has become chronological. Again, beware of blanks, which may signify source zero, but most likely indicates that this information has not yet been updated. In any case, the zero/blank paper for each source is likely to represent the largest number of velocities available from that source (e.g. the Second Reference Catalogue).

The RFN column in the catalog contains the file number of the spectrum which we have obtained for that galaxy. If this column is blank, we have not observed the galaxy. We have tried to fill this column in for all entries in zcat, not just with velocity entries measured by us (see section VIII for details on nomenclature).

Objects listed in the catalog that have no velocity and no listed velocity source (in the northern hemisphere) will be observed as part of the CfA survey extension. Give us time! (in particular, telescope time. ). In some cases, faint members of studied clusters are included to help users of this catalog determine which galaxies have been measured and which remain.

Velocity Errors

In general, the errors listed for velocities are the errors quoted by the original source. (i.e., random errors are quoted and systematic ones are neglected.) The only exceptions are where multiple measurements have significantly improved the velocity precision. Many sources quote errors that are really the internal mean error - e.g. the variance in the velocities measured from multiple lines in a single spectrum of a galaxy. These often do not include errors in zero points, errors caused by mis-centering the galaxy in the slit, other instrumental offsets, etc., and are always underestimates of the true external error in the velocity estimate. Some sources are better than others velocity errors from the CfA survey and most 21-cm sources are nearly within unity of the true external error (CfA errors are only about 10-20% low), while the uncertainties quoted in some older works, such as the RC2 and the RSA, are underestimates by more than a factor of two (see, for example, Sandage 1978). For several more detailed analyses of velocity uncertainties, see Lewis (1983), Rood (1982), Tifft (1990) and references therein.

A small number of our velocities are listed with the notation poor velocity.'' These are weak cross-correlation velocities or velocities from single emission lines that need to be checked. We will do that. In general, there is enough information in the spectra to suggest that they are nearly correct (but I wouldn't stake my first born child on them).

III. Magnitudes

Magnitudes for galaxies are a persistent and pesky problem. We have tried to do our best to adopt a more or less uniform system for the largest number of galaxies. That system is the B(0)-Zwicky system (Huchra 1976). Magnitude sources for quoted values are given in Table 3. B T magnitudes, when available, are given in columns 66-71. These are generally about 0.4 magnitude brighter than magnitudes on the B(0)-Zw system. Some additional galaxy magnitudes, especially for objects in deeper surveys, come from digital scans of photographic plates - mostly in the photographic J and R bands. These magnitudes, by definition, are rarely easily converted into the more standard isophotal or total photographic B systems each observer requires different zero point and color corrections. Some magnitudes have also been entered from the StScI Guide star scans (G) and from other such sources. Until proven otherwise and properly calibrated, these magnitudes are not to be trusted.

Temporarily, we have derived very approximate corrections from other systems to the B(0)-Zwicky system. These are given for sources 3-7 as:

Magnitudes are taken preferentially from the 1st Reference Catalogue of de Vaucouleurs - B(0) (magnitude source 0), Harvard Corrected (magnitude source 2), and then from the Zwicky Catalogue (magnitude source 1). Magnitudes from other sources are used only when necessary and/or available. As mentioned above, this choice of system maximizes the number of galaxy magnitudes available and will allow for easy conversion to other systems given diameter and morphological type information ( e.g. the BT system). Note that we have begun to include corrected Blue magnitudes from the RC3, as magnitude source A'' these should be nearly identical to BT magnitudes (source 6), but again may not be of high quality unless based on actual photoelectric or CCD photometry. Magnitudes for many faint sources have been derived from either CCD or photoelectic photometry (particularly for AGN, Hewett and Burbidge 1993).

There are several published systems of correction to the Zwicky catalogue magnitudes (Burakowskia and Rudnicki 1974 Bothun and Schommer 1982 Giovanelli and Haynes 1984 Bothun and Cornell 1992 Kron and Shane 1976), but generally these require full morphological type and diameter information for the transformation. User's of this catalog should transform the magnitudes as they require. Surprisingly, almost all of those papers have shown that Zwicky magnitudes are generally robust at the ±0.35 magnitude level as was origially shown in Huchra (1976).

2MASS magnitudes are listed as "khj=" in the comment field when available, same thing with SDSS magnitude, noted as "ugriz +2">IV. Morphological Types

The format for the morphological type designations is: I2, A1, I1, A1, where the first two digits are the numerically coded T type, the next letter is the Bar type, the next digit is the numericaly coded luminosity class, and the final letter denotes morphological perculiarities. The types are explained in more detail in Table 4.

Moderately detailed descriptions of morphological types have been given by Sandage (1966) and de Vaucouleurs et al. (1959 1963 1976). For this catalog we have chosen to used the numerically coded types, T types,'' devised by de Vaucouleurs and collaborators. Morphological types are de Vaucouleurs' T types from the RC2, Uppsala Catalogue and the Revised Shapley-Ames Catalog. Some additional types have been defined for peculiar and un-typed objects and for objects that are in catalogs of extragalactic objects but are really galactic in nature:

 24 = Open Star Cluster 25 = Plate Flaw, Star, etc. misclassified as a galaxy. 26 = TTauri Star 27 = Globular Cluster, Galactic 28 = Globular Cluster, Extragalactic 29 = Multiple Stars (Doubles/triples/. ) 30 = Planetary Nebula, misclassified as a galaxy. 31 = HII Region, part of a galaxy. 32 = HII Region, misclassified as a galaxy. 33 = Reflection Nebula, misclassified elsewhere as a galaxy. 35 = High Velocity Cloud (usually from HI survey) 40 = Part of a galaxy 50 = Unclassified artifact (i.e. look into it more) 51 = No object at coordinates 52 = Artifact due to bright star (diff. spike) 53 = Meteor streak

Many of these later classifications have been added to aid in classifying "extended sources" in the 2MASS Extended Source Catalog. And some additional generic types have been defined for objects that cannot or have not been classified fully in the de Vaucouleurs revised Hubble sequence:

 -9 = QSO/AGN, stellar, usually at high redshift -6 = Compact Elliptical (same designation as DV) -7 = Elliptical (generic) 11 = Compact Magellanic Irr (Extragalactic HII Region) 15 = Peculiar or untyped galaxy 16 = Irr II (a.k.a. "trainwreck") 20 = Sprial galaxy (generic)

Note that these would ordinarily be lumped into broader morphological bins, so 20's might be spread over types 1-6, -7's over -5 to -2, -6 would be lumped into -5, etc. if you want to use these types as part of the generic sequence.

We have decided to retain information on galactic objects misclassified as galaxies, on HII regions that are parts of other galaxies, and other such objects to prevent their inclusion in future lists of galaxies. Users should remove objects of type greater than 20 before using this catalog as a simple galaxy catalog --- otherwise you'll get all the HII regions in M101 listed separately as well a few plate flaws, stars and other assorted junk! We have also started (Fall of 1991) to include moderate redshift objects (z <

1.0) identified in AGN and Quasar searches since these are legitimately large extragalactic objects that can play an important part in mapping large scale structure. Such objects are included in the catalog with the type designation -9.''

Additional types for galaxies in the first CfA Redshift Survey region have been estimated by J. Huchra from glass copies of the Palomar Sky Survey at Kitt Peak National Observatory. Types for southern galaxies come from both the ESO catalog and the Vorontsov-Velyaminov Catalogues. More detailed types for the second CfA survey have been estimated by Harold Corwin.

. BEWARE Remember that types as well as source designations should be read in alphanumeric format to not confuse blanks with zeros.

Diameters are in arc minutes from the blue Palomar Sky Survey or the ESO quick blue survey à la Nilson, ESO, VV or the RC2. The input format is given below as F4.1, but be forewarned that several galaxies have diameters that exceed 99.9 arc-minutes (e.g. M31 and M33) and are stored as F4.0, and many, especially faint, compact galaxies have diameters smaller than 1 arc-minute that have been measured with precisions of two decimal places (e.g. 0.35'). As it stands, an input format of F4.n is sufficient to handle all the diameters in the catalog, but an output format of F6.2 is required to reproduce the catalog entries properly (without either overflow or truncation). Reading and writing diameters as A4 also works the variable can then be translated into a number.

VI. Complete Subset Catalogs

There are several subset catalogs that represent complete'' samples of galaxies. One, published in the Ap. J. Supplements in June of 1983 is called North Zwicky Forty'' or NZ40.DAT for short (fans of bad Burt Reynolds movies take note). It contains all galaxies in the merged Zwicky-Nilson catalog with the following properties:

The velocities for this sample are complete - it contains one star III ZW 92 (Zwicky wasn't perfect, but awfully close!) and

The other, large area, complete, magnitude-limited catalog is called the Bright Galaxy Redshift Catalogue'' or BGRC.DAT for short and contains all known galaxies brighter than B(0) = 13.21 in our adopted magnitude system. It is a whole sky catalog and the velocities are 99% complete. It contains

1350 galaxies. This sub-catalog has only been circulated as a private communication. This catalog is also extremely close to the Revised Shapley-Ames Catalogue of Sandage and Tammann.

ZCAT contains the data from the Southern Galaxy Redshift Survey (da Costa et al. 1987), which is an almost complete diameter limited sample of

1900 galaxies, and the Second Southern Sky Redshift Survey or SSRS2 of da Costa et al. 1998, with

5500 galaxies brighter than approximately 15.5 ESO blue magnitude. ZCAT also contains the data from the two IRAS galaxy surveys of M. Davis, J. Huchra, M. Strauss, J. Tonry and A. Yahil --- all objects above an absolute galactic latitude of 10 degrees with IR colors like galaxies and with F 60 > 1.95 Jy (Strauss et al. 1992) and above 1.2 Jy (Fisher et al. 1995). ZCAT also contains all the data from the Nearby Galaxy Catalogue of Tully and Fisher (1987), and is being continually updated with the data for the UGC catalog survey of Bothun et al. (1986).

The 2dF Galaxy Redshift Survey 100k Data Release, 30 June 2001 is now included. Less than 3000 galaxies of this survey were dropped because the velocities were not good enough. You will find in the comment field the 2dFGRS assigned names of each galaxy starting with "TGS" or "TGN". The names of the galaxies are as noted below (see section VII). The 2dF Galaxy Redshift Survey Final Data Release (June 2003) redshifts not in the previous release were added May 2005 (125,349 redshifts). Please note that there are over 4000 redshiftless entries, those had z=-9.000 in the data file from the 2dF webpage (in the file best.observations.idz from http://msowww.anu.edu.au/2dFGRS/ ). Review of about 100 charts from that sample showed galaxies, pairs or galaxy+star pair. They will need further observations to acquire redshifts.

The 6dF Galaxy Redshift Survey Data Release 1 issued March 2004 is now included. Of their original 52,048 spectra, the spectra with redshift measurement quality of 3 and 4 were chosen. There are 45,945 spectras meeting this criteria. From this sample, 31,083 galaxies from this survery were taken to put into ZCAT, the remaining were already in the catalog. The 6dF Galaxy Redshift Survey Data Release 2 issued May 2005 is now included with 23,390 new redshifts not include in DR1.

The FLAIR Shapley-Hydra (FLASH) redshift survey catalogue has been added to ZCAT. It contains 4613 galaxies.

A sample of 155,811 galaxies from the SDSS Data Release 1 is now included. More than 6200 galaxies of this survey were found in ZCAT and the SDSS magnitudes were added and/or velocities with errors were replaced ugriz (or combination) in the comment field means they are the SDSS u, g, r, i, z magnitudes. As of March 2005, 271,942 galaxies from SDSS Data Release 3 are also included.

Véron-Cetty and Véron's "A Catalogue of Quasars and Active Nuclei" 9th edition (source 4402) is included in ZCAT. Please note: magnitudes in ZCAT for these entries are noted as "V." However, they are not all V, please refer to the original publication for the correct magnitude source.

Finally, ZCAT also contains all of the published data for the galaxies in the CfA Redshift survey extension to m Zw = 15.5.

A variant of the whole CfA survey has been published by Falco et al. 1999. In addition, ZCAT contains (but without complete velocity information) all the Zwicky catalogue galaxies with m B < 15.5 in the CfA survey extensions.

Some of the small catalogs can be downloaded directly from the web. These are:

• nz40
• CfA2
• Updated Zwicky Catalogue
• LCRS
• 2dF
• SDSS (to get to the Space Telescope Science Institute's SDSS query web page, click here)

VII. Nomenclature, Comments, and Identifications

In this catalog, we rely as much as possible on good positions for proper identifcation of the galaxies listed. In clusters we also rely on published finding charts. In many cases, several authors have published velocities for the same galaxy with different ID's and discrepant positions. We are trying to standardize'' cluster id's by using Dressler's (1980) numbers in the comment field. We have done our best to remove such degeneracies, but know that some such duplicates still exist in the catalog. For good examples, one can look at the recent deconfusing'' of part of the NGC catalog and Zwicky catalogue by Thomson (1991, 1992). Other errors exist in catalogs and several other groups, Paturel et al. (1991) and the RC3 group (de Vaucouleurs et al. 1991) are working hard on correcting and documenting these. Harold Corwin has also produced a revised version of the NGC/IC catalog without many of the errors propagated through the RNGC (Sulentic and Tifft 1973) and NGC2000.0 (Sinnott 1988). We are incorporating these changes and corrections as rapidly as possible.

We have adopted the following priorities for nomenclature. (1) If a galaxy has an NGC or IC designation (Dreyer 1898, 1905), then that is its primary ZCAT name in A17 format with the first character N'' or I.'' (2) If a galaxy is in the Zwicky et al. catalog and not in the NGC or IC, then its designation is hhmmt±ddmm'' where hh = hours, mm = minutes, t = tenths of minutes of time, and dd = degrees. These coordinate names are taken directly from the Zwicky et al. catalog they are the coordinates minus the decimal point. Better coordinates from other sources may exist and may be found in the coordinate columns. Occasionally these improved coordinates contradict Zwicky's. The Zwicky name is a 10 character designation starting in the first character. (3) All other anonymous galaxies have names of the form hhmm±ddmm'' or Ahhmm±ddmm'' where ss = seconds and .s = tenths of seconds of time. Multiple components or multiple galaxies at nearly the same coordinates are designated by trailing letters such as hhmm±ddmmB'' where the B'' indicates the second object at that location. These addtional letter designations are usually added in order of right ascension. All coordinate names are made with the B1950.0 coordinates.

As of April 2004, ZCAT format names also include the 2MASS format names: hhmmssss ± ddmmsss or 2M hhmmssss ± ddmmsss where ssss (in right ascension) are the ss.ss without the decimal point and sss (declination) are ss.s without the decimal point. This name has the J2000 coordinates, as opposed to the ZCAT standard B1950 coordinates.

Many galaxies are listed in more than one catalog - it is not unusual for a galaxy to be in Zwicky, Nilson, the MCG, Markaryan's lists, etc. We have tried to include complete identifications from the UGC, ESO and Markaryan lists, but other identifcations are given for only a small fraction of the galaxies in the catalog. (Usually they have been entered when the measurers provide machine readable catalogs of their data with all the other names listed). When they exist, MCG designations will be found in the comment field and will generally look like Mnn-mm-ppp,'' where nn is the declination zone (negative zones are preceeded by -''), mm is the sky survey field in the zone running from 0h, and ppp is the galaxy number. ESO designations like ESOnnn-(I)Gmmm,'' where nnn is the ESO field number and mmm is the galaxy number on the plate, appear as nnnmmm in the same column as the UGC galaxies. We have not preserved the distinction between isolated (-G) and interacting (-IG) galaxies in ESO.

Even though all coordinates in this list are quoted to 0. s 1 and 1", the actual precision of positions for galaxies varies considerably. In general, coordinates from the Zwicky or Nilson catalogs are quoted to 1' and are precise to a little better than that. Coordinates from the MCG are often off by more than 2'. Galaxies from the above catalogs have coordinates quoted to only the nearest 1' and 6 s . Coordinates precise to 5"-6" have been taken from the RC2, from Spellman, Madore and Helou (1989), Dressler (1980), the ESO Catalog, the PGC, the RC3 and similar lists. We have endeavored to update and upgrade the coordinates in our lists as we can and also to remove confusion in crowded fields whenever we run across one. In some small number of cases, usually in the inner regions of clusters of galaxies, coordinates to this precision have been measured by us or our collaborators. A growing subset of galaxies in this catalog have coordinates measured to arc-second precision via measuring engine or plate scanner. This is particularly true for Seyfert galaxies, Markaryan galaxies, radio sources and other AGN, and also for data sets that come from multiple-fiber observations or new, deep small area surveys. Coordinates for IRAS sources extracted from the PSC are accurate to 20"-30", while strong sources that have been add-scanned will have more precise coordinates.

Many of the galaxies in the catalog (notably the ones in our own surveys) have spectra on line at CfA. These are indexed by either their Reduce File Number (RFN) from the early Reticon days, or by the date of observation (DDMMYY) with the new CCD spectrograph (FAST, built by Dan Fabricant) on the 1.5-m at Mt. Hopkins. For Reticon spectra, T designates those taken with the Tillinghast, M with the MMT, L refers to spectra reduced by us but taken by Steve Shectman at Las Capanas with their reticon system, and S refers to the SAAO Radcliffe 1.9-m telescope in South Africa.

Spetra on-line at CfA and available to the public (including all those in the CfA1 and CfA2 surveys and the UZC catalog) can be accessed at the CfA Telescope Data Center: Spectral Archive

IX. Other Notes

In a very few instances we have listed discrepant velocities (where two velocity measures disagree by more than double their combined external errors) found by other sources in the comment field - e.g. 1234(9) indicates a velocity of 1234 from source 9. Effort is being made to clear these up by remeasuring the galaxies.

In general, the velocities listed are the best available in terms of the quoted measurement errors and the reliablity of the source (some people persist in quoting errors considerably smaller than their true external errors). In only a few cases have we attempted to average high quality data to produce slightly better values. For almost all objects only one velocity is available. We do not think it appropriate to average low quality data with the newer, significantly better velocities available from 21-cm work and relatively high dispersion optical work. The purpose of this catalog is to be a complete list of galaxies with radial velocities for mapping and statistical studies. (Observers who feel that their velocities have been slighted for poorer velocities should contact J.P.H.) In several cases, we have omitted velocities derived from detailed HI maps of galaxies - primarily because a single dish measurement of sufficient quality is usually extant. The best quality optical and HI observations have velocity errors < 10 km sec -1 , which are well below the internal velocity dispersions of the galaxies. By definition, there is some question as to what such high precision'' velocities really mean relative to the centers of mass'' of galaxies.

Radial velocities greater than 100,000 km/sec are now included in ZCAT (previously located in ZBIG.DAT). Please note that the velocities are noted as redshifts in F7.4 format. Averaged radial velocities for Abell clusters will also be found in another catalog ABELL.DAT.

Some galaxies from zsource= 4559 (Cohen et al. 2000) have T type. These values were taken from a follow-up paper: van den Bergh, Sidney et al. 2001, AJ, 122, 611.

The cataloguers make no claim that this issue is complete or free from errors. All galaxies brighter than B(0)=13.2 have been included, even when no velocity is available, but otherwise there is no homogeneous magnitude limit to the catalog. Some galaxies are listed despite their lack of velocity. These are objects in complete samples that we are currently trying to observe, DDO dwarves without velocities, DOUBLE'' galaxies that have been split up for the production of North Zwicky Forty or galaxies from other interesting catalogs ( e.g. Binggeli et al.'s work on the Virgo Cluster dwarves - Ref 0109). Magnitudes on systems 0, 1 and 2 are more or less equivalent but other systems have not been well calibrated and are meant only to serve as a guide to the galaxy's brightness. Some of this data is unpublished, so authors are warned against making reference until this list is formally published.

Several frotran programs are available to make data cuts, searches and maps from our catalog data. Chief among them are

Msample is a program for taking coordinate, type and magnitude cuts in zcat format files. Circle is a program for doing cone searches. Map is a program for making Aitoff or Linear surface maps of data in zcat format.

We are constantly updating this list as new velocities, particularly better velocities, become available. We do not guarantee that what you see one day will be there the next!

A fairly large number of FORTRAN based utility programs now exists for sorting and searching in ZCAT including routines to do circle searches around annuli, cuts in galactic or equatorial coordinates, etc. See John Huchra for a more detailed description of these.

If errors are found, as some are sure to be in a compilation this large, please report them to the author (J.P.H.). If you wish to make additions, these will be gratefully accepted --- even more so if listings include accurate J2000 coordinates and heliocentric velocities and are transmitted electronically.

In this day and age, there is no need to present data in unusable formats, so we humbly request that all authors henceforth quote heliocentric velocities (or redshifts = (delta-lambda)/lambda), with their errors if available, and reasonably accurate J2000 coordinates in publications of data and that journal editors not accept papers presenting velocities in unusable forms. Presentation of velocities in undefined or poorly defined inertial reference frames ( e.g. Local Groupocentric or the microwave background frame) should be avoided at all costs. Editors please take note!

Special thanks are in order for all the people who have worked on this catalog over the years - Cathy Clemens, Dinah Danby, Bob Davis, Marc Davis, Ed Horine, Dave Latham, Jon Morse, Jim Peters, Suzanne Rapp, Michael Strauss, Susan Tokarz, John Tonry and Jeff Mader. Several other fearless catalogers of galaxies and galaxy properties, most notably Harold Corwin and Dave Burstein, deserve thanks if only for being the last of a dying breed, as well as for comments, corrections, classifications and data. Thanks are also extended to those other observers who have sent in redshifts (particularly those who send heliocentric z's and good coordinates!) and corrections like Tony Fairall, Ed Groth, Riccardo Giovanelli, Martha Haynes, George Helou, Lyle Hoffman, Nathan Krumm, Otto Richter, Ed Salpeter and Wayne Warren. Lastly, we would like to thank all those people who have been willing to send us electronic copies of extended catalogs these have certainly made our jobs significantly easier as well as reducing the probability of error on entry. This work has been supported by the Smithsonian Institution and by NASA grant NAGW-201. Some computer support has also been provided by the Digital Equipment Corporation.

IAU Working Group on Galaxy Redshifts
Harvard-Smithsonian Center for Astrophysics
60 Garden Street MS 20
Cambridge, MA 02138-1516
United States
(617) 495-7375

If you are interested in printing this document in its entirety, it is available as a postscript or PDF file:

Full text (except for references & tables) [ps] [pdf]
References & tables [ps] [pdf]
zsource [tex] [ps] [pdf] (not included in this web page)

Arp, H. C. 1966, Atlas of Peculiar Galaxies (Pasadena: Caltech). See also ApJS, 14, 1

Berger, J. & Fringant, A.-M., 1980, A&AS, 39, 39. (Faint Blue obj. catalogue)

Berger, J. & Fringant, A.-M., 1984, A&AS, 58, 565. (Faint Blue obj. catalogue)

Bothun, G.. Beers, T., Mould, J. & Huchra, J. 1986, ApJ, 308, 510.

Bothun, G. and Cornell, M. 1990, AJ, 99, 1004.

Bothun, G. & Schommer, R. 1982, ApJL, 255, L23.

Burakowska, M. & Rudnicki, K. 1974, Acta Cosmologica 2, 7.

Corwin, H. 1992, revised NGC catalog, private communication.

Cotton, W., Condon, J. & Arbizzani, E. 1999, ApJS, 125, 409.

da Costa, L., Pellegrini, P., Sargent, W. L. W., Tonry, J., Davis, M., Meiksin, A. , Latham, D. ,
Menzies, J.W. & Coulson, J.A. 1988, ApJ, 327, 544. (Southern Sky Redshift Survey)

da Costa, L., Willmer, C., Pellegrini, P., Chaves, O., Rité, C., Maia, M., Geller, M., Latham, D.,
Kurtz, D., Huchra, J., Ramella, M., Fairall, A., Smith, C., & Lipari, S. 1998, AJ, 116, 1.

de Vaucouleurs, G. 1959, in Handbuch der Physik, Bd. LIII, Astrophysik IV: Sternsysteme,
ed. S. Flüge (Berlin: Springer-Verlag), 275.

de Vaucouleurs, G. 1963, ApJS, 8, 31.

de Vaucouleurs, G. & de Vaucouleurs, A. 1964, Reference Catalogue of Bright Galaxies
(Austin: University of Texas Press)

de Vaucouleurs, G., de Vaucouleurs, A. & Corwin, H. 1976, Second Reference Catalogue of
Bright Galaxies (Austin: University of Texas Press)

de Vaucouleurs, G., de Vaucouleurs, A., Corwin, H., Buta, R., Paturel, G. & Fouqué, P. 1991,
Third Reference Catalogue of Bright Galaxies, Vols. I-III (Berlin: Springer-Verlag)

Dressler, A. 1980, ApJS, 42, 565. (Clusters)

Dreyer, J. 1888, MNRAS, 49, 1. (NGC)

Dreyer, J. 1895, MNRAS, 51, 185. (IC1)

Dreyer, J. 1908, MNRAS, 59, 105. (IC2)

Fairall, A. 1992, Obs, 112, 286.

Fairall, A. 1998, Large Scale Structure in the Universe (Cambridge: Cambridge)

Falco, E.E., Kurtz, M.J., Geller, M.J., Huchra, J.P., Peters, J., Berlind, P., Mink, D.J., Tokarz, S.P.,
& Elwell, B. 1999, PASP, 111, 438. (The Updated Zwicky Catalog)

Fisher, K., Huchra, J., Strauss, M., Davis, M., Yahil, A. & Schlegel, D. 1995, ApJS, 100, 69.

Giovanelli,R., & Haynes, M.P. 1984, AJ, 89, 1.

Gisler, G. & Friel, E. 1979, Index of Galaxy Spectra (Tucson: Pachart)

Hewett, A., & Burbidge, G. 1993, ApJS, 87, 451.

Huchra, J., Davis, M., Latham, D. & Tonry, J. 1983, ApJS, 52, 89.

Huchra, J., Geller, M., de Lapparent V., & Corwin, H. 1990, ApJS, 72, 433.

Huchra, J., Geller, M., & Corwin, H. 1995, ApJS, 99, 391.

Huchra, J., Vogeley, M., & Geller, M. 1999, ApJS, 121, 287. (CfA2 SGC)

Humason, M., Mayall, N. U., & Sandage, A. 1956, AJ, 61, 97.

Kron, G., & Shane, C. D. 1976, Ap&SS, 39, 401.

Lauberts, A. 1982, The ESO-Uppsala Survey of the ESO(b) Atlas (Garching: European
Southern Observatory)

Lewis, B. M. 1983, AJ, 88, 1695.

Mattig, W. 1959, Astr. Nachr., 285, 1.

Nilson, P. 1973, Uppsala General Catalogue of Galaxies, Ann. Uppsala Astron. Obs. Band 6,
Ser. V:A. Vol. 1 (Uppsala: Astronomiska Observatorium)

Palumbo, G., Tanzella-Nitti, G., & Vettolani, G. 1983, Catalogue of Radial Velocities of Galaxies
(New York: Gordon & Breach)

Paturel, G., Fouqué, P., Bottinelli, L., & Gougenheim, L. 1989, Catalogue of Principal Galaxies (PGC)
(Lyon: Observatoire de Lyon)

Paturel, G., Petit, C., Kogoshvili, N., Dubois, P., Bottinelli, L., Fouqué, P., Garnier, R., &
Gouguenheim, L. 1991, A&AS, 91, 371.

Sandage, A., & Tammann, G. 1981, A Revised Shapley-Ames Catalogue of Bright Galaxies
(Washington: Carnegie Institution of Washington)

Sinnott, R. 1988, The complete new general catalogue and index catalogues of nebulae
and star clusters by J.L.E. Dreyer(Cambridge: Sky Publishing) (NGC 2000.0)

Spellman, K., Madore, B., & Helou, G. 1989, PASP, 101, 360.

Strauss, M., Huchra, J., Davis, M., Yahil, A., Fisher, K., & Tonry. J. 1992, ApJS, 83, 29.

Sulentic, J., & Tifft, W. 1973, The Revised New General Catalogue of Astronomical Objects
(Tucson: U. of Arizona Press)

Thomson, M. J. 1991, QJRAS, 32, 17.

Thomson, M. J. 1992, QJRAS, 33, 59.

Tifft, W. G. 1990, ApJS, 73, 603.

Tully, R. B., & Fisher, R. F. 1987, Catalogue of Nearby Galaxies (Cambridge: Cambridge University
Press)

Vorontsov-Velyaminov, B. A. 1959, Atlas and Catalog of Interacting Galaxies, Sternberg
Institute, Moscow State University.

Vorontsov-Velyaminov, B. A., Krasnogorska, A., & Arihpova, V. 1962-68 Morphological Catalogue
of Galaxies (Moscow: Moscow State University)

Vorontsov-Velyaminov, B. A. 1977, A&AS, 28,1.Zwicky, F. 1971, Catalogue of Selected Compact Galaxies and of Post-Eruptive Galaxies
(Guemligen: Zwicky)

Zwicky, F., Sargent, W. L. W., & Kowal, C. 1975, AJ, 80, 545.

Zwicky, F., Herzog, E., Wild, P., Karpowicz, M. & Kowal, C. 1961-68, Catalogue of Galaxies & of
Clusters of Galaxies (Pasadena: California Institute of Technology)

## Where to find spectra from Las Campanas Redshift Survey? - Astronomy

Website
LDSS-3 is an optical imager and (multi-) slit spectrograph on the 6.5m Magellan II (Clay) telescope at Las Campanas Observatory. The instrument optics were designed to deliver very high throughput at red optical wavelengths. However, the current detector in the instrument does not take full advantage of this capability because its quantum efficiency falls off dramatically beyond 700 nm. We are currently working to upgrade the LDSS-3 camera with a state-of-the-art red-sensitive CCD. The detector we will use is one of the spare CCDs that were manufactured for the DECam. At 1000 nm, these CCDs have quantum efficiency of 50%, whereas the current LDSS-3 detector has a quantum efficiency of only 5%. The total spectroscopic throughput for LDSS-3 with the new detector as compared to the current detector and to IMACS, which is a similar instrument on Magellan I, is given below in the Figure. In addition to pure efficiency, the new detector will have reduced fringing at red wavelengths compared to the old chip due to its thickness and QE, and it will enable macroscopic nod-and-shuffle.

We will build a complete CCD system (housing, dewar, electronics) for the new detector that can be installed in place of the old system. This project will heavily leverage the knowledge and hardware developed for DECam. In particular, we will use the DECam optimized read-out electronics system that delivers only 7 electrons read-noise for a 17 seconds full-frame (2k x 4k), unbinned read.

Our motivation for performing this upgrade is to make LDSS-3 more useful for ground-based transit spectroscopy observations. Water vapor is one of the most important diagnostics of the structure and composition of exoplanet atmospheres. The spectral signatures of this molecule are difficult to observe from the ground due to its prevalence in Earth's atmosphere. However, water vapor in exoplanet atmospheres can be observed from the ground in the wavelength range 900 -- 1000 nm because the corresponding telluric features are relatively weak. Transit spectroscopy observations using our multi-object technique are typically photon-limited at the 1e-4 level of precision. Therefore, instrument efficiency, even on large telescopes, is critical for these measurements. LDSS-3 with the new detector will become a powerful instrument for revealing the nature of exoplanet atmospheres.

The proposed detector upgrade will also finally realize the original intent of the LDSS-2 to LDSS-3 upgrade project, which was to facilitate galaxy spectroscopy at redshifts beyond z=1. In particular, the upgraded LDSS-3 will become a powerful instrument for observations of early-type galaxies at these redshifts this will enable research on galaxy clusters in particular. With the current system, the G-band (which usefully defines the red edge of the spectral region which must be observed to robustly deduce absorption-line redshifts in clusters) can easily be observed to about z = 0.92, and the [OII] 3727 Ang doublet to z = 1.22. These redshifts correlate well with the difficulty of observing such galaxies with redshift - currently at z 1.2 observations rapidly become extremely difficult. The upgraded system will move these performance goalposts to from z = 0.92 to z = 1.35, and from z = 1.22 to z = 1.72, opening up a critical portion of redshift space that is currently difficult to address. This will be true whether the targets are cluster galaxies, or a more general population.

Also, note that LDSS-3 has been used extensively for single-object longslit spectroscopy of transients - both GRBs and supernovae. In particular, for the most distant GRBs this will move the observable redshift limit of high-z GRB dropouts to z = 6.7 from z = 5.3, where we have defined the limit using the wavelength of Ly-alpha + 100 Ang as a fiducial similar improvements are of course realized for any ultra-distant galaxy spectroscopy as well. A critical task for the Dark Energy Survey soon to start at the CTIO 4m will be the spectral typing of at least a subset of distant SNe. The most useful distinguishing feature is the SiII line seen in type Ia SNe. Robust identification of this feature requires rest frame spectra to approximately 4300 Ang. The improvement from this upgrade is thus very similar to the improvement above for absorption line galaxy studies: the redshift region where this is straightforward moves from z