J/AJ/128/1558 NOAO Fundamental Plane Survey (Smith+, 2004)
NOAO Fundamental Plane Survey. I. Survey design, redshifts, and velocity dispersion data. Smith R.J., Hudson M.J., Nelan J.E., Moore S.A.W., Quinney S.J., Wegner G.A., Lucey J.R., Davies R.L., Malecki J.J., Schade D., Suntzeff N.B. <Astron. J., 128, 1558-1569 (2004)> =2004AJ....128.1558S
ADC_Keywords: Clusters, galaxy ; Redshifts ; Velocity dispersion Keywords: galaxies: clusters: general - galaxies: distances and redshifts - galaxies: elliptical and lenticular, cD - surveys Abstract: We introduce the NOAO Fundamental Plane Survey (NFPS), a wide-field imaging/spectroscopic study of rich, low-redshift galaxy clusters. The survey targets X-ray-selected clusters at 0.010<z<0.067, distributed over the whole sky, with imaging and spectroscopic observations obtained for 93 clusters. This data set will be used in investigations of galaxy properties in the cluster environment and of large-scale velocity fields through the fundamental plane. In this paper, we present details of the cluster sample construction and the strategies employed to select early-type galaxy samples for spectroscopy. Details of the spectroscopic observations are reported. From observations of 5479 red galaxies, we present redshift measurements for 5388 objects and internal velocity dispersions for 4131. The velocity dispersions have a median estimated error ∼7%. The NFPS has ∼15% overlap with previously published velocity dispersion data sets. Comparisons to these external catalogs are presented and indicate typical external errors of ∼8%. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 87 114 The NFPS Cluster Sample table5.dat 85 5479 Merged Spectroscopic Data for NFPS Galaxies
See also: IX/10 : ROSAT All-Sky Bright Source Catalogue (1RXS) (Voges+ 1999) IX/29 : ROSAT All-Sky Survey Faint Source Catalog (Voges+ 2000) J/MNRAS/301/881 : The ROSAT brightest cluster sample - I. (Ebeling+, 1998) J/MNRAS/281/799 : XBACs, the sample (Ebeling+, 1996) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 8 A8 --- Cluster Cluster name 10- 11 I2 h RAh Hour of right ascension (J2000) (1) 13- 14 I2 min RAm Minute of right ascension (J2000) (1) 16- 19 F4.1 s RAs Second of right ascension (J2000) (1) 21 A1 --- DE- Sign of the Declination (J2000) (1) 22- 23 I2 deg DEd Degree of declination (J2000) (1) 25- 26 I2 arcmin DEm Arcminute of declination (J2000) (1) 28- 29 I2 arcsec DEs Arcsecond of declination (J2000) (1) 31- 36 F6.2 deg GLON Galactic longitude 38- 43 F6.2 deg GLAT Galactic latitude 45- 46 A2 --- Type Center type (2) 48- 52 I5 km/s cz Recession velocity in the CMB frame (3) 54- 56 I3 km/s e_cz ? Error in cz 58- 60 I3 --- o_cz ? Number of galaxy redshifts used in cz 62- 67 F6.2 fW/m2 FX ? ROSAT 0.1-2.4keV bandpass flux in units of 10-12ergs/s/cm2 (4) 69- 72 F4.2 10+37W LX ? ROSAT 0.1-2.4keV bandpass luminosity in units of 10+44ergs/s (4) 74 A1 --- Sample [ABC] Selection subsample to which the cluster belongs (5) 76- 78 A3 --- Cat X-ray catalog from which the cluster was selected (6) 80- 82 I3 --- Num ? Number of member galaxies with velocity dispersion measurements in this paper 84- 86 A3 --- Source Source of NFPS spectra (7)
Note (1): The coordinates are those of the cluster center, as judged from visual examination of Digitized Sky Survey and ROSAT data. Note (2): Center type is defined as follows: DX = Coordinates of a dominant galaxy coincident (or nearly so) with X-ray peak; GX = Coordinates derived from average of several prominent galaxies coincident (or nearly so) with X-ray peak; XP = Coordinates of an X-ray emission peak, without a clear dominant galaxy; XC = Coordinates from approximate centroid of large-scale X-ray emission, ignoring local peaks. Note (3): The cluster redshifts are derived from our own spectroscopic data where possible, otherwise they are from BCS/XBACS. Where our data are used, we give the error and number of galaxy redshifts. Note (4): Fluxes corrected according to Hogg & Turner (1998PASP..110..727H) to reflect the systematic bias affecting low signal-to-noise ratio (S/N) object detection. Note (5): Selection subsample to which the cluster belongs, defined as follows: A = The A subsample is limited to zCMB<0.06 in order to reduce the number of the most distant clusters, for which morphological analysis requires excellent image quality. The A clusters are further selected by X-ray luminosity. We impose luminosity cuts: LX,c>5.0x1043ergs/s for 0.04<z<0.06 and LX,c>2.0x1043ergs/s for z<0.04. The final A subsample is then composed of two overlapping subsets, each volume-limited in X-ray luminosity. Note that these redshift-luminosity limits correspond to a minimum flux of fX,c∼6x10-12ergs/cm2/s, comfortably above the BCS/XBACs flux limits. B = Clusters not belonging to the A subsample, but making the original selection cuts, form the "B" subsample. C = A few clusters that do not meet the overall selection criteria nonetheless have NFPS data; these are retained as a "C" subsample. Note (6): The X-ray catalog from which the cluster was selected from is defined as follows: BCS = Brightest cluster sample (Cat. J/MNRAS/301/881); XBA = X-ray brightest Abell clusters (Cat. J/MNRAS/281/799). Note (7): Source of NFPS spectra, defined as follows: W = WIYN (Wisconsin Iowa Yale NOAO Observatory); C = CTIO (Cerro Tololo Inter-American Observatory).
Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
1- 3 A3 --- --- [NFP] 4- 19 A16 --- NFP Galaxy identification (NFP JHHMMSS.s+DMMSS) 21- 29 F9.5 deg RAdeg Right ascension in decimal degrees (J2000) (1) 31- 39 F9.5 deg DEdeg Declination in decimal degrees (J2000) (1) 41 I1 --- o_cz ? Number of merged individual measurements in cz 43- 47 I5 km/s cz ? Heliocentric redshift 49- 51 I3 km/s e_cz ? Error in cz 53- 55 I3 --- S/N-cz ? Effective total signal-to-noise ratio (per Angstroem) in cz 57 I1 --- o_logS ? Number of merged individual measurements in log S (2) 59- 64 F6.4 [km/s] logS ? Logarithm of the velocity dispersion (3) 66- 71 F6.4 [km/s] e_logS ? Error n logS 73- 75 I3 --- S/N-logS ? Effective total signal-to-noise ratio (per Angstroem) in logS 77- 84 A8 --- Cluster Cluster to which the galaxy is assigned (4)
Note (1): Coordinates are expected to be accurate to ≲1". Note (2): Only spectra with SN-logS>15 are allowed to contribute to the merged data, so in some cases SN-logS>SN-cz. Note (3): Values are as observed through a 2" diameter fiber; no aperture corrections have been applied. Note (4): Cluster to which the galaxy is assigned by the algorithm discussed in the text. Missing data in this column indicate either that no redshift measurement was achieved or that the galaxy is not assigned to any cluster. Stars are indicated by the entry "star".
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Marianne Brouty [CDS] 18-Apr-2005
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