J/AJ/131/1891 Photometric survey of MS 1054-03 field (Foerster-Schreiber+, 2006)
Faint infrared extragalactic survey: data and source catalog of the MS 1054-03 field. Foerster-Schreiber N.M., Franx M., Labbe I., Rudnick G., Van Dokkum P.G., Illingworth G.D., Kuijken K., Moorwood A.F.M., Rix H.-W., Roettgering H., Van Der Werf P. <Astron. J., 131, 1891-1913 (2006)> =2006AJ....131.1891F (SIMBAD/NED BibCode)
ADC_Keywords: Surveys ; Clusters, galaxy ; Photometry, infrared ; Morphology Keywords: cosmology: observations - galaxies: evolution - infrared: galaxies Abstract: We present deep near-infrared Js-, H-, and Ks-band imaging of a field around MS 1054-03, a massive cluster at z=0.83. The observations were carried out with the ISAAC instrument at the ESO Very Large Telescope (VLT) as part of the Faint Infrared Extragalactic Survey (FIRES). The total integration time amounts to 25.9hr in Js, 24.4hr in H, and 26.5hr in Ks, divided nearly equally between four pointings covering 5.5'x5.3'. The 3 total limiting AB magnitudes for point sources from the shallowest to the deepest pointing are Jtots,AB=26.0-26.2, HtotAB=25.5-25.8, and Ktots,AB=25.3-25.7mag. The effective spatial resolution of the co-added images has FWHM=0.48", 0.46", and 0.52" in Js, H, and Ks, respectively. We complemented the ISAAC data with deep optical imaging using existing Hubble Space Telescope WFPC2 mosaics through the F606W and F814W filters and additional U-, B-, and V-band observations we obtained with the VLT FORS1 instrument. We constructed a Ks-band-limited multicolor source catalog down to Ktots,AB∼25mag (∼5σ for point sources). The catalog contains 1858 objects, of which 1663 have eight-band photometry. We describe the observations, data reduction, source detection, and photometric measurements method. We also present the number counts, color distributions, and photometric redshifts zph of the catalog sources. We find that our Ks-band counts at the faint end 22≲Ks,AB≲25, with slope dlogN/dm=0.20, lie at the flatter end of published counts in other deep fields and are consistent with those we derived previously in the Hubble Deep Field-South (HDF-S), the other FIRES field. Spectroscopic redshifts zsp are available for ∼330 sources in the MS 1054-03 field; comparison between zph and zsp shows very good agreement, with <|zsp-zph|/(1+zsp)≥0.078. The MS 1054-03 field observations complement our HDF-S data set with a nearly 5 times larger area at ∼0.7mag brighter limits, providing more robust statistics for the slightly brighter source populations. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file catalog.dat 477 1858 Main catalogue parameters (v3.1) zph.dat 33 1858 Photometric redshifts
See also: http://www.strw.leidenuniv.nl/~fires/data/ms1054/data/ : FIRES MS1054-03 Data Archive (Faint InfraRed Extragalactic Survey) J/ApJS/157/228 : Catalog of galaxy morphology in 4 clusters (Saintonge+ 2005) J/ApJ/644/30 : HST Observations of 2 high-z clusters (Blakeslee+ 2006) J/ApJ/661/750 : Photometry and spectroscopy of MS 1054-03 members (Tran+ 2007) Byte-by-byte Description of file: catalog.dat
Bytes Format Units Label Explanations
1- 4 I4 --- [FFL2006] Sequential number 6- 12 F7.2 pix xpos X position 14- 20 F7.2 pix ypos Y position 22- 23 I2 h RAh Right ascension (J2000) 24 A1 --- --- [:] 25- 26 I2 min RAm Right ascension (J2000) 27 A1 --- --- [:] 28- 33 F6.3 s RAs Right ascension (J2000) 35 A1 --- DE- Declination sign (J2000) 36- 37 I2 deg DEd Declination (J2000) 38 A1 --- --- [:] 39- 40 I2 arcmin DEm Declination (J2000) 41 A1 --- --- [:] 42- 46 F5.2 arcsec DEs Declination (J2000) 48- 55 F8.4 uJy Ucol ?=-99.0000 Flux in U colour aperture 57- 64 F8.4 uJy e_Ucol ?=-99.0000 rms uncertainty on fcolU 66- 73 F8.4 uJy Bcol ?=-99.0000 Flux in B colour aperture 75- 82 F8.4 uJy e_Bcol ?=-99.0000 rms uncertainty on fcolB 84- 91 F8.4 uJy Vcol ?=-99.0000 Flux in V colour aperture 93-100 F8.4 uJy e_Vcol ?=-99.0000 rms uncertainty on fcolV 102-109 F8.4 uJy V606col ?=-99.0000 Flux in V606 colour aperture 111-118 F8.4 uJy e_V606col ?=-99.0000 rms uncertainty on fcolV606 120-127 F8.4 uJy I814col ?=-99.0000 Flux in I814 colour aperture 129-136 F8.4 uJy e_I814col ?=-99.0000 rms uncertainty on fcolI814 138-146 F9.4 uJy Jcol ?=-99.0000 Flux in Js colour aperture 148-155 F8.4 uJy e_Jcol ?=-99.0000 rms uncertainty on fcolJs 157-165 F9.4 uJy Hcol ?=-99.0000 Flux in H colour aperture 167-174 F8.4 uJy e_Hcol ?=-99.0000 rms uncertainty on fcolH 176-184 F9.4 uJy Kcol ?=-99.0000 Flux in Ks colour aperture 186-193 F8.4 uJy e_Kcol ?=-99.0000 rms uncertainty on fcolKs 195-203 F9.4 uJy Ktot ?=-99.0000 Ks-band flux in total aperture (1) 205-212 F8.4 uJy e_Ktot ?=-99.0000 rms uncertainty on fcolKs 214-221 F8.4 uJy Uiso ?=-99.0000 Flux in U isophotal aperture 223-230 F8.4 uJy e_Uiso ?=-99.0000 rms uncertainty in fisoU 232-239 F8.4 uJy Biso ?=-99.0000 Flux in B isophotal aperture 241-248 F8.4 uJy e_Biso ?=-99.0000 rms uncertainty in fisoB 250-257 F8.4 uJy Viso ?=-99.0000 Flux in V isophotal aperture 259-266 F8.4 uJy e_Viso ?=-99.0000 rms uncertainty in fisoV 268-275 F8.4 uJy V606iso ?=-99.0000 Flux in V606 isophotal aperture 277-284 F8.4 uJy e_V606iso ?=-99.0000 rms uncertainty in fisoV606 286-293 F8.4 uJy I814iso ?=-99.0000 Flux in I814 isophotal aperture 295-302 F8.4 uJy e_I814iso ?=-99.0000 rms uncertainty in fisoI814 304-312 F9.4 uJy Jiso ?=-99.0000 Flux in Js isophotal aperture 314-321 F8.4 uJy e_Jiso ?=-99.0000 rms uncertainty in fisoJs 323-331 F9.4 uJy Hiso ?=-99.0000 Flux in H isophotal aperture 333-340 F8.4 uJy e_Hiso ?=-99.0000 rms uncertainty in fisoH 342-350 F9.4 uJy Kiso ?=-99.0000 Flux in Ks isophotal aperture 352-359 F8.4 uJy e_Kiso ?=-99.0000 rms uncertainty in fisoKs 361-369 F9.4 uJy Kauto ?=-99.0000 Ks-band flux in the Kron-like autoscaling aperture (2) 371-378 F8.4 uJy e_Kauto ?=-99.0000 rms uncertainty on fautoKs 380 I1 --- apcol [1/4] Type of aperture used for measuring the colour flux (3) 382 I1 --- aptot [1/2] Type of aperture used for measuring the total Ks-band flux (4) 384-388 F5.3 --- apcorr Scaling factor corresponding to the aperture correction applied to the Ks-band flux measured in the total aperture in order to estimate the total integrated flux. 390-394 F5.2 pix rcol Circularized radii used for colour fluxes (5) 396-400 F5.2 pix rtot Circularized radii used for total fluxes (5) 402-409 F8.2 pix2 Aiso Area of the aperture enclosed within the mu(Ks,AB)=24.8mag/arcsec2 isophote (6) 411-418 F8.2 pix2 Aauto Area of the Kron-like autoscaling aperture (6) 420-424 F5.2 pix FWHMKs FWHM of source from Ks-band detection map (7) 426-431 F6.2 pix FWHMI FWHM of source from I814-band map (7) 433-436 F4.2 --- w_Ucol 438-441 F4.2 --- w_Bcol Average of the effective weight in B band (8) 443-446 F4.2 --- w_Vcol Average of the effective weight in V band (8) 448-451 F4.2 --- w_V606col Average of the effective weight in V606 band (8) 453-456 F4.2 --- w_I814col Average of the effective weight in I814 band (8) 458-461 F4.2 --- w_Jcol Average of the effective weight in Js band (8) 463-466 F4.2 --- w_Hcol Average of the effective weight in H band (8) 468-471 F4.2 --- w_Kcol Average of the effective weight in Ks band (8) 473 I1 --- bias [0/1] Bias flag (9) 475 I1 --- blended [0/1] Blend flag (10) 477 I1 --- star [0/1] Star flag (11)
Note (1): Ks-band flux in the total aperture scaled by the aperture correction. Note (2): Ks-band flux in the Kron-like autoscaling aperture based on the light distribution in the Ks-band detection map (the MAG_AUTO computed by SExtractor). Note (3): Aperture for colour flux flag as follows: 1 = minimum circular aperture considered with diameter d=1.0 arcsec used whenever the isophotal aperture is smaller. 2 = maximum circular aperture considered with diameter d=2.0 arcsec used whenever the isophotal aperture is larger. 3 = isophotal aperture defined by the surface brightness threshold of mu(Ks,AB)=24.8mag/arcsec2 in the Ks-band detection map. 4 = circular aperture with diameter d=sqrt(Aiso/PI)/s where s=1.4 is the aperture reduction factor applied for blended sources. Note (4): Aperture for total Ks-band flux flag as follows: 1 = Kron-like autoscaling aperture based on the light distribution in the Ks-band detection map. 2 = Colour aperture used in the case of blended sources. Note (5): Circularized radii r=sqrt(A/PI) from the area of the apertures used to measure the colour and total fluxes. Units are pixels in the rectified images. Note (6): Units are squared pixels in the rectified images. Note (7): FWHM of sources assuming a Gaussian profile from the Ks-band detection map, and similarly from the non-PSF-matched I814 map filtered with a kernel approximating the PSF with FWHM=0.22arcsec. Units are pixels in the rectified images. Note (8): Average of the effective weight in each of the U, B, V, V606, I814, Js, H, Ks bandpasses within the point-source aperture for the PSF-matched set of maps (d=1.5xFWHM=1.0arcsec). The weights are normalized to a maximum of 1 over the maps. Note (9): 1 if the Kron-like autoscaling aperture contains >10% of bad pixels or if the flux measurement within this aperture is affected by neighbouring sources as determined from the light distribution in the Ks-band detection map. Note (10): 1 if the source overlaps with adjacent objects based on the Ks-band detection map. Note (11): 1 if the source satisfies all the star identification criteria (see Section 6 of the paper).
Byte-by-byte Description of file: zph.dat
Bytes Format Units Label Explanations
3- 6 I4 --- [FFL2006] Sequential number 11- 15 F5.3 --- zph Photometric redshift 19- 24 F6.3 --- e_zph Associated 68% confidence intervals (lower limit) (1) 28- 33 F6.3 --- E_zph Associated 68% confidence intervals (upper limit) (1)
Note (1): Associated 68% confidence intervals (given as zph, -zphl68/+zphu68) derived as described by Rudnick et al. 2001, Cat. J/AJ/122/2205 and Rudnick et al. (2003ApJ...599..847R).
History: Copied at http://www.strw.leidenuniv.nl/~fires/
(End) Patricia Vannier [CDS] 21-Sep-2007
|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|