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J/ApJ/727/1         IRAC/MUSYC SIMPLE survey                 (Damen+, 2011)

The SIMPLE survey: observations, reduction, and catalog. Damen M., Labbe I., Van Dokkum P.G., Franx M., Taylor E.N., Brandt W.N., Dickinson M., Gawiser E., Illingworth G.D., Kriek M., Marchesini D., Muzzin A., Papovich C., Rix H.-W. <Astrophys. J., 727, 1 (2011)> =2011ApJ...727....1D
ADC_Keywords: Surveys ; Galaxies, photometry; Photometry, UBVRI ; Photometry, infrared ; Morphology Keywords: catalogs - galaxies: evolution - galaxies: photometry - infrared: galaxies Abstract: We present the Spitzer IRAC/MUSYC Public Legacy Survey in the Extended CDF-South (SIMPLE), which consists of deep IRAC observations covering the ∼1600arcmin2 area surrounding GOODS-S. The limiting magnitudes of the SIMPLE IRAC mosaics typically are 23.8, 23.6, 21.9, and 21.7, at 3.6um, 4.5um, 5.8um, and 8.0um, respectively (5σ total point source magnitudes in AB). The SIMPLE IRAC images are combined with the 10'x15' GOODS IRAC mosaics in the center. We give detailed descriptions of the observations, data reduction, and properties of the final images, as well as the detection and photometry methods used to build a catalog. Using published optical and near-infrared data from the Multiwavelength Survey by Yale-Chile (MUSYC), we construct an IRAC-selected catalog, containing photometry in UBVRIz'JHK, [3.6um], [4.5um], [5.8um], and [8.0um]. The catalog contains 43,782 sources with S/N>5 at 3.6um, 19,993 of which have 13-band photometry. We compare this catalog to the publicly available MUSYC and FIREWORKS catalogs and discuss the differences. Using a high signal-to-noise sub-sample of 3391 sources with ([3.6]+[4.5])/2<21.2, we investigate the star formation rate history of massive galaxies out to z∼1.8. We find that at z∼1.8 at least 30±7% of the most massive galaxies (M*>1011M) are passively evolving, in agreement with earlier results from surveys covering less area. Description: The MUSYC E-CDFS dataset is a conglomeration of existing public and original observations, kindly made available to us by Edward Taylor. The E-CDFS IRAC data is based on the V1.0 release of the mosaics. For more information on the images and the reduction, see the documentation on the official release page: http://data.spitzer.caltech.edu/popular/simple/20070601_enhanced/ SExtracor is used in double mode on a combined image of IRAC's deepest bands, 3.6 and 4.5um. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file simple.dat 823 61233 IRAC detected UBVRIzJHK + 3.6,4.5,5.8,8.0 micron catalog of the Extended Chandra Deep Field South version 3.0, 11/11/2010
See also: J/ApJS/162/1 : MUSYC: optical source catalog (Gawiser+, 2006) J/AJ/134/1103 : MUSYC deep near-infrared imaging (Quadri+, 2007) Byte-by-byte Description of file: simple.dat
Bytes Format Units Label Explanations
1- 5 I5 --- Seq Detection number 7- 16 F10.5 pix Xpos Pixel position on MUSYC-BVR astrometric grid 18- 27 F10.5 pix Ypos Pixel position on MUSYC-BVR astrometric grid 29- 37 F9.6 deg RAdeg Right ascension in decimal degrees (J2000) 39- 48 F10.6 deg DEdeg Declination in decimal degrees (J2000) 50- 63 E14.8 363uJy FU ?=-999. Color aperture flux in band U (2) (1) 65- 78 E14.8 363uJy FB ?=-999. Color aperture flux in band B (1) (2) 80- 93 E14.8 363uJy FV ?=-999. Color aperture flux in band V (1) (2) 95-108 E14.8 363uJy FR ?=-999. Color aperture flux in band R (1) (2) 110-123 E14.8 363uJy FI ?=-999. Color aperture flux in band I (1) (2) 125-138 E14.8 363uJy Fz ?=-999. Color aperture flux in band z (1) (2) 140-153 E14.8 363uJy FJ ?=-999. Color aperture flux in band J (1) (2) 155-168 E14.8 363uJy FH ?=-999. Color aperture flux in band H (1) (2) 170-187 F18.11 363uJy FK ?=-999. Color aperture flux in band K (1) (2) 189-205 F17.11 363uJy F3.6 ?=-999. Color aperture flux in band IRAC 1 (3.6um) (1) (2) 207-223 F17.11 363uJy F4.5 ?=-999. Color aperture flux in band IRAC 2 (4.5um) (1) (2) 225-242 F18.11 363uJy F5.8 ?=-999. Color aperture flux in band IRAC 3 (5.8um) (1) (2) 244-261 F18.11 363uJy F8.0 ?=-999. Color aperture flux in band IRAC 4 (8.0um) (1) (2) 263-273 F11.8 363uJy e_FU ?=-1. rms uncertainty on FU (3) 275-285 F11.8 363uJy e_FB ?=-1. rms uncertainty on FB (3) 287-297 F11.8 363uJy e_FV ?=-1. rms uncertainty on FV (3) 299-309 F11.8 363uJy e_FR ?=-1. rms uncertainty on FR (3) 311-321 F11.8 363uJy e_FI ?=-1. rms uncertainty on FI (3) 323-332 F10.7 363uJy e_Fz ?=-1. rms uncertainty on Fz (3) 334-343 F10.7 363uJy e_FJ ?=-1. rms uncertainty on FJ (3) 345-355 F11.8 363uJy e_FH ?=-1. rms uncertainty on FH (3) 357-367 F11.7 363uJy e_FK ?=-1. rms uncertainty on FK (3) 369-379 F11.8 363uJy e_F3.6 ?=-1. rms uncertainty on F3.6 (3) (4) 381-391 F11.8 363uJy e_F4.5 ?=-1. rms uncertainty on F4.5 (3) (4) 393-403 F11.7 363uJy e_F5.8 ?=-1. rms uncertainty on F5.8 (3) (4) 405-416 F12.8 363uJy e_F8.0 ?=-1. rms uncertainty on F8.0 (3) (4) 418-431 E14.9 363uJy FKt ?=-999. Total flux in band K (1) (5) 433-450 F18.11 363uJy F3.6t ?=-999. Total flux in band IRAC 1 (1) (5) 452-469 F18.11 363uJy F4.5t ?=-999. Total flux in band IRAC 2 (1) (5) 471-489 F19.11 363uJy F5.8t ?=-999. Total flux in band IRAC 3 (1) (5) 491-509 F19.11 363uJy F8.0t ?=-999. Total flux in band IRAC 4 (1) (5) 511-524 E14.9 363uJy e_FKt [-106999,]?=-1. rms uncertainty on FKt 526-537 F12.9 363uJy e_F3.6t [-106999,]?=-1. rms uncertainty on F3.6t 539-551 F13.9 363uJy e_F4.5t [-106999,]?=-1. rms uncertainty on F4.5t 553-569 F17.11 363uJy e_F5.8t [-106999,]?=-1. rms uncertainty on F5.8t 571-588 F18.11 363uJy e_F8.0t [-106999,]?=-1. rms uncertainty on F8.0t 590-599 F10.7 arcsec apK Aperture diameter in K band (6) 601-610 F10.7 arcsec ap3.6 Aperture diameter in IRAC 1 band (6) 612-621 F10.7 arcsec ap4.5 Aperture diameter in IRAC 2 band (6) 623-632 F10.7 arcsec ap5.8 Aperture diameter in IRAC 3 band (6) 634-643 F10.7 arcsec ap8.0 Aperture diameter in IRAC 4 band (6) 645-656 F12.10 --- Uw ?=0 Relative weight in U band (vs z-band) (7) 658-669 F12.10 --- Bw ?=0 Relative weight in B band (vs z-band) (7) 671-682 F12.10 --- Vw ?=0 Relative weight in V band (vs z-band) (7) 684-696 F13.11 --- Rw ?=0 Relative weight in R band (vs z-band) (7) 698-709 F12.10 --- Iw ?=0 Relative weight in I band (vs z-band) (7) 711-719 F9.7 --- zw [1]?=0 Relative weight in z band (7) 721-734 E14.9 --- Jw ?=0 Relative weight in J band (vs z-band) (7) 736-748 F13.11 --- Hw ?=0 Relative weight in H band (vs z-band) (7) 750-763 E14.9 --- Kw ?=0 Relative weight in K band (vs z-band) (7) 765-776 F12.9 --- 3.6w ?=0 Relative weight in IRAC1 band (8) 778-789 F12.9 --- 4.5w ?=0 Relative weight in IRAC2 band (8) 791-802 F12.9 --- 5.8w ?=0 Relative weight in IRAC3 band (8) 804-815 F12.9 --- 8.0w ?=0 Relative weight in IRAC4 band (8) 817 I1 --- Sfl [0/1] Stellar flag: 0=galaxy, 1=star 819-820 I2 --- Bfl [0/15] Blended flag (9) 822-823 I2 --- Qfl [0/15] Quality flag (10)
Note (1): All fluxes are normalized to an AB magnitude zeropoint of 25.0, i.e. MAGAB(X)=-2.5*log10(FLUX(X))+25.0; in other words, fluxes are given in units of 0.363mJy Note (2): Colour aperture fluxes (i.e. Xcolf) are measured in 4.0" diameter apertures. The IRAC images have not yet been PSF matched. All images have been convolved with a Gaussian to the frame with the largest FWHM, which is the 8.0 micron image. Sources that fall outside the area covered by a specific band X, have their fluxes and photometric errors set to -9999. Note (3): The colour aperture errors (i.e. e_Xcolf) are determined by placing a large number of apertures on empty regions of each image, and thus account for pixel-pixel correlations introduced by dithering, astrometric correction. Errors have been weighted by means of the exposure map following: errxy=errm*sqrt(expm/expxy) where: * errxy is the error at position (x,y) = e_Xcolf * errm is the measured error * expm is the effective exposure time of the area used to measure the error (per pixel) * expxy is the exposure time of the source at position (x,y) Note (4): The IRAC bands consist of combined deep CDFS-S (GOODS) data and shallower SIMPLE data. Due to the difference in exposure time and reduction method of both areas, errors for the CDFS GOODS and E-CDFS SIMPLE data have been determined separately and scaled to GOODS-CDFS and E-CDFS exposure times, respectively. Note (5): Total fluxes are determined for all IRAC bands and MUSYC K-band using SExtractor's AUTO(APER) measurement. The fluxes in AUTO(APER) are multiplied by a certain factor that was derived from the growthcurves of stars for each band. Total fluxes for the rest of the MUSYC bands can be derived as: Xtotf = Xcolf*Ktotf/Kcolf Note (6): This corresponds the circularized diameter of APER(AUTO) when the Kron aperture is used. If the circularized diameter is smaller than 4", the entry is set to APER(COL)=4" . Note (7): Relative weights (i.e. Xw) give the value of the weight/exposure map, normalized to the upper 5 percentiles of the exposure time. Note (8): Using the highest percentiles exposure time as normalization value, for IRAC data, the E-CDFS gets relatively low weights (see Note 4). We therefore have normalized the IRAC weights to the maximum exposure time of the SIMPLE mosaic without GOODS. Weights of GOODS sources will, therefore, generally be > 1. (GOODS sources can be identified using the Qflag entry, see note 9) Note (9): Blended flag is bitwise encoded and contains the SExtractor deblending flag, which indicates whether a source suffers from blending (bit = 1) or whether it has a close neighbor (bit = 2). When a source's neighbour lies within its aperture diameter and when the flux of the neighbour is brighter than its own, Bflag is set to 4). Note (10): Quality flag can be used to identify contaminated/special areas and is bitwise encoded. 1 = source in GOODS field 2 = source in contaminated area (e.g. stellar trail) 4 = source outside MUSYC field 8 = source corrected for muxbleed
History: Copied at http://www.astro.yale.edu/dokkum/SIMPLE
(End) Patricia Vannier [CDS] 30-Sep-2011
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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