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J/ApJ/655/51        HDFS IRAC observations of 2<z<3.5 galaxies    (Wuyts+, 2007)

What do we learn from IRAC observations of galaxies at 2 < z < 3.5?. Wuyts S., Labbe I., Franx M., Rudnick G., Van Dokkum P.G., Fazio G.G., Forster Schreiber N.M., Huang J., Moorwood A.F.M., Rix H.-W., Rottgering H., Van Der Werf P. <Astrophys. J., 655, 51-65 (2007)> =2007ApJ...655...51W
ADC_Keywords: Galaxies, IR ; Photometry, infrared ; Redshifts Keywords: galaxies: evolution - galaxies: high-redshift - infrared: galaxies Abstract: We analyze very deep HST, VLT, and Spitzer photometry of galaxies at 2<z<3.5 in the Hubble Deep Field-South. The sample is selected from the deepest public K-band imaging currently available. We show that the rest-frame U-V versus V-J color-color diagram is a powerful diagnostic of the stellar populations of distant galaxies. Galaxies with red rest-frame U-V colors are generally red in rest-frame V-J as well. However, at a given U-V color a range in V-J colors exists, and we show that this allows us to distinguish young, dusty galaxies from old, passively evolving galaxies. We quantify the effects of IRAC photometry on estimates of masses, ages, and the dust content of z>2 galaxies. Description: Observations of the HDF-S WFPC2 field were obtained with IRAC on the Spitzer Space Telescope in 2004 June and 2005 June (GTO program 214). A field of view was covered by the four broadband filters at 3.6, 4.5, 5.8, and 8um. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table3.dat 69 75 K+IRAC photometry of HDFS galaxies at 2<z<3.5 table4.dat 73 75 Modeling results for HDFS galaxies at 2<z<3.5
See also: J/AJ/119/486 : HDF-S: STIS imaging (Gardner+, 2000) J/AJ/125/1107 : Ultra-deep near-IR observations in HDF-S (Labbe+, 2003) J/A+A/452/119 : EIS: infrared observations of CDF-S and HDF-S (Olsen+, 2006) J/AJ/131/2383 : Photometry and spectroscopy in the HDF-S (Glazebrook+, 2006) Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 3 I3 --- [LFR2003] Object identification number (1) 5- 9 F5.2 --- FKtot Total aperture K band flux (2) 11- 14 F4.2 --- e_FKtot Uncertainty in FKtot 16- 20 F5.2 --- FK Color aperture K band flux (2) 22- 25 F4.2 --- e_FK Uncertainty in FK 27- 31 F5.2 --- F3.6 Color aperture 3.6 micron flux (2) 33- 36 F4.2 --- e_F3.6 Uncertainty in f3.6 38- 42 F5.2 --- F4.5 Color aperture 4.8 micron flux (2) 44- 47 F4.2 --- e_F4.5 Uncertainty in f4.5 49- 53 F5.2 --- F5.8 Color aperture 5.8 micron flux (2) 55- 58 F4.2 --- e_F5.8 Uncertainty in f5.8 60- 64 F5.2 --- F8.0 Color aperture 8.0 micron flux (2) 66- 69 F4.2 --- e_F8.0 Uncertainty in f8.0
Note (1): Object identification number corresponds to that of the U-to-K catalog by Labbe et al. (2003, Cat. J/AJ/125/1107). Note (2): Scaled to an AB zeropoint of 25, i.e. magAB=25-2.5log(f).
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 3 I3 --- [LFR2003] Object identification number (1) 5- 8 F4.2 --- z Redshift 10- 13 F4.2 --- E_z Upper limit uncertainty on z 15- 18 F4.2 --- e_z Lower limit uncertainty on z 20- 29 A10 --- SFH Star-formation history (2) 31- 35 F5.2 [solMass] logM Log of the modeled mass 37- 40 F4.2 [solMass] E_logM Upper limit uncertainty on logM 42- 45 F4.2 [solMass] e_logM Lower limit uncertainty on logM 47- 49 F3.1 mag AV Model V band extinction 51- 53 F3.1 mag E_AV Upper limit uncertainty on AV 55- 57 F3.1 mag e_AV Lower limit uncertainty on AV 59- 63 F5.2 [Gyr] logA Log of the model mass-weighted age 65- 68 F4.2 [Gyr] E_logA Upper limit uncertainty on logA 70- 73 F4.2 [Gyr] e_logA Lower limit uncertainty on logA
Note (1): Object identification number corresponds to that of the U-to-K catalog by Labbe et al. (2003, Cat. J/AJ/125/1107). Note (2): Star-formation history is: CSF = constant star-formation; SSP = single stellar population; τ300 = an exponentially declining star-formation history with an e-folding timescale of 300Myr
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Patricia Vannier [CDS] 08-Dec-2008
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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