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/journal_tables/ApJ/546/694/

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J/ApJ/546/694       NICMOS star formation history            (Thompson +, 2001)
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Star formation history in the NICMOS Northern Hubble Deep Field.
    Thompson R.I., Weymann R.J., Storrie-Lombardi L.J.
      <Astrophys. J. 546, 694 (2001)>
      =2001ApJ...546..694T      (SIMBAD/NED BibCode)
================================================================================
ADC_Keywords: Galaxies, photometry ; Redshifts ; Extinction ;
              Photometry, infrared
Mission_Name: HST
Keywords: Cosmology: observations - galaxies: evolution -
          galaxies: fundamental parameters - galaxies: starburst -
          stars: formation

Abstract:
    We present the results of an extensive analysis of the star formation
    rates determined from the NICMOS deep images of the northern Hubble
    Deep Field. We use SED template fitting photometric techniques to
    determine both the redshift and the extinction for each galaxy in our
    field. Measurement of the individual extinctions provides a correction
    for star formation hidden by dust obscuration. We determine star
    formation rates for each galaxy based on the 1500{AA} UV flux and add
    the rates in redshift bins of width 1.0 centered on integer redshift
    values.

File Summary:
--------------------------------------------------------------------------------
 FileName      Lrecl  Records   Explanations
--------------------------------------------------------------------------------
ReadMe            80        .   This file
table1.dat       104      281   Listing of measured quantities
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See also:
   J/AJ/112/1335 : Hubble Deep Field observations (Williams+ 1996)
   J/AJ/117/17   : Hubble Deep Field near-IR obs. (Thompson+, 1999)
   J/ApJ/538/493 : HDF-South NICMOS field (Yahata+, 2000)

Byte-by-byte Description of file: table1.dat
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   Bytes Format Units     Label     Explanations
--------------------------------------------------------------------------------
   1- 10  F10.5 ---       NICMOS    NICMOS identification number (1)
  12- 19  A8    ---       [WBD96]   WFPC identification number from
                                     Williams et al., 1996, Cat. <J/AJ/112/1335>
  21- 24  F4.2  ---       z         Redshift
  26- 29  F4.2  mag       E(B-V)    (B-V) color excess
  31- 37  F7.3 solMass/yr SFR       Star formation rate determined in Section 5
  39- 46  E8.2  solLum    Lum       Bolometric luminosity (2)
  48- 51  F4.2  ---       Frac      Fraction of the luminosity removed by
                                     extinction and re-emitted in the
                                     mid & far-IR
  53- 60  E8.2  mJy       SCUBA     ? The SCUBA 850 microns flux
  62- 64  F3.1  ---       Temp      Template number of best fit between
                                      1.0 (early-cold) and 6.0 (late-hot)
  66- 69  F4.1  ---       Chi2      Modified Chi^2^ of the fit from Equ. 1 (3)
  71- 74  F4.1  mag       Totmag    ? The F160W AB magnitude (4)
  76- 79  F4.1  mag       Apmag     ? The 0.6" diameter aperture F160W magnitude
                                       See note (5)
  81- 82  I2    h         RAh       Right Ascension (J2000)
  84- 85  I2    min       RAm       Right Ascension (J2000)
  87- 91  F5.2  s         RAs       Right Ascension (J2000)
      93  A1    ---       DE-       Declination (J2000)
  94- 95  I2    deg       DEd       Declination (J2000)
  97- 98  I2    arcmin    DEm       Declination (J2000)
 100-104  F5.2  arcsec    DEs       Declination (J2000)
--------------------------------------------------------------------------------
Note (1): Objects with ID numbers less than 1000 are objects that are
           identified with sources in the original KFOCAS catalog of
           Thompson et al., 1999, Cat. <J/AJ/117/17>, [TSW99] NNN.NNN in Simbad.
          Objects with catalog numbers greater than or equal to 1000 are
           SExtractor objects that did not match in position with an original
           catalog entry to within 0.3".
Note (2): The flux of a galaxy is obtained by integrating over the unextincted
           selected template scaled by the factor A from equation 2. The
           bolometric luminosity then follows from the redshift and our adopted
           cosmology.
Note (3): It should be noted that the distribution of the modified chi^2^
           values will not rigorously follow a true chi^2^ distribution. The
           values are provided to give a qualitative indication of the relative
           goodness of fit for the best fit values of redshift, template type
           and E(B-V) from object to object.
Note (4): Derived from the aperture correction method described in
           Yan et al., 1998ApJ...503L..19Y.
Note (5): If no magnitude is listed the object had a zero or negative
           measured F160W flux.
--------------------------------------------------------------------------------

History:
    From electronic version of the journal

================================================================================
(End)                    Greg Schwarz [AAS], Patricia Bauer [CDS]    09-Mar-2001

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