Explanatory Notes
The X and Y coordinates refer to the Version 2 drizzled mosaic obtained from
here.
The magnitudes are on the ST system.
They correspond to a flux per wavelength interval
(as opposed to AB magnitudes which are a measure of flux per frequency interval).
In this system, a magnitude of M=0 is equivalent to
of 3.63E-12 W/m2/Å in all bands.
In these web pages (and tables), a magnitude of 33.000 means no detection.
The graphs show the photometry converted into fluxes as squares.
If an object was not detected in a band, this is denoted by
an arrow indicating an upper limit.
The best fitting template is shown as a solid line.
The dotted line indicates the limiting fluxes in the various bands.
When comparing the the templates to the fluxes remember that the fitting
is weighted by the uncertainty on each of the fluxes. Also, points
with no detection are given no weight.
The colour images of each galaxy are sub-sections of a the full scale publicity image
from
STScI
The black and white postage stamp images are from the FITS mosaic.
They are shown
on a logarithmic scale, renormalized to the brightest pixel.
This means that it is sometimes difficult to compare a galaxies appearance
in different bands.
Each postage stamp is a clickable map leading to the pages for nearby galaxies.
References for the spectroscopic redshifts are as follows:
-
(1) Cohen J.G., Cowie L.L., Hogg D.W., Songaila A., Blandford R.,
Hu E.M. & Shopbell P.,
1996,
Redshift
clustering in the Hubble Deep Field, Astroph. J. Let. 471 L5-L9.
Or check out the data
here .
-
(2) Lowenthal J., Koo D.C., Guzman R., Gallego J., Phillips A.C., Vogt N.P., Faber S.M., Illingworth G.D. & Gronwall C., 1997,
Keck spectroscopy of z=3 galaxies in the HDF, Astroph. J., 481, 673
Or check out the data
here .
-
(3) Steidel C.C., Giavalisco M., Pettini M., Dickinson M.E., & Adelberger K.L.
1996,
Spectroscopy of Lyman break galaxies in the Hubble Deep Field ,
Astron. J., 112, 352
-
(4) Zepf S.E., Moustakas L.A & Davis M,
1997
Keck Spectroscopy of Objects with Lens-like Morphologies in the
Hubble Deep Field,
Astroph. J., 474, L1
-
(5) Hogg D. W., Cohen J. G., Blandford R., Gwyn S. D. J., Hartwick F. D. A., Mobasher B., Mazzei P., Sawicki M., Huan L., Yee H. K. C., Connolly A. J., Brunner R. J., Csabai I., Dickinson M., Subbarao M. U., Szalay A. S., Fernandez-Soto A. S., Lanzetta K. M. & Yahil A.
1998,
A blind test of photometric
redshift prediction, Astron J. 115, 1418
-
(6) Fernandez-Soto A., Lanzetta K. M., & Yahil A. 1998,
A new catalog of photometric redshifts in the Hubble Deep Field
-
(7) Spinrad H., Stern D., Bunker A., Dey A., Lanzetta K. M., Yahil A., Pascarelle S. & Fernandez-Soto A. 1998,
A z=5.34 galaxy pair in the Hubble Deep Field Astron. J. 116, 2617
-
(8) Weynman R. J., Stern D., Bunker A., Spinrad H., Chaffee F. H., Thompson R. I. & Storrie-Lombardi L. J. 1998,
Keck spectroscopy and NICMOS photometry of a redshift z=5.60 galaxy, Astroph. J., 505, 95
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