From the web:
http://panisse.lbl.gov/hst_clusters/
Locally:
sauls:/autofs/panisse/www/production/htdocs/hst_clusters
Co-I's from Tony on 19 Jan:
saul@lbl.gov, galdering@lbl.gov, barrientos@astro.puc.cl, mark.brodwin@jpl.nasa.gov, KDawson@lbl.gov, dey@noao.edu, donahue@pa.msu.edu, prme@kromos.jpl.nasa.gov, elling@casa.colorado.edu, VAFadeyev@lbl.gov, fruchter@stsci.edu, gilbank@astro.utoronto.ca, gladders@ociw.edu, gerson@lbl.gov, anthony@astro.ufl.edu, ariel@physto.se, hoekstra@uvic.ca, imh@astro.ox.ac.uk, bjannuzi@noao.edu, MPKowalski@lbl.gov, NVKuznetsova@lbl.gov, clidman@eso.org, lmlubin@ucdavis.edu, cmullis@umich.edu, panagia@stsci.edu, rhodes@astro.caltech.edu, prosati@eso.org, DJSchlegel@lbl.gov, ALSpadafora@lbl.gov, adam@igpp.ucllnl.org, vall@physto.se, stern@zwolfkinder.jpl.nasa.gov, lifan@panisse.lbl.gov, hyee@astro.utoronto.ca, postman@stsci.edu
bias.eps
From Roman Miquel on 19 Jan 6:32 pm.
I'm attaching here a plot showing the bias in Riess procedure, according to
what we discussed earlier today.
WARNING: the bias changes subtantially when I change the seed for the random
numbers I use to simulate the E(B-V) original distribution.
However, the bias tends to be in this direction: more negative w_0, more
positive w_a. This plot was the very first I produced and it happens to match
rather precisely the result in Riess et al.! The true underlying cosmological
model is a cosmological constant, marked by a cross in the figure. Note that
the contour is 1-sigma projected (39% CL inside). I'm having technical problems
getting wider contours (the theory calculations do not converge for crazy
values of w_a).
cl1252_cmr.gif
cmd_scatter_vs_z.gif
From Marc Postman on 20 Jan 1:07 pm. After the 2004 election, nothing makes
sense to me any more. No seriously - the errors are fairly big on these
overdensity estimates. I am now re-computing the overdensities in another way
to see if I get similar results. I should have the answers shortly. I am
attaching the figures showing the scatter and slope of the CMD as a function
of redshift that I referred to in the telecon.
------------
r1252acs.ps
r1252cmd.ps
From Adam Stanford.
\caption{(left) A color composite made from ACS images in the $i$ and $z$
bands of the central 1 arcmin of RX1252-29 at $z=1.23$. The large
number of red early-type is obvious. (right) The very small scatter in
the colors measured in these data are seen in the color-magnitude
diagram for all galaxies with $i-z > 0.5$, excluding spectroscopically
known nonmembers, inside a radius of 1.9 arcmin. Circles and squares
are ellipticals and S0s respectively, used in the fits shown to the
color-magnitude relation. The relation for the Coma cluster
early-types, transformed to the observed bands with no evolution
correction is shown as a dot-dash line. The approximate luminosity
conversion to rest frame absolute B magnitude is shown at the top
assuming a WMAP cosmology and -1.4 mag of luminosity evolution.
early_oden_factor.ps
From Marc Postman on 20 Jan 11:02 am.
Attached is a plot of the estimated overdensities in E+S0 galaxies for the ACS
GTO clusters in our sample. The derived overdensities are:
Cluster E+S0 overdensity
Name zobs (relative to GOODS)
------------------------------------
RXJ0910+54 1.10 5.35
RXJ1252-29 1.24 3.72
RXJ0848+44 1.27 2.87 (x-ray selected)
CLJ0848+44B 1.27 2.12 (IR selected companion)
The cluster E+S0 classifications are based on visual classification from ACS
data. Cluster data restricted to central 250 kpc (radius).
The GOODS E+S0 surface density is estimated by multiplying the full surface
density by 0.25 - i.e., assumed that 75% of the galaxies in GOODS S+N fields
are spirals or Irregulars.
followup-mag.eps
followup.eps
From Marek Kowalski, most recently on 20 Jan 1:42 pm.
Simulated search, SN mags vs. time
hubble.ps
From Ariel Goobar 20 Jan 4:10 am
ms_hubble_type2.eps
From Sullivan et al paper. used in previous proposals.
overdensities.bysample.eps
overdensities.eps
From Anthony Gonzalez on 20 Jan 2;27 pm.
Two versions attached -- one shows just the cumulative histogram, the
other illustrates the contributions from each sample (but only includes
the RCS clusters for which I had L_B values). The RDCS and IRAC
overdensities are directly from the numbers each group sent; the
RCS values are scaled by comparing his L_B values (converted to have the
same area and evolved M_B*) to a typical IRAC cluster. Fairly rough, but
this should be sufficient for the proposal.
rdcs1252_BV_Rz_JK.jpg
rdcs1252_acs_iz.jpg
From Adam Stanford 19 Jan 1:06 pm.
Attached are a couple of images of 1252-29; perhaps worth sending in a color
image because there is the reasonable chance that the proposal will be viewed
in color on a laptop by the panel members, as opposed to a greyscale printout.
The first one is an HST ACS image of the central region, and the second is a
ground-based image covering a larger area along with X-ray contours.
samplecomp.ps
From Adam Stanford 19 Jan 12:20 pm.
Redshift distribution of our clusters compared to GTO clusters.
sn_z.eps
This from Henk Hoekstra on 20 Jan 5:52 pm.
I have adopted a mean mass for the clusters in our sample of 5x10^14 M_sun
(close to 800 km/s in velocity dispersion), based on what Piero Rosati and
Adam Stanford told me. This seems quite reasonable, although the
properties of the RCS sample are not fully known yet. I can't get a hold
of Mike...
I have attached a figure which we could use in the proposal if you want. The
upper panel shows the expected relative error in the mass for a cluster of 5e14
and 1e15 Msun. The lower panel shows the relative uncertainty in the
calibration of the mass-observable relation, which is the key ingredient for
cluster abundance work. As you can see, we get ~10% in 4 independent redshift
bins, enabling us to constrain the evolution in cluster properties to a
sufficient accuracy, especially once tied to the lower redshift work that is
going on. I have assumed the number in the plot that Saul sent me, and
truncated at z=1.4.
wwPrimeHSTclusterFig2.eps
From Saul 20 Jan 7 PM.