From: Chris Lidman (clidman@eso.org)
Date: Wed Dec 03 2003 - 15:39:19 PST
Hi Gaston,
Please find enclosed a list of suggestions from Peter. In addition to
the corrections listed here, Peter will also FAX you a list of
grammatical corrections.
Cheers, Chris.
attached mail follows:
Hi all,
Here are my comments on the paper.
(1) Redo the abstract.
(a) It is not well written.
(b) The statement about the amount of follow-up time being less is false -
well perhaps misleading is a better word - extinction measurements were
not accounted for and one would have to factor in this plus the amount of
time necessary to id the SN in comparison to taking this higher-quality
spectrum without host galaxy contamination (which definitely effects the
measurement of alpha(2+3).
(c) The statement about the ability to measure these features at high-z
should be studied a little more. I will mention this below.
This is a good paper and it should start with a good abstract. Other than
the first sentence this abstract fails to deliver. More often than not
this is the most important part of a paper. Effort should be put into
this since there is no way (regardless of how good the rest of the paper
is) that this could go before the entire group before this is cleaned up.
People would not bother with the rest...
(2) References look fairly good. I can add a couple in the next version.
(3) English problems abound. I gave up after the first two pages marking
them up. I can fax them to someone if you would like, but I won't type
them in, there are too many.
(4) Remove the Ni II Fisher et al comment. It is speculative at best. You
should just state that Ca II might be less abundant and/or the higher
temperatures reduce the strength of these features.
Things to do science-wise:
(1) The Saha distance to SN 1991T is a problem since all the other ones
are based on a Freedman et al measurement. I would suggest using the
Gibson et al measurement (cited below) since it will be consistent with
Freedman et al. Basically it doesn't matter which one you use as long as
you are consistent.
(2) Table 7: Add the distance moduli in the table for each SN as well as
the measurement for extinction with uncertainties (and references for
each). Also I completely dislike the use of M_B(max) and M_B(max)(dm15).
This also applies to the bottom of figure 12.
There is a measured peak brightness for an extinction-corrected SN Ia.
This is M_B(max). This is fine. The only use for M_B(max)(dm15) is for
the residual plot. Why not just show residuals (M_B(max) - the equation
for determining the brightness of a Ia w/ dm15) This is MUCH less
confusing.
I say this also since when you use the consistent analysis of SN 1991T
the point in Figure 12 for 1991T will move down by ~0.3mag or so. Then the
correlation in the bottom figure will go away. Which is neither good nor
bad, just interesting. The modified figure should be kept, regardless.
(3) Do a simple test for the effect of host galaxy contamination on the
measurement of alpha(2+3). Just add an early and late type galaxy spectrum
(normalized to V-band) in amounts going from 0 - 100% of the light in a
given SN spectrum (pick your favorite) and redo the calculation. Then you
can fairly state how well you can make this measurement at high-z under
these conditions and note the systematics involved. A graph of alpha(2+3)
vs. host gal. contam. would be enlightening.
Cheers,
Peter
@ARTICLE{2001ApJ...547L.103G,
author = {{Gibson}, B.~K. and {Stetson}, P.~B.},
title = "{Supernova 1991T and the Value of the Hubble Constant}",
journal = {\apjl},
year = 2001,
month = feb,
volume = 547,
pages = {L103-L106},
adsurl =
{http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=2001ApJ...547L.103G&db_key=AST},
adsnote = {Provided by the NASA Astrophysics Data System}
}
__
Peter E. Nugent
Staff Computational Scientist - Scientific Computing Group - NERSC
Lawrence Berkeley National Laboratory
M.S. 50F-1650 - 1 Cyclotron Road - Berkeley, CA, 94720-8139
Phone:(510) 486-6942 - Fax:(510) 486-5812
E-mail: penugent@LBL.gov - Web: http://supernova.LBL.gov/~nugent
This archive was generated by hypermail 2.1.4 : Wed Dec 03 2003 - 15:45:17 PST