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Spectra from Hook, I.M. et al 2005, AJ, 130, 2788.
Compiled 14 Feb 2006.
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There are two sets of spectra that were presented in the paper.

1) Original supernova (before host galaxy subtraction etc) and host
galaxy spectra. In most cases the light from the SN and host were
merged but in a few cases separate extractions were possible (as shown
in the paper).

IAU_name    SCP_name    Filename                       Comments
 
1997F       974         974_domec_ap2.asc              SN+host
1997G       972         972c_ap3.asc                   host
  "                     972c_ap2.asc                   SN
1997I       970         sn970opt2.asc                  SN+host
1997J       975         975d_ap2.asc                   SN+host
1997N       9710        sn9710opt.asc                  SN+host
1997R       9760        9760c_ap3.asc                  host
  "                     9760c_ap4.asc                  SN(+ some host)
1997S       9739        9739d_ap3.asc                  SN+host
1997ac      9765        sn9765_wcrd_ap3_clean.asc      SN
1997af      9781        sn9781_comb_wcrd_ap2_clean.asc SN+host
1997ag      9777        sn9777_wcrd_ap1_clean.asc      SN+host
1997ai      9779        sn9779_wcrd_ap2_clean.asc      SN
1997aj      9794        sn9794_comb_d_ap3.asc          host
  "                     sn9794_comb_d_ap2.asc          SN
1997am      9785        sn9785_wcrd_host.asc           host
  "                     sn9785_wcrd_clean.asc          SN
1997ap      9784        sn9784_comb_wcrc.asc           SN

# Note to IMH: the above filenames are taken from the IDL input files
# see ~/wdata/txt/papers/snspec/idlfiles/
# XXX_snz.in, XXX_galz.in, XXX_hostz.in, XXX_andy.in

2) Galaxy-subtracted spectra. Galaxy subtraction has been done using
the "superfit" program of D.A. Howell (this program calculates the
amount of galaxy to subtract by doing a chi-sq fit that gives the best
match to a Type-Ia template spectrum. The program also allows the
overall slope of the spectrum to be changed to give the best
fit). Prior to running the spectra through the program, narrow
features were interpolated across and the spectra were re-binned to
20A rest frame.

These are the spectra that were used in the plots that show
comparisons to nearby templates and also in Figs 17 and 18 of the
paper (i.e. the time sequence and the measurements of the Ca
velocity).

IAU_name     Filename

1997F   974.lc.6.sub.sft 
1997G   972.lc.1.sub.sft
1997I   970.lc.1.sub.sft  
1997J   975.lc.3.sub.sft
1997N   9710.lc.1.sub.sft 
1997R   9760.lc.1.sub.sft
1997S   9739.lc.1.sub.sft
1997ac  9765.lc.1.sub.sft
1997af  9781.lc.4.sub.sft
1997ag  9777_nolines.2.sub.sft
1997ai  9779.lc.1.sub.sft
1997aj  9794.lc.5.sub.sft
1997am  9785.lc.6.sub.sft
1997ap  9784.lc.1.sub.sft

# Notes to IMH: these file names are the ones used in snsh.pro, listed in 
# ~/wdata/txt/papers/snspec/isobel/andy_refits/andyfiles.list"