the group started to take form after the collaboration meeting in Berkeley last june. At that ocassion mainly the spectroscopy effort was discussed. The agreed strategy was that the reduction effort would be devided up according to following scheme:
Stockholm: NOT/INT/KPNO4.0/Lick3.0/ESO3.6m
Berkeley: APO3.5/CTIO4.0
It was also agreed that one of the ESO3.6 nights (april 10, 1999) would be reduced by all the reduction teams, including Chris Lidman to compare reduction quality.
On the photometry side, Nicolas Regnault was finishing his PhD thesis in Paris on the lightcurves of several of the Ia's in the sample, see http://panisse.lbl.gov/nearsearch/
The Lisbon group started to work on the reduction of images from Yalo1.0m and Lick1.0m.
August 2000:
sucesfull comparisons between the Stockholm group and Chris on the test night at ESO3.6m.
Documentation on reduction scheme at: "http://www.physto.se/~snova/private/near-z/spectroscopy/spectra.html"
Documentation on studies of errors estimation: "http://www.physto.se/~snova/private/near-z/spectroscopy/systematics.ps"
October 2000:low-z working group officially formed, Ariel Goobar asked to take the lead.
Nicolas moves to Berkeley and officially into the "SCP family", thus facilitating the photometry effort.
November 2000:
e-mail distribution list to reach all current members of the team: nearsearch99@physto.se. E-mail exchange accesible to all SCP-members at protected page http://www.physto.se/~snova/private/snovamail
Documentation on differential atmospheric refraction effects: http://www.physto.se/~snova/private/dar.ps
Analysis of non-Ia initiated by non-SCP member Hatano.... under the supervision of Peter Nugent
22 Sne in the reduced sample (not only Ia's) :
SN1999aa, ab, ac, ae, af, ai, ak, ao, as, au, av, aw, ax, ay ,bh, bi, bk, bm, bn, bp, bq ,z
A summary of reduced spectra is available at
"http://www.physto.se/~snova/private/near-z/spectroscopy/table_sn_total.html".
NOTE that the S/N value is computed as an average all over the spectrum,
but wavelength dependent uncertainty is also available.
Berkeley: 3/5 of CTIO Feb-Mar 99 reduced, totaling 30 spectra for 21 SNe
The 10 follow-up telescopes have been intercalibrated using the field stars. So far only the Danish 1.54 m has been calibrated. Ongoing calibration work with CTIO1.5m and Lick1.0m data.
Calibrated light curves have been produced for 15 SNIa.
SN1999aa,ac,ao,ar, at, au, av, aw, ax, be, bi, bk, bm, bn, bp
- 99bh and 99by are in the northern hemisphere. and not observable from La Silla with the Danish 1.54m.
Ongoing work with Lick1.0m will solve this problem
- 99as (Ic) not analysed yet (ongoing)
Lisbon (Ana): getting experience in different flatfielding and reduction techniques using two nights of Lick1.0m data. Documentation at http://supernova.ist.utl.pt/