SN 2002bo Ia in NGC 3190
OBJECT: SN 2002bo Ia in NGC 3190 (Sa galaxy) which in Leda is
NGC 3190 (Leda).
DISCOVERY: 2002mar9.08 UT by Cacella & Hirose
MAXIMUM: 2002mar23.0 (MJD 52356.0) in B benetti2004.
The Asiago Catalog gives 2002mar24 which is
the value adopted by SUSPECT, but
that's not very precise and who's to know which is better. benetti2004's value
is the published one and that's the paper reference for SN 2002bo.
Note that Modified Julian Date (MJD) is given by
MJD=JD-2400000.5 (Julian Date).
For some three centuries following 1858nov17.00 UT, the Julian day lies between 2400000 and 2500000.
The MJD drops those first "24" digits and gets rid of that annoying half day thing.
So Bmax as on JD 2452356.5.
See the US Navy Observatory
Julian Date Converter.
This day of the year 81.
SUPERNOVA of the YEAR: M = 67.
HEADER: Header Common header information for this supernovae.
The common header may (or may not) be updated relative to the header information here
(D. J. Jeffery (2006jan01)).
COMMENT: SN2002bo is broad line (BL) SN Ia.
The Asiago catalog gives 2002mar24 for Bmax (it seems). But benetti2004
gives the above date. For consistency, I'll trust the dates of the paper.
SPECTRUM LOG:
MJD times for the SN 2002bo spectra of benetti2004
Bmax from benetti2004 where the MJD Bmax is MJD 52356.0
but the error is probably at least .5 days.
As far as I know all the benetti2004 spectra from SUSPECT
are in the observer frame.
MJD Bmax Heliocentric velocity (Leda, 2007jun30)
52356.0 1309.
Heliocentric velocity Z redshift
1309.0000000000 0.0043663540
Index JD of some kind Observer phase Rest phase
1 52343.0600000000 -12.9400000000 -12.8837450084 ! benetti2004 2004mar10 3363.8074747526--7726.94645136275
2 52343.9900000000 -12.0100000000 -11.9577880642 ! benetti2004 2004mar10 3363.8074747526--7726.94645136275
3 52344.9900000000 -11.0100000000 -10.9621354360 ! benetti2004 2004mar11 3362.4255268009--7721.99072561971
4 52346.9100000000 -9.0900000000 -9.0504823900 ! benetti2004 2004mar13 3360.5078131688--7722.688521438
5 52347.4800000000 -8.5200000000 -8.4829603919 ! benetti2004 2004mar14
6 52347.4800000000 -8.5200000000 -8.4829603919 ! benetti2004 2004mar14
7 52348.0400000000 -7.9600000000 -7.9253949201 ! benetti2004 2004mar15
8 52349.9300000000 -6.0700000000 -6.0436114529 ! benetti2004 2004mar16
9 52351.8500000000 -4.1500000000 -4.1319584069 ! benetti2004 2004mar18 3184--7576.9759
10 52352.0200000000 -3.9800000000 -3.9626974601 ! benetti2004
11 52352.0500000000 -3.9500000000 -3.9328278812 ! benetti2004 2004mar19
12 52352.9400000000 -3.0600000000 -3.0466970422 ! benetti2004 2004mar19 3362.5--7725.81373299499
13 52353.9000000000 -2.1000000000 -2.0908705191 ! benetti2004 2004mar20 3305.8835449219--9040.43327188492
14 52354.0000000000 -2.0000000000 -1.9913052563 ! benetti2004 2004mar20
15 52354.8800000000 -1.1200000000 -1.1151309435 ! benetti2004 2004mar21
16 52354.9600000000 -1.0400000000 -1.0354787333 ! benetti2004 2004mar21 3306.8620605469--9036.44265747077
17 52355.1800000000 -0.8200000000 -0.8164351551 ! benetti2004 2004mar22
18 52356.0800000000 0.0800000000 0.0796522103 ! benetti2004 2004mar23 3356.3850097656--10201.7692260742
19 52356.0800000000 0.0800000000 0.0796522103 ! branch2006 2004mar23 3502.13--10000 synthetic spectrum
20 52361.9400000000 5.9400000000 5.9141766113 ! benetti2004 2004ma428 3099.8000488281--8801.34040498742
21 0.0000000000****************************** ! about 5600--5950 is a crude linear
22 0.0000000000****************************** ! interpolation of a gap.
23 52367.2900000000 11.2900000000 11.2409181719 ! benetti2004
24 52367.2900000000 11.2900000000 11.2409181719 ! benetti2004
25 52385.4000000000 29.4000000000 29.2721872679 ! benetti2004
26 52385.4000000000 29.4000000000 29.2721872679 ! benetti2004
27 52385.9100000000 29.9100000000 29.7799701082 ! benetti2004
28 52387.4000000000 31.4000000000 31.2634925242 ! benetti2004
29 52395.9000000000 39.9000000000 39.7265398635 ! benetti2004
30 52400.9400000000 44.9400000000 44.7446291094 ! benetti2004
31 52411.9000000000 55.9000000000 55.6569819141 ! benetti2004
32 52413.0000000000 57.0000000000 56.7521998050 ! benetti2004
33 52417.0000000000 61.0000000000 60.7348103177 ! benetti2004
34 52440.0000000000 84.0000000000 83.6348207653 ! benetti2004 2004jun14 3746--9742.30226295757
35 0.0000000000****************************** ! Some zero points at the end are cut off.
36 52440.9900000000 84.9900000000 84.6205168672 ! benetti2004
REFERENCES:
benetti2004 Specifically on SN 2002bo with
31 spectra of various kinds.
branch2006 Synthetic spectra for
SNe Ia at maximum light.
CfA List of Supernovae
where SN 2002bo is noted.
CfA Supernova Archive
For SN 2002bo, this has 0 spectra and 0 photometry.
conley2006 General value
of 19.4 days for Ia rise time in B.
paturel2003 (Leda) Leda refererence.
SUSPECT Index.
SUSPECT Index: SN 2002bo Ia.
There are 22 spectra all from benetti2004. Probably some are averages or composites of benetti2004's spectra.
But there is no a great picture of
Fritz Zwicky (Wikipedia).
Just say Fritz Zwicky aloud and you can tell he's an up-to-date person.
CORRECTIONS: Heliocentric velocity 1309 +/- 7 km/s (2007jun30) from
NGC 3190 (Leda).
Galactic foreground 0.11/4=.0275 reddening from
NGC 3190 (Leda).
But this isderived from
Schlegel et al. (1998)
OBSERVATIONS: From (1)
1) SUSPECT: benetti2004.
2) David Branch synthetic spectra.
3) David Branch directory /home/branch/synow/02bo: all the benetti2004 spectra are there, but
in FITS format.
PHASE:
For consistency we always use rest phase and for explicitness to more digits than are significant.
observer phase =
rest phase =
&specnamelist
aname='sn2002bo Ia 2002_03_'
ebv=.0275 !
epoch= ! This parameter needs to updated for the particular spectrum.
idifmake=0
iformat=1
ismooth=0 ! Smoothing?
itick=2
itickln=4
t_rise=19.4d0 ! \citep{conley2006}, Just an average rise time.
v_helio=1309.
ymin2=.2d-16
ymax2=100.d-16
ymin3=.3
ymax3=3.
wlammin1=
wlammax1=
wlammin2=
wlammax2=
wlammin3=
wlammax3=
/
Postscript plot of the spectrum.
Postscript plot of the spectrum with local normalization.
FITS: Fits format information from the observers.
