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J/A+A/477/717    Spectroscopy of Type Ia supernovae          (Bronder+, 2008)

SNLS spectroscopy: testing for evolution in type Ia supernovae. Bronder T.J., Hook I.M., Astier P., Balam D., Balland C., Basa S., Carlberg R.G., Conley A., Fouchez D., Guy J., Howell D.A., Neill J.D., Pain R., Perrett K., Pritchet C.J., Regnault N., Sullivan M., Baumont S., Fabbro S., Filliol M., Perlmutter S., Ripoche P. <Astron. Astrophys., 477, 717-734 (2008)> =2008A&A...477..717B
ADC_Keywords: Supernovae ; Photometry ; Equivalent widths Keywords: Supernovae: general - cosmology: observations - surveys Abstract: We present a quantitative study of a new data set of high redshift Type Ia supernovae spectra, observed at the Gemini telescopes during the first 34 months of the Supernova Legacy Survey. During this time 123 supernovae candidates were observed, of which 87 have been identified as SNe Ia at a median redshift of z=0.720. Spectra from the entire second year of the survey and part of the third year (59 total SNe candidates with 46 confirmed SNe Ia) are published here for the first time. The spectroscopic measurements made on this data set are used determine if these distant SNe comprise a population similar to those observed locally. Rest-frame equivalent width and ejection velocity measurements are made on four spectroscopic features. Corresponding measurements are presented for a set of 167 spectra from 24 low-z SNe Ia from the literature. Description: Full details of the methods used for CFHT Supernova Legacy Survey (SNLS) SN candidate selection and observation can be found in Sullivan et al. (2006AJ....131..960S) and Howell et al. (2005ApJ...634.1190H), respectively. In summary, the Canada-France-Hawaii Telescope Legacy Survey (CFHTLS), using the Megacam wide field imager, acquires real time light-curves of possible SNe by repeatedly imaging four, one square-degree fields approximately every four days (observers' frame) in several filters (a combination of g', r', i', and z') as part of the Deep component of the CFHTLS. Spectroscopic observations are then made at 8m-class telescopes in order to identify the SN-type and redshift of these candidates. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table6.dat 76 61 Observed properties and instrument settings for SNLS SNe candidates observed from November 2004 to May 2006 table7.dat 71 59 SNLS identifications and derived properties for SNe candidates observed from Nov. 2004 to May 2006 tablea1.dat 65 55 *Equivalent width and ejection velocity results for the published high redshift SNe Ia observed by the SNLS at the Gemini telescopes
Note on tablea1.dat: This set includes all of the SNLS objects (reduced by the author) that were confirmed as Type Ia SNe (a confidence index of 3 or higher) and were subject to less than 65% contamination from their host galaxies.
See also: B/sn : Asiago Supernova Catalogue II/189 : Magnitude Observations of Type I Supernovae (Cadonau+ 1990) J/AJ/112/2408 : Light Curves of 29 SNe (Hamuy+ 1996) J/A+A/437/789 : Restframe I-band light curves of SN Ia (Nobili+, 2005) J/AJ/131/527 : UBVRI light curves of 44 type Ia supernovae (Jha+, 2006) J/AJ/131/1648 : Type Ia supernovae at high and low redshifts (Blondin+, 2006) J/ApJ/645/488 : SN type Ia luminosities (Wang+, 2006) Byte-by-byte Description of file: table6.dat
Bytes Format Units Label Explanations
1- 6 A6 --- SNLS SN name 8- 9 I2 h RAh Right ascension (J2000) 11- 12 I2 min RAm Right ascension (J2000) 14- 19 F6.3 s RAs Right ascension (J2000) 21 A1 --- DE- Declination sign (J2000) 22- 23 I2 deg DEd Declination (J2000) 25- 26 I2 arcmin DEm Declination (J2000) 28- 32 F5.2 arcsec DEs Declination (J2000) 34- 43 A10 "YYYY-MM-DD" ObsDate Observation date 45- 48 I4 s ExpTime Exposure time 50- 52 A3 --- Mode Observing mode (1) 54- 56 I3 nm lambdac ? Central wavelength 58- 61 F4.2 arcsec Seeing Seeing 63- 67 F5.2 mag i'mag i' magnitude (2) 69 A1 --- l_Inc Limit flag on Inc 70- 74 I5 % Inc Percentage increase (2) (3) 76 A1 --- EW [*] For SN having equivalent width data in tablea1
Note (1): Observing mode as follows: C = classical N+S = nod-and-shuffle Note (2): Estimated from the light-curves and correspond to the date of spectroscopy. Note (3): Percentage increase relative to the host galaxy (interpolated to the date of spectroscopy)
Byte-by-byte Description of file: table7.dat
Bytes Format Units Label Explanations
1- 6 A6 --- SNLS SN name 8- 12 F5.3 --- z ?=- Redshift (1) 14- 18 F5.3 --- e_z ?=- rms uncertainty on z 20 I1 --- CI Confidence index 22- 27 A6 --- SNType Final object identification 29- 34 A6 --- Temp Template name of best low-z spectral fit 36- 38 I3 d TempDay ? Days past maximum of best low-z spectral fit 40- 71 A32 --- r_z Host features used to estimate z
Note (1): Redshifts identified with host galaxy features are accurate to ~±0.001. Redshifts identified with template matches are accurate to ~±0.01.
Byte-by-byte Description of file: tablea1.dat
Bytes Format Units Label Explanations
1- 6 A6 --- SNLS SN name 8- 12 F5.2 --- Day Rest-frame day, relative to B'max 14- 17 F4.2 --- e_Day rms uncertainty on Day 20- 24 F5.1 0.1nm EW(CaII) ?=- CaII equivalent width (1) 26- 29 F4.1 0.1nm e_EW(CaII) ?=- rms uncertainty in EW(CaII) (2) 33- 36 F4.1 0.1nm EW(SiII) ?=- SiII equivalent width (1) 38- 41 F4.1 0.1nm e_EW(SiII) ?=- rms uncertainty in EW(SiII) (2) 44- 48 F5.1 0.1nm EW(MgII) ?=- MgII equivalent width (1) 50- 53 F4.1 0.1nm e_EW(MgII) ?=- rms uncertainty in EW(MgII) (2) 56- 60 F5.2 10+4km/s Vej ?=- Ejection velocity (1) 62- 65 F4.2 10+4km/s e_Vej ?=- rms uncertainty on Vej
Note (1): The blank spaces (---) indicate where a measurement had to be removed due to inadequate wavelength coverage. Note (2): The uncertainties in the EW results include measurement errors, errors from any possible variance in the pseudo-continuum, and the uncertainty from the host galaxy contamination correction.
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 29-Feb-2008
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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