J/A+A/507/85 ESO/VLT 3rd year type Ia supernova data set (Balland+, 2009)
The ESO/VLT 3rd year type Ia supernova data set from the supernova legacy survey. Balland C., Baumont S., Basa S., Mouchet M., Howell D.A., Astier P., Carlberg R.G., Conley A., Fouchez D., Guy J., Hardin D., Hook I.M., Pain R., Perrett K., Pritchet C.J., Regnault N., Rich J., Sullivan M., Antilogus P., Arsenijevic V., Le Du J., Fabbro S., Lidman C., Mourao A., Palanque-Delabrouille N., Pecontal E., Ruhlmann-Kleider V. <Astron. Astrophys., 507, 85-103 (2009)> =2009A&A...507...85B
ADC_Keywords: Supernovae ; Redshifts Keywords: cosmology: observations - supernovae: general - methods: data analysis - techniques: spectroscopic Abstract: We present 139 spectra of 124 Type Ia supernovae (SNe Ia) that were observed at the ESO/VLT during the first three years of the Canada-France-Hawai Telescope (CFHT) supernova legacy survey (SNLS). This homogeneous data set is used to test for redshift evolution of SN Ia spectra, and will be used in the SNLS 3rd year cosmological analyses. Spectra have been reduced and extracted with a dedicated pipeline that uses photometric information from deep CFHT legacy survey (CFHT-LS) reference images to trace, at sub-pixel accuracy, the position of the supernova on the spectrogram as a function of wavelength. It also separates the supernova and its host light in ∼60% of cases. The identification of the supernova candidates is performed using a spectrophotometric SN Ia model. Description: Spectroscopy of SNLS SN candidates was performed on several 8 to 10-m class telescopes in both hemispheres, namely the VLT, Gemini-N and S, Keck I and II. During the first large program (2003-2005), we performed long slit spectroscopy (LSS) of SN candidates on FORS1 for a total of 60h of dark/grey time per semester. During the second large program (2005-2007), we observed using both FORS1 and FORS2 with the standard collimator in LSS and multi object spectroscopy (MOS) mode. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 73 139 *List of SNLS 3rd year ESO-VLT SN Ia and SN Ia* spectra table2.dat 51 142 Results of identifications of the SNLS 3rd year ESO-VLT SN Ia and SN Ia* spectra
Note on table1.dat: Except for 8 SN Ia taken in MOS mode.
See also: J/A+A/317/423 : Revised photometry of SNIa (Patat, 1997) J/ApJ/607/665 : Type Ia supernovae at z>1 discovered by HST (Riess+, 2004) 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 & low redshifts (Blondin+, 2006) J/ApJ/645/488 : SN type Ia luminosities (Wang+, 2006) J/AJ/133/403 : Light curve of 11 type Ia supernovae (Garg+, 2007) J/ApJ/659/122 : Improved distances to type Ia supernovae (Jha+, 2007) J/A+A/477/717 : Spectroscopy of Type Ia supernovae (Bronder+, 2008) J/MNRAS/389/1871 : Type Ia supernovae candidates from SDSS (Horesh+, 2008) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 6 A6 --- SN SN name (NNANaa) 8- 10 A3 --- n_SN Individual notes (1) 13- 14 I2 h RAh Right ascension (J2000) 16- 17 I2 min RAm Right ascension (J2000) 19- 23 F5.2 s RAs Right ascension (J2000) 25 A1 --- DE- Declination sign (J2000) 26- 27 I2 deg DEd Declination (J2000) 29- 30 I2 arcmin DEm Declination (J2000) 32- 36 F5.2 arcsec DEs Declination (J2000) 38- 47 A10 "YYYY-MM-DD" Date Spectrum date 49- 53 A5 s ExpTime Exposure time 55- 58 F4.2 arcsec Seeing Seeing 60- 63 F4.2 arcsec Dsep ?=- Host-supernova distance (from PHASE model) (2) 65- 68 F4.2 --- Air Air mass 70- 73 F4.1 mag i'mag SDSS i' magnitude
Note (1): Notes as follows: c = Observed with Grism 300I d = SNLS-03D4cy is identified as a SN Ia on the basis of a Gemini spectrum published in Howell et al. (2005ApJ...634.1190H). The VLT spectrum is shown here for reference e = There are two underlying galaxies in the line-of-sight of SNLS-04D1hx f = FORS2 spectrum Note (2): "---" either denotes cases for which a separate extraction of the supernova and the host component was not possible with PHASE or the absence of a detectable host.
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 6 A6 --- SN SN name (NNANaa) 8- 12 A5 --- SpType MK spectral type 14- 18 F5.3 --- z Redshift (of SN or host) 20- 24 F5.3 --- e_z rms uncertainty on z 26 A1 --- n_z [HS] Redshift source (H for Host, S for SN) 28- 31 F4.1 d Phase Phase (time from maximum brightness) 33- 40 A8 --- Mod Host model (1) 42- 45 F4.2 --- Fract ? Fraction of host used in best fitting model 47- 51 F5.2 --- <S/N> Average signal-to-noise ratio per 5Å pixel
Note (1): Host type of the best fitting model. The number in parenthesis is the age of the best fitting PEGASE template (in Gyrs). Two host types separated by a dash indicate that the best fitting host model is an interpolation between two Kinney et al. (1996ApJ...467...38K) templates. The label "NoGalaxy" denotes that the best fitting model is obtained with no host model.
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 05-Feb-2010
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