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 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:
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FileName Lrecl Records Explanations
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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
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Note on table1.dat: Except for 8 SN Ia taken in MOS mode.
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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
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Bytes Format Units Label Explanations
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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
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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 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.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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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
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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 1996ApJ...467...38K)
templates. The label "NoGalaxy" denotes that the best fitting model
is obtained with no host model.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 05-Feb-2010