Spectroscopy of High-Redshift Supernovae from the ESSENCE Project: The First 2 Years

Matheson, T.; Blondin, S.; Foley, R. J.; Chornock, R.; Filippenko, A. V.; Leibundgut, B.; Smith, R. C.; Sollerman, J.; Spyromilio, J.; Kirshner, R.; Clocchiatti, A.; Aguilera, C.; Barris, B.; Becker, A. C.; Challis, Peter; Covarrubias, R.; Garnavich, P.; Hicken, M.; Jha, Saurabh W.; Krisciunas, K.; Li, Weidong; Miceli, Anthony; Miknaitis, G.; Prieto, J. L.; Rest, A.; Riess, Adam G.; Salvo, M.; Schmidt, B. P.; Stubbs, C. W.; Suntzeff, Nicholas B.; Tonry, J.

doi:10.1086/429679

Cited by 61 publications

(118 citation statements)

References 40 publications

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“…We find 86 SN Ia (of which two are SN Ia_pec) and 38 SN Ia in our VLT sample, that is ∼30% of SN Ia . Other surveys such as SDSS-II (Zheng et al 2008) and ESSENCE (Matheson et al 2005) both find about 10% of probable SN Ia (equivalent to our SN Ia ). The SDSS-II survey targets low to intermediate redshifts (0.05 < z < 0.4, z ≈ 0.22), which probably makes identification easier.…”

Section: Discussionsupporting

confidence: 65%

The ESO/VLT 3rd year Type Ia supernova data set from the supernova legacy survey

Balland

Baumont²,

Basa

et al. 2009

A&A

104

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Aims. 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-Hawaï 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. Methods. 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. Results. A total of 124 SNe Ia, roughly 50% of the overall SNLS spectroscopic sample, have been identified using the ESO/VLT during the first three years of the survey. Their redshifts range from z = 0.149 to z = 1.031. The average redshift of the sample is z = 0.63 ± 0.02. This constitutes the largest SN Ia spectral set to date in this redshift range. The spectra are presented along with their best-fit spectral SN Ia model and a host model where relevant. In the latter case, a host subtracted spectrum is also presented. We produce average spectra for pre-maximum, maximum and post-maximum epochs for both z < 0.5 and z ≥ 0.5 SNe Ia. We find that z < 0.5 spectra have deeper intermediate mass element absorptions than z ≥ 0.5 spectra. The differences with redshift are consistent with the selection of brighter and bluer supernovae at higher redshift.

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Section: Discussionsupporting

confidence: 65%

The ESO/VLT 3rd year Type Ia supernova data set from the supernova legacy survey

Balland

Baumont²,

Basa

et al. 2009

A&A

104

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“…For lower values (r ≈ 3), we additionally required a spectrum/template spectral overlap >60% (lower overlap values usually indicate a poor type and redshift range) and/or a host with a spectroscopic classification of E/S0. A requirement of r 3 for SN Ia identification has also been adopted by other groups (Blondin et al 2007;Blondin & Tonry 2007;Matheson et al 2005). When these criteria are satisfied, we designate the SN as Type Ia ("Ia").…”

Section: Cross-correlation Analysismentioning

confidence: 99%

“…However, this latter approach sometimes fails, yielding only a low-S/N detection of the SN spectrum. In such cases, it is common to resort to a crosscorrelation technique similar to that used above (Matheson et al 2005). …”

Section: Spectral Decomposition and Host-galaxy Subtractionmentioning

confidence: 99%

First-Year Spectroscopy for the Sloan Digital Sky Survey-Ii Supernova Survey

Zheng¹,

Romani²,

Šako³

et al. 2008

The Astronomical Journal

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This paper presents spectroscopy of supernovae (SNe) discovered in the first season of the Sloan Digital Sky Survey-II SN Survey. This program searches for and measures multi-band light curves of SNe in the redshift range z = 0.05-0.4, complementing existing surveys at lower and higher redshifts. Our goal is to better characterize the SN population, with a particular focus on SNe Ia, improving their utility as cosmological distance indicators and as probes of dark energy. Our SN spectroscopy program features rapid-response observations using telescopes of a range of apertures, and provides confirmation of the SN and host-galaxy types as well as precise redshifts. 1766No. 5, 2008 SDSS-II SN SURVEY SPECTROSCOPY 1767We describe here the target identification and prioritization, data reduction, redshift measurement, and classification of 129 SNe Ia, 16 spectroscopically probable SNe Ia, 7 SNe Ib/c, and 11 SNe II from the first season. We also describe our efforts to measure and remove the substantial host-galaxy contamination existing in the majority of our SN spectra.

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“…We have selected high-redshift SN Ia spectra taken by members of the ESSENCE team [16,17], for which a redshift of the host galaxy could be obtained. This amounts to 47 SN Ia spectra in the redshift range 0.164 ≤ z ≤ 0.781.…”

Section: Redshift and Phase Determinationmentioning

confidence: 99%

Determining the Type, Redshift, and Phase of a Supernova Spectrum

Blondin¹,

Tonry²

2007

AIP Conference Proceedings

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Abstract. We present an algorithm to identify the types of supernova spectra, and determine their redshift and phase. This algorithm, based on the correlation techniques of Tonry & Davis, is implemented in the SuperNova IDentification code (SNID). It is used by members of the ESSENCE project to determine whether a noisy spectrum of a high-redshift supernova is indeed of type Ia, as opposed to, e.g., type Ib/c. Furthermore, by comparing the correlation redshifts obtained using SNID with those determined from narrow lines in the supernova host galaxy spectrum, we show that accurate redshifts (with a typical error σ z 0.01) can be determined for SNe Ia for which a spectrum of the host galaxy is unavailable. Last, the phase of an input spectrum is determined with a typical accuracy of σ t 3 days.

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Spectroscopy of High-Redshift Supernovae from the ESSENCE Project: The First 2 Years

Cited by 61 publications

References 40 publications

The ESO/VLT 3rd year Type Ia supernova data set from the supernova legacy survey

The ESO/VLT 3rd year Type Ia supernova data set from the supernova legacy survey

First-Year Spectroscopy for the Sloan Digital Sky Survey-Ii Supernova Survey

Determining the Type, Redshift, and Phase of a Supernova Spectrum

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