197 research outputs found
Photometric selection of high-redshift type Ia supernovae
We present a method for selecting high-redshift type Ia supernovae (SNe Ia)
located via rolling SN searches. The technique, using both color and magnitude
information of events from only 2-3 epochs of multi-band real-time photometry,
is able to discriminate between SNe Ia and core collapse SNe. Furthermore, for
the SNe Ia, the method accurately predicts the redshift, phase and light-curve
parameterization of these events based only on pre-maximum-light data. We
demonstrate the effectiveness of the technique on a simulated survey of SNe Ia
and core-collapse SNe, where the selection method effectively rejects most
core-collapse SNe while retaining SNe Ia. We also apply the selection code to
real-time data acquired as part of the Canada-France-Hawaii Telescope Supernova
Legacy Survey (SNLS). During the period May 2004 to January 2005 in the SNLS,
440 SN candidates were discovered of which 70 were confirmed spectroscopically
as SNe Ia and 15 as core-collapse events. For this test dataset, the selection
technique correctly identifies 100% of the identified SNe II as non-SNe Ia with
only a 1-2% false rejection rate. The predicted parameterization of the SNe Ia
has a precision of |delta_z|/(1+z_spec)<0.09 in redshift, and +/- 2-3
rest-frame days in phase, providing invaluable information for planning
spectroscopic follow-up observations. We also investigate any bias introduced
by this selection method on the ability of surveys such as SNLS to measure
cosmological parameters (e.g., w and omega matter), and find any effect to be
negligible.Comment: Accepted for publication in A
Gemini Spectroscopy of Supernovae from SNLS: Improving High Redshift SN Selection and Classification
We present new techiques for improving the efficiency of supernova (SN)
classification at high redshift using 64 candidates observed at Gemini North
and South during the first year of the Supernova Legacy Survey (SNLS). The SNLS
is an ongoing five year project with the goal of measuring the equation of
state of Dark Energy by discovering and following over 700 high-redshift SNe Ia
using data from the Canada-France-Hawaii Telescope Legacy Survey. We achieve an
improvement in the SN Ia spectroscopic confirmation rate: at Gemini 71% of
candidates are now confirmed as SNe Ia, compared to 54% using the methods of
previous surveys. This is despite the comparatively high redshift of this
sample, where the median SN Ia redshift is z=0.81 (0.155 <= z <= 1.01). These
improvements were realized because we use the unprecedented color coverage and
lightcurve sampling of the SNLS to predict whether a candidate is an SN Ia and
estimate its redshift, before obtaining a spectrum, using a new technique
called the "SN photo-z." In addition, we have improved techniques for galaxy
subtraction and SN template chi^2 fitting, allowing us to identify candidates
even when they are only 15% as bright as the host galaxy. The largest
impediment to SN identification is found to be host galaxy contamination of the
spectrum -- when the SN was at least as bright as the underlying host galaxy
the target was identified more than 90% of the time. However, even SNe on
bright host galaxies can be easily identified in good seeing conditions. When
the image quality was better than 0.55 arcsec the candidate was identified 88%
of the time. Over the five-year course of the survey, using the selection
techniques presented here we will be able to add approximately 170 more
confirmed SNe Ia than would be possible using previous methods.Comment: ApJ, accepted, 19 pages, 9 figure
Background Light in Potential Sites for the ANTARES Undersea Neutrino Telescope
The ANTARES collaboration has performed a series of {\em in situ}
measurements to study the background light for a planned undersea neutrino
telescope. Such background can be caused by K decays or by biological
activity. We report on measurements at two sites in the Mediterranean Sea at
depths of 2400~m and 2700~m, respectively. Three photomultiplier tubes were
used to measure single counting rates and coincidence rates for pairs of tubes
at various distances. The background rate is seen to consist of three
components: a constant rate due to K decays, a continuum rate that
varies on a time scale of several hours simultaneously over distances up to at
least 40~m, and random bursts a few seconds long that are only correlated in
time over distances of the order of a meter. A trigger requiring coincidences
between nearby photomultiplier tubes should reduce the trigger rate for a
neutrino telescope to a manageable level with only a small loss in efficiency.Comment: 18 pages, 8 figures, accepted for publication in Astroparticle
Physic
The Supernova Legacy Survey: Measurement of Omega_M, Omega_Lambda and w from the First Year Data Set
We present distance measurements to 71 high redshift type Ia supernovae
discovered during the first year of the 5-year Supernova Legacy Survey (SNLS).
These events were detected and their multi-color light-curves measured using
the MegaPrime/MegaCam instrument at the Canada-France-Hawaii Telescope (CFHT),
by repeatedly imaging four one-square degree fields in four bands. Follow-up
spectroscopy was performed at the VLT, Gemini and Keck telescopes to confirm
the nature of the supernovae and to measure their redshift. With this data set,
we have built a Hubble diagram extending to z=1, with all distance measurements
involving at least two bands. Systematic uncertainties are evaluated making use
of the multi-band photometry obtained at CFHT. Cosmological fits to this first
year SNLS Hubble diagram give the following results : Omega_M = 0.263 +/-
0.042(stat) +/- 0.032(sys) for a flat LambdaCDM model; and w = -1.023 +/-
0.090(stat) +/- 0.054(sys) for a flat cosmology with constant equation of state
w when combined with the constraint from the recent Sloan Digital Sky Survey
measurement of baryon acoustic oscillations.Comment: (The SNLS Collaboration) 24 pages, 13 figures, Accepted in A&A.
Computer readable tables at http://snls.in2p3.fr/conf/papers/cosmo1
Performance of the front-end electronics of the ANTARES neutrino telescope
ANTARES is a high-energy neutrino telescope installed in the Mediterranean
Sea at a depth of 2475 m. It consists of a three-dimensional array of optical
modules, each containing a large photomultiplier tube. A total of 2700
front-end ASICs named Analogue Ring Samplers (ARS) process the phototube
signals, measure their arrival time, amplitude and shape as well as perform
monitoring and calibration tasks. The ARS chip processes the analogue signals
from the optical modules and converts information into digital data. All the
information is transmitted to shore through further multiplexing electronics
and an optical link. This paper describes the performance of the ARS chip;
results from the functionality and characterization tests in the laboratory are
summarized and the long-term performance in the apparatus is illustrated.Comment: 20 pages, 22 figures, published in Nuclear Instruments and Methods
First results of the Instrumentation Line for the deep-sea ANTARES neutrino telescope
In 2005, the ANTARES Collaboration deployed and operated at a depth of 2500 m a so-called Mini Instrumentation Line equipped with Optical Modules (MILOM) at the ANTARES site. The various data acquired during the continuous operation from April to December 2005 of the MILOM confirm the satisfactory performance of the Optical Modules, their front-end electronics and readout system. as well as the calibration devices of the detector. The in situ measurement of the Optical Module time response yields a resolution better than 0.5 ns. The performance of the acoustic positioning system, which enables the spatial reconstruction of the ANTARES detector with a precision of about 10 cm, is verified. These results demonstrate that with the full ANTARES neutrino telescope the design angular resolution of better than 0.3 degrees can be realistically achieved
The data acquisition system for the ANTARES neutrino telescope
The ANTARES neutrino telescope is being constructed in the Mediterranean Sea.
It consists of a large three-dimensional array of photo-multiplier tubes. The
data acquisition system of the detector takes care of the digitisation of the
photo-multiplier tube signals, data transport, data filtering, and data
storage. The detector is operated using a control program interfaced with all
elements. The design and the implementation of the data acquisition system are
described.Comment: 20 pages, 6 figures, accepted for publication in Nucl. Instrum. Meth.
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