188 research outputs found
Supernova Discoveries 2010-2011: Statistics and Trends
We have inspected all supernova discoveries reported during 2010 and 2011
(538 and 926 events, respectively). We examine the statistics of all discovered
objects, as well as those of the subset of spectroscopically-confirmed events.
In these two years we see the rise of wide-field non-targeted supernova surveys
to prominence, with the largest numbers of events reported by the CRTS and PTF
surveys (572 and 393 events in total respectively, contributing together 74% of
all reported discoveries in 2011), followed by the integrated contribution of
numerous amateurs (184 events). Among spectroscopically-confirmed events the
PTF (393 events) leads, followed by CRTS (170 events), and amateur discoveries
(144 events). Traditional galaxy-targeted surveys, such as LOSS and CHASE,
maintain a strong contribution (86 and 61 events, respectively) with high
spectroscopic completeness (~90% per cent). It is interesting to note that the
community managed to provide substantial spectroscopic follow-up for relatively
brighter amateur discoveries (=16.5 mag), but significant less help for
fainter (and much more numerous) events promptly released by the CRTS (=18.6
mag). Inspecting discovery magnitude and redshift distributions we find that
PS1 discoveries have similar properties (=21.6 mag, =0.23) to events
found in previous seasons by cosmology-oriented projects (e.g., SDSS-II), while
PTF (=19.2 mag, =0.095) and CRTS (=18.6 mag, =0.049) populate the
relatively unexplored phase space of faint SNe (>19 mag) in nearby galaxies
(mainly PTF), and events at 0.05<z<0.2 (CRTS and PTF). Examining the specific
question of reporting channels over the previous dozen years, we find that
traditional reports via CBET telegrams now account only for a minority of SN
discoveries.Comment: PASP, in pres
Affiliation-Hiding Authentication with Minimal Bandwidth Consumption
Part 3: Lightweight AuthenticationInternational audienceAffiliation-Hiding Authentication (AHA) protocols have the seemingly contradictory property of enabling users to authenticate each other as members of certain groups, without revealing their affiliation to group outsiders. Of particular interest in practice is the group-discovering variant, which handles multiple group memberships per user. Corresponding solutions were only recently introduced, and have two major drawbacks: high bandwidth consumption (typically several kilobits per user and affiliation), and only moderate performance in scenarios of practical application.While prior protocols have O(n2) time complexity, where n denotes the number of affiliations per user, we introduce a new AHA protocol running in O(nlogn) time. In addition, the bandwidth consumed is considerably reduced. We consider these advances a major step towards deployment of privacy-preserving methods in constraint devices, like mobile phones, to which the economization of these resources is priceless
DSH: Deniable secret handshake framework
National Research Foundation (NRF) Singapor
The Centurion 18 telescope of the Wise Observatory
We describe the second telescope of the Wise Observatory, a 0.46-m Centurion
18 (C18) installed in 2005, which enhances significantly the observing
possibilities. The telescope operates from a small dome and is equipped with a
large-format CCD camera. In the last two years this telescope was intensively
used in a variety of monitoring projects.
The operation of the C18 is now automatic, requiring only start-up at the
beginning of a night and close-down at dawn. The observations are mostly
performed remotely from the Tel Aviv campus or even from the observer's home.
The entire facility was erected for a component cost of about 70k$ and a labor
investment of a total of one man-year.
We describe three types of projects undertaken with this new facility: the
measurement of asteroid light variability with the purpose of determining
physical parameters and binarity, the following-up of transiting extrasolar
planets, and the study of AGN variability. The successful implementation of the
C18 demonstrates the viability of small telescopes in an age of huge
light-collectors, provided the operation of such facilities is very efficient.Comment: 16 pages, 13 figures, some figures quality was degraded, accepted for
publication in Astrophysics and Space Scienc
Study of the plutino object (208996) 2003 AZ84 from stellar occultations: size, shape and topographic features
We present results derived from four stellar occultations by the plutino
object (208996) 2003~AZ, detected at January 8, 2011 (single-chord
event), February 3, 2012 (multi-chord), December 2, 2013 (single-chord) and
November 15, 2014 (multi-chord). Our observations rule out an oblate spheroid
solution for 2003~AZ's shape. Instead, assuming hydrostatic equilibrium,
we find that a Jacobi triaxial solution with semi axes ~km % axis ratios and
, can better account for all our occultation observations.
Combining these dimensions with the rotation period of the body (6.75~h) and
the amplitude of its rotation light curve, we derive a density ~g~cm a geometric albedo . A grazing chord
observed during the 2014 occultation reveals a topographic feature along
2003~AZ's limb, that can be interpreted as an abrupt chasm of width
~km and depth ~km or a smooth depression of width ~km
and depth ~km (or an intermediate feature between those two extremes)
PTF11eon/SN2011dh: Discovery of a Type IIb Supernova From a Compact Progenitor in the Nearby Galaxy M51
On May 31, 2011 UT a supernova (SN) exploded in the nearby galaxy M51 (the
Whirlpool Galaxy). We discovered this event using small telescopes equipped
with CCD cameras, as well as by the Palomar Transient Factory (PTF) survey, and
rapidly confirmed it to be a Type II supernova. Our early light curve and
spectroscopy indicates that PTF11eon resulted from the explosion of a
relatively compact progenitor star as evidenced by the rapid shock-breakout
cooling seen in the light curve, the relatively low temperature in early-time
spectra and the prompt appearance of low-ionization spectral features. The
spectra of PTF11eon are dominated by H lines out to day 10 after explosion, but
initial signs of He appear to be present. Assuming that He lines continue to
develop in the near future, this SN is likely a member of the cIIb (compact
IIb; Chevalier and Soderberg 2010) class, with progenitor radius larger than
that of SN 2008ax and smaller than the eIIb (extended IIb) SN 1993J progenitor.
Our data imply that the object identified in pre-explosion Hubble Space
Telescope images at the SN location is possibly a companion to the progenitor
or a blended source, and not the progenitor star itself, as its radius (~10^13
cm) would be highly inconsistent with constraints from our post-explosion
photometric and spectroscopic data
PTF11rka: an interacting supernova at the crossroads of stripped-envelope and H-poor superluminous stellar core collapses
The hydrogen-poor supernova (SN) PTF11rka (z = 0.0744), reported by the Palomar Transient Factory, was observed with various telescopes starting a few days after the estimated explosion time of 2011 December 5 UT and up to 432 rest-frame days thereafter. The rising part of the light curve was monitored only in the R_(PTF) filter band, and maximum in this band was reached âŒ30 rest-frame days after the estimated explosion time. The light curve and spectra of PTF11rka are consistent with the core-collapse explosion of a âŒ10 M_â carbonâoxygen core evolved from a progenitor of main-sequence mass 25â40 M_â, that liberated a kinetic energy E_k â 4 Ă 10â”Âč erg, expelled âŒ8 M_â of ejecta, and synthesized âŒ0.5 M_â of â”â¶Ni. The photospheric spectra of PTF11rka are characterized by narrow absorption lines that point to suppression of the highest ejecta velocities (âł 15â000âkm sâ»Âč). This would be expected if the ejecta impacted a dense, clumpy circumstellar medium. This in turn caused them to lose a fraction of their energy (âŒ5 Ă 10â”â° erg), less than 2 per cent of which was converted into radiation that sustained the light curve before maximum brightness. This is reminiscent of the superluminous SN 2007bi, the light-curve shape and spectra of which are very similar to those of PTF11rka, although the latter is a factor of 10 less luminous and evolves faster in time. PTF11rka is in fact more similar to gamma-ray burst SNe in luminosity, although it has a lower energy and a lower E_k/M_(ej) ratio
PTF11rka: an interacting supernova at the crossroads of stripped-envelope and H-poor superluminous stellar core collapses
The hydrogen-poor supernova PTF11rka (z = 0.0744), reported by the Palomar Transient Factory, was observed with various telescopes starting a few days after the estimated explosion time of 2011 Dec. 5 UT and up to 432 rest-frame days thereafter. The rising part of the light curve was monitored only in the R_PTF filter band, and maximum in this band was reached ~30 rest-frame days after the estimated explosion time. The light curve and spectra of PTF11rka are consistent with the core-collapse explosion of a ~10 Msun carbon-oxygen core evolved from a progenitor of main-sequence mass 25--40 Msun, that liberated a kinetic energy (KE) ~ 4 x 10^{51} erg, expelled ~8 Msun of ejecta (Mej), and synthesised ~0.5 Msun of 56Nichel. The photospheric spectra of PTF11rka are characterised by narrow absorption lines that point to suppression of the highest ejecta velocities ~>15,000 km/s. This would be expected if the ejecta impacted a dense, clumpy circumstellar medium. This in turn caused them to lose a fraction of their energy (~5 x 10^50 erg), less than 2% of which was converted into radiation that sustained the light curve before maximum brightness. This is reminiscent of the superluminous SN 2007bi, the light-curve shape and spectra of which are very similar to those of PTF11rka, although the latter is a factor of 10 less luminous and evolves faster in time. PTF11rka is in fact more similar to gamma-ray burst supernovae (GRB-SNe) in luminosity, although it has a lower energy and a lower KE/Mej ratio
MOA-2011-BLG-293Lb: A test of pure survey microlensing planet detections
Because of the development of large-format, wide-field cameras, microlensing
surveys are now able to monitor millions of stars with sufficient cadence to
detect planets. These new discoveries will span the full range of significance
levels including planetary signals too small to be distinguished from the
noise. At present, we do not understand where the threshold is for detecting
planets. MOA-2011-BLG-293Lb is the first planet to be published from the new
surveys, and it also has substantial followup observations. This planet is
robustly detected in survey+followup data (Delta chi^2 ~ 5400). The planet/host
mass ratio is q=5.3+/- 0.2*10^{-3}. The best fit projected separation is
s=0.548+/- 0.005 Einstein radii. However, due to the s-->s^{-1} degeneracy,
projected separations of s^{-1} are only marginally disfavored at Delta
chi^2=3. A Bayesian estimate of the host mass gives M_L = 0.43^{+0.27}_{-0.17}
M_Sun, with a sharp upper limit of M_L < 1.2 M_Sun from upper limits on the
lens flux. Hence, the planet mass is m_p=2.4^{+1.5}_{-0.9} M_Jup, and the
physical projected separation is either r_perp = ~1.0 AU or r_perp = ~3.4 AU.
We show that survey data alone predict this solution and are able to
characterize the planet, but the Delta chi^2 is much smaller (Delta chi^2~500)
than with the followup data. The Delta chi^2 for the survey data alone is
smaller than for any other securely detected planet. This event suggests a
means to probe the detection threshold, by analyzing a large sample of events
like MOA-2011-BLG-293, which have both followup data and high cadence survey
data, to provide a guide for the interpretation of pure survey microlensing
data.Comment: 29 pages, 6 figures, Replaced 7/3/12 with the version accepted to Ap
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