901 research outputs found
On the Rates of Type Ia Supernovae in Dwarf and Giant Hosts with ROTSE-IIIb
We present a sample of 23 spectroscopically confirmed Type Ia supernovae that
were discovered in the background of galaxy clusters targeted by ROTSE-IIIb and
use up to 18 of these to determine the local (z = 0.05) volumetric rate. Since
our survey is flux limited and thus biased against fainter objects, the
pseudo-absolute magnitude distribution (pAMD) of SNeIa in a given volume is an
important concern, especially the relative frequency of high to low-luminosity
SNeIa. We find that the pAMD derived from the volume limited Lick Observatory
Supernova Search (LOSS) sample is incompatible with the distribution of SNeIa
in a volume limited (z<0.12) sub sample of the SDSS-II. The LOSS sample
requires far more low-luminosity SNeIa than the SDSS-II can accommodate. Even
though LOSS and SDSS-II have sampled different SNeIa populations, their
volumetric rates are surprisingly similar. Using the same model pAMD adopted in
the SDSS-II SNeIa rate calculation and excluding two high-luminosity SNeIa from
our sample, we derive a rate that is marginally higher than previous
low-redshift determinations. With our full sample and the LOSS pAMD our rate is
more than double the canonical value. We also find that 5 of our 18 SNeIa are
hosted by very low-luminosity (M_B > -16) galaxies, whereas only 1 out 79
nearby SDSS-II SNeIa have such faint hosts. It is possible that previous works
have under-counted either low luminosity SNeIa, SNeIa in low luminosity hosts,
or peculiar SNeIa (sometimes explicitly), and the total SNeIa rate may be
higher than the canonical value.Comment: 18 pages; accepted for publication in The Astronomical Journa
SN 2010jl in UGC 5189: Yet another luminous type IIn supernova in a metal-poor galaxy
We present ASAS data starting 25 days before the discovery of the recent type
IIn SN 2010jl, and we compare its light curve to other luminous IIn SNe,
showing that it is a luminous (M_I ~ -20.5) event. Its host galaxy, UGC 5189,
has a low gas-phase oxygen abundance (12 + log(O/H) = 8.2), which reinforces
the emerging trend that over-luminous core-collapse supernovae are found in the
low-metallicity tail of the galaxy distribution, similar to the known trend for
the hosts of long GRBs. We compile oxygen abundances from the literature and
from our own observations of UGC 5189, and we present an unpublished spectrum
of the luminous type Ic SN 2010gx that we use to estimate its host metallicity.
We discuss these in the context of host metallicity trends for different
classes of core-collapse objects. The earliest generations of stars are known
to be enhanced in [O/Fe] relative to the Solar mixture; it is therefore likely
that the stellar progenitors of these overluminous supernovae are even more
iron-poor than they are oxygen-poor. A number of mechanisms and massive star
progenitor systems have been proposed to explain the most luminous
core-collapse supernovae; any successful theory will need to include the
emerging trend that points towards low-metallicity for the massive progenitor
stars. This trend for very luminous supernovae to strongly prefer
low-metallicity galaxies should be taken into account when considering various
aspects of the evolution of the metal-poor early universe. (abridged)Comment: 27 pages, 7 figures, 2 tables. Accepted for publication in Ap
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An evaluation of a pre-charging pulse-jet filter for small combustor particulate control
The objective of this test program is the performance and economic evaluation of a pre-charged-pulse jet filter as the principal particulate control device for a commercial or industrial scale coal fired combustor. Performance factors that will be considered are the effects of particle charge, air/cloth ratio, fabric types, percent humidity and inlet particulate loading on fine particle collection efficiency, and pressure drop. Economic factors that will be considered are capital costs, energy and other operating costs, and maintenance costs. The program will result in a recommendation regarding the relative suitability of the pre charged pulse-jet filter for small combustor particulate control, as compared to other control devices. Fine particle control capability, ease of operation, and overall economics will be taken into consideration in making comparisons
The Impact of Reliable Symmetries on Pipelined Cryptoanalysis
Fiber-optic cables must work. In our research, authors disconfirm the synthesis of kernels. We explore new “fuzzy” technology, which we call Hug
SN 2006bp: Probing the Shock Breakout of a Type II-P Supernova
HET optical spectroscopy and unfiltered ROTSE-III photometry spanning the
first 11 months since explosion of the Type II-P SN 2006bp are presented. Flux
limits from the days before discovery combined with the initial rapid
brightening suggest the supernova was first detected just hours after shock
breakout. Optical spectra obtained about 2 days after breakout exhibit narrow
emission lines corresponding to HeII 4200, HeII 4686, and CIV 5805 in the rest
frame, and these features persist in a second observation obtained 5 hours
later; however, these emission lines are not detected the following night nor
in subsequent observations. We suggest that these lines emanate from material
close to the explosion site, possibly in the outer layers of the progenitor
that have been ionized by the high energy photons released at shock breakout. A
P-Cygni profile is observed around 4450 A in the +2 and +3 day spectra.
Previous studies have attributed this feature to high velocity H-beta, but we
discuss the possibility that this profile is instead due to HeII 4687. Further
HET observations (14 nights in total) covering the spectral evolution across
the photometric plateau up to 73 days after breakout and during the nebular
phase around day +340 are presented, and expansion velocities are derived for
key features. The measured decay slope for the unfiltered light curve is 0.0073
+/- 0.0004 mag/day between days +121 and +335, which is significantly slower
than the decay of rate 56Co. We combine our HET measurements with published
X-ray, UV, and optical data to obtain a quasi-bolometric light curve through
day +60. We see a slow cooling over the first 25 days, but no sign of an early
sharp peak; any such feature from the shock breakout must have lasted less than
~1 day.[ABRIDGED]Comment: ApJ accepted, 43 page
The Exceptionally Luminous Type Ia Supernova 2007If
SN 2007if was the third over-luminous Type Ia supernova (SN Ia) detected after 2003fg and 2006gz. We present the photometric and spectroscopic observations of the SN and its host by ROTSE-III, HET, and Keck. From the H a line identified in the host spectra, we determine a redshift of 0.0736. At this distance, the SN reached an absolute magnitude of -20.4, brighter than any other SNe Ia ever observed. If the source of luminosity is radioactive decay, a large amount of radioactive nickel (similar to 1.5 M(circle dot)) is required to power the peak luminosity, more than can be produced realistically in a Chandrasekhar mass progenitor. Low expansion velocity, similar to that of 2003fg, is also measured around the maximum light. The observations may suggest that SN 2007if was from a massive white dwarf progenitor, plausibly exploding with mass well beyond 1.4 M(circle dot). Alternatively, we investigate circumstellar interaction that may contribute to the excess luminosity.NASA NNX-08AN25G, NNX-08AV63GNSF AST-0707769, PHY-0801007Australian Research CouncilUniversity of New South WalesUniversity of TexasUniversity of MichiganAstronom
Discovery of the Ultra-Bright Type II-L Supernova 2008es
We report the discovery by the Robotic Optical Transient Experiment
(ROTSE-IIIb) telescope of SN 2008es, an overluminous supernova (SN) at z=0.205
with a peak visual magnitude of -22.2. We present multiwavelength follow-up
observations with the Swift satellite and several ground-based optical
telescopes. The ROTSE-IIIb observations constrain the time of explosion to be
23+/-1 rest-frame days before maximum. The linear decay of the optical light
curve, and the combination of a symmetric, broad H\alpha emission line profile
with broad P Cygni H\beta and Na I \lambda5892 profiles, are properties
reminiscent of the bright Type II-L SNe 1979C and 1980K, although SN 2008es is
greater than 10 times more luminous. The host galaxy is undetected in
pre-supernova Sloan Digital Sky Survey images, and similar to Type II-L SN
2005ap (the most luminous SN ever observed), the host is most likely a dwarf
galaxy with M_r > -17. Swift Ultraviolet/Optical Telescope observations in
combination with Palomar photometry measure the SED of the SN from 200 to 800
nm to be a blackbody that cools from a temperature of 14,000 K at the time of
the optical peak to 6400 K 65 days later. The inferred blackbody radius is in
good agreement with the radius expected for the expansion speed measured from
the broad lines (10,000 km/s). The bolometric luminosity at the optical peak is
2.8 x 10^44 erg/s, with a total energy radiated over the next 65 days of 5.6 x
10^50 erg. We favor a model in which the exceptional peak luminosity is a
consequence of the core-collapse explosion of a progenitor star with a low-mass
extended hydrogen envelope and a stellar wind with a density close to the upper
limit on the mass-loss rate measured from the lack of an X-ray detection by the
Swift X-Ray Telescope. (Abridged).Comment: Accepted to ApJ, 14 pages, 7 figures, 3 tables, emulateapj,
corrections from proofs adde
Far-Ultraviolet to Near-Infrared Spectroscopy of A Nearby Hydrogen Poor Superluminous Supernova Gaia16apd
We report the first maximum-light far-Ultraviolet to near-infrared spectra
(1000A - 1.62um, rest) of a H-poor superluminous supernova, Gaia16apd. At
z=0.1018, it is one of the closest and the UV brightest such events, with 17.4
(AB) magnitude in Swift UV band (1928A) at -11days pre-maximum. Assuming an
exponential form, we derived the rise time of 33days and the peak bolometric
luminosity of 3x10^{44}ergs^-1. At maximum light, the estimated photospheric
temperature and velocity are 17,000K and 14,000kms^-1 respectively. The
inferred radiative and kinetic energy are roughly 1x10^{51} and 2x10^{52}erg.
Gaia16apd is extremely UV luminous, emitting 50% of its total luminosity at
1000 - 2500A. Compared to the UV spectra (normalized at 3100A) of well studied
SN1992A (Ia), SN2011fe(Ia), SN1999em (IIP) and SN1993J (IIb), it has orders of
magnitude more far-UV emission. This excess is interpreted primarily as a
result of weaker metal line blanketing due to much lower abundance of
iron-group elements in the outer ejecta. Because these elements originate
either from the natal metallicity of the star, or have been newly produced, our
observation provides direct evidence that little of these freshly synthesized
material, including 56Ni, was mixed into the outer ejecta, and the progenitor
metallicity is likely sub-solar. This disfavors Pair-Instability Supernova
(PISN) models with Helium core masses >=90Msun, where substantial 56Ni material
is produced. Higher photospheric temperature of Gaia16apd than that of normal
SNe may also contribute to the observed far-UV excess. We find some indication
that UV luminous SLSNe-I like Gaia16apd could be common. Using the UV spectra,
we show that WFIRST could detect SLSNe-I out to redshift of 8.Comment: 19 pages. Match with the version accepted in Ap
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