669 research outputs found
The Production Rate of SN Ia Events in Globular Clusters
In globular clusters, dynamical evolution produces luminous X-ray emitting
binaries at a rate about 200 times greater than in the field. If globular
clusters also produce SNe Ia at a high rate, it would account for much of the
SN Ia events in early type galaxies and provide insight into their formation.
Here we use archival HST images of nearby galaxies that have hosted SNe Ia to
examine the rate at which globular clusters produce these events. The location
of the SN Ia is registered on an HST image obtained before the event or after
the supernova faded. Of the 36 nearby galaxies examined, 21 had sufficiently
good data to search for globular cluster hosts. None of the 21 supernovae have
a definite globular cluster counterpart, although there are some ambiguous
cases. This places an upper limit to the enhancement rate of SN Ia production
in globular clusters of about 42 at the 95% confidence level, which is an order
of magnitude lower than the enhancement rate for luminous X-ray binaries. Even
if all of the ambiguous cases are considered as having a globular cluster
counterpart, the upper bound for the enhancement rate is 82 at the 95%
confidence level, excluding an enhancement rate of 200. Barring unforeseen
selection effects, we conclude that globular clusters are not responsible for
producing a significant fraction of the SN Ia events in early-type galaxies.Comment: 28 pages, 5 figures; ApJ submitte
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4He decay of excited states in 14C
A study of the 7Li(9Be,4He 10Be)2H reaction at E{beam}=70 MeV has been
performed using resonant particle spectroscopy techniques and provides the
first measurements of alpha-decaying states in 14C. Excited states are observed
at 14.7, 15.5, 16.4, 18.5, 19.8, 20.6, 21.4, 22.4 and 24.0 MeV. The
experimental technique was able to resolve decays to the various particle bound
states in 10Be, and provides evidence for the preferential decay of the high
energy excited states into states in 10Be at ~6 MeV. The decay processes are
used to indicate the possible cluster structure of the 14C excited states.Comment: accepted for publication in PR
Supersoft X-rays reveal a classical nova in the M 31 globular cluster Bol 126
[Abridged] Classical novae (CNe) represent the main class of supersoft X-ray
sources (SSSs) in the central region of our neighbouring galaxy M 31. Only
three confirmed novae and three SSSs have been discovered in globular clusters
(GCs) of any galaxy so far, of which one nova and two SSSs (including the nova)
were found in M 31 GCs. To study the SSS state of CNe we carried out a
high-cadence X-ray monitoring of the M 31 central area with XMM-Newton and
Chandra. We analysed X-ray and optical data of a new transient X-ray source in
the M 31 GC Bol 126, discovered serendipitously in Swift observations. Our
optical data set was based on regular M 31 monitoring programmes from five
different small telescopes. Additionally, we made use of Pan-STARRS 1 data
obtained during the PAndromeda survey. Our observations reveal that the X-ray
source in Bol 126 is the third SSS in an M 31 GC and can be confirmed as the
second CN in the M 31 GC system. This nova is named M31N 2010-10f. Its
properties in the X-ray and optical regimes agree with a massive white dwarf
(M_WD >~ 1.3 M_sun) in the binary system. Incorporating the data on previously
found (suspected) novae in M 31 GCs we used our high-cadence X-ray monitoring
observations to estimate a tentative nova rate in the M 31 GC system of 0.05
/yr/GC. An optical estimate, based on the recent 10.5-year WeCAPP survey, gives
a lower nova rate, which is compatible with the X-ray rate on the 95%
confidence level. There is growing evidence that the nova rate in GCs is higher
than expected from primordial binary formation and under conditions as in the
field. Dynamical binary formation and/or additional accretion from the
intracluster medium are possible scenarios for an increased nova rate, but
observational confirmation for this enhancement has been absent, so far.
Regular X-ray monitoring observations of M 31 provide a promising strategy to
find these novae.Comment: 14 pages, 6 figures, 3 tables; accepted by Astronomy and Astrophysic
V1647 Orionis: Reinvigorated Accretion and the Re-Appearance of McNeil's Nebula
In late 2003, the young eruptive variable star V1647 Orionis optically
brightened by over 5 magnitudes, stayed bright for around 26 months, and then
decline to its pre-outburst level. In August 2008 the star was reported to have
unexpectedly brightened yet again and we herein present the first detailed
observations of this new outburst. Photometrically, the star is now as bright
as it ever was following the 2003 eruption. Spectroscopically, a pronounced P
Cygni profile is again seen in Halpha with an absorption trough extending to
-700 km/s. In the near-infrared, the spectrum now possesses very weak CO
overtone bandhead absorption in contrast to the strong bandhead emission seen
soon after the 2003 event. Water vapor absorption is also much stronger than
previously seen. We discuss the current outburst below and relate it to the
earlier event.Comment: 6 pages, 3 figure
Transient study of the oxygen reduction reaction on reduced Pt and Pt alloys microelectrodes: evidence for the reduction of pre-adsorbed oxygen species linked to dissolved oxygen
Using chronoamperometry at preconditioned oxide-free Pt microdisc electrodes in aqueous media, we investigated the oxygen reduction reaction (ORR) on the millisecond timescale and obtained results consistent with the reduction of oxygen species which adsorb on the electrode before the ORR is electrochemically driven. Furthermore these adsorbed species are clearly linked to oxygen in solution. At long times, the amperometric response is solely controlled by the diffusion of dissolved oxygen towards the microelectrode. However, at short times, typically below 50 ms, the reduction of pre-adsorbed oxygen produces a large extra current whose magnitude depends on the oxygen concentration in solution, deliberate electrode poisoning and the rest time before the potential step. Using sampled current voltammetry we show that this extra current affects the entire potential range of the ORR. Using microdisc electrodes made with Pt alloys we find that the amperometric response is sufficiently sensitive to distinguish oxygen coverage differences between Pt, Pt0.9Rh0.1 and Pt0.9Ir0.1 microdiscs. These unexpected and, to our knowledge, never previously reported results provide new insight into the oxygen reduction reaction on Pt. The existence over a wide potential range of irreversibly adsorbed oxygen species arising from dissolved oxygen and different from Pt oxide is particularly relevant to the development of oxygen reduction catalysts for low temperature fuel cells
The Young and Bright Type Ia Supernova ASASSN-14lp: Discovery, Early-Time Observations, First-Light Time, Distance to NGC 4666, and Progenitor Constraints
On 2014 Dec. 9.61, the All-Sky Automated Survey for SuperNovae (ASAS-SN or
"Assassin") discovered ASASSN-14lp just days after first light using a
global array of 14-cm diameter telescopes. ASASSN-14lp went on to become a
bright supernova ( mag), second only to SN 2014J for the year. We
present prediscovery photometry (with a detection less than a day after first
light) and ultraviolet through near-infrared photometric and spectroscopic data
covering the rise and fall of ASASSN-14lp for more than 100 days. We find that
ASASSN-14lp had a broad light curve (), a
-band maximum at , a rise time of days, and moderate host--galaxy extinction (). Using ASASSN-14lp we derive a distance modulus for NGC 4666 of
corresponding to a distance of Mpc.
However, adding ASASSN-14lp to the calibrating sample of Type Ia supernovae
still requires an independent distance to the host galaxy. Finally, using our
early-time photometric and spectroscopic observations, we rule out red giant
secondaries and, assuming a favorable viewing angle and explosion time, any
non-degenerate companion larger than .Comment: 12 pages, 9 figures, 4 tables. Accepted to ApJ. Photometric data
presented in this submission are included as an ancillary file. For a brief
video explaining this paper, see https://www.youtube.com/watch?v=1bOV-Cqs-a
Distance determination to 12 Type II-P Supernovae using the Expanding Photosphere Method
We use early-time photometry and spectroscopy of 12 Type II plateau
supernovae (SNe IIP) to derive their distances using the expanding photosphere
method (EPM). We perform this study using two sets of Type II supernova (SN II)
atmosphere models, three filter subsets (, , ), and
two methods for the host-galaxy extinction, which leads to 12 Hubble diagrams.
We find that systematic differences in the atmosphere models lead to 50%
differences in the EPM distances and to a value of between 52 and
101 . Using the filter subset we obtain the
lowest dispersion in the Hubble diagram, { mag}. We
also apply the EPM analysis to the well-observed SN IIP 1999em. With the
filter subset we derive a distance ranging from 9.3 0.5 Mpc to
13.9 1.4 Mpc depending on the atmosphere model employed.Comment: Accepted for publication in the Astrophysical Journa
Optical studies of SN 2009jf: A type Ib supernova with an extremely slow decline and aspherical signature
Optical photometry and medium resolution spectroscopy of the type Ib
supernova SN 2009jf, during the period to +250days with respect to
the maximum are reported. The light curves are broad, with an extremely
slow decline. The early post-maximum decline rate in the band is similar to
SN 2008D, however, the late phase decline rate is slower than other studied
type Ib supernovae. With an absolute magnitude of
magnitude at peak, SN 2009jf is a normally bright supernova. The peak
bolometric luminosity and the energy deposition rate via Ni
Co chain indicate that
M of Ni was ejected during the explosion. He\,I 5876 \AA\ line
is clearly identified in the first spectrum of day , at a velocity of
km sec. The [O\,I] 6300-6364 \AA\ line seen in the nebular
spectrum has a multi-peaked and asymmetric emission profile, with the blue peak
being stronger. The estimated flux in this line implies \ga 1.34 M
oxygen was ejected. The slow evolution of the light curves of SN 2009jf
indicates the presence of a massive ejecta. The high expansion velocity in the
early phase and broader emission lines during the nebular phase suggest it to
be an explosion with a large kinetic energy. A simple qualitative estimate
leads to the ejecta mass of M M, and kinetic energy
E erg. The ejected mass estimate is indicative
of an initial main-sequence mass of \ga 20- 25 M.Comment: 14 pages, 13 figures; accepted for publication in MNRA
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