114 research outputs found
Improved distance determination to M51 from supernovae 2011dh and 2005cs
The appearance of two recent supernovae, SN 2011dh and 2005cs, both in M51,
provides an opportunity to derive an improved distance to their host galaxy by
combining the observations of both SNe. We apply the Expanding Photosphere
Method to get the distance to M51 by fitting the data of these two SNe
simultaneously. In order to correct for the effect of flux dilution, we use
correction factors (zeta) appropriate for standard type II-P SNe atmospheres
for 2005cs, but find zeta ~ 1 for the type IIb SN 2011dh, which may be due to
the reduced H-content of its ejecta. The EPM analysis resulted in D_M51 = 8.4
+/- 0.7 Mpc. Based on this improved distance, we also re-analyze the HST
observations of the proposed progenitor of SN 2011dh. We confirm that the
object detected on the pre-explosion HST-images is unlikely to be a compact
stellar cluster. In addition, its derived radius (~ 277$ R_sun) is too large
for being the real (exploded) progenitor of SN 2011dh. The supernova-based
distance, D = 8.4 Mpc, is in good agreement with other recent distance
estimates to M51.Comment: 6 pages, 5 figures, accepted for publication in A&
Interacting supernovae and supernova impostors. SN 2007sv: the major eruption of a massive star in UGC 5979
We report the results of the photometric and spectroscopic monitoring
campaign of the transient SN 2007sv. The observables are similar to those of
type IIn supernovae, a well-known class of objects whose ejecta interact with
pre-existing circum-stellar material. The spectra show a blue continuum at
early phases and prominent Balmer lines in emission, however, the absolute
magnitude at the discovery of SN 2007sv (M_R = - 14.25 +/- 0.38) indicate it to
be most likely a supernova impostor. This classification is also supported by
the lack of evidence in the spectra of very high velocity material as expected
in supernova ejecta. In addition we find no unequivocal evidence of broad lines
of alpha - and/or Fe-peak elements. The comparison with the absolute light
curves of other interacting objects (including type IIn supernovae) highlights
the overall similarity with the prototypical impostor SN 1997bs. This supports
our claim that SN 2007sv was not a genuine supernova, and was instead a
supernova impostor, most likely similar to the major eruption of a luminous
blue variable.Comment: Accepted for publication in MNRAS. 15 pages, 11 figures, 5 table
Three-Dimensional Simulations of Mixing Instabilities in Supernova Explosions
We present the first three-dimensional (3D) simulations of the large-scale
mixing that takes place in the shock-heated stellar layers ejected in the
explosion of a 15.5 solar-mass blue supergiant star. The outgoing supernova
shock is followed from its launch by neutrino heating until it breaks out from
the stellar surface more than two hours after the core collapse. Violent
convective overturn in the post-shock layer causes the explosion to start with
significant asphericity, which triggers the growth of Rayleigh-Taylor (RT)
instabilities at the composition interfaces of the exploding star. Deep inward
mixing of hydrogen (H) is found as well as fast-moving, metal-rich clumps
penetrating with high velocities far into the H-envelope of the star as
observed, e.g., in the case of SN 1987A. Also individual clumps containing a
sizeable fraction of the ejected iron-group elements (up to several 0.001 solar
masses) are obtained in some models. The metal core of the progenitor is
partially turned over with Ni-dominated fingers overtaking oxygen-rich bullets
and both Ni and O moving well ahead of the material from the carbon layer.
Comparing with corresponding 2D (axially symmetric) calculations, we determine
the growth of the RT fingers to be faster, the deceleration of the dense
metal-carrying clumps in the He and H layers to be reduced, the asymptotic
clump velocities in the H-shell to be higher (up to ~4500 km/s for the
considered progenitor and an explosion energy of 10^{51} ergs, instead of <2000
km/s in 2D), and the outward radial mixing of heavy elements and inward mixing
of hydrogen to be more efficient in 3D than in 2D. We present a simple argument
that explains these results as a consequence of the different action of drag
forces on moving objects in the two geometries. (abridged)Comment: 15 pages, 8 figures, 30 eps files; significantly extended and more
figures added after referee comments; accepted by The Astrophysical Journa
SPLOT : a Snapshot survey for polarised light in optical transients
We present SPLOT, a small scale pilot survey to test the potential of snapshot (single epoch) linear imaging polarimetry as a supplementary tool to traditional transient follow-up. Transients exist in a vast volume of observational parameter space and polarimetry has the potential to highlight sources of scienti c interest and add value to near real-time transient survey streams. We observed a sample of 50 randomly selected optical transients with the EFOSC2 and SofI instruments, on the 3.6m New Technology Telescope (NTT) to test the feasibility of the survey. Our sample contained a number of interesting individual sources: a variety of supernovae, X-ray binaries, a tidal disruption event, blazar outbursts, and, by design, numerous transients of unknown nature. We discuss the results, both for the individual sources and the survey in detail. We provide an overview on the success and limitations of SPLOT and also describe a novel calibration method for removing instrumental polarisation e ects from Nasymth-mounted telescopes. We nd that a SPLOT-like survey would be a bene t to the large scale future transient survey streams such as LSST. The polarimetric measurements have added scienti c value to a signi cant number of the sources and, most importantly, has shown the potential to highlight unclassi ed transient sources of scienti c interest for further study
The Transitional Stripped-Envelope SN 2008ax: Spectral Evolution and Evidence for Large Asphericity
Supernova (SN) 2008ax in NGC 4490 was discovered within hours after shock
breakout, presenting the rare opportunity to study a core-collapse SN beginning
with the initial envelope-cooling phase immediately following shock breakout.
We present an extensive sequence of optical and near-infrared spectra, as well
as three epochs of optical spectropolarimetry. Our initial spectra, taken two
days after shock breakout, are dominated by hydrogen Balmer lines at high
velocity. However, by maximum light, He I lines dominated the optical and
near-infrared spectra, which closely resembled those of normal Type Ib
supernovae (SNe Ib) such as SN 1999ex. This spectroscopic transition defines
Type IIb supernovae, but the strong similarity of SN 2008ax to normal SNe Ib
beginning near maximum light, including an absorption feature near 6270A due to
H-alpha at high velocities, suggests that many objects classified as SNe Ib in
the literature may have ejected similar amounts of hydrogen as SN 2008ax,
roughly a few x 0.01 M_sun. Early-time spectropolarimetry (6 and 9 days after
shock breakout) revealed strong line polarization modulations of 3.4% across
H-alpha, indicating the presence of large asphericities in the outer ejecta.
The continuum shares a common polarization angle with the hydrogen, helium, and
oxygen lines, while the calcium and iron absorptions are oriented at different
angles. This is clear evidence of deviations from axisymmetry even in the outer
ejecta. Intrinsic continuum polarization of 0.64% only nine days after shock
breakout shows that the outer layers of the ejecta were quite aspherical. A
single epoch of late-time spectropolarimetry, as well as the shapes of the
nebular line profiles, demonstrate that asphericities extended from the
outermost layers all the way down to the center of this SN. [Abridged]Comment: 24 pages, 21 figures, 4 tables, appendix, minor revisions to match
version accepted by Ap
SN 2005cs in M51 I. The first month of evolution of a subluminous SN II plateau
Early time optical observations of supernova (SN) 2005cs in the Whirlpool
Galaxy (M51), are reported. Photometric data suggest that SN 2005cs is a
moderately under-luminous Type II plateau supernova (SN IIP). The SN was
unusually blue at early epochs (U-B ~ -0.9 about three days after explosion)
which indicates very high continuum temperatures. The spectra show relatively
narrow P-Cygni features, suggesting ejecta velocities lower than observed in
more typical SNe IIP. The earliest spectra show weak absorption features in the
blue wing of the He I 5876A absorption component and, less clearly, of H
and H. Based on spectral modelling, two different interpretations can
be proposed: these features may either be due to high-velocity H and He I
components, or (more likely) be produced by different ions (N II, Si II).
Analogies with the low-luminosity, Ni-poor, low-velocity SNe IIP are
also discussed.
While a more extended spectral coverage is necessary in order to determine
accurately the properties of the progenitor star, published estimates of the
progenitor mass seem not to be consistent with stellar evolution models.Comment: 12 pages, 11 Figures. Accepted for publication in MNRA
SN 2005cs in M51 II. Complete Evolution in the Optical and the Near-Infrared
We present the results of the one year long observational campaign of the
type II-plateau SN 2005cs, which exploded in the nearby spiral galaxy M51 (the
Whirlpool Galaxy). This extensive dataset makes SN 2005cs the best observed
low-luminosity, 56Ni-poor type II-plateau event so far and one of the best
core-collapse supernovae ever. The optical and near-infrared spectra show
narrow P-Cygni lines characteristic of this SN family, which are indicative of
a very low expansion velocity (about 1000 km/s) of the ejected material. The
optical light curves cover both the plateau phase and the late-time radioactive
tail, until about 380 days after core-collapse. Numerous unfiltered
observations obtained by amateur astronomers give us the rare opportunity to
monitor the fast rise to maximum light, lasting about 2 days. In addition to
optical observations, we also present near-infrared light curves that (together
with already published UV observations) allow us to construct for the first
time a reliable bolometric light curve for an object of this class. Finally,
comparing the observed data with those derived from a semi-analytic model, we
infer for SN 2005cs a 56Ni mass of about 0.003 solar masses, a total ejected
mass of 8-13 solar masses and an explosion energy of about 3 x 10^50 erg.Comment: 18 pages, 18 figures, accepted for publication in MNRA
Massive stars as thermonuclear reactors and their explosions following core collapse
Nuclear reactions transform atomic nuclei inside stars. This is the process
of stellar nucleosynthesis. The basic concepts of determining nuclear reaction
rates inside stars are reviewed. How stars manage to burn their fuel so slowly
most of the time are also considered. Stellar thermonuclear reactions involving
protons in hydrostatic burning are discussed first. Then I discuss triple alpha
reactions in the helium burning stage. Carbon and oxygen survive in red giant
stars because of the nuclear structure of oxygen and neon. Further nuclear
burning of carbon, neon, oxygen and silicon in quiescent conditions are
discussed next. In the subsequent core-collapse phase, neutronization due to
electron capture from the top of the Fermi sea in a degenerate core takes
place. The expected signal of neutrinos from a nearby supernova is calculated.
The supernova often explodes inside a dense circumstellar medium, which is
established due to the progenitor star losing its outermost envelope in a
stellar wind or mass transfer in a binary system. The nature of the
circumstellar medium and the ejecta of the supernova and their dynamics are
revealed by observations in the optical, IR, radio, and X-ray bands, and I
discuss some of these observations and their interpretations.Comment: To be published in " Principles and Perspectives in Cosmochemistry"
Lecture Notes on Kodai School on Synthesis of Elements in Stars; ed. by Aruna
Goswami & Eswar Reddy, Springer Verlag, 2009. Contains 21 figure
The He-rich Stripped-Envelope Core-Collapse Supernova 2008ax
Extensive optical and near-infrared (NIR) observations of the type IIb
supernova 2008ax are presented, covering the first year after the explosion.
The light curve is mostly similar in shape to that of the prototypical type IIb
SN 1993J, but shows a slightly faster decline rate at late phases and lacks the
prominent narrow early-time peak of SN 1993J. From the bolometric light curve
and ejecta expansion velocities, we estimate that about 0.07-0.15 solar masses
of 56Ni were produced during the explosion and that the total ejecta mass was
between 2 and 5 solar masses, with a kinetic energy of at least 10^51 erg. The
spectral evolution of SN 2008ax is similar to that of the type Ib SN 2007Y,
exhibiting high-velocity Ca II features at early phases and signs of
ejecta-wind interaction from H-alpha observations at late times. NIR spectra
show strong He I lines similar to the type Ib SN 1999ex, and a large number of
emission features at late times. Particularly interesting are the strong,
double-peaked He I lines in late NIR spectra, which - together with
double-peaked [O I] emission in late optical spectra - provide clues for
asymmetry and large-scale Ni mixing in the ejecta.Comment: 19 pages, 17 figures; accepted for publication in MNRA
The massive binary companion star to the progenitor of supernova 1993J
The massive star which underwent core-collapse to produce SN1993J was
identified as a non-variable red supergiant star in images of the galaxy M81
taken before explosion. However the stellar source showed an excess in UV and
B-band colours that suggested it had either a hot, massive companion star or
was embedded in an unresolved young stellar association. The spectra of SN1993J
underwent a remarkable transformation between a hydrogen-rich Type II supernova
and a helium-rich (hydrogen-deficient) Type Ib. The spectral and photometric
peculiarities were explained by models in which the 13-20 solar mass supergiant
had lost almost its entire hydrogen envelope to a close binary companion. The
binary scenario is currently the best fitting model for the production of such
type IIb supernovae, however the hypothetical massive companion stars have so
far eluded discovery. Here we report the results of new photometric and
spectroscopic observations of SN1993J, 10 years after explosion. At the
position of the fading SN we detect the unambiguous signature of a massive
star, the binary companion to the progenitor. This is evidence that this type
of SN originate in interacting binary systems.Comment: 18 pages (3 figures
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