552 research outputs found
The Disappearance of the Progenitors of Supernovae 1993J and 2003gd
Using images from the Hubble Space Telescope (HST) and the Gemini Telescope
we confirm the disappearance of the progenitors of two Type II supernovae
(SNe), and evaluate the presence of other stars associated with them. We find
that the progenitor of SN 2003gd, an M-supergiant star, is no longer observed
at the SN location, and determine its intrinsic brightness using image
subtraction techniques. The progenitor of SN 1993J, a K-supergiant star, is
also no longer present, but its B-supergiant binary companion is still
observed. The disappearance of the progenitors confirms that these two SNe were
produced by Red Supergiants.Comment: Science, in press, published online 19/03/09, 28 pages (MS+SOM)
(high-res figures available at
http://www.dark-cosmology.dk/~justyn/research/
The Progenitor of SN 2005cs in the Whirlpool Galaxy
The progenitor of SN 2005cs, in the galaxy M51, is identified in
pre-explosion HST ACS WFC imaging. Differential astrometry, with post-explosion
ACS HRC F555W images, permitted the identification of the progenitor with an
accuracy of 0.006". The progenitor was detected in the F814W pre-explosion
image with I=23.3+/-0.2, but was below the detection thresholds of the F435W
and F555W images, with B<24.8 and V<25 at 5-sigma. Limits were also placed on
the U and R band fluxes of the progenitor from pre-explosion HST WFPC2 F336W
and F675W images. Deep images in the infra-red from NIRI on the Gemini-North
telescope were taken 2 months prior to explosion, but the progenitor is not
clearly detected on these. The upper limits for the JHK magnitudes of the
progenitor were J<21.9,H<21.1 and K<20.7. Despite having a detection in only
one band, a restrictive spectral energy distribution of the progenitor star can
be constructed and a robust case is made that the progenitor was a red
supergiant with spectral type between mid-K to late-M. The spectral energy
distribution allows a region in the theoretical HR diagram to be determined
which must contain the progenitor star. The initial mass of the star is
constrained to be M(ZAMS)=9+3/-2 M_solar, which is very similar to the
identified progenitor of the type II-P SN 2003gd, and also consistent with
upper mass limits placed on five other similar SNe. The upper limit in the deep
K-band image is significant in that it allows us to rule out the possibility
that the progenitor was a significantly higher mass object enshrouded in a dust
cocoon before core-collapse. This is further evidence that the trend for type
II-P SNe to arise in low to moderate mass red supergiants is real.Comment: Accepted (31/08/05) for publication in MNRAS Letter
Supernova Asymmetries
All core collapse supernovae are strongly aspherical. The "Bochum event,"
with velocity components displaced symmetrically about the principal H
line, strongly suggests that SN 1987A was a bi-polar rather than a uni-polar
explosion. While there is a general tendency to display a single prominant axis
in images and spectropolarimetry, there is also growing evidence for frequent
departures from axisymmetry. There are various mechanisms that might contribute
to large scale departures from spherical symmetry: jet-induced processes, the
spherical shock accretion instability (SASI) and associated phenomena, and
non-axisymmetric instabilities (NAXI). The MRI gives inevitable production of
large toroidal magnetic fields. In sum: no without B. The role of
magnetic fields, non-axisymmetric instabilities, and of the de-leptonization
phase are discussed.Comment: 8 pages, 3 figures, to be published in the proceedings of the
conference "Supernova 1987A: 20 Years After" Aspen, 200
Exploring the Polarization of Axially Symmetric Supernovae with Unsupervised Deep Learning
The measurement of non-zero polarization can be used to infer the presence of
departures from spherical symmetry in supernovae (SNe). The origin of the
majority of the intrinsic polarization observed in SNe is in electron
scattering, which induces a wavelength-independent continuum polarization that
is generally observed to be low (<1%) for all SN types. The key indicator of
asymmetry in SNe is the polarization observed across spectral lines, in
particular the characteristic ``inverse P Cygni'' profile. The results of a
suite of 900 Monte Carlo radiative transfer simulations are presented here.
These simulations cover a range of possible axisymmetric structures (including
unipolar, bipolar and equatorial enhancements) for the line forming region of
the Ca II infrared triplet. Using a Variational Autoencoder, 7 key latent
parameters are learned that describe the relationship between Stokes I and
Stokes q, under the assumption of an axially symmetric line forming region and
resonant scattering. Likelihood-free inference techniques are used to invert
the Stokes I and q line profiles, in the latent space, to derive the underlying
geometries. For axially symmetric structures, that yield an observable
``dominant axis'' on the Stokes plane, we propose the existence of a
geometry ``conjugate" (which is indistinguishable under a rotation of ). Using this machine learning infrastructure, we attempt to identify
possible geometries associated with spectropolarimetric observations of the
Type Ib SN 2017gax.Comment: 16 pages, 14 figures, MNRAS accepte
The death of massive stars - II. Observational constraints on the progenitors of type Ibc supernovae
The progenitors of many type II core-collapse supernovae have now been
identified directly on pre-discovery imaging. Here we present an extensive
search for the progenitors of type Ibc supernovae in all available
pre-discovery imaging since 1998. There are 12 type Ibc supernovae with no
detections of progenitors in either deep ground-based or Hubble Space Telescope
archival imaging. The deepest absolute BVR magnitude limits are between -4 and
-5. We compare these limits with the observed Wolf-Rayet population in the
Large Magellanic Cloud and estimate a 16 per cent probability we have failed to
detect such a progenitor by chance. Alternatively the progenitors evolve
significantly before core-collapse or we have underestimated the extinction
towards the progenitors. Reviewing the relative rates and ejecta mass estimates
from lightcurve modelling of Ibc SNe, we find both incompatible with Wolf-Rayet
stars with initial masses >25Msun being the only progenitors. We present binary
evolution models that fit these observational constraints. Stars in binaries
with initial masses <20Msun lose their hydrogen envelopes in binary
interactions to become low mass helium stars. They retain a low mass hydrogen
envelope until approximately 10,000 years before core-collapse; hence it is not
surprising that galactic analogues have been difficult to identify.Comment: Accepted by MNRAS. 31 pages, 12 figures, 8 table
The birth place of the type Ic Supernova 2007gr
We report our attempts to locate the progenitor of the peculiar type Ic SN
2007gr in HST pre-explosion images of the host galaxy, NGC 1058. Aligning
adaptive optics Altair/NIRI imaging of SN 2007gr from the Gemini (North)
Telescope with the pre-explosion HST WFPC2 images, we identify the SN position
on the HST frames with an accuracy of 20 mas. Although nothing is detected at
the SN position we show that it lies on the edge of a bright source, 134+/-23
mas (6.9 pc) from its nominal centre. Based on its luminosity we suggest that
this object is possibly an unresolved, compact and coeval cluster and that the
SN progenitor was a cluster member, although we note that model profile fitting
favours a single bright star. We find two solutions for the age of this assumed
cluster; 7-/+0.5 Myrs and 20-30 Myrs, with turn-off masses of 28+/-4 Msun and
12-9 Msun respectively. Pre-explosion ground-based K-band images marginally
favour the younger cluster age/higher turn-off mass. Assuming the SN progenitor
was a cluster member, the turn-off mass provides the best estimate for its
initial mass. More detailed observations, after the SN has faded, should
determine if the progenitor was indeed part of a cluster, and if so allow an
age estimate to within ~2 Myrs thereby favouring either a high mass single star
or lower mass interacting binary progenitor.Comment: 12 pages, 3 figures, resolution of fig 1. has been reduced, some
revision based on referee's comments, Accepted ApJL 27 Nov 200
On the nature of the progenitors of three type II-P supernovae: 2004et, 2006my and 2006ov
The pre-explosion observations of the type II-P supernovae 2006my, 2006ov and
2004et, are re-analysed. In the cases of supernovae 2006my and 2006ov we argue
that the published candidate progenitors are not coincident with their
respective supernova sites in pre-explosion Hubble Space Telescope
observations. We therefore derive upper luminosity and mass limits for the
unseen progenitors of both these supernovae, assuming they are red supergiants:
2006my (log L/Lsun = 4.51; mass < 13Msun) and 2006ov (log L/Lsun = 4.29; mass <
10Msun). In the case of supernova 2004et we show that the yellow-supergiant
progenitor candidate, originally identified in Canada France Hawaii Telescope
images, is still visible ~3 years post-explosion in observations from the
William Herschel Telescope. High-resolution Hubble Space Telescope and Gemini
(North) adaptive optics late-time imagery reveal that this source is not a
single yellow supergiant star, but rather is resolved into at least three
distinct sources. We report the discovery of the unresolved progenitor as an
excess of flux in pre-explosion Isaac Newton Telescope i'-band imaging.
Accounting for the late-time contribution of the supernova using published
optical spectra, we calculate the progenitor photometry as the difference
between the pre- and post-explosion, ground-based observations. We find the
progenitor was most likely a late K to late M-type supergiant of 8 +5/-1 Msun.
In all cases we conclude that future, high-resolution observations of the
supernova sites will be required to confirm these results.Comment: 43 pages (pre-print format), 12 figures, 10 tables. Significant
revision following referee's comments. Accepted for publication in MNRA
The Early Asymmetries of Supernova 2008D / XRF 080109
Spectropolarimetry of the Type Ib SN 2008D, associated with the XRF 080109,
at two separate epochs, are presented. The epochs of these observations
correspond to V-band light curve maximum and 15 days after light curve maximum
(or 21 and 36 days after the XRF). We find SN 2008D to be significantly
polarized, although the largest contribution is due to the interstellar
polarization component of Q_ISP=0+/-0.1% and U_ISP=-1.2+/-0.1%. At the two
epochs, the spectropolarimetry of SN 2008D is classified as being
D1+L(HeI)+L(Ca II). The intrinsic polarization of continuum wavelength regions
is <0.4%, at both epochs, implying an asymmetry of the photosphere of <10%.
Similar to other Type Ibc SNe, such as 2005bf, 2006aj and 2007gr, we observed
significant polarization corresponding to the spectral features of Ca II, He I,
Mg I, Fe II and, possibly, O I 7774, about a close-to-spherically-symmetric
photosphere. We introduce a new plot showing the chemically distinct line
forming regions in the ejecta and comment on the apparent ubiquity of highly
polarized high-velocity Ca II features in Type Ibc SNe. The polarization angle
of Ca II IR triplet was significantly different, at both epochs, to those of
the other species, suggesting high-velocity Ca II forms in a separate part of
the ejecta. The apparent structure in the outer layers of SN 2008D has
implications for the interpretation of the early-time X-ray emission associated
with shock break-out. (abridged)Comment: ApJ Subm., 45 pages, 13 figure
A spectropolarimetric view on the nature of the peculiar Type I SN 2005hk
We report two spectropolarimetric observations of SN 2005hk, which is a close
copy of the "very peculiar" SN 2002cx, showing low peak luminosity, slow
decline, high ionization near peak and an unusually low expansion velocity of
only about 7,000 km s^-1. Further to the data presented by Chornock et al.,
(2006), at -4 days before maximum, we present data of this object taken on 9
November 2005 (near maximum) and 23 November (+ two weeks) that show the
continuum and most of the spectral lines to be polarized at levels of about
0.2-0.3%. At both epochs the data corresponds to the Spectropolarimetric Type
D1. The general low level of line polarization suggests that the line forming
regions for most species observed in the spectrum have a similar shape to that
of the photosphere, which deviates from a spherical symmetry by <10%. In
comparison with spectropolarimetry of Type Ia and Core-collapse SNe at similar
epochs, we find that the properties of SN 2005hk are most similar to those of
Type Ia SNe. In particular, we find the low levels of continuum and line
polarization to indicate that the explosion mechanism is approximately
spherical, with homogeneous ejecta (unlike the chemically segregated ejecta of
CCSNe). We discuss the possibility that SN 2005hk was the result of the pure
deflagration of a white dwarf and note the issues concerning this
interpretation.Comment: ApJ accepted, uses emulateapj, 16 pages, 10 figures, figures 3 and 4
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