1,465 research outputs found
Optical and Infrared Observations of Radioactive Elements in Supernovae
At late phases the powering of supernova light curves is often provided by
the decay of radioactive elements synthesized in the explosions. This is
unambiguously revealed when the light curve decline follows the half life time
of the decaying elements, and the bolometric luminosity then directly provides
the mass of ejected radioactive material. I will focus on the best observed
element, Nickel-56, and demonstrate that different supernovae eject different
amounts of this element. SN 1994W ejected very small amounts of nickel,
possibly caused by black hole formation. SN 1998bw may instead have ejected
more Nickel-56 than any other supernova to date.
I will also discuss our ISO non-detection of [Fe II] 26 micron in SN 1987A,
which can be used to estimate an upper limit on the mass of ejected radioactive
Titanium-44.Comment: 9 pages, 3 figures, In press in New Astronomy Review
Late-time emission of type Ia supernovae: optical and near-infrared observations of SN 2001el
We present optical and near-infrared light curves of SN 2001el from 310 to
445 days past maximum light, obtained with the Very Large Telescope. The
late-time optical (UBVRI) light curves decay in a nearly linear fashion with
decay time scales of 1.43\pm0.14, 1.43\pm0.06, 1.48\pm0.06, 1.45\pm0.07, and
1.03\pm0.07 magnitudes (per hundred days) in the U, B, V, R and I bands,
respectively. In contrast, in the near-infrared (JHKs) bands the time evolution
of the flux appears to be nearly constant at these epochs. We measure decline
rates (per hundred days) of 0.19\pm0.10 and 0.17\pm0.11 magnitudes in the J and
H bands, respectively. We construct a UVOIR light curve, and find that the
late-time luminosity has a decay time scale nearly consistent with complete
depostion of positron kinetic energy. The late-time light curves of the normal
type Ia SN 2001el demonstrate the increased importance of the near-infrared
contribution. This was previously observed in the peculiar SN 2000cx, and the
results for SN 2001el thus ensure that the conclusions previously based on a
single peculiar event are applicable to normal type Ia supernovae. The measured
late-time UVOIR decline rate suggests that a majority of the positrons are
trapped within the ejecta. This results does not favor the predictions of a
weak and/or radially combed magnetic field configuration.Comment: 4 pages with 2 figures plus 7 tables. Accepted for publication in A&A
letter. Constructive comments welcome
SN 1998bw at late phases
We present observations of the peculiar supernova SN 1998bw, which was
probably associated with GRB 980425. The photometric and spectroscopic
evolution is monitored up to 500 days past explosion. We also present modeling
based on spherically symmetric, massive progenitor models and very energetic
explosions. The models allow line identification and clearly show the
importance of mixing. From the late light curves we estimate that about 0.3-0.9
solar masses of ejected Nickel-56 is required to power the supernova.Comment: With 3 figures Accepted for ApJ Letter
GRBs as Probes of Massive Stars Near and Far
Long-duration gamma-ray bursts are the manifestations of massive stellar
death. Due to the immense energy release they are detectable from most of the
observable universe. In this way they allow us to study the deaths of single
(or binary) massive stars possibly throughout the full timespan massive stars
have existed in the Universe. GRBs provide a means to infer information about
the environments and typical galaxies in which massive stars are formed. Two
main obstacles remain to be crossed before the full potential of GRBs as probes
of massive stars can be harvested: i) we need to build more complete and well
understood samples in order not to be fooled by biases, and ii) we need to
understand to which extent GRBs may be intrinsically biased in the sense that
they are only formed by a limited subset of massive stars defined by most
likely a restricted metallicity interval. We describe the status of an ongoing
effort to build a more complete sample of long-duration GRBs with measured
redshifts. Already now we can conclude that the environments of GRB progenitors
are very diverse with metallicities ranging from solar to a hundredth solar and
extinction ranging from none to A_V>5 mag. We have also identified a sightline
with significant escape of Lyman continuum photons and another with a clear
2175AA extinction bump.Comment: Invited review - in "Massive Stars as Cosmic Engines", IAU Symp. 250
(Kauai), ed. F. Bresolin, P. A. Crowther, and J. Puls (Cambridge University
Press), p. 443-456. Typos and refs correcte
The Vela Pulsar in the Near-Infrared
We report on the first detection of the Vela pulsar in the near-infrared with
the VLT/ISAAC in the Js and H bands. The pulsar magnitudes are Js=22.71 +/-
0.10 and H=22.04 +/- 0.16. We compare our results with the available
multiwavelength data and show that the dereddened phase-averaged optical
spectrum of the pulsar can be fitted with a power law F_nu propto
nu^(-alpha_nu) with alpha_nu = 0.12 +/- 0.05, assuming the color excess
E(B-V)=0.055 +/-0.005 based on recent spectral fits of the emission of the Vela
pulsar and its supernova remnant in X-rays. The negative slope of the pulsar
spectrum is different from the positive slope observed over a wide optical
range in the young Crab pulsar spectrum. The near-infrared part of the Vela
spectrum appears to have the same slope as the phase-averaged spectrum in the
high energy X-ray tail, obtained in the 2-10 keV range with the RXTE. Both of
these spectra can be fitted with a single power law suggesting their common
origin. Because the phase-averaged RXTE spectrum in this range is dominated by
the second X-ray peak of the pulsar light curve, coinciding with the second
main peak of its optical pulse profile, we suggest that this optical peak can
be redder than the first one. We also detect two faint extended structures in
the 1.5''-3.1'' vicinity of the pulsar, projected on and aligned with the
south-east jet and the inner arc of the pulsar wind nebula, detected in X-rays
with Chandra. We discuss their possible association with the nebula.Comment: 12 pages, 8 figures, accepted for publication in A&A, the associated
near-infrared images in the fits format are available at
http://www.ioffe.ru/astro/NSG/obs/vela-ir
High Resolution Spectroscopy of Balmer-Dominated Shocks in the RCW 86, Kepler and SN 1006 Supernova Remnants
We report results from high resolution optical spectroscopy of three
non-radiative galactic supernova remnants, RCW 86, Kepler's supernova remnant
and SN 1006. We have measured the narrow component H-alpha line widths in
Balmer-dominated filaments in RCW 86 and SN 1006, as well as the narrow
component width in a Balmer-dominated knot in Kepler's SNR. The narrow
component line widths measured in RCW 86 and Kepler's SNR show FWHM of 30-40
km/s, similar to what has been seen in other Balmer-dominated remnants. Of the
remnants in our sample, SN 1006 is the fastest shock (~3000 km/s). The narrow
component H-alpha and H-beta lines in this remnant have a FWHM of merely 21
km/s. Comparing the narrow component widths measured in our sample with those
measured in other remnants shows that the width of the narrow component does
not correlate in a simple way with the shock velocity. The implications for the
pre-heating mechanism responsible for the observed line widths are discussed.Comment: Accepted by A&
NOT Stockholm Supernovae
This proceeding contribution is a short summary of the invited talk about
observational supernova science at Stockholm University that has been conducted
at the Nordic Optical Telescope over the past 25 years, and some expectations
for the future.Comment: Conference proceeding for NOT - a telescope for the futur
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