635 research outputs found
GRB 030329: 3 years of radio afterglow monitoring
Radio observations of gamma-ray burst (GRB) afterglows are essential for our
understanding of the physics of relativistic blast waves, as they enable us to
follow the evolution of GRB explosions much longer than the afterglows in any
other wave band. We have performed a three-year monitoring campaign of GRB
030329 with the Westerbork Synthesis Radio Telescopes (WSRT) and the Giant
Metrewave Radio Telescope (GMRT). Our observations, combined with observations
at other wavelengths, have allowed us to determine the GRB blast wave physical
parameters, such as the total burst energy and the ambient medium density, as
well as investigate the jet nature of the relativistic outflow. Further, by
modeling the late-time radio light curve of GRB 030329, we predict that the
Low-Frequency Array (LOFAR, 30-240 MHz) will be able to observe afterglows of
similar GRBs, and constrain the physics of the blast wave during its
non-relativistic phase.Comment: 5 pages, 2 figures, Phil. Trans. R. Soc. A, vol.365, p.1241,
proceedings of the Royal Society Scientific Discussion Meeting, London,
September 200
iPTF15eqv: Multi-wavelength Expos\'e of a Peculiar Calcium-rich Transient
The progenitor systems of the class of "Ca-rich transients" is a key open
issue in time domain astrophysics. These intriguing objects exhibit unusually
strong calcium line emissions months after explosion, fall within an
intermediate luminosity range, are often found at large projected distances
from their host galaxies, and may play a vital role in enriching galaxies and
the intergalactic medium. Here we present multi-wavelength observations of
iPTF15eqv in NGC 3430, which exhibits a unique combination of properties that
bridge those observed in Ca-rich transients and Type Ib/c supernovae. iPTF15eqv
has among the highest [Ca II]/[O I] emission line ratios observed to date, yet
is more luminous and decays more slowly than other Ca-rich transients. Optical
and near-infrared photometry and spectroscopy reveal signatures consistent with
the supernova explosion of a < 10 solar mass star that was stripped of its
H-rich envelope via binary interaction. Distinct chemical abundances and ejecta
kinematics suggest that the core collapse occurred through electron capture
processes. Deep limits on possible radio emission made with the Jansky Very
Large Array imply a clean environment ( 0.1 cm) within a radius of
cm. Chandra X-ray Observatory observations rule out alternative
scenarios involving tidal disruption of a white dwarf by a black hole, for
masses > 100 solar masses). Our results challenge the notion that
spectroscopically classified Ca-rich transients only originate from white dwarf
progenitor systems, complicate the view that they are all associated with large
ejection velocities, and indicate that their chemical abundances may vary
widely between events.Comment: 24 pages, 16 figures. Closely matches version published in The
Astrophysical Journa
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Ultrafast modulation of the chemical potential in BaFe2As2 by coherent phonons
Time- and angle-resolved extreme ultraviolet photoemission spectroscopy is used to study the electronic structure dynamics in BaFe2As2 around the high-symmetry points Γ and M. A global oscillation of the Fermi level at the frequency of the A1g(As) phonon mode is observed. It is argued that this behavior reflects a modulation of the effective chemical potential in the photoexcited surface region that arises from the high sensitivity of the band structure near the Fermi level to the A1g(As) phonon mode combined with a low electron diffusivity perpendicular to the layers. The results establish a novel way to tune the electronic properties of iron pnictides: coherent control of the effective chemical potential. The results further suggest that the equilibration time for the effective chemical potential needs to be considered in the ultrafast electronic structure dynamics of materials with weak interlayer coupling. © 2014 American Physical Society
Interaction Between The Broad-lined Type Ic Supernova 2012ap and Carriers of Diffuse Interstellar Bands
The diffuse interstellar bands (DIBs) are absorption features observed in
optical and near-infrared spectra that are thought to be associated with
carbon-rich polyatomic molecules in interstellar gas. However, because the
central wavelengths of these bands do not correspond with electronic
transitions of any known atomic or molecular species, their nature has remained
uncertain since their discovery almost a century ago. Here we report on
unusually strong DIBs in optical spectra of the broad-lined Type Ic supernova
SN 2012ap that exhibit changes in equivalent width over short (~30 days)
timescales. The 4428 and 6283 Angstrom DIB features get weaker with time,
whereas the 5780 Angstrom feature shows a marginal increase. These nonuniform
changes suggest that the supernova is interacting with a nearby source of the
DIBs and that the DIB carriers possess high ionization potentials, such as
small cations or charged fullerenes. We conclude that moderate-resolution
spectra of supernovae with DIB absorptions obtained within weeks of outburst
could reveal unique information about the mass-loss environment of their
progenitor systems and provide new constraints on the properties of DIB
carriers.Comment: 6 pages, 3 figures, accepted for publication in ApJ
Detailed study of the GRB 030329 radio afterglow deep into the non-relativistic phase
We explore the physics behind one of the brightest radio afterglows ever, GRB
030329, at late times when the jet is non-relativistic. We determine the
physical parameters of the blast wave and its surroundings, in particular the
index of the electron energy distribution, the energy of the blast wave, and
the density (structure) of the circumburst medium. We then compare our results
with those from image size measurements. We observed the GRB 030329 radio
afterglow with the Westerbork Synthesis Radio Telescope and the Giant Metrewave
Radio Telescope at frequencies from 325 MHz to 8.4 GHz, spanning a time range
of 268-1128 days after the burst. We modeled all the available radio data and
derived the physical parameters. The index of the electron energy distribution
is p=2.1, the circumburst medium is homogeneous, and the transition to the
non-relativistic phase happens at t_NR ~ 80 days. The energy of the blast wave
and density of the surrounding medium are comparable to previous findings. Our
findings indicate that the blast wave is roughly spherical at t_NR, and they
agree with the implications from the VLBI studies of image size evolution. It
is not clear from the presented dataset whether we have seen emission from the
counter jet or not. We predict that the Low Frequency Array will be able to
observe the afterglow of GRB 030329 and many other radio afterglows,
constraining the physics of the blast wave during its non-relativistic phase
even further.Comment: 9 pages, 2 figures; accepted for publication in Astronomy &
Astrophysics after minor revisions; small changes in GMRT fluxes at 1280 MH
The dark nature of GRB 051022 and its host galaxy
We present multiwavelength (X-ray/optical/near-infrared/millimetre)
observations of GRB 051022 between 2.5 hours and ~1.15 yr after the event. It
is the most intense gamma-ray burst (~ 10^-4 erg cm^-2) detected by HETE-2,
with the exception of the nearby GRB 030329. Optical and near infrared
observations did not detect the afterglow despite a strong afterglow at X-ray
wavelengths. Millimetre observations at Plateau de Bure (PdB) detected a source
and a flare, confirming the association of this event with a moderately bright
(R = 21.5) galaxy. Spectroscopic observations of this galaxy show strong [O
II], Hbeta and [O III] emission lines at a redshift of 0.809. The spectral
energy distribution of the galaxy implies Av (rest frame) = 1.0 and a starburst
occuring ~ 25 Myr ago, during which the star-forming-rate reached >= 25
Msun/yr. In conjunction with the spatial extent (~ 1'') it suggests a very
luminous (Mv = - 21.8) blue compact galaxy, for which we also find with Z Zsun.
The X-ray spectrum shows evidence of considerable absorption by neutral gas
with NH, X-ray = 3.47(+0.48/-0.47) x 10^22 cm^-2 (rest frame). Absorption by
dust in the host galaxy at z = 0.809 certainly cannot account for the
non-detection of the optical afterglow, unless the dust-to-gas ratio is quite
different than that seen in our Galaxy (i.e. large dust grains). It is likely
that the afterglow of the dark GRB 051022 was extinguished along the line of
sight by an obscured, dense star forming region in a molecular cloud within the
parent host galaxy. This galaxy is different from most GRB hosts being brighter
than L* by a factor of 3. We have also derived a SFR ~ 50 Msun/yr and predict
that this host galaxy will be detected at sub-mm wavelengths.Comment: 7 Pages, 7 figures. Accepted in Astronomy and Astrophysic
Interaction Between the Broad-Lined Type Ic Supernova 2012ap and Carriers of Diffuse Interstellar Bands
The diffuse interstellar bands (DIBs) are absorption features observed in optical and near-infrared spectra that are thought to be associated with carbon-rich polyatomic molecules in interstellar gas. However, because the central wavelengths of these bands do not correspond with electronic transitions of any known atomic or molecular species, their nature has remained uncertain since their discovery almost a century ago. Here we report on unusually strong DIBs in optical spectra of the broad- lined Type Ic supernova SN2012ap that exhibit changes in equivalent width over short (. 30 days) timescales. The 4428 A and 6283 A DIB features get weaker with time, whereas the 5780 A feature shows a marginal increase. These nonuniform changes suggest that the supernova is interacting with a nearby source of the DIBs and that the DIB carriers possess high ionization potentials, such as small cations or charged fullerenes. We conclude that moderate-resolution spectra of supernovae with DIB absorptions obtained within weeks of outburst could reveal unique information about the mass-loss environment of their progenitor systems and provide new constraints on the properties of DIB carriers
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