105 research outputs found
Gamma-ray Bursts: Light on the distant Universe
Observations of a long-lasting Gamma-ray burst, one that has the brightest
optical counterpart yet discovered, challenge theoretical understanding of
these bursts but may enhance their usefulness as cosmic probes.Comment: News and Views article for Nature (Sept. 11, 2008
New direction for gamma-rays
The origin of energetic gamma-ray bursts is still unknown. But the detection
of polarization of gamma-rays provides fresh insight into the mechanism driving
these powerful explosions.Comment: Nature "News & Views", RE Coburn & Boggs (astro-ph/0305377
A large age for the pulsar B1757-24 from an upper limit on its proper motion
The "characteristic age" of a pulsar usually is considered to approximate its true age, but this assumption has led to some puzzling results, including the fact that many pulsars with small characteristic ages have no associated supernova remnants. The pulsar B1757-24 is located just beyond the edge of a supernova remnant; the properties of the system indicate that the pulsar was born at the centre of the remnant, but that it has subsequently overtaken the expanding blast-wave. With a characteristic age of 16,000 yr, this implies an expected proper motion by the pulsar of 63-80 milliarcsec per year. Here we report observations of the nebula surrounding the pulsar which limit its proper motion to less than 25 mas/yr, implying a minimum age of 39,000 yr. A more detailed analysis argues for a true age as great as 170,000 yr, significantly larger than the characteristic age. From this result and other discrepancies associated with pulsars, we conclude that characteristic ages seriously underestimate the true ages of pulsars
The sub-energetic GRB 031203 as a cosmic analogue to GRB 980425
Over the six years since the discovery of the gamma-ray burst GRB 980425,
associated with the nearby (distance, ~40 Mpc) supernova 1998bw, astronomers
have fiercely debated the nature of this event. Relative to bursts located at
cosmological distances, (redshift, z~1), GRB 980425 was under-luminous in
gamma-rays by three orders of magnitude. Radio calorimetry showed the explosion
was sub-energetic by a factor of 10. Here, we report observations of the radio
and X-ray afterglow of the recent z=0.105 GRB 031203 and demonstrate that it
too is sub-energetic. Our result, when taken together with the low gamma-ray
luminosity, suggest that GRB 031203 is the first cosmic analogue to GRB 980425.
We find no evidence that this event was a highly collimated explosion viewed
off-axis. Like GRB 980425, GRB 031203 appears to be an intrinsically
sub-energetic gamma-ray burst. Such sub-energetic events have faint afterglows.
Intensive follow-up of faint bursts with smooth gamma-ray light curves (common
to both GRBs 031203 and 980425) may enable us to reveal their expected large
population.Comment: To Appear in Nature, August 5, 200
Radio Follow-Up of Gravitational-Wave Triggers During Advanced Ligo O1
The American Astronomical Society. All rights reserved.We present radio follow-up observations carried out with the Karl G. Jansky Very Large Array during the first observing run (O1) of the Advanced Laser Interferometer Gravitational-wave Observatory (LIGO). A total of three gravitational-wave triggers were followed-up during the 4 months of O1, from 2015 September to 2016 January. Two of these triggers, GW150914 and GW151226, are binary black hole (BH) merger events of high significance. A third trigger, G194575, was subsequently declared as an event of no interest (i.e., a false alarm). Our observations targeted selected optical transients identified by the intermediate Palomar Transient Factory in the Advanced LIGO error regions of the three triggers, and a limited region of the gravitational-wave localization area of G194575 not accessible to optical telescopes due to Sun constraints, where a possible high-energy transient was identified. No plausible radio counterparts to GW150914 and GW151226 were found, in agreement with expectations for binary BH mergers. We show that combining optical and radio observations is key to identifying contaminating radio sources that may be found in the follow-up of gravitational-wave triggers, such as emission associated with star formation and active galactic nuclei. We discuss our results in the context of the theoretical predictions for radio counterparts to gravitational-wave transients, and describe our future plans for the radio follow-up of Advanced LIGO (and Virgo) triggers. © 2016
The bright optical afterglow of the nearby gamma-ray burst of 29 March 2003
Many past studies of cosmological gamma-ray bursts (GRBs) have been limited
because of the large distance to typical GRBs, resulting in faint afterglows.
There has long been a recognition that a nearby GRB would shed light on the
origin of these mysterious cosmic explosions, as well as the physics of their
fireballs. However, GRBs nearer than z=0.2 are extremely rare, with an
estimated rate of localisation of one every decade. Here, we report the
discovery of bright optical afterglow emission from GRB 030329. Our prompt
dissemination and the brilliance of the afterglow resulted in extensive
followup (more than 65 telescopes) from radio through X-ray bands, as well as
measurement of the redshift, z=0.169. The gamma-ray and afterglow properties of
GRB 030329 are similar to those of cosmological GRBs (after accounting for the
small distance), making this the nearest known cosmological GRB. Observations
have already securely identified the progenitor as a massive star that exploded
as a supernova, and we anticipate futher revelations of the GRB phenomenon from
studies of this source.Comment: 13 pages, 4 figures. Original tex
A Common Origin for Cosmic Explosions Inferred from Fireball Calorimetry
Past studies suggest that long-duration gamma-ray bursts (GRBs) have a
standard energy of E_gamma ~ 10^51 erg in ultra-relativistic ejecta when
corrected for asymmetry ("jets"). However, recently a group of sub-energetic
bursts, including the peculiar GRB 980425 associated with SN 1998bw (E_gamma ~
10^48 erg), has been identified. Here we report radio observations of GRB
030329, the nearest burst to date, which allow us to undertake calorimetry of
the explosion. Our observations require a two-component explosion: a narrow (5
degrees) ultra-relativistic component responsible for the gamma-rays and early
afterglow, and a wide, mildly relativistic component responsible for the radio
and optical afterglow beyond 1.5 days. While the gamma-rays are energetically
minor, the total energy release, dominated by the wide component, is similar to
that of other GRBs. Given the firm link of GRB 030329 with SN 2003dh our result
suggests a common origin for cosmic explosions in which, for reasons not
understood, the energy in the highest velocity ejecta is highly variableComment: Accepted to Natur
The X-ray emission lines in GRB afterglows: the evidence for the two-component jet model
Recently, X-ray emission lines have been observed in X-ray afterglows of
several -ray bursts. It is a major breakthrough for understanding the
nature of the progenitors. It is proposed that the X-ray emission lines can be
well explained by the Geometry-Dominated models, but in these models the
illuminating angle is much larger than that of the collimated jet of the
-ray bursts(GRBs). For GRB 011211, we obtain the illuminating angle is
about , while the angle of GRB jet is only ,
so we propose that the outflow of the GRBs with emission lines should have two
distinct components. The wide component illuminates the reprocessing material,
and produces the emission lines, while the narrow one produces the -ray
bursts. The observations show that the energy for producing the emission lines
is higher than that of the GRBs. In this case, when the wide component
dominates the afterglows, a bump will appear in the GRBs afterglows. For GRB
011211, the emergence time of the bump is less than 0.05 days after the GRB, it
is obviously too early for the observation to catch it. With the presence of
the X-ray emission lines there should also be a bright emission component
between the UV and the soft X-rays. These features can be tested by the
satellite in the near future.Comment: 10 pags, 1 figure, ChJAA in pres
Discovery of a Radio Source following the 27 December 2004 Giant Flare from SGR 1806-20
Over a decade ago it was established that the remarkable high energy
transients, known as soft gamma-ray repeaters (SGRs), are a Galactic population
and originate from neutron stars with intense (<~ 10^15 G) magnetic fields
("magnetars"). On 27 December 2004 a giant flare (fluence >~ 0.3 erg/cm^2) was
detected from SGR 1806-20. Here we report the discovery of a fading radio
counterpart. We began a monitoring program from 0.2GHz to 250GHz and obtained a
high resolution 21-cm radio spectrum which traces the intervening interstellar
neutral Hydrogen clouds. Analysis of the spectrum yields the first direct
distance measurement of SGR 1806-20. The source is located at a distance
greater than 6.4 kpc and we argue that it is nearer than 9.8 kpc. If true, our
distance estimate lowers the total energy of the explosion and relaxes the
demands on theoretical models. The energetics and the rapid decay of the radio
source are not compatible with the afterglow model that is usually invoked for
gamma-ray bursts. Instead we suggest that the rapidly decaying radio emission
arises from the debris ejected during the explosion.Comment: 16 pages, 2 figures, submitted to Nature (substantial revisions
Radio Remnants of Compact Binary Mergers - the Electromagnetic Signal that will follow the Gravitational Waves
The question "what is the observable electromagnetic (EM) signature of a
compact binary merger?" is an intriguing one with crucial consequences to the
quest for gravitational waves (GW). Compact binary mergers are prime sources of
GW, targeted by current and next generation detectors. Numerical simulations
have demonstrated that these mergers eject energetic sub-relativistic (or even
relativistic) outflows. This is certainly the case if the mergers produce short
GRBs, but even if not, significant outflows are expected. The interaction of
such outflows with the surround matter inevitably leads to a long lasting radio
signal. We calculate the expected signal from these outflows (our calculations
are also applicable to short GRB orphan afterglows) and we discuss their
detectability. We show that the optimal search for such signal should,
conveniently, take place around 1.4 GHz. Realistic estimates of the outflow
parameters yield signals of a few hundred Jy, lasting a few weeks, from
sources at the detection horizon of advanced GW detectors. Followup radio
observations, triggered by GW detection, could reveal the radio remnant even
under unfavorable conditions. Upcoming all sky surveys can detect a few dozen,
and possibly even thousands, merger remnants at any give time, thereby
providing robust merger rate estimates even before the advanced GW detectors
become operational. In fact, the radio transient RT 19870422 fits well the
overall properties predicted by our model and we suggest that its most probable
origin is a compact binary merger radio remnant
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