|Canonical Name:||GRB 190114C|
|TeVCat Name:||TeV J0338-269|
|R.A.:||03 38 01.17 (hh mm ss)|
|Dec.:||-26 56 46.73 (dd mm ss)|
|Gal Long: ||222.47 (deg)|
|Gal Lat: ||-53.08 (deg)|
|Distance: ||z=0.4245 |
|Flux:|| (Crab Units)|
|Energy Threshold:||300 GeV|
|Discovered By: ||MAGIC|
|TeVCat SubCat:||Default Catalog|
Overview of the Detection:
From MAGIC Collaboration
- "Gamma-rays were observed in the energy range 0.2–1 teraelectronvolt
from about one minute after the burst (at more than 50 standard
deviations in the first 20 minutes), revealing a distinct emission
component of the afterglow with power comparable to that of the
- "The observed similarity in the radiated power and temporal
behaviour of the teraelectronvolt and X-ray bands points to processes
such as inverse Compton upscattering as the mechanism of the
- "Triggered by the Swift-BAT alert, the Major Atmospheric Gamma
Imaging Cherenkov (MAGIC) telescopes observed GRB 190114C from:
T0 + 57s until T0 + 15,912 s"
MAGIC have detected sub-TeV emission from GRB 190114C:
An extract from their ATel
- "The MAGIC telescopes performed a rapid follow-up observation of GRB 190114C
(Gropp et al.
, GCN 23688; Tyurina et al.
, GCN 23690,
de Ugarte Postigo et al.
, GCN 23692, Lipunov et al.
Selsing et al.
GCN 23695). This observation was triggered by the
Swift-BAT alert; we started observing at about 50s after Swift T0:
20:57:03.19. The MAGIC real-time analysis shows a significance >20
sigma in the first 20 min of observations (starting at T0+50s) for
energies >300GeV. The relatively high detection threshold is due to
the large zenith angle of observations (>60 degrees) and the presence
of partial Moon. Given the brightness of the event, MAGIC will
continue the observation of GRB 190114C until it is observable tonight
and also in the next days. We strongly encourage follow-up
observations by other instruments."
From MAGIC Collaboration
- A long GRB: "GRB 190114C was first identified as a long-duration GRB
by the Burst Alert Telescope (BAT) onboard the Neil Gehrels Swift
) and the Gamma-ray Burst Monitor (GBM
onboard the Fermi satellite"
- T0: 14 January 2019, 20:57:03 (UT)
- T90: "Its duration in terms of T90 (the time interval containing 90%
of the total photon counts) was measured to be about 116 s by
and about 362 s by Swift-BAT
The GRB position quoted is that from Tyurina et al.
- R.A. (J2000): 03h 38m 01.17s
- Dec. (J2000): -26d 56m 46.73s
From Castro-Tirado et al.
- "Following the detection of the ultra-bright GRB 190114C ... optical
spectroscopy of the reported optical afterglow has been undertaken at
the 10.4m GTC telescope (+OSIRIS) at the Spanish island of La Palma
starting on Jan 14, 23:32 UT (2.6 hr post-burst). The two spectra
(600s each, at high airmass) covered the range 3,700-9.600 A and the
detection of Ca H & K lines and the Na I doublet (as well as other
Fraunhofer lines) confirms the redshift value reported by Selsing et al.
which we refine to z = 0.4245 +/- 0.0005, supporting
the association with the galaxy detected in the Pan-STARRS archival
data (de Ugarte Postigo et al.
From Selsing et al.
- "We immediately followed up with spectroscopic observations using
the Alfosc instrument, in which the afterglow is very clearly
detected. From the detection of strong absorption lines from Ca H & K
along with Na ID in the afterglow spectrum, we derive a redshift of z = 0.42,
which we suggest is the redshift of the GRB."
From MAGIC Collaboration
- "The observed spectrum can be fitted in the energy range 0.2–1 TeV
with a simple power law with photon index:
... A_obs = 5.43 +/- 0.22 (statistical error only),
one of the steepest spectra ever observed for a gamma-ray source. It
is remarkable that photons are observed at Energy of approx. 1 TeV,
despite the severe EBL attenuation expected at these energies (by a
factor of about 300, according to plausible EBL models"
- The spectrum was derived by assuming a simple power-law spectrum for
the intrinsic spectrum of the form: dF/dE = F0 x (E/E0)^-A
- The EBL model of Dominguez et al.
(2011) was used to
de-absorb the measured spectrum to determine the intrinsic spectral
- A_int: 2.22 +0.23 (stat) -0.25 (stat) +0.21 (syst) -0.25 (syst)
- F0_int: 8.45 +0.68 (stat) -0.65 (stat) +4.42 (syst) -3.97 (syst) x10e-9 TeV-1 cm-2 s-1
- E0: 0.46 TeV
- the authors report that "there is no significant evidence for spectral variability"
From MAGIC Collaboration et al.
- "Here we report multi-frequency observations of GRB 190114C, and
study the evolution in time of the GRB emission across 17 orders of
magnitude in energy, from 5 x 10e−6 to 10e12 electronvolts."
- "We find that the broadband spectral energy distribution is
double-peaked, with the teraelectronvolt emission constituting a
distinct spectral component with power comparable to the synchrotron
- "This component is associated with the afterglow and is
satisfactorily explained by inverse Compton up-scattering of
synchrotron photons by high-energy electrons."
- "We find that the conditions required to account for the observed
teraelectronvolt component are typical for GRBs, supporting the
possibility that inverse Compton emission is commonly produced in
From MAGIC Collaboration
- the light curve of the GRB "is well fitted with a simple power-law
function F(t) proportional to tB with:
... B = -1.60 +/-0.07.
The flux evolves from:
... F(t) approx. 5 × 10e-8 erg cm-2 s-1 at t approx. T0 +80s
... F(t) approx. 6 × 10e-10 erg cm-2 s-1 at t greater/equal than T0 + 103 s
... after which it falls below the sensitivity level of the telescopes
and is undetectable. There is no clear evidence for breaks or cutoffs
in the light curve, nor irregular variability beyond the monotonic
decay. The light curves in the kiloelectronvolt and gigaelectronvolt
bands display behaviour similar to the teraelec- tronvolt band, with a
somewhat shallower decay slope for the gigaelectronvolt band."
- "These properties indicate that most of the observed emission is
associated with the afterglow phase, rather than the prompt phase,
which typically shows irregular variability. "
From Axelsson et al.
- "The data from the Fermi-LAT show a significant increase in the
event rate that is spatially correlated with the GBM trigger with high
significance. The highest-energy photon is a 22.9 GeV event which is
observed 15 s after the GBM trigger.
- The estimated photon index above 100 MeV is -1.98 +/- 0.06, with an
estimated photon and energy flux of 2.69e-03 +/- 1.86e-04 ph/cm2/s and
2.06e-06 +/- 1.42e-07 erg/cm2/s, respectively."
Seen by: MAGIC
Constraints on the intergalactic magnetic field from gamma-ray observations of GRB 190114C
Wang, Ze-Rui et al., arXiv e-prints parXiv:2001.01186 (2020) [LINK]
Bounds on Lorentz invariance violation from MAGIC observation of GRB 190114C
MAGIC Collaboration et al., arXiv e-prints parXiv:2001.09728 (2020) [LINK]
Can we constrain the extragalactic magnetic field from very high energy observations of GRB 190114C?
Dzhatdoev, T.A. and Podlesnyi, E.I., arXiv e-prints parXiv:2002.06918 (2020) [LINK]
First time detection of a GRB at sub-TeV energies; MAGIC detects the GRB 190114C
Mirzoyan, R. on behalf of the MAGIC Collaboration, The Astronomer's Telegram 12390 p1 (2019) [LINK]
GRB 190114C: from prompt to afterglow?
Ravasio, M.E. et al., arXiv e-prints p (2019) [LINK]
Synchrotron self-Compton emission from afterglow shocks as the origin of the sub-TeV emission in GRB 180720B and GRB 190114C
Wang, Xiang-Yu et al., arXiv e-prints parXiv:1905.11312 (2019) [LINK]
The physical conditions of the afterglow implied by MAGIC's sub-TeV observations of GRB 190114C
Derishev, Evgeny and Piran, Tsvi, arXiv e-prints parXiv:1905.08285 (2019) [LINK]
MAGICal GRB 190114C: Cutoff in the spectrum at sub-GeV energies
Chand, V. et al., arXiv e-prints parXiv:1905.11844 (2019) [LINK]
Analysis and modelling of the multi-wavelength observations of the luminous GRB 190114C
Fraija, N. et al., arXiv e-prints parXiv:1904.06976 (2019) [LINK]
Synchrotron self-Compton as a likely mechanism of photons beyond the synchrotron limit in GRB 190114C
Fraija, N. et al., arXiv e-prints parXiv:1907.06675 (2019) [LINK]
Less noticeable shallow decay phase in early X-ray afterglows of GeV/TeV-detected gamma-ray bursts
Yamazaki, Ryo et al., arXiv e-prints parXiv:1910.04097 (2019) [LINK]
Fermi and Swift Observations of GRB 190114C: Tracing the Evolution of High-Energy Emission from Prompt to Afterglow
Ajello, M. et al., arXiv e-prints parXiv:1909.10605 (2019) [LINK]
Self-Similarities and Power-laws in the Time-resolved Spectra of GRB 190114C, GRB 130427A, GRB 160509A, and GRB 160625B
Liang, L. et al., arXiv e-prints parXiv:1910.12615 (2019) [LINK]
East Asia VLBI Network observations of the TeV Gamma-Ray Burst 190114C
An, Tao et al., arXiv e-prints parXiv:1911.03646 (2019) [LINK]
Multi-messenger astronomy with very-high-energy gamma-ray observations
Hinton, Jim and Ruiz-Velasco, Edna, arXiv e-prints parXiv:1911.06097 (2019) [LINK]
Low frequency view of GRB 190114C reveals time varying shock micro-physics
Misra, K. et al., arXiv e-prints parXiv:1911.09719 (2019) [LINK]
Lowly polarized light from a highly magnetized jet of GRB 190114C
Jordana-Mitjans, N. et al., arXiv e-prints parXiv:1911.08499 (2019) [LINK]
GRB 190114C in the nuclear region of an interacting galaxy -- A detailed host analysis using ALMA, HST and VLT
de Ugarte Postigo, A. et al., arXiv e-prints parXiv:1911.07876 (2019) [LINK]
Inverse Compton Signatures of Gamma-Ray Burst Afterglows
Zhang, Hao et al., arXiv e-prints parXiv:1910.14049 (2019) [LINK]
Extreme emission seen from gamma-ray bursts
Zhang, Bing, Nature Vol. 575 News and Views, (2019) [LINK]
Teraelectronvolt emission from the gamma-ray burst GRB 190114C
MAGIC Collaboration, Nature 575, pages 455-458 (2019) [LINK]
Observation of inverse Compton emission from a long gamma-ray burst
MAGIC Collaboration et al., Nature 575, pages 459-463 (2019) [LINK]
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