GRB 240414A
GCN Circular 37576
Subject
GRB 240414A: further radio observations with the VLA
Date
2024-09-20T14:43:52Z (a year ago)
From
Stefano Giarratana at INAF-OAB <s.giarratana@ira.inaf.it>
Via
email
S. Giarratana (INAF-OAB), M. Giroletti (INAF-IRA),
G. Ghirlanda (INAF-OAB), N. Di Lalla (Stanford Univ.),
N. Omodei (Stanford Univ.), O. S. Salafia (INAF-OAB)
At 01:21:27 UT on 2024 April 23 (T_mid = 8.98 days post-burst)
and at 05:22:12 on 2024 May 15 (T_mid = 31.15 days post-burst)
the Karl G. Jansky VLA started observing the field of GRB 240414A
(Caputo et al., GCN 36083) at a central frequency of 6 and 10 GHz.
The standard J1331+3030 (3C286) was used as bandpass and flux density
calibrator, while J1217+5835 was used as complex gain calibrator.
From a preliminary analysis, the radio source coincident with
GRB 240414A (Rhodes et al., GCN 36229; Giarratana et al., GCN 36231;
de Ugarte Postigo et al., GCN 36318) is detected at both frequencies:
================================================================
T_mid Freq Peak r.m.s. Beam PA
[days] [GHz] [uJy/b] [uJy/b] [arcsec] [deg]
================================================================
8.98 6 33 9 4.64x3.44 -86
8.98 10 48 7 3.16x2.24 -82
31.15 6 18 6 1.15x0.92 -40
31.15 10 21 6 0.67x0.56 -38
================================================================
We would like to thank the staff of the VLA for approving, executing,
and processing the observations.
The National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc.
These observations were carried out as part of project SF161095,
approved in the framework of the Fermi - NRAO joint program agreement.
GCN Circular 36318
Subject
GRB 240414A: NOEMA detection
Date
2024-04-26T15:39:53Z (a year ago)
From
Antonio de Ugarte Postigo at OCA <deugarte@oca.eu>
Via
email
A. de Ugarte Postigo (CNRS/OCA & LAM), M. Bremer (IRAM), C. C. Thoene (ASU-CAS), J. F. Agui Fernandez (CAHA), S. Antier (OCA), S. Basa (LAM), M. Michalowski (AOI-AMU), D. A. Perley (LJMU), J.-G. Ducoin (CPPM) report:
We observed the field of GRB 240414A (Caputo et al. GCN 36083; Myers et al. GCN 36120; Cheung et al. GCN 36147) with the NOEMA interferometer, located at the Plateau de Bure (France). The observation, performed on the 23rd April, was tuned with sidebands at 74 and 90 GHz.
When combining all the data, we obtain a weak, 3-sigma detection at the position of the afterglow (Schneider et al. GCN 36084; Adami et al. GCN 36085; de Ugarte Postigo GCN 36087; Dutton et al. 36097; Turpin et al. GCN 36101; Osborne et al. GCN 36102; Dichiara et al. GCN 36104; Pankov et al. GCN 36113; Siegel et al. GCN 36115; de Ugarte Postigo et al. GCN 36117; Wang et al. GCN 36131; Rossi et al. GCN 36228; Rhodes et al. GCN 36229; Giarratana et al. GCN 36231) with a flux density of ~55 uJy.
Based on observations carried out under project number W23DI with the IRAM NOEMA Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain).
GCN Circular 36231
Subject
GRB 240414A: radio detection with the VLA
Date
2024-04-22T16:59:02Z (a year ago)
From
Stefano Giarratana at University of Bologna <s.giarratana@ira.inaf.it>
Via
email
S. Giarratana (INAF-OAB), M. Giroletti (INAF-IRA),
G. Ghirlanda (INAF-OAB), N. Di Lalla (Stanford Univ.),
N. Omodei (Stanford Univ.)
At 01:42:45 UT on 2024 April 17 (T_mid = 2.99 days post-burst) the
Karl G. Jansky VLA started observing the field of GRB 240414A
(Caputo et al., GCN 36083) at a central frequency of 6 and 10 GHz.
The standard J1331+3030 (3C286) was used as bandpass and flux density
calibrator, while J1217+5835 was used as complex gain calibrator.
From a preliminary analysis, an unresolved radio source is clearly
detected at both frequencies at a position:
RA: 12:19:08.08 +- 0.01
Dec: +56:44:28.7 +- 0.2
The surface brightness peak is 40 uJy/beam and 60 uJy/beam at 6
and 10 GHz, respectively. The r.m.s. noise level of the images is
7 uJy/beam at both 6 and 10 GHz.
The synthesized beams are 4.1 x 3.0 arcsec (PA: 70deg) at 6 GHz
and 2.7 x 1.9 arcsec (PA: 76deg) at 10 GHz.
While no source is detected at the aforementioned position in previous
radio surveys (FIRST, NVSS, VLASS), their r.m.s. noise levels (1sigma)
is above 100 uJy/b, well above the derived surface brightness peak.
Therefore, we cannot exclude the contribution from the GRB host galaxy yet.
We would like to thank the staff of the VLA for approving, executing,
and processing the observations.
The National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc.
These observations were carried out as part of project SF161095,
approved in the framework of the Fermi - NRAO joint program agreement.
GCN Circular 36229
Subject
GRB 240414A: AMI-LA radio observations
Date
2024-04-22T15:06:17Z (a year ago)
From
Lauren Rhodes at Oxford <lauren.rhodes@physics.ox.ac.uk>
Via
Web form
Lauren Rhodes, Rob Fender (Oxford), Dave Green, Dave Titterington (Cambridge) report:
We observed the field of the afterglow candidate GRB 240414A (GCN #36083) with the Arcminute Microkelvin Imager Large-Array (AMI-LA) at 15.5 GHz beginning at 18:54UT on 20-Apr-2024 for a total of 4 hours. The flux standard 3c286 was used to calibrate the bandpass response and flux scale of the AMI-LA and J1219+4829 was used as an interleaved complex gain calibrator.
We do not detect any radio emission at the position of the afterglow candidate as reported in GCN #36102 at a 3 sigma upper limit of 297uJy/beam.
We thank the staff at the Mullard Radio Astronomy Observatory for carrying out these observations and operating the AMI-LA.
GCN Circular 36228
Subject
GRB 240414A: LBT optical detection
Date
2024-04-22T14:43:25Z (a year ago)
From
Andrea Rossi at INAF <andrea.rossi@inaf.it>
Via
Web form
A. Rossi, E. Maiorano, E. Palazzi (INAF-OAS), M . De Pasquale (Univ. of Messina), report on behalf of the CIBO collaboration:
We observed the field of GRB 240414A (Caputo et al. GCN 36083) simultaneously in the blue and red arms with the g'-, r'-, and z'-bands with the MODS instrument mounted on LBT (Mt Graham, AZ, USA). Observations were obtained at the midtime 05:41 UT on 2024-04-14, 3 hours and 20 minutes after the burst trigger.
We detect the optical transient (Schneider et al., GCN 36084, Aryan et al., GCN 36094, Dutton et al., GCN 36097, Xu et al., GCN 36105, Pankov et al., GCN 36113, Wang et al., GCN 36131) in all bands and we measure a preliminary AB magnitudes r'=19.1+-0.1, calibrated against SDSS field stars, and not corrected for the foreground Galactic extinction.
We acknowledge the excellent support from the LBTO and LBT-INAF staff, particularly A. Cardwell, J. Williams, F. Cusano and D. Paris, in obtaining these observations.
GCN Circular 36147
Subject
GRB 240414A: Glowbug gamma-ray detection
Date
2024-04-17T14:54:25Z (a year ago)
From
C.C. Cheung at Naval Research Lab <Teddy.Cheung@nrl.navy.mil>
Via
Web form
C.C. Cheung, R. Woolf, M. Kerr, J.E. Grove (NRL), A. Goldstein (USRA), C.A. Wilson-Hodge, D. Kocevski (MSFC), and M.S. Briggs (UAH) report:
The Glowbug gamma-ray telescope [1,2], operating on the International Space Station, reports the detection of GRB 240414A, which was also detected by Swift/BAT (GCN 36083, 36140) and Fermi/GBM (GCN 36120).
The detection occurred during a time of high background, thus complicating the analysis. Using an adaptive window with a resolution of 32-ms, the primary peak was recovered, with a burst onset determined to be 2024-04-14 02:20:36.904 with a duration of 4.1 s and a total significance of about 9.7 sigma. Lower-level emission is observed up to ~T0+30s.
The analysis results presented here are preliminary and use a response function that lacks a detailed characterization of the surrounding passive structure of the ISS.
Glowbug is a NASA-funded technology demonstrator for sensitive, low-cost gamma-ray transient telescopes developed, built, and operated by the U.S. Naval Research Laboratory (NRL) with support from the University of Alabama in Huntsville, USRA, and NASA MSFC. It was launched on 2023 March 15 aboard the Department of Defense Space Test Program’s STP-H9 to the ISS. The detector comprises 12 large-area (15 cm x 15 cm) CsI:Tl panels covering the surface of a half cube, and two hexagonal (5-cm diameter, 10-cm length) CLLB scintillators, giving it a large field of view (instantaneous FoV ~2/3 sky) over a wide energy band of 50 keV to >2 MeV.
[1] Grove, J.E. et al. 2020, Proc. Yamada Conf. LXXI, arXiv:2009.11959
[2] Woolf, R.S. et al. 2022, Proc. SPIE, 12181, id. 121811O
[3] Goldstein, A. et al. 2020, ApJ 895, 40, arXiv :1909.03006
Distribution Statement A: Approved for public release. Distribution is unlimited.
GCN Circular 36140
Subject
GRB 240414A: Swift-BAT refined analysis
Date
2024-04-16T19:56:23Z (a year ago)
From
Mike Moss at NASA GSFC <mikejmoss3@gmail.com>
Via
Web form
C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC),
R. Caputo (GSFC), H. A. Krimm (NSF),
S. Laha (GSFC/UMBC), A. Y. Lien (U Tampa),
M. J. Moss (GSFC), D. M. Palmer (LANL),
T. Parsotan (GSFC), T. Sakamoto (AGU)
(i.e. the Swift-BAT team):
Using the data set from T-61 to T+199 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 240414A (trigger #1221714)
(Caputo, et al., GCN Circ. 36083). The BAT ground-calculated position is
RA, Dec = 184.781, 56.734 deg which is
RA(J2000) = 12h 19m 07.5s
Dec(J2000) = +56d 44' 03.0"
with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 91%.
The mask-weighted light curve shows multiple pulses starting at T0-35 s through
T0+40 s, with another pulse at T0+110 s. There may be additional emission prior
to the currently available data starting from ~T0-61 s.
T90 (15-350 keV) is 88.28 +- 50.41 sec (estimated error including systematics).
The time-averaged spectrum from TTBD to TTBD sec is best fit by a power law
with an exponential cutoff. This fit gives a photon index 0.99 +- 0.36,
and Epeak of 97.0 +- 62.5 keV (chi squared 46.83 for 56 d.o.f.). For this
model the total fluence in the 15-150 keV band is 3.5 +- 0.2 x 10^-06 erg/cm2
and the 1-sec peak flux measured from T+2.04 sec in the 15-150 keV band is
1.5 +- 0.2 ph/cm2/sec. A fit to a simple power law gives a photon index
of 1.49 +- 0.08 (chi squared 53.19 for 57 d.o.f.). All the quoted errors
are at the 90% confidence level.
The results of the batgrbproduct analysis are available at
https://swift.gsfc.nasa.gov/results/batgrbcat/BAT_refined_circular/1221714
GCN Circular 36137
Subject
GRB 240414A: AbAO optical upprer limit
Date
2024-04-16T14:12:25Z (a year ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
Via
legacy email
N. Pankov (HSE, IKI), R. Ya. Inasaridze (AbAO), A. Pozanenko (IKI),
S. Belkin (IKI) report on behalf of GRB-IKI-FuN:
We observed the field of GRB 240414A (Caputo et. al., GCN 36083) at
redshift z=1.833 (Adami et al., GCN 36085; de Ugarte Postigo et al., GCN 36087) with 70-cm AS-32 telescope of Abastumani Observatory (AbAO). The observations were started on 2024-04-14 (UT) 22:06:33, i.e. ~20 hr since the Swift trigger. We took 117 frames 60 sec each in the R-filter. The optical counterpart (Schneider et al., GCN 36084; Adami et al., GCN 36085; de Ugarte Postigo et al., GCN 36087; Niwano et al., GCN 36088; Lipunov et al., GCN 36095; Dutton et al., GCN 36097; Peretto, GCN 36100; Turpin et al., GCN 36101; Karambelkar et al., GCN 36103; Odeh et al., GCN 36111; Pankov et al., GCN 36113; Siegel & Caputo, GCN 36115; de Ugarte Postigo et al., GCN 36117; Xiong et al., GCN 36130; Wang et al., GCN 36131; Lopresti et al., GCN 36133) is not detected in the stacked image of 113x60 sec. Preliminary photometry is following:
Date UT_start t-T0 Filter Exp. OT err UL(3sigma)
(mid, days) (s)
2024-04-14 22:06:33 0.86281 R 113*60 n/d n.d 21.4
The magnitudes were calibrated with nearby USNO-B1.0 stars.
The result is in agreement with observations carried out by other groups, in particular, with (de Ugarte Postigo et al., GCN 36117) at the similar epoch.
GCN Circular 36133
Subject
GRB 240414A: GAD Observatory, La Spezia, Italy ,upper limit
Date
2024-04-16T10:25:27Z (a year ago)
From
Claudio Lopresti <cl3lop@gmail.com>
Via
legacy email
Claudio Lopresti (Gruppo Astronomia Digitale - GAD Observatory, La Spezia, Italy)
Member of:
UAI/SSV - Unione Astrofili Italiani/sezione stelle variabili, GRB section.
GAD - Gruppo Astronomia Digitale.
in a large collaboration with:
M.G. Dainotti (National Astronomical Observatory of Japan), Y. Niino (Tokyo University, Institute of Astronomy), K. Kalinowski (Aarhus University, Department of Physics and Astronomy), B. De Simone (Universita' degli Studi Di Salerno), Unione Astrofili Italiani (UAI)
report:
We imaged the field of GRB 240414Adetected by SWIFT(trigger 1221714)
with the telescope LX200 12” of GAD Observatory, La Spezia, Italy
The observations started 1026 min after the GRB trigger,
with a Shmidt-Cassegrain telescope D=304 mm with reducer F/D=4.75.
at the following position (+/- 2 arcsec):
RA (J2000): 12h 19m 8.07s
Dec (J2000): +56d 44' 26.0"
scope D=300 mm F/D=4.8.
Weather conditions were medium.
The observation with a series of exposures started at 024-04-14 19:28:17 UT
and ended at 2024-04-14 22:27:10 UT
We co-added 88 exposures of 90 sec each.
Start T0+ End T0+ R lim
1026 min 1205 min 19,9
We did not found any optical counterpart in 12h 19m 8.07s +56d 44' 26.0" position and in the error box of the XRT candidate.
ref.: K.L. Page at U Leicester GCN 36083
Magnitudes were estimated with the Gaia EDR3 cat. and
are not corrected for galactic dust extinction.
Reference:
https://www.parcodellestelle.com/
The message may be cited.
GCN Circular 36131
Subject
GRB 240414A: GMG observation
Date
2024-04-16T06:54:24Z (a year ago)
From
wangbaiting@ynao.ac.cn
Via
Web form
B.-T. Wang, R.-Z. Li, J. Mao, X.-L. Zhang, J.-M. Bai (YNAO) report:
We observed the field of GRB 240414A (Caputo et al. GCN 36083) by the GMG telescope in Yunnan observatories. The observation time began from UT 14:25:26.531 April 14, 2024, about 12 hours from the trigger. The preliminary results are shown as
----------------------------------------------------
UT filter mag
----------------------------------------------------
2024-04-14T14:25:26.531 sdssr 20.6 ± 0.3
----------------------------------------------------
GCN Circular 36120
Subject
GRB 240414A: Fermi GBM Observation
Date
2024-04-15T20:36:01Z (a year ago)
From
Ava Myers at NASA GSFC <ava.myers@nasa.gov>
Via
Web form
A. Myers (NPP/GSFC) reports on behalf of the Fermi Gamma-ray Burst Monitor Team:
"At 02:20:39.26 UT on 14 April 2024, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 240414A (trigger 734754044/240414098).
which was also detected by Swift BAT (R. Caputo et al. 2024, GCN 36083).
The event was originally mislabeled as GRB 240414B
(Fermi GBM Team, GCN 36612). The Fermi GBM on-ground
location is consistent with the Swift BAT position.
The angle from the Fermi LAT boresight is 49 degrees.
The GBM light curve contains a double emission episode with a duration (T90)
of about 82 s (50-300 keV). The time-averaged spectrum
from T0-1.5 to T0+80.4 s is best fit by
a power law function with an exponential high-energy cutoff.
The power law index is -0.9 +/- 0.1 and the cutoff energy,
parameterized as Epeak, is 150 +/- 20 keV.
The event fluence (10-1000 keV) in this time interval is
(5.556 +/- 1.065)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0-0.19 s in the 10-1000 keV band is 2.7 +/- 0.2 ph/s/cm^2.
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog:
https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html
For Fermi GBM data and info, please visit the official Fermi GBM Support Page:
https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/"
GCN Circular 36117
Subject
GRB 240414A: Photometric observation from 2.2m CAHA
Date
2024-04-15T15:11:19Z (2 years ago)
From
Antonio de Ugarte Postigo at OCA <deugarte@oca.eu>
Via
email
A. de Ugarte Postigo (CNRS, OCA, LAM), J.F. Agui Fernandez (CAHA), C.C. Thoene (ASU-CAS), Y. Calatayud-Borras and S. Gongora (both CAHA) report:
We observed the field of GRB 240414A (Caputo et al. GCN 36083) to obtain photometry of the optical afterglow (Schneider et al. GCN 36084, Dutton et al. GCN 36097, Turpin et al. GCN 36101, Pankov et al. GCN 36113, Siegel et al. GCN 36115) at a redshift of 1.833 (Adami et al. GCN 36085, de Ugarte Postigo et al. GCN 36087). The observation was performed with CAFOS, mounted on the 2.2m Calar Alto Telescope, in Almeria (Spain). Our imaging started at 2024-04-14T23:28:42 UT (21.14 hr after the burst onset) and consisted of 5x200s exposures in each of the g, r, and i bands
The afterglow is well detected in all three bands, and had decayed to r(AB) = 22.11+/-0.18 mag, as compared to field stars of the SDSS. Further observations are scheduled.
GCN Circular 36115
Subject
GRB 240414A: Swift/UVOT Detection
Date
2024-04-15T13:29:21Z (2 years ago)
From
Mike Siegel at PSU/Swift MOC <mhs18@psu.edu>
Via
Web form
M. H. Siegel (PSU) and R. Caputo (GSFC) report on behalf of the
Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 240414A
9754s after the BAT trigger (Caputo et al., GCN Circ. 36083). A source consistent
with the XRT position (Obsorne et al., GCN Circ. 36102) and the previously reported
optical counterpart (Schneider et al., GCN Circ. 36084, Aryan et al., GCN Circ. 36094,
Dutton et al., GCN Circ. 36097, Xu et al., GCN Circ. 36105, Pankov et al., GCN Circ. 36113)
is detected in the initial UVOT exposures.
The preliminary UVOT position is:
RA (J2000) = 12:19:08.09 = 184.78370 (deg.)
Dec (J2000) = +56:44:28.6 = 56.74127 (deg.)
with an estimated uncertainty of 0.4 arc sec. (radius, 90% confidence).
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the initial exposures are:
Filter T_start(s) T_stop(s) Exp(s) Mag
b 9754 10628 853 19.23+/-0.07
uvm2 15403 16303 885 >20.33
u 22136 22862 707 19.29+/-0.11
v 62457 62769 302 >19.60
uvw1 16310 22129 1262 20.04+/-0.18
uvw2 26698 27465 755 >20.54
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.02 in the direction of the burst
(Schlegel et al. 1998).
GCN Circular 36113
Subject
GRB 240414A: Mondy optical observations
Date
2024-04-15T13:04:11Z (2 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
Via
legacy email
N. Pankov (HSE, IKI), A. Pozanenko (IKI), E. Klunko (ISTP), S. Belkin (IKI) report on behalf of GRB-IKI-FuN:
We observed the field of GRB 240414A (Caputo et. al., GCN 36083) at redshift z=1.833 (Adami et al., GCN 36085; de Ugarte Postigo et al., GCN 36087) with 1.5-meter AZT-33IK telescope of Sayan observatory at Mondy. The observations were started on 2024-04-14 (UT) 13:56:41, i.e. ~12 hr since the Swift trigger. We took 45 frame 120 s each in the R-filter.
The optical counterpart (Schneider et al., GCN 36084; Adami et al., GCN 36085; de Ugarte Postigo et al., GCN 36087; Niwano et al., GCN 36088; Lipunov et al., GCN 36095; Dutton et al., GCN 36097; Peretto, GCN 36100; Turpin et al., GCN 36101; Karambelkar et al., GCN 36103) is well detected in the stacked image at coordinates of (J2000) 12:19:08.09 +56:44:28.8. Preliminary photometry of the optical source is following:
Date UT_start t-T0 Filter Exp. OT err UL(3sigma)
(mid, days) (s)
2024-04-14 13:56:41 0.51395 R 44*120 20.60 0.12 22.2
The magnitudes were calibrated with respect to nearby USNO-B1.0 stars.
Assuming no spectral evolution between earlier observations(Turpin et al., GCN 36101), we estimate a power law decay index to be alpha~1.2, which is in agreement with SkyNet observations (Dutton et al., GCN 36097).
GCN Circular 36111
Subject
GRB 240414A: AKO Optical Upper Limit
Date
2024-04-15T10:28:18Z (2 years ago)
From
Mohammad Odeh at Al Khatim Observatory M44 <mshodeh@gmail.com>
Via
legacy email
Mohammad Odeh (Al-Khatim Observatory, AKO, operated by the International
Astronomical Center in Abu Dhabi, UAE), Nidhal Guessoum and Dalya Akl
(American University of Sharjah, UAE), report:
As a follow-up for the GRB 240414A (Caputo et al., GCN 36083), where the
optical afterglow was detected by (Schneider et al., GCN 36084; Adami et
al., GCN 36085; de Ugarte Postigo et. al., GCN 36087; Dutton et al., GCN
36097; Turpin et. al., GCN 36101).
We observed the field of this GRB using our 0.36m f/7.7 robotic telescope.
Our observation started on 14 April 2024 at 21:00:26 UT, 18.7 hours after
the GRB trigger. No new optical source was detected within the error box
(Osborne et al., GCN 36102) down to 19.9 magnitude in the stacked image
(total 20x180s, Ic band). The magnitude was estimated using the Atlas
catalogue as a reference, and it is not corrected for galactic extinction.
Our non-detection is consistent with the results of (Niwano et al., GCN
36088; Peretto et al., GCN 36100; Karambelkar et al., GCN 36103).
GCN Circular 36104
Subject
GRB 240414A: Swift-XRT refined Analysis
Date
2024-04-15T03:00:26Z (2 years ago)
From
Phil Evans at U of Leicester <pae9@star.le.ac.uk>
Via
email
S. Dichiara (PSU), J.A. Kennea (PSU), A. Tohuvavohu (U. Toronto), J.P.
Osborne (U. Leicester), K.L. Page (U. Leicester), M.G. Bernardini
(INAF-OAB), E. Ambrosi (INAF-IASFPA) , M. Capalbi (INAF-IASFPA) and
P.A. Evans report on behalf of the Swift-XRT team:
We have analysed 5.4 ks of XRT data for GRB 240414A, from 9.9 ks to
74.3 ks after the BAT trigger. The data are entirely in Photon
Counting (PC) mode.
The light curve can be modelled with a power-law decay with a decay
index of alpha=1.0 (+/-0.4).
A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.0 (+0.4, -0.3). The
best-fitting absorption column is 3.7 (+8.5, -2.3) x 10^20 cm^-2,
consistent with the Galactic value of 1.4 x 10^20 cm^-2 (Willingale et
al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum is 3.2 x 10^-11 (3.5 x
10^-11) erg cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 3.7 (+8.5, -2.3) x 10^20 cm^-2
Galactic foreground: 1.4 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index: 2.0 (+0.4, -0.3)
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01221714.
This circular is an official product of the Swift-XRT team.
GCN Circular 36103
Subject
GRB240414A : J-band upper limits from WINTER
Date
2024-04-14T22:55:41Z (2 years ago)
From
Viraj Karambelkar at Indian Inst of Tech,Bombay <karambelkarvraj21197@gmail.com>
Via
legacy email
Viraj Karambelkar (Caltech), Tomas Ahumada (Caltech), Geoffrey Mo (MIT),
Danielle Frostig (MIT), Robert Stein (Caltech), Nathan Lourie (MIT), Robert
Simcoe (MIT), Mansi Kasliwal (Caltech)
We observed the field of the GRB 240414A (GCN #36084, #36083, #36087, #36088,
#36093, #36095, #36097, #36100, #36101) in the near-infrared J-band with
the Palomar 1-m telescope, equipped with the 1 square degree WINTER camera
(Lourie et al. 2020).
Our observations started at UTC 2024-04-14T20:16:20 (MJD 60414.45) and
lasted a total of 50 minutes. The images were processed through the WINTER
data reduction pipeline implemented using mirar (
https://zenodo.org/records/10888437), with image subtraction performed
relative to reference images built from the UKIRT Hemisphere Survey (Dye et
al. 2017).
We do not detect the optical counterpart reported by GCN #36084, #36085,
#36097, #36101 in the J-band WINTER images, and derive a limiting mag. of J
~ 19 mag (AB).
WINTER (Wide-field INfrared Transient ExploreR) is a partnership between
MIT and Caltech, housed at Palomar Observatory, and funded by NSF MRI, NSF
AAG, the David and Lucille Packard Foundation, and the MIT Kavli Institute
for Astrophysics and Space Research
GCN Circular 36102
Subject
GRB 240414A: Enhanced Swift-XRT position
Date
2024-04-14T22:35:36Z (2 years ago)
From
Phil Evans at U of Leicester <pae9@star.le.ac.uk>
Via
email
J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester)
report on behalf of the Swift-XRT team.
Using 872 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 240414A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 184.78364, +56.74056 which is equivalent
to:
RA (J2000): 12h 19m 8.07s
Dec (J2000): +56d 44' 26.0"
with an uncertainty of 3.2 arcsec (radius, 90% confidence).
This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).
This circular was automatically generated, and is an official product of the
Swift-XRT team.
GCN Circular 36101
Subject
GRB 240414A : OHP/T193 second epoch of optical follow-up and afterglow detection
Date
2024-04-14T21:59:49Z (2 years ago)
From
Damien Turpin at CEA-Saclay <dturpin-astro@hotmail.com>
Via
Web form
D. Turpin (CEA Paris-Saclay), B. Schneider (MIT), C. Adami, Ny Avo Rakotondrainibe, Olivier Ilbert, S. Basa (LAM/Pytheas/AMU), A. de Ugarte Postigo (OCA/LAM), E. Le Floc'h (CEA Paris-Saclay), S. D. Vergani (GEPI, Obs. de Paris), report on behalf of a larger collaboration:
We performed a second epoch of observation of the GRB 240414A afterglow candidate (Caputo et al., GCN 36083, Schneider et al. GCN 36084, Dutton et al. GCN 36097) using the T193cm telescope at Observatoire de Haute-Provence (France) equipped with the MISTRAL spectro-imager. After stacking 8 r-band images (total exp = 4080sec), we clearly detect the optical afterglow with the following preliminary magnitude:
-----------------------------------------------
T-T0 (in days, midtime) | mag | filter
-----------------------------------------------
0.7397 | 21.84 ± 0.16 mag (AB) | r'
-----------------------------------------------
We also report the g-band magnitude of the afterglow for the previous night (2x120s):
-----------------------------------------------
T-T0 (in days, midtime) | mag | filter
-----------------------------------------------
0.0645 | 18.39 ± 0.03 mag (AB) | g'
-----------------------------------------------
Based on our two epochs in r-band, we obtain a temporal slope alpha ~ -1.1 which is roughly consistent with the one of Dutton et al. GCN 36097.
We acknowledge the excellent support from Observatoire de Haute-Provence and in particular Jean-Pierre Troncin for the MISTRAL observations.
GCN Circular 36100
Subject
GRB 240414A: MarSEC Observatory, Vicenza, Italy, UPPER LIMIT
Date
2024-04-14T21:27:52Z (2 years ago)
From
I. Peretto at MarSEC (Marana Space Explorer Center) <ricerca@marsec.org>
Via
Web form
Ivo Peretto (MarSEC, Marana Space Explorer Center, Marana Di Crespadoro, VI, Italy)
Member of:
UAI/SSV - Unione Astrofili Italiani/Sezione Stelle Variabili, GRB section.
AAVSO (American Association Variable Stars Observers)
In collaboration with: Stefano Lora and Giovanni Furlato (MarSEC, Marana Space Explorer Center, Marana di Crespadoro, VI, Italy)
report:
We imaged the field of GRB 240414A detected by SWIFT(trigger=1221714)
with the telescope 14” RC Officine Stellari of MarSEC (Marana Space Explorer Center).
The observations with a series of 120 sec exposures started at 2024-01-01 18:18 UT, 958 min. after the GRB trigger, with a Ritchey-Chretien telescope D=360 mm f/ 8.
at the following position:
RA(J2000) = 12h 19m 09s
Dec(J2000) = +56d 43' 37"
Weather conditions were medium with Moon illuminated 40,5%.
We co-added 30 exposures of 120 sec each.
Start T0+ End T0+ R lim.
958 min 1018 min 20.82
We did not found any optical counterpart in A.R. 12 19 09, DEC. +56 43 37 position and in the error box of the XRT candidate.
ref.: GCN Circular 36083
Magnitudes were estimated with the APASS and
are not corrected for galactic dust extinction.
Reference:
https://www.marsec.org/
The message may be cited.
GCN Circular 36097
Subject
GRB 240414A: Skynet Optical Afterglow Observations
Date
2024-04-14T18:19:53Z (2 years ago)
From
Dylan Dutton at UNC Chapel Hill <ddutton59@gmail.com>
Via
Web form
Dylan Dutton, Megan Dubay, Ruide Fu, Donovan Schlekat, Daniel Reichart, Joshua Haislip, Vladimir Kouprianov, Daniel Caton, Lee Hawkins, Dean Glace, Daryl Janzen, Kim Janzen, James Davidson, Edward Murphy, and Carlos Salgado report on behalf of the Skynet Robotic Telescope Network at the University of North Carolina at Chapel Hill.
We observed the field of GRB 240414A with three of our North American robotic telescopes. The first detection occurred at 02:36:17 UTC on Apr 14 2024, approximately 15 minutes after the trigger reported by Swift (Caputo et al., GCN 36083).
We obtained multiple exposures in the B, V, and R filters. Exposure lengths were calculated using our automated exposure length scaling model.
We detect the optical afterglow with coordinates consistent to those reported by OHP/T193 (B. Schneider et al., GCN 36084).
The coordinates are:
R.A. (J2000): 12:19:08.12
Dec. (J2000): 56:44:28.70
We report the photometry below. We estimate a temporal index of about -0.9 and spectral index of about -0.5.
ExpLen | Filter | Mag | Mag Error | MJD
------------------------------------------------
51.99 | B | 17.02 | 0.066 | 60414.108
52.82 | V | 16.92 | 0.068 | 60414.110
27.18 | R | 16.46 | 0.086 | 60414.111
76.20 | V | 17.77 | 0.122 | 60414.115
38.54 | R | 17.02 | 0.117 | 60414.117
103.4 | B | 17.86 | 0.096 | 60414.120
52.39 | R | 17.26 | 0.117 | 60414.124
138.1 | V | 17.45 | 0.084 | 60414.128
63.67 | R | 17.13 | 0.117 | 60414.130
300 | R | 18.77 | 0.116 | 60414.204
300 | R | 18.61 | 0.101 | 60414.207
300 | V | 19.04 | 0.064 | 60414.208
300 | V | 19.03 | 0.063 | 60414.208
300 | R | 18.89 | 0.126 | 60414.211
300 | V | 18.85 | 0.054 | 60414.211
300 | V | 18.85 | 0.054 | 60414.211
300 | R | 18.54 | 0.091 | 60414.214
300 | V | 18.97 | 0.059 | 60414.215
300 | V | 18.98 | 0.059 | 60414.215
300 | R | 18.92 | 0.134 | 60414.218
300 | V | 19.03 | 0.063 | 60414.218
300 | V | 19.03 | 0.063 | 60414.218
300 | R | 18.94 | 0.138 | 60414.221
300 | V | 19.03 | 0.062 | 60414.222
300 | V | 19.04 | 0.062 | 60414.222
300 | R | 18.67 | 0.106 | 60414.225
300 | V | 19.12 | 0.065 | 60414.225
300 | V | 19.05 | 0.061 | 60414.225
300 | R | 18.67 | 0.106 | 60414.228
300 | V | 19.15 | 0.070 | 60414.229
300 | V | 19.16 | 0.070 | 60414.229
300 | R | 18.96 | 0.137 | 60414.232
300 | V | 19.16 | 0.069 | 60414.233
300 | V | 19.20 | 0.072 | 60414.233
300 | R | 18.72 | 0.113 | 60414.236
300 | V | 19.30 | 0.076 | 60414.236
300 | V | 19.29 | 0.075 | 60414.236
300 | V | 19.16 | 0.071 | 60414.240
300 | V | 19.21 | 0.075 | 60414.240
300x3 | R | 19.02 | 0.138 | 60414.243
300x3 | R | 19.26 | 0.090 | 60414.295
300x3 | R | 19.22 | 0.088 | 60414.306
300x3 | R | 19.35 | 0.080 | 60414.316
300x3 | R | 19.54 | 0.092 | 60414.327
300x3 | R | 19.35 | 0.159 | 60414.337
300x5 | R | 19.59 | 0.147 | 60414.351
Our images have been calibrated using stars from the APASS catalog.
GCN Circular 36095
Subject
Swift GRB 240414A: Global MASTER-Net observations report
Date
2024-04-14T17:28:49Z (2 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
Via
legacy email
V. Lipunov, V.Kornilov, E. Gorbovskoy, K. Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, V.Senik, D. Vlasenko,
G.Antipov, D.Zimnukhov, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov, D. Cheryasov, Ya.Kechin, Yu.Tselik, A. Sosnovskij
(Lomonosov Moscow State University, SAI, Physics Department),
R. Podesta, C.Lopez, F. Podesta, C.Francile
(Observatorio Astronomico Felix Aguilar OAFA),
R. Rebolo, M. Serra
(The Instituto de Astrofisica de Canarias),
D. Buckley
(South African Astronomical Observatory),
O.A. Gress, N.M. Budnev, O.Ershova
(Irkutsk State University, API),
L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez,
A.R.Corella, L.H.Rodriguez
(INAOE, Guillermo Haro Astrophysics Observatory),
A. Tlatov, D. Dormidontov
(Kislovodsk Solar Station of the Pulkovo Observatory),
V. Yurkov, A. Gabovich
(Blagoveschensk Educational State University)
MASTER-Tavrida robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Lomonosov MSU, SAI Crimea astronomical station) was pointed to the Swift GRB 240414A ( R. Caputo et al., GCN 36083) errorbox 53869 sec after notice time and 53925 sec after trigger time at 2024-04-14 17:19:21 UT, with upper limit up to 17.3 mag. Observations started at twilight. The observations began at zenith distance = 32 deg. The sun altitude is -10.0 deg.
The galactic latitude b = 60 deg., longitude l = 131 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/observ.php?id=2422039
We obtain a following upper limits.
Tmid-T0 | Site |Filt.| Expt. | Limit| Comment
_________|_____________________|_____|_______|______|________
54015 | MASTER-Tavrida | C | 180 | 17.3 |
Filter C is a clear (unfiltred) band.
The observation and reduction will continue.
The message may be cited.
GCN Circular 36088
Subject
GRB 240414A : MITSuME Akeno optical upper limits
Date
2024-04-14T12:00:04Z (2 years ago)
From
Masafumi Niwano at Tokyo Institute of Technology <niwano@hp.phys.titech.ac.jp>
Via
Web form
M. Niwano, M. Sasada, I. Takahashi, N. Higuchi, S. Hayatsu, H. Seki, Y. Yatsu and N. Kawai (Tokyo Tech) report on behalf of the MITSuME collaboration:
We observed the field of GRB 240414A (Caputo et al., GCN 36083) with the optical three-color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50-cm telescope Akeno.
The observation started at 2024-04-14 09:46:06 UT (7.4 hrs after the Swift/BAT trigger). We stacked the images with good conditions. We did not detect any uncatalogued sources within the enhanced Swift/XRT error region (Caputo et al., GCN 36083), despite the detection report of Schneider et al., (GCN 36084). We obtained the 5-sigma limits of the stacked images as follows.
T0+[hrs] | MID-UT | T-EXP[sec] | 5-sigma limits
------------------------------------------------------------------------------------------------
7.7 | 2024-02-14 10:27:15.26 | 900 | g'>17.7, Rc>18.7, Ic>18.2
------------------------------------------------------------------------------------------------
T0+ : Elapsed time after the trigger
T-EXP: Total Exposure time
We used the PS1 catalog for flux calibration. The catalog magnitudes in PS1 g, r and i bands were converted to our g', Rc and Ic band magnitudes following Tonry et al. (2012), Table 6. The magnitudes are expressed in the AB system. The images were processed in real-time through the MITSuME GPU reduction pipeline (Niwano et al. 2021, PASJ; https://github.com/MNiwano/Eclaire).
GCN Circular 36087
Subject
GRB 240414A: Redshift confirmation from GTC/OSIRIS+
Date
2024-04-14T07:07:37Z (2 years ago)
From
Antonio de Ugarte Postigo at OCA <deugarte@oca.eu>
Via
email
A. de Ugarte Postigo (CNRS, OCA, LAM), G. Lombardi (GRANTECAN), J. F. Agui Fernandez (CAHA), C. C. Thoene (ASU-CAS), J. P. U. Fynbo (DAWN/NBI), L. Izzo (INAF-OACn & DARK/NBI), N. R. Tanvir (U. Leicester), A. Martin-Carrillo (UCD), S. Geier (GRANTECAN) report:
We have obtained spectroscopy of the afterglow of GRB 240414A (Caputo et al. GCN 36083, Schneider et al. GCN 36084) with OSIRIS+ on the 10.4m GTC on the Roque de los Muchachos Observatory (Spain). The observation consisted of 3x900s exposure with grism R1000B covering the range between 3600 and 7880 AA at a mean epoch 2.11 hrs after the burst.
We detect a strong continuum over all the spectral range with absorption features that we identify as due to OI, CII, SiIV, SiII, CIV, AlII, NiII, AlIII, ZnII, FeII and MnII, as well as SiII* and FeII*, all at a common redshift of 1.833, consistent with the redshift determined by Adami et al. (GCN 36085).
Additionally, we identify an absorption system with CIV and MgII at z=1.703 and another one with MgII at z=1.067. Finally, there is a further strong and slightly broadened feature at 4056 AA that could be due to an intervening system of CIV at z=1.618, but there are no other related features to confirm it.
GCN Circular 36085
Subject
GRB 240414A : OHP/T193 redshift determination
Date
2024-04-14T04:55:18Z (2 years ago)
Edited On
2024-04-15T13:14:08Z (2 years ago)
From
Christophe Adami at LAM <christophe.adami@lam.fr>
Edited By
Judith Racusin at NASA/GSFC <judith.racusin@nasa.gov> on behalf of Christophe Adami at LAM <christophe.adami@lam.fr>
Via
Web form
C. Adami, O. Ilbert, S. de la Torre (LAM/Pytheas/AMU), A. de Ugarte Postigo (OCA/LAM), B. Schneider (MIT), E. Le Floc’h (CEA Paris-Saclay), report on behalf of a larger collaboration:
We observed the optical counterpart of GRB 240414A (Caputo et al., GCN 36083, Schneider et al., GCN 36084)
in spectroscopy with the MISTRAL instrument in blue mode using the T193cm telescope at Observatoire de
Haute-Provence (France).
We detect the optical GRB afterglow at RA = 12:19:08.08 and DEC = +56:44:28.8 (J2000).
Our spectra cover the wavelength range 4200-8000 AA and consist of 3 exposures of 900 seconds each.
Observations started at 03:17:09 UT on April 14, 2024 (~57 min after the X-ray trigger). We detect a strong
continuum with absorption features which we identify as AlII, AlIII, FeII, MnII and MgII at a common redshift
of z=1.833 that we interpret as the redshift of GRB 240414A.
Our photometric data reduction continue with g' band observations.
We acknowledge the excellent support from Observatoire de Haute-Provence and in particular Jean-Pierre Troncin
for the MISTRAL observations.
GCN Circular 36084
Subject
GRB 240414A : OHP/T193 optical counterpart detection
Date
2024-04-14T03:35:59Z (2 years ago)
From
Christophe Adami at LAM <christophe.adami@lam.fr>
Via
Web form
B. Schneider (MIT), C. Adami, O. Ilbert, S. de la Torre (LAM/Pytheas/AMU) report on behalf of a larger collaboration:
We observed the field of the GRB 240414A (Caputo et al., GCN 36083) using the T193cm telescope at Observatoire de Haute-Provence (France) equipped with the MISTRAL spectro-imager. In a single exposure of 60s in the r-band at 02:56:37UT on 2024-04-14 (36 min after the trigger), we clearly detect a source consistent with the XRT error:
The preliminary magnitude derived for that source is
r = 17.61 +/- 0.01 mag (AB)
The photometric calibration was performed using nearby stars from the PanSTARRS catalog and the magnitude is not corrected for Galactic extinction.
Spectroscopy observations using MISTRAL are currently on going.
We acknowledge the excellent support from Observatoire de Haute-Provence and in particular Jean-Pierre Troncin for the MISTRAL observations.
GCN Circular 36083
Subject
GRB 240414A: Swift detection of a burst
Date
2024-04-14T02:36:27Z (2 years ago)
From
K.L. Page at U Leicester <klp5@leicester.ac.uk>
Via
email
R. Caputo (GSFC), C. Gronwall (PSU), J.D. Gropp (PSU),
A. Y. Lien (U Tampa), M. J. Moss (GSFC), K. L. Page (U Leicester) and
D. M. Palmer (LANL) report on behalf of the Neil Gehrels Swift
Observatory Team:
At 02:20:36 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 240414A (trigger=1221714). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 184.786, +56.727 which is
RA(J2000) = 12h 19m 09s
Dec(J2000) = +56d 43' 37"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a complex
structure with a duration of at least 60 sec, with a possible smaller
peak around T+120s (during the XRT observation). The peak count rate
was ~2600 counts/sec (15-350 keV), at ~2 sec after the trigger.
The XRT began observing the field at 02:22:19.6 UT, 103.2 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 184.7855, 56.7381 which is equivalent to:
RA(J2000) = 12h 19m 8.52s
Dec(J2000) = +56d 44' 17.2"
with an uncertainty of 4.9 arcseconds (radius, 90% containment). This
location is 39 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy.
UVOT data are not available at this time.
Burst Advocate for this burst is R. Caputo (regina.caputo AT nasa.gov).
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)