GRB 211023A
GCN Circular 31596
Subject
GRB 211023A: evidence of supernova in LBT spectra
Date
2022-02-16T08:49:19Z (4 years ago)
From
Andrea Rossi at INAF <andrea.rossi@inaf.it>
A. Rossi, E. Pian, E. Palazzi (INAF-OAS), A. Melandri (INAF-OAB), on
behalf of the CIBO collaboration, B. Rothberg (LBTO/GMU), A. Pozanenko,
S. Belkin (IKI), and D. A. Kann (HETH/IAA-CSIC) report :
We report the results of the photometric and spectroscopic follow-up
observations of GRB 211023A (Fermi GBM team, GCN 30958; Di Lalla et al.,
GCN 30961; Lesage et al, GCN 30965; Ursi et al, GCN 30969; Poolakkil,
GCN 30998; Ridnaia et al., GCN 31022) at z = 0.390 (Pozanenko et al.,
GCN 31053) obtained with the Multi-Object Double Spectrographs (MODS)
instrument mounted on the 2x8.4-m LBT telescope (Mt. Graham, AZ, USA).
Data were obtained at ~12 UT on 2021-11-05, ~13 days (i.e. 9 rest-frame
days) after the burst trigger.
Spectroscopy of the source was obtained for a total of 4x900 s, covering
the wavelength range 3200-10000 AA. The spectrum has been corrected for
Galactic extinction (A_V = 0.45 mag). The contribution of the host
galaxy was removed via a galaxy template matching the emission line
fluxes. The low S/N spectrum shows features similar to those exhibited
by XRF-associated SN2006aj at a similar phase (Mazzali et al. 2006,
Nature, 442, 1018). This confirms the bump observed by Belkin et al.
(GCN 31098), as due to the emerging contribution of the SN.
We acknowledge the excellent support from the LBTO in particular O. Kuhn
and S. Allanson, and from the LBT-INAF staff, particularly F. Cusano, S.
Paiano, and E. Marini in obtaining these observations.
GCN Circular 31134
Subject
GRB 211023A: Xinglong 2.16m optical observations
Date
2021-11-29T05:33:13Z (4 years ago)
From
Liping Xin at NAOC, SVOM <xlp@nao.cas.cn>
L. P. Xin (NAOC), J. Wang(GXU), C. Gao(GXU), Y. L. Qiu(NAOC),
J. Y. Wei(NAOC), B. Ren(GXU), L. H. Li (NAOC), C. Wu(NAOC),
E. W. Liang(GXU), X. H. Han (NAOC) and J. S. Deng(NAOC) report:
We observed the field of the GRB 211023A (Fermi GBM team, GCN 30958; Di
Lalla et al., GCN 30961; Lesage et al, GCN 30965; Ursi et al, GCN 30969;
Poolakkil, GCN 30998; Ridnaia et al., GCN 31022 )
with 2.16m optical telescope at Xinglong observatory, China.
Ten images in R band were obtained from 2021-11-12T16:46:10 UT to
2021-11-12T17:32:18 UT, about 20.16 days after the burst.
The exposure time for each image was 300 sec.
The optical counterpart (Lipunov et al., GCN 30970; Zhirkov et al, GCN 30977;
Kann et al, GCN 30982; Hu et al, GCN 30990; Belkin et al, GCN 31004; Vinko et al, GCN
31008; Belkin et al, GCN 31018; Belkin et al, GCN 31020; Kumar et al,
GCN 31023; Gupta et al., GCN 31041; Strobl et al., GCN 31042; Pozanenko
et al., GCN 31053; Moskvitin et al., GCN 31066, , Belkin et al., GCN 31098)
was clearly detected in our the stacked image with a brightness of 22.0 magnitude
in R-band. The photometry was calibrated with several nearby USNO B1.0 catalogs.
GCN Circular 31133
Subject
GRB 211023A: Xinglong 2.16m optical observations
Date
2021-11-29T05:06:21Z (4 years ago)
From
Liping Xin at NAOC, SVOM <xlp@nao.cas.cn>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GCN Circular 31098
Subject
GRB 211023A: optical observations and photometric evidence of supernova
Date
2021-11-20T14:54:34Z (4 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
S. Belkin (IKI), A. Pozanenko (IKI), I. Sokolov (INASAN, KIAM), E.
Klunko (ISTP), A. S. Moskvitin (SAO RAS), V. Kim (HSE, FAI), V.
Rumyantsev (CrAO), R. Ya. Inasaridze (AbAO), M. Krugov (FAI), D.
Berezin (IC AMER NASU), G. Butenko (IC AMER NASU), N. Pankov (HSE), D.
Datashvili (AbAO), V. R. Ayvazian (AbAO), G. V. Kapanadze (AbAO) report
on behalf of GRB IKI FuN:
We observed the field of the GRB 211023A (Fermi GBM team, GCN 30958; Di
Lalla et al., GCN 30961; Lesage et al, GCN 30965; Ursi et al, GCN 30969;
Poolakkil, GCN 30998; Ridnaia et al., GCN 31022) with Zeiss-2000 and
Zeiss-600 telescopes of Terskol observatory, AZT-33IK telescope of Sayan
observatory (Mondy), AZT-20 telescope of Assy-Turgen observatory, ZTSh
2.6m-telescope of CrAO observatory, AS-32 telescope of AbAO observatory,
and Zeiss-1000 1-m telescope of SAO RAS. The optical counterpart
(Lipunov et al., GCN 30970; Zhirkov et al, GCN 30977; Kann et al, GCN
30982; Hu et al, GCN 30990; Belkin et al, GCN 31004; Vinko et al, GCN
31008; Belkin et al, GCN 31018; Belkin et al, GCN 31020; Kumar et al,
GCN 31023; Gupta et al., GCN 31041; Strobl et al., GCN 31042; Pozanenko
et al., GCN 31053; Moskvitin et al., GCN 31066) was detected in most of
the stacked images. A preliminary light curve based on our observations
and GCN Circulars cited above can cab be found at
http://grb.rssi.ru/GRB211023A/GRB211023A_LC.png
Starting from the fifth day, a systematic flux excess over the
approximation of the afterglow by a single power law is observed. After
subtraction of the afterglow approximated by the light curve with
a power law (Belkin et al, GCN 31020), and neglecting a contribution of
the host galaxy we determine a preliminary light curve of possible SN, see
http://grb.rssi.ru/GRB211023A/GRB211023A_AG_subtracted_LC.png
Using redshift of GRB 211023A (Pozanenko et al., GCN 31053)
we calculated an absolute magnitude at the maximum of the supposed
supernova (M_R=-19.9 +0.40 -0.29; adjusted by a Galactic extinction
(Schlafly & Finkbeiner, 2011)) and a time since the burst trigger in
the observer frame (t-T0 = 16.9+/-1.5). These parameters are in
agreement with parameters of known SN-GRB (e.g. see Figure 12 from
Belkin et al., Astronomy Letters, 2020). The supernova associated with
GRB 211012A is in agreement with early predictions (Kann et al, GCN
30982; Aimuratov et al., GCN 31056; Minaev et al., GCN 31081).
GCN Circular 31081
Subject
GRB 211023A: classification and SPI-ACS/INTEGRAL registration
Date
2021-11-13T19:43:24Z (4 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
P. Minaev (IKI), A. Pozanenko (IKI), S. Grebenev (IKI), I. Chelovekov
(IKI) report on behalf of GRB IKI FuN
We analyzed GRB 211023A (Di Lalla et al. GCN 30961; Lesage et al. GCN
30965; Ursi et al. GCN 30969; Ridnaia et al. GCN 31022) using publicly
available data of GBM/Fermi and SPI-ACS/INTEGRAL.
Using GBM/Fermi we clearly detect early emission, starting about 80 s
before the GBM trigger. The extended emission (possibly associated with
the activity detected by LAT, Di Lalla et al. GCN 30961, and/or its
extremely bright afterglow, Zhirkov et al. GCN 30977; Kann et al. GCN
30982) was also found, becoming dominant since approximately 150 s the
trigger. Thus, a time profile consists of three episodes with a total
burst duration of more than 300 s in GBM/Fermi (7 - 850 keV), while T90
= 117 +/- 0.5 s. GRB 211023A was also registered by SPI-ACS/INTEGRAL
with marginal detection of the early and the extended emission (T90 =
120 +/- 9 s). Time profiles of GBM and SPI-ACS are presented at
http://grb.rssi.ru/GRB211023A/GRB211023A_GBM_ACS_light_curve.png
We performed spectral analysis of the burst using GBM/Fermi data in the
time interval of (-20, 160) s after the GBM trigger, covering the main
part of GRB activity. The best parameters of Band model are following:
Ep = 96 +/- 5 keV, alpha = -1.67 +/- 0.03, beta = -2.21 +/- 0.05 and
fluence F = (1.341 +/- 0.004)*10^-4 erg/cm^2 in 10 - 1000 keV range.
Assuming a redshift z = 0.390 (Pozanenko et al., GCN 31053) we estimated
Eiso = (7.45 +/- 0.05)*10^52 erg in the 1 keV - 10 MeV energy band.
The position of the burst at Ep,i - Eiso and T90,i - EH diagram [1,2] is
shown by black annuli at
http://grb.rssi.ru/GRB211023A/GRB211023A_Ep-Eiso_two_episodes_SN.png
and
http://grb.rssi.ru/GRB211023A/GRB211023A_EHD_two_episoses_SN.png
The position is typical for type II (long) GRBs, although it is in the
lower bound of their 2 sigma correlation region. This is because of its
relatively low value of the Ep,i parameter. Note that low values of Ep,i
are typical for the nearby bursts (z < 0.5), associated with supernovae
(shown by red annuli at
http://grb.rssi.ru/GRB211023A/GRB211023A_Ep-Eiso_two_episodes_SN.png
and
http://grb.rssi.ru/GRB211023A/GRB211023A_EHD_two_episoses_SN.png )
[1] - Minaev et al., MNRAS, 492, 1919, 2020
[2] - Minaev et al., Astronomy Letters, 46, 9, 573, 2020
GCN Circular 31066
Subject
GRB 211023A: SAO RAS optical observations
Date
2021-11-09T17:32:28Z (4 years ago)
From
Moskvitin Alexander at SAO RAS <mosk@sao.ru>
A. S. Moskvitin and O. I. Spiridonova (SAO RAS),
on behalf of the GRB follow-up team report:
We observed the field of GRB 211023A (Fermi GBM team, GCN 30958,
Di Lalla et al. GCN 30961, Lesage et al. GCN 30965, Ursi et al.
GCN 30969, Poolakkil GCN 30998, Ridnaia et al., GCN 31022)
with the SAO RAS 1-m telescope Zeiss-1000 + CCD-photometer
on November 9. We obtained 6 x 300 sec. frames in Rc band
(00:25:41 -- 01:31:04 UT, T_mid-T0 = 16.4949 days) and 6 x 300 sec.
frames in Ic (00:31:28 -- 01:36:45 UT, T_mid-T0 = 16.4989 days).
The afterglow (Zhirkov et al. GCN 30977, Kann et al. GCN 30982,
Hu et al.GCN 30990, Belkin et al. GCN 31004, Vinko et al. GCN 31008,
Belkin et al. GCN 31018, Belkin et al. GCN 31020, Amit Kumar et al.
GCN 31023, Rahul Gupta et al. GCN 31041, Strobl et al. GCN 31042,
Pozanenko et al. GCN 31053) is clearly detected in our stacked frames
with the following brightness: R = 21.69 +/- 0.09, I = 21.27 +/- 0.14
(the preliminary photometry is based on nearby stars of PS1 catalogue,
gri -> R and I by Lupton 2005 transformations).
GCN Circular 31056
Subject
GRB 211023A: A BdHN of type I
Date
2021-11-08T19:17:11Z (4 years ago)
From
Remo Rufinni at ICRA <ruffini@icra.it>
Y. Aimuratov, L. Becerra, C.L. Bianco, Y-C. Chen, C. Cherubini, S.
Eslamzadeh, S. Filippi, M. Karlica, Liang Li, G.J. Mathews, R. Moradi,
M. Muccino, G.B, Pisani, F. Rastegar Nia, J.A. Rueda, R. Ruffini, N.
Sahakyan, Y. Wang, S.S. Xue, on behalf of the ICRANet and ICRA-USTC
team, report:
The identification of the redshift z=0.36 of GRB 211023A (A. Pozanenko
et al. 2021, GCN 31053), with the isotropic energy of Eiso~6x10^52 erg
in 10-1000 keV (S. Lesage et al. 2021, GCN 30965, S. Poolakkil et al.
2021, GCN 30998), qualify GRB 211023A as a BdHN I, confirmed by the
observation of the GeV emission (N. Di Lalla et al. 2021, GCN 30961),
originated from the black hole (R. Ruffini et al. 2019 ApJ 886 82,
Moradi et al 2021. Phys. Rev. D 104, 063043) and the afterglow emission
(Jan Strobl et al. 2021 GCN 31042) originated from the newborn neutron
star (J.A. Rueda et al. 2020 ApJ 893 148).
Following Ruffini et al. 2021 (MNRAS, 504, 5301,
doi:10.1093/mnras/stab724) we indicate the appearance of the peak of
optical supernova to be observed at (18.4+/-2.6) days after the trigger
(November 10th 2021, uncertainty from November 8th 2021 to November
12th 2021), with the bolometric optical luminosity of
L=(9.0+/-2.7)x10^42 erg/s.
The follow-up optical observations for the SN are recommended.
--
Prof. Remo Ruffini
APS Fellow
Google Fellow
Director of ICRANet
Piazza della Repubblica 10
65122 Pescara (PE) Italy
mobile: +39 339 4752566
Tel. Rome +39 06 49914304
Tel. Pescara +39 085 23054201
Fax: +39 085 4219252
e-mail: ruffini@icra.it
GCN Circular 31053
Subject
GRB 211023A: BTA spectroscopic redshift
Date
2021-11-08T15:16:33Z (4 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
A. Pozanenko (IKI), A. Moiseev (SAO RAS), A. Moskvitin (SAO RAS), E.
Malygin (SAO RAS), S. Belkin (IKI, HSE), N. Pankov (IKI, HSE), V. Kim
(HSE, FAI) on behalf of GRB IKI FuN, A. Rossi (INAF-OAS), D. A. Kann
(HETH/IAA-CSIC) report:
We observed the afterglow of GRB 211023A (Zhirkov et al, GCN 30977, see
also Kann et al, GCN 30982; Hu et al, GCN 30990; Belkin et al, GCN
31004; Vinko et al, GCN 31008; Belkin et al, GCN 31018; Belkin et al,
GCN 31020; Kumar et al, GCN 31023; Gupta et al., GCN 31041; Strobl et
al., GCN 31042) with BTA SAO RAS telescope equipped with SCORPIO-2
(VPHG940@600 grism). A total of 7200 s (6x1200 s) of spectra were
obtained starting on 21-11-05 (UT) 20:50:00, i.e. approximately 13.3016
days after burst. The afterglow is well detected in the acquisition
imaging with R = 21.61 +/- 0.04 (3 x 90 sec. 21-11-05 (UT) 20:43:59 --
20:50:58), and a continuum is visible across the bandwidth of a spectrum
4000 - 8500 A. The spectrum contain significant emission lines H_beta,
[OII] 3727, [OIII] 5007, at a common redshift of z=0.390. We assume
that the lines are from a host galaxy and, therefore, this is the
redshift of GRB 211023A. No evident lines of a possible SN were found.
Calibration of photometry is preliminary and based on nearby stars of
PS1 catalogue, gri -> R by Lupton transformations.
We are grateful to the directorate of SAO RAS for the TOO allocation.
GCN Circular 31042
Subject
GRB 211023A: optical detection by SBT in Ondrejov
Date
2021-11-05T07:08:47Z (4 years ago)
From
Martin Jelinek at Astro.Inst-AVCR,Ondrejov <martin.jelinek@asu.cas.cz>
Jan Strobl, Martin Jelinek, Rene Hudec, Cyril Polasek (ASU CAS Ondrejov, CZ)
We observed the optical afterglow of The Fermi/GBM/AGILE GRB 211023A (Fermi
GBM team, GCN 30958, Di Lalla et al. GCN 30961, Lesage et al. GCN 30965,
Ursi et al. GCN 30969, Poolakkil GCNC 30998) with the double 20cm
wide-field Small Binocular Telescope (SBT, cf. Strobl et al., AN
340,7,p.633, 2019) in Ondrejov observatory starting October 25 at 1:19 UT,
36.2h after the GRB detection. The afterglow (Vladimirov et al. GCN 30970,
Tiurina et al. GCN 30977, Kann et al. GCN 30982, Hu et al. GCN 30990,
Belkin et al. GCN 31004, Vinko et al. GCN 31008, Belkin et al. GCN 31018,
Belkin et al. GCN 31020, Ghosh et al. GCN 31023) is well detected in our
2x80x120s coadded exposure from both tubes:
Tmid-T0 Texp mag dmag filter
1.5706d 10762s 19.61 0.13 clear, calibrated as SDSS-r'(AB)
GCN Circular 31041
Subject
GRB 211023A: continued 1.3m DFOT Optical Observations and possible jet break
Date
2021-11-05T06:00:44Z (4 years ago)
From
Rahul Gupta at ARIES, India <rahulbhu.c157@gmail.com>
Rahul Gupta, S. B. Pandey, Amit Ror, Amit Kumar, Dimple, Ankur Ghosh, Amar
Aryan, Bhavya, and Kuntal Misra (ARIES) report:
We further observed the bright GRB 211023A (Fermi GBM Team 2021, GCN
30958; Lesage et al. 2021, GCN 30965; N. Di Lalla et al. 2021, GCN
30961; Ursi et al. 2021, GCN 30969; and Ridnaia et al. 2021, GCN
31022) with 1.3m Devasthal Fast Optical Telescope (DFOT) located at
Devasthal observatory of Aryabhatta Research Institute of
Observational Sciences (ARIES), India, starting on 2021-10-29 at
19:19:13 UT, i.e., ~ 6.26 days after the Fermi trigger. We obtained 24
and 18 frames having an exposure time of 300 sec in the R and I
filters, respectively. We detected the optical afterglow of GRB
211023A (Lipunov et al. 2021, GCN 30970; Zhirkov et al. 2021, GCN
30977; Kann et al. 2021, GCN 30982; Hu et al. 2021, GCN 30990; Belkin
et al. 2021, GCN 31004, 31018, 31020; Vinko et al. 2021, GCN 31008;
and Kumar et al. 2021, GCN 31023) in our stacked images of both the
filters. The preliminary photometric estimate of the afterglow in the
R filter is following :
Date Start UT T-T0 (mid, days) Filter Exp time (sec) Magnitude
=========================================================2021-10-29
19:19:13 ~6.28 R 300*24 22.58 +/- 0.33
Based on the preliminary photometry reported by using various
ground-based optical telescopes (Kann et al. 2021, GCN 30982; Hu et
al. 2021, GCN 30990; and Belkin et al. 2021, GCN 31004, 31018, 31020)
and our first epoch observations using 1.3m DFOT (Kumar et al. 2021,
GCN 31023), we measure the optical flux decay power-law index of the
afterglow light curve (Galactic extinction corrected) of GRB 211023A
equal to 1.49 +/- 0.04, consistent with those reported earlier (Belkin
et al. 2021, GCN 31004