GRB 190323.85, GRB 190323, GRB 190323A

V. Sharma, D. Bhattacharya, A. Vibhute and T. Khanam (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data showed the detection of a long GRB 190323A, which was also detected by Insight-HXMT/HE (Luo Q. et al., GCN # 24005).

The source was clearly detected in the 40-200 keV energy range. The light curve shows multiple pulses of emission with strongest peak at 21:05:40.500 UT. The measured peak count rate associated with the burst is 153 cts/s above the background in the combined data of four quadrants, with a total of 1848 cts. The local mean background count rate was 533 cts/s. Using cumulative rates, we measure a T90 of 36.6 s.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project.

Q. Luo, C. K. Li, X. B. Li, G. Li, J. Y. Liao, S. L. Xiong, 
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, X. F. Lu,
A. M. Zhang, Y. F. Zhang, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP),
report on behalf of the Insight-HXMT team:

At 2019-03-23T21:05:24.000 (T0), the Insight-HXMT/HE detected
GRB 190323A(trigger ID: HEB190323878) in a routine search of the data,
which was also triggered by Fermi/GBM(F. Kunzweiler et al. ,GCN 23990).

The Insight-HXMT/HE light curve mainly consists of multiple 
pulses with a duration (T90) of 42.40 s measured from T0-5.50 s.
The 1-ms peak rate, measured from T0-0.190 s, is 938 cnts/sec.
The total counts from this burst is 13490 counts.
URL_LC: http://www.hxmt.org/images/GRB/HEB190323878_lc.jpg

All measurements above are made with the CsI detectors operating in the
regular mode with the energy range of about 80-800 keV (record energy).
Only gamma-rays with energy greater than about 200 keV can penetrate
the spacecraft and leave signals in the CsI detectors installed inside
of the telescope.

Insight-HXMT is the first Chinese space X-ray telescope, which was
fundedjointly by the China National Space Administration (CNSA) and
the Chinese Academy of Sciences (CAS).
More information about it could be found at:
http://www.hxmt.org.

V. Lipunov, E. Gorbovskoy, V.Kornilov, D.Kuvshinov, N.Tyurina, P.Balanutsa,
A.Kuznetsov, V.V.Chazov, D. Vlasenko
Lomonosov Moscow State University,
Sternberg Astronomical Institute, Moscow State University

A. Tlatov, V.Senik, A.V. Parhomenko, D. Dormidontov
Kislovodsk Solar Station of the Pulkovo Observatory

K. Ivanov, O. Gres, N.M. Budnev, S. Yazev, O. Chuvalaev, V. Poleshchuk
Irkutsk State University

V. Yurkov, A. Gabovich, Yu. Sergienko
Blagoveschensk Educational State University, Blagoveschensk

R. Podesta, Carlos Lopez and F. Podesta
Observatorio Astronomico Felix Aguilar (OAFA)

Hugo Levato and Carlos Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)

R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres
The Instituto de Astrofisica de Canarias

D. Buckley, S. Potter, A. Kniazev, M. Kotze
South African Astronomical Observatory



MASTER-IAC robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Spain (IAC Teide Observatory) was pointed to the  SWIFT GRB190323.85 (  2h 40m 36.72s , +61d 14m 45.60s, R=0.05) 41 sec after trigger time at 2019-03-23 20:31:28 UT, with upper limit up to  18.5 mag. The observations began at zenit distance = 57 deg. The sun  altitude  is -17.5 deg. 

MASTER-Tunka robotic telescope  located in Russia (Applied Physics Institute, Irkutsk State University) was pointed to the  SWIFT GRB190323.85 68 sec after trigger time at 2019-03-23 20:31:55 UT, with upper limit up to  16.7 mag. The observations began at zenit distance = 67 deg. The sun  altitude  is -23.2 deg. 

The galactic latitude b = -60 deg., longitude l = 98 deg.

We obtain a following upper limits.  

Tmid-T0  |          Site       |Filt.| Expt. | Limit| Comment
_________|_____________________|_____|_______|______|________

      46 |          MASTER-IAC |  P- |    10 | 16.4 |        
      46 |          MASTER-IAC |  P| |    10 | 16.8 |        
      74 |        MASTER-Tunka |   C |    10 | 12.3 |        
     101 |          MASTER-IAC |  P- |    20 | 17.0 |        
     101 |          MASTER-IAC |  P| |    20 | 17.3 |        
     138 |          MASTER-IAC |  P- |    20 | 17.0 |        
     138 |          MASTER-IAC |  P| |    20 | 17.3 |        
     180 |          MASTER-IAC |  P- |    30 | 17.2 |        
     180 |          MASTER-IAC |  P| |    30 | 17.6 |        
     233 |          MASTER-IAC |  P- |    40 | 17.4 |        
     233 |          MASTER-IAC |  P| |    40 | 17.9 |        
     293 |          MASTER-IAC |  P- |    50 | 17.7 |        
     293 |          MASTER-IAC |  P| |    50 | 18.0 |        
     368 |          MASTER-IAC |  P| |    70 | 18.2 |        
     368 |          MASTER-IAC |  P- |    70 | 17.8 |        
     411 |        MASTER-Tunka |  P| |    70 | 16.4 |        
     458 |          MASTER-IAC |  P- |    80 | 18.0 |        
     458 |          MASTER-IAC |  P| |    80 | 18.4 |        
     563 |          MASTER-IAC |  P- |   100 | 18.0 |        
     563 |          MASTER-IAC |  P| |   100 | 18.5 |        
     567 |        MASTER-Tunka |  P| |   100 | 16.5 |        
    1239 |        MASTER-Tunka |  P| |   180 | 15.5 |        
    1489 |        MASTER-Tunka |  P| |   180 | 15.1 |        
    2272 |        MASTER-Tunka |  P| |   180 | 16.4 |        
    2524 |        MASTER-Tunka |  P| |   180 | 16.7 |        
Filter C is a clear (unfiltred) band. 


The observation and reduction will continue. 
The message may be cited.

F. Kunzweiler, B. Biltzinger, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
575067924 at 21:05:19 on 23 March 2019 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 36.6+/-0.5 deg
Decl.(2000.0) = 3.0+/-0.8 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB190323879/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB190323879/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB190323879/json

F. Kunzweiler, B. Biltzinger, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
575018216 at 07:16:51 on 23 March 2019 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 138.6+/-2.9 deg
Decl.(2000.0) = 2.6+/-3.3 deg
We estimate an additional systematic error of 2 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB190323303/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB190323303/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB190323303/json