GRB 190613A

E. Ambrosi (INAF-IASFPA), A. D'Ai (INAF-IASFPA), V. D'Elia (SSDC),
J.D. Gropp (PSU), N. J. Klingler (PSU), A. Y. Lien (GSFC/UMBC),
F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL), M. H. Siegel (PSU)
and A. Tohuvavohu (PSU) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 04:07:18 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 190613A (trigger=908288).  Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 182.559, +67.233 which is
   RA(J2000) = 12h 10m 14s
   Dec(J2000) = +67d 13' 58"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty).  The BAT light curve showed a single peak
structure with a duration of about 30 sec.  The peak count rate
was ~500 counts/sec (15-350 keV), at ~10 sec after the trigger.

The XRT began observing the field at 04:09:34.8 UT, 136.5 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 182.53286, 67.23489 which
is equivalent to:
   RA(J2000)  = 12h 10m 07.89s
   Dec(J2000) = +67d 14' 05.6"
with an uncertainty of 4.0 arcseconds (radius, 90% containment). This
location is 37 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. No
spectrum from the promptly downlinked event data is yet available to
determine the column density.

The initial flux in the 2.5 s image was 1.18e-09 erg cm^-2 s^-1 (0.2-10
keV).

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 144 seconds after the BAT trigger. There is a candidate afterglow in
the list of sources generated on-board at
  RA(J2000)  =  12:10:07.01 = 182.52919
  DEC(J2000) = +67:14:07.0  =  67.23528
with a 90%-confidence error radius of about 1.10 arc sec. This position is 9.9
arc sec. from the center of the XRT error circle. The estimated magnitude is
18.28. No correction has been made for the expected extinction corresponding to
E(B-V) of 0.02.

Burst Advocate for this burst is E. Ambrosi (elena.ambrosi AT inaf.it).
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/)

The Fermi GBM team reports the detection of a likely LONG GRB

At 04:07:18 UT on 13 Jun 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190613A (trigger 582091643.234478 / 190613172).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 176.4, Dec = 64.8 (J2000 degrees, equivalent to J2000 11h 45m, 64d 47'), with a statistical uncertainty of 3.0 degrees.

The angle from the Fermi LAT boresight is 11.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190613172/quicklook/glg_skymap_all_bn190613172.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190613172/quicklook/glg_healpix_all_bn190613172.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190613172/quicklook/glg_lc_medres34_bn190613172.gif

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

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
582091643 at 04:07:18 on 13 June 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) = 200.2+/-13.8 deg
Decl.(2000.0) = 66.4+/-3.8 deg
We estimate an additional systematic error of 2 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB190613172/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB190613172/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB190613172/json

WeiKang Zheng and Alexei V. Filippenko (UC Berkeley) report on
behalf of the KAIT GRB team:

The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at
Lick Observatory, responded to the Swift GRB 190613A (Ambrosi et al.,
GCN 24798
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 ) starting at 734s after the burst. Observations were
performed with a sequence in the clear (roughly R), V, and I filters,
and the exposure time was 60 s per image. We detected a fading source
at the Swift/UVOT reported afterglow position (Ambrosi et al.,
GCN 24798
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 ) in all the filters. We estimate the clear band magnitude
to be ~18.2 at 764s after the burst and faded to ~19.0 at 1290s after the
burst.
Observation are on going, multi-band follow-ups are encouraged.

[GCN OPS NOTE(14jun19):  The typo in Swift's name was corrected.]

V. Lipunov, E.Gorbovskoy, V.Kornilov, N.Tiurina, A.Kuznetsov, I.Gorbunov, 
V.Vladimirov, P.Balanutsa, D.Vlasenko, D.Zimnukhov, F.Balakin,A. Chasovnikov,
V.Topolev, V.Senik, D.Kuvshinov(Lomonosov Moscow State University, SAI, Physics Department),

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

D. Buckley (South African Astronomical Observatory),

R. Podesta, C. Lopez, C.Francile, F. Podesta (Observatorio Astronomico Felix Aguilar OAFA, San Juan National University),

H.Levato (Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE, SJNU)

O. Gress, N.M. Budnev, O.Ershova, S.Yazev (Applied Physics Institute, Irkutsk State University),

V. Yurkov, A. Gabovich, Yu. Sergienko, D. Kobcev (Blagoveschensk Educational State University),

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

MASTER-IAC robotic telescope (MASTER Global Robotic Net:  Lipunov et al., 
2010, Advances in Astronomy,vol.2010, 30L  (http://observ.pereplet.ru)
located in Spain (IAC Teide Observatory) was pointed to 
the  GRB 190613A (Swift alert, Ambrosi et al. GCN 24798
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 , Fermi 
localization GCN 24799
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 , BALROG localization Burgess et al. GCN 24800
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 )
38 sec after notice time (104 sec after trigger time)
at 2019-06-13 04:09:09 UT (Lipunov et al. GCN 24802
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 ).

On our first (20s exposure)  set MASTER auto-detection system
found 1 optical transient within Swift error-box (ra=182.558 dec=67.2325 r=0.05) 
brighter than 16.4.


  T-Tmid      Date      Time       Expt.        Ra                Dec           Mag
---------|---------------------|-------|-----------------|-----------------|-------
      114   2019-06-13 04:09:09      20   ( 12h 10m 07.08s , +67d 14m 06.5s)    15.96


this OT, discovered by Swift and also confirmed by KAIT(Ambrosi et al. GCN 24798
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 , WeiKang Zheng et al. GCN 24801
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 )

The 5-sigma upper limit has been about 16.4mag

J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 3378 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 190613A, 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 = 182.52964, +67.23535 which is equivalent
to:

RA (J2000): 12h 10m 7.11s
Dec (J2000): +67d 14' 07.3"

with an uncertainty of 1.5 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.

D.N. Burrows (PSU), J.P. Osborne (U. Leicester), K.L. Page (U.
Leicester), A.P. Beardmore (U. Leicester), V. D'Elia (ASDC), A. D'Ai
(INAF-IASFPA), A. Melandri (INAF-OAB), A. Tohuvavohu (PSU), S. J.
LaPorte (PSU) and  report on behalf of the Swift-XRT team: report on
behalf of the Swift-XRT team:

We have analysed 8.1 ks of XRT data for GRB 190613A, from 142 s to 18.3
ks after the  BAT trigger. The data comprise 127 s in Windowed Timing
(WT) mode with the remainder in Photon Counting (PC) mode. The enhanced
XRT position for this burst was given by Osborne et al. (GCN Circ.
24809
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 ).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=5.1 (+1.1, -0.9). At T+174 s  the decay
flattens to an alpha of -1.500000 (+0.905300, -0.000007). The light
curve breaks again at T+207 s to a decay with alpha=5.0 (+0.7, -0.6), 
and  again at T+372 s s to alpha=1.44 (+0.18, -0.15),  before a final
break at T+7345 s s after which the decay index is -1.5 (+0.0, -1.4).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index	of 2.01 (+/-0.12). The
best-fitting absorption column is  5.1 (+2.8, -2.6) x 10^20 cm^-2, in
excess of the Galactic value of 1.5 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.75 (+0.22, -0.15)
and a best-fitting absorption column of 2.0 (+4.9, -0.5) x 10^20 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.7 x 10^-11 (3.8 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:	     2.0 (+4.9, -0.5) x 10^20 cm^-2
Galactic foreground: 1.5 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:	     1.75 (+0.22, -0.15)

If the light curve continues to decay with a power-law decay index of
-1.5, the count rate at T+24 hours will be 0.41 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.5 x
10^-11 (1.6 x 10^-11) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00908288.

This circular is an official product of the Swift-XRT team.

F. E. Marshall (NASA/GSFC) and E. Ambrosi (INAF-IASFPA)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 190613A
145 s after the BAT trigger (Ambrosi et al., GCN Circ. 24798
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 ).
A source consistent with the enhanced XRT position
(Osborne et al. GCN Circ. 24809
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 )
is detected in the initial UVOT exposures.

The preliminary UVOT position is:
    RA  (J2000) =  12:10:07.01 = 182.52920 (deg.)
    Dec (J2000) = +67:14:07.0  =  67.23529 (deg.)
with an estimated uncertainty of 0.43 arc sec. (radius, 90% confidence).

Preliminary detections and 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are:
Filter         T_start(s)   T_stop(s)      Exp(s)           Mag

white              145          295          147         17.88 +/- 0.04
v                  634         1061           58         18.63 +/- 0.29
b                  560          753           39         18.93 +/- 0.21
u                  303          553          246         18.88 +/- 0.11
w1                 685        11118         1121        >20.1
m2                5323         6859          296        >20.8
w2                4913         6548          393        >21.5

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).

S. Poolakkil (UAH) and C. Meegan (UAH)
report on behalf of the Fermi GBM Team:

"At 04:07:18.23 UT on 13 June 2019, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 190613A (trigger 582091643/ 190613172),
which was also detected by the Swift/BAT (Ambrosi et al. 2019, GCN 24798
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 ).
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight
at the GBM trigger time is 9 degrees.

The GBM light curve shows a single peak
with a duration (T90) of about 18 s (50-300 keV).
The time-averaged spectrum from T0-1.0 s to T0+19.4 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is 0.06 +/- 0.18 and
the cutoff energy, parameterized as Epeak, is 108 +/- 5 keV.

The event fluence (10-1000 keV) in this time interval is
(3.092 +/- 0.129)E-06 erg/cm^2. The 1-sec peak photon flux
measured starting from T+11.9 s in the 10-1000 keV band
is 2.3 +/- 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/"

M. Stamatikos (OSU), E. Ambrosi (INAF-IASFPA)
S. D. Barthelmy (GSFC), J. R. Cummings (CPI),
H. A. Krimm (NSF), A. Y. Lien (GSFC/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), T. N. Ukwatta (LANL)
(i.e. the Swift-BAT team):

Using the data set from T-239 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 190613A (trigger #908288)
(Ambrosi et al., GCN Circ. 24798
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 ).  The BAT ground-calculated position is
RA, Dec = 182.552, 67.244 deg which is
   RA(J2000)  =  12h 10m 12.5s
   Dec(J2000) = +67d 14' 39.7"
with an uncertainty of 2.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 9%.

The mask-weighted light curve shows a weak pulse that starts at ~T0, peaks
at ~T+7 s, and ends at ~T+20 s. T90 (15-350 keV) is 17.6 +- 3.1 sec
(estimated error including systematics).

The time-averaged spectrum from T+0.6 to T+20.3 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.22 +- 0.26.  The fluence in the 15-150 keV band is 1.7 +- 0.3 x 10^-6
erg/cm2.
The 1-sec peak photon flux measured from T+6.88 sec in the 15-150 keV band
is 1.5 +- 0.7 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/908288/BA/

[GCN OPS NOTE(13jun19): Per author's request, in the 3rd line
"GCN Circ. 908288" was corrected to read "GCN Circ. 24798".

Martin Jelinek, Jan Strobl (ASU CAS Ondrejov, CZ),
Martin Masek, Petr Janecek, Sergey Karpov, Jakub Jurysek,
Jan Ebr, Ronan Cunniffe, Petr Travnicek and Michael Prouza
(Institute of Physics, Prague, CZ)

report:

The 25cm robotic telescope FRAM-ORM at La Palma (Spain)
reacted robotically to the alert of GRB190613A (Ambrosi et al,
GCNC 24798), starting with a series of 20 s unfiltered images
at 04:10:11 UT, i.e. 3 min post trigger.

We clearly detect the source reported by (Ambrosi et al, GCN
24798
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 ; Zheng & Filipenko, GCN 24801
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  and Lipunov et al, GCN
24803
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 ), decaying at a rate of alpha ~ 1.51. The brightnes of
the object was R = 18.2 +- 0.2 at an image centered at 04:25:15
UT, i.e. 18 min post burst.

[GCN OPS Note(15jun19): Per OPS, the extra "Subject:" was removed
from the Subject line.]

V. Cunningham (U of Maryland), J. D. Neill (Caltech), S. B. Cenko
(NASA GSFC), and R. Walters (Caltech) report on behalf of the
SEDM team:

We observed the optical counterpart to GRB 190613A (Ambrosi et al., GCN
24798
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 ) with the Spectral Energy Distribution Machine (SEDM) on the 60 inch
telescope at Palomar Observatory. The SEDM is a low resolution (R ~ 100)
integral field unit spectrometer with a multi-band (ugri) rainbow camera imager
(see Blagorodnova et al. 2018, PASP, 130, 035003, and Rigault et al. 2019,
astro-ph/1902.08526).

The SEDM began observing the optical counterpart at 04:18:22 UTC (8.75
minutes after the burst trigger time). We performed an 1800 s exposure over the
wavelength range 3800-9200 A. The continuum emission is well-fit by a power
law spectrum with index alpha = 0.56 (f_nu ~ nu^-alpha).  We detect an
absorption line at an observed wavelength of ~ 4597 A. We tentatively identify
this line as due to Lyman alpha at z = 2.78 - however due to the lack of
corroborating features we consider this redshift tentative currently.

[GCN OPS NOTE(07sep19): Per author's request, in the last paragraph,
the "alpha = 0.56" was changed to "alpha = 1.4".]

S. Belkin (IKI), A. Novichonok (KIAM), A. Zhornichenko (KIAM), R. Ya. 
Inasaridze (AbAO),  V.R. Ayvazian (AbAO), A. Pozanenko (IKI), E. Mazaeva 
(IKI), A. Volnova (IKI), I. Molotov (KIAM), Sh. Ehgamberdiev (UBAI) report 
on behalf of larger IKI GRB FuN collaboration:

We observed the field of the  GRB 190613A (Ambrosi et al., GCN  24798
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 ) 
with RC-36  telescope of Kitab Observatory  and AS-32 of Abastumani 
observatory . We do not detect the optical afterglow (Ambrosi et al., GCN 
24798
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 ; Zheng et al., GCN  24801
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 ;  Lipunov et al., GCN  24803
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 ).  Preliminary 
photometry of the field is following.

Date       UT start   t-T0       Filter Exp.   OT  Err.   UL(3sigma) 
Telescope
                       (mid, days)        (s)

2019-06-13 16:26:41  0.54575    CR     5500  n/d  n/d   20.6  RC-36
2019-06-13 21:33:40  0.73706      R      1800  n/d  n/d   21.0  AS-32


The photometry is based on the nearby USNO-B1 (R2) stars
USNO-B1.0_id  R2
1572-0165015 13.62
1572-0164999 14.91
1572-0164916 14.28

[GCN OPS NOTE(15jun19): Per OPS, the typo in the Subject-line
"1906013A" was changed to "190613A".]

V. Cunningham (U of Maryland), J. D. Neill (Caltech), S. B. Cenko

(NASA GSFC), and R. Walters (Caltech) report on behalf of the

SEDM team:

We observed the optical counterpart to GRB 190613A (Ambrosi et al., GCN

24798
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 ) with the Spectral Energy Distribution Machine (SEDM) on the 60 inch

telescope at Palomar Observatory. The SEDM is a low resolution (R ~ 100)

integral field unit spectrometer with a multi-band (ugri) rainbow camera
imager

(see Blagorodnova et al. 2018, PASP, 130, 035003, and Rigault et al. 2019,

astro-ph/1902.08526).

The SEDM began observing the optical counterpart at 04:18:22 UTC (8.75

minutes after the burst trigger time). We performed an 1800 s exposure over
the

wavelength range 3800-9200 A. The continuum emission is well-fit by a power

law spectrum with index alpha = 0.56 (f_nu ~ nu^-alpha).  We detect an

absorption line at an observed wavelength of ~ 4597 A. We tentatively
identify

this line as due to Lyman alpha at z = 2.78 - however due to the lack of

corroborating features we consider this redshift tentative currently.