GRB 190701A

T. N. Ukwatta (LANL), A. P. Beardmore (U Leicester),
N. J. Klingler (PSU), H. A. Krimm (NSF), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester) and A. Tohuvavohu (PSU) report on behalf of
the Neil Gehrels Swift Observatory Team:

At 09:45:20 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 190701A (trigger=912310).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 28.063, +58.906 which is 
   RA(J2000) = 01h 52m 15s
   Dec(J2000) = +58d 54' 23"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multi-peaked
structure with a duration of about 100 sec.  The peak count rate
was ~800 counts/sec (15-350 keV), at ~37 sec after the trigger. 

The XRT began observing the field at 09:47:41.9 UT, 141.1 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source located at RA, Dec 28.08019, 58.91005 which
is equivalent to:
   RA(J2000)  = 01h 52m 19.25s
   Dec(J2000) = +58d 54' 36.2"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 35 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. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 6.36
x 10^21 cm^-2 (Willingale et al. 2013). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 144 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the large, but uncertain, extinction expected. 

Burst Advocate for this burst is T. N. Ukwatta (tilan.ukwatta AT gmail.com). 
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/)

P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team:

Using  promptly downlinked XRT event data for GRB 190701A, we find an
enhanced XRT position of the afterglow: RA, Dec: 28.0815, 58.9095 which
is equivalent to:
   RA (J2000)  = 01 52 19.56
   Dec (J2000) = +58 54 34.3
with an uncertainty of 2.1 arcseconds (radius, 90% confidence).
Analysis of the promptly available data is online at
http://www.swift.ac.uk/sper/912310.

Position enhancement is is described by Goad et al. (2007, A&A, 476,
1401) and Evans et al. (2009, MNRAS, 397, 1177).

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

K. Setoguchi (Kyoto U.), H. Negoro, M. Nakajima, W. Maruyama, M. Aoki, K. Kobayashi (Nihon U.), 
S. Nakahira, T. Mihara, T. Tamagawa, M. Matsuoka (RIKEN),
T. Sakamoto, M. Serino, S. Sugita, H. Nishida, A. Yoshida (AGU), 
Y. Tsuboi, W. Iwakiri, R. Sasaki, H. Kawai, T. Sato (Chuo U.), 
M. Shidatsu (Ehime U.),
N. Kawai, M. Sugizaki, M. Oeda, K. Shiraishi (Tokyo Tech), 
S. Ueno, H. Tomida, M. Ishikawa, Y. Sugawara, N. Isobe, R. Shimomukai, M. Tominaga (JAXA), 
Y. Ueda, A. Tanimoto, S. Yamada, S. Ogawa, T. Yoshitake (Kyoto U.), 
H. Tsunemi, T. Yoneyama, K. Asakura, S. Ide (Osaka U.), 
M. Yamauchi, S. Iwahori, Y. Kurihara, K. Kurogi, K. Miike (Miyazaki U.), 
T. Kawamuro (NAOJ), 
K. Yamaoka (Nagoya U.),
Y. Kawakubo (LSU)
report on behalf of the MAXI team:

The MAXI/GSC nova alert system triggered a bright uncatalogued X-ray transient 
source at 09:46:42 UT on July 1, 2019.
Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (27.548 deg, 58.852 deg) = (01 50 11, +58 51 06) (J2000)
with a 90% C.L. statistical error of 0.16 deg and an additional systematic uncertainty 
of 0.1 deg (90% containment radius).
Without assumptions on the source constancy, we obtain a rectangular error box
for the transient source with the following corners: 
(25.762, 59.105) deg = (01 43 02, +59 06 17) (J2000)
(25.721, 58.781) deg = (01 42 53, +58 46 51) (J2000)
(29.166, 58.620) deg = (01 56 39, +58 37 11) (J2000)
(29.239, 58.942) deg = (01 56 57, +58 56 31) (J2000).
This position is consistent with that of GRB 190701A detected 
by Swift (Ukwatta et al., GCN 24934
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 , Evans et al., GCN 24935
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 ).

The X-ray flux averaged over the scan was 416 +- 39 mCrab
(4.0-10.0keV, 1 sigma error).

There was no significant excess flux in the previous transit at UT 08:14 
and in the next transit at 11:19 UT with an upper limit of 20 mCrab for each.

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

Using 890 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 190701A, 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 = 28.08140, +58.90943 which is equivalent
to:

RA (J2000): 01h 52m 19.54s
Dec (J2000): +58d 54' 33.9"

with an uncertainty of 1.9 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.

Rosa L. Becerra (UNAM), Alan M. Watson (UNAM),  Nat Butler (ASU),
Diego Gonz��lez (UNAM),Alexander Kutyrev (GSFC), William H. Lee (UNAM),
Margarita Pereyra (UNAM), and Eleonora Troja (GSFC) report:

We observed the field of GRB 190701A (Ukwatta et al., GCN Circ.
24934
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 ) with the COATLI 50-cm telescope and interim imager at the
Observatorio Astron��mico Nacional on the Sierra de San Pedro M��rtir
(http://coatli.astroscu.unam.mx) from 2019-07-01 09:47:03 to 10:05:06
(from 25.6 seconds after the alert or 103 seconds to 0.33 hours after
the trigger), obtaining a total of 490 seconds of exposure in the w filter.

Comparing to the USNO and Pan-STARRS1 catalogs, we do not detect any new
sources brighter than w = 20.99 (3-sigma limiting mag) in the XRT error
region
(Osborne et al., GCN Circ. 24940
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 ).

Our w magnitudes are calibrated against the Pan-STARRS1 catalog, are on
an approximate AB system, and are not corrected for Galactic extinction
in the direction of the GRB.

We thank the COATLI technical team and the staff of the Observatorio
Astron��mico Nacional.

H. Kumar, V. Karambelkar, K. Deshmukh, G. Waratkar, V. Bhalerao (IITB), G.
C. Anupama, T. Stanzin (IIA) report on behalf of the GROWTH collaboration:

We observed GRB190701A reported by T. N. Ukwatta et al, (GCN 24934
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 ) with
0.7m GROWTH-India telescope. The field was observed in g, r and i filters.
We didn���t detect any new source within an uncertainty region of 1.9
arcseconds (radius, 90% containment) around RA(J2000) = 01h 52m 19.54s,
Dec(J2000) = +58d 54' 33.9" (J.P. Osborne et al, GCN 24940
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 ).

We obtained the following upper limits:

------------------------------------------------------------------

 JD(Start)| Exposure(sec) | Filter | lim_Mag |

------------------------------------------------------------------

 2458666.351 | 600 | g | 19.18|

 2458666.373 | 600 | r | 20.57|

 2458666.382 | 600 | i | 19.52|

------------------------------------------------------------------


The GROWTH India Telescope (GIT) is a 70-cm telescope with a 0.7 degree
field of view, set up by the Indian Institute of Astrophysics and the
Indian Institute of Technology Bombay with support from the Indo-US Science
and Technology Forum (IUSSTF) and the Science and Engineering Research
Board (SERB) of the Department of Science and Technology (DST), Government
of India (https://sites.google.com/view/growthindia/). It is located at the
Indian Astronomical Observatory (Hanle), operated by the Indian Institute
of Astrophysics (IIA).

M. H. Siegel (PSU) and T. N. Ukwatta (LANL)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 190701A
145 s after the BAT trigger (Ukwatta et al., GCN Circ. 24934
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 ).
No optical afterglow consistent with the enhanced XRT position
(Osborne et al. GCN Circ. 24940
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 )
is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag

white_FC           145          295          147         >20.3
u_FC               303          553          246         >19.8
white              145         6776          727         >21.2
v                  629        11104          409         >19.3
b                  559         6570          432         >20.6
u                  303         6365          659         >20.6
w1                 677         6160          432         >19.9
m2                 652         5955          432         >19.3
w2                 610        10926         1158         >20.2

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.59 in the direction of the burst
(Schlegel et al. 1998).

E. Ambrosi  (INAF-IASFPA) , V. D'Elia (ASDC), D.N. Burrows (PSU), J. D.
Gropp (PSU), A. Tohuvavohu (PSU), K.L. Page (U. Leicester), A.P.
Beardmore (U. Leicester), P.A. Evans (U. Leicester), A. D'Ai
(INAF-IASFPA) and T.N. Ukwatta report on behalf of the Swift-XRT team:

We have analysed 8.4 ks of XRT data for GRB 190701A (Ukwatta et al. GCN
Circ. 24934
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 ), from 144 s to 34.9 ks after the  BAT trigger. The data
comprise 10 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. 24935
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 ).

The light curve can be modelled with an initial power-law decay with an
index of alpha=8.0 (+0.0, -0.9), followed by a break at T+239 s to an
alpha of 0.40 (+0.08, -0.09).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.81 (+0.23, -0.12). The
best-fitting absorption column is  consistent with the Galactic value
of 6.4 x 10^21 cm^-2 (Willingale et al. 2013). The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 4.7 x 10^-11 (7.1 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:	     6.4 (+/-1.0) x 10^21 cm^-2
Galactic foreground: 6.4 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:	     1.81 (+0.23, -0.12)

If the light curve continues to decay with a power-law decay index of
0.40, the count rate at T+24 hours will be 0.018 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 8.5 x
10^-13 (1.3 x 10^-12) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00912310.

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

A. Y. Lien (GSFC/UMBC), S. D. Barthelmy (GSFC),  J. R. Cummings (CPI),
H. A. Krimm (NSF), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), M. Stamatikos (OSU), 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 190701A (trigger #912310)
(Ukwatta, et al., GCN Circ. 24934
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 ).  The BAT ground-calculated position is
RA, Dec = 28.131, 58.899 deg which is 
  RA(J2000)  =  01h 52m 31.5s 
  Dec(J2000) = +58d 53' 56.9" 
with an uncertainty of 2.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 52%.

The mask-weighted light curve shows a multi-peaked structure.  The main period
of emission includes three broad peaks between roughly T+0 sec and T+100 sec,
peaking about T+38 sec.  T90 (15-350 keV) is 52.4 +- 4.0 sec (estimated error
including systematics).

The time-averaged spectrum from T+35.0 to T+90.0 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.91 +- 0.27.  The fluence in the 15-150 keV band is 8.7 +- 1.5 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+37.92 sec in the 15-150 keV band
is 1.2 +- 0.3 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/912310/BA/