////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  932
SUBJECT: BeppoSAX ALERT: GRB010214
DATE:    01/02/14 12:45:30 GMT
FROM:    Luigi Piro at IAS/CNR Frascati  <piro@ias.rm.cnr.it>

BeppoSAX ALERT: GRB010214

On Feb. 14, 08:48:11 U.T. a new Valentine GRB (GRB010214) has been
detected simultaneously by the GRBM and WFC2 aboard BeppoSAX.

Preliminary  coordinates from WFC are:

R.A.(2000)= 265.191
DEC.(2000)= 48.564

The error radius at this stage of analysis is 5'.

We are planning a BeppoSAX-NFI observation.


G. Gandolfi on behalf of
BeppoSAX Mission Scientist

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  933
SUBJECT: GRB010214 refined WFC position
DATE:    01/02/14 14:18:40 GMT
FROM:    Luigi Piro at IAS/CNR Frascati  <piro@ias.rm.cnr.it>

GRB010214 refined WFC position

Refined  coordinates of GRB010214 from WFC are:

R.A.(2000)= 265.252
DEC.(2000)= 48.544

The error radius is 3'.

G. Gandolfi
on behalf of BeppoSAX Mission Scientist

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  935
SUBJECT: GRB 010214, optical observations
DATE:    01/02/15 05:21:27 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

S. Klose, B. Stecklum (Thueringer Landessternwarte Tautenburg), 
A. Castro-Tirado (LAEFF-INTA, Madrid, and IAA-CSIC, Granada), and
J. Greiner (AIP Potsdam)

report:

The error circle of GRB 010214 (Gandolfi et al., GCN #933) was imaged in R 
and I on February 15, 0:55 UT - 3:49 UT (about 16 - 19 hrs after the burst), 
using the Tautenburg Schmidt telescope equipped with the Schmidt focus CCD 
camera (fov 35 x 35 arcmin). 

A visual comparison of the combined R-band frames with the DSS2 red and the IR 
sky survey does not reveal any afterglow candidate brighter than about R=20. 
(The DSS IR sky survey excludes a promising candidate at RA, DEC (J2000) = 
17:40:55.0, 48:30:51 +/- 1 arcsec which seems to have no counterpart on 
the DSS2 red survey; these coordinates are based on the DSS2 red fits file.)

This message is quotable.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  937
SUBJECT: GRB010214: BeppoSAX/NFI Observations
DATE:    01/02/15 14:29:39 GMT
FROM:    Luigi Piro at IAS/CNR Frascati  <piro@ias.rm.cnr.it>

GRB010214: BeppoSAX/NFI Observations

A BeppoSAX TOO observation of GB010214 has started about 6
hours after the GRB.
Preliminary analysis of the first orbits show a source in the
MECS(1.6-10 keV) image.

The position is:

RA = 265.234
Delta = 48.566

The error radius is 1.5 arcminutes.

We detect a clear fading behaviour of the X-ray source, but at this stage
we cannot exclude a faint contamination by RASSFS Catalogue source 1RXS
J174042.9+48340 at 2.2' which may slightly affect the position of the
afterglow. More refined analysis are in progress.

G. Gandolfi
on behalf of BeppoSAX Mission Scientist

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  938
SUBJECT: GRB010214 Optical Observation
DATE:    01/02/15 15:25:56 GMT
FROM:    Jin Zhu at BAO  <zj@bac.pku.edu.cn>

GRB010214 Optical Observation

J. Zhu, S. J. Xue, on behalf of the Beijing Astronomical Observatory GRB 
team, report:

"The 58 x 58 arcmin area centered at the BeppoSAX WFC error circle of
GRB010214 (G. Gandolfi, GCN #933) were imaged on Feb. 14 between 16:48 UT
to 17:29 UT and 19:02 UT to 21:53 UT (8 to 13 hours after the burst)
with the BAO 0.6/0.9-m Schmidt telescope. Image information is as
followes:

No     Image Name      start time exposure   Filter  Notes
                          (UT)    (seconds)
-- -------------------- ---------- --------- ------- --------------
01 p1751955MG01i039.fit 16:47:45.0  600       BATC-i star elongated
02 p1751955MG01i040.fit 17:01:25.0  300       BATC-i
03 p1751955MG01i041.fit 17:09:13.0  300       BATC-i
04 p1751955MG01i042.fit 17:16:44.0  300       BATC-i
05 p1751955MG01i043.fit 17:24:00.0  300       BATC-i
06 p1751955MG01i047.fit 19:02:16.0 1200       BATC-i
07 p1751955MG01i048.fit 19:24:31.0 1200       BATC-i
08 p1751955MG01n050.fit 20:24:59.0 1200       BATC-n
09 p1751955MG01n051.fit 20:47:26.0 1200       BATC-n
10 p1751955MG01n052.fit 21:10:03.0 1200       BATC-n
11 p1751955MG01n053.fit 21:32:59.0 1200       BATC-n

There were no guiding for images (01)-(05) and the first image had very
bad tracing for the low pointing direction of the telescope. The filters 
used were BATC-i (6660A +/- 240A) and BATC-n (8480A +/- 75A).

Visual comparison of the BeppoSAX WFC error circle area for the combined 
image of (06) and (07) (detection limit about R=20) and the combined image 
of (08)-(11) with the DSS2 red image shows no afterglow candidate.

There is a faint object only appeared in image (2) at RA(2000)=17:40:57.68,
Dec(2000)=+48:33:58.3, with R=19.1 (comparison star: RA=17:41:01.76, Dec=
+48:33:13.7, R=15.6). It was not bad pixel or ghost image. But the 
possibility of cosmic ray could not be excluded completely. Observations
with large telescope might be necessary.

The central part of the image (2) could be found at
http://vega.bac.pku.edu.cn/~zj/grb/grb010214/p1751955MG01i040.gif

This report may be cited."

-- 
========================================================================
Jin Zhu                          | Tel.:  +86-10-62751286 (O)
Beijing Astronomical Observatory |        +86-314-5520267 (Schmidt dome)
Chinese Academy of Sciences      | Pager: +86-10-96301682333
P. R. China                      | Fax :  +86-10-62765031
------------------------------------------------------------------------
Room 2919, No. 2 Science Building, CAS-PKU Beijing Astrophysics Center,
Peking University, Beijing 100871, P. R. CHINA.
------------------------------------------------------------------------
email: zj@bac.pku.edu.cn                  http://vega.bac.pku.edu.cn/~zj
========================================================================
////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  939
SUBJECT: Possible InfraRed Transient of GRB 010214.
DATE:    01/02/15 17:33:01 GMT
FROM:    Angelo Antonelli at Obs. Astro. di Roma  <angelo@coma.mporzio.astro.it>

A. Di Paola, F. D'Alessio, L.A. Antonelli, Osservatorio Astronomico 
di Roma, Italy, M. Dolci, Osservatorio Astronomico di Teramo, Italy,
on behalf of a larger collaboration report:

"We observed the BeppoSAX WFC error circle of GRB 010214 
(Gandolfi, GCN #933) with the AZT-24 1.1-meter telescope 
at Campo Imperatore (AQ), Italy.

The J-band observation started at February 15.17928 UT and 
the field was imaged for a total exposure time of 2550 sec. 
We detected a faint point-like source which is not present 
in the Digital Sky Survey-2 IR, R and B plates nor the
2MASS plates. The source is located at:

    RA(J2000)=   17h 40m 54.0s
    DEC(J2000)= +48d 32' 20"
    (uncertainty is 2")

This position lies within the WFC error circle (GCN #933)
and is just outside the BeppoSAX NFI error circle quoted
by Gandolfi GCN #937.

The source was detected with a S/N=12 and had a magnitude of 
J=19.1+/-0.3.

Further observations are needed in order to confirm that this 
is the IR counterpart of GRB 010214.

The J-band image is posted at 
http://argos.mporzio.astro.it/angelo/grb010214/

This message is citable."





////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  942
SUBJECT: GRB010214, optical observations
DATE:    01/02/15 22:13:45 GMT
FROM:    Rene Hudec at AIO  <rhudec@asu.cas.cz>

R. Hudec, M. Jelinek, Astronomical Institute Ondrejov, Czech Republic,
M. Tichy, J. Ticha, Klet Observatory, Czech Republic, report:

Unfiltered optical images of the GRB010214 BeppoSAX WFC error box
(GCN#933) were acquired on 2001 February 15.07 with the 0.57-meter
telescope (+CCD camera SBIG ST-8) of the Klet Observatory, Czech
Republic, for a total exposure time of 600 sec.

No new or noticeable object down to a magnitude ~20.5 is detected inside
the WFC error box when we compare our summed frame with the DSS-II
Digital Sky Survey. We also note that no objects are present at the
positions indicated by A. Di Paola et al. (possible infrared transient,
GCN#939) and by J. Zhu and S. J. Xue (possible optical transient,
GCN#938).

This message can be cited.

Correction: in the GCN#941 (GRB010213, optical observations), one should
read February 15.09 instead of January 15.09.




////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  943
SUBJECT: GRB010214, Radio Observations
DATE:    01/02/16 00:02:31 GMT
FROM:    Edo Berger at Caltech  <ejb@astro.caltech.edu>

E. Berger (Caltech) and D. A. Frail (NRAO) report on behalf of a larger
collaboration:

"Beginning on February 15.41 UT we observed the entire BeppoSAX refined 
WFC error circle of GRB010214 (GCN#933) with the VLA at 4.86 and 8.46 
GHz.  We find no new sources with a flux density level larger than 310 
and 210 microJy, respectively (5 sigma).  A limit of 160 and 130 microJy,
respectively can be placed on the absence of a radio source at the 
position of the possible IR transient (GCN#939)."

This message may be cited.




////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  944
SUBJECT: J-Band Observation of GRB 010214.
DATE:    01/02/16 12:25:30 GMT
FROM:    Angelo Antonelli at Obs. Astro. di Roma  <angelo@coma.mporzio.astro.it>

L.A. Antonelli, F. D'Alessio, A. Di Paola, Osservatorio Astronomico
di Roma, Italy, M. Dolci, Osservatorio Astronomico di Teramo, Italy,
on behalf of a larger collaboration report:

On February 16.078935 UT we observed again the field of the suspect 
J-band counterpart of GRB 010214 (Di Paola et al., GCN #939)
for a total exposure time of 7200 sec, with the AZT-24 1.1-meter 
telescope at Campo Imperatore (AQ), Italy.

The point-like source reported in GCN #939 was still detected 
with a S/N=20 and a magnitude of J=19.1+/-0.1 consistent with the 
previous measurement. 

The source could be a very red foreground object but at this time, 
due to the few existent IR measures of GRBs afterglow, an anomalous 
IR afterglow cannot be excluded. Further IR observations are needed.
 
The new J-band image is posted at
http://argos.mporzio.astro.it/angelo/grb010214/

This message is citable."
////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  948
SUBJECT: GRB 010214 optical observation
DATE:    01/02/19 11:42:38 GMT
FROM:    Taichi Kato at Kyoto U  <tkato@kusastro.kyoto-u.ac.jp>

GRB 010214 optical observation

M. Uemura, T. Kato, Kyoto Univ., and H. Yamaoka, Kyushu Univ., on
behalf of VSNET-GRB collaboration report:

"We observed the field of GRB 010214 starting at Feb. 14, 15:44 UT,
i.e. about 7.0 hours after the burst with 0.30-m Schmidt-Cassegren
telescope (+ unfiltered CCD) at Kyoto University.  The earlier images
(total exposure 930 seconds, limiting mag about 17.5) contained the
western half of the 5' WFC error circle (GCN #933), and the later
images (starting at 16:14 UT, 7.5 hours after the burst, total
exposure 1500 seconds, limiting mag about 18.0) fully contained the
error circle.  Compared with the DSS images after the full reduction,
both image has shown no new source brighter than the limit, nor the
candidates reported earlier by other observers (GCN #938(optical),
#939(IR)). 

This message may be cited."

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  949
SUBJECT: GRB 010214, Optical Observations
DATE:    01/02/19 22:02:08 GMT
FROM:    Javier Gorosabel at LAEFF-INTA, Madrid  <jgu@laeff.esa.es>

J. Gorosabel (DSRI, Copenhagen), J. P. U. Fynbo (ESO, Garching),
B. L. Jensen, H. Pedersen, J. Hjorth (U. of Copenhagen),
M. I. Andersen (U. of Oulu), 
K. Aksnes, T. Grav (U. of Oslo),
M. Holman (CFA, Harvard),
A. A. Kaas, T. Abbott (Nordic Optical Telescope), report

"Using the 2.56-m Nordic Optical Telescope (+ALFOSC), La Palma,
we have obtained R-band imaging of GRB 010214 (Gandolfi et al.
GCN #932), starting ~20 and ~45 hours after the burst:

UT              Filter    Exp.time   Seeing      Limit
======================================================
2001 Feb 15.22    R       6x300s     1.2" FWHM  R~21.3
2001 Feb 16.24    R       6x300s     0.9" FWHM  R~23.5

No candidate GRB counterpart is detected inside the 
1.5' SAX/NFI error-circle (Gandolfi et al. GCN #937)
to R~21.3.

The possible infrared candidate reported by Paola et al. 
(GCN #939) is detected at R~22.1 in the Feb 16 image.
We find no object at the position of the possible optical 
candidate reported by Zhu and Xue (GCN #938)."

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  950
SUBJECT: GRB 010214: X-Ray afterglow 
DATE:    01/02/20 15:50:12 GMT
FROM:    Angelo Antonelli at Obs. Astro. di Roma  <angelo@coma.mporzio.astro.it>

F. Frontera, C. Guidorzi, Universita' di Ferrara, Ferrara; 
L.A. Antonelli, Osservatorio Astronomico di Roma, Rome; 
G. Tassone, D. Ricci, L. Bruca, BeppoSAX Science Operations Center, 
Telespazio, Rome; M. Capalbi, BeppoSAX Science Data Center, Rome; 
R. Kaptein, E. Kulkeers, Space Research Organization Netherlands, 
Utrecht and L. Piro, Istituto di Astrofisica Spaziale, CNR, Rome;
report: 

"GRB 010214 (another ``Valentine's Day Burst'') was observed with 
the Narrow Field Instruments (NFI) on board BeppoSAX from Feb. 14.62 
to Feb. 16.52 UT (starting about 6 hrs after the burst trigger time;
Gandolfi, GCN #933) . In the 2-10 keV image from MECS units 2 and
3, a fading point source (1SAX J174058+4834.6) is detected within 
the WFC error circle (Gandolfi GCN #933). The source position is 
R.A. = 17h40m58s, Decl. = +48d34'37" (Eq. 2000) with 1 arcmin error 
radius. The centroid position is consistent with the preliminary
NFI analysis reported by Gandolfi (GCN #937). 

In the first 12,000 s the source had a 2-10 keV flux of about 6E-13
erg/cmE2/s, while a 2-sigma upper limit of about 5e-14 erg/cmE2/s 
was derived in the last part of the observation. We conclude that 
1SAX J174058+4834.6 is the X-ray afterglow of GRB 010214. The source
fading appears faster than usual, with a power-law index of about 1.6."

This message may be cited.
////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  951
SUBJECT: GRB010214: BeppoSAX WFC and GRBM preliminary data
DATE:    01/02/20 17:10:01 GMT
FROM:    Filippo Frontera at ITESRE CNR  <filippo@tesre.bo.cnr.it>

C. Guidorzi, F. Frontera, Universita' di Ferrara, Ferrara; G. Gennaro,
R. Manzo, A. Paolino, D. Ricci, M. Stornelli, F. Verrecchia, Scientific
Operation Centre, Telespazio, Roma; E. Kuulkers, J. in't Zand, Space
Research Organization of the Netherlands (SRON), Utrecht; E. Costa, M.
Feroci, G. Gandolfi, IAS/CNR, Roma; L. Amati, ITESRE/CNR, Bologna, 
report:

"The BeppoSAX Gamma Ray Burst Monitor (GRBM) and the Wide Field Camera
(WFC) unit 2 observed the GRB 010214 (2nd Valentine's burst) on
February 14.36679 UT. The event detected by the GRBM shows a single pulse
with a time duration of about 20 s and a peak  countrate of about 
650 cts/s in the 40-700 keV energy band. In the WFC, the duration is about
30 s and the peak flux is 0.8 Crab (2-26 keV). The centroid position of
the X-ray counterpart from the WFC image is R.A.= 17h 41m 00s,
Decl.= +48deg 32' 38" (equinox 2000.0) with a 99% error radius of 3'
(se also GCN 933). Results of the BeppoSAX follow-up observation  are
reported by Frontera et al. (GCN 950)."


This message can be cited.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  954
SUBJECT: GRB010214, optical observations
DATE:    01/02/21 15:04:27 GMT
FROM:    Nicola Masetti at ITeSRE,CNR,Bologna  <masetti@tesre.bo.cnr.it>

N. Masetti, E. Palazzi (ITeSRE, CNR, Bologna), E. Pian (Oss. Astron. Trieste),
S. Desidera, E. Giro, A. Frigo (Oss. Astron. Asiago), R. Falomo (Oss.
Astron. Padova), A. Zacchei, A. Magazzu, F. Ghinassi, and M. Pedani (TNG), 
on behalf of a larger collaboration, report:


"We acquired optical R-band images of the BeppoSAX NFI error box 
(Frontera et al., GCN #950) of GRB010214 (Guidorzi et al., GCN #951)
with the 1.8m "Copernicus" telescope (+AFOSC) located at Cima Ekar in
Asiago (Italy). We also observed this field in B, V and R at the
Canary Islands with TNG+Dolores.
Total exposure times, limiting magnitudes and seeing for each of these
observations are reported in the table below.


  telescope      date       band   exptime   3-sigma    seeing
                 (UT)               (min)     limit      (")
 --------------------------------------------------------------
   Asiago   2001 Feb 16.19    R      30      ~22.5       2.0
   TNG       "    "  16.23    R      10      ~23.5       1.2
   TNG       "    "  16.24    V      10      ~24         1.2
   TNG       "    "  16.25    B      15      ~24         1.2
   Asiago    "    "  21.11    R      35      ~21.5       4.0


Photometric calibration was performed using the USNO-A2.0 catalog star
U1350_09300715, which has magnitudes R = 18.3 and B = 19.3 and coordinates
(J2000) RA = 17 40 53.13; Dec = +48 34 08.8. Using those magnitudes and
assuming a starlike blackbody spectrum for this object, we estimated
its V magnitude to be 18.7.
We could not tie our photometry to the USNO star used by Zhu & Xue 
(GCN #938) because it was saturated in all of our images.

The comparison between the two Asiago images does not reveal any object
with significant brightness variation down to a 3-sigma limiting
magnitude R ~ 21.5 inside the NFI error box.

The IR object reported by Di Paola et al. (GCN #939) is detected in TNG V
and R images at magnitudes V = 23.8 +- 0.3 and R = 22.02 +- 0.05
(excluding zero-point calibration uncertainties), while it is
not detected in the B band down to the frame limit (B > 24).
The object is also detected in the first Asiago image at an R magnitude
consistent with that measured at TNG.
This very red object is not present on the DSS-II as its R magnitude
is below the limit of this survey.
Based on our data we cannot confirm that it does not vary. But, given its
constancy in the J band reported by Antonelli et al. (GCN #945), and the
fact that it lies ~2.4 arcmin from the NFI error box, we can confidently
say that this object is unlikely the counterpart of GRB010214. 

Also, we do not detect any object down to the frame limits in all images
at the position reported by Zhu & Xue (GCN #938).".


This message can be cited.


////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  955
SUBJECT: GRB010214, candidate optical afterglow
DATE:    01/02/21 17:41:23 GMT
FROM:    Evert Rol at U.Amsterdam  <evert@astro.uva.nl>

E. Rol, I. Salamanca, L. Kaper, P. Vreeswijk (University of
Amsterdam), P. Lacerda (Leiden Observatory), S. Hodgkin, P.
Tzanavaris (University of Cambridge), N. Tanvir (University of
Hertfordshire), report on behalf of a larger collaboration:

"We have observed the BeppoSAX error box of GRB010214 (Gandolfi, GCN
#932) with the 4.2m William Herschel Telescope (+ Prime Focus) and
with the 2.2m Isaac Newton Telescope (+ WFC) at La Palma, as follows:


  Telescope     Date          Filter  Exp.time  Seeing   Lim. mag.
		(UT)		       (secs)    (")     (3 sigma)  
  =================================================================
  WHT (+PF)   2001 Feb 15.26    R      2 x 225   0.84     ~23.5
  INT (+WFC)  2001 Feb 17.25    R      2 x 900   1.2	  ~24.2

(Note that in our calibration, the USNO star mentioned by Masetti et
al. (GCN #945) has a magnitude of R=18.4 instead of R=18.3.)

Within the refined NFI error box (Frontera et al., GCN #950), we
detect one object which faded from R = 22.9 to R = 24.1 (1 sigma error
about 0.2 mag) between the two observations. 
The source seems to be extended, likely to be due to an underlying
galaxy. We consider this object to be a strong candidate for the optical
afterglow of GRB010214. The candidate is located at RA = 17:41:02.9
and Dec = 48:34:30 (J2000; error about 1 arcsec).

Another variable source is located just outside the refined NFI error
box, though within the initial NFI error box (Gandolfi, GCN #937),
with a position of RA = 17:41:04.6, Dec = 48:33:47 (J2000). This
source has faded from R = 23.1 to 24.0 (error of ~0.2 mag).  The
infrared object mentioned by Di Paola et al. (GCN #939; see also
Antonelli, GCN #944) is clearly visible in our images (R~22.6 in the
WHT image). We measure two slightly different magnitudes (difference
of about 0.3), which might indicate a variable star.

Images and more information can be found on
http://www.astro.uva.nl/~evert/grb010214/


This message can be cited."

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  964
SUBJECT: GRB010214B,Gamma Ray Observations
DATE:    01/02/22 14:01:49 GMT
FROM:    Srikanta Sinha at ISRO/ISAC  <sinha@isac.ernet.in>

S.Sinha,P.Sreekumar,K.Kasturirangan, on behalf of SROSS C-2 (INDIAN
GRB EXPERIMENT)team report:
      
        SROSS C-2 observed this burst at 49981.001 UT (this time is 
not corrected for small systematic errors). As observed by SROSS C-2
,it had a duration (T90) of 14.92 +-0.06 secs. Its fluence in the
20-100 keV band is equal to 5.39.10-6 +-1.53.10-7 ergs cm-2 and in
the 100-1024 keV band is equal to 1.74.10-5 +-1.23.10-6 ergs cm-2
respectively. These fluences are not corrected for the sec(theta)
factor since its direction is unknown to us. The peak flux(256 ms)
in the 20-100 keV band is 9.66 photons cm-2 sec-1 and the peak flux
(256 ms) in the 100-1024 keV band is equal to 12.20 photons cm-2 sec-1.
The hardness ratio for this burst (when the signal peaks in the 100-1024
keV channel) is equal to 0.69+- 0.13. Our hardness ratio is defined as
[counts(100-1024 keV)/counts(20-100 keV)].
        This message is citable.
 
-Srikanta Sinha, on behalf of the SROSS C-2 (INDIAN GRB EXPT.TEAM) at
the Technical Physics Division, ISRO Satellite Center, Bangalore-560 017,
INDIA



////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  972
SUBJECT: GRB 010214, Optical Observations
DATE:    01/02/22 23:35:54 GMT
FROM:    Javier Gorosabel at LAEFF-INTA, Madrid  <jgu@laeff.esa.es>

J. Gorosabel (DSRI, Copenhagen), J. P. U. Fynbo (ESO, Garching),
B. L. Jensen, H. Pedersen, J. Hjorth (U. of Copenhagen),
M. I. Andersen (University of Oulu), 
K. Aksnes, T. Grav (University of Oslo), M. Holman (CFA, Harvard),
A. A. Kaas, T. Abbott (Nordic Optical Telescope), report

"We have examined the variable optical sources reported by Rol et al. 
(GCN #955) in our NOT images taken on Feb 16.24 UT (GCN #949). We report 
the following preliminary magnitudes assuming R = 18.4 for the USNO-A2.0 
catalog star U1350_09300715 (GCN #955).

             Date(UT)  Filter    Magnitude
  ===========================================
   Object 1  Feb 16.24   R      22.88 +-0.22
   Object 2  Feb 16.24   R      23.01 +-0.22

These values are consistent with the magnitudes found on Feb 15.26 (GCN #955)."


////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  978
SUBJECT: GRB010214 follow-up from Hanle
DATE:    01/02/23 11:34:00 GMT
FROM:    SG Bhargavi at Indian Inst of Astrophysics  <bhargavi@iiap.ernet.in>

On behalf of the GRB follow-up team at Indian Institute
of Astrophysics, Bangalore India , Ramanath Cowsik reports:
 
The field of GRB 010214 centered at BeppoSAX WFC error circle (GCN-933)
was imaged using the new 2.01m telescope at Indian Astronomical Observatory
(IAO), Mt. Saraswati, Hanle, India.
 
Two exposures of 600s each in B and R band were taken on 15th and 16th Feb,
2001. No flaring or fading sources have been detected w.r.t DSS2 image
down to the limit R > 22.0; we do see many objects below DSS limit, but
these have not varied >0.1 m between 2 epochs of our observations.
 
The J-band source reported by Di poala et al.(GCN-939) is detected
at R=22.2 +/- 0.22 on Feb 15.99 UT and is found to be constant in
brightness within the photometric error and
consistent with the measurements of Gorosabel et al(GCN-949)
It is at B >23.0 in the combined image of 1200 s on Feb 16.99 UT.
The photomertic calibration is done with respect to 12 of USNO-A2.0 stars
in this field.
 
The optical candidate reported by Jhu et al. (GCN-938) is not detected
in our images. The afterglow candidates reported by Rol et al. (GCN-955)
are not detected in our images , as they are below our detection limit.
 


////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  988
SUBJECT: GRB010214, field photometry
DATE:    01/02/25 01:14:33 GMT
FROM:    Arne A. Henden at USNO/USRA  <aah@nofs.navy.mil>

A. Henden (USRA/USNO) reports on behalf of the USNO GRB team:

We have acquired preliminary BVRcIc all-sky photometry for
the field of GRB010214 with the USNOFS 1.0-m telescope on one
photometric night with poor seeing.  This 11x11arcmin field includes
the proposed counterpart and extends to approximately V=20.
All stars brighter than V=14 are saturated and should be used
with care.  We have placed the photometric data on our
anonymous ftp site:
ftp://ftp.nofs.navy.mil/pub/outgoing/aah/grb/grb010214.dat
The current photometry has a potential external zero-point
error of about two percent that needs to be added in
quadrature to the Poisson errors given in the datafile.
The astrometry in this file is based on linear
plate solutions with respect to USNO-A2.0. The internal errors
are less than 100mas.

At least two additional nights of photometry will be added to the data
file when weather conditions permit.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  997
SUBJECT: GRB 010214, I-band data
DATE:    01/02/28 16:50:52 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

S. Klose, B. Stecklum, H. Linz, and U. Laux (Thueringer Landessternwarte 
   Tautenburg) 


report:

The error box of GRB 010214 (Gandolfi et al., GCN #932) was imaged
in the I-band using the Tautenburg Schmidt telescope equipped with
the Schmidt focus CCD camera (2k x 2k). The observing log is as follows:

  Run 1:   Feb 15,  0:55 UT - 1:35 UT  and   2:24 UT - 3:05 UT 
  Run 2:   Feb 16,  2:01 UT - 2:48 UT  and   3:38 UT - 3:48 UT 
  Run 3:   Feb 27,  3:44 UT - 4:24 UT.                         

The R-band afterglow candidate reported by Rol et al. (GCN #955) is
clearly detected on the combined frames taken during the second
observing run. Based on the DSS2 red coordinate system we obtain for this
source RA, DEC (2000) = 17:41:03.0, 48:34:29 (+/- 0.4"). Using the
photometric standards provided by Henden (GCN #988) we measure a mean 
I-band magnitude of 21.9 +/- 0.4 during run 2.

The combined frames of run 1 are somewhat less deep and the same holds for
the combined frames of run 3. The source is also detectable on these
images but very close to the detection limit which excludes an aperture
photometry. However, a visual comparison of the optical appearance of the
afterglow candidate on these images with the optical appearance of a
near-by, faint stellar object at RA, DEC (2000) = 17:41:07.7, 48:35:02
(+/- 0.8") allows us to state that we see no evidence for a fading of the
afterglow candidate between run 1 and run 3. Any fading must be less than
about 0.5 mag.
 
In conclusion, if this source is the combined OT + underlying host
galaxy then even during our first observing run (about 0.7 days after the
burst) the I-band flux of the afterglow did not exceed the I-band flux of
the underlying host by more than about 50 percent.

The I-band image is posted on the Tautenburg Web page at
http://www.tls-tautenburg.de/research/grb010214.html. It can also be
obtained via anonymous ftp from ftp.tls-tautenburg.de, directory
/pub/klose/GCN/.


This message is quotable.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  1059
SUBJECT: GRB010214, optical observations
DATE:    01/05/04 10:43:04 GMT
FROM:    Evert Rol at U.Amsterdam  <evert@astro.uva.nl>

E. Rol, I. Salamanca, L. Kaper, P. Vreeswijk (University of
Amsterdam), N. Tanvir (University of Hertfordshire), report on behalf
of a larger collaboration:


In order to verify the possible counterpart to GRB010214 (Rol et al.,
GCN 955), we obtained another set of images with the Isaac Newton
Telescope on February 21, 2001. Examination and comparison of these
images with those obtained at the INT on February 17 shows no evidence
for a further fading of the possible counterpart, as already suggested
in other reports (Gorosabel et al., GCN 972; Klose et al., GCN 997;
Fynbo, private comm.). Instead, the source has the same magnitude as
measured in the images obtained at the William Herschel Telescope on
February 16, R = 22.9 (Rol et al, GCN 955). We therefore conclude that
the optical counterpart of GRB010214 has not been detected, with upper
limits R ~ 23.5, R ~ 24.2 and R ~ 23.8 on Feb. 15.26, Feb. 17.25 and
Feb. 22.22 respectively (using the calibration of Henden, GCN
988). Since the decrease in intensity on Feb. 17 does not appear to be
an artifact in the images, the detected source likely is a variable
star.

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