//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 17095 SUBJECT: GRB141124A: MASTER Detection of New Flare of QSO NVSS J075043+790917 During the Fermi Error Box inspection DATE: 14/11/24 17:57:33 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk Irkutsk State University V. Shumkov, E. Gorbovskoy, D.Denisenko, V. Lipunov, M.Pruzhinskaya, V.Kornilov, D.Kuvshinov, N.Tyurina, P.Balanutsa, D.Zimnukhov, A.Kuznetsov Lomonosov Moscow State University, Sternberg Astronomical Institute, Moscow State University V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov Blagoveschensk Educational State University, Blagoveschensk A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik Kislovodsk Solar Station of the Pulkovo Observatory V.Krushinsky, I.Zalozhnih, A. Popov Ural Federal University, Yekaterinburg, Kourovka Hugo Levato and Carlos Saffe Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE) Claudio Mallamaci, Carlos Lopez and Federico Podest Observatorio Astronomico Felix Aguilar (OAFA) MASTER OT J075043.33+790917.1 - new flare of QSO NVSS J075043+790917 = MASTER OT J075042.60+790918.2 MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru) located in Tunka was starting survey on the FERMI GRB141124A (GBM trigger number 438503903 ) error-box 2286 sec after notice time and 15886 sec after trigger time at 2014-11-24 11:03:07 UT. During the inspection of the Fermi error box MASTER-Tunka auto-detection system discovered OT source at (RA, Dec) = 07h 50m 43.33s +79d 09m 17.1s on 2014-11-24.62164 UT. The OT unfiltered magnitude is 17.5m (limit 18.4m). The OT is seen in 3 images. There is no minor planet at this place. We have reference image without OT on 2010-11-13.70064 UT with unfiltered magnitude limit 21.2m. The OT is a new flare of quasar NVSS J075043+790917 that was previously detected by MASTER-Amur on 2013-04-26.694 UT as MASTER OT J075042.60+790918.2 (see ATel #5044, S. Shurpakov et al.). The object is marginally visible on the Blue Palomar plate with jmag=22.31 in GSC 2.3.2. There is an infrared counterpart AllWISE J075043.29+790917.1 (W1=14.05+/-0.03 W2=13.01+/-0.03 W3=9.53+/-0.03 W4=7.20+/-0.09). This area of sky is not covered by SDSS and CRTS. Color-combined DSS finder chart is uploaded to http://master.sai.msu.ru/static/OT/J075043+790917-BRIR.jpg (10'x10' FOV). We note that in our previous observations of this field by MASTER-Tunka on 2014-10-26.644 UT (by the coincidence, also during Fermi error box inspection for trigger number 436028617) the object was marginally detected at ~18.5m. Multi-wavelength follow up observations are required. The discovery and reference images are available at: http://master.sai.msu.ru/static/OT/075043.33790917.1.png The inspection map of Fermi error box is available at: http://master.sai.msu.ru/static/OT/1468936236.png The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 17097 SUBJECT: GRB 141124A​: iPTF upper limits​ DATE: 14/11/24 18:38:42 GMT FROM: Varun Bhalerao at IUCAA V. Bhalerao (IUCAA), S. B. Cenko (NASA/GSFC), L. P. Singer (Caltech) ​and ​ M. M. Kasliwal (Carnegie Observatories/Princeton) ​ ​ report on behalf of the intermediate Palomar Transient Factory (iPTF) collaboration: We searched for optical counterparts of GRB 141124A ​ (GCN Notice http://gcn.gsfc.nasa.gov/other/438503903.fermi) using the Palomar 48-inch Oschin telescope (P48). At about 18 minutes after the burst, we began imaging 30 fields spanning an area of 2 ​12​ deg2, covering most of the 1-sigma statistical+systematic region of the initial Fermi GBM localization, as well as about half of the 1-sigma statistical + systematic region of the final Fermi GBM localization (Fermi trigger 438503903 / 141124277). Based on the GBM localization, we estimate a ​44% chance that these fields contain the true location of the source. Sifting through candidate variable sources using ​ image subtraction and standard iPTF vetting procedures, we detected the ​ ​ following optical transient candidates ​:​ iPTF14ihm RA (J2000) 08:22:15.03 (125.562634 deg) Dec (J2000) +74:50:00.5 (+74.833477 deg) Consistent with stellar source, photometry does not show rapid evolution. iPTF14ihn RA (J2000) 10:36:56.79 (159.236626 deg) Dec (J2000) +71:10:52.0 (+71.181099 deg) Likely high proper motion star, photometry does not show rapid evolution. iPTF14iho RA (J2000) 09:45:09.42 (146.289253 deg) Dec (J2000) +74:20:12.1 (+74.336707 deg) Near undocumented galaxy, photometry does not show rapid evolution. iPTF14ihp RA (J2000) 10:54:59.28 (163.746991 deg) Dec (J2000) +68:11:53.5 (+68.198184 deg) Photometry shows decline over 60-minute period, but the image subtraction residuals are centered on a stellar source in the reference image. This is most likely a galactic variable. ​We conclude that we have not detected the optical afterglow of GRB 141124A​.