3rd Integral Bart Work Shop Chocerady - November 1-3, Patrizia Ferrero GRB Too observations in Loiano Patrizia Ferrero (IASF-BO, OACT & Universita’ di Teramo)

Patrizia Ferrero 3rd Integral Bart Work Shop Chocerady - November 1-3, Our collaboration Patrizia Ferrero (IASF-BO, OACT & Universita’ di Teramo) Corrado Bartolini, Adriano Guarnieri, Adalberto Piccioni (Universita’ di Bologna) Graziella Pizzichini (IASF-BO)

Patrizia Ferrero 3rd Integral Bart Work Shop Chocerady - November 1-3, The 152 cm telescope in Loiano The 152 cm Cassini telescope of the Bologna Astronomical Observatory is located in Loiano, about 40 Km south of Bologna. The location is Lat. 44d 15’ 30’’ N, Long. 11d 20’ 12’’ E, altitude 785 m a.s.l.. General description of the 152 cm telescope Optical configuration : Ritchey-Chretien Mount Type : English Total weight : 9000 Kg Main concave mirror : total diameter : cm useful diameter: cm focal ratio F/3 Secondary mirror : total diameter: 58.0 cm useful diameter 55.5 cm Mirror distance : cm Cassegrain Focus : equivalent focal length: 1200 cm equivalent focal ratio: F/8 scale :17"/mm useful corrected field: 70' We use the Cassini Telescope equipped with the BFOSC (Bologna Faint Object Spectrograph & Camera) to acquire CCD frames. The detector is an EEV CCD with an array of 1300x1340 pixels and its main features are: quantum efficiency: 500 nm, 900 nm, 300 nm; pixel size: 20x20 micron; pixel scale: 0.58 arcsec/pixel; field of view: 12.6’x13’; read-out noise: 1.73 e-/px; conversion factor: 2.13 e-/ADU. At present UBVRI Johnson-Kron-Cousin and GRZI Thuan-Gunn filters can be mounted.

Patrizia Ferrero 3rd Integral Bart Work Shop Chocerady - November 1-3, Summary of our observational activity in Loiano From mid-2001 to October 2004, it was possible to observe 18 Gamma-Ray Burst locations. In this period the GRB events were more than 18, but our observations are limited by:  bad weather;  GRB coordinates: in order to avoid telescope optics stress, we cannot observe the objects which have Declination less than -10 degrees;  GRB error boxes: we don’t analyse error boxes which are greater than about 40’ x 30’;

Patrizia Ferrero 3rd Integral Bart Work Shop Chocerady - November 1-3,  target of opportunity program: every semestr we have six nights to observe GRB locations and these observations have to be compatible with the scheduled ones and the telescope instruments (BFOSC). We had positive detections (i.e. we detected the optical afterglow) for GRB , , , , , , and positive detections (i.e. we detected the optical afterglow) for GRB , , , , , , and negative detections for GRB , , , , , , , , , a and b. negative detections for GRB , , , , , , , , , a and b.

Patrizia Ferrero 3rd Integral Bart Work Shop Chocerady - November 1-3, Images’ Analysis To reduce our images and do photometry, we use IRAF: Image Reduction and Analysis Facility IRAF: Image Reduction and Analysis Facility while to astrometrize GAIA: Graphical Astronomy and Image Analysis Tool GAIA: Graphical Astronomy and Image Analysis Tool

Patrizia Ferrero 3rd Integral Bart Work Shop Chocerady - November 1-3, GCNs* which include our observations *The GRB Coordinates Network (

Patrizia Ferrero 3rd Integral Bart Work Shop Chocerady - November 1-3, And now some examples of our observations and results...

Patrizia Ferrero 3rd Integral Bart Work Shop Chocerady - November 1-3, GRB040825a N E  R.A.= 22h 58m 59s and Declination= -10d 56’ 01’’ (center of the error box)  Mean time of observations: August UT, hours after the GRB  Magnitude limit Rc=19.5: our limit is the first in Rc filter  GCN 2664  In GCN 2661 Tristram et al. reported R(similar to Ic)=21.1

Patrizia Ferrero 3rd Integral Bart Work Shop Chocerady - November 1-3, GRB040825b N E  R.A.=22h 46m 34s and Declination=-02d 24’ 27’’ (center of error box)  R.A.= 22h 46m 40s and Declination= -02d 21’ 42’’ (center of our 1st subfield of the error box)  R.A.= 22h 46m 38s and Declination= -02d 28’ (center of our 2nd subfield of the error box)  Mean Time of observations: August UT, hours after the GRB  Magnitude limit Rc=19.5  GCN 2663

Patrizia Ferrero 3rd Integral Bart Work Shop Chocerady - November 1-3, GRB N E  Mean Time of observations: April OT: R.A.= 10h 54m 34s and Declination= -07d 01’ 40’’  UT, hours after the GRB  OT magnitude Rc=20.5+/- 0.3, Rc=20.7+/-0.3 & Ic=19.8 +/-0.2  GCN 2284

Patrizia Ferrero 3rd Integral Bart Work Shop Chocerady - November 1-3, GRB N E  OT: R.A.= 12h 10m 48s and Declination= -09d 20’ 51’’  Mean Time of observations: March UT, hours after the GRB  OT magnitude Rc= / & Rc=20.30+/-0.08  GCN 2008

Patrizia Ferrero 3rd Integral Bart Work Shop Chocerady - November 1-3, GRB N E  OT: R.A.= 11h 33m 05s and Declination= 25d 53’ 56’’  Mean Time of observations: February UT, hours after the GRB  OT magnitude Rc=19.9+/ 0.1, Ic=19.6+/-0.2, V= /-0.05, B=21.44+/-0.10  GCN

Patrizia Ferrero 3rd Integral Bart Work Shop Chocerady - November 1-3, GRB N E  OT: R.A.= 00h 26m 55s and Declination= 18d 55’ 41’’  Mean Time of observations: October UT & UT, respectively and hours after the GRB  OT magnitude Rc=19.69+/ 0.13, Ic=19.3+/-0.2, V= /-0.12, B=20.63+/-0.13  GCN 1603

Patrizia Ferrero 3rd Integral Bart Work Shop Chocerady - November 1-3, The Future Hete-2 and Integral satellites are expected to continue their activity of detection of gamma ray bursts, while the imminent launch of Swift should lead to almost 1 GRB/day with a faster localization of the optical afterglow due to the on board telescope, which can automatically re-point toward the burst direction, and a more intense observational activity of all observatories, Loiano included.

Patrizia Ferrero 3rd Integral Bart Work Shop Chocerady - November 1-3, The end.