3rd integral bart work shop chocerady - november 1-3, 2004 1 patrizia ferrero grb too observations...

3rd Integral Bart Work Shop Cho3rd Integral Bart Work Shop Chocerady - November 1-3, 2004cerady - November 1-3, 2004

11Patrizia Ferrero Patrizia Ferrero

GRB Too observations in GRB Too observations in LoianoLoiano

Patrizia Ferrero Patrizia Ferrero (IASF-BO, OACT & Universita’ di Teramo)(IASF-BO, OACT & Universita’ di Teramo)

Patrizia Ferrero Patrizia Ferrero 3rd Integral Bart Work Shop Cho3rd Integral Bart Work Shop Chocerady - November 1-3, 2004cerady - November 1-3, 2004

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Our collaborationOur collaboration

Patrizia FerreroPatrizia Ferrero (IASF-BO, OACT & Universita’ di Teramo)(IASF-BO, OACT & Universita’ di Teramo)

Corrado Bartolini, Adriano Guarnieri, Corrado Bartolini, Adriano Guarnieri, Adalberto PiccioniAdalberto Piccioni

(Universita’ di Bologna)(Universita’ di Bologna)

Graziella PizzichiniGraziella Pizzichini(IASF-BO)(IASF-BO)


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The 152 cm telescope in The 152 cm telescope in LoianoLoiano

The 152 cm Cassini The 152 cm Cassini telescope of the Bologna telescope of the Bologna Astronomical Observatory Astronomical Observatory is located in Loiano, about is located in Loiano, about 40 Km south of Bologna.40 Km south of Bologna.

The location is Lat. 44d The location is Lat. 44d 15’ 30’’ N, Long. 11d 20’ 15’ 30’’ N, Long. 11d 20’ 12’’ E, altitude 785 m 12’’ E, altitude 785 m a.s.l..a.s.l..

General description of the 152 cm telescopeOptical configuration : Ritchey-ChretienMount Type : English Total weight : 9000 Kg

Main concave mirror : total diameter : 152.4 cm useful diameter: 150.0 cm focal ratio F/3

Secondary mirror : total diameter: 58.0 cm useful diameter 55.5 cm

Mirror distance : 308.7 cm

Cassegrain Focus : equivalent focal length: 1200 cmequivalent 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: 80% @ 500 nm, 32% @ 900 nm, >50% @ 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.


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Summary of our observational Summary of our observational activity in Loianoactivity in Loiano

From mid-2001 to October 2004,From mid-2001 to October 2004, it it was possible to was possible to observe 18 Gamma-Ray Burst locations. In this observe 18 Gamma-Ray Burst locations. In this period the GRB events were more than 18, but our period the GRB events were more than 18, but our observations are limited by: observations are limited by: bad weather; bad weather; GRB coordinates: in order to avoid telescope GRB coordinates: in order to avoid telescope optics stress, we cannot observe the objects which optics stress, we cannot observe the objects which have Declination less than -10 degrees;have Declination less than -10 degrees; GRB error boxes: we don’t analyse error boxes GRB error boxes: we don’t analyse error boxes which are greater than about 40’ x 30’;which are greater than about 40’ x 30’;


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target of opportunity program: every semestr we target of opportunity program: every semestr we have six nights to observe GRB locations and have six nights to observe GRB locations and these observations have to be compatible with these observations have to be compatible with the scheduled ones and the telescope the scheduled ones and the telescope instruments (BFOSC).instruments (BFOSC).

We hadWe had

• positive detections (i.e. we detected the optical positive detections (i.e. we detected the optical afterglow) for GRB 020813, 021004, 030226, afterglow) for GRB 020813, 021004, 030226, 030328, 030329, 030418, 041006 and 030328, 030329, 030418, 041006 and

• negative detections for GRB 020317, 020812, negative detections for GRB 020317, 020812, 020819, 030217, 030227, 030324, 030418, 020819, 030217, 030227, 030324, 030418, 040422, 040624, 040825a and 040825b.040422, 040624, 040825a and 040825b.


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Images’ AnalysisImages’ Analysis

To reduce our images and do photometry, we use To reduce our images and do photometry, we use

• IRAF: IRAF: Image Reduction and Analysis FacilityImage Reduction and Analysis Facility

whilewhile to astrometrizeto astrometrize

• GAIA: GAIA: Graphical Astronomy and Image Analysis Graphical Astronomy and Image Analysis ToolTool


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GCNs* which include our GCNs* which include our observationsobservations

GRB GCN GRB 020317 1287 GRB 020812 1486 GRB 020819 1509 1511 GRB 030217 1873 GRB 021004 1603 GRB 030226 1892 1940 GRB 030324 1963 GRB 030328 2008 GRB 030329 2003 2030 2136 2228 GRB 030418 2284 GRB 031111 2524 (with OGS-Tenerife data) GRB 040422 2578 GRB 040825a 2664 GRB 040825b 2663 GRB 041006 2777 2804

*The GRB Coordinates Network (http://gcn.gsfc.nasa.gov/)


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And now some examples of And now some examples of our observations and our observations and results. . .results. . .


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GRB040825aGRB040825aN

E

R.A.= 22h 58m 59s and R.A.= 22h 58m 59s and Declination= -10d 56’ 01’’ Declination= -10d 56’ 01’’ (center of the error box)(center of the error box)

Mean time of Mean time of observations: August observations: August 26.035 UT, 21.336 hours 26.035 UT, 21.336 hours after the GRBafter the GRB

Magnitude limit Magnitude limit Rc=19.5: our limit is the Rc=19.5: our limit is the first in Rc filterfirst in Rc filter

GCN 2664GCN 2664

In GCN 2661 Tristram et In GCN 2661 Tristram et al. reported R(similar to al. reported R(similar to Ic)=21.1Ic)=21.1


1010

GRB040825bGRB040825bN

E

R.A.=22h 46m 34s and R.A.=22h 46m 34s and Declination=-02d 24’ 27’’ Declination=-02d 24’ 27’’ (center of error box)(center of error box)R.A.= 22h 46m 40s and R.A.= 22h 46m 40s and Declination= -02d 21’ 42’’ Declination= -02d 21’ 42’’ (center of our 1st subfield of the (center of our 1st subfield of the error box)error box)

R.A.= 22h 46m 38s and R.A.= 22h 46m 38s and Declination= -02d 28’ (center Declination= -02d 28’ (center of our 2nd subfield of the error of our 2nd subfield of the error box)box)

Mean Time of Mean Time of observations: August observations: August 25.975 UT, 7.050 hours 25.975 UT, 7.050 hours after the GRBafter the GRB

Magnitude limit Magnitude limit Rc=19.5Rc=19.5

GCN 2663GCN 2663


1111

GRB030418GRB030418N

E

Mean Time of Mean Time of observations: April OT: observations: April OT: R.A.= 10h 54m 34s and R.A.= 10h 54m 34s and Declination= -07d 01’ 40’’Declination= -07d 01’ 40’’

18.85411 UT, 10.5219 18.85411 UT, 10.5219 hours after the GRBhours after the GRB

OT magnitude OT magnitude Rc=20.5+/-0.3, Rc=20.5+/-0.3, Rc=20.7+/-0.3 & Ic=19.8 Rc=20.7+/-0.3 & Ic=19.8 +/-0.2+/-0.2

GCN 2284GCN 2284


1212

GRB030328GRB030328N

E

OT: R.A.= 12h 10m 48s OT: R.A.= 12h 10m 48s and Declination= -09d 20’ and Declination= -09d 20’ 51’’51’’

Mean Time of Mean Time of observations: March observations: March 28.93889 UT, 11.184 28.93889 UT, 11.184 hours after the GRBhours after the GRB

OT magnitude OT magnitude Rc=20.32 +/- 0.10 & Rc=20.32 +/- 0.10 & Rc=20.30+/-0.08Rc=20.30+/-0.08

GCN 2008GCN 2008


1313

GRB030226GRB030226N

E

OT: R.A.= 11h 33m 05s OT: R.A.= 11h 33m 05s and Declination= 25d 53’ and Declination= 25d 53’ 56’’56’’

Mean Time of Mean Time of observations: February observations: February 27.160718 UT, 20.484 27.160718 UT, 20.484 hours after the GRBhours after the GRB

OT magnitude OT magnitude Rc=19.9+/ 0.1, Ic=19.6+/-Rc=19.9+/ 0.1, Ic=19.6+/-0.2, V=20.50 +/-0.05, 0.2, V=20.50 +/-0.05, B=21.44+/-0.10B=21.44+/-0.10

GCN 1892 1940GCN 1892 1940


1414

GRB021004GRB021004N

E

OT: R.A.= 00h 26m 55s OT: R.A.= 00h 26m 55s and Declination= 18d 55’ and Declination= 18d 55’ 41’’41’’

Mean Time of Mean Time of observations: October observations: October 6.05294 UT & 7.90313 UT, 6.05294 UT & 7.90313 UT, respectively 37.1674 and respectively 37.1674 and 81.5712 hours after the 81.5712 hours after the GRBGRB

OT magnitude OT magnitude Rc=19.69+/ 0.13, Rc=19.69+/ 0.13, Ic=19.3+/-0.2, V=19.99 Ic=19.3+/-0.2, V=19.99 +/-0.12, B=20.63+/-0.13+/-0.12, B=20.63+/-0.13

GCN 1603GCN 1603


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


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The end.The end.

3rd integral bart work shop chocerady - november 1-3, 2004 1 patrizia ferrero grb too observations...

Documents

grb locations

grb 040825a2664grb

grb gcngrb

grb events

degrees grb error boxes

grb coordinates network

bad weather grb coordinates

total diameter