RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 1 Presentations...
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RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 1
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
Relativistic and particle Astrophysicsthe past and the present
This part of the institute has systematically grown and is now ~ 40% of IASF
Senior scientists, expert technicians, many young reserchers, graduation and PHD thesis, post-doc.
Many projects reasonably staffed but (according to italian standards) too much unbalanced toward temporary positions on external funds.
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 2
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
The first stepsIn the Gratton Era
1968-1969. Two rocketts for all sky X-Ray survey: a Nike-Apache and a Skylark.Payloads all made in the house except detectors (purchased from LND)
LAS
1975 – 1977 A rocket experiment in collaboration with AS&E and MIT → CFA
1-d Baez telescope with an imaging proportional counter:
Role of LAS (now IASF): refurbishment, alignment and calibration of the telescope. IPC. Front End. Electronics.
1975-1976 Preparation of a rocket experiment with CFA (never flown):
Si(Li) detector in the focus of a grazing incidence concentrator.
Role of LAS: Detector, telescope, electronics.
R&D driven by these experiments:
Imaging Proportional Counters, X-ray optics, Electronics
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 3
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
The Balloon Era (1976 – 1990)
Experiments aboard stratospheric Balloons launched from Sicily, USA, Brazil, India, Australia for HardX-Ray Soft -Ray Astronomy
An all domestic line:
Large area high pressure proportional counters coolimated
Imaging high pressure proportional counters with coded masks
In collaboration with other institutes (+Southampton, Saclay, Toulouse, Tubingen)
Large area -ray imager with coded mask
Large area -ray timing experiment
Low background scintillators
Some success, some failure, more than a decent scientific throughput
A great school! How to handle an experiment from the first concept, to the building, to flight operations, to data analysis.A boost to R&D: Proportional Counters, Imaging Detectors, Scintillators, theory and practice of Coded Masks
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 4
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
High Energy Astrophysicsnot only connected to hardware
e.g. 25 years study of symbiotic star AG Draconis
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 5
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
XMM & ground observations of AG Dra during quiescence and outburst
burst min
Energy distribution at V min & V max
AG DRACONIS K 3 III + WD
Pop II symbiotic binary
Recurrent outbursts
Strong UV source
Super Soft XR source (15 eV,2600 L)
Optical and X-ray light curves Path of the WD in the L-T diagram (from IUE)
X-ray Vs. visual/UV anticorrelation
XMM observations before & after the 2005 burst
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 6
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
AG Draconis is a symbiotic binary composed of a red giant stars and a White Dwarf.
The wind of the giant is accreted onto the WD surface. The hydrogen burning heats the WD to 15 eV.
Since 3 decades we are monitoring AG Draconis in optical, ultraviolet and X-ray bands.
AG Draconis is subject to recurrent light maxima, or bursts, during which the optical and ultraviolet flux increases – while the X-rays above 100 eV nearly disappear. (See the EXOSAT, ROSAT and XMM light curves on the top of the panel).
The next panel shows the path of the WD in the L-T diagram as derived from our IUE observations.
The third panel shows variation of the X ray to optical energy distribution. The X-ray variations are best seen in the next panel, where XMM observations taken 44 days apart before and after the beginning of a new burst are shown.
Finally, XMM unveiled the presence of a, probably steady, higher energy tail that we suppose be formed in a shocked region around the system.
Our XMM observations are basic to best quantify the X-ray Vs. optical-ultraviolet ANTICORRELATION, as seen in the last panel.
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 7
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
Another long term research
Multifrequency Studies
an example:
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 8
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
GeV – TeV anticorrelated emission from Cyg X-1
1-10 GeVjet+counter jet
1-10 GeVjet
> 0.2 TeVjet+counter jet
> 0.2 TeVjet
-ray light curves produced by electrons accelerated in the jets of Cyg X-1
Power law spectrum of electrons E-2
Bednarek, W. & Giovannelli, F.: 2007, A&A 464, 437-445
AGILEGLAST
MAGICVERITAS
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 9
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICSSAXSAX was proposed to CNR (ASI would arrive later) in June 1981
IAS is present from the first proposal
A role in all the Working Groups of the mission and in the Science Management
The role of IAS increases wit time and becomes outstanding after the launch: Mission Scientist, Leadership in GRB research, leadership in LMXRB
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 10
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
The Role of IASF
A role in the Payload Development: • Phoswich Detector System
• Gamma Ray Burst Monitor
• Wide Field Cameras
A role in science management• Experiment Investigator WG
• DataAnalysis WG
• Science WG After the Launch Mission Scientist from IASF
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 11
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
GRB: The BeppoSAX ERAThe major discoveries
• X-ray afterglow• Optical Afterglow• Host Galaxy• Red-shift• Broad Band Variability • Dark Afterglows• Supernova Connection• X-ray Flash• Ep – Eiso relation
The discovery of the X-ray afterglow was the starting point of all the Beppo Sax revolution. It proceeded from the combined use of the wide field/narrow field instruments of SAX following an ad hoc procedure involving many teams (GRBM/PDS, WFC, MECS, Science Operation Center, Operation Control Center, Mission Scientist, Mission Director). 2 out of the 4 coordinators and 3 out of the 8 PIs were from IAS.
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 12
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
Clues of GRB revolution
GRBM
First X-Ray Afterglow
First Optical Afterglo
w
First Red-shift
First Radio
Afterglow
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 13
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
SAX not only GRBs
An instance of relevant result:
The hard X-Ray emission of some Clusters
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 14
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
NT HXR emission was predicted in 1970s in clusters showing diffuse radio emission (see: Perola & Reinhardt 1972, Rephaeli 1979) IC emission relativistic radio electrons CMB photons
Observations:
Balloon experiments Bazzano et al 1984;1990
HEAO-1 Rephaeli, Gruber & Rothschild 1987
Rephaeli & Gruber 1988
OSSE exp. (Compton-GRO) Rephaeli, Ulmer & Gruber 1994
RXTE & ASCA Delzer & Henriksen 1998
Cluster Hard Excess
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 15
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
Coma Cluster & Abell 2256
Excess ~ 4.8FNT
X ~ 1.5 x 10-11 cgs (20-80 keV)
Fusco-Femiano et al 2004 Fusco-Femiano et al. 2005
Coma A2256
FNTX ~ 9 x 10-12 cgs
(20-80 keV)
BeppoSAX BeppoSAX
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 16
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
GRBs in the SWIFT Era
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 17
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
GRB engine re-activation? X-ray versus GeV flares •Roughly 40% of GRBs show X-ray flares at hundreds-thousands of seconds
after the prompt, carrying a significant amount of the total energy.
•Most present models require a central source producing energy on time scales much longer than few seconds. Crucial to the understanding of the central source
• HOW ? We predict that X-ray flares should be associated with high energy flares (expected by IC), and find that their properties are strictly connected and model dependent. Simultaneous X-ray (SWIFT) and GeV observations (AGILE and GLAST) are thus very important to constrain the duration of engine activity.Delayed External Shock
LAT sensitivity
XRT BAT
Late InternalShock
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 18
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
The mysterious origin of X-Ray Flashes
HIGH REDSHIFT SCENARIO: XRFs are GRBs at high redshift (z >5) . Swift XRFs are at low redshift. This clearly rules out the high distance hypothesis.
OFF AXIS SCENARIO: XRFs are GRBs seen at large angles from the direction of the jet. Different jet structures have been proposed which predict a specific value of the GRB-to-XRF X-ray afterglow luminosity ratio.
Swift has permitted for the first time the access to XRF X-ray afterglow luminosity. Only a jet with uniform energy distribution can account for XRF afterglow properties. However, this models does not explain prompt emission properties …
A NEW POPULATION of subenergetic progenitors?
XRFs are a new population of GRBs discovered by BeppoSAX with most of the energy emitted in the X-ray band.
We are investigating their origin using BeppoSAX and Swift data.
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 19
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
Long and short GRBs are likely related to different progenitors:Long and short GRBs are likely related to different progenitors:collapsars vs compact binary coalescencecollapsars vs compact binary coalescence
E.g. of E.g. of 22 mapping (Emapping (E52 52 - n - n
plane) around plane) around the best fit the best fit solution for solution for short GRB short GRB
051221051221
The The circum-burst mediumcircum-burst medium should should reflect this difference: relatively high reflect this difference: relatively high density environments vs a more density environments vs a more tenuous ISM. Using a numerical tenuous ISM. Using a numerical routine based on routine based on 2 mapping, broad-2 mapping, broad-band afterglow data are analyzed in band afterglow data are analyzed in the standard fireball model, to test if the standard fireball model, to test if present data allow to discern the present data allow to discern the expected difference in density expected difference in density between short-long GRBs.between short-long GRBs.
In the gravitational wave (GW) In the gravitational wave (GW) domain, an in-spiral signal is a domain, an in-spiral signal is a telltail signature for distinguishing a telltail signature for distinguishing a short GRB progenitor from a short GRB progenitor from a collapsar. We thus develop a collapsar. We thus develop a parallel study in the GW domain, parallel study in the GW domain, using Virgo & LIGO data collected using Virgo & LIGO data collected between May and September 2007, between May and September 2007, and in view of the future advanced and in view of the future advanced configurations of these detectors.configurations of these detectors. ns-ns m1= m2 =1.4 M
- - - - in-spiral - - - - in-spiral - - -merger
53 Mpc
220 Mpc
1100 Mpc
Advanced VirgoVirgo
Short GRBs: environment and GW signal as clues to the progenitorShort GRBs: environment and GW signal as clues to the progenitor
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 20
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
INTEGRAL
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 21
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
INTEGRALINTEGRALGamma-ray observatory 15 keV – 10 MeVHigh resolution spectroscopy (SPI) and fine imaging (IBIS) within large FOVMedium-size mission (ESA, Russia, NASA), launched in Oct 2002Community involved via AOs Public archive access, User Group, TAC
IBIS/INTEGRAL: THE unique imager for high energy point sources
Fine imaging of high energy sources and monitoring of large parts of the highly variable sky is crucial for astrophysics
IBIS (Imager)IBIS (Imager)
9x99x9°° PCFOV PCFOV30x3030x30° FOV° FOV
12’ angular resolution12’ angular resolution
positions to ~1’positions to ~1’
ISGRI: 15keV – 1MeVISGRI: 15keV – 1MeVPICSIT: 0.2 – 10 MeVPICSIT: 0.2 – 10 MeV
~10% energy ~10% energy resolutionresolution
<<1ms timing<<1ms timing
IASF-Roma responsible for IBIS in-flightPerformances & Instrument responce
Core Programme Assigned Scientific Topics:Weak BHCs ,X-ray Bursts sources, 1E1740.7-2942, and SURVEY
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 22
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
Spectral evolution of Black hole candidates, Capitanio et al., 2006
Observational INTEGRAL data as inputs for modelling, 1E1740.9-2942 from Del Santo et a., 2006
X-ray Burst Sources most of time @ low luminosity hard state with energy “flat” spectra very similar (Fiocchi et al. 2007)
First Non-thermal emission detected in the hard state for 4U1820-30, Tarana et al.,2007
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 23
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
From BeppoSAX/WFCs to INTEGRAL/IBIS
30 sources detected in the bulge in the 3-20 keV band and 2003 ‘s view of sky distribution of X-ray binaries
~ 70 sources in a ±10 degree region around G.C. and 120 in a ±20 degree, 20-100 keV460 souces in total! i.e. 1‰ of the classical (>10 keV) X-ray sources discovered so far
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 24
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
0
20
40
60
80
100
120
CV AGN HMXB LMXB Other ?
Cat 1
Cat 2
Cat 3
0
10
20
30
40
50
LMXB HMXB AGN Others ?
Sources at energy > 100 keV
Survey 2
Survey 1
Bird A.J., Malizia A., Bazzano A. and Survey team 2007
The nature of the Galactic diffuse continuum emission :
E <100 keV, 80% due to point sources
Individual point souces contribute for 70-80% in the 100 keV-300 KeV band
While active galaxies account for only 3% of the X ray background for E>100 keV
Bazzano A. Stephen J. , Fiocchi MT.and Survey team 2006 and 2007
IBIS Survey, specific source classes analysis and follow-up in collaboration with Soton University & IASF Bologna
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 25
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
What we expect in 1993!!
Compact stellar-size objectsHigh energy transientsExtragalactic sourcesStellar and Explosive NucleosynthesisDiffuse continuum &diffuse line emission plus: Unexpected Discoveries !!
UNEXPECTED DISCOVERIS already!
Obscured HMXB:Find slow (100-1000s) NS, <1013 G, no cyclotron lines, no BH.-: Transient and persistent sources with NH in excess of 10 23 cm-2 difficult to
catch
Super-giant fast transients:Accretion via wind, but disk is
needed to explain fast luminosity increase (x 102 – 103).
-: Transient sources, difficult to catch
A long term monitoring programme with large FOV is crucial to enlarge the database
V. Sguera et al., ApJ 646, 453 2006
IGR J174544-2619 2 hr flare
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 26
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
The keV to TeV connection: a new class of cosmic accelerators
X & Gamma-ray observations of TeV sources crucial to discriminate between leptonic versus hadronic scenarios a source natureThe Integral survey with about 500 sources in the 20-100 keV band provide a fantastic tool to this item.
Ubertini et al., 2005
Dean A.J., De Rosa A. et al., 2007
HESS J1813-178 characteristcs pointed to a PWN/SNR nature:
IGR J1813-1751 from IBIS plus ASCA archival data clearly identified it
IBIS measurement of the composite SNR G11.2-0.3 and associated Pulsar, suggested that soft γ-ray emission is NOT coming from SNR but originates within complex structure associated with the Pulsar and its PWN system
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 27
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
The last son
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 28
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
AGILEThe AGILE Payload: a highly compact instrument for high-energy astrophysics: it combines for the first time a gamma-ray imager (30 MeV- 30 GeV) with a hard X-ray imager (18-60 keV) with large FOVs (2.5 sr and 1 sr respectively) and optimal angular resolution.
Compactness from Si microstrip technology.
Complex functions implemented aboard: 1 DSP, 27 FPGA.
High resolution (2 s) timing with PPS
And all this with:only ~100 kg of Payloadonly ~100 W of PL absorbed poweronly 350 kg of satellite…limited budget and resources
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 29
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
An all italian mission: ASI with contributions of INAF&INFNINAF: IASF Roma, IASF Bologna, IASF MilanoINFN: Sez.Trieste, Sez. Roma I, Sez. Roma IIUniversità di Roma “Tor Vergata”, Università “La Sapienza”CIFS - Consorzio Interuniversitario per la Fisica Spaziale (Torino)
ASI Scientific Data Center has an important role in archiving, interface to the community, support to guest activities, S/W documentation.
PI (M.Tavani) and PI Team, Payload Management, Team Data CenterThe X-ray monitor SuperAGILE
The role of IASF Roma
The role of the community
AOO, Open Archive, Distribution by web of X-ray fluxes, networks of multifrequency observers
Selected topics on the Core Program:
GRBs, Diffuse, New Sources, Selcted Targets
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 30
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICSWho has done what
ANTICOINCIDENCE
INAF-IASF-Mi (F.Perotti)
HARD X-RAY IMAGER (SUPER-AGILE)
INAF-IASF-Rm (E.Costa, M. Feroci)
GAMMA-RAY IMAGER
SILICON TRACKER
INFN-Trieste
(G.Barbiellini, M. Prest)
(MINI) CALORIMETER
INAF-IASF-Bo, Thales-Alenia Space (LABEN)
(G. Di Cocco, C. Labanti)
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 31
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
GRID Effective Area
20-100 MeV
500-> 400 cm²
Gamma Ray Imaging Detecor - GRID
A Silicon TrackerA Silicon Tracker
AndAnd
A Mini-CalorimeterA Mini-Calorimeter
Thanks to Silicon Strip Technique and onboard preselection and on ground selection of events based on logic only (no TOF, no Cherekov) the GRID has a very large f.o.v. = 2.5 sr
Information from MCAL combined with information on scattering of pairs in converters allows for energy reconstruction
10 planes with * 0.07 X0
40 mm resolutionTotal: ~0.9 X0
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 32
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
PSLV-C8 launch, 23 Apr. 2007
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 33
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
AGILE first results (July-November, 2007)• Vela and Crab PSR calibration
• Several Galactic hard X-ray sources• 4 detections of blazars
3C 279 3C 454.3 (repeated gamma-ray flares) HB 1510-089 TXS 0716+714 • Several GRBs detected by Super-A and MCAL (MCAL detects ~ 1/week)• 2 GRBs positioned by SA (X-ray AG by SWIFT) and 1 by SA+IPN
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 34
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
September 28, 2007
The Great Triade
AGILE AND PULSARS
Thanks to PPS we can easily handle high resolution timing.
Agreements are active with radio telescopes to have ephemeris of known and candidate PSR
By folding photons (E>100MeV) detected within the PSF of PS0835-45, in bins of 0.5 ms with the radio period we have the light curve (20 days, July – August 2007)
.
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 35
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
More than 30 sources already detected (+GRBs+SGR)
SuperAGILE is a double 1-d imager based on Silicon Strip Detectors and Tungsten coded mask. ~ 10 kg ~ 10W (Feroci et al.NIM 2007)
SuperAGILE View of the Galactic Plane(3.6 days, l=337, b=8)
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 36
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
BLAZARS
3C 279 ! (9-13 July, 2007)
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 37
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
3C 454.3
+AGILE pointing centroid
~ 36°
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 38
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 39
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
HB 1510-089
Galactic Center
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 40
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
GRBs with AGILE
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 41
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
GRB 071104, at ~22º Localized by SA, XRT by SWIFT, OT by Telescopio Nazionale Galileo
SA (20-60keV)
Light curve
Image
Minicalorimeter 350-700 keV
GRIDS-events (<30MeV)suspect activity
>30MeV
No activity
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 42
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
Something Very Recent
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 43
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
3C 454.3
Cygnus region
AGILE gamma-ray sky: 22 Nov. 2007
INTEGRAL
TOO
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 44
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
Commissioning of AGILE was not completed in July.
Some activities are in progress in these weeks included Activation of the GRB onboard
capability.The GRB is triggered as a step in the counting rate of SA and/or
MCAL v/s moving average.
The SuperAGILE image is analysed aboard (included corrections for aspect instability) and compared with pre-burst image. The coordinates of the Burst are determined and transmitted to ground via a text message by ORBCOMM network.
Trigger Deconvolved Image to ORBCOMM
Del Monte et al. 2007 A&A
RELATIVISTIC and PARTICLE ASTROPHYSICS Enrico Costa – IASF, 25 november 2007 – 45
Presentations to the Visiting Committee
RELATIVISTIC and PARTICLE ASTROPHYSICS
Waiting for future missions….