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LNF-INFN Frascati. BTF. Peak luminosity evolution in 2004-5. Luminosity is what matter…in our case. L = 1.46 10 32 cm -2 s -1 (to day). KLOE FINUDA LUCE DI SINCROTRONE FISICA di MACCHINA-SRFF FASCI ESTRATTI. …..and the physics…. KLOE – (K LOng Exp.).

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Presentation Transcript
slide1

LNF-INFN

Frascati

slide3

Peak luminosity evolution in 2004-5

Luminosity is what matter…in our case

L = 1.46 1032 cm-2s-1 (to day)

KLOE

FINUDA

LUCE DI SINCROTRONE

FISICA di MACCHINA-SRFF

FASCI ESTRATTI

…..and the physics….

slide4

KLOE – (K LOng Exp.)

Sistematic study of exotic nuclei

DAFNE experiments

KLOE is running his year

FINUDA Kaons absorbed by nuclei

DAFNE e+e- F KK is a source of monochromatic correlated

low energy Kaons

slide5

The program is well defined for the coming three years

KLOE

FINUDA

exotic

nuclei

FINUDA

exotic

nuclei

SRFF ?

SIDDHARTA

Kaonic

atoms

2006 2007 2008

TODAY

slide6

KLOE physics results:

Vus from KL, KS and charged K’s

Kaon form factors

Pion form factors/g-2

Ks rare decays

charged kaon decays

KS semileptonic decays

KL branching ratios

KL life time

KS to gg

F radiative decays

eta decays

KO-KObar interference

slide7

Collect 2 fbarn-1 on F resonance – end of the current year

  • 2) Scan over the F resonance 50 pbarn-1
  • 3) 250 pbarn-1 at 1000MeV , below the F, to measure pion form factors

1st April 2006 END of KLOE

2006 Nuclear Physics with FINUDA

2007 Kaonic Atoms with SIDDHARTA

2008 FINUDA and SRFF with DAFNE

slide8

Experimental studies on short-bunches and bunch-length modulation at DAFNE

SRFF = Superconductive RadioFrequency Focusing

EXPERIMENT

SC 1.3 GHz cavity

Longitudinal phase space

IP

RF input

RF center

RF output

Energy

spread

Bunch length

slide9

The 7th and 8th of November we have in Frascati an international workshop on Bunch Dynamics.

We hope to have the scientific case at the end of the workshop.

You are invited to collaborate

You can find the relevant information for the workshop on the web: www.lnf.infn.it

slide11

1)LNFExperiments in other Laboratories

  • ATLAS @ CERN LHCb@CERN
  • DIRAC@ CERN EXPLORER@CERN
  • LVD @ LNGSOPERA @ LNGS
  • BABAR@SLACAIACE@TJNAF
  • CDF@FNALBTeV @ FNAL
  • HERMES@ DESYAccelerators @ DESY, SLAC,CERN
  • VIRGO @ Cascina
  • WIZARD @ Pamela
eu@sinbad

2) Use of the Synchrotron light lines

2) Synchrotron light facility much used by external users

EU@SINBAD
  • June 2005
  • 30 proposals
  • >70 users

TARI1+I3

slide13

3)Beam Test Facility

Electrons

Positrons and

Tagged Photons beams

Control room

  • Flux: 11010 particles/pulse
  • Energy: 25750 MeV
  • Repetition rate 50 Hz
  • Pulse Duration 1 or 10 ns
  • p resolution: 1%
  • Spot size sx,y ≈ 2 mm
4 cnao

Centro Nazionale di Adroterapia Oncologica

4)CNAO

GSI RFQ+linac

A proton synchrotron

In the hospital of Pavia

Scanning and monitoring stations

slide15

LNF-AD participates to the

Assembling

Commissioning

First running

Technology transfer

slide16

Delay Loop and transfer line

final lay-out

Transfer line:

installed and commissioned.

Delay Loop: installation

spring-summer 2005,

commissioning autumn 2005

D.Alesini, G.Benedetti,

C.Biscari, R.Boni, M.Castellano,

A.Clozza, A.Drago, D.Filippetto,

A.Gallo, A.Ghigo (resp), F.Marcellini, C.Milardi, L.Pellegrino, B.Preger, M.A.Preger, R.Ricci, C.Sanelli, M.Serio, F.Sgamma, A.Stecchi, A.Stella, M.Zobov

+

Accelerator Division Technical Staff

slide17

5) At CERN CTF3 (CLIC Test Facility)

Delay Loop, transfer line, combiner ring

slide18

6) FEL nei LNF

Sorgente

Pulsata

Auto-amplificata

Radiazione

Coerente

Self-Amplified Pulsed Coherent Radiation

L.Palumbo

slide19

synchronisation

uncompressed pulse

vacuum compressor

acceleration

chamber

detectors

area

control

& data

LINAC

UNDULATOR

7 experimental setup for lwfa acceleration of externally injected electrons in a gas jet plasma
7) Experimental setup for LWFA acceleration of externally injected electrons in a gas-jet plasma

TeraWatt

GigaVolt/m

Frascati

Laser for

Acceleration and

Multidisciplinary

Experiments

Approved: The construction is starting now

brilliance of x ray radiation sources
Brilliance of X-ray radiation sources

8) SPARC-X

12.4

1.24

0.124

l (nm)

FEL for X-rays

Covering from the VUV

to

the 1 Å X-ray spectral range

Approved

SPARX

linac2 high energy section

Etot ~ w 4 S-band :

1.5 GeV e-,1GeV e+

Now : Etot ~ 1.2 GeV

Etot ~ w 4 X-band 2 GeV e-

Linac2: High energy section

dogleg start

slide25

PROGRAM 2005 2006 2007 2008 2009 2010

KLOE END-------------------------------------

FINUDA ---------------------------------------END--------------

SIDDARTHA ---------------------------------------END--------------

LHC --------------------------------------------------------------------------------

SPARC ---------------------------------------END

SPARCX ---------------------------------------------------------------START------

FLAME ----------------------------------------START------------------------------

CTF3 ---------------------------END

CNAO ----------------------------------------END

BTF --------------------------------------------------------------------------------

SYNCH.LIGHT-------------------------------------------------------------------------------

BABAR ----------------------------------------END

CDF ----------------------------------------------------END

HERMES ----------------------------------------------------END

OPERA ---------------------------END----------------------------------------------

ILC -------------------------------------------------------------------------------

slide26

What about the short range future ?

  • WE ARE THINKING ABOUT the possible
  • DAFNE UPGRADE in luminosity AND energy
  • To do what?
  • To complete the Kaon physics program
  • To measure the P, N, L time like form factors
  • To measure gg interactions below 2.4 GeV
  • To measure the total cross section
  • To continue the systematic studies of exotic heavy and light nuclei
  • To have the most advanced accelerator technology
  • To have an even more intense Synchrotron light source
starting point for the accelerator design
Starting point for the accelerator design

DAFNE2 e+ e- collider

Optimized to run on the F meson but able to go up in energy

slide28

DAFNE2

SKETCH OF NEW LAYOUT

Two rings

One IR

EXP

Rf cavities

wigglers

DAFNE HALL

slide29

accumulator

  • Injection system
  • upgrade
  • The proposed transfer lines pass in existing controlled area
  • Additional shielding needed in the area between the accumulator and DAFNE buildings

new e- line

BTF

SPARCX

new e+ line

DAFNE2

rf system
RF system

Higher frequencies – lower acceptance

Lower frequencies – higher voltage

A possible candidate cavity

500 MHz SC cavity operating at KEKB

R&D on SC cavities with SRFF experiment in DAFNE

slide31

We can make use of the

recent progress in SUPERCONDUCTING wiggler technology

Operating experiences:

CESRc, ELETTRA, CAMD

Why wigglers are important?

  • To achieve the short damping times and ultra-low beam emittances needed in LC Damping Rings
  • To increase the wavelength and/or brightness of emitted radiation in synchrotron light sources
  • To increase radiation damping and control emittance in colliders

R&D in progress:

ILC, ATF, PETRA3, …

E. Levichev

slide33

CONCLUSIONS

VERY ACTIVE Laboratory for the coming three-four years

INFN will define the future of the Lab in the course of 2006

da f ne the 16th of september
DAFNE the 16th of September

Lpeak = 1.46 cm-2 sec-1

KLOE WILL STOP DAQ END 2005

With 2000 pbarn-1 integrated

Integrated luminosity = 8.8 pbarn-1/day