Search for Dark Matter in the Sky

Aldo Morselli INFN Roma Tor Vergata 14 Jun 2012

Dark Side of the Univers Aldo2012 Morselli, INFN Buzios Roma Tor Vergata 10-15 June 1 Aldo Morselli, INFN Roma Tor Vergata 2 Neutralino WIMPs

Assume χ present in the galactic halo • χ is its own antiparticle => can annihilate in galactic halo producing gamma-rays, antiprotons, positrons…. • Antimatter not produced in large quantities through standard processes (secondary production through p + p --> anti p + X) • So, any extra contribution from exotic sources (χ χ annihilation) is an interesting signature • ie: χ χ --> anti p + X • Produced from (e. g.) χ χ --> q / g / gauge boson / Higgs boson and subsequent decay and/ or hadronisation.

Aldo Morselli, INFN Roma Tor Vergata 3 They Play Together!

Aldo Morselli, INFN Roma Tor Vergata 4 Differential yield for each annihilation channel

WIMP mass=200GeV

A.Cesarini, F.Fucito, A.Lionetto, A.Morselli, P.Ullio, Aldo Astroparticle Morselli, INFN Physics, Roma Tor Vergata 21, 267, 2004 [astro-ph/0305075] 5 Differential yield for b bar

neutralino mass

A.Cesarini, F.Fucito, A.Lionetto, A.Morselli, Aldo P.Ullio, Morselli, Astroparticle INFN Roma Tor Vergata Physics, 21, 267-285, 2004 [astro-ph/0305075] 6 Happy 4th Birthday Fermi !!

11 June 2008

Aldo Morselli, INFN Roma Tor Vergata 7 Fermi Symposium Roma, May 9-12 1011

Aldo Morselli, INFN Roma Tor Vergata 8 4 years in orbit • over 1.37 billion Fermi LAT events to the FSSC • the LAT Collaboration has published 199 papers (Cat I and Cat II). Collectively these papers have been cited nearly 10,000 times. • Fermi satellite, the GBM has triggered on 1949 transients (and at 939 GRBs are creeping ever closer to the 1000 mark). The observatory has performed 77 autonomous repoints and the mission overall has produced over 800 refereed papers with new Fermi results or using/interpreting Fermi results and issued over 30 press/web releases.

Aldo Morselli, INFN Roma Tor Vergata 9 The Fermi LAT gamma-ray sky 3-year all-sky map, E > 1 GeV

Aldo Morselli, INFN Roma Tor Vergata 10 The Fermi LAT 2FGL Source Catalog http://fermi.gsfc.nasa.gov/ssc/data/access/lat/2yr_catalog/ August 4, 2008, to July 31, 2010 100 MeV to 100 GeV energy range

1873 sources 1095 AGN’s 589 unidentified Fermi Coll. ApJS (2012) 199, 31 arXiv:1108.1435 Aldo Morselli, INFN Roma Tor Vergata 11 Third EGRET Catalog 1991-2000, 270 sources , 1.5 M γ’s

Aldo Morselli, INFN Roma Tor Vergata 12 • Towards the Second Fermi LAT Catalog 2FGL:

1095 589

13 Aldo Morselli, INFN Roma Tor Vergata 13 Fermi Gamma-Ray Large Area Space Telescope Tracker 1.68 m

84 cm

Grid Silicon Tracker tower ACD Thermal 18 planes of X Y silicon detectors + converters Anticoincidence Blanket 12 planes with 3% R.L. of W , 4 planes with 18% R.L 2 planes without converters Shield total 1.5 R.L. DAQDAQ Electronics Electronics Calorimeter ( 8.6 Rad.Length)

Aldo Morselli, INFN Roma Tor Vergata 14 How Fermi LAT detects gamma rays Incoming γ 4 x 4 array of identical towers with:

• Precision Si-strip tracker (TKR) Conversion – With W converter foils (γ in e+/e-) in W foils • Hodoscopic CsI calorimeter (CAL) • DAQ and Power supply box γ Incoming direction reconstruction by tracking the charged particles

e+ e- Energy measurement with e.m. calorimeter An anticoincidence detector around the telescope distinguishes gamma- rays from charged particles

Aldo Morselli, INFN Roma Tor Vergata 15 Aldo Morselli, INFN Roma Tor Vergata 16 6

5 0.15Xo(deg) 0.07Xo(deg) Multiple 4 0.05Xo(deg) 3 Scattering 2

10 1 projected angular distribution ( degrees)

0 0.1 1 10 0.15Xo(deg) 1 0.07Xo(deg) E(GeV) 0.05Xo(deg)

0.1 projected angular distribution ( degrees)

0.01 0.1 1 E(GeV) 10 E(GeV)

Aldo Morselli, INFN Roma Tor Vergata 17 Fermi Instrument Response Function

http://www.slac.stanford.edu/exp/glast/groups/canda/lat_Performance.htm Aldo Morselli, INFN Roma Tor Vergata 18 Fermi Instrument Response Function

http://www.slac.stanford.edu/exp/glast/groups/canda/lat_Performance.htm Aldo Morselli, INFN Roma Tor Vergata 19 How Fermi LAT detects electrons Trigger and downlink • LAT triggers on (almost) Incoming Electron every particle that crosses the LAT ACD identifies – ~ 2.2 kHz trigger rate charged particle • On board processing removes many charged particles events Main track – But keeps events with more pointing to the that 20 GeV of deposited hit ACD tile energy in the CAL – ~ 400 Hz downlink rate • Only ~1 Hz are good γ-rays Same tracking and Electron identification energy • The challenge is identifying reconstruction algorithms used the good electrons among for γ-rays the proton background – Rejection power of 103 – 104 required – Can not separate electrons from positrons

Aldo Morselli, INFN Roma Tor Vergata 20 Event topology A candidate electron A candidate hadron (recon energy 844 GeV) (raw energy > 800 GeV)

• TKR: clean main track with extra-clusters • TKR: small number of extra very close to the track clusters around main track • CAL: clean EM shower profile, not fully contained • CAL: large and asymmetric shower • ACD: few hits in conjunction with the track profile • ACD: large energy deposit per tile

Aldo Morselli, INFN Roma Tor Vergata 21 Fermi Electron + Positron spectrum

Extended Energy Range (7 GeV - 1 TeV) One year statistics (8M evts)

Fermi LAT Coll. Physical Review D, Aldo 82 Morselli, 092004 INFN (2010) Roma Tor[arXiv:1008.3999] Vergata 22 Geomagnetic field + Earth shadow = directions from which only electrons or only positrons are allowed

events arriving from West: e+ allowed, e- blocked

events arriving from East: e- allowed, e+ blocked

• For some direcons, e- or e+ forbidden • Pure e+ region looking West and pure e- region looking East • Regions vary with parcle energy and spacecra posion • To determine regions, use code by Don Smart and Peggy Shea (numerically traces trajectory in geomagnec ﬁeld) • Using Internaonal Geomagnec Reference Field for the 2010 epoch

Aldo Morselli, INFN Roma Tor Vergata 23 Positron Fraction

The Fermi-LAT has measured the cosmic-ray positron and electron spectra separately, between 20 and 130 GeV, using the Earth's magnetic field as a charge discriminator •Two independent methods of background subtraction produce consistent results •The observed positron fraction is consistent with the one measured by PAMELA Differences between different experiments below few GeV’s probably due to charge-sign-dependent modulation but still under study Fermi Coll., PRL, 108 (2012) 011103 arXiv:1109.0521 Aldo Morselli, INFN Roma Tor Vergata 24 Positron to Electron Fraction

• Positron Ratio do not behave as expected

Aldo Morselli, INFN Roma Tor Vergata 25 Antiproton-Proton Ratio

• PAMELA ( preliminary)

A.Lionetto, et.al JCAP09 (2005) 010 [astro-ph/0502406]

Diffuse and Convention Propagation Model Upper and lower bounds A.Lionetto, A.Morselli, V.Zdravkovic JCAP09 (2005) 010 [astro-ph/0502406] antiprotons compatible with standard production

Aldo Morselli, INFN Roma Tor Vergata 26 Lepto- philic Models here we assume a democratic dark matter pair- annihilation branching ratio into each charged lepton species: 1/3 into e+e-, 1/3 into µ+ µ- and 1/3 into τ+ τ- Here too antiprotons are not produced in dark matter pair annihilation.

Astrp Phys.32 (2009) 140 [arXiv:0905.0636] Aldo Morselli, INFN Roma Tor Vergata 27 Lepto- philic Models here we assume a democratic dark matter pair- annihilation branching ratio into each charged Pamela + Fermi positrons lepton species: 1/3 into e+e-, 1/3 into µ+ µ- and 1/3 into τ+ τ- Here too antiprotons are not produced in dark matter pair annihilation.

Astrp Phys.32 (2009) 140 [arXiv:0905.0636] Aldo Morselli, INFN Roma Tor Vergata 28 Pulsars

1. On purely energetic grounds they work (relatively large efficiency)

2. On the basis of the spectrum, it is not clear 1. The spectra of PWN show relatively flat spectra of pairs at Low energies but we do not understand what it is 2. The general spectra (acceleration at the termination shock) are too steep

The biggest problem is that of escape of particles from the pulsar 1. Even if acceleration works, pairs have to survive losses 2. And in order to escape they have to cross other two shocks

Extensive discussion two week ago @ GGI ( Serpico, Blasi .. ) New Fermi data on pulsars will help to constrain the pulsar models Aldo Morselli, INFN Roma Tor Vergata 29 What if we randomly vary the pulsar parameters relevant for e+e- production? (injection spectrum, e+e- production efficiency, PWN “trapping” time)

Under reasonable assumptions, electron/positron emission from pulsars offers a viable interpretation of Fermi CRE data which is also consistent with the HESS and Pamela results. D.Grasso et al. Astropart. Phys. 32 (2009), pp.140 [arXiv:0905.0636] Aldo Morselli, INFN Roma Tor Vergata 30 Cosmic Ray Electrons Anisotropy

the levels of anisotropy expected for Geminga-like No-anisotropy map and Monogem-like sources (i.e. sources with similar distances and ages) seem to be higher than the scale of anisotropies excluded by the results However, it is worth to point out that the model results are affected by large uncertainties related to the choice of the free parameters Flight data sky map

Distribuon of signiﬁcance, ﬁed by a Gaussian

Fermi Coll. Physical Review D 82, Signiﬁcance map 092003 (2010) [arXiv:1008.5119]

Aldo Morselli, INFN Roma Tor Vergata 31 electron + positron expected anisotropy in the directions of Monogem and Vela

Fermi/LAT ULs Vela

GALPROP spectrum

Monogem

Fermi Coll. Physical Review D 82, 092003 (2010) [arXiv:1008.5119] Aldo Morselli, INFN Roma Tor Vergata 32 other Astrophysical solution

• Positrons created as secondary products of hadronic interactions inside the sources • Secondary production takes place in the same region where cosmic rays are being accelerated -> Therefore secondary positron have a very ﬂat spectrum, which is responsible, after propagation in the Galaxy, for the observed positron excess

Blasi, arXiv:0903.2794

Aldo Morselli, INFN Roma Tor Vergata 33 B/C Ratio

CREAM 2008 Astr.Phys. 30 133 [arXiv:0808.1718]

ATIC-2 Panov et al., ICRC 2007 spallaon during propagaon only spallaon also during acceleraon Philipp Mertsch, Subir Sarkar Phys.Rev.Lett.103:081104,2009 arXiv:0905.3152

Aldo Morselli, INFN Roma Tor Vergata 34 Search Strategies Satellites: Galactic center: Milky Way halo: Low background and Good statistics but source Large statistics but good source id, but low confusion/diffuse background diffuse background statistics And electrons! and Anisotropies Spectral lines: No astrophysical Galaxy Extra-galactic: uncertainties, good clusters: Large statistics, but source id, but low astrophysics,galactic Low background but diffuse background statistics low statistics Pre-launch sensitivities published in Baltz et al., 2008, JCAP 0807:013 [astro-ph/0806.2911] Aldo Morselli, INFN Roma Tor Vergata 35 Constraints from the Milky Way halo testing the LAT diffuse data for a contribution from a Milky Way DM annihilation/decay signal

2 years of data 1-100 GeV energy range ROI: 5° <|b|<15° and |l|<80°, chosen to: • minimize DM profile uncertainty (highest in the Galactic Center region) • limit astrophysical uncertainty by masking out the Galactic plane and cutting- out high- latitude emission from the Fermi lobes and Loop I

Aldo Morselli, INFN Roma Tor Vergata 36 Constraints from the Milky Way halo bbar channel ISO Halo proﬁle

• Blue = “no-background limits” Fermi Coll. arXiv:1205.6474 • Black = limits obtained by marginalization over the CR source distribution, diffusive halo height and electron injection index, gas to dust ratio, and in which CR sources are held to zero in the inner 3 kpc • Limits with NFW density profile (not shown) are only slightly stronger Aldo Morselli, INFN Roma Tor Vergata 37 Constraints from the Milky Way halo only photons produced by muons (no electrons) to set “no-background limits”

“no-background limits” including Fermi e+ + e- region FSR+IC from dark Pamela positrons region matter limits from profile likelihood and CR sources set to zero in the inner 3 kpc DM interpretation of PAMELA/Fermi CR anomalies disfavored Fermi Coll. arXiv:1205.6474 Aldo Morselli, INFN Roma Tor Vergata 38 Dwarf spheroidal galaxies (dSph) : promising targets for DM detection

Aldo Morselli, INFN Roma Tor Vergata 39 Dwarf Spheroidal Galaxies upper-limits

No detection by Fermi with 11 months of data. 95% flux upper limits are placed for several possible annihilation final states.

Flux upper limits are combined with the DM density inferred by the stellar data(*)for a subset of 8 dSph (based on quality of stellar data) to extract constraints on <σv> vs WIMP mass for specific DM models

(*) stellar data from the Keck observatory (by Martinez, Bullock, Kaplinghat) Fermi Coll. ApJ 712 (2010) 147-158 [arXiv:1001.4531] Aldo Morselli, INFN Roma Tor Vergata 40 Dwarf Spheroidal Galaxies upper-limits Update

robust constraints including J-factor uncertainties NFW. For cored dark matter proﬁle, the J-factors for most of the dSphs would either increase or not change much Fermi Lat Coll., PRL 107, 241302 (2011) [arXiv:1108.3546] Aldo Morselli, INFN Roma Tor Vergata 41 Dwarf Spheroidal Galaxies upper-limits Update

robust constraints including J-factor uncertainties Fermi Lat Coll., PRL 107, 241302 (2011) Aldo Morselli, INFN Roma Tor Vergata [arXiv:1108.3546] 42 DM limit improvement estimate in 10 years with the composite likelihood approach (2008- 2018)

• 10 years of data instead of 2(5x) • 30 dSphs (3x) (supposing that the new optical surveys will find new dSph) • -10% from spatial extension (source extension increases the signal region at high energy E > 10 GeV, M > 200 GeV )

• There are many assumptions in this prediction • Doesn’t deal with a possible detections. Aldo Morselli, INFN Roma Tor Vergata 43 Clusters of galaxies

• Largest virialized and most massive structures in the universe : • • Radio emission suggests cosmic ray (CR) population • Lensing and X-Ray observations indicate large dark matter (DM)

Aldo Morselli, INFN Roma Tor Vergata Abell 2065 44 6 Clusters Stacked Residual Map • 24 Months of LAT P6V11 Diffuse data (P7V6 analysis is ongoing) • Binned analysis, 10 deg ROI, 20 Energy Bins from 200 MeV to100 GeV • Clusters modeled as point sources • No signiﬁcant excess in stacked residual map!

And from outside the collaboration: • Using 3y P7V6 data and 8 clusters (together and singularly) authors ofJCAP01(2012)042 don’t find signal above 3σ. • Authors of arXiv:1201.1003v1, using 3 years of P7V6 data and assuming no CR emission, they obtain a detection of DM in Virgo at 4.4σ (2.1 σ when optimal CR model is included Aldo Morselli, INFN Roma Tor Vergata 45 Fermi LAT Clusters Combined Upper Limits on <σv> (from P6V11 analysis, currently working on P7V6)

• Combined DM Limits ~ factor 2 better than individual ones • S/N tests indicates several more within reach of Fermi-LAT Aldo Morselli, INFN Roma Tor Vergata 46 Fermi Lat Coll., PRD 85, 083007 (2012) [arXiv:1202.2856] Aldo Morselli, INFN Roma Tor Vergata 47 SED of the isotropic diffuse emission (1 keV–100 GeV)

PRL104, 101101-1-7 (2010) arXiv:1002.3603

Aldo Morselli, INFN Roma Tor Vergata 48 the Isotropic Gamma-ray Background (IGRB)

Preliminary

• Total contribution from FSRQ + BL Lac + Radio galaxies + Star-forming galaxies: ~ 50%- 80% • 25% foreground modeling uncertainty not included in EGB error bands. The remaining contribution could be due to more unresolved point sources populations or different diffuse process (as cosmological DM annihilation). Aldo Morselli, INFN Roma Tor Vergata 49 Update on the Isotropic Gamma-ray Background (IGRB) 200 MeV to 580 GeV

Preliminary

Also Consistent with a softening at high energies ( E> 100 GeV ) Aldo Morselli, INFN Roma Tor Vergata 50 The Fermi LAT 2FGL Inner Galactic Region

August 4, 2008, to July 31, 2010 100 MeV to 100 GeV energy range

Fermi Coll. ApJS (2012) 199, 31 arXiv:1108.1435

Aldo Morselli, INFN Roma Tor Vergata 51 (r) ρ r -1 log log

r -3

log (r)

High DM density at the Galactic center

Aldo Morselli, INFN Roma Tor Vergata 52 Milky Way Dark All proﬁles are normalized to the local Matter Profiles density 0.3 GeV cm－3 at the Sun’s location r ≈ 8.5 kpc

A.Lapi et al. arXiv:0912.1766

Aldo Morselli, INFN Roma Tor Vergata 53 Different spatial behaviour for decaying or annihilating dark matter

The angular profile of the gamma-ray signal is shown, as function of the angle θ to the centre of the galaxy for a Navarro-Frenk-White (NFW) halo distribution for decaying DM, solid (red) line, compared to the case of self-annihilating DM, dashed (blue) line Aldo Morselli, INFN Roma Tor Vergata 54 Spectrum (E> 400 MeV, 7°x7° region centered on the Galactic Center analyzed with binned likelihood analysis )

data (stat. error) preliminary

best diffuse model and isotropic emission

12 Fermi 1 year catalog sources

Fermi Coll. NIM A630 (2011) 147 Aldo [arXiv:0912.3828] Morselli, INFN Roma Tor Vergata 55 GC Residuals 7°x7° region centered on the Galactic Center 11 months of data, E >400 MeV, front-converting events analyzed with binned likelihood analysis ) • The systematic uncertainty of the effective area (blue area) of the LAT is ~10% at 100 MeV, decreasing to 5% at 560 MeV and increasing to 20% at 10 GeV

Fermi Coll. NIM A630 (2011) 147 Aldo [arXiv:0912.3828] Morselli, INFN Roma Tor Vergata 56 Residual Emission for 15 * 15 degrees around the Galactic center

32 Months Data (Front events)

DATA DATA- Model (diffuse+ sources)

Diffuse emission and point sources account for most of the emission observed in the region. Low-level residuals remain, the interpretation of these is work in-progress Papers are forthcoming and will include dark matter results. Aldo Morselli, INFN Roma Tor Vergata 57 Galactic-Centre Gamma Rays in CMSSM Dark Matter Scenarios

A0=0 µ>0 A0=0 µ>0 NFW proﬁle Einasto proﬁle mχ=400 GeV mχ=400 GeV FERMI FERMI constraints constraints

mχ=300 GeV mχ=300 GeV

The constraints due to the absences of charginos and the Higgs boson at LEP are also shown, as black dashed and red dot-dashed lines, respectively. Regions excluded by the requirements of electroweak symmetry breaking and a neutral LSP are shaded dark pink and brown, respectively. The green region is excluded by b → sγ, and the pink region is favoured by the supersymmetric interpretation of the discrepancy between the Standard Model calculation and the experimental measurement of gμ － 2 within 1 and 2 standard deviations (dashed and solid lines, respectively) Ellis et al., arXiv:1106.0768 Aldo Morselli, INFN Roma Tor Vergata 58 Wimp lines search

Aldo Morselli, INFN Roma Tor Vergata 59 Search for Spectral Gamma Lines ➡ Smoking gun signal of dark matter Search for lines in the first 11 months of Fermi data (30-200 GeV en.range) Search region |b|>10o and 30o around galactic center • For the region within 1oof the GC, no point source removal was done as this would have removed the GC • For the remaining part of the ROI, point sources were masked from the analysis using a circle of radius 0.2 deg • The data selection includes additional cuts to remove residual charged particle contamination.

Aldo Morselli, INFN Roma Tor Vergata 60 Fermi LAT 23 Month Line search results Flux Upper Limits, 7 GeV - 200 GeV • ± 20 % overall scale systematic error (+20 % systematic for UL). Additional systematic on spectral structures with LAT resolution for E < 13.2 GeV of s/bg ~ 1%. • 7 and 10 GeV bins use a modiﬁed event selection to reduce the systematic uncertainty associated with public IRFs. • For E > 12 GeV no indication of a spectral structure systematic effect is seen.

Fermi Lat Coll., PRD accepted Spectral Line Energy (GeV) arXiv:1205.2739 Aldo Morselli, INFN Roma Tor Vergata 61 Decay lifetime lower limits • Limits similar for all 3 DM density profiles due to linear dependence of flux on ρ • Disfavors lifetimes smaller than 1029 s

Fermi Lat Coll., PRD accepted arXiv:1205.2739 Aldo Morselli, INFN Roma Tor Vergata 62 Fermi LAT 23 Month Zγ-Cross-section limits 7 GeV - 200 GeV • ± 20 % overall scale systematic error (+20 % systematic for UL). Additional systematic on spectral structures with LAT resolution for E<13.2 GeV of s/bg ~ 1%.

Fermi Lat Coll., PRD accepted arXiv:1205.2739 Aldo Morselli, INFN Roma Tor Vergata 63 Fermi LAT 23 Month γγ-Cross-section limits 7 GeV - 200 GeV • ± 20 % overall scale systematic error (+20 % systematic for UL). Additional systematic on spectral structures with LAT resolution for E<13.2 GeV of s/bg ~ 1%.

Fermi Lat Coll., PRD accepted arXiv:1205.2739 Aldo Morselli, INFN Roma Tor Vergata 64 Cross section upper limits for dark matter annihilation

Fermi best fit region

PAMELA best fit region

cross section for a thermally produced WIMP

No photons from astrophysical background sources have been included, making these limits very conservative. Fermi Lat Coll., PRD accepted arXiv:1205.2739 Aldo Morselli, INFN Roma Tor Vergata 65 Cross section upper limits for dark matter annihilation

Fermi best fit region

PAMELA best fit region

cross section for a thermally produced WIMP

Weniger arXiv:1204.2797 Aldo Morselli, INFN Roma Tor Vergata 67 A line at ~ 130 GeV ? see also Tempel et al. arXiv:1205.1045 Kyae & Park arXiv:1205.4151 Dudas Mambrini et al. arXiv:1205.1520 Boyarsky et al. arXiv:1205.4700 Lee et al. arXiv:1205.4700 Acharya, Kane et al. arXiv:1205.5789 Buckley, Hooper arXiv:1205.6811 Su, Finkbeiner arXiv:1206.1616 Chu,Hambye et al. arXiv:1206.2279

Aldo Morselli, INFN Roma Tor Vergata 68 All-sky Fermi -LAT 3.7 year sky maps in 4 energy bins

－2◦ < b < 2◦ masked and source subtraction Su, Finkbeiner arXiv:1206.1616 Aldo Morselli, INFN Roma Tor Vergata 69 smoothed with a Gaussian kernel of FWHM = 10◦ without source subtraction

Su, Finkbeiner arXiv:1206.1616 The null hypothesis of zero intensity is ruled out by 5.0σ (3.7σ with trials factor) Aldo Morselli, INFN Roma Tor Vergata 70 Fermi LAT 23 Month γγ-Cross-section limits 7 GeV - 200 GeV • ± 20 % overall scale systematic error (+20 % systematic for UL). Additional systematic on spectral structures with LAT resolution for E<13.2 GeV of s/bg ~ 1%.

Weniger 2012 NFW fit

Weniger 2012 Einasto fit

Fermi Lat Coll., PRD accepted arXiv:1205.2739 Aldo Morselli, INFN Roma Tor Vergata 71 GC Residuals 7°x7° region centered on the Galactic Center 11 months of data, E >400 MeV, front-converting events analyzed with binned likelihood analysis ) • The systematic uncertainty of the effective area (blue area) of the LAT is ~10% at 100 MeV, decreasing to 5% at 560 MeV and increasing to 20% at 10 GeV

Fermi Coll. NIM A630 (2011) 147 Aldo [arXiv:0912.3828] Morselli, INFN Roma Tor Vergata 72 Gamma-light scheme 40+1 x-y planes AC 100 µm pitch each

~0.256 X0

54.7 cm height of a plane 1.3 cm

2 Xo Calorimiter 100 µm 50 cm 50 cm pitch 9.5 cm

Aldo Morselli, INFN Roma Tor Vergata 73 Flux Sensitivity

5σ COMPTEL

GAMMA-LIGHT Fermi LAT ( Front+Back)

Aldo Morselli, INFN Roma Tor Vergata 74 Effective area (0-30 degrees) G-LIGHT set-up: 40 planes, no tungsten, 1.3 cm spacing, Si pitch 120 micron, analog (alternate) readout, Kalman reconstruction, assumed bkg rejection eff. 10-4.

Aldo Morselli, INFN Roma Tor Vergata 75 PSF (68% containment radius) (Fermi: 0°; G-LIGHT: 30°) G-LIGHT set-up: 40 planes, no tungsten, 1.3 cm spacing, Si pitch 120 micron, analog (alternate) readout, Kalman reconstruction, assumed bkg rejection eff. 10-4.

Aldo Morselli, INFN Roma Tor Vergata 76 Aldo Morselli, INFN Roma Tor Vergata 77 Compton scaering and pair producon telescope. No high-Z converter. Opmal PSF. ESA Call for Small Missions: June, 2012

Aldo Morselli, INFN Roma Tor Vergata 78 Gamma-light payload

Power~ 400 W Weight~600 Kg

Aldo Morselli, INFN Roma Tor Vergata 79 Summary and Conclusions • The Fermi-LAT has made great progress toward constraining/ identifying the nature of DM – Many independent search strategies (dSphs, clusters, MW halo, etc.) - Best LAT constraints (dwarf stacking) are already beginning to reach some interesting areas of parameter space • Fermi-LAT DM sensitivity is anticipated to improve -Improved understanding of astrophysical backgrounds -Increased exposure (sensitivity gain linear in time at high energies) -Improvements in analysis and understanding of detector response • Constraints provided by the Fermi-LAT are highly complementary to direct and accelerator searches Aldo Morselli, INFN Roma Tor Vergata 80 Future Surprises We are just beginning... • Exposure continues to increase - Fainter sources become detectable - Increasingly detailed studies of bright sources - Catalogs become deeper and more detailed • Time domain studies enter longer regimes • Solar cycle beginning to warm up • Plus, efforts continue to further improve performance and enhance analysis, particularly at low and high energies Exciting progress on Pass8, expected to be the ultimate IRF version. The longer we look, the more surprises we will see Aldo Morselli, INFN Roma Tor Vergata 81 thank you for your attention !

Aldo Morselli, INFN Roma Tor Vergata 82