A. Karle UW Madison 1. 2 Why neutrino astronomy? Astrophysical Accelerators Neutrinos allow for...

44
A. Karle UW Madison 1

Transcript of A. Karle UW Madison 1. 2 Why neutrino astronomy? Astrophysical Accelerators Neutrinos allow for...

A. Karle UW Madison

1

A. Karle UW Madison

2

Why neutrino astronomy?Astrophysical Accelerators

Neutrinos allow for observation of ‘hidden regions’ of cosmic accelerators (BH, pulsars, initial epochs of SN explosions). The penetrating power of νs is important also for moderately opaque sources from which we may be seeing ϒ spectra that are significantly distorted

DM annihilation CasA Supernova Remnant in X-rays

Accretion disk with jets

A. Karle UW Madison

3

Drilling experience

AMANDA drilling (1950m) 90 hrs

IceCube drilling (2450m) 35 hrs

Thermal power: 5MW

NSF, Aug 7, 2007 Tom Gaisser, IceCube Status 4

Detector reliability

• Very good survival rate during installation.

• 98.5% of all deployed sensors are commissioned and being used in the first science run.

• In 1000 DOM years of accumulated live time only 2 sensors failed after commissioning.– Estimated survival rate after 15 years: 97+1.5

-3.5%– Estimate based on the assumption of a constant failure rate.

A. Karle UW Madison

5

IceCube Laboratory and Data Center

Commissioned for operation in January 2007.

3 Winter-over scientists operate and maintain instrument during winter

Only two winter-overs planned for 2008

17 racks of electronics

Power: 60 kW total for full IceCube

NSF, Aug 7, 2007 Tom Gaisser, IceCube Status 6

IceCube 22: 2007 operation since “physics” start

• May 23, run 107868 until July 30, run 108975– 95.9% uptime– Trigger

• In-ice: > 7 hits in 5 s• IceTop > 5 hits in 2 s

– Typical rates:• in i3+AMANDA(twr) mode: 610 Hz• In i3-only: 525 Hz

• Since start of I3 physics filtering (July 7 - now):– 99.4% uptime (special ops –like CV flashing- while running

at least partial I3 detector)• Data

– 200 GBytes/day raw data written to disk– 25 GBytes/day filtered and sent north via satellite– Monitoring files posted daily at http://icecube.berkeley.edu/i3-

monitoring/2007/monitor.shtml

NSF, Aug 7, 2007 Tom Gaisser, IceCube Status 7

List of deployed filters (31/07/07)

Name in FilterMask Prescale (1/N) Summary of event selection

IceCubeMuonFilter 1 (Linefit.theta >= 70.0 and NChannelInIce >=10) OR

(Linefit.theta >= 60.0 and NChannelInIce >=40)

CascadeFilter 1 TensorOfInertia.evalratio>.109 and Linefit.velocity<.25

(all based on LCSpan 1)

EHEFilter 1 NChannelInIce >= 80

MoonFilter 1 No events currently selected (moon down)

LowEnergyContainedFilter 1 Linefit.velocity (0.1,0.5) & NChannelInIce < 16 &

Many Others (see proposal)

IceTopSMT 5 Any event with an IceTop SMT trigger present

IceTopSMT_Large 1 Any event with NChannelIceTop >= 16

IceTopSMT_InIceCoincidence 1 Any event with BOTH InIce SMT and IceTop SMT

triggers present

InIceSMT_IceTopCoincidence 5 Any event with an InIce SMT and any IceTop station

hit

FilterMinBias 200 Any event seen in the JEB.

NSF, Aug 7, 2007 Tom Gaisser, IceCube Status 8

Offline Data Flow

From Pole to North by satellite

Physics analysis

Dec

om

pre

sse

d

Cal

ibra

ted

Ref

ilter

ed

9

IceTop

InIce

Air shower detector

80 pairs of ice

Cherenkov tanks

Threshold ~ 300 TeV

Goal of 80 strings of 60

optical modules each

17 m between modules

125 m string separation

2004-2005 : 1 string

2005-2006: 8 strings

AMANDA-II

19 strings

677 modules

2006-2007:

13 strings deployed

IceCubeCurrent configuration- 22 strings- 52 surface tanks

Completion by 2011.2007/08: add 14 to 18 strings and tank stations

1450m

2450m

AMANDA now operating as part of IceCube

NSF, Aug 7, 2007 Tom Gaisser, IceCube Status 10

IC22 Events

Downward cosmic-ray event (“muon bundle”) Upward candidate event

( Red hits = early; yellow/green/blue = later ) IceCube DOM locations blue, AMANDA OM locations red

11

Azimuth distributions: IC9 and IC22

Downgoing muons.

Azimuth distribution illustrates detector response.

At lower energies one can see azimuthal structure due to detector geometry.

Rate for 22 strings~4 times higher

12

IC22 - Online zenith distribution

Zenith distribution is compared to simulations. (Crosses: data, line: MC, normalized)

Events with zenith angle > 80° pass online filter and are sent to North.

(There are numerous other filter streams, eg. Nu_e and nu-tau, GRB, WIMPs, …)

Cos(zenith)

NSF, Aug 7, 2007 Tom Gaisser, IceCube Status 13

IceTop – 2 tanks per station

Preliminary energy spectrum with 2006 data

NSF, Aug 7, 2007 Tom Gaisser, IceCube Status 14

Reconstruction of big, coincident event: E ~ 0.5 EeV by IceTop

0.5 EeV ~2000 at 2.5 km

NSF, Aug 7, 2007 Tom Gaisser, IceCube Status 15

Cosmic-ray physics with IceCube

• Measure spectrum/composition– from <1 PeV to >1 EeV– IceTop alone– In-Ice alone (muon bundles)– Hybrid, coincident events

• Calibration with IceTop tagged events• Measure physics background

– Muons and muon bundles

NSF, Aug 7, 2007 Tom Gaisser, IceCube Status 16

Atmospheric with IceCube-9

Note severe cuts needed to reject background with only 9 strings.Situation will improve as detector grows

Phys. Rev. D (to be published)arXiv:0705.1781

NSF, Aug 7, 2007 Tom Gaisser, IceCube Status 17

Growth of detector

AMANDA ANTARES

+IC9

+IC36-40+IC22

Full IceCube 2011

Km3Net

NSF, Aug 7, 2007 Tom Gaisser, IceCube Status 18

IC 9 in 2006

Point source catalog• Many involve jets • IC-9 point source search reported at ICRC2007

NSF, Aug 7, 2007 Tom Gaisser, IceCube Status 19

Point source search, example: MILAGRO MGRO2019+37 in Cygnus

Note: small signal with signal/background ~1

Photon flux: data & model fits to MGRO J 2019 +37

NSF, Aug 7, 2007 Tom Gaisser, IceCube Status 20

IceCube Sensitivity

• IC9 sensitivity ~10-7 GeV-1 cm-2 s-1 (EGeV)-2

– ~2 orders of magnitude above predicted signal from MGRO J2019 +37

– Cuts remove large fraction of signal (90% for atmospheric spectrum, less for harder spectrum)

• Sensitivity grows faster than detector size– For example, IC22 sensitivity is 4-5 times IC9

while size ratio is 2.5– Angular resolution improves with longer tracks

NSF, Aug 7, 2007 Tom Gaisser, IceCube Status 21

Expectations for point source search with IceCube

• Expected signals small– < few events per year– Background of atmospheric in search bin

comparable to expected signal– Optimize search techniques

• Unbinned searches • Sensitivity to expected hard spectrum• Source stacking

• Multi-messenger approach:– Use correlation with physically related

variability in multi-wavelength data – Examples: flaring AGNs; GRB

NSF, Aug 7, 2007 Tom Gaisser, IceCube Status 22

Multi-messenger/multi-wavelength

• Coordination with MAGIC, VERITAS, HESS…• Two IceCube talks this week at

• Optical follow-up scheme proposed– Like ROTSE to look for GRB afterglow or SN light

curve or choked GRB– Trigger on 2 or more in time/direction window

• Two guest investigator proposals to GLAST

NSF, Aug 7, 2007 Tom Gaisser, IceCube Status 23

Search for neutrinos from GRB

Cascade(Trig & Roll)

Cascade(Rolling)

search

All flavor limits by AMANDAGRB models

Waxman-BahcallPRL 78 (1997) 2292

Murase-Nagataki APRD 73 (2006) 063002

Supranova,Razzaque et al.PRL 90 (2003) 241103

Choked burstsMeszaros-WaxmanPRL 87 (2001) 171102

Limits on neutrinos from GRB from AMANDA: -from cascades (e, ), Ap.J. 664 (2007) 397-from neutrino-induced muons, Ap.J (to be published)

NSF, Aug 7, 2007 Tom Gaisser, IceCube Status 24

Prospects for detecting GRB ’s with IceCube

• AMANDA limits– Already disfavor some models– Sensitivity close to classic Waxman-Bahcall

fireball prediction (expected ~ 1 in 400 GRBs)• IceCube sensitivity ~20 times AMANDA

– 200 GRB / yr expected from GLAST– Expect 3 detection of Waxman-Bahcall level in

70 GRB with full IceCube– Non-observation would indicate GRB jets are

pure Poynting flux (Blandford) rather than baryon loaded plasma (Piran, Meszaros, …)

NSF, Aug 7, 2007 Tom Gaisser, IceCube Status 25

Cascades—a way to avoid background of atmospheric

Neutral Current (NC) : X N X X , where x = e, ,

Charged Current (CC) : e N e X N X

M.Kowalski [astro-ph/0505506Atmospheric -induced cascade events:- 9-strings: 10 events / year- 22-strings: 30 events / year

Prompt -induced cascades from charm- 15 events/year with 22 string-array

Diffuse extraterrestrial neutrino flux (expected from AGNs or GRBs)

- With 22 strings Waxman-Bahcall rate (with source evolution) E2<5x10-8 GeV-1sr-1s-1 may be detectable

NSF, Aug 7, 2007 Tom Gaisser, IceCube Status 26

Take advantage of -oscillations: use the channel

• No atmospheric background

• But rare, ~1 event / yr in full IceCube

27

AMANDA+IC22:Improves low-energy capability for point source search

including from WIMP annihilation in Sun

AMANDA+IC22AMANDA

Angular Resolution Effective Area

AMANDA gives to IceCube more area at lower energyfrom ~ 100 GeV

IceCube gives to AMANDAa better angular resolution up to ~ 50 TeV

Optimization scheme in order to fight atmospheric neutrinos (dominant at this energy):- Search for from dark matter- X-ray Binary: energy spectrum and time characteristic- Pulsar Wind Nebulae: energy spectrum - SNr near Molecular Clouds: stacking

AMANDA+IC22

IC22

preliminary

preliminary

NSF, Aug 7, 2007 Tom Gaisser, IceCube Status 28

AMANDA/IceCube as MeV detector…first proposed by Halzen, Jacobsen & Zas, astro-ph/9512080

PMT noise low (~ 300 Hz) ice uniformly illuminated

detect correlated rate increase on top of PMT noise

NSF, Aug 7, 2007 Tom Gaisser, IceCube Status 29

Supernova watch with IceCube

• IceCube SN DAQ– Now running with 1300 DOMs

– Total noise rate shown • Connection to SNEWS

– Planned for 07/08 season

– Depends on good monitoring

• Sensitivity– Example shows SN at gal. cntr. – Good probability of detection out

to LMC

IceCube deployment 2005-2011AMANDA

IceCube string and IceTop station deployed 12/05 – 01/06

IceTop station only 2006

2560 DOMs deployed to date

ONLY 3 ? FAILED SO FAR

3 more seasons planned

Crucial planning period during the next 4 – 6 months

21

3029

40

50

3938

4748

49

595857

6667

74

65

73

7778

46

56

72

IceCube string and IceTop station deployed 01/05

IceCube string and IceTop station deployed 12/06 – 01/07

71

64

55

IceTop station only in 06 / 07

7576

7069

68

6362

6160

5354

52

4544

Deployed in 07 / 08

2004 / 05

2005 / 06

2006 / 07

2007 / 08

NSF, Aug 7, 2007 Tom Gaisser, IceCube Status 31

Extras

NSF, Aug 7, 2007 Tom Gaisser, IceCube Status 32

Detector operation(Snapshot as of 31-07/07)

PnF Physics Filter Rates

Filter Hz Filter Hz

CascadeFilter 17.6188 EHEFilter 1.2611

FilterMinBias 2.57963 IceCubeMuonFilter 19.0078

IceTopSMT 2.51175 IceTopSMT_InIceCoincidence 2.2141

IceTopSMT_Large 0.832898 InIceSMT_IceTopCoincidence 2.09922

JAMSMuonFilter 0 LowEnergyContainedFilter 3.95822

MoonFilter (*) 0 MuonFilter 19.0078

Latest Status from Experiment Control

*Moon data is taken only when it is > 15 degrees above horizon

NSF, Aug 7, 2007 Tom Gaisser, IceCube Status 33

Properties of coincident events

NSF, Aug 7, 2007 Tom Gaisser, IceCube Status 34

Compare AMANDA-IC9

NSF, Aug 7, 2007 Tom Gaisser, IceCube Status 35

Point source search with IC9

IC9 Neutrino effective area (Dumm, Finley & Montaruli, ICRC2007)

NSF, Aug 7, 2007 Tom Gaisser, IceCube Status 36

Growth of detector volume

37

Photon data: light curves combination

Elisa Resconi

M. Tluczykont, M. Shayduk, O. Kalekin, E. Bernardini

38

What do we gain? Analysis cuts re-optimized using the blocks distribution For the moment NO energy spectrum optimization (to be come soon) How does it look like the Detection Probability ??

Preliminary

NSF, Aug 7, 2007 Tom Gaisser, IceCube Status 39

Optical follow-up

Teresa Montaruli for Multi-wavelength conference, Adler Planetarium, Aug 9

NSF, Aug 7, 2007 Tom Gaisser, IceCube Status 40

Take advantage of -oscillations: use the channel

• No atmospheric background

• Assume diffuse flux at AMANDA limit– 3 x Waxman-Bahcall limit– A total of ~0.48 events per year is

expected for all tau signature in IC-22 • Lollipops: ~0.16 events per year• Inverted Lollipops: ~0.19 per year• Double Bangs: ~0.13 per year

July 22, 2007 Tom Gaisser 41

All strings with 60 DOMs on

July 22, 2007 Tom Gaisser 42

Local coincidence count rates versus depth (std. occupancy plot)

Note that rates are lower in this standard occupancy plot-- Note: SMT >= 8 per string is required

Future high-energy

extensions ?

1500

2500

Low energy core ?

• AMANDA has no veto coverage from top, (which is where the muons come from)• Ice below 2100m is exceptionally clear, significantly better even than current ice model.

A. Karle