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IceCube radio extension Status and results

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Presentation on theme: "IceCube radio extension Status and results"— Presentation transcript:

1 IceCube radio extension Status and results
Hagar Landsman, University of Wisconsin, Madison For the IceCube Collaboration

2 ARENA 2010, Nantes IceCube RF extension Hagar Landsman
RICE NARC AURA SATRA ARA RASTA or How many acronyms can one slide hold? South Pole Under Ice RF instrumentation: RICE (Ilya Kravchenko) Part of IceCube DAQ: “AURA” sub-working group (Full WF digitization) Askaryan Underice Radio Array “SATRA” sub-working group (Transient detection) Sensor Array for Transient Radio Astrophysics Future independent collaboration: ARA – Askaryan Radio Array (Kara Hoffman) South Pole Surface RF Instrumentation: Surface radio - RASTA – Radio Air Shower Transient Array (Sebastian Boser) This talk “NARC” Neutrino Array Radio Calibration ARENA 2010, Nantes IceCube RF extension Hagar Landsman

3 NARC – Neutrino Array Radio Calibration
In ice digitization . Combination of ANITA/IceCube/RICE technologies: 2 clusters in 3 clusters in Depth of 1450 m or 300 m AKA “AURA”  Envelope detection. 6 units deployed at -35, -5 meters ( ) 6 units in other depth/location (On top of a building, terminated, -250m) AKA “SATRA” Calibration Set of transmitters and passive antennas for calibration (including cable symmetrical antennas) ARENA 2010, Nantes IceCube RF extension Hagar Landsman

4 IceCube-radio hardware Fully digitized WFs
Use IceCube’s resources: holes, comm. and power Each Cluster contains: Digital Radio Module (DRM) – Electronics 4 Antennas – With front end electronics 1 Array Calibration Unit (ACU) - Transmitter Deployed above the IceCube array: “Free” Deep holes “Free” Power distribution and communication Signal conditioning and amplification happen at the front end RICE Broad band fat dipole antennas centered at 400 MHz 450 MHz Notch filter 200 MHz High pass filter (2 units with 100Mhz) ~50dB amplifiers (+~20 dB in DRM) Signal is digitized and triggers formed in DRM (a’la’ANITA) 512 samples per 256 ns (2 GSPS). Wide frequency range and multiple antennas are required for triggering surface junction box Counting house ARENA 2010, Nantes IceCube RF extension Hagar Landsman

5 ARENA 2010, Nantes IceCube RF extension Hagar Landsman
Deployment The “Big Red Box” Shipping and testing crate Going down Antennas Pressure vessels DRM Antenna cables Waiting to be deployed ARENA 2010, Nantes IceCube RF extension Hagar Landsman

6 Calibration WFs and Feature extraction
Source at surface: Source In Ice: 256 ns 256 ns Surface pulser to Doris Deep KU pulser to Doris ARENA 2010, Nantes IceCube RF extension Hagar Landsman

7 Wind generated RF noise:
Correlated with trigger rates: Correlated with power: Wind velocity (knots) Trigger rates (arbitrary) Trigger rates Wind speed Day of year Due to charge separation in drifting snow Latham, “The electrification of snow storms” (1963) New model: Gordon, Taylor (2008) : E>25 KV/m near surface ARENA 2010, Nantes IceCube RF extension Hagar Landsman

8 ARENA 2010, Nantes IceCube RF extension Hagar Landsman
Background event reconstruction Use reconstructed depth to separate background from neutrinos No quality cuts With quality cuts Comparing two reconstruction methods ARENA 2010, Nantes IceCube RF extension Hagar Landsman

9 ARENA 2010, Nantes IceCube RF extension Hagar Landsman
Effective Volume NARC was not designed to set a neutrino limit but it is something we can do preliminary RICE NARC , 2 DRMs NARC, 3 DRMs ARENA 2010, Nantes IceCube RF extension Hagar Landsman

10 ARENA 2010, Nantes IceCube RF extension Hagar Landsman
Transient detection Nick name: SATRA - (Sensor Array for Transient Radio Astrophysics) sjb DAQ box Transient detector (“SATRA”) 6 in ice units on 3 strings in holes #8, #9 and #16 1 antenna each: 2 antennas per hole. 35m and 5 m deep Each pair of antennas has a local-coincidence triggering Dry holes Log amp envelope detection 5 m 30 m satra IceCube cable See Kael Hanson’s talk later today for more on transient detection ARENA 2010, Nantes IceCube RF extension Hagar Landsman

11 ARENA 2010, Nantes IceCube RF extension Hagar Landsman
Some SATRA readouts The ultimate goal is to have each transient unit reporting a time and amplitude. This year’s design enable us to capture the envelope WF: In Ice Pulser source “Just” background WF Top WF Top amplitude amplitude WF Bottom WF Bottom time time High threshold Medium threshold Positive times= up going Negative times = down going Low thresold -200 200 -100 100 -200 -100 100 200 ARENA 2010, Nantes IceCube RF extension Hagar Landsman Dt (top – bottom) [ns] Dt (top – bottom) [ns]

12 ARENA 2010, Nantes IceCube RF extension Hagar Landsman
The mystery noise ARENA 2010, Nantes IceCube RF extension Hagar Landsman

13 ARENA 2010, Nantes IceCube RF extension Hagar Landsman
The noise source NOAA Sonde (National Oceanic and Atmospheric Administration) Model RS80-15 MHz signal Fridays only Plastic baloon (rises slower) MET Sonde Model RS92-SGP MHz Daily rubber balloons ARENA 2010, Nantes IceCube RF extension Hagar Landsman

14 In Ice Pulser As seen by SATRA
Pulser on Oh oh, one unit dead ?!?!?!?! Pulser off Trigger rate KHz Trigger rate KHz Trigger rate KHz Trigger rate KHz Trigger rate KHz Trigger rate KHz Time Time Time Time Time Time Hole 8 top Hole9 top Hole 8 bottom Hole 9 bottom Hole 16 top Hole 16 bottom ARENA 2010, Nantes IceCube RF extension Hagar Landsman No signal on one of the antennas….

15 SATRA Average envelope WFs For In Ice Pulser events
Hole 8, Bottom Hole 8, Top There is nothing here: fewer events and in lower amplitudes Hole 9, Bottom Hole 9, Top Hole 16, Bottom Hole 16, Top ARENA 2010, Nantes IceCube RF extension Hagar Landsman

16 Ice Properties: Index Of Refraction
RICE Measurements (2004, Down to 150 m, 200MHz-1GHz) Ice Core Measurements (…-1983, down to 237 meters) 1.77 Kravchenko et al. J.Glaciology, 50,171,2004 ARENA 2010, Nantes IceCube RF extension Hagar Landsman

17 Ray tracing from pulser to SATRA
Top antenna -5m surface Reflected rays Bottom antenna -35m Depth [m] Direct rays Source at -250m Measured time differences: Time differences between direct rays And between direct and reflected rays can be calculated XY separation [m] ARENA 2010, Nantes IceCube RF extension Hagar Landsman

18 SATRA Average envelope WFs For In Ice Pulser events
Hole 8, Bottom Hole 8, Top Hole 9, Bottom Hole 9, Top Hole 16, Bottom Hole 16, Top ~44 bins = ~139 ns Simulated results=137 ns Simulated results=14 ns ARENA 2010, Nantes IceCube RF extension Hagar Landsman

19 ARENA 2010, Nantes IceCube RF extension Hagar Landsman
There are 5 secondary-direct time differences on the same antenna There are 10 direct-direct time differences between different antennas dt (ns) Measured dt Model 1 Model 2 Model 3 ARENA 2010, Nantes IceCube RF extension Hagar Landsman

20 This is why this channel did not see the pulser.
30 ns 50 ns n_c n_shallow Simulated Time differences between direct hits in hole 9 bottom and top Simulated time diff between Direct & secondary ray For Bottom ant hole 16 n_c n_shallow 180 ns 140 ns 90 ns n_c n_shallow Simulated absolute travel time from pulser to top antenna, hole 8 no solution 2950 ns 2650 ns Improved Ray trace simulation (Chris Weaver) n(z) = n_d + (n_s - n_d)*en_c*z donates used variations based on RICE measurement or ice density & temperature This is why this channel did not see the pulser. It is in the invisible region due to ray tracing ARENA 2010, Nantes IceCube RF extension Hagar Landsman

21 ARENA 2010, Nantes IceCube RF extension Hagar Landsman
n_shallow n_c Based on set of hit time differences between antennas and between primary and secondary hits on the same antenna, a limit on the index of refraction model can be obtained. Systematics taken into account: n_deep, Geometry, timing resolution, WF features ARENA 2010, Nantes IceCube RF extension Hagar Landsman

22 ARENA 2010, Nantes IceCube RF extension Hagar Landsman
Summary & Future plans Several styles of Radio detectors in several depths were deployed with IceCube. Data taking is ongoing and will continue for a while (see list of ongoing analyses ) Stronger pulsers and symmetrical antennas will improve our ice properties knowledge Further investigation on timing with the transient method The next step- ARA “Askaryan Radio Array” See Kara Hoffman’s talk later today On going IceCube radio analyses Operation: Detector calibration reconstruction studies WF analysis Ice Properties: Attenuation length n(z) Birefringence Background environment: Transient and ambient noises Suitability of IceCube environment for RF studies Physics: Coincidences with IceTop array (and IceCube) GZK neutrino limits Thank you! ARENA 2010, Nantes IceCube RF extension Hagar Landsman

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