--

Contribution to the 5th International Symposium on NEUTRINO TELESCOPES

Venice March 2-41993 0 NESTOR 5

A NEUTRINO PARTICLE ASTROPHYSICS UNDERWATER LABORATORY FOR THE MEDITERRANEAN

presented by L K Resvanis representing the NESTOR Collaboration

EAnassontzis MBarone GContopoulos PHatzios Ploannou GKalkanis SKatsanevas CKourkoumelis AManousakis-Katsikakis RNicolaidou PPramantiotis LKResvanis

ISiotis GVoulgaris University ofAthens National Observatory ofAthens Demokritos NRC

HBradner University ofCalifornia San Diego and Scripps Institute ofOceanography

LDellAgnelo THong BMonteleoni VNaumov University ofFlorence and INFN

JGLearned VJStenger University ofHawaii ~ 9)

~ UKeusen PKoske IRathleu GVoigt Cb

University ofKiel ~ (t~ IFBarinov AODeineko VAGaidash MAMarkov AAPerrnyako~~~in ~

LMZakarov IMZheleznykh VAZhukov Ii i t Institute for Nuclear Research Russian Academy ofSciences

APEremeev VVLedenev MNPlatonov VKRucol NASheremet Institute ofOceanology Russian Academy ofSciences

U Camerini RMarch University ofWisconsin

A new program for an underwater neutrino astrophysics laboratory to be located in the international waters off the Southwest of Greece near the town of Pylos has now been funded for the initial stage In the last 2 years a group of physicists from Greece and Russia have carried out two demonstration experiments in 4km deep water counting muons and verifying the adequacy ofthe deep sea site Plans are presented for a 100000 m2 high energy neutrino detector composed ofa hexagon ofhexagonal towers with 1176 optical detector units A progress report is given and the physics potential of a single tower with 168 phototubes (currently under construction) is described

I hope that everyone here is a believer that neutrino astrophysics will soon become an

important part of both Elementary Particle Physics and Astrophysics Clearly the field was born

with the detection of neutrinos from supernova 1987 A by 1MB and Kamiokande Very soon

with the deployment of DlTMAND off the coast of Hawaii the detection of high energy

neutrinos will become a reality also The laboratory of Gran Sasso is a real proof of the

importance that the European Physics community gives to extraterrestrial neutrino physics but

1000m2 is the maximum sensitive area that an underground detector can have Most of us

believe that in order to get into the point astronomy with neutrinos a sensitive area of 100000m2

or more is needed the only way that one can get to these huge areas is to go deep into the water

One has to go deep (usually around 4000m deep) in order to reduce the huge cosmic ray

background (noise to signal on the earths surface of 10II) to a level that is both manageable

by fast electronics and efficient reconstruction The water is a beautiful Cerenkov medium with

a Cerenkov angle of --430 and a water transmission length that can be as good as 60 meters So

the sea water acts as I) an absorber that filters out cosmic rays II) a target with which the

neutrinos interact and III) an active detector medium which with the Cerenkov effect illuminates

large areas quite a distance away from the passage of the particles (mainly the muon) that are

produced in neutrino interactions

We believe that Europe needs its own dedicated underwater neutrino laboratory that will

extend the sensitive reach of Gran Sasso to more than a million square meters The Baltic Sea

the Black Sea and the North Sea are relatively shallow and the required depths of 4000m are

found only in the Mediterranean and the Atlantic The deep Atlantic sites are far away from

shores and good harbours a fact that gives nightmares to many of us especially when we worry

about deployment and is compounded by the high waves and the big swells that are always

present to contrast this the placid (most of the time) waters of the Mediterranean offer a haven

In fact there are two underwater plateaus in the Mediterranean with depths of 4000m or more

one off the South East coast of Rhodos and the other 75 miles South West of Sapienza near

Pylos (figl) where a little further away one finds the deepest part of the Mediterranean 5200m

This is the location we have chosen to deploy our neutrino telescope Further the Bay of

Navarino (Pylos) is a perfect testing station for underwater hardware and a good assembling area

before going out a few miles away to deploy the telescope towers

We call our projecd l ] NESTOR because we want to honour the most famous man of the

land of Pylos Nestor was the wise king of Pylos who counselled the Greeks during the Trojan

war To us now the name underlies the scientific goals of our laboratory to engage in the

detection of both low energy and high energy neutrinos so it is an acronym NEutrinos from

supernovae and Tevsources Ocean Range Although our finances right now are such that we

cannot afford to built an extragalactic supernova detector we have designed a high energy neutrino detector that is also an efficient low energy neutrino detector (in order to do

atmospheric neutrino oscillations) and still is a competitive galactic supernova detector

Site

As you can see from the chart of isobaths (fig2) we have located at a depth of 3750m a

rectangular plateau with sides of 8km 9km (at a distance of 75 nautical miles from the

lighthouse of Sapienza (where our counting room will be located) then the processed data will

be transferred from Sapienza to Pylos by either microwave link or optical fiber It is worth

emphasise that the slope of the plateau is indeed flat and horizontal its depth changes only by

100m over 9 kilometers it is also interesting to note that on a two dimensional projection our

site lies on the extrapolation of a straight line from CERN to Gran Sasso

Water Transmissivity

The water transmissivity at the depth of 3800m is the most important environmental

parameter This is why we have spent a lot of effort to measure it Basically there are three ways

of measuring it

1) taking a large number of samples (47 in our case) from different depths at various

locations in the vicinity of the deployment site and measuring the attenuation coefficient aboard

the oceanographic ship with a highly collimated monochromator spectrophotometerpound21 This

technique yielded an attenuation coefficient ranging from 025 to 045 (fig3) at 4600

Angstroms But the scattering of the light does not take light away from a water Cerenkov

experiment[3] we therefore have to correct the attenuation coefficient for scattering

Oceanographers differ in this correction[2][3] and their estimates range from 20 to 50 If you

believe the first number then the absorption length (Le the inverse of the attenuation coefficient

corrected for scattering) is somewhere between 28n1 and 50m If you believe the 50 correction

then the transmission length is between 35m and 60m In either case the water transparency is

very good

2) Taking an autonomous module[2] eg a photometer and deploying it in situ Three

such deployments were made down to depths of 4000m Since there was no reference cell one

gets relative numbers only The shape we get is consistent with the results of method 1 which

means that we understand the systematics For more details see reference 2

3) A high energy physicists way of doing the measurements ie measuring in situ the light

detected as a function of the distance between the light source and the detector Indeed such a

device was designed and built by Hugh Bradner was used for the DUMAND measurements The

advantage of this technique is that the light beam is not highly collimated so one does not have

to correct for the scattered light The same device[4] was deployed four times in the NESTOR

location and measurements gave a transmission length of 54plusmn1 Om (fig4) This result is clearly

consistent with the one described in 1 above I f one considers that the cost of the detector drops

inversely with the third power of the transmission length I can only say that we are very

fortunate to have such great water transnlission length

Underwater Currents The underwater currents in the proposed NESTOR site were measured in October 1989

JulyAugust 1991 and OctoberlNovember 92 Their values are a few cmsec truly minimal

There is a detailed presentation in a paper by Demidova[51 We will soon embark on a long term

program ofcontinuous measurement of the underwater currents in order to accumulate long term

statistics

Sedimentology

A large number of photographs of the sea bottom around the proposed site were taken

Nine core samples (almost 2 meters long) and 3 core grabs were taken also and careful

sedimentology studies were made The result is nice firm clay good anchoring ground The

detailed sedimentology study is presented in a paper by Trimonis et aH61

Deep Water Cosmic Ray Measurements In The Nestor Site

During July 1991 a collaboration of the Institute for Nuclear Research and the Institute of

Oceanology of the Russian Academy of Sciences and the University of Athens carried out a

successful cruise using the RN VITYAZ off the coast ofPylos We deployed[l] a Russian built

hexagonal structure fig 5a5b5cSd (7m radius) built out of titanium using 10 phototubes (15

inch photocathodes) facing upwards down to a depth of 4100m Six of the phototubes were

located at the comers of the hexagon and four 35 meters below the center We successfully

measured the vertical muon intensity and the angular distribution of downcoming muons As one

can see from figures 6-7 our results at 3300m 3700m and 4100m agree very well with

DUMAND I the deep mine measurements and Miyakes formula

In November 1992 we deployed[7] a linear string of five 15 inch phototubes (again the

photocathodes were facing upwards) This time the deployment was made from the Russian

research vessel Ac Mstislav Keldysh The string was deployed in depths from 3700m to

3900m the vertical intensity of cosmic ray muons and their dependence of the muon flux as a

function of the zenith angle was obtained The results are in good agreement with the previous

measurements and calculations

To summarise at depths between 3700m and 3900m the vertical flux (98plusmn40)middot 10-9

cm-2s- lsr-l The background due to radioactive K40 and water bioluminescence is 597plusmn150

photonscm2middots We note that this is an upper limit because since the phototubes were suspended

from the ship the vertical motion excites the various organisms giving very high values for the

bioluminescence compared to anchored phototubes

Basic Detector Element Omni Directional Module

Instead of using one 15 inch phototube facing down (like DUMAND) we will use two 15

inch phototubes (each in its own protective glass 1 7 inch Benthosphere) tested to 600

Atmospheres of pressure one looking up and the other looking down (fig8 detail) This way we

get a detector element with an isotropic ( 4n) response

Two Dimensional Array Element A 16m Hexagon

Six Omni-Directional Modules wiJl be placed at the corners of a horizontal hexagon and a

seventh one in its center The radius of the hexagon is planned for 16m and the arms made out

of titanium piping This design is a straightforward extension of the hexagonal autonomous

module we used during the tests off Pylos in the summer of 91 and the increase of the hexagon

radius from 7m to 16m may easily be achieved We are investigating the feasibility of

constructing titanium hexagons with 20m radius in order to increase the active detection area

Three Dimensional Element 330m Tower

By stacking hexagons we can built towers figure 8 The vertical distance between these

hexagonal floors will be around 30m this spacing matches well the light transmission length of

55mplusmn10m (at 460nm) we have measured in these waters With 30m inter-hexagonal floor

spacing and 7 phototubes from a lower hexagon looking up and 7 phototubes from a higher

hexagon looking down the active volume between hexagonal floors will be monitored

efficiently A total of 12 such hexagonal floors is planned for one tower At this moment the

number of floors is constrained to 12 by the number of optical fibers in currently commercially

available electro-optical cables for the data transmission to the shore and for the supply of

electrical power to the tower Each floor will be electrically and electronically independent from

the other floors and will have its own optical fiber for data transmission

Single Tower Sensitivity

The beauty of the water Cerenkov technique is that the detector sensitive area reaches out

quite a bit further away than the actual geometrical area of the detector Clearly the effective

area is a function of the energy of the muon In fig9 we see that for 10deg reconstruction accuracy

of the direction of a IOTeV muon the effective area is 20OOOm2 and 50OOOm2 for 103TeV

muons and 40deg reconstruction accuracy( compare this to 400m2 for 1MB and 1000m2 for

MACRO) The angular resolution along the horizontal for a single tower is of course not as

good as needed for point source astronomy simply due to the restricted lever arm Note however

that the predictions for the flux of UHE neutrinos for Active Galactic Nuclei is for a diffuse

background of neutrinos with energies up to 10 16eV so very good pointing is not needed in

order to get started

Full Detector Array eg A Hexagon or Hexagonal Towers

The need for a full 105m2 array can be satisfied with a hexagonal configuration of another

six towers deployed on the apexes of an tOOm or 150m radius hexagon centered around the

original tower fig t O Such an arrangement would provide an overall angular resolution of better

than 1deg excellent for point astronomy and sensitive area bigger than 105m2 for neutrinos of

ITeV The total cost of such an array is less than 15M$ Such a detector would have a sensitive

area ofgt 100OOOm2 angular resolution of lt to enclosed massgt 20 Megatons and would almost

certainly be able to begin the field of high energy neutrino point source astronomy

Off course the possibilities do not stop at 105m2The bcaty of the deep approach is the

potential for following the physics as one gains cxpericnce and first looks at the dataA bigger

detector is obviously possiblcfls are configurations that maximisc low energy sensitivity or

tune on any particular facet of the science that may prove worth pursuing

The Physics Potential Of Nestor With Only One Tower

There is a multitude of existing physics that wc can do with one NESTOR towerwhile

waiting for the events of extratcrrestrial origin to corne in These include atmospheric neushy

trino oscillations long baseline oscillations with CERN (perhaps in conjuction with a deshy

tector at Grand Sasso)

Atmospheric neutrino oscillations

The subject of neutrino oscillations first suggested by Pontecorvo has been a topic of

intense interest for more than 15 years For somc rccent rcviews sce [8) If neutrino oscillations

occur in their simplest form assulning a two flavor oscillation the probability of oscillation

IS

(1)

where dn2 = m~ - m~ is the difference of the nlass eig~nvalLies in eV2 0 is the two flavor

mixing angle L is the v propagation length in Kitorneters and El is the neutrino energy in

GeV

Recent results by the J(AMIOI(A 111D and SUDAN2 collaborations suggest that pershy

haps as much as 40 of the atmospheric lIevents in the encrgy range from 02-15 GeV

have oscillated to some other type of ncutrino (9)(10)[11) Othcr less sensitive experiments

did not record any effect [12] NESTOR will be able to tcst by studying atmospheric neutrino

oscillations at a higher energy legitne ( above 5 Ge V) The higher energy regime diminishes

the dependence of the study on geomagnetic cffccts and on the uncertainties of the Oxyshy

gen cross section and other nuclear effectsThe NESTOIt design is such that the top floors

can be used to veto downcoming cosmic raysTherefore we can he sensitive to neutrinos

arriving from a1l zenith anglesThis way ollr L dependence varicfol from 101ltm to 13000kln

giving NESTOR an unprecedented sensitivity in ~fn2 spanning four orders of magnitude

Further since we intend to study the oscil1atiotls as a disappcarence experiment that is by

nlcasllring the ratio of rnnons coming fron1 dirrclcnt 7-clIith anglcs we will be independent

from theoretical flux predictions which currently arc the source of considerable systematic

uncertainties in I(AMIOKA 111n and SUDAN20ur cXperill1Cnt win be internally normalshy

isable ie comparing the expected nUlnber of neutrinos coming frOin all directions to anyone

we choose to use as the control direction this way Jl1oltiulo solid angle effects the number of

muonlike neutrinos should be constant as a function of zenith if tJICIC is a decrease it would

be caused uniquely by neutrino oscillations ie JnuonJike neutrino oscillations to another

1000m2 is the maximum sensitive area that an underground detector can have Most of us

believe that in order to get into the point astronomy with neutrinos a sensitive area of 100000m2

or more is needed the only way that one can get to these huge areas is to go deep into the water

One has to go deep (usually around 4000m deep) in order to reduce the huge cosmic ray

background (noise to signal on the earths surface of 10II) to a level that is both manageable

by fast electronics and efficient reconstruction The water is a beautiful Cerenkov medium with

a Cerenkov angle of --430 and a water transmission length that can be as good as 60 meters So

the sea water acts as I) an absorber that filters out cosmic rays II) a target with which the

neutrinos interact and III) an active detector medium which with the Cerenkov effect illuminates

large areas quite a distance away from the passage of the particles (mainly the muon) that are

produced in neutrino interactions

We believe that Europe needs its own dedicated underwater neutrino laboratory that will

extend the sensitive reach of Gran Sasso to more than a million square meters The Baltic Sea

the Black Sea and the North Sea are relatively shallow and the required depths of 4000m are

found only in the Mediterranean and the Atlantic The deep Atlantic sites are far away from

shores and good harbours a fact that gives nightmares to many of us especially when we worry

about deployment and is compounded by the high waves and the big swells that are always

present to contrast this the placid (most of the time) waters of the Mediterranean offer a haven

In fact there are two underwater plateaus in the Mediterranean with depths of 4000m or more

one off the South East coast of Rhodos and the other 75 miles South West of Sapienza near

Pylos (figl) where a little further away one finds the deepest part of the Mediterranean 5200m

This is the location we have chosen to deploy our neutrino telescope Further the Bay of

Navarino (Pylos) is a perfect testing station for underwater hardware and a good assembling area

before going out a few miles away to deploy the telescope towers

We call our projecd l ] NESTOR because we want to honour the most famous man of the

land of Pylos Nestor was the wise king of Pylos who counselled the Greeks during the Trojan

war To us now the name underlies the scientific goals of our laboratory to engage in the

detection of both low energy and high energy neutrinos so it is an acronym NEutrinos from

supernovae and Tevsources Ocean Range Although our finances right now are such that we

cannot afford to built an extragalactic supernova detector we have designed a high energy neutrino detector that is also an efficient low energy neutrino detector (in order to do

atmospheric neutrino oscillations) and still is a competitive galactic supernova detector

Site

As you can see from the chart of isobaths (fig2) we have located at a depth of 3750m a

rectangular plateau with sides of 8km 9km (at a distance of 75 nautical miles from the

lighthouse of Sapienza (where our counting room will be located) then the processed data will

be transferred from Sapienza to Pylos by either microwave link or optical fiber It is worth

emphasise that the slope of the plateau is indeed flat and horizontal its depth changes only by

100m over 9 kilometers it is also interesting to note that on a two dimensional projection our

site lies on the extrapolation of a straight line from CERN to Gran Sasso

Water Transmissivity

The water transmissivity at the depth of 3800m is the most important environmental

parameter This is why we have spent a lot of effort to measure it Basically there are three ways

of measuring it

1) taking a large number of samples (47 in our case) from different depths at various

locations in the vicinity of the deployment site and measuring the attenuation coefficient aboard

the oceanographic ship with a highly collimated monochromator spectrophotometerpound21 This

technique yielded an attenuation coefficient ranging from 025 to 045 (fig3) at 4600

Angstroms But the scattering of the light does not take light away from a water Cerenkov

experiment[3] we therefore have to correct the attenuation coefficient for scattering

Oceanographers differ in this correction[2][3] and their estimates range from 20 to 50 If you

believe the first number then the absorption length (Le the inverse of the attenuation coefficient

corrected for scattering) is somewhere between 28n1 and 50m If you believe the 50 correction

then the transmission length is between 35m and 60m In either case the water transparency is

very good

2) Taking an autonomous module[2] eg a photometer and deploying it in situ Three

such deployments were made down to depths of 4000m Since there was no reference cell one

gets relative numbers only The shape we get is consistent with the results of method 1 which

means that we understand the systematics For more details see reference 2

3) A high energy physicists way of doing the measurements ie measuring in situ the light

detected as a function of the distance between the light source and the detector Indeed such a

device was designed and built by Hugh Bradner was used for the DUMAND measurements The

advantage of this technique is that the light beam is not highly collimated so one does not have

to correct for the scattered light The same device[4] was deployed four times in the NESTOR

location and measurements gave a transmission length of 54plusmn1 Om (fig4) This result is clearly

consistent with the one described in 1 above I f one considers that the cost of the detector drops

inversely with the third power of the transmission length I can only say that we are very

fortunate to have such great water transnlission length

Underwater Currents The underwater currents in the proposed NESTOR site were measured in October 1989

JulyAugust 1991 and OctoberlNovember 92 Their values are a few cmsec truly minimal

There is a detailed presentation in a paper by Demidova[51 We will soon embark on a long term

program ofcontinuous measurement of the underwater currents in order to accumulate long term

statistics

Sedimentology

A large number of photographs of the sea bottom around the proposed site were taken

Nine core samples (almost 2 meters long) and 3 core grabs were taken also and careful

sedimentology studies were made The result is nice firm clay good anchoring ground The

detailed sedimentology study is presented in a paper by Trimonis et aH61

Deep Water Cosmic Ray Measurements In The Nestor Site

During July 1991 a collaboration of the Institute for Nuclear Research and the Institute of

Oceanology of the Russian Academy of Sciences and the University of Athens carried out a

successful cruise using the RN VITYAZ off the coast ofPylos We deployed[l] a Russian built

hexagonal structure fig 5a5b5cSd (7m radius) built out of titanium using 10 phototubes (15

inch photocathodes) facing upwards down to a depth of 4100m Six of the phototubes were

located at the comers of the hexagon and four 35 meters below the center We successfully

measured the vertical muon intensity and the angular distribution of downcoming muons As one

can see from figures 6-7 our results at 3300m 3700m and 4100m agree very well with

DUMAND I the deep mine measurements and Miyakes formula

In November 1992 we deployed[7] a linear string of five 15 inch phototubes (again the

photocathodes were facing upwards) This time the deployment was made from the Russian

research vessel Ac Mstislav Keldysh The string was deployed in depths from 3700m to

3900m the vertical intensity of cosmic ray muons and their dependence of the muon flux as a

function of the zenith angle was obtained The results are in good agreement with the previous

measurements and calculations

To summarise at depths between 3700m and 3900m the vertical flux (98plusmn40)middot 10-9

cm-2s- lsr-l The background due to radioactive K40 and water bioluminescence is 597plusmn150

photonscm2middots We note that this is an upper limit because since the phototubes were suspended

from the ship the vertical motion excites the various organisms giving very high values for the

bioluminescence compared to anchored phototubes

Basic Detector Element Omni Directional Module

Instead of using one 15 inch phototube facing down (like DUMAND) we will use two 15

inch phototubes (each in its own protective glass 1 7 inch Benthosphere) tested to 600

Atmospheres of pressure one looking up and the other looking down (fig8 detail) This way we

get a detector element with an isotropic ( 4n) response

Two Dimensional Array Element A 16m Hexagon

Six Omni-Directional Modules wiJl be placed at the corners of a horizontal hexagon and a

seventh one in its center The radius of the hexagon is planned for 16m and the arms made out

of titanium piping This design is a straightforward extension of the hexagonal autonomous

module we used during the tests off Pylos in the summer of 91 and the increase of the hexagon

radius from 7m to 16m may easily be achieved We are investigating the feasibility of

constructing titanium hexagons with 20m radius in order to increase the active detection area

Three Dimensional Element 330m Tower

By stacking hexagons we can built towers figure 8 The vertical distance between these

hexagonal floors will be around 30m this spacing matches well the light transmission length of

55mplusmn10m (at 460nm) we have measured in these waters With 30m inter-hexagonal floor

spacing and 7 phototubes from a lower hexagon looking up and 7 phototubes from a higher

hexagon looking down the active volume between hexagonal floors will be monitored

efficiently A total of 12 such hexagonal floors is planned for one tower At this moment the

number of floors is constrained to 12 by the number of optical fibers in currently commercially

available electro-optical cables for the data transmission to the shore and for the supply of

electrical power to the tower Each floor will be electrically and electronically independent from

the other floors and will have its own optical fiber for data transmission

Single Tower Sensitivity

The beauty of the water Cerenkov technique is that the detector sensitive area reaches out

quite a bit further away than the actual geometrical area of the detector Clearly the effective

area is a function of the energy of the muon In fig9 we see that for 10deg reconstruction accuracy

of the direction of a IOTeV muon the effective area is 20OOOm2 and 50OOOm2 for 103TeV

muons and 40deg reconstruction accuracy( compare this to 400m2 for 1MB and 1000m2 for

MACRO) The angular resolution along the horizontal for a single tower is of course not as

good as needed for point source astronomy simply due to the restricted lever arm Note however

that the predictions for the flux of UHE neutrinos for Active Galactic Nuclei is for a diffuse

background of neutrinos with energies up to 10 16eV so very good pointing is not needed in

order to get started

Full Detector Array eg A Hexagon or Hexagonal Towers

The need for a full 105m2 array can be satisfied with a hexagonal configuration of another

six towers deployed on the apexes of an tOOm or 150m radius hexagon centered around the

original tower fig t O Such an arrangement would provide an overall angular resolution of better

than 1deg excellent for point astronomy and sensitive area bigger than 105m2 for neutrinos of

ITeV The total cost of such an array is less than 15M$ Such a detector would have a sensitive

area ofgt 100OOOm2 angular resolution of lt to enclosed massgt 20 Megatons and would almost

certainly be able to begin the field of high energy neutrino point source astronomy

Off course the possibilities do not stop at 105m2The bcaty of the deep approach is the

potential for following the physics as one gains cxpericnce and first looks at the dataA bigger

detector is obviously possiblcfls are configurations that maximisc low energy sensitivity or

tune on any particular facet of the science that may prove worth pursuing

The Physics Potential Of Nestor With Only One Tower

There is a multitude of existing physics that wc can do with one NESTOR towerwhile

waiting for the events of extratcrrestrial origin to corne in These include atmospheric neushy

trino oscillations long baseline oscillations with CERN (perhaps in conjuction with a deshy

tector at Grand Sasso)

Atmospheric neutrino oscillations

The subject of neutrino oscillations first suggested by Pontecorvo has been a topic of

intense interest for more than 15 years For somc rccent rcviews sce [8) If neutrino oscillations

occur in their simplest form assulning a two flavor oscillation the probability of oscillation

IS

(1)

where dn2 = m~ - m~ is the difference of the nlass eig~nvalLies in eV2 0 is the two flavor

mixing angle L is the v propagation length in Kitorneters and El is the neutrino energy in

GeV

Recent results by the J(AMIOI(A 111D and SUDAN2 collaborations suggest that pershy

haps as much as 40 of the atmospheric lIevents in the encrgy range from 02-15 GeV

have oscillated to some other type of ncutrino (9)(10)[11) Othcr less sensitive experiments

did not record any effect [12] NESTOR will be able to tcst by studying atmospheric neutrino

oscillations at a higher energy legitne ( above 5 Ge V) The higher energy regime diminishes

the dependence of the study on geomagnetic cffccts and on the uncertainties of the Oxyshy

gen cross section and other nuclear effectsThe NESTOIt design is such that the top floors

can be used to veto downcoming cosmic raysTherefore we can he sensitive to neutrinos

arriving from a1l zenith anglesThis way ollr L dependence varicfol from 101ltm to 13000kln

giving NESTOR an unprecedented sensitivity in ~fn2 spanning four orders of magnitude

Further since we intend to study the oscil1atiotls as a disappcarence experiment that is by

nlcasllring the ratio of rnnons coming fron1 dirrclcnt 7-clIith anglcs we will be independent

from theoretical flux predictions which currently arc the source of considerable systematic

uncertainties in I(AMIOKA 111n and SUDAN20ur cXperill1Cnt win be internally normalshy

isable ie comparing the expected nUlnber of neutrinos coming frOin all directions to anyone

we choose to use as the control direction this way Jl1oltiulo solid angle effects the number of

muonlike neutrinos should be constant as a function of zenith if tJICIC is a decrease it would

be caused uniquely by neutrino oscillations ie JnuonJike neutrino oscillations to another

emphasise that the slope of the plateau is indeed flat and horizontal its depth changes only by

100m over 9 kilometers it is also interesting to note that on a two dimensional projection our

site lies on the extrapolation of a straight line from CERN to Gran Sasso

Water Transmissivity

The water transmissivity at the depth of 3800m is the most important environmental

parameter This is why we have spent a lot of effort to measure it Basically there are three ways

of measuring it

1) taking a large number of samples (47 in our case) from different depths at various

locations in the vicinity of the deployment site and measuring the attenuation coefficient aboard

the oceanographic ship with a highly collimated monochromator spectrophotometerpound21 This

technique yielded an attenuation coefficient ranging from 025 to 045 (fig3) at 4600

Angstroms But the scattering of the light does not take light away from a water Cerenkov

experiment[3] we therefore have to correct the attenuation coefficient for scattering

Oceanographers differ in this correction[2][3] and their estimates range from 20 to 50 If you

believe the first number then the absorption length (Le the inverse of the attenuation coefficient

corrected for scattering) is somewhere between 28n1 and 50m If you believe the 50 correction

then the transmission length is between 35m and 60m In either case the water transparency is

very good

2) Taking an autonomous module[2] eg a photometer and deploying it in situ Three

such deployments were made down to depths of 4000m Since there was no reference cell one

gets relative numbers only The shape we get is consistent with the results of method 1 which

means that we understand the systematics For more details see reference 2

3) A high energy physicists way of doing the measurements ie measuring in situ the light

detected as a function of the distance between the light source and the detector Indeed such a

device was designed and built by Hugh Bradner was used for the DUMAND measurements The

advantage of this technique is that the light beam is not highly collimated so one does not have

to correct for the scattered light The same device[4] was deployed four times in the NESTOR

location and measurements gave a transmission length of 54plusmn1 Om (fig4) This result is clearly

consistent with the one described in 1 above I f one considers that the cost of the detector drops

inversely with the third power of the transmission length I can only say that we are very

fortunate to have such great water transnlission length

Underwater Currents The underwater currents in the proposed NESTOR site were measured in October 1989

JulyAugust 1991 and OctoberlNovember 92 Their values are a few cmsec truly minimal

There is a detailed presentation in a paper by Demidova[51 We will soon embark on a long term

program ofcontinuous measurement of the underwater currents in order to accumulate long term

statistics

Sedimentology

A large number of photographs of the sea bottom around the proposed site were taken

Nine core samples (almost 2 meters long) and 3 core grabs were taken also and careful

sedimentology studies were made The result is nice firm clay good anchoring ground The

detailed sedimentology study is presented in a paper by Trimonis et aH61

Deep Water Cosmic Ray Measurements In The Nestor Site

During July 1991 a collaboration of the Institute for Nuclear Research and the Institute of

Oceanology of the Russian Academy of Sciences and the University of Athens carried out a

successful cruise using the RN VITYAZ off the coast ofPylos We deployed[l] a Russian built

hexagonal structure fig 5a5b5cSd (7m radius) built out of titanium using 10 phototubes (15

inch photocathodes) facing upwards down to a depth of 4100m Six of the phototubes were

located at the comers of the hexagon and four 35 meters below the center We successfully

measured the vertical muon intensity and the angular distribution of downcoming muons As one

can see from figures 6-7 our results at 3300m 3700m and 4100m agree very well with

DUMAND I the deep mine measurements and Miyakes formula

In November 1992 we deployed[7] a linear string of five 15 inch phototubes (again the

photocathodes were facing upwards) This time the deployment was made from the Russian

research vessel Ac Mstislav Keldysh The string was deployed in depths from 3700m to

3900m the vertical intensity of cosmic ray muons and their dependence of the muon flux as a

function of the zenith angle was obtained The results are in good agreement with the previous

measurements and calculations

To summarise at depths between 3700m and 3900m the vertical flux (98plusmn40)middot 10-9

cm-2s- lsr-l The background due to radioactive K40 and water bioluminescence is 597plusmn150

photonscm2middots We note that this is an upper limit because since the phototubes were suspended

from the ship the vertical motion excites the various organisms giving very high values for the

bioluminescence compared to anchored phototubes

Basic Detector Element Omni Directional Module

Instead of using one 15 inch phototube facing down (like DUMAND) we will use two 15

inch phototubes (each in its own protective glass 1 7 inch Benthosphere) tested to 600

Atmospheres of pressure one looking up and the other looking down (fig8 detail) This way we

get a detector element with an isotropic ( 4n) response

Two Dimensional Array Element A 16m Hexagon

Six Omni-Directional Modules wiJl be placed at the corners of a horizontal hexagon and a

seventh one in its center The radius of the hexagon is planned for 16m and the arms made out

of titanium piping This design is a straightforward extension of the hexagonal autonomous

module we used during the tests off Pylos in the summer of 91 and the increase of the hexagon

radius from 7m to 16m may easily be achieved We are investigating the feasibility of

constructing titanium hexagons with 20m radius in order to increase the active detection area

Three Dimensional Element 330m Tower

By stacking hexagons we can built towers figure 8 The vertical distance between these

hexagonal floors will be around 30m this spacing matches well the light transmission length of

55mplusmn10m (at 460nm) we have measured in these waters With 30m inter-hexagonal floor

spacing and 7 phototubes from a lower hexagon looking up and 7 phototubes from a higher

hexagon looking down the active volume between hexagonal floors will be monitored

efficiently A total of 12 such hexagonal floors is planned for one tower At this moment the

number of floors is constrained to 12 by the number of optical fibers in currently commercially

available electro-optical cables for the data transmission to the shore and for the supply of

electrical power to the tower Each floor will be electrically and electronically independent from

the other floors and will have its own optical fiber for data transmission

Single Tower Sensitivity

The beauty of the water Cerenkov technique is that the detector sensitive area reaches out

quite a bit further away than the actual geometrical area of the detector Clearly the effective

area is a function of the energy of the muon In fig9 we see that for 10deg reconstruction accuracy

of the direction of a IOTeV muon the effective area is 20OOOm2 and 50OOOm2 for 103TeV

muons and 40deg reconstruction accuracy( compare this to 400m2 for 1MB and 1000m2 for

MACRO) The angular resolution along the horizontal for a single tower is of course not as

good as needed for point source astronomy simply due to the restricted lever arm Note however

that the predictions for the flux of UHE neutrinos for Active Galactic Nuclei is for a diffuse

background of neutrinos with energies up to 10 16eV so very good pointing is not needed in

order to get started

Full Detector Array eg A Hexagon or Hexagonal Towers

The need for a full 105m2 array can be satisfied with a hexagonal configuration of another

six towers deployed on the apexes of an tOOm or 150m radius hexagon centered around the

original tower fig t O Such an arrangement would provide an overall angular resolution of better

than 1deg excellent for point astronomy and sensitive area bigger than 105m2 for neutrinos of

ITeV The total cost of such an array is less than 15M$ Such a detector would have a sensitive

area ofgt 100OOOm2 angular resolution of lt to enclosed massgt 20 Megatons and would almost

certainly be able to begin the field of high energy neutrino point source astronomy

Off course the possibilities do not stop at 105m2The bcaty of the deep approach is the

potential for following the physics as one gains cxpericnce and first looks at the dataA bigger

detector is obviously possiblcfls are configurations that maximisc low energy sensitivity or

tune on any particular facet of the science that may prove worth pursuing

The Physics Potential Of Nestor With Only One Tower

There is a multitude of existing physics that wc can do with one NESTOR towerwhile

waiting for the events of extratcrrestrial origin to corne in These include atmospheric neushy

trino oscillations long baseline oscillations with CERN (perhaps in conjuction with a deshy

tector at Grand Sasso)

Atmospheric neutrino oscillations

The subject of neutrino oscillations first suggested by Pontecorvo has been a topic of

intense interest for more than 15 years For somc rccent rcviews sce [8) If neutrino oscillations

occur in their simplest form assulning a two flavor oscillation the probability of oscillation

IS

(1)

where dn2 = m~ - m~ is the difference of the nlass eig~nvalLies in eV2 0 is the two flavor

mixing angle L is the v propagation length in Kitorneters and El is the neutrino energy in

GeV

Recent results by the J(AMIOI(A 111D and SUDAN2 collaborations suggest that pershy

haps as much as 40 of the atmospheric lIevents in the encrgy range from 02-15 GeV

have oscillated to some other type of ncutrino (9)(10)[11) Othcr less sensitive experiments

did not record any effect [12] NESTOR will be able to tcst by studying atmospheric neutrino

oscillations at a higher energy legitne ( above 5 Ge V) The higher energy regime diminishes

the dependence of the study on geomagnetic cffccts and on the uncertainties of the Oxyshy

gen cross section and other nuclear effectsThe NESTOIt design is such that the top floors

can be used to veto downcoming cosmic raysTherefore we can he sensitive to neutrinos

arriving from a1l zenith anglesThis way ollr L dependence varicfol from 101ltm to 13000kln

giving NESTOR an unprecedented sensitivity in ~fn2 spanning four orders of magnitude

Further since we intend to study the oscil1atiotls as a disappcarence experiment that is by

nlcasllring the ratio of rnnons coming fron1 dirrclcnt 7-clIith anglcs we will be independent

from theoretical flux predictions which currently arc the source of considerable systematic

uncertainties in I(AMIOKA 111n and SUDAN20ur cXperill1Cnt win be internally normalshy

isable ie comparing the expected nUlnber of neutrinos coming frOin all directions to anyone

we choose to use as the control direction this way Jl1oltiulo solid angle effects the number of

muonlike neutrinos should be constant as a function of zenith if tJICIC is a decrease it would

be caused uniquely by neutrino oscillations ie JnuonJike neutrino oscillations to another

statistics

Sedimentology

A large number of photographs of the sea bottom around the proposed site were taken

Nine core samples (almost 2 meters long) and 3 core grabs were taken also and careful

sedimentology studies were made The result is nice firm clay good anchoring ground The

detailed sedimentology study is presented in a paper by Trimonis et aH61

Deep Water Cosmic Ray Measurements In The Nestor Site

During July 1991 a collaboration of the Institute for Nuclear Research and the Institute of

Oceanology of the Russian Academy of Sciences and the University of Athens carried out a

successful cruise using the RN VITYAZ off the coast ofPylos We deployed[l] a Russian built

hexagonal structure fig 5a5b5cSd (7m radius) built out of titanium using 10 phototubes (15

inch photocathodes) facing upwards down to a depth of 4100m Six of the phototubes were

located at the comers of the hexagon and four 35 meters below the center We successfully

measured the vertical muon intensity and the angular distribution of downcoming muons As one

can see from figures 6-7 our results at 3300m 3700m and 4100m agree very well with

DUMAND I the deep mine measurements and Miyakes formula

In November 1992 we deployed[7] a linear string of five 15 inch phototubes (again the

photocathodes were facing upwards) This time the deployment was made from the Russian

research vessel Ac Mstislav Keldysh The string was deployed in depths from 3700m to

3900m the vertical intensity of cosmic ray muons and their dependence of the muon flux as a

function of the zenith angle was obtained The results are in good agreement with the previous

measurements and calculations

To summarise at depths between 3700m and 3900m the vertical flux (98plusmn40)middot 10-9

cm-2s- lsr-l The background due to radioactive K40 and water bioluminescence is 597plusmn150

photonscm2middots We note that this is an upper limit because since the phototubes were suspended

from the ship the vertical motion excites the various organisms giving very high values for the

bioluminescence compared to anchored phototubes

Basic Detector Element Omni Directional Module

Instead of using one 15 inch phototube facing down (like DUMAND) we will use two 15

inch phototubes (each in its own protective glass 1 7 inch Benthosphere) tested to 600

Atmospheres of pressure one looking up and the other looking down (fig8 detail) This way we

get a detector element with an isotropic ( 4n) response

Two Dimensional Array Element A 16m Hexagon

Six Omni-Directional Modules wiJl be placed at the corners of a horizontal hexagon and a

seventh one in its center The radius of the hexagon is planned for 16m and the arms made out

of titanium piping This design is a straightforward extension of the hexagonal autonomous

module we used during the tests off Pylos in the summer of 91 and the increase of the hexagon

radius from 7m to 16m may easily be achieved We are investigating the feasibility of

constructing titanium hexagons with 20m radius in order to increase the active detection area

Three Dimensional Element 330m Tower

By stacking hexagons we can built towers figure 8 The vertical distance between these

hexagonal floors will be around 30m this spacing matches well the light transmission length of

55mplusmn10m (at 460nm) we have measured in these waters With 30m inter-hexagonal floor

spacing and 7 phototubes from a lower hexagon looking up and 7 phototubes from a higher

hexagon looking down the active volume between hexagonal floors will be monitored

efficiently A total of 12 such hexagonal floors is planned for one tower At this moment the

number of floors is constrained to 12 by the number of optical fibers in currently commercially

available electro-optical cables for the data transmission to the shore and for the supply of

electrical power to the tower Each floor will be electrically and electronically independent from

the other floors and will have its own optical fiber for data transmission

Single Tower Sensitivity

The beauty of the water Cerenkov technique is that the detector sensitive area reaches out

quite a bit further away than the actual geometrical area of the detector Clearly the effective

area is a function of the energy of the muon In fig9 we see that for 10deg reconstruction accuracy

of the direction of a IOTeV muon the effective area is 20OOOm2 and 50OOOm2 for 103TeV

muons and 40deg reconstruction accuracy( compare this to 400m2 for 1MB and 1000m2 for

MACRO) The angular resolution along the horizontal for a single tower is of course not as

good as needed for point source astronomy simply due to the restricted lever arm Note however

that the predictions for the flux of UHE neutrinos for Active Galactic Nuclei is for a diffuse

background of neutrinos with energies up to 10 16eV so very good pointing is not needed in

order to get started

Full Detector Array eg A Hexagon or Hexagonal Towers

The need for a full 105m2 array can be satisfied with a hexagonal configuration of another

six towers deployed on the apexes of an tOOm or 150m radius hexagon centered around the

original tower fig t O Such an arrangement would provide an overall angular resolution of better

than 1deg excellent for point astronomy and sensitive area bigger than 105m2 for neutrinos of

ITeV The total cost of such an array is less than 15M$ Such a detector would have a sensitive

area ofgt 100OOOm2 angular resolution of lt to enclosed massgt 20 Megatons and would almost

certainly be able to begin the field of high energy neutrino point source astronomy

Off course the possibilities do not stop at 105m2The bcaty of the deep approach is the

potential for following the physics as one gains cxpericnce and first looks at the dataA bigger

detector is obviously possiblcfls are configurations that maximisc low energy sensitivity or

tune on any particular facet of the science that may prove worth pursuing

The Physics Potential Of Nestor With Only One Tower

There is a multitude of existing physics that wc can do with one NESTOR towerwhile

waiting for the events of extratcrrestrial origin to corne in These include atmospheric neushy

trino oscillations long baseline oscillations with CERN (perhaps in conjuction with a deshy

tector at Grand Sasso)

Atmospheric neutrino oscillations

The subject of neutrino oscillations first suggested by Pontecorvo has been a topic of

intense interest for more than 15 years For somc rccent rcviews sce [8) If neutrino oscillations

occur in their simplest form assulning a two flavor oscillation the probability of oscillation

IS

(1)

where dn2 = m~ - m~ is the difference of the nlass eig~nvalLies in eV2 0 is the two flavor

mixing angle L is the v propagation length in Kitorneters and El is the neutrino energy in

GeV

Recent results by the J(AMIOI(A 111D and SUDAN2 collaborations suggest that pershy

haps as much as 40 of the atmospheric lIevents in the encrgy range from 02-15 GeV

have oscillated to some other type of ncutrino (9)(10)[11) Othcr less sensitive experiments

did not record any effect [12] NESTOR will be able to tcst by studying atmospheric neutrino

oscillations at a higher energy legitne ( above 5 Ge V) The higher energy regime diminishes

the dependence of the study on geomagnetic cffccts and on the uncertainties of the Oxyshy

gen cross section and other nuclear effectsThe NESTOIt design is such that the top floors

can be used to veto downcoming cosmic raysTherefore we can he sensitive to neutrinos

arriving from a1l zenith anglesThis way ollr L dependence varicfol from 101ltm to 13000kln

giving NESTOR an unprecedented sensitivity in ~fn2 spanning four orders of magnitude

Further since we intend to study the oscil1atiotls as a disappcarence experiment that is by

nlcasllring the ratio of rnnons coming fron1 dirrclcnt 7-clIith anglcs we will be independent

from theoretical flux predictions which currently arc the source of considerable systematic

uncertainties in I(AMIOKA 111n and SUDAN20ur cXperill1Cnt win be internally normalshy

isable ie comparing the expected nUlnber of neutrinos coming frOin all directions to anyone

we choose to use as the control direction this way Jl1oltiulo solid angle effects the number of

muonlike neutrinos should be constant as a function of zenith if tJICIC is a decrease it would

be caused uniquely by neutrino oscillations ie JnuonJike neutrino oscillations to another

seventh one in its center The radius of the hexagon is planned for 16m and the arms made out

of titanium piping This design is a straightforward extension of the hexagonal autonomous

module we used during the tests off Pylos in the summer of 91 and the increase of the hexagon

radius from 7m to 16m may easily be achieved We are investigating the feasibility of

constructing titanium hexagons with 20m radius in order to increase the active detection area

Three Dimensional Element 330m Tower

By stacking hexagons we can built towers figure 8 The vertical distance between these

hexagonal floors will be around 30m this spacing matches well the light transmission length of

55mplusmn10m (at 460nm) we have measured in these waters With 30m inter-hexagonal floor

spacing and 7 phototubes from a lower hexagon looking up and 7 phototubes from a higher

hexagon looking down the active volume between hexagonal floors will be monitored

efficiently A total of 12 such hexagonal floors is planned for one tower At this moment the

number of floors is constrained to 12 by the number of optical fibers in currently commercially

available electro-optical cables for the data transmission to the shore and for the supply of

electrical power to the tower Each floor will be electrically and electronically independent from

the other floors and will have its own optical fiber for data transmission

Single Tower Sensitivity

The beauty of the water Cerenkov technique is that the detector sensitive area reaches out

quite a bit further away than the actual geometrical area of the detector Clearly the effective

area is a function of the energy of the muon In fig9 we see that for 10deg reconstruction accuracy

of the direction of a IOTeV muon the effective area is 20OOOm2 and 50OOOm2 for 103TeV

muons and 40deg reconstruction accuracy( compare this to 400m2 for 1MB and 1000m2 for

MACRO) The angular resolution along the horizontal for a single tower is of course not as

good as needed for point source astronomy simply due to the restricted lever arm Note however

that the predictions for the flux of UHE neutrinos for Active Galactic Nuclei is for a diffuse

background of neutrinos with energies up to 10 16eV so very good pointing is not needed in

order to get started

Full Detector Array eg A Hexagon or Hexagonal Towers

The need for a full 105m2 array can be satisfied with a hexagonal configuration of another

six towers deployed on the apexes of an tOOm or 150m radius hexagon centered around the

original tower fig t O Such an arrangement would provide an overall angular resolution of better

than 1deg excellent for point astronomy and sensitive area bigger than 105m2 for neutrinos of

ITeV The total cost of such an array is less than 15M$ Such a detector would have a sensitive

area ofgt 100OOOm2 angular resolution of lt to enclosed massgt 20 Megatons and would almost

certainly be able to begin the field of high energy neutrino point source astronomy

Off course the possibilities do not stop at 105m2The bcaty of the deep approach is the

potential for following the physics as one gains cxpericnce and first looks at the dataA bigger

detector is obviously possiblcfls are configurations that maximisc low energy sensitivity or

tune on any particular facet of the science that may prove worth pursuing

The Physics Potential Of Nestor With Only One Tower

There is a multitude of existing physics that wc can do with one NESTOR towerwhile

waiting for the events of extratcrrestrial origin to corne in These include atmospheric neushy

trino oscillations long baseline oscillations with CERN (perhaps in conjuction with a deshy

tector at Grand Sasso)

Atmospheric neutrino oscillations

The subject of neutrino oscillations first suggested by Pontecorvo has been a topic of

intense interest for more than 15 years For somc rccent rcviews sce [8) If neutrino oscillations

occur in their simplest form assulning a two flavor oscillation the probability of oscillation

IS

(1)

where dn2 = m~ - m~ is the difference of the nlass eig~nvalLies in eV2 0 is the two flavor

mixing angle L is the v propagation length in Kitorneters and El is the neutrino energy in

GeV

Recent results by the J(AMIOI(A 111D and SUDAN2 collaborations suggest that pershy

haps as much as 40 of the atmospheric lIevents in the encrgy range from 02-15 GeV

have oscillated to some other type of ncutrino (9)(10)[11) Othcr less sensitive experiments

did not record any effect [12] NESTOR will be able to tcst by studying atmospheric neutrino

oscillations at a higher energy legitne ( above 5 Ge V) The higher energy regime diminishes

the dependence of the study on geomagnetic cffccts and on the uncertainties of the Oxyshy

gen cross section and other nuclear effectsThe NESTOIt design is such that the top floors

can be used to veto downcoming cosmic raysTherefore we can he sensitive to neutrinos

arriving from a1l zenith anglesThis way ollr L dependence varicfol from 101ltm to 13000kln

giving NESTOR an unprecedented sensitivity in ~fn2 spanning four orders of magnitude

Further since we intend to study the oscil1atiotls as a disappcarence experiment that is by

nlcasllring the ratio of rnnons coming fron1 dirrclcnt 7-clIith anglcs we will be independent

from theoretical flux predictions which currently arc the source of considerable systematic

uncertainties in I(AMIOKA 111n and SUDAN20ur cXperill1Cnt win be internally normalshy

isable ie comparing the expected nUlnber of neutrinos coming frOin all directions to anyone

we choose to use as the control direction this way Jl1oltiulo solid angle effects the number of

muonlike neutrinos should be constant as a function of zenith if tJICIC is a decrease it would

be caused uniquely by neutrino oscillations ie JnuonJike neutrino oscillations to another

Off course the possibilities do not stop at 105m2The bcaty of the deep approach is the

potential for following the physics as one gains cxpericnce and first looks at the dataA bigger

detector is obviously possiblcfls are configurations that maximisc low energy sensitivity or

tune on any particular facet of the science that may prove worth pursuing

The Physics Potential Of Nestor With Only One Tower

There is a multitude of existing physics that wc can do with one NESTOR towerwhile

waiting for the events of extratcrrestrial origin to corne in These include atmospheric neushy

trino oscillations long baseline oscillations with CERN (perhaps in conjuction with a deshy

tector at Grand Sasso)

Atmospheric neutrino oscillations

The subject of neutrino oscillations first suggested by Pontecorvo has been a topic of

intense interest for more than 15 years For somc rccent rcviews sce [8) If neutrino oscillations

occur in their simplest form assulning a two flavor oscillation the probability of oscillation

IS

(1)

where dn2 = m~ - m~ is the difference of the nlass eig~nvalLies in eV2 0 is the two flavor

mixing angle L is the v propagation length in Kitorneters and El is the neutrino energy in

GeV

Recent results by the J(AMIOI(A 111D and SUDAN2 collaborations suggest that pershy

haps as much as 40 of the atmospheric lIevents in the encrgy range from 02-15 GeV

have oscillated to some other type of ncutrino (9)(10)[11) Othcr less sensitive experiments

did not record any effect [12] NESTOR will be able to tcst by studying atmospheric neutrino

oscillations at a higher energy legitne ( above 5 Ge V) The higher energy regime diminishes

the dependence of the study on geomagnetic cffccts and on the uncertainties of the Oxyshy

gen cross section and other nuclear effectsThe NESTOIt design is such that the top floors

can be used to veto downcoming cosmic raysTherefore we can he sensitive to neutrinos

arriving from a1l zenith anglesThis way ollr L dependence varicfol from 101ltm to 13000kln

giving NESTOR an unprecedented sensitivity in ~fn2 spanning four orders of magnitude

Further since we intend to study the oscil1atiotls as a disappcarence experiment that is by

nlcasllring the ratio of rnnons coming fron1 dirrclcnt 7-clIith anglcs we will be independent

from theoretical flux predictions which currently arc the source of considerable systematic

uncertainties in I(AMIOKA 111n and SUDAN20ur cXperill1Cnt win be internally normalshy

isable ie comparing the expected nUlnber of neutrinos coming frOin all directions to anyone

we choose to use as the control direction this way Jl1oltiulo solid angle effects the number of

muonlike neutrinos should be constant as a function of zenith if tJICIC is a decrease it would

be caused uniquely by neutrino oscillations ie JnuonJike neutrino oscillations to another

species Figure 11 shows the distance that the neutrinos have transversed from their point

of production as a function of zenith angle

Further our sensitivity will profit from the matter enhanccrnent of the to veosci1lations

We took the density profile of the earth froJn reference (13) For the purpose of this study we

estitnated the incoming neutrino flux by using 3 different calculations those of Butkevitch

et al (14) Mitsui et al (15) and Volkova [Hi] and a fourth one using the low energy spectra of

(17) together with the Volkova spectrum For our energies the flux predictions differ by 10-15

See fig 12and table 1

Evcnts Mean E in GeV E Spectrurn Butkevitch ct al 1043 6877 Mitsui ct al 880 6901 Volkova ct al 956 6365 Gaisscr+ Volkova 862 6690

TabJe 1 Fluxes and Energy cOlnparison

The downcoming cosmic ray muons are usually a Inajor obstacle to downward detection

of contained neutrino events in shallow watcr ltlctcctors but in our case prescnt a difficult but

manageable background Figure 13 shows the flux of downconling nluons per year compared

to the number of contained ncutrino atrllospheric evcnts as a function of the zenith angle

The ratio of signal to background fronl 0 to 60 degrees is of the ordcr of 10 Preliminary

studies have shown that we can reject the downcOJning cosmic ray Inuons at this leveJ by

using veto techniques

Our efficiency to reconstruct a muon with 20 degrees pointing reolution is shown in

figure 14 We are sensitive down to 5 GeVneutdno energy

Finally figure 15 shows the sensitivity we should lwve The systematic errors due to

the separation between vand 1einteractions are not included htlt they are estimated to

be less than 10 therefore comparahle to our statistical errors See the discussion of the

same systematics in the next section (111lt1 reference (181 Note that our sensitivity includes

the IltAMIOIltA solution

Long baseline oscillations with CERN

As we have denlonstrated in the preceding section a 2 1T zenith fit to the expected number of atmospheric neutrinos gives us an unprecedented sensitivity in J1U

2 on the other hand

accelerator experiments provide aJl extrclllcJy useful tool for systenlatic control (pulsed beam

selectivity of v or D) and by selecting the neutrino energy one can study in detail seJected

regions of 07n2 bull A c0l11plelnclltary study to the atrnospheric ncutrino oscillation can be

conducted with a long baseline experitnent with a CERN bcaln (sec (19) for reviews of the

o

long baseline techniques) As part of the work of the LIIC project injection transfer lines

are being designed to bring the fast extracted beams from SPS to the new collider The

primary proton beam for a neutrino production target to feed Gran Sasso with only minor

modifications can be derived frolTI the one TItt8 which links SPSLSS4 to LHCP8 See

reference (20] for more details

On a two dimensional projection CERN Gran Sasso and Nestor are Jined up Calculashy

tions from MMayoud (the head of the CERN surveyors) are reported in table 2 One sees

that a neutrino beam pointing to Nestor would need to he diverted by only 1 degree to the

west in azimuth (easi1y acommoded) and 5 degrees or 75 downwards in declination from

the one pointing to Gran Sasso

Place fjJ Az a Distance CERN G0732 4G2tttt2 - - -Gran Sasso 1357lt1middot1 12lt1525 122502 3283 731 1(ln

NESTOR 213500 363500 12lt11775 852G 1G7G Iltnl

Table 2 Coordinates absolute (fjJ) and relative wrt 1ltt8 CERN beam (Aza) of Gran Sasso and NESTOR (angles are in degrees)

For demonstration purposes we have run the heanl rvf C with the horns used for CHORUS

and NOMAD (in other words not optitllized for our energies) and we have found that for

1019 protons on target (which is equivalent to cUl optirnistic year of running but noting

the fftct that the horn has not been optitnized for 0111 connguration) we should have 27000

events in one tower ( without including our emciency) for a proton beam of 450 GeV and one

order of magnitude fewer events for a proton beam of 1GO GeV The flux energy spectra are

shown in fig 16 The beam diverges at the NESTOR location by about 15 km matching

well the detector dimensions (rv 300 In for one tower)Clearly such an experiment will require

more than one tower approprieteiy configured to enhance et separation

We shall detect the oscillation as a change of the ratio of neutral (NC) to charged current

(CC) interactions since all charged clirrent Ilcevents will apear as NC or muonless events

In the case of oscHlation to liT all CC events will appear rnuonless except the fraction where

the T decays to a e (this fraction is Bt=17 ) there will also be a kinematical suppression

71 (rv 25 ) due to the high mass of the T Therefore the sensitivity to IIT oscillations will be

less than the one to lie If P is the osdl1fttion pTobahility shown in (1) the change of the

ratio for the 11tO lItis oscillation is showil below The case of 1Ito leis obtained by setting

1=1 and 0=0 IinIt + II 11D I

Robll = V - (2) 1 - I + 1711 P

We have appJied the detection efficiency shown in ngure 14

o

long baseline techniques) As part of the work of the LIIC project injection transfer lines

are being designed to bring the fast extracted beams from SPS to the new collider The

primary proton beam for a neutrino production target to feed Gran Sasso with only minor

modifications can be derived frolTI the one TItt8 which links SPSLSS4 to LHCP8 See

reference (20] for more details

On a two dimensional projection CERN Gran Sasso and Nestor are Jined up Calculashy

tions from MMayoud (the head of the CERN surveyors) are reported in table 2 One sees

that a neutrino beam pointing to Nestor would need to he diverted by only 1 degree to the

west in azimuth (easi1y acommoded) and 5 degrees or 75 downwards in declination from

the one pointing to Gran Sasso

Place fjJ Az a Distance CERN G0732 4G2tttt2 - - -Gran Sasso 1357lt1middot1 12lt1525 122502 3283 731 1(ln

NESTOR 213500 363500 12lt11775 852G 1G7G Iltnl

Table 2 Coordinates absolute (fjJ) and relative wrt 1ltt8 CERN beam (Aza) of Gran Sasso and NESTOR (angles are in degrees)

For demonstration purposes we have run the heanl rvf C with the horns used for CHORUS

and NOMAD (in other words not optitllized for our energies) and we have found that for

1019 protons on target (which is equivalent to cUl optirnistic year of running but noting

the fftct that the horn has not been optitnized for 0111 connguration) we should have 27000

events in one tower ( without including our emciency) for a proton beam of 450 GeV and one

order of magnitude fewer events for a proton beam of 1GO GeV The flux energy spectra are

shown in fig 16 The beam diverges at the NESTOR location by about 15 km matching

well the detector dimensions (rv 300 In for one tower)Clearly such an experiment will require

more than one tower approprieteiy configured to enhance et separation

We shall detect the oscillation as a change of the ratio of neutral (NC) to charged current

(CC) interactions since all charged clirrent Ilcevents will apear as NC or muonless events

In the case of oscHlation to liT all CC events will appear rnuonless except the fraction where

the T decays to a e (this fraction is Bt=17 ) there will also be a kinematical suppression

71 (rv 25 ) due to the high mass of the T Therefore the sensitivity to IIT oscillations will be

less than the one to lie If P is the osdl1fttion pTobahility shown in (1) the change of the

ratio for the 11tO lItis oscillation is showil below The case of 1Ito leis obtained by setting

1=1 and 0=0 IinIt + II 11D I

Robll = V - (2) 1 - I + 1711 P

We have appJied the detection efficiency shown in ngure 14

1

The separation of It from e and hadrons in the detector is under study Preliminary Me results indicate that we will be able to distinguish between muonless (NC) and muonshy

full (eC) events by using the time distribution of the events ( Cerenkov light from muons

comes earlier than the one from the hadronic or electromagnctic showers) andor the lonshy

gitudinaJ shower development of the event ( the fnnons (Jistribute their light evenly while

electrons emmit their light according to the devcl0Plnent of the c1ectromagnetic shower)

The systematic effect due to this statistical separation is estimated to be of the order of

10 We are currently insta1ling our code in GEANT to assess in more detail the above

method In the case of V to venlattel effects could enhance the oscillation but as seen in

figures 17 and 18 1676 Km is not enough distance to produce a significant difference from

the matter effects Further as we see in figures 19 and 20 the statistics due to the larger

beam divergence disfavonr the 160 GcVproton heanl option This can only improve with

an optimized beam design We (lre cUllently studying it together wHh ABall The 450

GeVbaseline oscillation with CEllN as one can sec froln figure 18 wi)) cover better the area

of small mixing angles due to better statistics providcd that we will be able to control our

systematics

Sensitivity to Active Galactic Nuclei

We have estimated the cxpected AGN ncutrino events in NESTOR by tI~ing the neutrino

fluxes as they were calcttlatcd for various AGN typcs and parametrized by VStenger (21J

1221 The final nurnber of events is given by the fornHtla

R = p JF(Ev)A(EII)dEII JV( E)dy Jo(x y EII)dx (3)

where F(E) is the differential flux of neutrinos as it is given by VStcngers routine A(E

is the attenuation of the neutrinos due to interaction with the Earth and o(xyE) is the

vN differential cross section and where x and yare thc conventional scaling variables Ea is

the muon energy depending from y and the ncutrino energy via the type Ea=(I-y)E We

integrated over a mean solid angle of 2 7T bull Thc total cross section is a parametrization of the

plots shown at the DUMA NO Proposal [23J where cross sections are ploted versus neutrino

energy The parametrizcd cross sections are lTIultiplied with a terrn involving the structure

functions giving us the differential cross section in tenns of x and y The mean fraction of

the energy of the neutrino taken froll1 the produced fntlOn is 51 for the case of the neutrino

and 66 in the case of the antincutrino

The second integration in our fonnuln involves the integration over the y scaling pashy

nuneter and the effective voltl1ne has to he taken into account The effective volume was

calculated as the product of the effective area tilnes the nluon rangeThe calculation of the

lTItlOn range is based on the formula

I -l a + bEttl - n (4)

b a +bElO

-----~--~--~~---------

IV

In conclusion it will be cxtrclnely djfficult to see individual sources with one year of

running ( an average of 1 event is expected froln most hnninous sources) while we should

detect IV 80 events of diffused AGNs above the atmospheric neutrino background (above IV

150 TeV figure 21)

References

1 LlCResvanis et aI NESTORA Neutrino Partide Astrophysics Underwater Laboratory

for the Mediterranean lligh EnelYY Nefttdno All1ophysics WOlkstop Hawaii March 1992

VJ Stenger Editor

2 SA1lthanaev and AFIltuleshov ~1e~StlreTnCJlts of water transparency South- West of

Greece Proceedings of the tnd NESTOR Intcnlalionai IVofksholJ 1992 LlCResvanis editor

3 II Dradner Attenuation of light in clear deep ocean water Proceedings of the nJ

NESTOR Intelational lVofA~shol) 1992 LIltflcsvalJis editor

4 EGAnassontzis etal ~1eaStlrCnlcl1t of light transmissivity in clear and deep sea water

Proceedings of the tnd NESTOR Inte1national lVolkshop 1992 LIltResv8nis editor

5 TRA Demidova and IA Repin Investigation of neRr hoUotn currents in Inouse pit in the

vicinity of NESTOR area Proceedings of the tud NESTOIl International WOfkshop 1992

LIltResvanis editor

6 ETrimonis Geomorphology and bottonl scciinJcnts of the Pylos area Proceedings of the

fnd NESTOR lnternational lVo7ksholJ 1992 LKRcsvanis editor

7 EGAnassontzis etaJ NgSTOH progress rcport f31d International Cosmic Ray Conshy

ference Calgary 1993

8 S~1nilenky Neutrino Mixing DFTT 6792 November 1992 AAcker JLearned

SPakvasa TJWeiler UH-511-746-92 VAND-TJI-92-6 ~fay 1992 Sublnitted to Physics Letshy

lefs B May 1992 John Bahcall At17olhysics PfelJrillt Series IASSNS-AST 9259 December

1992 C Rubbia CERN-PPE93-08

9 ICSHirata etal Phys Lefl D280 146 (1992)

10 DCasper etalPhY8 Rev LeU 662561 (1991)

11 f1aury Goodman et ai ANL-J1EP-CP-92-121

12 Ch Berger et a1P11Y8 Leli B227 -189 (1989) Tv1Ag1ietta et aI EurophY8 Lett 8

611 (1989)

13 L Wolfenstein Phys RCl D Vol 17(9) 1 MAY 1978 p2369 Eric D Carlson Phys

Rev D Vol 34(5)1 Septcnlher 1986 pltJ5tJ (used especially for density)

14 AVButkevich Sov Nuclear Phys 50 (1989) 112

15 (C Mitsui Y Minorikawa II K011l0ri Nttovo (ilnrnlo v9C n5 p995-1019

16 LVVolkova Sov NurI Phys 31 (UJ80) 1510

17 G Barr TIltGaisscr TStancv Physiral RCtiew D 39(3) June 1989 GBattistoni

etaJ Nucleaf InsltunlCllt5 and Afdhotls in Physics Research 219( 1984) 300-310 Bionta

IV

In conclusion it will be cxtrclnely djfficult to see individual sources with one year of

running ( an average of 1 event is expected froln most hnninous sources) while we should

detect IV 80 events of diffused AGNs above the atmospheric neutrino background (above IV

150 TeV figure 21)

References

1 LlCResvanis et aI NESTORA Neutrino Partide Astrophysics Underwater Laboratory

for the Mediterranean lligh EnelYY Nefttdno All1ophysics WOlkstop Hawaii March 1992

VJ Stenger Editor

2 SA1lthanaev and AFIltuleshov ~1e~StlreTnCJlts of water transparency South- West of

Greece Proceedings of the tnd NESTOR Intcnlalionai IVofksholJ 1992 LlCResvanis editor

3 II Dradner Attenuation of light in clear deep ocean water Proceedings of the nJ

NESTOR Intelational lVofA~shol) 1992 LIltflcsvalJis editor

4 EGAnassontzis etal ~1eaStlrCnlcl1t of light transmissivity in clear and deep sea water

Proceedings of the tnd NESTOR Inte1national lVolkshop 1992 LIltResv8nis editor

5 TRA Demidova and IA Repin Investigation of neRr hoUotn currents in Inouse pit in the

vicinity of NESTOR area Proceedings of the tud NESTOIl International WOfkshop 1992

LIltResvanis editor

6 ETrimonis Geomorphology and bottonl scciinJcnts of the Pylos area Proceedings of the

fnd NESTOR lnternational lVo7ksholJ 1992 LKRcsvanis editor

7 EGAnassontzis etaJ NgSTOH progress rcport f31d International Cosmic Ray Conshy

ference Calgary 1993

8 S~1nilenky Neutrino Mixing DFTT 6792 November 1992 AAcker JLearned

SPakvasa TJWeiler UH-511-746-92 VAND-TJI-92-6 ~fay 1992 Sublnitted to Physics Letshy

lefs B May 1992 John Bahcall At17olhysics PfelJrillt Series IASSNS-AST 9259 December

1992 C Rubbia CERN-PPE93-08

9 ICSHirata etal Phys Lefl D280 146 (1992)

10 DCasper etalPhY8 Rev LeU 662561 (1991)

11 f1aury Goodman et ai ANL-J1EP-CP-92-121

12 Ch Berger et a1P11Y8 Leli B227 -189 (1989) Tv1Ag1ietta et aI EurophY8 Lett 8

611 (1989)

13 L Wolfenstein Phys RCl D Vol 17(9) 1 MAY 1978 p2369 Eric D Carlson Phys

Rev D Vol 34(5)1 Septcnlher 1986 pltJ5tJ (used especially for density)

14 AVButkevich Sov Nuclear Phys 50 (1989) 112

15 (C Mitsui Y Minorikawa II K011l0ri Nttovo (ilnrnlo v9C n5 p995-1019

16 LVVolkova Sov NurI Phys 31 (UJ80) 1510

17 G Barr TIltGaisscr TStancv Physiral RCtiew D 39(3) June 1989 GBattistoni

etaJ Nucleaf InsltunlCllt5 and Afdhotls in Physics Research 219( 1984) 300-310 Bionta

I I

cta1 Phys Rev Let 5middot1(21) 198) a11d Plrylt Het l bull ) lR(J) 1988

1ft VStenger intcrnal J)UIf 1 ND Hport

19 Stfphcll J PIIU(E FEHllILIB-Conr-912)J T S(pt(rllh(r 1))J ~ltnt1ry Gooornan

1 N L-JI EP-CP-92-17 Surnolnry talk of thc IFor~8ol) on IJo71g lJn8dine Neullino Oltcilshy

lulionltFerrnilahNovf1l11wr 17-20 1))I RBfrllst(in Fri~RIllLAB Conr-92fiJ Jdcas for a

L01lg- Baseline Neutrino Iletfctor Fehruary 1))2

20 C Hnhbia CEllN-PPE91-08

21 lIigh Energy NC11trino A~lrophy~ics Potential Sonrers and tlHir Ultlcnvater Detection

VICTOR 1 STENGI~R Prorecflillgs or t1w 2Hd NFSTOIl ucnJalio71ul lV01ksh01 1992

LTltH(svanis editor

22 VJStenger II NUOfIO (im(lo Vo1)( N 2 I nR() pt17) The Igtdrfltfrrr~triaJ Neutrino

Flux Srnsitivify or Undergrolllld lJHl illd(rs(il 1111011 I)(l(dor~

21 IllJfv1AND proposal If De 2-RR AlI~lI~f I)RR

Figure 1

13

ISOBATfIS

CONTOURS OF EQUAL DEPTII

The lighthouse of Sapientza will be the counting room Then the data will be transmitted to PYLOS by cable or microwave link

21-410 bull21eetO

ATLANTIC bEPAlTMENT OF P P SHIRSHOV INStil UTE OF OCEANOLOGY kUSf1AN ACADtMY Of SCIENCES

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13

ISOBATfIS

CONTOURS OF EQUAL DEPTII

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26

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007

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FULL NEsrrOR ARRAY

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10angular resolution -shyenclosed volumegt 20 megatons total number of phototubes 1176

TIllS CONFIGURATION SIJOIJLD BE BfG ENOUGII TO BEGIN TIlE FIELD OF IflGII ENERGY NEUTRINO POINT SOURCE ASTRONOMY

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FULL NEsrrOR ARRAY

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TIllS CONFIGURATION SIJOIJLD BE BfG ENOUGII TO BEGIN TIlE FIELD OF IflGII ENERGY NEUTRINO POINT SOURCE ASTRONOMY

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FULL NEsrrOR ARRAY

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- 100 m - 150 m I

J

sensitive areagt 100000 In2

10angular resolution -shyenclosed volumegt 20 megatons total number of phototubes 1176

TIllS CONFIGURATION SIJOIJLD BE BfG ENOUGII TO BEGIN TIlE FIELD OF IflGII ENERGY NEUTRINO POINT SOURCE ASTRONOMY

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__l-LLLJ LLI----L---LJ-I-11 I L--t-L-L-l-t-l_LI105

0- 0-1 0-1

Figure 17 Long Baseline Oscillation 10 efor 160 GeV

1 0

gt 1cu 10

5 CI

0 e

10

t 10

MAU[R ~ tJAlltR (-middotmiddotmiddotmiddotcmiddotmiddotmiddot~middotmiddotmiddotmiddotmiddotmiddotmiddotmiddotmiddotmiddot 4- ~riCSUff CTS - INClUl)[DINClUDED

~

I bullbull Ll

Figure 18 Long BCtsclilic Oscillation I to vor 150 GeV

2q

I

~ -I 10

5 Ct

e o

10

J1f- 180 CaV

Cmiddotmiddotmiddotmiddotmiddotmiddotmiddot

- bull bull bull I bull I_lL1_------LLLLlU-J10

10 10-1 10-

(sin2 theta) +middot2

Figure 19 Long Baseline Oscillation lto LIe for 160 all(1 450 GeV

10

450CeV -)

gtcv

10

5 Ct

e 0

10

- 0

II--L-L-1- ILLtI -bull L-lll L--~_bull__---LI~L bull~J

10 -2 10

Figure 20 Long Daselinc Oscillation vllto vTfor 160 and 450 GeV

cd QJ ~- I e til

~ 0

c ~

j c ~

(i)

(- Atmolphere

Riermo~ AGNt _ ~

to - ~

rrothert ~~~~

to

2 3 4 5

log(Emu) in GeV

Figure 21 Dirruse iGNs

cd QJ ~- I e til

~ 0

c ~

j c ~

(i)

(- Atmolphere

Riermo~ AGNt _ ~

to - ~

rrothert ~~~~

to

2 3 4 5

log(Emu) in GeV

Figure 21 Dirruse iGNs