KM3NeT - KM3NeT

New publication:  core-collapse supernova explosions

11 March 2021 – In February 2021, the KM3NeT Collaboration released a publication describing the potential of KM3NeT to detect low-energy neutrinos from a future core-collapse supernova. The publication is submitted to the European Physical Journal  C.

What is a core-collapse supernova?

Core-collapse supernovae  are very energetic explosions that can end the life of massive stars. They have the peculiar feature of releasing about 99% of their energy as a huge flux of low-energy neutrinos. The neutrinos can escape the stellar core carrying information on the physical processes at play in the collapse, when the star is still opaque to light.

How well can KM3NeT observe a core-collapse supernova?

Thanks to the technology of KM3NeT based on the multifaceted modules with light sensors the KM3NeT detectors are particularly sensitive to the low-energy neutrinos from a supernova.  In the publication it is shown that KM3NeT  – when finished building the detectors –  can reach a 5 sigma discovery potential to observe a core-collapse supernova happening in the Milky Way. For the most optimistic theoretical models describing core-collapse supernovae, the detection threshold can extend up to the Large Magellanic Cloud.

The potential sensitivity of the KM3NeT detectors with 230 detection units in the ARCA detector and 115 units in the ORCA detector as a function of distance of the core-collapsed supernova. Curves are shown for three different masses of the progenitors.

Details

Once a core-collapsed supernova is observed, researchers of KM3NeT can study aspects of the neutrino emission such as the detected neutrino light curve and the neutrino spectrum. This will provide the potential for discrimination between different theoretical models of core-collapse supernovae and help to understand the physical processes behind the explosion mechanism. The time of arrival of the neutrino signal can be determined with an accuracy better than 10 ms for a source at the Galactic Center. The oscillating signature of hydrodynamical instabilities and other physical processes impacting the neutrino time profile can also be detected for nearby events: 3 sigma at 3-8 kpc, depending on the model. From the recorded coincidences, KM3NeT will be able to infer the properties of the neutrino spectrum, estimating the mean neutrino energy with a precision of about 2% if the other spectral parameters such as the energy scale and pinching parameter are known with a small uncertainty.

Neutrino light curves expected using the future full ARCA detector of 230 detection units, from a core-collapse supernova at a distance of 5 kpc and a progenitor of 27 solar masses.

What is possible with the current six detection units of the ORCA detector?

Already with the six detection units of the ORCA detector currently taking data, a detection at 5 sigma level of a core-collapse supernova can be achieved for supernovae at distances up to 10 kpc. The online analysis pipeline is in place, sending warning messages to SNEWS  – the worldwide network  for early warning for supernova events. The first MeV neutrino follow-ups of warnings by gravitational-wave detectors were performed using the data of only four ORCA detection detection units  that were active at that time, bringing the first KM3NeT physics results.

 

Exciting times are ahead. KM3NeT is ready for the observation of the next core-collapse supernova event in our Galaxy!

A collaboration in corona times

18 February 2021 – Like everyone else the KM3NeT Collaboration has to follow the restrictive measures against the COVID-19 pandemic. So, once more, the last two weeks we held our Collaboration meeting on-line. At this virtual meeting we discussed the many details of building the telescopes, analysing the data and developing the simulation programs.  We are very encouraged by the large progress with constructing the many detector components and the installation of the ARCA and ORCA telescope infrastructures. We are excited by the many analyses of data from the installed detector units on which we will  report at the upcoming conferences. Nevertheless, we  tremendously miss our colleagues.  In particular, for the young scientists in our Collaboration these are difficult times, but they are amazing in their efforts for the Collaboration.

During the Collaboration meeting we virtually said goodbye and thank you to Marco Anghinolfi, who will be retiring soon after many years of service to the Collaboration.  We hope you enjoy your retirement. Arrivederci, but no goodbye!

We virtually raised a glass to thank Mauro Taiuti for his four years of leadership as Spokesperson of KM3NeT. Fortunately, he has promised to continue his scientific career in the Collaboration!

We are looking forward to the new leadership of Paschal Coyle and his team. All the best for executing the tremendous task ahead of building the telescopes and executing the scientific program – also in corona times. We will do our best to support you!

We virtually applauded our PhD students who have recently completed their theses and wished our postdocs leaving the Collaboration all the best for their careers!

We virtually welcomed new students and postdocs who will work on the nitty gritty of data analysis and detector calibration. We hope to meet you face-to-face very soon!

Last but not least, we  virtually welcomed LPC Caen, France as a new group in the collaboration who  will participate in both the construction work and the scientific program. Super!

On the bright side of virtual meetings our conference committee reported a more diverse participation of our Collaboration in the international conferences. More people took part and the representation among speakers was better balanced in seniority and gender.

Building and operating a telescope is an attractive, tremendous, collaborative effort relying on  a lot of human interaction, hard to recreate in a virtual environment – but we did our best! We were still able to generate our customary  Collaboration group picture as you can see below: a collaboration in corona times.

 

 

Upgrade of ARCA infrastructure

21 December 2020 – Just in time for the winter break, a nice Christmas present was delivered to KM3NeT:  the second main cable between the ARCA detector site and the shore station in the lovely village of Porto Palo di Capo Passero at the isle of Sicily, Italy has been installed. It is an important step in the program of upgrading the ARCA seafloor network for the ARCA detector near Sicily, Italy.

Read more

‘Draw me a neutrino’

13 December 2020 – Have a look at the banner pictures of the KM3NeT home page. During December 2020 and January 2021, we display amazing drawings of the three neutrino-flavours: muon-neutrinos, electron-neutrinos and tau-neutrinos.

The drawings are made by the winners of the KM3NeT contest ‘Draw me a neutrino‘. We invited everyone from young to old to use their imagination and picture a neutrino.

 

About 500 people from Ecuador, France, Georgia, Greece, India, Italy, Morocco, Netherlands, Switzerland, Russian Federation, Spain and the UK took up the challenge.

The best drawings are now on display in an online exhibition in our Virtual Neutrino Art Centre (hub.link/ZZwzhf7).

You can find the drawings and the names of their authors here.

And a high resolution version of the drawings .

 

Enjoy!

New paper: Deep-sea deployment of the KM3NeT neutrino telescope detection units by self-unrolling

20 November 2020 – The KM3NeT Collaboration has published a new paper, in which we describe in detail the innovative deployment method for KM3NeT detection units.

No standard moorings

A custom design was necessary, because the KM3NeT mooring – the detection unit -is different from moorings typically used for oceanography.

For instance, in KM3NeT moorings the instrumentation is contained in transparent and thus unprotected glass spheres. That makes them vulnerable during deployment. Moreover, we use a long, thin and soft tube with optical fibres and thin copper wires for data transmission and electrical power for the instruments. That makes the units even more vulnerable.

On top of that, because we use thin Dyneema ropes as strength members in stead of a standard steel cable the mooring is not strong enough to carry the weight of the anchor during deployment.

All this makes it more difficult to deploy the unit without breaking it and we needed a customised deployment method.

Different from other telescopes

Compared to other neutrino telescopes such as ANTARES in the Mediterranean Sea and GVD in Lake Baikal, we designed the KM3NeT detection unit even more slender to minimise the amount of material used for support of the sensor modules. An other – economical – difference is that we have to deploy hundreds of units more for KM3NeT in a period of a few years while keeping the costs for sea operations at a minimum. These are even more reasons for innovation of the deployment method.

The LOM

We developed a custom-made, fast deployment method. Despite the length of the detection unit of several hundreds of metres, we managed to compact it into a small, re-usable spherical launching vehicle instead of deploying it weight down from a surface vessel – the standard method in oceanography. We dubbed the vehicle LOM for Launcher of Optical Modules.

The tric

Once the LOM has reached the seafloor, the innovative tric begins. The buoyant LOM rolls upwards along the Dyneema ropes. While doing so, it spits out the glass spheres with instrumentation attached to the ropes. As a result, while floating to the surface, the LOM leaves the detection unit behind at the seabed, unfurled to its full vertical length. Ready for data taking during many years to come.

Cost effective

The LOM has two economical advantages. First, it does not take a lot in space. Therefore, during a sea operation many LOMs can be stored on deck of a ship. Secondly, we can lower the LOM to the seabed at high speed. As a result, we need less expensive ship time for the installation of the KM3NeT telescope.

Cooperation

As far as we know, the method of compact deployment of moorings with a LOM is unique. The method is the result of close cooperation between engineers and scientists in the KM3NeT Collaboration from both oceanographic and astrophysics institutes. We hope it will inspire oceanographic scientists for the design and deployment of their future moorings.

Details

In the paper, we describe the details of the design of the LOM, the loading with a detection unit, and its underwater self-unrolling. You find the reference below.

LOM in pictures

Pictures below reflect the  process from idea to realisation. First an impression of the initial ideas for deployment by @Marijn van der Meer/Quest. Followed by the technical design of the KM3NeT detection units that must be installed and the design of the LOM launcher vehicle. Finally, photos of the first prototype of the LOM and the final version that is now regularly used for the installation of the detection units of the ARCA and ORCA detectors of the KM3NeT telescope.

 


 

Reference

Deep-sea deployment of the KM3NeT neutrino telescope detection units by self-unrolling

The KM3NeT Collaboration: S. Aiello et al 

2020 JINST 15 P11027

https://doi.org/10.1088/1748-0221/15/11/P11027

Data taking with KM3NeT

19 August 2019 – Since this spring, the KM3NeT telescopes are routinely operating with five detection units: four at the ORCA site, one at the ARCA site. First data results have been reported on the international conferences and workshops.

For the ORCA detector, off shore the French Provencal coast, four units were installed and connected to the seabed network. An earlier deployed unit was damaged during inspection and had to be recovered for repair in the labs of the Collaboration. It will be re-deployed in a next sea campaign. Also during the Spring-campaigns, three autonomous acoustic beacons were deployed at the seabed in the vicinity of the ORCA array. They are used for acoustic positioning of the optical modules in the detection units that move with the slowly varying deep sea currents. Sea campaigns for further expansion of the ORCA detector are scheduled after the summer break.

Offshore Sicily at the site of ARCA, after a fix of the seabed network, a detection unit that was deployed three years ago, could be revived and is again taking data since. Currently, the seabed network is being re-designed to allow for the extension of the ARCA detector to more than 200 detector units. The successful though temporary fix of the existing network makes connection of more detection units possible, while waiting for the implementation of the upgraded network.

 

Differences between ARCA and ORCA

The technology used for the ARCA and ORCA detectors is  almost identical, but the difference in volume and height of the detectors and the density of optical modules in the detectors are strikingly different.  When finished, the volume of ARCA  will be more than 100 times larger then that of ORCA. ARCA will have a volume of about 1 Gton and ORCA ‘only’ about 8 Mton, while the number of optical modules in ARCA will only be twice that of ORCA: about 4000 vs about 2000. Consequently,  module density in ORCA will be about five times larger than that in ARCA. How is that achieved? In both detectors, eighteen optical modules are attached to each vertical detection unit. In ARCA, the distance between the lowest and the highest module is about 600. In ORCA this is about 150 m. Also the horizontal spacing between detection units is different: about 90 m in ARCA vs about 20 m in ORCA. Although, ARCA will have only twice the number of detection units, its foot print on the sea bed is much larger  that that of ORCA.

The geometrical differences reflect the main scientific purpose for which the detectors will be used. These are also visible in the first character of their names: ARCA stands for ‘Astroparticle Research with Cosmics in the Abyss’. The sparsely instrumented detector is optimised for the detection of high-energy cosmic neutrinos from distant sources in the Universe. ORCA is the acronym for ‘Oscillation Research with Cosmics in the Abyss’. The more densily instrumented detector is optimised to measure lower energy neutrinos,  thus providing data for the study of neutrinos oscillating between the three known neutrino flavours. The words ‘in the Abyss’ refer to the locations of the detectors several kilometres deep in the Mediterranean Sea.

 

KM3NeT-ARCA and ORCA
KM3NeT: Comparison of the physical size of the ARCA and ORCA detectors.

 

KM3NeT at #icrc2019

 

28 July 2019 – The bi-annual International Cosmic Ray Conference (ICRC) is one of the most important conferences  where astroparticle physicists share their latest results. This year’s conference, the 36th edition,  is organised in Madison, Wisconsin, USA, from 24 July – 1 August.

Together, the ANTARES and KM3NeT Collaborations present their results in a highlight talk by Rosa Coniglione and in total 35 talks and posters.

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

 

For the experts:

Below a gallery of  contributions  presented  at #icrc2019 on be half of the KM3NeT Collaboration. They comprise technical work, calibration work, data analysis, software developments and predictions of  sensitivities of the detectors and theoretical limits. Click on the images for the proceedings.

Talks:

Posters:

 

ORCA is operational

8 March 2019 – Last month, the KM3NeT team of CPPM, Marseille together with the ship crews successfully installed an ORCA detection unit. It was the first unit connected to the refurbished main electro-optical cable to shore. After a few weeks of technology tests, the unit is given free for physics runs. ORCA is operational!

Unfortunately, after the deployment of one unit, the winch of the heavy lift line failed and three other units could not be deployed. They will be deployed during the next sea campaign.

In the mean time, KM3NeT researchers have taken up the duty of 24/7 shifts overlooking proper functioning of the detection units at both the ORCA and ARCA site. It is a pleasure to watch good quality data streaming to shore.

Pictures below: Four detection units in their deployment mode on deck of RV Castor (left), the package with the detection unit hanging on the heavy weight lift line just above the water surface (middle) and a plot of the signals that a down-going muon particle leaves in the detection unit: height vs the time of the recorded light signals (right).