Rencontres de Blois

Leonardo de Vinci spent many of his latter days in the Loire Valley and if you visit Ambrois you may still see his ghost parading for the tourists. While he was there he contributed a number of beautiful designs into the châteaux of the region including this spiral staircase at the Royal Chateau de Blois. There is an even more spectacular example in the nearby picturesque Chateau de Chambord where he used a double helix design so that people can pass from one floor to another without meeting, but it is at Blois where this week we find a conference to discuss some new findings in particle physics and cosmology.

Dark Matter in Cosmology

Yesterday included a talk by Joe Silk, prof of astronomy at Oxford, who summarised our understanding on the cold dark matter model including dark energy and dark matter. Simulations of galactic cluster and structure formation favour a model where dark matter is made of weakly interacting cold particles. The mass should be in the range 10GeV to 10TeV. The lighter end seems at odds with accelerator experiments which should have produced such particles unless they have a very low cross-section for production from interaction with standard model particles. However, some of the detectors build to directly detect passing WIMPs have found evidence for 7 GeV particles. They have even seen an annual variation in the signal consistent with a cosmological origin. Dark Matter particles may also annihilate to produce a cosmic halo of positrons and electrons that space observatories such as PAMELA may have detected. From the slides Silk seems to have neglected to mention the results from Xenon100, now in theory the most sensitive dark matter detector, which is at odds with other results because it sees nothing. Over all it is a very exciting time for dark matter with the hope that the LHC will resolve the matter by producing the expected particles in proton collision.

Silk also looked at dark energy results and provided this awe-inspiring plot of how different observations constrain the two parameter space of cosmological models.

The blue SNe area is from the supernova data that first indicated the acceleration of the universe. This was followed by the CMB cosmic microwave background analysis that produced an orthogonal constraint to pin down the cosmological parameters to a narrow region consistent with a flat universe. This year a third source of data came from measurements of galactic structures giving the BAO band in excellent agreement with earlier data. This is also sufficient to show that dark energy is well modeled by a cosmological constant rather than a variable that changes with time. The effect of the constant is to have less impact in the early universe, while now it accounts for 73% of the non-gravitational energy of the universe. As the universe ages the cosmological constant will continue to increase its domination. Despite this observational triumph its theoretical origin remains mysterious and should be tied up with theories of quantum gravity not yet understood.

Searches for the Higgs Boson

Later in the afternoon Giovanni Punzi delivered a talk that has already caused a stir around the blogosphere, see here, here, here, here. First take a look at some of his collected plots for Higgs searches.

All these plots show a small excess around the 110GeV – 120GeV region, but the size is not significant and the positions are not quite consistent. Will we look back on these graphics in a few months time as the first signals of the Higgs or as statistical flukes?

The real interest today is in observations from jets at CDF. Here is a plot from a few weeks back that appeared to show a mystery bump. This was widely poo-poo’ed by commentators including myself who said that it could be a statistical fluke or a background effect.

Now they have fought back with a second plot from a completely independent run of data

It shows exactly the same thing! This rules out a statistical fluke at about the 5 sigma level. CDF has also responded to suggestions that it could be due to incorrect scaling of the background, showing that this cannot account for the excess when modelled carefully. Finally they rule out a standard model effect from top quarks. We are left to conclude that it must be a real new effect due to a particle of 150 GeV that is not part of the standard model. the big question is whether it is also seen at D0 and will the LHC confirm it?

11 Responses to Rencontres de Blois

  1. The lepto-phobic character of the bump is very difficult to explain without ad-hoc rules. Things become simple if the bump is pion of the scaled up variant of hadron physics predicted for 15 years ago by p-adic length scale hypothesis. The bumps at 325 GeV detected by D0 and CDF could be interpreted in terms of kaons of the new hadron physics.

    See my blog:

  2. The lepto-phobic character of the 150 GeV bump bump is very difficult to explain without ad-hoc rules. Things become simple if the bump is pion of the scaled up variant of hadron physics predicted for 15 years ago by p-adic length scale hypothesis. The bumps at 325 GeV detected by D0 and CDF could be interpreted in terms of kaons of the new hadron physics.

    See my blog:

    The dark matter candidate at 7 GeV and related DAMA-Xenon100 discrepancy can be resolved
    if tau-pions (dark in the sense having non-standard value of Planck constant) are in question. Here TGD based view about color and p-adic length scale hypothesis are essential. Same mechanism would explain the production as in the case of two and one half year old already forgotten CDF anomaly. See the blog posting: .

    The Pamela anomaly for which Fermi gave additional support in turn would correspond to electropion of leptohadron physics with ordinary value of Planck constant and characterized by same Mersenne prime M_89 as the new hadron physics is in question (this guarantees that weak boson decay widths are not affected). This explains the electro-philic tendencies of the particle in this case. The particles predicted by competing scenarios seem to suffer all kinds of -philies and -phobies which does not predict long lifetime;-).

    Mass of electro-pion would be 500 GeV from direct scaling of the electro-pion candidate discovered already at seventies but was put under the rug because weak boson decay widths did not allow new light particles so that they indeed became dark matter also in this sense. Mu-pion and tau-pion suffered the same fate. Interpretation as dark variant of lepto-pions allows these particle to creep back to the day light . I hope that colleagues are finally mature to see them;-). See the blog posting: .

    For the brief overall view about how the overall pattern about anomalies consistent with basic TGD predictions of TGD is emerging see the latest posting: .

    • Ray Munroe says:

      Hi Matti,

      When Francis (th)E mule called this bump “leptophobic” a few weeks ago, I gave a partial answer as to how this might happen. In my book, I proposed more massive W’ bosons (I called it “Hyperflavor-Weak”) that couple to right-handed fundamental particles (rather than left-handed). Thus, the leptonic decay channel would involve right-handed electrons and right-handed neutrinos.

      IMHO, neutrino oscillations imply neutrino mass. If a neutrino has mass, then it must always travel slower than c (even if that happens to be 0.99999 c). Now Lorentz transform ahead of the neutrino (say at 0.999999 c), look back at it, and you will observe a “backwards-spinning” neutrino – i.e. an elusive right-handed neutrino. These right-handed neutrinos do not have color, electric, or “normal” weak interactions, and their gravitational interactions would be insignificant, so you can’t “tag” a right-handed neutrino with a right-handed electron to properly identify the event.

      Thus, the only events that can be properly reconstructed would be W’ decaying into right-handed quarks/ jets.

      Have Fun!

  3. Luboš Motl says:

    Hi Phil, do you remember that the excess was only occurring in the events where W decayed to muon pairs? What happened with that? Do they see the same with the electrons now? Or is the strange correlation still there?

    • Philip Gibbs says:

      I wish I knew such details. Shame they don’t have videos of these talks.

      • Luboš Motl says:

        Not sure whether the video would contain anything beyond the PDF file.

        In my opinion, the asymmetry between the muon-decaying W-boson and electron-decaying one may invalidate the very assumption that this class of excess events has a W-boson in it at all.

      • Philip Gibbs says:

        Interesting idea, but what else could it be, another new particle similar to the W but not decaying to electrons?

      • Luboš Motl says:

        I must have confused it with another bump, or just bought some misconception seen somewhere. I don’t see any significant asymmetry for the electrons-muons in the paper now.

  4. […] Something Real?,” Cosmic Variance, May 30th, 2011; Philip Gibbs, “Rencontres de Blois,” viXra log, May 31, 2011; Jester, “CDF: Wjj bump almost 5 sigma!!!,” Monday, […]

  5. Leo Vuyk says:

    A possible geometrical alternative;
    See: “Fermilab Tevatron Bump explained according to Quantum FFF theory.”
    see for detail geometry of 36 compound quark configurations added with one possible extra Top prime Quark configuration:

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