tag:blogger.com,1999:blog-1513704378254120283.post4046038842368922120..comments2019-01-20T11:14:49.288-08:00Comments on The Trenches of Discovery: Dark energy: onus of proof reversedShaun Hotchkisshttps://plus.google.com/111971223871759820367noreply@blogger.comBlogger7125tag:blogger.com,1999:blog-1513704378254120283.post-37384371195445724662016-02-10T19:25:48.749-08:002016-02-10T19:25:48.749-08:00Regarding ISW, you're right that I know about ...Regarding ISW, you're right that I know about the problems there. Unfortunately, the anomaly I spent some time working on didn't re-appear when looking for structures in other areas of the universe. This leads me to err on the side of believing that the original was just a statistical fluke. I hope it isn't though.<br /><br />This paragraph is just me splitting tacks, but I *now* wouldn't call that anomaly an "ISW" anomaly, basically because where LCDM has predicted ISW signals to exist, they have been found and do match LCDM's predictions (e.g. <a href="http://arxiv.org/abs/1401.1193" rel="nofollow">here</a>. The other stacking measurement of <a href="http://arxiv.org/abs/0805.2974" rel="nofollow">Granett et al.</a> doesn't match LCDM, but nor should it be called "ISW" (in my current opinion).<br /><br />Of course, if a backreaction calculation matched ISW where LCDM predicts it *and* also can explain what Granett et al. saw I would be ecstatic and would jump on that bandwagon right away!Shaun Hotchkisshttps://www.blogger.com/profile/04832423210563130467noreply@blogger.comtag:blogger.com,1999:blog-1513704378254120283.post-72226498936496959442016-02-10T12:13:05.833-08:002016-02-10T12:13:05.833-08:00Hi Sean: I said all data for which calculations ha...Hi Sean: I said all data for which <em>calculations have been done so far</em>. ISW/Rees-Sciama is a hard one. I have ideas about how to approach ISW, which will take at least a few years of more than one good PhD student to do. We have started actually. As you know the amplitude of the ISW effect is observationally a big headache for LCDM, so that should not be held up as one of its successes. (Some fellow backreactionistas and I have a recent summary of the tensions for LCDM in <a href="http://arxiv.org/abs/1512.03313" rel="nofollow">arXiv:1512.03313</a>.)<br /><br />My strategy for dealing with ISW is the same one which we hope may shed light on the large angle anomalies - namely ray tracing in Szekeres models that match actual structures in the Universe on < 70/h Mpc scales, as Krzysztof Bolejko, Ahsan Nazer and I do in <a href="http://arxiv.org/abs/1512.07364" rel="nofollow">arXiv:1512.07364</a>. We can already match features of the local expansion that standard FLRW assumptions do not, and by the end of the year we hope to have a model with more actual structures that even better fits local expansion, that can then actually be tested in the CMB map making pipeline for its effect on anomalies. As we are at an early stage, I am not prepared to discuss much of this publically, but I have started to talk to people within the Planck collaboration.<br /><br />For ISW, rather than looking at the features of our own "peculiar potential", one wants a statistical ensemble of nonlinear structures (Szekeres models being the best) that model the variety of structures we see. That is a much bigger problem. The ray-tracing effect itself is independent of the model of backreaction, and independent of timescape, as is our local "peculiar potential" work of <a href="http://arxiv.org/abs/1512.07364" rel="nofollow">arXiv:1512.07364</a>. To go to ISW one has to take an statistical average - it is at that stage that the specific model of backreaction - timescape or otherwise, becomes important. That involves steps over and above the numerics of ray-tracing, which I assure you are already complex enough if you are dealing with thousands of sources from actual galaxy surveys, as we do.David Wiltshirehttp://www2.phys.canterbury.ac.nz/~dlw24/noreply@blogger.comtag:blogger.com,1999:blog-1513704378254120283.post-25762711047252807772016-02-10T02:21:32.187-08:002016-02-10T02:21:32.187-08:00Thanks for the comment David. I wasn't aware t...Thanks for the comment David. I wasn't aware that timescape cosmology required the same number of parameters as LCDM, so that's good news. When you say it fits *all* the data have you calculated the expected ISW (or equivalent) effect and the slow down on growth of structure (as seen in e.g. galaxy cluster abundances and weak lensing signals)? These are both additional evidence for LCDM as well as the now usual supernovae, BAO and the CMB, but they also track how structures form, as well as just the background/average expansion. If the same two parameters can also fit ISW and structure growth rates that'd be awesome! (In LCDM both observables give similar values for Omega_m... though with a small amount of tension - so maybe there's room for timescape cosmology to do better than LCDM).<br /><br />I definitely accept that the assumption that even at last scattering the universe is close to FRW is unrpoven and needs to be taken, for LCDM, as an assumption. It seems to work, but of course that also isn't proof that it is correct.<br /><br />Thanks again for the comment.Shaun Hotchkisshttps://www.blogger.com/profile/04832423210563130467noreply@blogger.comtag:blogger.com,1999:blog-1513704378254120283.post-50547878716735410902016-02-10T00:51:02.043-08:002016-02-10T00:51:02.043-08:00Sean: you say you are "unaware of any backrea...Sean: you say you are <em>"unaware of any backreaction model in 2016 that is *calculable* and has only one free parameter and still fits all the data available today."</em><br /><br />Actually, the <a href="http://arxiv.org/abs/1311.3787" rel="nofollow">timescape cosmology</a> is calculable, fits the data for which the calculations have been done so far, and has the same number of free parameters as the spatially flat LCDM model; which for average expansion are <em>two</em>: the Hubble constant and the matter density parameter. The differences between timescape and the standard model are at the level that understanding systematic uncertainties in supernova data reduction is needed to distinguish the models (<a href="http://arxiv.org/abs/arXiv:1009.5855" rel="nofollow">MNRAS 413 (2011) 367</a>), but by the Clarkson-Basset-Lu test the timescape model will be distinguishable from the standard model using the Euclid satellite (<a href="http://arxiv.org/abs/1402.2236" rel="nofollow">Sapone et al, PRD (2014) 023012</a>).<br /><br />When it comes to the CMB anisotropy spectrum Ahsan Nazer found after two years of recoding of the standard MCMC analysis, that although we get likelihoods for the timescape model comparable to LCDM on Planck data, that when it comes to the (more than two) parameters of the standard model - such as baryon to photon ratio, spectral index etc - that the systematic uncertainties generated by uncertainties of less than 1/10^5 in energy density at last scattering nonetheless give systematic uncertainties of order 8-13% today (<a href="http://arxiv.org/abs/1410.3470" rel="nofollow"> PRD 91 (2015) 063519</a>).<br /><br />To do the job properly for the timescape case we actually have to consider backreaction in the primordial plasma - which nobody does. People assume, as Adamek et al do, or Ahsan and I did in starting our investigation, that since the universe is so close to smooth before last scattering then the FLRW approximation is good enough. But no! Actually, there is a fundamental issue at stake in assuming a single global FLRW universe ever. In my view, the Einstein equations are evolution equations that should provide a well posed causal initial value problem. Many would agree with that. But if the notion of spacetime itself is generated as a solution of the equations there is no requirement that the same notion of spacetime must hold on scales outside the particle horizon for which there is no causal contact. That is of course the same problems that inflation solves phenomenologically. But people just add scalar fields to a global spacetime to get the phenomenology. In my view this problem must have a more fundamental solution, and the notion of spacetime must be emergent to fundamentally deal with the very early universe.<br /><br />Dealing with the fundamental issues is not easy; but any real solution to questions involving dark energy and the like do mean going back to first principles about the nature of gravity and the nature of spacetime, which many researchers do not find comfortable. I have discussed the <a href="http://eddiecurrent.blogspot.com/2013/01/dark-energy-too-big-to-fail.html?showComment=1359626440108#c1038214054293161911" rel="nofollow">sociology of this elsewhere in the blogosphere</a>, and will not do so again here. But a few of us are working on calculable, testable models - just to do it with both conceptual and mathematical rigour is a slow, hard job.David Wiltshirehttp://www2.phys.canterbury.ac.nz/~dlw24/noreply@blogger.comtag:blogger.com,1999:blog-1513704378254120283.post-52759123818602492632016-02-09T21:02:12.202-08:002016-02-09T21:02:12.202-08:00The age problem you're referring to is based o...The age problem you're referring to is based on assuming <em>decoupling</em> of matter inhomogeneities from the expansion, i.e. it assumes <em>no</em> backreaction. In backreaction studies, <em><a href="http://arxiv.org/abs/gr-qc/0102049" rel="nofollow">"the averaged densities are directly coupled to the evolution of the averaged spatial curvature"</a></em>.Boudhttps://cosmo.torun.pl/blognoreply@blogger.comtag:blogger.com,1999:blog-1513704378254120283.post-23486216433826169052016-02-09T20:46:51.485-08:002016-02-09T20:46:51.485-08:00I agree with you Boud regarding whether Green and ...I agree with you Boud regarding whether Green and Wald have proven that backreaction is irrelevant and I can empathise with the frustration that must come from interacting with people who haven't had time to look at the situation closely and thus take G and W at face value.<br /><br />My thoughts on what side has the "onus is proof" is vaguely the following. When the accelerated expansion was first observed LCDM was a pre-existing, calculable model with just one new parameter. It still fits the data now in 2016. I'm unaware of any backreaction model in 2016 that is *calculable* and has only one free parameter and still fits all the data available today. Therefore, even if backreaction seemed very compelling at first, the fact that this alternative model has fitted the data well for 15 years suggests that either backreaction mimics that model very closely for some subtle and profound reason (maybe the backreaction effects exponentiate??), or that the effects of backreaction are small in our universe and Lambda is correct.<br /><br />Also, the other work, not normally mentioned in these debates (surprisingly to me) of Adamek, Daveiro, Durrer and Kunz (latest being: <a href="http://arxiv.org/abs/1509.01699" rel="nofollow">this one</a>) seems much more relevant. They don't assume that the universe is close to FRW *at all times*, only explicitly requiring it at early times and calculated forward in time from that initial state. If backreaction were true their framework should break down, but it doesn't appear to. There are certainly loopholes in their analysis, but the loopholes (e.g. the universe *not* being FRW at early times) seem unlikely.<br /><br />Anyway, I don't think backreaction research should be given up on, I'm just stating my opinion on the probability that it is the explanation of the physics normally attributed to Lambda. I definitely don't think it has been proven to be irrelevant beyond any reasonable doubt.Shaun Hotchkisshttps://www.blogger.com/profile/04832423210563130467noreply@blogger.comtag:blogger.com,1999:blog-1513704378254120283.post-21340733394549441842016-02-09T12:47:56.150-08:002016-02-09T12:47:56.150-08:00If you propose that, to simplify things a bit, you...If you propose that, to simplify things a bit, you can explain lambda away with back reaction, you run into the age problem, because the Hubble constant on large (CMB) scales would, without lambda, indicate a universe which is too young.<br /><br />Also, all the talk of voids and so on assumes that most of the matter traces the light. What if it doesn't? Dark matter could be much more homogeneous than visible matter.<br />Phillip Helbighttps://www.blogger.com/profile/12067585245603436809noreply@blogger.com