Lately, there have been different reports about the Hubble Tension from JWST, with different teams and methods. It’s been hard to follow. But initial sample sizes were small so in a new paper we combined, for the first time, all measurements to date, includes 5 JWST programs, and it makes a pretty clear picture. 🧵arxiv.org/abs/2408.11770
The first main question is “Do other techniques/instruments/teams JWST galaxy distances agree with past HST measurements?” It’s a resounding yes! 👏 All the offsets are on the 0.03 mag level and 1sigma from HST SH0ES, much smaller than Hubble tension scale of 0.18 mag. Conclusion, Hubble Tension is not a distance measuring problem.
The second question: “Could HST Cepheid measurements be non-linear, i.e., change with distance?”. This one is my favorite plot of paper - and is a resounding no. This is first time all the distance measurements have been compared to check linearity (or offset) and find linearity of 0.994+-0.01, non-linearity that would explain Hubble tension ruled out at 7 sigma level. Thats bigger than the Tension itself!
The third question is “Are different values of H0 from early JWST subsamples consistent? ” We made this graphic to show that you have to select some SN hosts and compare some of their stars (TRGB/Ceph/JAGB) to the SN to measure H0. However, the SNe have a lot of scatter and JWST samples are really small, so what H0 you get depends on the luck of which ones you pick, which is why you need a lot to reduce that uncertainty.
Since HST observed all the SN, we can ask this question as “what H0 would you expect if you only looked at this or that small subsample of SNe with JWST?”. It turns out, one would predict just what different groups are measuring with JWST - we can show the fluctuations are almost entirely what HST expected. This is just small sample differences.
If one combines all the JWST measurements from all the teams, and propagates the covariance and uncertainties correctly, you get the "reversion to the mean" of larger samples: H0=72.6+-2.0 km/s/Mpc from JWST. HST would have predicted H0=72.8 for the same sample, so again JWST and HST agree.
This is pretty amazing. The HST and JWST data are telling a consistent story, just that early JWST samples are too small to measure H0 well. I think that story got a little muddled by latest CCHP paper because some uncertainties were getting removed when they shouldn’t have been, but the important thing to me is that the actual measurements agree between telescopes & teams & methods.
Having lived through this Hubble tension stuff for some time, I’d say this is the most solid ground these measurements have ever been on. Please ask any questions!
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The main premise of the distance ladder is neither physics nor astrophysics change between rungs because galaxies (identically selected) don’t know which rung they are on. Over the last couple of years, some have proposed breaking that premise to resolve H0 tension. A 🧵.
Normally we correct SN dust by the amount it reddens colors and by following “dust rules” which minimize Hubble residuals. These include the ratio of reddening-to-dimming and the likelihood of amount of dust, decreasing from peak at ~0. eg Hatano+98.
A new paper proposes different dust rules, ratios and likelihoods for the second versus third rung. The new likelihood says we see *all* 2nd Rung SNe through a significant amount (or screen) of dust.arxiv.org/abs/2403.10388
Arguably one of biggest curiosities about Hubble Tension is why TRGB+Supernova gives values between the two tentpoles of Tension, 67 and 73. We have new paper from CATS team doing 🍜 to 🥜🥜 analysis of TRGB+SN and get H0=73.2+-2.0 km/s/Mpc. How/why? A 🧵arxiv.org/abs/2304.06693
Idea behind TRGB is relatively simple - red giants, no matter size, should reach brightest phase when Helium ignites-that shows up as break in the Color Magnitude Diagram (CMD). CMD can be made by plotting the brightness of stars (here in ~I band) versus the color (like ~V-I).
In practice, shown here, this tip can look fuzzy, not sharp, due to noise, or contamination from other younger, brighter (AGB) stars. So finding the precise tip can be tricky and the recipe used varies case-by-case.
So last night arxiv.org/abs/2105.11461 claimed could remove H0 tension because of dust. I’m all for us discovering that dust is really weird, but paper changes H0 by changing Black Body physics for Cepheids, not dust. What has been discovered (something/nothing)? A thread.
The paper has two approaches: 1. looks at color excess (i.e., just dust) compared to the intrinsic color and measures the reddening ratio for each host. They get H0=71.8+-1.6, a little lower than SH0ES by making dust weird, but still tension .
This is similar to work @LloydEKnox did who saw similar results, 73.3 +/- 1.7, difference depends on how weird let dust get (most interesting part of this to me is @DillonBrout and I have been saying dust around sne in galaxies is weird, but don't know if it's galaxies or sne).