Luyện nói tiếng Anh bằng Shadowing qua video: We Found Galaxies Too Old for the Universe

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The James Webb Space Telescope found galaxies that are too ancient-looking for our young universe. Now you may have heard that, but JWST keeps finding them, and our recent efforts to solve this conundrum point in wildly different directions. Have we found galaxies older than the universe, or did we just learn something incredible about how galaxies form?

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Telescopes are time machines. Light takes time to get to us, so we see distant objects as they were when their light began its Earthward journey. As our telescopes become more powerful they see further, and so more and more of the past becomes accessible to us. The James Webb Space Telescope is one of the most powerful time machines ever built. It’s powerful enough that it’s discovered galaxies whose light has been traveling to us since the universe was a little over 2% of its current age. The universe back then should look different, right? Those galaxies should look different. After all, this is when galaxies first started to grow, when they should have been vigorously forming many of their stars. They should look like hyperactive kids. Those types of galaxies are around back then, yet JWST has also seen much more developed, “adult” galaxies. Some that look way too big, and way too ancient-looking for a universe only a few hundred million years old.

Over the past year or two, this mystery has made the pop-sci rounds. That included some breathless speculation—like the idea that the entire Big Bang model is wrong. If there are ancient galaxies 13 billion years ago, then how can the universe be only 13 and a half billion years old?

So far we haven’t weighed in on this conundrum. Now many others have done a fantastic job laying it out and debunking some of the foolishness. Dr Becky in particular was on top of the progress as new data came in from JWST. So, why should we cover it now? First, a lot of you have asked for our take and it’s time to go on record. Second, the evolution of this mystery has been quite an emotional rollercoaster, swinging from unsolvable to solved, and now there’s new work that swings back in the direction of WTF. So let’s talk about the current status of the early galaxy conundrum.

And before that, let’s talk a bit more about what we actually expect the early universe galaxies to look like.

Galaxies pulled themselves together from tiny density fluctuations in the very early universe that we see in the dappling of the cosmic microwave background. The CMB reveals regions with tiny excesses of matter—hydrogen gas, but more importantly dark matter which outweighs the gas by a factor of at least five. As dark matter pulled itself together by gravity it pulled the gas in with it. And as that gas compacted, the first stars were also born. These very early galaxies must have started small, but with pretty crazy star formation due to the enormous abundance of gas at that time. As those galaxies continued to grow, they collided and merged, and eventually built themselves up into the mature galaxies that we see today.

We think we understand this stuff pretty well - or at least thought we did. Between the precise CMB measurements and our theoretical understanding of gravity, star formation, etc., our computer simulations allow us to explore the possible growth scenarios for galaxies. We can predict, for example, that early galaxies should be forming stars like crazy due to the enormous amounts of raw material—-hydrogen gas—that was around back then.

One thing that should be even more robust as a prediction is the size of dark matter halos.

These are the giant pools of dark matter that encompass all galaxies and hold them together.

Because dark matter should not be strongly effected by the complicated behavior of the gas and stars, we have high confidence in our understanding of how those halos grew over time. Or at least we thought we knew.

One very clear prediction of this whole model is that a lot of this halo growth should have happened in the first 10% of the universe’s age. In that first 1.5 billion years since the big bang there shouldn’t have been essentially no very large halos, and so no very large galaxies.

And that’s what the theory and the simulations say. But to check these we need powerful time machines— telescopes. Now as the telescopes got bigger and our cameras got more sensitive we were finally able to probe early enough times to properly test our models of halo growth. And this is where the problem started around 15-16 years ago when our “high redshift galaxy surveys” - aka really far away galaxy surveys - finally reached these distances we got some answers.

And those surveys started seeing a few cases of what looked like giant halos at earlier and earlier times. And also the hint of overly red galaxies in the early universe.

Galaxies that are actively forming new stars should be bright at short wavelengths because they have lots of giant, hot, short-lived stars. They are relatively blue in color compared to older galaxies. And older galaxies that are no longer so actively forming stars look much redder because these short-lived blue stars exploded already.

Those early surveys didn't reveal anything crazy yet—just a handful of cases where the galaxies looked too big and/or too evolved compared to what was expected from our models. In 2018, Charles Steinhardt and team articulated this emerging tension in their paper “the impossibly early galaxy problem”. But impossible things are well, impossible. It’s right there in the name. So several not-impossible explanations for these galaxies were devised.

For one, we don’t see these overly-large dark matter halos directly. We only see the starlight, and we use that starlight to infer the mass of the stars and then the mass of halos that contain them. But that step requires assumptions, and if any of those assumptions are wrong then perhaps we got the wrong halo mass. And the redness that suggests an old stellar population could be due to other things too, and there are several other issues with these inferences besides. I’ll come back to possible solutions in a bit.

But even if the galaxies observed in these ground-based surveys were really too old looking and too big looking, well we haven’t quite broken all of astrophysics and cosmology yet. If we strain our models of galaxy formation, we can potentially speed up galaxy evolution to show why these things exist by the time the universe is 10% of its current age. What we’d really like to do is to look back even further in time to see if we can find the time when these galaxies were themselves growing. And that’s what we did with the James Webb Space Telescope.

JWST was designed to push this early-galaxies game to new extreme limits. It’s the largest telescope ever deployed to space, which means the most powerful. It’s also designed to be sensitive to very long wavelengths of light—deep into the infrared part of the electromagnetic spectrum.

The “mid-infrared” as we like to call it. That’s important for these first galaxies because of the expansion of the universe. Their light has been traveling to us for much of the age of the universe. Because these EM waves traveled through expanding space, they were stretched out—their wavelengths lengthened. This is cosmological redshift, and higher redshift means longer travel time and greater distance. For the galaxies we’re interested in, this redshift converts visible and even ultraviolet light into mid-infrared—which is why JWST is needed.

The first efforts with JWST used similar methods to our ground-based galaxy surveys. So maybe I give you a bit more detail on that. The first thing you do in a galaxy survey is to take pics with different filters corresponding to different wavelength bands and then you compare the amount of light in each filter—we call this photometric imaging. We can learn a lot of stuff from the ratios of filter brightnesses— and so the colors. We discover candidate galaxies this way, we make a crude estimate of the distance because the color ratios suggest a redshift, we can constrain the stellar population—both the number of stars and the distribution of different types—for example, the redder colors mean an older population with few massive stars.

So what did JWST find? Well first, it confirmed the presence of overly massive and overly old-looking galaxies from the earlier studies—and remember that was from a cosmic age of around 10%--a redshift of 4. Now a critical advantage of JWST is that it’s sensitive enough to do proper spectroscopy on these galaxies—it can measure their “spectrum”-- the amount of light as a function of wavelength. These spectra confirmed that the redshifts are indeed very high. They also confirmed that the redness of the spectra is due to highly evolved stellar populations, rather than, say, there being a lot of dust in the galaxies, which can cause similar reddening in photometric analyses.

With these confirmations of old-looking early galaxies, researchers more broadly really started to pay attention. The media started to pick up on it when JWST pushed to greater distances and earlier times and kept finding these things. Currently, the earliest candidate giant, evolved galaxy discovered by JWST is at redshift 7.3, at just 5% of the universe’s age.

Now it seems we have a real conflict with our models of galaxy formation.

Dark matter halos too large and stellar populations too evolved for the short amount of time they had to develop. And this is about why we started to hear some hysterical claims that the universe is twice as old as we thought, or that the big bang model is completely overturned.

It’s not. And it isn't. There’s just so much independent corroboration of our model of an expanding 13 point something billion year old universe. You can’t point to one admittedly intriguing discrepancy and decide to throw the baby universe out with the bath water. There are much more parsimonious explanations for our improbably early galaxies.

Let’s look at one of the most compelling. Remember that when we calculate the masses of these supposedly gigantic dark matter halos, we based them on the starlight that we see, and that requires an understanding of the relationship between these two things, the starlight and the dark matter halo mass.

And that involves assumptions. Here’s how that works. One assumption is that halo mass is connected to the mass in stars, and that “stellar mass” is connected to the amount of light we see in those stars.

But we don’t see the light from all of the stars—typically the light we collect is dominated by the brightest stars in the galaxy. We then have to decide on the relative numbers of the different types of stars so we can extrapolate from the observer starlight to the mass of all stars, seen and unseen. And there's another assumption. And, yes, from there we can get to the halo mass.

Knowing the distribution of stellar masses in a galaxy on the other side of the universe takes some guesswork to say the least. And maybe the biggest unknown there is something called the initial mass function—the IMF. It tells us the relative numbers of stars at different masses that form when a burst of star formation happens.

We typically use the IMF that has been measured for the Milky Way galaxy, sometimes with various refinements. But we don’t know that stars formed with similar mass distributions in the early universe. And they probably didn’t. For example, when there’s less heavy elements around from generations of old stars, its easier to make really gigantic stars because gas clouds don’t fragment as much when the collapse. That would give what we call a “top-heavy” IMF— so more massive stars form in a given burst of star formation relative to what happens in the Milky Way. And more bright, massive stars means that these galaxies would be overly bright for a given halo mass. So if we’re determining halo mass from the light of those massive stars then we over estimate halo mass. Such a “top-heavy” IMF is probably the leading contender for explaining the apparent giantness of the dark matter halos. And this may even solve the conundrum.

But the mystery does stop here. A new study just found exactly the opposite result of this. This study claims to have identified a sample of galaxies that are what those “impossibly early” galaxies became in this part of the universe.

And because this sample is much closer, we can detect the light of much fainter, lower-mass stars. And so figure out the initial mass function down to much lower masses.

And the result is bad. This study found that the IMF is actually bottom-heavy in those galaxies. There are way more low mass stars—little red dwarfs and whatnot—compared to the Milky Way for example. And definitely very bottom-heavy compared to what we think a top-heavy IMF might look like. The top-heavy IMF that was supposed to solve the problem of the impossible galaxies. And in fact, this bottom-heavy IMFworsens the problem. An excess of low-mass stars means that when we convert galaxy light to stellar mass we underestimate that stellar mass, and presumably underestimate it's dark matter halo mass. And that makes it even harder to figure out how those things grew so fast so quick.

OK, before we join our crazy uncle on the anti-Big Bang conspiracy facebook group, some words of caution. We don’t really know whether this new study really did successfully identify the modern counterparts of our impossible galaxies, and the authors admit that, calling them “likely descendents”. We also don’t know what complicating interactions these galaxies could have had in the intervening 13 billion years to muddle the IMF. We also don’t know that a bottom-heavy IMF rules out an IMF that’s also top-heavy. In other words, there could be an over-abundance of low mass stars AND of high mass stars all compared to masses around that of the Sun. And it is plausible to assume an IMF like this that would still bring down those early halo masses.

There are similar challenges in explaining the apparent redness of these early galaxies.

The key here is that we need a way to shut star formation down much more quickly than we thought likely. Perhaps the leading contender is quite awesome—early quasars—supermassive black holes in the hearts of these galaxies blasting out radiation and winds that heats up and expels gas so that stars stop forming and the population can evolve quickly. We know this sort of feedback from quasars happens, but we now need to understand why its so extreme in the early universe. That involves very rapid growth of supermassive black holes—yet another very real and very interesting problem.

The most likely solution to all of this is that we’re going to learn an enormous amount about the surprising processes behind structure growth, star formation, black hole seeding and growth, and who knows what else. And once we figure it out, the impossible early galaxies will become more than just possible—they’ll become inevitable: a natural part of our updated understanding of our early spacetime.

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Từ vựng và ghi chú luyện nói cho bài học này

Bài luyện nói trình độ C1 này dựa trên video “We Found Galaxies Too Old for the Universe”. Những từ được nhắc lại nhiều nhất trong bài: galaxies, star, mass, halo, universe. Video này có 47 câu và 3028 từ để luyện shadowing. Phần lời nói dài 19:42. Người nói nói với tốc độ tự nhiên, khoảng 154 từ mỗi phút, gần với hội thoại hằng ngày. Chỉ 81% số từ nằm trong 3.000 từ tiếng Anh thông dụng nhất, nên từ vựng khá khó.

Từ vựng quan trọng trong video

15 từ khó nhất trong video, kèm phiên âm và nghĩa:

Từ	Phiên âm	Nghĩa
telescope danh từ	/ˈtɛl.əˌskoʊp/	kính thiên văn, kính viễn vọng
redshift danh từ	/ˈɹɛdˌʃɪft/	dịch chuyển đỏ
starlight danh từ	/ˈstɑː(ɹ)laɪt/	ánh sao
wavelength danh từ	/ˈweɪvˌlɛŋ(k)θ/	bước sóng
conundrum danh từ	/kəˈnʌn.dɹəm/	nan đề
infrared tính từ	/ˌɪnfɹəˈɹɛd/	hồng ngoại
impossibly trạng từ	/ɪmˈpɒ.sɪb.li/	một cách không thể
quasar danh từ	/ˈkweɪ.zɑɹ/	chuẩn tinh
gigantic tính từ	/d͡ʒaɪˈɡæntɪk/	khổng lồ
cosmic tính từ	/ˈkɑz.mɪk/	vũ trụ
abundance danh từ	/əˈbʌn.dn̩s/	phong phú
hydrogen danh từ	/ˈhaɪdɹəd͡ʒ(ə)n/	hiđrô, hi-đrô
devise động từ	/dɪˈvaɪz/	đề ra, vạch ra
electromagnetic tính từ	/ɪˌlɛk.tɹoʊ.mæɡˈnɛ.tɪk/	điện từ
merge động từ	/mɝd͡ʒ/	kết hợp, hợp nhất

Ngữ pháp trong video

Những cấu trúc người nói dùng nhiều nhất, kèm đúng cụm từ trong video:

Cấu trúc	Trong video
Thì hiện tại hoàn thành tiếp diễn have/has been + -ing — việc bắt đầu từ trước và vẫn đang tiếp tục	has been traveling
Câu bị động be + quá khứ phân từ — nhấn vào việc xảy ra, không phải người làm	were also born · was expected · was designed
Thì hiện tại hoàn thành have/has + quá khứ phân từ — việc đã xảy ra nhưng còn liên quan đến hiện tại	we've also learned · has also seen · has made
Mệnh đề quan hệ who / which + mệnh đề — thêm thông tin về người hoặc vật	space, which means · galaxies, which can

Phát âm cần chú ý

Người nói dùng 30 dạng rút gọn, ví dụ don't, we're, didn't. Hãy nói theo dạng ngắn đúng như bạn nghe.

Âm “th”: wavelength /ˈweɪvˌlɛŋ(k)θ/, theoretical /ˌθi.əˈɹɛt.ɪ.kəl/
Âm “sh” và “zh”: redshift /ˈɹɛdˌʃɪft/, assumption /əˈsʌm(p).ʃ(ə)n/, simulation /ˌsɪm.jəˈleɪ.ʃn̩/, prediction /pɹɪˈdɪkʃən/, caution /ˈkɔːʃ(ə)n/
Từ dài — đặt trọng âm cho đúng: geodesic /ˌd͡ʒiː.əˈdɛs.ɪk/, impossibly /ɪmˈpɒ.sɪb.li/, photometric /ˌfoʊ.təˈmɛt.ɹɪk/, underestimate /ʌndɚˈɛs.tɪ.meɪt/, electromagnetic /ɪˌlɛk.tɹoʊ.mæɡˈnɛ.tɪk/

Những âm người Việt thường gặp khó:

Cụm phụ âm cuối — đọc đủ từng âm, đừng nuốt âm cuối: redshift /ˈɹɛdˌʃɪft/, wavelength /ˈweɪvˌlɛŋ(k)θ/, evolve /ɪˈvɑlv/, correspond /ˌkoɹəˈspɑnd/, fragment /ˈfɹæɡmənt/
Âm /tʃ/, /dʒ/ và /ʒ/ — tiếng Việt không có, đừng đọc thành “ch” hay “gi”: merch /mɝt͡ʃ/, geodesic /ˌd͡ʒiː.əˈdɛs.ɪk/, gigantic /d͡ʒaɪˈɡæntɪk/, hydrogen /ˈhaɪdɹəd͡ʒ(ə)n/, merge /mɝd͡ʒ/
Âm /æ/ — mở miệng rộng hơn âm “e”: tab /tæb/, gigantic /d͡ʒaɪˈɡæntɪk/, fragment /ˈfɹæɡmənt/, electromagnetic /ɪˌlɛk.tɹoʊ.mæɡˈnɛ.tɪk/, calculate /ˈkælkjʊleɪt/

Cách luyện với video này

Nghe hết video một lần, chưa cần nói, và ghi lại những từ bạn chưa biết.
Bắt đầu ở tốc độ 0,75×, nói đuổi từng câu, rồi quay lại tốc độ bình thường khi đã quen.
Ghi âm giọng mình rồi so với bản gốc, chú ý các từ như telescope, redshift, starlight.

Phương Pháp Shadowing Là Gì?

Shadowing là kỹ thuật học ngôn ngữ có cơ sở khoa học, ban đầu được phát triển cho chương trình đào tạo phiên dịch viên chuyên nghiệp và được phổ biến rộng rãi bởi nhà đa ngôn ngữ học Dr. Alexander Arguelles. Nguyên lý cốt lõi đơn giản nhưng cực kỳ hiệu quả: bạn nghe tiếng Anh của người bản xứ và lặp lại to ngay lập tức — như một "cái bóng" (shadow) đuổi theo người nói với độ trễ chỉ 1–2 giây. Khác với luyện ngữ pháp hay học từ vựng bị động, Shadowing buộc não bộ và cơ miệng phải đồng thời xử lý và tái tạo ngôn ngữ thực tế. Các nghiên cứu khoa học xác nhận phương pháp này cải thiện đáng kể phát âm, ngữ điệu, nhịp điệu, nối âm, kỹ năng nghe và độ lưu loát khi nói — đặc biệt hiệu quả cho người luyện IELTS Speaking và muốn giao tiếp tiếng Anh tự nhiên như người bản ngữ.

Phương pháp shadowing: đọc hướng dẫn từng bước đầy đủ →

Luyện nói tiếng Anh bằng Shadowing qua video: We Found Galaxies Too Old for the Universe

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Từ vựng và ghi chú luyện nói cho bài học này

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Ngữ pháp trong video

Phát âm cần chú ý

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Phương Pháp Shadowing Là Gì?