— First Review —
This is such a great introductory book to the past, present, and future of astronomy: beginning in the Solar System, continuing in the Milky Way and the Local Group, until we eventually reach the entire observable Universe. I will recommend this to anyone in the future for a holistic picture of the Universe that we live in. The graphics are simple, yet informative and intuitive. It is always helpful for me to read popular science books such as these, to build experience discussing complex topics in simple terms. Also, Jo Dunkley was one of my former undergraduate advisors!
— Second Review —
This book was even better on my second read through. I concur with my original review in saying that this is such a great introduction to the past, present, and future of astronomy. I will definitely be forcing Laurel and Cole read this in the near future, so that they can better understand my field of study.
I loved the presentation of the history of astronomy, which is a difficult and multi-faceted story to tell. Jo Dunkley, who was one of my former undergraduate advisors, does an impressive of job presenting this history in a manner that is easy to follow.
Reading this history of astronomy and presenting some of the most important unsolved questions makes me super excited to be a scientist, but especially an astronomer. Some parts of the section about cosmic dawn gave me chills, since this is what I am studying, and my recent work has shed new light on this unknown period of our history.
I have listed below my favorite figures, which are simple yet informative. I have also listed some of my favorite quotations, although these are too numerous to completely include here…
••••
Figure 1.1, Page 23: A person casts a longer shadow on a smaller, more curved, planet.
Figure 1.4, Page 34: Venus transit of Sun determines distance.
Figure 1.5, Page 46: The relative sizes of the planets in our Solar System.
Figure 1.6, Page 56: Using parallax to measure the distance to a star.
Figure 1.8, Page 75: Realms of the universe.
Figure 2.3, Page 92: The full range of light.
Figure 3.2, Page 151: Evidence for dark matter from a galaxy’s rotation curve.
Figure 3.3, Page 155: Cartoon of cosmic web of dark matter.
Figure 3.5, Page 161: Light from a galaxy gets bent by a heavy object.
Figure 3.6, Page 166: Two marbles can take paths of different lengths across the trampoline.
Figure 4.1, Page 187: Two different ways for a one-dimensional space to have no ends.
Figure 4.2, Page 189: How an expanding one-dimensional space looks from different viewpoints.
Figure 4.4, Page 193: In an expanding space, the more distant galaxies should appear to recede faster from the Milly Way.
Figure 4.5, Page 195: If a galaxy is receding, its light will be received with a lengthened wavelength, known as redshift.
Figure 4.9, Page 219: Different geometries of space.
Figure 4.11, Page 225: Some different topologies that a strip of paper can have.
Figure 5.2, Page 240: Proportions of elements formed in first few minutes after the Big Bang.
Figure 5.3, Page 241: Timeline for first 400,000 years after the Big Bang.
Figure 5.4, Page 243: The formation of the cosmic microwave background light.
Figure 5.5: Timeline for first 9 billion years of the universe.
Figure 5.7, Page 264: Cartoon showing how we found out that the expansion of space is speeding up.
Figure 5.8; Page 267: Current ingredients of the universe.
••••
“… Astronomy is the study of everything that lies outside our Earth’s atmosphere, and the quest to understand why those things behave the way they do.” — Pages 3-4
“Vision is enabled by light. The more light you can collect, the further out into space you can see. A telescope is, partly, a much larger bucket for collecting light than the human eye, allowing us to peer further out into the darkness of space and to see features in better detail…” — Page 8
“… When we look at the stars, we are looking back in time. This is an incredible gift. We can see parts of space, parts of our universe, as they were many years ago. The further we can collect light from, the further back in time we can look. If you look at the bright star Betelgeuse, which glows in the Orion constellation, you wind time back more than six hundred years. Its reddish glow started its journey to Earth in the Middle Ages. The stars in Orion’s belt are even further away. Their light, familiar to generations of humans, has travelled at least 1,000 years to reach us. This means we have a chance of understanding the history of the universe because we can see the more distant parts of it as they were in the past, thousands or millions or billions of years ago. This ability to look back in time has existed since humans first looked at the stars but has only become a key feature of astronomy in the past century as we have looked out beyond the Milky Way. The great extent of the universe in both space and time can make modern-day astronomy seem overwhelming. Space is so immense that the numbers describing distances are at risk of becoming meaningless. Numbers with too many zeros are hard to process. To get around this, we come up with ways of making sense of the different scales of space, and we simplify things and let go of some of the details…” — Page 14
“Much of this story reflects how we still do astronomy today, more than 200 years later: working out how to make a difficult measurement, coming up with different ways to do it, planning many years ahead and going to often inhospitable and inaccessible places to get the best measurement possible. Central to the project’s success was applying for funding from national governments for equipment, salaries and travel costs, coordinating with national and international teams, and combining results from different groups. These are all things we still do now in astronomy. Like today, each country’s groups were happy to work together towards a common purpose but were particularly eager to make the best measurement themselves. As scientists we are often both competitive and collaborative in our pursuit of nev discoveries.” — Page 38
“We now take our final step outwards, arriving at the extraordinary viewpoint that takes in our entire observable universe, On this largest scale the universe appears as an intricate network of galaxy superclusters that together contain about 100 billion galaxies. Those galaxies are themselves huddled together throughout space in their smaller collections of clusters and galaxy groups. Each of those galaxies has around 100 billion stars, and a huge number of those stars will have their own systems of planets orbiting around them. With such numbers, it is no wonder that most astronomers suspect that life exists in some form elsewhere in the cosmos. When we refer to ‘observable’ universe we mean what we are able to see from Earth. What limits this is not how good our telescopes are, but how old the universe is. The universe as we know it has not been around for ever. If we are to be able to see some distant galaxy, that means its light has had time to travel through space to us on Earth. A galaxy that is further away, so far away that its light has not yet had time to get to us, is beyond our cosmic horizon, and beyond our reach. So how far away is this horizon? We will come around later, in chapter 4, to the idea of the birth of the universe and its age. For now we can say that astronomers have worked out that the cosmic horizon is about 50 billion light-years away from us in all directions. It is more than 14 billion light-years, the distance light could travel during what we now know to be the life-span of the universe, because space has been growing during that time. Our observable universe is therefore spherical, centred on ourselves here on Earth. This does not of course mean that we are at the middle of the universe. We are just, by definition, at the middle of the part we can see. If we now imagine putting the whole observable universe in our basketball court, our home supercluster Laniakea would be about the size of a cookie right in the centre…” — Pages 72-73
“From what we can tell, there is dark matter in every galaxy, and in every group and cluster of galaxies. It also not only lies within and around those great cosmic objects but threads through space to form a great interconnected cosmic web. This web looks reminiscent of the neurons in our brains, blown up to gigantic proportions. It dominated over the visible stuff, with five times more mass in dark matter than regular atoms. The starlit parts of the galaxies are just the bright jewels in this larger dark network.” — Page 153
“… Computer coding, coupled with telescopes, has become the foundation of modern astronomy, and our ability to understand our universe is closely connected to how powerful our computers are. In the case of tracking how dark matter evolves, each sum is simple, as it just involves the simple law of gravity, but tracking how each bit of the dark matter interacts with all the other ones requires a huge number of calculations to be performed in quick succession.” — Pages 156-157
“Returning now to our place in the universe, we locate ourselves on our small planet travelling around the Sun. Our Sun is surrounded in space by its neighbouring stars, many of them encircled by their own tiny planets. Our neighbouring stars move around in the longer spiralling arm of stars that makes up part of our larger home, the Milky Way galaxy. Our Galaxy, a huge disc of stars and gas embedded in a much larger halo of invisible dark matter, is spinning gently around. We look out to our neighbouring galaxy, the majestic spiralling Andromeda, slowly moving towards us through the depths of space. Around us there are many more galaxies, scattered through space and grouped together in smaller groups or larger clusters. Inside them, stars are born and die. Further out, we find more galaxies in their groups and clusters, as far as we can see. If we look far enough, we see them grouped into even larger structures, the megalopolis-like superclusters. The galaxies and clusters of galaxies are the bright lights on the backbone of the universe, the web of dark matter. We know that the universe has not always been like this. It is not only individual stars that get born, but entire galaxies too. They have not always been there, and the stars within them have not always shone brightly. By noticing that the galaxies surrounding us seem, on average, to be moving away from us, we have worked out that our universe must be growing. Everything in space is getting further away from everything else. If we then wind time backwards, we are led to the inevitable conclusion that, sometime in the past, our whole universe must have started to grow. It had something that could be called a beginning…” — Pages 233-234
“After a couple of hundred million years the universe approaches the end of the Dark Ages. At last the clumps of atoms have become dense enough to form the first mini-galaxies at the dense nodes of the cosmic web of dark matter. These proto-galaxies would have been quite unlike the galaxies that we can see around us in the universe now. Many times smaller, they would have been just tens of light-years across and perhaps a million times heavier than our Sun. At first they would have contained no stars at all. By following what happens in computer simulations, we have come to think that these galaxies were each made of a disc of gas, embedded in a larger, sphere-like shape of dark matter. The ingredients of the gas would have been only hydrogen and helium, very different to star-forming gas in galaxies like our own. The ingredients of solar systems like ours, with elements like carbon and oxygen, did not yet exist. What happened inside those mini-galaxies? The pull of gravity would have compressed the gas, heating it up to about 1,000 degrees. Where the gas was densest it would clump together ever more tightly, bringing hydrogen and helium atoms close together. Before a clump of gas can collapse into a star, though, the atoms inside it need to get cold enough for their inward-pulling gravity to win out over their outward-pushing pressure. The colder the gas, the lower the pressure. In practice this means cooling the gas clumps down to hundreds of degrees below zero, which happens when the atoms collide with each other. This slows them down, lowering their temperature, until at last the dense clouds of hydrogen and helium atoms can collapse into the very first stars. As we learned in chapter 2, fusion can then begin in their cores, generating light and heat. Hydrogen and helium atoms do not collide and cool down as readily as gases made of elements like carbon and oxygen. This means that these earliest clumps of gas would have had a stronger outward-pushing gas pressure than we find within gas clouds in the Milky Way today. That, in turn, means that those first stars were likely born on average much heavier than a typical star today, with a stronger inward-pull from gravity to counteract the pressure. There would have been many more of the short-lived white and blue stars, the heaviest and hottest of all the stars. We believe that the first stars formed in this way a couple of hundred million years after the Big Bang, marking the start of the ‘Cosmic Dawn’ of the universe. Astronomers have not yet determined the exact time this happened, because we cannot see their starlight…” — Pages 247-248
“Our community of astronomers has come an enormous way in advancing our understanding of our universe and our place within it. It is extraordinary to think that a century ago we did not even know that there were other galaxies beyond our own, we didn’t know how stars created their light and we were not aware that space is growing. Even in the past twenty years we have transformed our understanding of such basic matters as the age of the universe, the nature of solar systems around other stars and the fundamental ingredients of the universe. We can now trace the evolution of the universe from the earliest moments through its almost 14-billion-year history, understanding how galaxies, stars and planets like ours came to be. Our understanding of how things work in space has taken leaps forward, allowing astronomy to evolve from a science based mainly in empirical observation into a science grounded in our deeper understanding of the physical behaviour of the objects and phenomena we see in the sky. This is a golden age for astronomy, full of interest and possibility. One of the great excitements is that there are undoubtedly new discoveries just around the corner. Discoveries of new planets will continue apace, and perhaps soon there will be signs of conditions that hint at the possibility of extraterrestrial life. In the next few years we will no doubt see many more gravitational wave signals coming from black holes and neutron stars colliding throughout space, giving us a new way to see and understand the universe. We hope to soon discover what the invisible dark matter particles really are. And in the coming years we expect to at last see the first galaxies that formed in the universe. These discoveries are being made possible with magnificent new telescopes coupled with ever-increasing computing capabilities. The telescopes being prepared for the next decade span all of the wavelengths of light, as well as gravitational waves, and they will target high-definition views of particular objects as well as broad surveys of the entire sky. Highlights include the Square Kilometre Array to measure radio waves, the James Webb Space Telescope to examine the infrared and the Large Synoptic Survey Telescope to map the skies in visible wavelengths. To interpret the data, our computers will continue to increase in speed and capacity, allowing ever better simulations of the cosmos and the objects within it. There will also be discoveries that are not just around the corner, which will take much longer to reach. Being able to observe a planet suitable for life in great detail could take decades. So, too, will compiling a complete history of how our Milky Way was created. Understanding why the universe is growing ever faster, and how it started growing in the first place, will likely be a long process. But we can contemplate working towards each of these goals, because doing this work is a continual process that each of us plays a small part in. We stand on the shoulders of our scientific predecessors, all of whom have contributed in some way to the scaffolding that holds us up and that lets us together climb up further. When we look to the future, we hand our tools and knowledge on to our students, and we plan for things that might happen fifty or a hundred years from now, anticipating the success of those who follow in our footsteps. Our past is strewn with examples of visionary astronomers and physicists who did not make the discovery that they dreamed of. Halley never got to see the transit of Venus. Hale never got to see his magnificent telescope completed. Zwicky never saw a gravitational lens. But these were not failures. These scientists inspired younger generations to keep following their path and equipped them to make their own new discoveries. While we strive towards new discoveries, our past experience also tells us that our bigger picture of the universe and the laws of nature may still need some major aajustments. Our observations are certainly real, and our current interpretation of them tells a consistent story, but we should reasonably assume that some future shifts in the big picture are yet to come. The most exciting discoveries are the ones we least expect, ones that can radically change what we thought was true and ultimately lead us to a better understanding of our wider world. We look forward to them with eager anticipation.” — Pages 276-277