💜 - Matthew Opdyke

What is the Atacama Large Millimeter/submillimeter Array (ALMA)?

High on the Chajnantor plateau in the Chilean Andes, the European Southern Observatory (ESO), together with its international partners, is operating the Atacama Large Millimeter/submillimeter Array (ALMA) — a state-of-the-art telescope to study light from some of the coldest objects in the Universe. This light has wavelengths of around a millimetre, between infrared light and radio waves, and is therefore known as millimetre and submillimetre radiation. ALMA comprises 66 high-precision antennas, spread over distances of up to 16 kilometres. This global collaboration is the largest ground-based astronomical project in existence.

The antennas can be moved across the desert plateau over distances from 150 m to 16 km, which will give ALMA a powerful variable “zoom”, similar in its concept to that employed at the Very Large Array (VLA) site in New Mexico, United States.

What is submillimetre astronomy?

Light at these wavelengths comes from vast cold clouds in interstellar space, at temperatures only a few tens of degrees above absolute zero, and from some of the earliest and most distant galaxies in the Universe. Astronomers can use it to study the chemical and physical conditions in molecular clouds — the dense regions of gas and dust where new stars are being born. Often these regions of the Universe are dark and obscured in visible light, but they shine brightly in the millimetre and submillimetre part of the spectrum.

Why build ALMA in the high Andes?

Millimetre and submillimetre radiation opens a window into the enigmatic cold Universe, but the signals from space are heavily absorbed by water vapour in the Earth’s atmosphere. Telescopes for this kind of astronomy must be built on high, dry sites, such as the 5000-m high plateau at Chajnantor, one of the highest astronomical observatory sites on Earth.

The ALMA site, some 50 km east of San Pedro de Atacama in northern Chile, is in one of the driest places on Earth. Astronomers find unsurpassed conditions for observing, but they must operate a frontier observatory under very difficult conditions. Chajnantor is more than 750 m higher than the observatories on Mauna Kea, and 2400 m higher than the VLT on Cerro Paranal.

Source: eso.org

When Dead Stars Collide!

Gravity has been making waves - literally.  Earlier this month, the Nobel Prize in Physics was awarded for the first direct detection of gravitational waves two years ago. But astronomers just announced another huge advance in the field of gravitational waves - for the first time, we’ve observed light and gravitational waves from the same source.

There was a pair of orbiting neutron stars in a galaxy (called NGC 4993). Neutron stars are the crushed leftover cores of massive stars (stars more than 8 times the mass of our sun) that long ago exploded as supernovas. There are many such pairs of binaries in this galaxy, and in all the galaxies we can see, but something special was about to happen to this particular pair.

Each time these neutron stars orbited, they would lose a teeny bit of gravitational energy to gravitational waves. Gravitational waves are disturbances in space-time - the very fabric of the universe - that travel at the speed of light. The waves are emitted by any mass that is changing speed or direction, like this pair of orbiting neutron stars. However, the gravitational waves are very faint unless the neutron stars are very close and orbiting around each other very fast.

As luck would have it, the teeny energy loss caused the two neutron stars to get a teeny bit closer to each other and orbit a teeny bit faster.  After hundreds of millions of years, all those teeny bits added up, and the neutron stars were *very* close. So close that … BOOM! … they collided. And we witnessed it on Earth on August 17, 2017.  

Credit: National Science Foundation/LIGO/Sonoma State University/A. Simonnet

A couple of very cool things happened in that collision - and we expect they happen in all such neutron star collisions. Just before the neutron stars collided, the gravitational waves were strong enough and at just the right frequency that the National Science Foundation (NSF)’s Laser Interferometer Gravitational-Wave Observatory (LIGO) and European Gravitational Observatory’s Virgo could detect them. Just after the collision, those waves quickly faded out because there are no longer two things orbiting around each other!

LIGO is a ground-based detector waiting for gravitational waves to pass through its facilities on Earth. When it is active, it can detect them from almost anywhere in space.

The other thing that happened was what we call a gamma-ray burst. When they get very close, the neutron stars break apart and create a spectacular, but short, explosion. For a couple of seconds, our Fermi Gamma-ray Telescope saw gamma-rays from that explosion. Fermi’s Gamma-ray Burst Monitor is one of our eyes on the sky, looking out for such bursts of gamma-rays that scientists want to catch as soon as they’re happening.

And those gamma-rays came just 1.7 seconds after the gravitational wave signal. The galaxy this occurred in is 130 million light-years away, so the light and gravitational waves were traveling for 130 million years before we detected them.

After that initial burst of gamma-rays, the debris from the explosion continued to glow, fading as it expanded outward. Our Swift, Hubble, Chandra and Spitzer telescopes, along with a number of ground-based observers, were poised to look at this afterglow from the explosion in ultraviolet, optical, X-ray and infrared light. Such coordination between satellites is something that we’ve been doing with our international partners for decades, so we catch events like this one as quickly as possible and in as many wavelengths as possible.

Astronomers have thought that neutron star mergers were the cause of one type of gamma-ray burst - a short gamma-ray burst, like the one they observed on August 17. It wasn’t until we could combine the data from our satellites with the information from LIGO/Virgo that we could confirm this directly.

This event begins a new chapter in astronomy. For centuries, light was the only way we could learn about our universe. Now, we’ve opened up a whole new window into the study of neutron stars and black holes. This means we can see things we could not detect before.

The first LIGO detection was of a pair of merging black holes. Mergers like that may be happening as often as once a month across the universe, but they do not produce much light because there’s little to nothing left around the black hole to emit light. In that case, gravitational waves were the only way to detect the merger.

Image Credit: LIGO/Caltech/MIT/Sonoma State (Aurore Simonnet)

The neutron star merger, though, has plenty of material to emit light. By combining different kinds of light with gravitational waves, we are learning how matter behaves in the most extreme environments. We are learning more about how the gravitational wave information fits with what we already know from light - and in the process we’re solving some long-standing mysteries!

Want to know more? Get more information HERE.

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I am pleased to announce a NEW RELEASE to my Space Opera series. It is now available on Amazon in eBook and paperback formats! Pathway to the Stars: Part 6, Erin Carter Enjoy Erin’s beginning journey, in the sixth of a multi-story series, called Pathway to the Stars! "We can guide you, we can answer questions whenever you have them, but the greatest learning comes from freedom." ~ Eliza Williams, "Pathway to the Stars: Part 6, Erin Carter" #spaceopera #futurism #scifiauthor #sciencefiction #scififantasy #biotech #nanotech #neurotech #spacetravel #solarsystem #politicalscifi #strongfemalelead #entertain #educate https://www.instagram.com/p/BvXufGTg5Lb/?utm_source=ig_tumblr_share&igshid=i0paozefwqiv

Pathway to the Stars: Part 1, Vesha Celeste

Pathway to the Stars: Part 1, Vesha Celeste

Soon to be released, is the first in a latched-on (or related) series, Pathway to the Stars: Part 1, Vesha Celeste. This will be a slightly more descriptive portion that goes into more detail of the first character introduced, Vesha Celeste. Please pre-order, read, review, comment, and enjoy! Thank you!

Vesha Celeste journeys with Yesha Alevtina and her dream-angel, Sky, following a long life of…

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Challenge and tragedy comes to everyone, it does not discriminate between good or bad... Our resolve to overcome these challenges and tragedies while maintaining our kindness and compassion, our dignity and grace, our vision to see a broader perspective and our strength of character to persevere are how we should measure ourselves... Only judge others based on the level of kindness they demonstrate, no matter what life brings, but be kind and love no matter the burden or reward... - 💜 -- Matt Opdyke

Curl up, read a new series of books, and be edified! Out now, Part 1, Vesha Celeste, and Part 2, Eliza Williams, have been paired together, and are available for those interested in the types and directions of science and the speculation that lead to well-being and quality of life. Please feel free to follow, message, share ideas, and be a part of a positive future where, if we choose, we can prepare properly to navigate the stars. This is just the beginning of this series and prequel, “Pathway to the Stars,” to an even more giant series, “Further than Before!” Please enjoy. https://www.amazon.com/author/matthewopdyke #sciencefiction #scifi #sciencefictionfantasy #scififantasy #politicalscifi #physiology #neurology #physics #Apolitical #strongfemalelead #biotechnology #neuroscience #theoreticalphysics #problemresolution #productivepursuits #spaceopera #cerebraldrama #sophisticateddialogue #solarsystem #spacemining #physiologicaloptimization, #neurologicaloptimization #transhumanism #universalethics #wellbeing #genetherapy #CRISPR #politicalsciencefiction #matthewopdyke https://www.instagram.com/p/BpUMW6ZgB1I/?utm_source=ig_tumblr_share&igshid=wy078mgrbgmm

Please enjoy my new sci-fi fantasy novel currently available on Amazon! Further than Before: Pathway to the Stars (2 book series) amazon.com/author/matthewopdyke #scififantasy #spaceopera #sciencefiction #fantasy #mustread #scifinovels #fantasynovels #biotechnology #nanotechnology #theoreticalphysics #physics #darkmatter #utopian #strongfemalelead https://www.instagram.com/p/Bo1Z9Xlg2uc/?utm_source=ig_tumblr_share&igshid=1rhtcswancrx1

All three versions (chill, rock, orchestra) Further than Before: Pathway to the Stars, Part 1 -- Audible “Nature and humanity can be amazing, but likewise, it can be brutal. Brutality, as far too many know it, is unnecessary if we consider and implement one thing, innovation with purpose—a good purpose is brutality’s ideal replacement, and it comes minus unnecessary misery. It’s starting to become clear to me now what it is that we can do and how we can do it.” - Eliza Williams to Yesha Alevtina (Further than Before: Pathway to the Stars, Part 1) #books #sciencefictionbooks #SpaceOpera #scifi #ftbpathwaypublications #grahambessellieu #matthewjopdyke #politicalsciencefiction https://www.instagram.com/p/BxGfu74g5Vb/?igshid=16f1jd0ctbwq

2020 February 19

UGC 12591: The Fastest Rotating Galaxy Known Image Credit: NASA, ESA, Hubble; Processing & Copyright: Leo Shatz

Explanation: Why does this galaxy spin so fast? To start, even identifying which type of galaxy UGC 12591 is difficult – featured on the lower left, it has dark dust lanes like a spiral galaxy but a large diffuse bulge of stars like a lenticular. Surprisingly observations show that UGC 12591 spins at about 480 km/sec, almost twice as fast as our Milky Way, and the fastest rotation rate yet measured. The mass needed to hold together a galaxy spinning this fast is several times the mass of our Milky Way Galaxy. Progenitor scenarios for UGC 12591 include slow growth by accreting ambient matter, or rapid growth through a recent galaxy collision or collisions – future observations may tell. The light we see today from UGC 12591 left about 400 million years ago, when trees were first developing on Earth.

∞ Source: apod.nasa.gov/apod/ap200219.html