Our solar system and sun is located inside a pancake shaped galaxy. Imagine a scale model where the plane of the Milky Way is a DVD, and the central bulge is a ping pong ball glued in the center. It is this narrow plane that we see across the sky on a sufficiently dark night from Earth, from our vantage point inside it. Dust blocks much of our view. But at other wavelengths astronomers can probe the heart of our galaxy.

The center of our Milky Way Galaxy, located 26,000 light-years away, houses a black hole as massive as a million suns, surrounded by very dense nest of stars and bright clouds. The density of stars in the innermost regions of the Milky Way is up to one million times greater than in our portion of the galaxy. This region contains extreme and unusual conditions that can influence the types of stars that reside there. The density of stars and clouds creates streaming patterns. There are large massive star clusters that cannot not be found outside that region. The radiation environment is intense in the galactic center.

The near-infrared image (Hubble) shows the knots of cloud edges and emission that mark the plane of our galaxy. The mid-infrared image (Spitzer) highlights the clouds of gas and dust and star forming regions. The X-ray image (Chandra) tracks the most luminous and powerful stars in the area conspicuously revealing the galactic center region itself – including the million-solar mass black hole at the very hub of our galaxy. In addition, several other X-ray emitting locations can be seen, linked to massive star clusters.

Video: NASA, ESA, and G. Bacon (STScI)
Image Credits: NASA, ESA, CXC, SSC and STScI

I found this cool area with boiling mud pools all around so I thought, why not dip an iPhone X in there? Unfortunately, I wasn’t able to retrieve any footage due to the hardened mud in the port.

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I poured resin on an iPhone X to see what happens in the liquid glass like material!

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The Milky Way’s Bulge: From a Hypothesized Blob to a Remarkably Detailed Picture
David Nataf of Johns Hopkins University

The central bulge of our Milky Way galaxy is host to roughly 30 percent of its stars, including a substantial fraction of both the oldest stars and the most metal-rich stars. The ages of the stars indicate that some formed via hierarchical collapse early in the universe, while most formed later on, due to dynamical processes within the disk. The differences in chemical abundances among the stars may have effects on the formation of planets and the evolution of life. Astronomers’ understanding and characterization of the Milky Way bulge creates a relatively complex picture, but it is still incomplete.

Host: Dr. Frank Summers

Recorded live on Tuesday, July 3 at the Space Telescope Science Institute in Baltimore, Maryland, U.S.A.

More information: http://hubble.stsci.edu/about_us/public_talks/

In this scientific visualization, two spiral galaxies are set on a collision course. As one slices through the other, both are disrupted. The tidal forces of gravity produce long tails of material streaming away from the collision. The central regions relatively quickly fall together and merge. The visualization is based on research data from a supercomputer simulation, with stars shown in yellow and gas shown blue. Time passes at about 30 million years per second, lasting a total of about 1.5 billion years.

This version was rendered for a planetarium dome format (polar coordinate hemisphere projection). The camera choreography was designed for uni-directional seating, where there is a common focus point of the audience (front and center, about 60 degrees up).

The camera motion is somewhat complex, and can be discerned by watching the movement of the background galaxy field. The camera starts by dropping down to reveal the first galaxy in the front right and then the second galaxy to the front left. The camera also moves in toward the galaxies to get a closer view of the initial collision. After the initial collision, the camera continues to drop slowly, now increasing the distance to the galaxies and tilting a bit to keep the tidal tails on screen as much as possible. The camera also rotates slowly to increase the sweeping feel of the tidal tails passing above.

Visualization: Frank Summers, Space Telescope Science Institute

Simulation: Chris Mihos, Case Western Reserve University, and Lars Hernquist, Harvard University

This visualization of a computer simulation showcases the ‘cosmic web’, the large scale structure of the universe. Each bright knot is an entire galaxy, while the purple filaments show where material exists between the galaxies. To the human eye, only the galaxies would be visible, and this visualization allows us to see the strands of material connecting the galaxies and forming the cosmic web.

This visualization is based on a scientific simulation of the growth of structure in the universe. The matter, dark matter, and dark energy in a region of the universe are followed from very early times of the universe through to the present day using the equations of gravity, hydrodynamics, and cosmology. The normal matter has been clipped to show only the densest regions, which are the galaxies, and is shown in white. The dark matter is shown in purple. The size of the simulation is a cube with a side length of 134 megaparsecs (437 million light-years).

The camera choreography is a straight line path through the simulation. The camera accelerates from a standstill at the start, flies at a constant speed, and then decelerates to a stop at the end. The “cruising speed” of the camera is 250,000 parsecs per frame, or about 20 million light-years per second (at 24 frames per second). That’s more than 600 trillion times the speed of light. Buckle your seatbelts.

The simulation is periodic, and the camera flies through it several times. A skew angle is used to avoid showing the same structures on each fly through. The camera path (after accelerating to full speed) does repeat every 2000 frames. Hence, one can get an infinite loop by showing the frames 100 – 2099 over and over.

Visualization: Frank Summers, Space Telescope Science Institute

Simulation: Martin White and Lars Hernquist, Harvard University

This version of “Flight Through the Orion Nebula in Visible Light” has been rendered onto a hemispherical format (azimuthal equidistant projection) for use in planetarium domes. The black circular mask in the images denotes the edge of the hemispherical dome projection. The video is for preview purposes. Planetariums will want to download the frames and the audio files from HubbleSite: http://hubblesite.org/video/1155

This visualization explores the Orion Nebula as seen in visible-light observations from the Hubble Space Telescope. This movie is designed to be compared and contrasted against the companion movie using infrared-light observations from the Spitzer Space Telescope.

As the camera flies into the star-forming region, it reveals a glowing gaseous landscape that has been illuminated and carved by the high-energy radiation and strong stellar winds from the massive hot stars in the central cluster. The high-resolution visible observations show fine details including the wispy bow shocks and tadpole-shaped proplyds.

This version of “Flight Through the Orion Nebula in Infrared Light” has been rendered onto a hemispherical format (azimuthal equidistant projection) for use in planetarium domes. The black circular mask in the images denotes the edge of the hemispherical dome projection. The video is for preview purposes. Planetariums will want to download the frames and the audio files from HubbleSite: http://hubblesite.org/video/1154

This visualization explores the Orion Nebula as seen in infrared-light observations from the Spitzer Space Telescope. This movie is designed to be compared and contrasted against the companion movie using visible-light observations from the Hubble Space Telescope.

As the camera flies into the star-forming region, it reveals a glowing gaseous landscape that has been illuminated and carved by the high-energy radiation and strong stellar winds from the massive hot stars in the central cluster. The infrared observations generally show cool temperature gas at a deep layer that shows the full bowl shape of the nebula. In addition, the infrared showcases many faint stars that shine primarily at longer wavelengths.

This version of “Flight Through the Orion Nebula in Visible and Infrared Light” has been rendered onto a hemispherical format (azimuthal equidistant projection) for use in planetarium domes. The black circular mask in the images denotes the edge of the hemispherical dome projection. The video is for preview purposes. Planetariums will want to download the frames and the audio files from the HubbleSite page: http://hubblesite.org/video/1153

This visualization explores the Orion Nebula using both visible and infrared light. The sequence begins with a wide-field view of the sky showing the plane of our Milky Way Galaxy, then zooms down to the scale of the Orion Nebula. The visible light observation (from the Hubble Space Telescope) and the infrared light observation (from the Spitzer Space Telescope) are compared first in two-dimensional images, and then in three-dimensional models.

As the camera flies into the star-forming region, the sequence cross-fades back and forth between the visible and infrared views. The glowing gaseous landscape has been illuminated and carved by the high energy radiation and strong stellar winds from the massive hot stars in the central cluster. The infrared observations generally show cooler temperature gas at a deeper layer of the nebula that extends well beyond the visible image. In addition, the infrared showcases many faint stars that shine primarily at longer wavelengths. The higher resolution visible observations show finer details including the wispy bow shocks and tadpole-shaped proplyds. In this manner, the movie illustrates the contrasting features uncovered by multi-wavelength astronomy.