I Could’a Been A Contender… NGC 2903 by Warren Keller

This beautiful Leo spiral galaxy – NGC 2903 – is only some 20 million light-years away and is one of the brightest galaxies visible from the northern hemisphere. Despite easily being seen in larger binoculars and small telescopes, for some reason it was never included in Charles Messier’s famous catalog of celestial grandeur. “You don’t understand! I could’a had class. I could’a been a contender. I could’a been somebody instead of a bum, which is what I am.” This incredible color image taken with an amateur ground-based telescope shows off the galaxy’s exquisite spiral arms – including intriguing details of NGC 2903’s core region, a stunning amalgamation of old and young star clusters with immense dust and gas clouds. But there’s a whole lot more there to be seen…

Just a little smaller than our own Milky Way, NGC 2903 is about 80,000 light-years across and displays an exceptional rate of star formation activity near its core in visible light – but it also screams bright in radio, infrared, ultraviolet, and x-ray bands. While in every respect, this galaxy is much like our own home neighborhood, just like “On The Waterfront”, there’s some mysterious goings-on along that central bar – very young, hot globular clusters. Apparently, star formation is absolutely running rampant in a 2000 light-year wide circumnuclear ring surrounding NGC 2903’s center. “This isolated system strikingly reveals a soft extended X-ray feature reaching in north-west direction up to a projected distance of 5.2 kpc from the center into the halo. The residual X-ray emission in the disk reveals the same extension as the Ha disk. Since galactic superwinds, giant kpc-scale galactic outflows, seem to be a common phenomenon observed in a number of edge-on galaxies, especially in the X-ray regime, and are produced by excess star-formation activity, the existence of hot halo gas as found in NGC 2903 can be attributed to events such as central starbursts.” says D. Tschoke (et al), “That such a starburst has taken place in NGC 2903 must be proven. The detection of hot gas above galaxy disks also with intermediate inclination, however, encounters the difficulty of discriminating between that contribution from disk and active nuclear region.”

So what causes extremely starburst activity? As we’ve learned from our astrophoto lessons – galaxy interaction is a prime suspect. “NGC 2903 is found to have an H I envelope that is larger than previously known, extending to at least three times the optical diameter of the galaxy. Our search for companions yields one new discovery. The companion is 64 kpc from NGC 2903 in projection, is likely associated with a small optical galaxy of similar total stellar mass, and is dark matter dominated. In the region surveyed, there are now two known companions: our new discovery and a previously known system that is likely a dwarf spheroidal, lacking H I content.” says Judith A. Irwin (et al), “If H I constitutes 1% of the total mass in all possible companions, then we should have detected 230 companions, according to cold dark matter (CDM) predictions. Consequently, if this number of dark-matter clumps are indeed present, then they contain less than 1% H I content, possibly existing as very faint dwarf spheroidals or as starless, gasless dark-matter clumps.”

So how do we study what we cannot see? Only through photography and understanding how each phase of cosmic construction affects photographic results. “These results, and other considerations, have led to the hypothesis that the dark matter surrounding spiral galaxies consists of cold gas, mainly in the form of molecular hydrogen. The spatial distribution of this cold gas should be similar to that of the observed neutral hydrogen.” says H. Hoekstra of the Kapteyn Astronomical Institut, “There is a potentially powerful selection effect that may cause a relationship between the surface densities of HI and dark matter for the galaxies in our sample. This is because the HI surface density distributions of the galaxies in our sample have the common characteristic that the highest values in the inner regions, as well as the lowest values in the outer regions are similar from galaxy to galaxy.”

Now that we understand how astrophotos are used to determine galactic properties, open the image and take a closer look at all the galaxies hidden nearby NGC 2903 – and the details inside. When Warren Keller and David Plesko at Cherry Mountain Observatory collaborated on this photo, you can bet the first results from the raw data didn’t look like this finished work of art. For those of you who already understand the ins and outs of what makes deep space imaging what it is – perhaps I’ll totally explain this wrong, because it’s a new concept to me… But that’s why the world has Warren Keller.

When processing a raw image, there’s a lot more to it that just whacking it into photoshop and tweaking this or adjusting that. There’s things hiding inside and just like a great symphony, it takes a composer and a virtuoso to end up with music to make you cry. Because I don’t fully understand the process, I asked Warren to help me along, so I might also understand how these tiny details are drawn from thin air… or the blankness of space. “One of my big things is color balance- being true to the data, coupled with an understanding of how the object should look. What I see though is what I call assumptive processing- ‘It’s a galaxy and its arms must be really blue!’ In reality, each is very different and that’s why I love ’em so much. That sets a precedent, but I say be faithful to the data (once gradients are eliminated).”

And taking that data and teaching others how to process it is what Warren is all about. “All that being said, I’m aware of Atmospheric Extinction, CCD’s relative insensitvity to Blue, especially front lit and ABGs and the cancellation of Blue by the yellowing lens of middle-aged folks.” But is there a way that even us yellowing old dogs can be taught new tricks? Yeah. Warren not only knows how to sing the song, but he’s a music teacher. He’s created a teaching program called Image Processing for Astrophotography – or IP4AP. Say’s Warren: “IP4AP “Image Processing For Astrophotography” was created for Astrophotographers of all skill levels. There are many resources for learning Image Processing, but we believe these techniques are best taught – Visually!”

So, I was curious… And here’s a introductory look at Warren’s teaching style:

Before you take a cut out of me for being “commercial”, please remember that my job as a astronomical reporter is to also find products and methods which I find exciting and our readers might want to be made aware of. And, quite frankly, after having looking at many of Warren’s images and how his lesson plans work, I thought there just might be more than one budding (or seasoned) astrophotographer out there that might find what IP4AP has to offer of great value. As a matter of fact, even premier astro imagers like Dietmar Hager have used it. “Having had a couple of sessions with Warren covering essential facts about sophisticated usage of AstroArt and Photoshop was like leading me out of the dark basement of astrophotography into the highlighted groundfloor and further up. Guys, and I can tell you this is a high rise building and Warren is the perfect guide. Thanks for enriching my knowledge about digital processing!”

Go on, open it… Count all the details you can see in this image of NGC 2903 and its companions… and when you’re ready to become a contender, you can find IP4AP at many great retailers like OPT, Adirondak Astronomy and High Point Scientific. You’ve made a large investment in equipment – Now make a small one and learn the secrets of producing stunning astrophotographs!

Possible New Impact on Jupiter

Anthony Wesley from Canberra, Australia has captured a new impact spot on Jupiter. Credit: Anthony Wesle

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Amateur astronomer Anthony Wesley from Canberra, Australia captured an image of Jupiter on July 19 showing a possible new impact site. Anthony’s image shows a new dark spot in the South Polar Region of Jupiter, at approximately 216° longitude in System 2. It looks very similar to the impact marks made on Jupiter when comet Shoemaker-Levy 9 crashed into the gas giant in 1994. (But read the Bad Astronomer’s post that the black spot could also be weather.)

UPDATE (7/20): It has been confirmed this is an impact on Jupiter. Mike Salway shared the news Glenn Orton from JPL has imaged the Jupiter black spot with the NASA Infrared Telescope and he has confirmed it’s an impact.

The list below shows the times (in UT) when the black spot will be visible again (generated in WinJupos by Hans-Joerg Mettig), and found on the Mike Salway’s Ice In Space website.

2009 Jul 19 06:09 ( 216°) 16:05 ( 216°)
2009 Jul 20 02:00 ( 216°) 11:56 ( 216°) 21:52 ( 216°)
2009 Jul 21 07:47 ( 216°) 17:43 ( 216°)
2009 Jul 22 03:38 ( 216°) 13:34 ( 216°) 23:30 ( 216°)
2009 Jul 23 09:25 ( 216°) 19:21 ( 216°)
2009 Jul 24 05:16 ( 216°) 15:12 ( 216°)
2009 Jul 25 01:08 ( 216°) 11:03 ( 216°) 20:59 ( 216°)
2009 Jul 26 06:54 ( 216°) 16:50 ( 216°)
2009 Jul 27 02:45 ( 216°) 12:41 ( 216°) 22:37 ( 216°)
2009 Jul 28 08:32 ( 216°) 18:28 ( 216°)
2009 Jul 29 04:23 ( 216°) 14:19 ( 216°)2009
Jul 30 00:15 ( 216°) 10:10 ( 216°) 20:06 ( 216°)
2009 Jul 31 06:01 ( 216°) 15:57 ( 216°)

If you get the opportunity to observe or image this potential new discovery, please do.

On his observing blog, Anthony said he began observing Jupiter at approximately 11pm local time (1300UTC), using a 14.5″ Newtonian telescope. “I’d noticed a dark spot rotating into view in Jupiter’s south polar region and was starting to get curious,” he wrote. “When first seen close to the limb (and in poor conditions) it was only a vaguely dark spot, I thought likely to be just a normal dark polar storm. However as it rotated further into view, and the conditions also improved, I suddenly realized that it wasn’t just dark, it was black in all channels, meaning it was truly a black spot.”

First he thought it might be a dark moon (like Callisto) or a moon shadow, but it was in the wrong place and the wrong size. “Also I’d noticed it was moving too slow to be a moon or shadow. As far as I could see it was rotating in sync with a nearby white oval storm that I was very familiar with – this could only mean that the back feature was at the cloud level and not a projected shadow from a moon. I started to get excited.”

Hard-Hat tip to Mike Salway for alerting UT to the news.

What is Entropy?

After some time, this cold glass will reach thermal equilibrium

Perhaps there’s no better way to understand entropy than to grasp the second law of thermodynamics, and vice versa. This law states that the entropy of an isolated system that is not in equilibrium will increase as time progresses until equilibrium is finally achieved.

Let’s try to elaborate a little on this equilibrium thing. Note that in the succeeding examples, we’ll assume that they’re both isolated systems.

First example. Imagine putting a hot body and a cold body side by side. What happens after some time? That’s right. They both end up in the same temperature; one that is lower than the original temperature of the hotter one and higher than the original temperature of the colder one.

Second example. Ever heard of a low pressure area? It’s what weather reporters call a particular region that’s characterized by strong winds and perhaps some rain. This happens because all fluids flow from a region of high pressure to a region of low pressure. Thus, when the fluid, air in this case, comes rushing in, they do so in the form of strong winds. This goes on until the pressures in the adjacent regions even out.

In both cases, the physical quantities which started to be uneven between the two bodies/regions even out in the end, i.e., when equilibrium is achieved. The measurement of the extent of this evening-out process is called entropy.

During the process of attaining equilibrium, it is possible to tap into the system to perform work, as in a heat engine. Notice, however, that work can only be done for as long as there is a difference in temperature. Without it, like when maximum entropy has already been achieved, there is no way that work can be performed.

Since the concept of entropy applies to all isolated systems, it has been studied not only in physics but also in information theory, mathematics, as well as other branches of science and applied science.

Because the accepted view of the universe is that of one that is finite, then it can very well be considered as a closed system. As such, it should also be governed by the second law of thermodynamics. Thus, like in all isolated systems, the entropy of the universe is expected to be increasing.

So what? Well, also just like all isolated systems, the universe is therefore also expected to end up in a useless heap in equilibrium, a.k.a. a heat death, wherein energy can no longer be extracted from anymore. To give you some relief, not everyone involved in the study of cosmology is totally in agreement with entropy’s so-called role in the grand scheme of things though.

You can read more about entropy here in Universe Today. Want to know why time might flow in one direction? Have you ever thought about the time before the Big Bang? The entire entropy concept plays an important role in understanding them.

There’s more about entropy at NASA and Physics World too. Here are a couple of sources there:

Here are two episodes at Astronomy Cast that you might want to check out as well:

Source:
Hyperphysics

Acceleration Due to Gravity

Low gravity on an asteroid would be a big issue (NASA)

[/caption]The acceleration due to gravity is the acceleration of a body due to the influence of the pull of gravity alone, usually denoted by ‘g’. This value varies from one celestial body to another. For example, the acceleration due to gravity would be different on the Moon as compared to the one here on Earth. Similarly, you would have different values for both Jupiter and Pluto.

Since acceleration is a vector quantity, it must possess both a magnitude and a direction. The values we were referring to earlier pertained to the magnitude. As for the direction, in all instances, it should be directed to the center of the celestial body. Now, since these celestial bodies are rather large relative to the size of the observer, in this case being you and I, the direction is taken as downward.

Direction of g

Why downward? Well, as stated earlier, g is the acceleration of a body if we consider only the pulling force of the gravitational field. Now, since the acceleration of a body always takes the direction of the net force acting on that body, and since the only force we are considering is that of gravity, then this acceleration should take the direction of gravity, i.e., downward.

Don’t worry. The direction of g is mostly important only in the mathematical solutions of physics problems. What you should be more concerned with is the magnitude of g. Although this magnitude varies from one celestial body to another, you might want to know what the value of g is here on Earth.

Magnitude of g

The average value of g on the surface of the Earth is around 9.8 m/s2. Average? So there are other possible values? That’s right. The value of g becomes larger as the object gets nearer to the Earth’s core. So, you’d have a slightly larger g at sea level compared to what you’d have at the peak of say, the Himalayas.

Furthermore, since the Earth is not a perfect sphere but, rather, an oblate spheroid, i.e., bulging at the equator and flat at the poles, then you would have greater g’s at the poles than at the equator.

To end, let me just elaborate more on what we mean by 9.8 m/s2 as some people confuse this with speed. When we say that an object falling freely (under the influence of gravity alone) accelerates at 9.8 m/s2, we simply mean that its speed is increasing by 9.8 m/s every second. Hence, after 1 second of falling, its speed would be 9.8 m/s. After another 2 seconds of falling, it would then be 19.6 m/s and so on.

We have some related articles here that may interest you:

There’s more about it at NASA. Here are a couple of sources there:

Here are two episodes at Astronomy Cast that you might want to check out as well:
Decelerating Black Holes, Earth-Sun Tidal Lock, and the Crushing Gravity of Dark Matter
Gravity

Sources:
Wikipedia
The Physics Classroom
Haverford College

Visible Light

Sunlight passing through a prism. Image credit: NASA

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Of all the wavelengths in the electromagnetic spectrum, those that lie between 400 nm to 700 nm are the ones most familiar to us. That’s because these are the waves that comprise what we call visible light. 

When we see objects, it’s because they’re being illuminated by visible light. When we see that the sky is blue, or the grass is green, or hair black, or that an apple is red, that’s because we’re seeing different wavelengths within the 400nm-700nm band. Because of the waves in this band, a lot has been learned about the properties of electromagnetic waves.

Through visible light, reflection & refraction are easily observed. So are interference and diffraction. Mirrors, lenses, prisms, diffraction gratings, and spectrometers have all been put to use to understand and manifest the qualities of the light that we see through our naked eyes.

Galileo’s telescope, which was composed of a simple set of lenses, made use of the refractive properties of light to magnify distant objects. Today’s  binoculars and periscopes capitalize on the optical phenomenon called Total Internal Reflection by using prisms to improve on what early refractive telescopes were capable of achieving.

As mentioned earlier, visible light is made up of the wavelengths that range from 400 nm to 700 nm. Each wavelength is characterized by a unique color, with violet on one end (adjacent to ultraviolet light) and red on the other (adjacent to infrared light). When all these wavelengths are combined together, they make up what is known as white light. 

You can separate these wavelengths (and the corresponding colors) by letting them pass through either a prism or a diffraction grating. The magnificent array of colors that we see in a rainbow, on a diamond, or even a peacock’s tail are examples of this separation.

All phenomena of visible light such as reflection, refraction, interference, and diffraction are also exhibited by non-visible wavelengths. Hence, by understanding these phenomena, and applying them to the non-visible wavelengths, scientists were able to unearth many of nature’s secrets. In fact, if we trace back the roots of modern physics, particularly the wave-particle duality of matter, we will be led back to its manifestation in visible light. 

The study of visible light falls under the realm of optics. Among the scientists who have contributed substantially to the development of optics are Christiaan Huygens for his wavelets and a wave theory of light, Isaac Newton for his contributions on reflection and refraction, James Clerk Maxwell for the propagation of electromagnetic waves as explained in a series of equations, and Heinrich Hertz for verifying the truth of those equations through experiments.

You can read more about visible light here in Universe Today. Want to know where visible light comes from? How about a visible light image of a distant galaxy?

There’s more about it at NASA and Physics World:
Visible Light Waves
The special effect of physics

Here are two episodes at Astronomy Cast that you might want to check out as well:
Optical Astronomy
Interferometry

Sources:
Windows to Universe
NASA: Visible Light
Wikipedia: Christiaan Huygens
NASA: Maxwell and Hertz

Book Review: Magnificent Desolation, by Buzz Aldrin

Magnificent Desolation, the new autobiography by Buzz Aldrin

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I very much enjoyed chatting with Buzz Aldrin a couple of weeks ago, for some stories leading up to the 40th anniversary of the July 20, 1969 Apollo 11 landing on the moon. I found him honest, personable and generous with his time.

But when his publicist offered to send a copy of his new book, “Magnificent Desolation,” I didn’t set my expectations too high. I didn’t know what to make of an autobiography by a retired Air Force pilot and astronaut. Doesn’t that history put the “Rocket Hero” pretty squarely in the category of techie or a jock — a non-writer type?

Well, color me impressed. The book arrived late last week, and I turned the last page this morning — looking for more to read!

Courtsey of Buzz Aldrin
Courtsey of Buzz Aldrin

Granted, Aldrin got help when he teamed up with writer Ken Abraham. But no writer can spin a book like “Magnificent Desolation” without an incredible story, and Aldrin is a master of that.

The book opens with a few chapters on the Apollo program that made him famous. Even though I’ve dabbled in some research the past few weeks — including catching up on the movie “In the Shadow of the Moon” and leafing through some books — I learned new details both whimsical and serious.

Who knew, for example, that American astronauts traditionally eat steak and eggs prior to launch? Or that Aldrin is such a font of deep thoughts, which has apparently been true for a long time:

“From space there were no observable borders between nations, no observable reasons for the wars we were leaving behind,” he remembers musing as the Earth got smaller in Apollo 11’s windows.

“Magnificent Desolation” is about as revealing as you can get in personal realms. Aldrin engages in a lengthy discussion of his decade of deep depression and alcoholism following the Apollo years, from which he eventually escaped. At his rock bottom, Aldrin had lost faith in himself, had no vision for his purpose in life, and was failing at his job — as a salesman of Cadillacs.

During our interview, Aldrin said he turned his life around by deciding that he could share his experiences for a greater good.

“Do you continue to descend into an abyss? Or do you try to make a difference with what you know best?” he remembers thinking.

These days, Aldrin lives a life fitting for a hero. He hobnobs with greats in every field, from journalists and athletes to international leaders, scientists and movie stars. He and his wife, Lois, have traveled the world for scuba diving excursions, ski trips and unflagging efforts to promote his primary passion (besides Lois): a return to the collective national motivation that helped fuel the lunar landings. He desperately wants to see America lead the charge toward space exploration — to Mars and/or a moon of Mars, and beyond.

Aldrin admits he’s been criticized in the past, even by some of his astronaut peers, for garnering so much publicity as the second man (after Neil Armstrong) to set foot on the moon.

“The truth was, no other astronaut, active or inactive, was out in the public trying to raise awareness about America’s dying space program. None of them,” he writes. He points out that he is not promoting himself: “I did not want ‘a giant leap for mankind’ to be nothing more than a phrase from the past.”

Besides pushing for a new era of space exploration, the book is also a testament to the benefits of citizen space travel, which Aldrin avidly promotes through his outreach efforts, including his non-profit Sharespace Foundation. Among them: “The United States will capture the lion’s share of the global satellite market,” and “NASA’s planetary probes will become far more affordable.”

Aldrin has used traditional channels to advance his ideas, addressing international audiences of all stripes and testifying before Congress. But the really fun stuff comes when he reaches out to younger audiences. He seems to stop at nothing to reach out to the next generations, to ensure that his space exploration dreams will stay alive.

“I look forward to these things happening during my lifetime,” he writes, “but if they don’t, please keep this dream alive; please keep going; Mars is waiting for your footsteps.”

This review is cross-posted at the writer’s website, anneminard.com.

Fun Buzz Aldrin links:

Buzz Aldrin’s Web site

Training Buzz Lightyear for a NASA mission (YouTube video)

Comical interview with Ali G. (YouTube video)

“Rocket Experience” rap with Snoop Dogg

Other Universe Today Apollo 11 40th anniversary stories:

How to Handle Moon Rocks and Lunar Bugs: A Personal History of Apollo’s Lunar Receiving Lab

Q & A with Apollo 11 Astronaut Michael Collins

LRO Images Apollo Landing Sites (w00t!)

NASA Laments Missing Apollo 11 Film, Makes Do With What’s Left

And finally, the treasure trove: Apollo 11 Anniversary Link-O-Rama

How to Handle Moon Rocks and Lunar Bugs: A Personal History of Apollo’s Lunar Receiving Lab

Apollo 11 crew in quarantine talking with President Richard Nixon. Credit: NASA

50 lbs. of moon rocks. That’s how much weight was allocated for the Apollo 11 astronauts to bring back lunar samples to Earth. But this would be the first time materials from another world would be brought to our planet. What should be done with these alien rocks, and could they possibly be a threat to life as we know it?

What started out as a seemingly straightforward idea of building a facility to store and study rocks from the Moon ended up becoming a power struggle between engineers building the facility and scientists who wanted to study the rocks and those who wanted to save the world from biological disaster — not to mention even more squabbling between the various governmental agencies and politicians. In the middle of it all was James McLane, Jr. one of the engineers tasked with the early planning for the Manned Spaceflight Center –now known as Johnson Space Center in Houston — and in particular, he led a group to determine the requirements and design concept of NASA’s Lunar Receiving Laboratory.

James C. McLane Jr. in 1971.  Photo courtesy of James McLane Jr.
James C. McLane Jr. in 1971. Photo courtesy of James McLane Jr.

“We started the Manned Spaceflight Center from scratch and a cadre of people envisioned what we should have for the space program’s ground facilities,” said McLane, in an interview from his home with Universe Today. “A whole range of facilities were recommended. For a year or so I went from one design review to another to add my two bits as to how things might be done. The new facilities included a big manned centrifuge, electronics labs, and a thermal vacuum lab with a couple of very big space simulation chambers to test the Apollo spacecraft and its onboard crew under conditions similar to those to be found during the lunar missions. There was just about everything you could think of that was needed to support the Apollo program.”

While engineers at the MSC were intent on designing unique, world-class facilities (as well as rockets and spacecraft to take humans to the moon) scientists were excited about the prospect of researching pristine lunar materials.

Lunar Receiving lab concept drawing. Credit: NASA
Lunar Receiving lab concept drawing. Credit: NASA

During this time, a couple of young MSC scientists, chemist Don Flory and geologist Elbert King had been given responsibility of designing the airtight sample return containers in which lunar samples would be brought back to Earth. But, said McLane, no one had given much thought as to how the rocks should be handled or stored once they were brought back to Earth. “There really wasn’t much direction on what should be done after we got them back to Earth,” he said. “Oh, there were scientific committees of course, but for some reason this was down low on their priority list. I think they were thinking more about the research they were going to do with the rocks.”

But one day Flory and King showed up in their boss’s office and said since they had the responsibility for the container they were a little concerned what would be done with it after the astronauts returned the samples. They suggested that, at least, the containers ought to be opened in a vacuum chamber.

“They asked, ‘Does anyone around the Center have a small vacuum chamber where we can open these boxes?’ And that started the whole business of what would happen to the lunar samples and what was required to do that,” said McLane. “A small office was setup under the Assistant Director of Engineering, Aleck Bond, and I was assigned to head it. We were charged with determining what was needed to receive, protect, catalog, and distribute the materials collected from the surface of the moon. We were guided and assisted by a committee appointed by NASA headquarters, consisting mostly of people who had been selected, or expected to be selected as principal investigators for some of the many examinations and experiments proposed for the lunar samples.”

The initial plan called for a clean room approximately “ten feet by ten feet by seven feet” where the sample box could be opened under vacuum conditions and repackaged for distribution to various researchers.

But some NASA officials concluded just a single room wouldn’t be sufficient, and quickly came up with a plan for a 2,500 square foot research facility where the lunar samples would not only be stored, but studied as well. After more discussion, an 8,000 square-foot version was proposed.

Scientists in the Lunar Receiving Laboratory. Credit: NASA
Scientists in the Lunar Receiving Laboratory. Credit: NASA

Working with the scientific advisory committee to develop a workable plan for the ever-growing and changing proposed facility turned out to be an interesting challenge for McLane and his team.

“The biggest challenges were political,” McLane said. “All the scientists involved in studying the samples had laboratories of their own. They didn’t want to do anything unless it was going to benefit their facility back home. Others were suspicious that we were trying to appropriate activities that weren’t in the Manned Spacecraft Center’s charter at the expense of other NASA Centers. So, it was difficult to get everybody to cooperate and agree on just on the initial receiving procedure. A few of the experiments such as those to determine low level radiation properties of the samples were very time dependant. Thus it became evident that the facility and equipment required to perform those experiments would have to be located very near the point where the samples were first available. That point was Houston, and it particularly rankled some of the scientists to see new state-of-the-art facilities and equipment being located at Houston rather than at their home laboratories.”

“I had never worked with high level scientists before, and our advisory committee usually consisted of people who were at the level of principal assistants to Nobel Prize winners,” McLane continued.”Overall, it was a great group to work with, with one important exception. They each reserved the right to change his mind. It was not unusual for us to settle a contentious issue only to have it brought up again some weeks later. This caused some real schedule problems, but the instigator would plead ’Well, I was just wrong before’, or ‘I changed my mind’, often ignoring schedule and reality.

For example, one issue was whether to use glove boxes or use a closed container with mechanical manipulators (McLane equated them to the toy grappling machines in restaurants, only a little fancier) to work with the moon rocks. It took many discussions and debates to decide, and the decision would make a big different on what direction the engineers needed to go for building the lab, and they had a limited amount of time to decide.

McLane was also surprised about all the different scientific speculation that took place. “Some of the leading scientists of this country thought the moon was covered with several hundred feet of lunar dust and thought that when we landed on the moon the spacecraft would sink into the dust,” he said. “Fortunately that didn’t happen. Others thought the rocks on the moon, sitting in hard vacuum and bombarded with radiation and meteorites, that when first exposed to air they might catch on fire or explode. The speculations by good, smart, reputable people were just unlimited. But I guess they were trying to think of all the possibilities. We were fortunate that no one forced us to plan for any of these extreme speculations. Overall, our advisors did a good job of things.”

The Lunar Receving Lab shortly after it was built. Credit: NASA
The Lunar Receving Lab shortly after it was built. Credit: NASA

But then at one of the meetings in Washington to meet with advisors at NASA Headquarters, a scientist from the Public Health Service showed up and asked how NASA was going to protect against contamination of the Earth by lunar microorganisms.

McLane said the initial reaction by everyone else was, “What?”

For a couple of years a small group of scientists (which included a young and relatively unknown scientist named Carl Sagan) had been discussing the remote possibility that lunar samples brought back to Earth might contain deadly organisms that could destroy life on Earth. Even the spacecraft and the astronauts themselves could possibly bring back non-terrestrial organisms that could be harmful. Several governmental agencies, including the Department of Agriculture, the US Army, and the National Institute of Health got wind of this idea — and perhaps blew it a little out of proportion — and NASA was forced to take action to prevent a possible biological disaster.

“The ‘lunar bugs’ as we called them,” said McLane, “well, nobody really believed there was life on the Moon, especially something that might affect people – make them sick or kill off our civilization, that sort of thing.”

McLane said that the first time Deke Slayton, head astronaut at the time, heard about this, he just about “flew out the window.”

“He said, ‘No way is somebody going to step in and put these restraints on the program. It’s difficult enough to just fly to the moon without all these precautions about contamination.’ But NASA had meetings with the Surgeon General of the US, and he took the attitude, ‘How much is the Apollo program going to cost – $20 billion or so? I don’t think it is outlandish to set aside one percent of that to guard against great catastrophe on Earth.'”

“We said that we would take on the challenge of guarding against organisms, but the Surgeon General would have to justify it to the Congress, about the increased costs to the program,” McLane recalled. “And he did. So that got settled. We developed a scheme and it was approved. Everyone had to accept it, there wasn’t any choice.”

That changed the entire complexion of what McLane and his team had to accomplish before astronauts could go to the Moon. What started out a just a small clean room would now have to be a research lab, plus a quarantine facility. Plans for the facility grew to an 86,000 square foot structure that would cost over $9 million.

Lunar Receiving Lab.  This drawing illustrates the complex design of the LRL, with its several different components including Lunar Sample Laboratory, Astronaut Reception Area, Radiation Laboratory, and Support and Administration. Credit: NASA
Lunar Receiving Lab. This drawing illustrates the complex design of the LRL, with its several different components including Lunar Sample Laboratory, Astronaut Reception Area, Radiation Laboratory, and Support and Administration. Credit: NASA


“We had to devise all the precautions,” said McLane, “as well as the facilities and procedures for quarantine of the astronauts, as well as accepting the samples and initiating tests on the rocks that had to be done quickly behind absolute biological barriers to test for any contamination before anything could be distributed to the scientific community. It was very interesting work.”

The LRL had accommodations for all the people and equipment that needed to be quarantined. “The astronauts were picked up in the ocean and they had to wear a special suit that was supposedly impervious to ‘lunar bugs,'” McLane said. “The astronauts were put into a modified Grumman Airstream trailer and delivered to Houston, trailer and all, waving at everyone through the windows, and talking to the president. They were taken to the Lunar Receiving Lab and placed in quarantine. It was comfortable in there, but the astronauts didn’t particularly like being in quarantine. We tried to limit the number of people who went into quarantine with them, but inevitably there were a few people– mostly ambitious secretaries and that sort of thing— who intentionally violated procedure and exposed themselves to the hypothetical lunar bugs and had move into the quarantine quarters.” The astronauts stayed in quarantine for three weeks.

First lunar samples arrive from Apollo 11.  Credit: NASA
First lunar samples arrive from Apollo 11. Credit: NASA

By the time Apollo 11 launched McLane had moved on to other projects. “My part of the organization was the engineering directorate, and I was only charged with determining the requirements for the facility and staffing the facility,” he said. “Once we reached the point where the design had come along and the staffing was pretty well up, leading the lab required someone with an interest in science as opposed to engineering.”

But he watched with interest as the first mission to the Moon unfolded. He even had a place in the Mission Control VIP viewing gallery for the launch, sitting just behind science-fiction writer Arthur C. Clarke.

Of course, it was determined that there were no “lunar bugs” and the quarantine requirement was dropped after Apollo 14. But the LRL safely stored, distributed and allowed for study of the lunar samples. In 1976 a portion of the samples were moved to Brooks Air Force Base in San Antonio, Texas for second-site storage.
The LRL building is currently occupied by NASA’s Life Sciences division. It contains biomedical and environment labs, and is used for experiments involving human adaptation to microgravity.

James C. McLane Jr today.  Photo courtesy of James McLane Jr.
James C. McLane Jr today. Photo courtesy of James McLane Jr.

The lessons learned from creating the LRL will certainly be used in preparing for the first Mars sample return mission. Now, 86 years of age, will McLane offer any words of advice?

“The best that I hear now is that the techniques of isolation we used wouldn’t be adequate for a sample coming back from Mars,” he said, “so somebody else has a big job on their hands.”

McLane will be attending a special Apollo 11 celebration at Johnson Space Center – “just for the old timers,” he said.

For more information on the history of the Lunar Receiving Lab, see NASA’s “Lunar Receiving Laboratory Project History.”

Additional source: “Moon Rocks and Moon Germs: A History of NASA’s Lunar Receiving Laboratory,” Astronautics and Aeronauts, Winter 2001.

Plane of the Ecliptic

Solar eclipse. Credit: NASA

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Plane of the ecliptic, also known as the ecliptic plane, is a phrase you will often hear in astronomy. A basic definition is that the plane of the ecliptic is the plane of the Earth’s orbit, but that does not mean much to most people. Space is a three-dimensional vacuum, which you can think of as a kind of pool with the planets suspended in it. The Earth orbits the Sun on a particular angle and its orbit is elliptical in shape. The orbit is often shown as an ellipse made of dotted lines with the Sun at its center. If you made this ellipse a solid surface and extended it infinitively, then you would have the plane of the ecliptic. Actually our entire Solar System can be thought of as flat because all of the planets’ orbits are near or on this plane.

The ecliptic plane is used as the main reference when describing the position of other celestial objects in our Solar System. The angle between the plane of the ecliptic and the plane of an orbit is called the inclination. Until it was stripped of its status as a planet, Pluto was the planet with the most extreme inclination – 17°. Mercury is the only other planet with a significant inclination of 7°. There is also a 7° inclination between the plane of the Sun’s equator and the ecliptic plane. There are other celestial bodies that have a much greater inclination than any of the planets, such as Eris with a 44° inclination or Pallas with a 34° inclination.

The ecliptic plane got its name from the fact that a solar eclipse can only happen when the Moon crosses this plane to block out the Sun. Our Moon crosses the ecliptic about twice a month. A solar eclipse occurs when a new Moon crosses the ecliptic, and a lunar eclipse occurs when a full Moon crosses it.

Seasons on Earth are caused by our planet’s axial tilt of 23.5°, which causes variations in the amount of sunlight different parts of the Earth receive. This goes for all the other planets too. For example, Uranus rotates on its side with an axial tilt of 97.8°, which results in extreme variations in its seasons. The eclipse is also home to the constellations of the zodiac. There are twelve constellations in the zodiac, which are important symbols in astrology and can also be found in the Chinese calendar.  Here’s a list of all the zodiac symbols.

Universe Today has a number of articles including Virgo one of the zodiac signs and axial tilt.

You should also check out these articles on the ecliptic plane and ecliptic facts for more information.

Do not forget to tune into Astronomy Cast’s episode about the planet’s orbits.

Reference:
NASA: The Path of the Sun, the Ecliptic

Minor Planets

Main Belt Asteroids
Ceres, the recently promoted dwarf planet in the asteroid belt is still too small to be easily seen by Hubble credit: NASA/ESA/STScI

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Minor planet is a term used to refer to a celestial object – that is not a planet or comet – which orbits the Sun. Found in 1801, Ceres, also known as a dwarf planet, was the first minor planet discovered. The term minor planet has been in use since the 1800’s. Planetoids, asteroids, and minor planets have all been used interchangeably, but the situation became even more confusing when the International Astronomical Union (IAU) committee reclassified minor planets and comets into the new categories of dwarf planets and small solar system bodies. At the same time, the IAU created a new definition of what a planet is, and Pluto was reclassified as a dwarf planet. Hydrostatic equilibrium – the ability to maintain a roughly spherical shape – is what separates dwarf planets from the more irregularly shaped small solar system bodies. The names become even more confusing because the IAU still recognizes the use of the term minor planets.

Minor planets are extremely common with over 400,000 registered and thousands more found each month. Approximately 15,000 minor planets have been given official names while the rest are numbered. When asteroids were first discovered, they were named after characters from Greek and Roman mythology like Ceres was. At first, astronomers thought that the asteroids, especially Ceres and Pallas were actually planets. Astronomers also created symbols for the first asteroids found. There were symbols created for 14 asteroids and some of them were very complex like Victoria’s symbol, which looks like a plant with three leaves growing out of an off center starburst. Soon, astronomers ran out of mythological names and started christening asteroids after television characters, famous people, and relatives of discoverers. Most names were feminine, attesting to an unnamed  tradition. As the numbers ran into the thousands, scientists started using their pets as inspiration. After an asteroid was named 2309 Mr. Spock, pet’s names were banned. That did not stop the oddness though because names such as 9007 James Bond and 6402 Chesirecat have been suggested and actually accepted.

There are a number of different categories that minor planets fall into including asteroids, Trans-Neptunian objects, and centaurs. There  are various types of asteroids, although most of them can be found in the asteroid belt, which is the region of space between Mars and Jupiter. Trans-Neptunian objects are celestial bodies found orbiting beyond Neptune, and centaurs are celestial bodies with unstable orbits located between Jupiter and Neptune. The categories also overlap, making classifying things a nightmare. For example, Ceres is a dwarf planet and minor planet, additionally it can also be classified as an asteroid.

Universe Today has a number of articles including astronomers find new minor planet and why Pluto is no lone a planet.

You can also check out these articles on asteroids and the solar system.

Astronomy Cast has an episode on the asteroid belt you will want to listen to.

Reference:
Wikipedia

Habitable Planet

Habitable zone

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The term “habitable planet” seems rather broad. Does it mean that it is habitable for humans? Is it merely capable of supporting some other form of life? Quite simply, planetary habitability refers to a planet’s ability to both develop and sustain life.

Unfortunately, scientists have had to base their calculations for a habitable planet on Earth’s characteristics and do some guesswork. Some of the factors that astronomers look at when evaluating a planet’s habitability are mass, surface characteristics, orbit, rotation, and geochemistry.

One of the most basic assumptions that astronomers make when searching for a habitable planet is that it has to be terrestrial. This means that the planet is composed mostly of rock and metal and has a solid surface. A gas giant on the other hand has no solid surface, which makes it an unlikely candidate for supporting life. Mass is also an important factor, because low mass planets have too little gravity to keep their atmosphere. They also do not have live volcanoes and other geologic activity, which helps temper the surface to support life, because they lose energy as a result of a small diameter. Planets with high orbital eccentricity – the irregularity of the orbit – have a greater fluctuation in surface temperatures because they are closer to the Sun at some points and much further away at other points in the orbit. In order to be habitable, a planet has to have a moderate rotation. If there is no axial tilt then there are no change of seasons, and if the axial tilt is too severe than the planet will have a difficult time achieving homeostasis – balance. Another assumption astronomers make when determining planetary habitability is that life on other planets will also be carbon-based. The four elements most important for life are oxygen, nitrogen, carbon, and hydrogen. With so many considerations, it is not surprising that scientists have a difficult time determining whether a planet can sustain life.

Astronomers are searching for habitable planets in other solar systems too. They have started by searching in the habitable zones of other solar systems. A habitable zone is the region in space with conditions most favorable for supporting life. Astronomers are unsure exactly what the extent of the habitable zone of our Solar System is. Earth is located in the center of it, but it may even extend as far as Mars, and it almost reaches Venus. The habitable zone and planetary habitability focus on carbon-based life, so they do not help predict other forms of life.

Universe Today has a number of articles you should take a look at including the habitable zone and number of habitable planets.

You should also check out habitable planets and habitable planets are common.

Astronomy Cast has an episode on the search for water on Mars, which tells why finding water is a clue to finding life.