Moon plays lead role in new astronomical technique

Lunar occultation sky maps of Cygnus X-1 obtained using the Lunar Prospector Gamma-Ray Spectrometer. The features correspond to the location of the Moon’s horizon, projected onto the celestial sphere (equatorial coordinates), during intervals when Cygnus X-1 rose and set relative to the spacecraft. Also shown is an illustration of the Lunar Prospector spacecraft. Credit: Richard S. Miller/UAH

A University of Alabama in Huntsville (UAH) professor and astrophysicist has detected the first high-energy astrophysical source from the moon.

The detection was part of a proof-of-principle effort to verify a new paradigm: using an instrument in lunar orbit and the unique characteristics of the moon for nuclear astrophysics observations. The relative simplicity of this approach can give scientists an effective way to study the universe that is less expensive than other techniques without sacrificing performance, says UAH’s Dr. Richard S. Miller, who led its development and testing.

The technique is useful for detecting and characterizing objects in the universe whose properties change in time, Dr. Miller says. “This type of ‘time domain’ astrophysics is a new and evolving discipline in which variability gives insights into the nature of cosmic processes, helping us probe supernovae, explore black holes and the life cycle of matter and energy in the galaxy and beyond.”

The Lunar Occultation Technique utilizes the occultation, or eclipses, of a cosmic source by the moon to take gamma ray “snapshots” of the universe beyond.

“The pattern of eclipses is unique for every sky location since it depends only on the relative orientation of the moon, spacecraft, and the position in the sky of interest,” says Dr. Miller. “The technique gives optimal performance around airless planetary bodies, which is why we’ve gone to the moon. In addition, we have developed a new data analysis toolbox that allows the occultation data to be rapidly studied to identify the specific cosmic sources and characterize their radiation output.”

Validation of the technique was an important step supporting the Lunar Occultation Explorer (LOX), a dedicated mission concept being developed for future consideration as part of NASA’s Medium-class Explorer (MIDEX) program. Missions in this program have a maximum price tag of $250 million, and Dr. Miller says LOX is expected to be a relative bargain compared to traditional techniques designed to address the same science, which he says are complex and may require development of technologies that do not currently exist.

“The challenge of those big technology driven, traditional approaches is what got me thinking, ‘How can we do the same science in a more cost-effective way?'” says Dr. Miller. “While the instrument that will orbit the moon will be fairly large, it will be not be nearly as complex as other large telescopes that seek to probe this part of the electromagnetic spectrum. LOX is analogous to a large planetary spacecraft, and we have extensive experience operating similar smaller instruments at the moon and elsewhere.”
Dr. Miller joined with co-author Dr. David Lawrence of the Johns Hopkins University Applied Physics Laboratory to prove the technique by repurposing data from the NASA Lunar Prospector’s Gamma Ray Spectrometer (LP-GRS), which orbited the moon for a year and a half back in 1998 and 1999. Dr. Lawrence has led many lunar science analyses using LP-GRS data.

“Encoded in these data is the pattern of occultations generated by the moon,” Dr. Miller says. “Using the pattern of eclipses, we can determine whether a gamma ray source exists at any location in the sky.”

The original purpose of the Lunar Prospector was to study the elemental composition of the lunar surface, but the scientists instead used the data it collected to look skyward. Doing so, they identified the first astrophysical source ever detected from the moon, Cygnus X-1, a well-known galactic x-ray source thought to include a black hole.

“We didn’t discover Cygnus X-1, but rather, we used it as a validation – a test,” Dr. Miller says. “Could we see the source? Using this technique, we absolutely did.”

The research, which was accepted in just five days for publication in “Astrophysical Journal Letters,” succeeded in detecting the source, localizing it in the sky, and monitoring it over a six-month period.

“Those are three of the key elements of doing time domain astronomy,” Dr. Miller says. “Understanding the variation in time is critical to understanding the nature of the sources.”

The work continues several years of lunar science research Dr. Miller has conducted with the goal of developing the moon for use in astrophysics.

“A key benefit of the moon in astrophysics is that it has no atmosphere or magnetosphere,” which can impact data quality, says Dr. Miller. “It also has a relatively stable and well-understood radiation background. I believe this gives us a real opportunity to think out of the box with this new approach. It supports important astrophysics goals, overcomes technical and cost challenges of other techniques and ultimately helps further establish the moon as a platform for science.”

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Hubble finds universe may be expanding faster than expected

This illustration shows the three steps astronomers used to measure the universe's expansion rate to an unprecedented accuracy, reducing the total uncertainty to 2.4 percent. Astronomers made the measurements by streamlining and strengthening the construction of the cosmic distance ladder, which is used to measure accurate distances to galaxies near and far from Earth. Beginning at left, astronomers use Hubble to measure the distances to a class of pulsating stars called Cepheid variables, employing a basic tool of geometry called parallax. This is the same technique that surveyors use to measure distances on Earth. Once astronomers calibrate the Cepheids' true brightness, they can use them as cosmic yardsticks to measure distances to galaxies much farther away than they can with the parallax technique. The rate at which Cepheids pulsate provides an additional fine-tuning to the true brightness, with slower pulses for brighter Cepheids. The astronomers compare the calibrated true brightness values with the stars' apparent brightness, as seen from Earth, to determine accurate distances. Once the Cepheids are calibrated, astronomers move beyond our Milky Way to nearby galaxies (shown at center). They look for galaxies that contain Cepheid stars and another reliable yardstick, Type Ia supernovae, exploding stars that flare with the same amount of brightness. The astronomers use the Cepheids to measure the true brightness of the supernovae in each host galaxy. From these measurements, the astronomers determine the galaxies' distances. They then look for supernovae in galaxies located even farther away from Earth. Unlike Cepheids, Type Ia supernovae are brilliant enough to be seen from relatively longer distances. The astronomers compare the true and apparent brightness of distant supernovae to measure out to the distance where the expansion of the universe can be seen (shown at right). They compare those distance measurements with how the light from the supernovae is stretched to longer wavelengths by the expansion of space. They use these two values to calculate how fast the universe expands with time, called the Hubble constant. Credit: NASA, ESA, A. Feild (STScI), and A. Riess (STScI/JHU) 

Astronomers using NASA’s Hubble Space Telescope have discovered that the universe is expanding 5 percent to 9 percent faster than expected.

“This surprising finding may be an important clue to understanding those mysterious parts of the universe that make up 95 percent of everything and don’t emit light, such as dark energy, dark matter, and dark radiation,” said study leader and Nobel Laureate Adam Riess of the Space Telescope Science Institute and The Johns Hopkins University, both in Baltimore, Maryland.

The results will appear in an upcoming issue of The Astrophysical Journal.

Riess’ team made the discovery by refining the universe’s current expansion rate to unprecedented accuracy, reducing the uncertainty to only 2.4 percent. The team made the refinements by developing innovative techniques that improved the precision of distance measurements to faraway galaxies.

The team looked for galaxies containing both Cepheid stars and Type Ia supernovae. Cepheid stars pulsate at rates that correspond to their true brightness, which can be compared with their apparent brightness as seen from Earth to accurately determine their distance. Type Ia supernovae, another commonly used cosmic yardstick, are exploding stars that flare with the same brightness and are brilliant enough to be seen from relatively longer distances.

By measuring about 2,400 Cepheid stars in 19 galaxies and comparing the observed brightness of both types of stars, they accurately measured their true brightness and calculated distances to roughly 300 Type Ia supernovae in far-flung galaxies.

The team compared those distances with the expansion of space as measured by the stretching of light from receding galaxies. The team used these two values to calculate how fast the universe expands with time, or the Hubble constant.

The improved Hubble constant value is 73.2 kilometers per second per megaparsec. (A megaparsec equals 3.26 million light-years.) The new value means the distance between cosmic objects will double in another 9.8 billion years.

This refined calibration presents a puzzle, however, because it does not quite match the expansion rate predicted for the universe from its trajectory seen shortly after the big bang. Measurements of the afterglow from the big bang by NASA’s Wilkinson Microwave Anisotropy Probe (WMAP) and the European Space Agency’s Planck satellite mission yield predictions for the Hubble constant that are 5 percent and 9 percent smaller, respectively.

“If we know the initial amounts of stuff in the universe, such as dark energy and dark matter, and we have the physics correct, then you can go from a measurement at the time shortly after the big bang and use that understanding to predict how fast the universe should be expanding today,” said Riess. “However, if this discrepancy holds up, it appears we may not have the right understanding, and it changes how big the Hubble constant should be today.”

Comparing the universe’s expansion rate with WMAP, Planck, and Hubble is like building a bridge, Riess explained. On the distant shore are the cosmic microwave background observations of the early universe. On the nearby shore are the measurements made by Riess’ team using Hubble.

“You start at two ends, and you expect to meet in the middle if all of your drawings are right and your measurements are right,” Riess said. “But now the ends are not quite meeting in the middle and we want to know why.”

There are a few possible explanations for the universe’s excessive speed. One possibility is that dark energy, already known to be accelerating the universe, may be shoving galaxies away from each other with even greater—or growing—strength.

Another idea is that the cosmos contained a new subatomic particle in its early history that traveled close to the speed of light. Such speedy particles are collectively referred to as “dark radiation” and include previously known particles like neutrinos. More energy from additional dark radiation could be throwing off the best efforts to predict today’s expansion rate from its post-big bang trajectory.

The boost in acceleration could also mean that dark matter possesses some weird, unexpected characteristics. Dark matter is the backbone of the universe upon which galaxies built themselves up into the large-scale structures seen today.

And finally, the speedier universe may be telling astronomers that Einstein’s theory of gravity is incomplete.

“We know so little about the dark parts of the universe, it’s important to measure how they push and pull on space over cosmic history,” said Lucas Macri of Texas A&M University in College Station, a key collaborator on the study.

The Hubble observations were made with Hubble’s sharp-eyed Wide Field Camera 3 (WFC3), and were conducted by the Supernova H0 for the Equation of State (SH0ES) team, which works to refine the accuracy of the Hubble constant to a precision that allows for a better understanding of the universe’s behavior.

The SH0ES Team is still using Hubble to reduce the uncertainty in the Hubble constant even more, with a goal to reach an accuracy of 1 percent. Current telescopes such as the European Space Agency’s Gaia satellite, and future telescopes such as the James Webb Space Telescope (JWST), an infrared observatory, and the Wide Field Infrared Space Telescope (WFIRST), also could help astronomers make better measurements of the expansion rate.

Before Hubble was launched in 1990, the estimates of the Hubble constant varied by a factor of two. In the late 1990s the Hubble Space Telescope Key Project on the Extragalactic Distance Scale refined the value of the Hubble constant to within an error of only 10 percent, accomplishing one of the telescope’s key goals. The SH0ES team has reduced the uncertainty in the Hubble constant value by 76 percent since beginning its quest in 2005.

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Dozens of new variable stars found in a dense globular cluster

Messier 54 as imaged by the Hubble Space Telescope. Credit: ESA/Hubble & NASA
June 1, 2016 by Tomasz Nowakowski

(Phys.org)—Located some 87,000 light years away, a dense globular cluster named Messier 54 (also known as NGC 6715) is a real gold mine for astronomers. Recently, an international team has discovered dozens of new variable stars in this cluster, improving the stellar census of Messier 54. The findings were presented in a paper published online on May 23 on the arXiv pre-print server.

The team, led by Roberto Figuera Jaimes of the European Southern Observatory (ESO), made use of the Danish 1.54 meter Telescope at ESO’s La Silla observatory in Chile in order to obtain high-precision photometry of the very crowded central region of Messier 54. They have analyzed the light curves of 1,405 stars in this stellar system. Their observations were highly successful, resulting in the discovery 67 new variable stars.

“A total of 1,405 stars in the field covered by the reference image were statistically studied for variable star detection. (…) We discovered 67 new variable stars, which consist of 30 RR Lyrae, 21 long-period irregular, three semi-regular, one W Virginis, one eclipsing binary, and 11 unclassified stars,” the researchers wrote in the paper.

RR Lyrae variables are pulsating horizontal branch stars of spectral class A or F, with a mass of around 0.5 solar masses. They are used as standard candles to measure extragalactic distances. Among the group of 30 newly detected stars of this class, the team was able to discern that 17 of them are pulsating in the fundamental mode, eight are pulsating in the first overtone, one is a double-mode pulsator and four remain with an uncertain subtype. The periods of the newly found stars in the RR Lyrae group range from 0.28 to 0.76 days with amplitudes between 0.06 and 1.69 mag.

However, according to Jaimes and his colleagues, the most intriguing addition to the stellar catalog of Messier 54 is the W Virginis variable. The scientists noted that this star’s variation does not follow the pattern found for the other variable stars studied and classified in their work. They found a very well phased light curve with a period of about 14.8 days and an amplitude of 0.71 mag.

“This is the only bright variable star on the blue side of the color-magnitude diagram far away from the red giant branch,” the paper reads.

The scientists revealed that the amplitudes of 21 long-period irregular variables range from 0.05 to 0.46 mag, however they found no clear periods for these stars. According to the research, the amplitudes of the three semi-regular stars range from 0.04 to 0.45 mag and their periods span between 20 and 150 days. The eclipsing binary’s period was found to be approximately 0.2 days, while the amplitude of the deeper eclipse is of the order of 0.8 mag and the amplitude of the secondary eclipse equals 0.5 mag.

The researchers concluded that their findings, especially regarding detecting new RR Lyrae variables, confirm that Messier 54 is of intermediate Oosterhoff type. The so-called ‘Oosterhoff groups’ are two populations of globular clusters, nearly as old as the universe itself, that have weak lines of metallic elements, though they differ in their metal abundances.

Read more at: http://phys.org/news/2016-06-dozens-variable-stars-dense-globular.html#jCp