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  • richardmitnick 3:53 pm on May 23, 2023 Permalink | Reply
    Tags: "How Artificial Intelligence is helping astronomers", AI algorithms have begun helping astronomers tame massive data sets and discover new knowledge about the universe., , , Better telescopes and more data, , Ground based Astronomy, , ,   

    From “EarthSky” : “How Artificial Intelligence is helping astronomers” 

    1

    From “EarthSky”

    5.23.23
    Chris Impey | University of Arizona

    1

    AI is helping astronomers

    “The famous first image of a black hole just got two times sharper.

    2
    Researchers used computer simulations of black holes and machine learning to generate a revised version (right) of the famous first image of a black hole that was released back in 2019 (left). Medeiros et al 2023 [below]

    A research team used artificial intelligence to dramatically improve upon its first image from 2019, which now shows the black hole at the center of the Messier 87 galaxy as darker and bigger than the first image depicted.

    I’m an astronomer who studies and has written about cosmology, black holes and exoplanets. Astronomers have been using AI for decades. In fact, in 1990, astronomers from the University of Arizona, where I am a professor, were among the first to use a type of AI called a neural network to study the shapes of galaxies.

    Since then, AI has spread into every field of astronomy. As the technology has become more powerful, AI algorithms have begun helping astronomers tame massive data sets and discover new knowledge about the universe.

    Better telescopes and more data

    As long as astronomy has been a science, it has involved trying to make sense of the multitude of objects in the night sky. That was relatively simple when the only tools were the unaided eye or a simple telescope, and all that we could see were a few thousand stars and a handful of planets.

    A hundred years ago, Edwin Hubble used newly built telescopes to show that the universe teems with not just stars and clouds of gas, but countless galaxies.

    Edwin Hubble Cepheid variable moving with Messier 31 at the 100 inch Hooker telescope on Mt Wilson, California.

    As telescopes have continued to improve, the sheer number of celestial objects humans can see and the amount of data astronomers need to sort through have both grown exponentially, too.

    For example, the soon-to-be-completed Vera Rubin Observatory in Chile will make images so large that it would take 1,500 high-definition TV screens to view each one in its entirety.

    Over 10 years it is expected to generate 0.5 exabytes of data – about 50,000 times the amount of information held in all of the books contained within the Library of Congress.

    There are 20 telescopes with mirrors larger than 20 feet (6 meters) in diameter.

    Some examples:

    AI algorithms are the only way astronomers could ever hope to work through all of the data available to them today. There are a number of ways AI is proving useful in processing this data.

    3
    One of the earliest uses of AI in astronomy was to pick out the multitude of faint galaxies hidden in the background of images. Image credit J. Rigby via NASA/ESA/CSA Webb. J.CC BY.

    Picking out patterns

    Astronomy often involves looking for needles in a haystack. About 99% of the pixels in an astronomical image contain background radiation, light from other sources or the blackness of space. Only 1% have the subtle shapes of faint galaxies.

    AI algorithms – in particular, neural networks that use many interconnected nodes and learn to recognize patterns – are perfectly suited for picking out the patterns of galaxies. Astronomers began using neural networks to classify galaxies in the early 2010s. Now the algorithms are so effective that they can classify galaxies with an accuracy of 98%.

    We’ve seen this in other areas of astronomy. Astronomers working on SETI, the Search for Extraterrestrial Intelligence, use radio telescopes to look for signals from distant civilizations. Early on, radio astronomers scanned charts by eye to look for unexplained anomalies. More recently, researchers harnessed 150,000 personal computers and 1.8 million citizen scientists to look for artificial radio signals. Now, researchers are using AI to sift through reams of data much more quickly and thoroughly than people can. This has allowed SETI efforts to cover more ground while also greatly reducing the number of false positive signals.

    Another example is the search for exoplanets. Astronomers discovered most of the 5,300 known exoplanets by measuring a dip in the amount of light coming from a star when a planet passes in front of it. AI tools can now pick out the signs of an exoplanet with 96% accuracy.

    3
    AI tools can help astronomers discover new exoplanets like TRAPPIST-1 b. Image credit: Joseph Olmsted (STScI) NASA/ ESA/ CSA Webb , CC BY.

    Making new discoveries

    AI has proved itself to be excellent at identifying known objects – like galaxies or exoplanets – that astronomers tell it to look for. But it is also quite powerful at finding objects or phenomena that are theorized but have not yet been discovered in the real world.

    Teams have used this approach to detect new exoplanets, learn about the ancestral stars that led to the formation and growth of the Milky Way, and predict the signatures of new types of gravitational waves.

    To do this, astronomers first use AI to convert theoretical models into observational signatures, including realistic levels of noise. Then they use machine learning to sharpen the ability of AI to detect the predicted phenomena.

    Finally, radio astronomers have also been using AI algorithms to sift through signals that don’t correspond to known phenomena. Recently a team from South Africa found a unique object that may be a remnant of the explosive merging of two supermassive black holes. If this proves to be true, the data will allow a new test of general relativity: Albert Einstein’s description of space-time.

    Not well explicated, this might be either of the two objects below, found with MeerkAT or HERA.

    5
    A portion of the field centered on GRS 1915+105 as seen by the MeerKAT radio telescope at 1.28 GHz. Credit: Motta et al., 2023.

    6
    MeerKAT 1.3 GHz radio continuum image of a newly discovered double relic associated with the galaxy cluster PSZ2 G277.93+12.34. Credit: Koribalski et al, 2023.

    Making predictions and plugging holes

    As in many areas of life recently, generative AI and large language models like ChatGPT are also making waves in the astronomy world.

    The team that created the first image of a black hole in 2019 used a generative AI to produce its new image [The Astrophysical Journal Letters (below)]. To do so, it first taught an AI how to recognize black holes by feeding it simulations of many kinds of black holes. Then, the team used the AI model it had built to fill in gaps in the massive amount of data collected by the radio telescopes on the black hole M87.

    Using this simulated data, the team was able to create a new image that is two times sharper than the original and is fully consistent with the predictions of general relativity.

    Astronomers are also turning to AI to help tame the complexity of modern research. A team from the Harvard-Smithsonian Center for Astrophysics created a language model called astroBERT to read and organize 15 million scientific papers on astronomy. Another team, based at NASA, has even proposed using AI to prioritize astronomy projects, a process that astronomers engage in every 10 years.

    As AI has progressed, it has become an essential tool for astronomers. As telescopes get better, as data sets get larger and as AIs continue to improve, it is likely that this technology will play a central role in future discoveries about the universe.

    The Astrophysical Journal
    The Astrophysical Journal Letters
    6
    Image of black hole M87* reconstructed to an amazing higher resolution using AI. https://www.360onhistory.com
    More instructive images are available in the science papers.

    See the full article here .

    Comments are invited and will be appreciated, especially if the reader finds any errors which I can correct. Use “Reply”.


    five-ways-keep-your-child-safe-school-shootings
    Please help promote STEM in your local schools.


    Stem Education Coalition

    Deborah Byrd created the EarthSky radio series in 1991 and founded EarthSky.org in 1994. Today, she serves as Editor-in-Chief of this website. She has won a galaxy of awards from the broadcasting and science communities, including having an asteroid named 3505 Byrd in her honor. A science communicator and educator since 1976, Byrd believes in science as a force for good in the world and a vital tool for the 21st century. “Being an EarthSky editor is like hosting a big global party for cool nature-lovers,” she says.

     
  • richardmitnick 10:56 am on May 3, 2023 Permalink | Reply
    Tags: , , , , Ground based Astronomy, ,   

    From The California Institute of Technology: “Star Eats Planet and Brightens Dramatically” 

    Caltech Logo

    From The California Institute of Technology

    5.3.23
    Whitney Clavin
    (626) 395‑1944
    wclavin@caltech.edu

    For the first time, astronomers have caught a star in the act of swallowing a planet whole. The sun-like star, called ZTF SLRN-2020, lies about 15,000 light-years away in our galaxy and is thought to have engulfed a hot gas giant about the size of Jupiter or smaller. Scientists already knew that older stars will, as they puff up with age, ultimately ingest their inner orbiting planets. Our own sun is predicted to do so in 5 billion years, consuming Mercury, Venus, and likely Earth. But nobody had seen direct evidence for such a remarkable scenario until now.

    “The confirmation that sun-like stars engulf inner planets provides us with a missing link in our understanding of the fates of solar systems, including our own,” says Kishalay De (MS ’18, PhD ’21), a postdoctoral scholar at MIT and lead author of a new study about the findings in the journal Nature [below].

    1
    This artist’s impression shows a doomed planet skimming the surface of its star. Astronomers used a combination of telescopes to spot the first direct evidence of an aging, bloated sun-like star, like the one pictured here, engulfing its planet. These telescopes included the Zwicky Transient Facility (ZTF) at Caltech’s Palomar Observatory, the W.M. Keck Observatory, and NASA’s NEOWISE mission.


    Planetary Death Spiral.

    The plump star was first spotted by Zwicky Transient Facility, or ZTF, a National Science Foundation–funded instrument that scans the skies every night from Caltech’s Samuel Oschin Telescope at Palomar Observatory near San Diego. ZTF observations showed that the star had dramatically brightened and begun to fade in a period of about a week. At first, De thought this variable star might have resulted from a nova explosion, which occurs when a dead star called a white dwarf steals matter from its companion star. But follow-up observations with the W. M. Keck Observatory atop Maunakea in Hawaiʻi revealed something else was going on.

    “I had been looking for erupting stars called novae,” De says. “But the Keck data indicated that the star was not lighting up hot gas as is expected for novae. I couldn’t make any sense of it.”

    De, who was then a graduate student at Caltech, put the object aside to finish his PhD thesis and came back to it about a year later after he had moved to MIT. He and his colleagues then obtained infrared data from a camera at Palomar’s Hale Telescope called WIRC (Wide-field Infrared Camera), “and that’s when things got really interesting,” he says.

    Those observations showed that the star was brightening over time in not only optical light as ZTF had observed but also in infrared light, which indicates the presence of dust. The researchers then turned to NASA’s NEOWISE space telescope in search of more clues. NEOWISE, formerly known as WISE (Wide-field Infrared Survey Explorer), has been scanning the skies regularly since shortly after its launch in 2009. NEOWISE detected the star brightening in infrared light about nine months before ZTF caught the extreme rise in optical light. Even now, after the optical light has faded, NEOWISE continues to pick up infrared light from the star.

    “The infrared observations were one of the main clues that we were looking at a star engulfing a planet,” says Viraj Karambelkar (MS ’21), a grad student at Caltech and co-author of the study.

    Once the science team put all the evidence together, they realized that the dust they were seeing with NEOWISE was being generated as a planet spiraled into the star’s puffy atmosphere. Like other older stars, the star had begun to expand in size as it aged, bringing it closer to the orbiting planet. As the planet skimmed the surface of the star, it pulled hot gas off the star that then drifted outward and cooled, forming dust. In addition, material from the disintegrating planet blew outward, also forming dust.

    What happened next, according to the astronomers, triggered the flare of optical light seen by ZTF.

    “The planet plunged into the core of the star and got swallowed whole. As it was doing this, energy was transferred to the star,” De explains. “The star blew off its outer layers to get rid of the energy. It expanded and brightened, and the brightening is what ZTF registered.”

    Some of this expanding stellar material then escaped from the star and traveled outward. Like the boiled-off layers of the star and planet that previously drifted outward, this material also cooled to form dust.

    NEOWISE is detecting the infrared glow of all the newly minted dust.

    “NEOWISE data are a treasure trove,” says co-author Mansi Kasliwal (MS ’07, PhD ’11), professor of astronomy at Caltech and a co-investigator on the ZTF project. “ZTF caught the event, which is what it excels at, while NEOWISE and other telescopes all helped us figure out what is going on.”

    The planetary engulfment is similar to what happens when two stars merge, events called red novae. Stars in our universe often form in pairs. Over time, as one star ages and expands faster than its companion, it can essentially ingest its partner. Twenty of these star mergers have been detected to date by ZTF and other instruments, mostly in galaxies beyond the Milky Way.

    “Star mergers are thousands of times brighter than this event,” says Karambelkar, who has observed eight of these eruptions using ZTF as part of his PhD thesis. “This was another clue that we were looking at a planet being eaten by its star. The level of brightening was much fainter due to the small size of the planet.”

    “This is just spectacular,” Kasliwal adds. “We are still amazed that we caught a star in the act of ingesting its planet, something our own sun will do to its inner planets. That’s a long time from now, in five billion years, so we don’t have to worry just yet.”

    Nature

    See the full article here .

    See also the full article from The W.M. Keck Observatory here.

    Comments are invited and will be appreciated, especially if the reader finds any errors which I can correct. Use “Reply”.


    five-ways-keep-your-child-safe-school-shootings


    Please help promote STEM in your local schools.

    Stem Education Coalition

    The California Institute of Technology is a private research university in Pasadena, California. The university is known for its strength in science and engineering, and is one among a small group of institutes of technology in the United States which is primarily devoted to the instruction of pure and applied sciences.

    The California Institute of Technology was founded as a preparatory and vocational school by Amos G. Throop in 1891 and began attracting influential scientists such as George Ellery Hale, Arthur Amos Noyes, and Robert Andrews Millikan in the early 20th century. The vocational and preparatory schools were disbanded and spun off in 1910 and the college assumed its present name in 1920. In 1934, The California Institute of Technology was elected to the Association of American Universities, and the antecedents of National Aeronautics and Space Administration ‘s Jet Propulsion Laboratory, which The California Institute of Technology continues to manage and operate, were established between 1936 and 1943 under Theodore von Kármán.

    The California Institute of Technology has six academic divisions with strong emphasis on science and engineering. Its 124-acre (50 ha) primary campus is located approximately 11 mi (18 km) northeast of downtown Los Angeles. First-year students are required to live on campus, and 95% of undergraduates remain in the on-campus House System at The California Institute of Technology. Although The California Institute of Technology has a strong tradition of practical jokes and pranks, student life is governed by an honor code which allows faculty to assign take-home examinations. The The California Institute of Technology Beavers compete in 13 intercollegiate sports in the NCAA Division III’s Southern California Intercollegiate Athletic Conference (SCIAC).

    As of October 2020, there are 76 Nobel laureates who have been affiliated with The California Institute of Technology, including 40 alumni and faculty members (41 prizes, with chemist Linus Pauling being the only individual in history to win two unshared prizes). In addition, 4 Fields Medalists and 6 Turing Award winners have been affiliated with The California Institute of Technology. There are 8 Crafoord Laureates and 56 non-emeritus faculty members (as well as many emeritus faculty members) who have been elected to one of the United States National Academies. Four Chief Scientists of the U.S. Air Force and 71 have won the United States National Medal of Science or Technology. Numerous faculty members are associated with the Howard Hughes Medical Institute as well as National Aeronautics and Space Administration. According to a 2015 Pomona College study, The California Institute of Technology ranked number one in the U.S. for the percentage of its graduates who go on to earn a PhD.

    Research

    The California Institute of Technology is classified among “R1: Doctoral Universities – Very High Research Activity”. Caltech was elected to The Association of American Universities in 1934 and remains a research university with “very high” research activity, primarily in STEM fields. The largest federal agencies contributing to research are National Aeronautics and Space Administration; National Science Foundation; Department of Health and Human Services; Department of Defense, and Department of Energy.

    In 2005, The California Institute of Technology had 739,000 square feet (68,700 m^2) dedicated to research: 330,000 square feet (30,700 m^2) to physical sciences, 163,000 square feet (15,100 m^2) to engineering, and 160,000 square feet (14,900 m^2) to biological sciences.

    In addition to managing NASA-JPL/Caltech , The California Institute of Technology also operates the Caltech Palomar Observatory; The Owens Valley Radio Observatory;the Caltech Submillimeter Observatory; the W. M. Keck Observatory at the Mauna Kea Observatory; the Laser Interferometer Gravitational-Wave Observatory at Livingston, Louisiana and Hanford, Washington; and Kerckhoff Marine Laboratory in Corona del Mar, California. The Institute launched the Kavli Nanoscience Institute at The California Institute of Technology in 2006; the Keck Institute for Space Studies in 2008; and is also the current home for the Einstein Papers Project. The Spitzer Science Center, part of the Infrared Processing and Analysis Center located on The California Institute of Technology campus, is the data analysis and community support center for NASA’s Spitzer Infrared Space Telescope [no longer in service].


    The California Institute of Technology partnered with University of California-Los Angeles to establish a Joint Center for Translational Medicine (UCLA-Caltech JCTM), which conducts experimental research into clinical applications, including the diagnosis and treatment of diseases such as cancer.

    The California Institute of Technology operates several Total Carbon Column Observing Network stations as part of an international collaborative effort of measuring greenhouse gases globally. One station is on campus.

     
  • richardmitnick 10:54 am on May 3, 2023 Permalink | Reply
    Tags: , Astronomers Spot First Direct Evidence of a Star Engulfing Its Planet., , , , Ground based Astronomy, ,   

    From The W.M. Keck Observatory: “Star Eats Planet and Brightens Dramatically” 

    W.M. Keck Observatory two ten meter telescopes operated by California Institute of Technology and The University of California, at Mauna Kea Observatory, Hawai’i, altitude 4,207 m (13,802 ft). Credit: Caltech.

    Keck Laser Guide Star Adaptive Optics on two 10 meter Keck Observatory telescopes, Mauna Kea Hawai’i, altitude 4,207 m (13,802 ft). Credit: Caltech.

    Mauna Kea Observatories Hawai’i altitude 4,213 m (13,822 ft).

    From The W.M. Keck Observatory

    5.3.23

    Mari-Ela Chock (She/Her/Hers)
    Communications Officer
    Phone: 808.554.0567
    Email: mchock@keck.hawaii.edu

    Astronomers Spot First Direct Evidence of a Star Engulfing Its Planet.

    2
    This artist’s impression shows a doomed planet skimming the surface of its star. Astronomers used a combination of telescopes to spot the first direct evidence of an aging, bloated sun-like star, like the one pictured here, engulfing its planet. These telescopes included the Zwicky Transient Facility (ZTF) at Caltech’s Palomar Observatory, the W.M. Keck Observatory, and NASA’s NEOWISE mission.

    The aging star depicted here, called ZTF SLRN-2020, is roughly 10 billion years old. It had begun to inflate over hundreds of thousands of years as it transformed into a red giant, and, as a result, inched closer to its inner planet. According to astronomers, when the planet was almost touching the surface of the star, the increasing frictional forces caused the planet to rapidly spiral inward. Eventually, on timescales that are not certain, the planet plunged into the core of the star. When that happened, the star inflated to four times its size and brightened by a factor of more than a hundred. ZTF SLRN-2020 lies about 15,000 light-years away in the constellation Aquila. Credit: K. Miller/R. Hurt (Caltech/IPAC)

    For the first time, astronomers have caught a star in the act of swallowing a planet whole. The sun-like star, called ZTF SLRN-2020, lies about 15,000 light-years away in our Milky Way galaxy and is thought to have engulfed a hot gas giant planet about the size of Jupiter or smaller.

    Scientists already knew that older stars will, as they puff up with age, ultimately ingest their inner orbiting planets. Our own Sun is predicted to do so in 5 billion years, consuming Mercury, Venus, and likely Earth. But nobody had seen direct evidence for such a remarkable scenario until now.

    “The confirmation that sun-like stars engulf inner planets provides us with a missing link in our understanding of the fates of solar systems, including our own,” says Kishalay De, a postdoctoral scholar at MIT and lead author of a new study about this so-called “Death Star” publishing May 4, Star Wars Day, in the journal Nature.

    The plump star was first spotted by Zwicky Transient Facility, or ZTF, a National Science Foundation-funded instrument that scans the skies every night from Caltech’s Samuel Oschin Telescope at Palomar Observatory near San Diego. ZTF observations showed the star had dramatically brightened and begun to fade in a period of about a week.

    At first, De thought this variable star might have resulted from a nova explosion, which occurs when a dead star called a white dwarf steals matter from its companion star. But follow-up observations with the W. M. Keck Observatory atop Mauna Kea on Hawaiʻi Island revealed something else was going on.
    ===
    “I had been looking for erupting stars called novae,” De says. “But the Keck data indicated that the star was not lighting up hot gas as is expected for novae. I couldn’t make any sense of it.”

    Keck Observatory’s Low Resolution Imaging Spectrometer (LRIS) [below] confirmed the chemical composition and temperature of the gas, which indicated the outburst was surrounded by cooler material.

    De, who was then a graduate student at Caltech, said he put the object aside to finish his PhD thesis and came back to it about a year later after he had moved to MIT. He and his colleagues then obtained infrared data from a camera at Palomar’s Hale Telescope called WIRC (Wide-field Infrared Camera), “and that’s when things got really interesting,” he says.

    Those observations showed the star was brightening over time in not only optical light as ZTF had observed but also in infrared light, which indicates the presence of dust.

    The researchers then turned to NASA’s NEOWISE space telescope in search of more clues. NEOWISE, formerly known as WISE (Wide-field Infrared Survey Explorer), has been scanning the skies regularly since shortly after its launch in 2009. NEOWISE detected the star brightening in infrared light about nine months before ZTF caught the extreme rise in optical light. Even now, after the optical light has faded, NEOWISE continues to pick up infrared light from the star.

    “The infrared observations were one of the main clues that we were looking at a star engulfing a planet,” says Viraj Karambelkar, a grad student at Caltech and co-author of the study.

    Keck Observatory’s Near-Infrared Echellette Spectrograph (NIRES) confirmed that the aftermath was indeed surrounded by a layer of cool gas and dust.

    Once the science team put all the evidence together, they realized the dust they were seeing with NEOWISE was being generated as the planet spiraled into the star’s puffy atmosphere. Like other older stars, the star had begun to expand in size as it aged, bringing it closer to the orbiting planet. As the planet skimmed the surface of the star, it pulled hot gas off the star that then drifted outward and cooled, forming dust. In addition, material from the disintegrating planet blew outward, also forming dust.

    What happened next, according to the astronomers, triggered the flare of optical light seen by ZTF.

    For the first time, astronomers have caught a star in the act of engulfing its planet, an ill-fated encounter that will play out in our own solar system in 5 billion years. Animation credit: R. Hurt/K. Miller (Caltech/IPAC)

    “The planet plunged into the core of the star and got swallowed whole. As it was doing this, energy was transferred to the star,” De explains. “The star blew off its outer layers to get rid of the energy. It expanded and brightened, and the brightening is what ZTF registered.”

    Some of this expanding stellar material then escaped from the star and traveled outward. Like the boiled-off layers of the star and planet that previously drifted outward, this material also cooled to form dust.

    NEOWISE is detecting the infrared glow of all the newly minted dust.

    The planetary engulfment is similar to what happens when two stars merge, events called red novae. Stars in our universe often form in pairs. Over time, as one star ages and expands faster than its companion, it can essentially ingest its partner. 20 of these star mergers have been detected to date by ZTF and other instruments, mostly in galaxies beyond the Milky Way.

    “Star mergers are thousands of times brighter than this event,” says Karambelkar, who has observed eight of these eruptions using ZTF as part of his PhD thesis. “This was another clue that we were looking at a planet being eaten by its star. The level of brightening was much fainter due to the small size of the planet.”

    “This is just spectacular,” says co-author Mansi Kasliwal, professor of astronomy at Caltech and a co-investigator on the ZTF project. “We are still amazed that we caught a star in the act of ingesting its planet, something our own Sun will do to its inner planets. Though that’s a long time from now, in five billion years, so we don’t have to worry just yet.”

    The Nature study was funded by NASA, the National Science Foundation (NSF), and the Heising–Simons Foundation.
    https://www.nature.com/articles/s41586-023-05842-x
    __________________________________________________________________________________________________
    ABOUT LRIS

    The Low Resolution Imaging Spectrometer (LRIS) is a very versatile and ultra-sensitive visible-wavelength imager and spectrograph built at the California Institute of Technology by a team led by Prof. Bev Oke and Prof. Judy Cohen and commissioned in 1993. Since then it has seen two major upgrades to further enhance its capabilities: the addition of a second, blue arm optimized for shorter wavelengths of light and the installation of detectors that are much more sensitive at the longest (red) wavelengths. Each arm is optimized for the wavelengths it covers. This large range of wavelength coverage, combined with the instrument’s high sensitivity, allows the study of everything from comets (which have interesting features in the ultraviolet part of the spectrum), to the blue light from star formation, to the red light of very distant objects. LRIS also records the spectra of up to 50 objects simultaneously, especially useful for studies of clusters of galaxies in the most distant reaches, and earliest times, of the universe. LRIS was used in observing distant supernovae by astronomers who received the Nobel Prize in Physics in 2011 for research determining that the universe was speeding up in its expansion.

    ABOUT NIRES

    The Near-Infrared Echellette Spectrograph (NIRES) is a prism cross-dispersed near-infrared spectrograph built at the California Institute of Technology by a team led by Chief Instrument Scientist Keith Matthews and Prof. Tom Soifer. Commissioned in 2018, NIRES covers a large wavelength range at moderate spectral resolution for use on the Keck II telescope and observes extremely faint red objects found with the Spitzer and WISE infrared space telescopes, as well as brown dwarfs, high-redshift galaxies, and quasars. Support for this technology was generously provided by the Mt. Cuba Astronomical Foundation.

    See the full article here .

    See also the full article From Caltech here.

    Comments are invited and will be appreciated, especially if the reader finds any errors which I can correct. Use “Reply”.


    five-ways-keep-your-child-safe-school-shootings
    Please help promote STEM in your local schools.


    Stem Education Coalition

    Mission
    To advance the frontiers of astronomy and share our discoveries with the world.

    The W. M. Keck Observatory operates the largest, most scientifically productive telescopes on Earth. The two, 10-meter optical/infrared telescopes on the summit of Mauna Kea on the Island of Hawaii feature a suite of advanced instruments including imagers, multi-object spectrographs, high-resolution spectrographs, integral-field spectrometer and world-leading laser guide star adaptive optics systems. Keck Observatory is a private 501(c) 3 non-profit organization and a scientific partnership of the California Institute of Technology, the University of California and NASA.

    Today Keck Observatory is supported by both public funding sources and private philanthropy. As a 501(c)3, the organization is managed by The California Association for Research in Astronomy(CARA), whose Board of Directors includes representatives from the California Institute of Technologyand the University of California with liaisons to the board from The National Aeronautics and Space Agency and the Keck Foundation.


    Keck UCal

    Instrumentation

    Keck 1

    HIRES – The largest and most mechanically complex of the Keck’s main instruments, the High Resolution Echelle Spectrometer breaks up incoming starlight into its component colors to measure the precise intensity of each of thousands of color channels. Its spectral capabilities have resulted in many breakthrough discoveries, such as the detection of planets outside our solar system and direct evidence for a model of the Big Bang theory.

    Keck High-Resolution Echelle Spectrometer (HIRES), at the Keck I telescope.
    LRIS – The Low Resolution Imaging Spectrograph is a faint-light instrument capable of taking spectra and images of the most distant known objects in the universe. The instrument is equipped with a red arm and a blue arm to explore stellar populations of distant galaxies, active galactic nuclei, galactic clusters, and quasars.

    UCO Keck LRIS on Keck 1.

    VISIBLE BAND (0.3-1.0 Micron)

    MOSFIRE – The Multi-Object Spectrograph for Infrared Exploration gathers thousands of spectra from objects spanning a variety of distances, environments and physical conditions. What makes this huge, vacuum-cryogenic instrument unique is its ability to select up to 46 individual objects in the field of view and then record the infrared spectrum of all 46 objects simultaneously. When a new field is selected, a robotic mechanism inside the vacuum chamber reconfigures the distribution of tiny slits in the focal plane in under six minutes. Eight years in the making with First Light in 2012, MOSFIRE’s early performance results range from the discovery of ultra-cool, nearby substellar mass objects, to the detection of oxygen in young galaxies only 2 billion years after the Big Bang.

    Keck/MOSFIRE on Keck 1.

    OSIRIS – The OH-Suppressing Infrared Imaging Spectrograph is a near-infrared spectrograph for use with the Keck I adaptive optics system. OSIRIS takes spectra in a small field of view to provide a series of images at different wavelengths. The instrument allows astronomers to ignore wavelengths where the Earth’s atmosphere shines brightly due to emission from OH (hydroxl) molecules, thus allowing the detection of objects 10 times fainter than previously available.
    Keck OSIRIS on Keck 1.

    Keck 2

    DEIMOS – The Deep Extragalactic Imaging Multi-Object Spectrograph is the most advanced optical spectrograph in the world, capable of gathering spectra from 130 galaxies or more in a single exposure. In ‘Mega Mask’ mode, DEIMOS can take spectra of more than 1,200 objects at once, using a special narrow-band filter.

    Keck/DEIMOS on Keck 2.

    NIRSPEC – The Near Infrared Spectrometer studies very high redshift radio galaxies, the motions and types of stars located near the Galactic Center, the nature of brown dwarfs, the nuclear regions of dusty starburst galaxies, active galactic nuclei, interstellar chemistry, stellar physics, and solar-system science.

    NIRSPEC on Keck 2.

    ESI – The Echellette Spectrograph and Imager captures high-resolution spectra of very faint galaxies and quasars ranging from the blue to the infrared in a single exposure. It is a multimode instrument that allows users to switch among three modes during a night. It has produced some of the best non-AO images at the Observatory.

    KECK Echellette Spectrograph and Imager (ESI).

    KCWI – The Keck Cosmic Web Imager is designed to provide visible band, integral field spectroscopy with moderate to high spectral resolution, various fields of view and image resolution formats and excellent sky-subtraction. The astronomical seeing and large aperture of the telescope enables studies of the connection between galaxies and the gas in their dark matter halos, stellar relics, star clusters and lensed galaxies.

    Keck Cosmic Web Imager on Keck 2 schematic.

    Keck Cosmic Web Imager on Keck 2.

    NEAR-INFRARED (1-5 Micron)

    ADAPTIVE OPTICS – Adaptive optics senses and compensates for the atmospheric distortions of incoming starlight up to 1,000 times per second. This results in an improvement in image quality on fairly bright astronomical targets by a factor 10 to 20.

    LASER GUIDE STAR ADAPTIVE OPTICS [pictured above] – The Keck Laser Guide Star expands the range of available targets for study with both the Keck I and Keck II adaptive optics systems. They use sodium lasers to excite sodium atoms that naturally exist in the atmosphere 90 km (55 miles) above the Earth’s surface. The laser creates an “artificial star” that allows the Keck adaptive optics system to observe 70-80 percent of the targets in the sky, compared to the 1 percent accessible without the laser.

    NIRC-2/AO – The second generation Near Infrared Camera works with the Keck Adaptive Optics system to produce the highest-resolution ground-based images and spectroscopy in the 1-5 micron range. Typical programs include mapping surface features on solar system bodies, searching for planets around other stars, and analyzing the morphology of remote galaxies.

    Keck NIRC2 Camera on Keck 2.
    ABOUT NIRES
    The Near Infrared Echellette Spectrograph (NIRES) is a prism cross-dispersed near-infrared spectrograph built at the California Institute of Technology by a team led by Chief Instrument Scientist Keith Matthews and Prof. Tom Soifer. Commissioned in 2018, NIRES covers a large wavelength range at moderate spectral resolution for use on the Keck II telescope and observes extremely faint red objects found with the Spitzer and WISE infrared space telescopes, as well as brown dwarfs, high-redshift galaxies, and quasars.


    Future Instrumentation

    KCRM – The Keck Cosmic Reionization Mapper will complete the Keck Cosmic Web Imager (KCWI), the world’s most capable spectroscopic imager. The design for KCWI includes two separate channels to detect light in the blue and the red portions of the visible wavelength spectrum. KCWI-Blue was commissioned and started routine science observations in September 2017. The red channel of KCWI is KCRM; a powerful addition that will open a window for new discoveries at high redshifts.

    KCRM – Keck Cosmic Reionization Mapper KCRM on Keck 2.

    KPF – The Keck Planet Finder (KPF) will be the most advanced spectrometer of its kind in the world. The instrument is a fiber-fed high-resolution, two-channel cross-dispersed echelle spectrometer for the visible wavelengths and is designed for the Keck II telescope. KPF allows precise measurements of the mass-density relationship in Earth-like exoplanets, which will help astronomers identify planets around other stars that are capable of supporting life.

    KPF Keck Planet Finder on Keck 2.

     
  • richardmitnick 4:47 pm on May 1, 2023 Permalink | Reply
    Tags: "Combining observations to better visualize a superflare", , , , , Ground based Astronomy, Some stars have been seen releasing superflares more than 10 times larger than the largest solar flare ever seen on the sun., , The details of how superflares and prominence eruptions on stars occur have been unclear., The team succeeded in capturing a superflare with continuous and high temporal resolution observations., V1355 Orionis is located 400 light years away in the constellation Orion.   

    From The National Astronomical Observatory of Japan [国立天文台] (JP) Via “phys.org” : “Combining observations to better visualize a superflare” 

    From The National Astronomical Observatory of Japan [国立天文台] (JP)

    Via

    “phys.org”

    4.28.23

    1
    Artist’s impression of the superflare observed on one of the stars in the V1355 Orionis binary star system. The binary companion star is visible in the background on the right. Credit: NAOJ.

    A team of Japanese astronomers used simultaneous ground-based and space-based observations to capture a more complete picture of a superflare on a star. The observed flare started with a very massive, high-velocity prominence eruption. These results give us a better idea of how superflares and stellar prominence eruptions occur.

    Some stars have been seen releasing superflares more than 10 times larger than the largest solar flare ever seen on the sun. The hot ionized gas released by solar flares can influence the environment around the Earth, referred to as space weather. More powerful superflares must have an even greater impact on the evolution of any planets forming around the star, or the evolution of any life forming on those planets. But the details of how superflares and prominence eruptions on stars occur have been unclear.

    A team led by Shun Inoue at Kyoto University used the 3.8-m Seimei Telescope in Japan [below] and the Transiting Exoplanet Survey Satellite (TESS) to monitor the binary star system V1355 Orionis which is known to frequently release large-scale superflares.

    V1355 Orionis is located 400 light years away in the constellation Orion.

    The team succeeded in capturing a superflare with continuous, high temporal resolution observations. Data analysis shows that the superflare originated with a phenomenon known as a prominence eruption. Calculating the velocity of the eruption requires making some assumptions about aspects that aren’t directly observably, but even the most conservative estimates far exceed the escape velocity of the star (347 km/s), indicating that the prominence eruption was capable of breaking free of the star’s gravity and developing into Coronal Mass Ejections (CMEs). The prominence eruption was also one of the most massive ever observed, carrying trillions of tons of material.

    These results were published in The Astrophysical Journal.
    https://iopscience.iop.org/article/10.3847/1538-4357/acb7e8/pdf
    See the science paper for instructive material with images.

    See the full article here .

    Comments are invited and will be appreciated, especially if the reader finds any errors which I can correct. Use “Reply”.

    five-ways-keep-your-child-safe-school-shootings

    Please help promote STEM in your local schools.

    Stem Education Coalition

    The National Astronomical Observatory of Japan (NAOJ) [国立天文台] (JP) is an astronomical research organization comprising several facilities in Japan, as well as an observatory in Hawaii. It was established in 1988 as an amalgamation of three existing research organizations – the Tokyo Astronomical Observatory of The University of Tokyo [東京大学](JP), International Latitude Observatory of Mizusawa, and a part of Research Institute of Atmospherics of Nagoya University [名古屋大学](JP).

    In the 2004 reform of national research organizations, NAOJ became a division of the National Institutes of Natural Sciences .

    sft
    Solar Flare Telescope.

     
  • richardmitnick 11:48 am on April 22, 2023 Permalink | Reply
    Tags: "Making Better Measurements of the Composition of Galaxies", , , , Ground based Astronomy, Scientists are trying to measure the composition of gases inside galaxies., Scientists used optical and infrared astronomy to measure oxygen abundance in dwarf galaxy Markarian 71., , The ratio of oxygen to hydrogen can help astronomers understand how many and what kinds of stars are being formed in a distant object.,   

    From The University of California-Davis: “Making Better Measurements of the Composition of Galaxies” 

    UC Davis bloc

    From The University of California-Davis

    4.20.23
    Media Contacts:

    Yuguang Chen
    Physics and Astronomy
    yugchen@ucdavis.edu

    Tucker Jones
    Physics and Astronomy
    tdjones@ucdavis.edu

    Andy Fell
    News and Media Relations
    530-304-8888
    ahfell@ucdavis.edu

    1
    Composite image of dwarf galaxy Markarian 71, 11 million light years from Earth. Optical and infrared observations of Mrk71 resolve a question about two methods used to measure the composition of galaxies and could lead to improved studies with infrared space telescopes. (Hubble Space Telescope)

    A study using data from telescopes on Earth and in the sky resolves a problem plaguing astronomers working in the infrared and could help make better observations of the composition of the universe with the James Webb Space Telescope and other instruments. The work is published April 20 in Nature Astronomy [below].

    “We’re trying to measure the composition of gases inside galaxies,” said Yuguang Chen, a postdoctoral researcher working with Professor Tucker Jones in the Department of Physics and Astronomy at the University of California, Davis.

    Most elements other than hydrogen, helium and lithium are produced inside stars, so the composition and distribution of heavier elements — especially the ratio of oxygen to hydrogen — can help astronomers understand how many and what kinds of stars are being formed in a distant object.

    Astronomers use two methods to measure oxygen in a galaxy, but unfortunately, they give different results. One common method, collisionally excited lines, gives a strong signal, but the results are thought to be sensitive to temperature changes, Chen said. A second method uses a different set of lines, called recombination lines, which are fainter but not thought to be affected by temperature.

    The recombination line method consistently produces measurements about double those from collisionally excited lines. Scientists attribute the discrepancy to temperature fluctuations in gas clouds, but this has not been directly proven, Chen said.

    Chen, Jones and colleagues used optical and infrared astronomy to measure oxygen abundance in dwarf galaxy Markarian 71, about 11 million light years from Earth. They used archived data from the recently retired SOFIA flying telescope and the retired Herschel Space Observatory, as well as making observations with telescopes at the W.M. Keck Observatory in Mauna Kea, Hawai’i.

    SOFIA (Stratospheric Observatory For Infrared Astronomy) was a telescope mounted in a Boeing 747 aircraft. By flying at 38,000 to 45,000 feet, the aircraft could get above 99% of the water vapor in Earth’s atmosphere, which effectively blocks infrared light from deep space from reaching ground level. A joint project of NASA and the German space agency, SOFIA made its last operational flight in September 2022 and is now headed for a museum display in Tucson.

    The Herschel Space Observatory, named after astronomers William and Caroline Herschel, was an infrared space telescope operated by the European Space Agency. It was active from 2009 to 2013.

    A surprising result

    With data from these instruments, Chen and Jones examined oxygen abundance in Markarian 71 while correcting for temperature fluctuations. They found that the result from collisionally excited infrared lines was still 50% less than that from the recombination line method, even after eliminating the effect of temperature.

    “This result is very surprising to us,” Chen said. There is no consensus on an explanation for the discrepancy, he said. The team plans to look at additional objects to figure out what properties of galaxies correlate with this variation, Chen said.

    One of the goals of the James Webb Space Telescope, launched in 2022, is to make infrared observations of the composition of distant galaxies in the first billion years of the universe. The new results provide a framework for making these measurements with the JWST and the Atacama Large Millimeter Array in Chile.

    Additional co-authors on the paper are: Ryan Sanders and Erin Huntzinger, UC Davis; Dario Fadda, Jessica Sutter and Robert Minchin, SOFIA Science Center, NASA Ames Research Center; Peter Senchyna, Observatories of the Carnegie Institute for Science, Pasadena; Daniel Stark and Benjamin Weiner, Steward Observatory, University of Arizona; Justin Spilker, Texas A&M University; and Guido Roberts-Borsani, UCLA. The work was financially supported in part by NASA. SOFIA was jointly operated by the Universities Space Research Association, Inc., and the Deutsches SOFIA Institut.

    The W.M. Keck Observatory is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA, with financial support from the W.M. Keck Foundation. The researchers would like to thank the Hawaiian community for the privilege of allowing them to conduct observations on Mauna Kea, which plays a significant cultural and religious role.

    Nature Astronomy

    See the full article here .

    Comments are invited and will be appreciated, especially if the reader finds any errors which I can correct. Use “Reply”.

    five-ways-keep-your-child-safe-school-shootings

    Please help promote STEM in your local schools.

    Stem Education Coalition

    UC Davis Campus

    The University of California-Davis is a public land-grant research university near Davis, California. Named a Public Ivy, it is the northernmost of the ten campuses of The University of California system. The institution was first founded as an agricultural branch of the system in 1905 and became the seventh campus of the University of California in 1959.

    The university is classified among “R1: Doctoral Universities – Very high research activity”. The University of California-Davis faculty includes 23 members of The National Academy of Sciences, 30 members of The American Academy of Arts and Sciences, 17 members of the American Law Institute, 14 members of the Institute of Medicine, and 14 members of the National Academy of Engineering. Among other honours that university faculty, alumni, and researchers have won are two Nobel Prizes, a Presidential Medal of Freedom, three Pulitzer Prizes, three MacArthur Fellowships, and a National Medal of Science.
    Founded as a primarily agricultural campus, the university has expanded over the past century to include graduate and professional programs in medicine (which includes the University of California-Davis Medical Centre), law, veterinary medicine, education, nursing, and business management, in addition to 90 research programs offered by University of California-Davis Graduate Studies. The University of California-Davis School of Veterinary Medicine is the largest veterinary school in the United States and has been ranked first in the world for five consecutive years (2015–19). The University of California-Davis also offers certificates and courses, including online classes, for adults and non-traditional learners through its Division of Continuing and Professional Education.

    The University of California-Davis Aggies athletic teams compete in NCAA Division I, primarily as members of the Big West Conference with additional sports in the Big Sky Conference (football only) and the Mountain Pacific Sports Federation.

    Seventh UC campus

    In 1959, the campus was designated by the Regents of The University of California as the seventh general campus in the University of California system.

    University of California-Davis’s Graduate Division was established in 1961, followed by the creation of the College of Engineering in 1962. The law school opened for classes in fall 1966, and the School of Medicine began instruction in fall 1968. In a period of increasing activism, a Native American studies program was started in 1969, one of the first at a major university; it was later developed into a full department within the university.

    Graduate Studies

    The University of California-Davis Graduate Programs of Study consist of over 90 post-graduate programs, offering masters and doctoral degrees and post-doctoral courses. The programs educate over 4,000 students from around the world.

    UC Davis has the following graduate and professional schools, the most in the entire University of California system:

    UC Davis Graduate Studies
    Graduate School of Management
    School of Education
    School of Law
    School of Medicine
    School of Veterinary Medicine
    Betty Irene Moore School of Nursing

    Research

    University of California-Davis is one of 62 members in The Association of American Universities, an organization of leading research universities devoted to maintaining a strong system of academic research and education.

    Research centers and laboratories

    The campus supports a number of research centers and laboratories including:

    Advanced Highway Maintenance Construction Technology Research Laboratory
    BGI at UC Davis Joint Genome Center (in planning process)
    Bodega Marine Reserve
    C-STEM Center
    CalEPR Center
    California Animal Health and Food Safety Laboratory System
    California International Law Center
    California National Primate Research Center
    California Raptor Center
    Center for Health and the Environment
    Center for Mind and Brain
    Center for Poverty Research
    Center for Regional Change
    Center for the Study of Human Rights in the Americas
    Center for Visual Sciences
    Contained Research Facility
    Crocker Nuclear Laboratory
    Davis Millimeter Wave Research Center (A joint effort of Agilent Technologies Inc. and UC Davis) (in planning process)
    Information Center for the Environment
    John Muir Institute of the Environment (the largest research unit at UC Davis, spanning all Colleges and Professional Schools)
    McLaughlin Natural Reserve
    MIND Institute
    Plug-in Hybrid Electric Vehicle Research Center
    Quail Ridge Reserve
    Stebbins Cold Canyon Reserve
    Tahoe Environmental Research Center (TERC) (a collaborative effort with Sierra Nevada University)
    UC Center Sacramento
    UC Davis Nuclear Magnetic Resonance Facility
    University of California Pavement Research Center
    University of California Solar Energy Center (UC Solar)
    Energy Efficiency Center (the very first university run energy efficiency center in the Nation).
    Western Institute for Food Safety and Security

    The Crocker Nuclear Laboratory on campus has had a nuclear accelerator since 1966. The laboratory is used by scientists and engineers from private industry, universities and government to research topics including nuclear physics, applied solid state physics, radiation effects, air quality, planetary geology and cosmogenics. University of California-Davis is the only University of California campus, besides The University of California-Berkeley, that has a nuclear laboratory.

    Agilent Technologies will also work with the university in establishing a Davis Millimeter Wave Research Center to conduct research into millimeter wave and THz systems.

     
  • richardmitnick 9:19 am on April 14, 2023 Permalink | Reply
    Tags: "New Exoplanet-Hunting Technique Leads to Successful Direct Image of a Super-Jupiter", , , , , , , Ground based Astronomy, , Performing both direct imaging and astrometry allows scientists to gain a full understanding of an exoplanet for the first time., The planet HIP 99770 b,   

    From The W.M. Keck Observatory: “New Exoplanet-Hunting Technique Leads to Successful Direct Image of a Super-Jupiter” 

    W.M. Keck Observatory two ten meter telescopes operated by California Institute of Technology and The University of California, at Mauna Kea Observatory, Hawai’i, altitude 4,207 m (13,802 ft). Credit: Caltech.

    Keck Laser Guide Star Adaptive Optics on two 10 meter Keck Observatory telescopes, Mauna Kea Hawai’i, altitude 4,207 m (13,802 ft). Credit: Caltech.

    Mauna Kea Observatories Hawai’i altitude 4,213 m (13,822 ft).

    From The W.M. Keck Observatory

    4.13.23
    Mari-Ela Chock (She/Her/Hers)
    Communications Officer
    808.554.0567
    mchock@keck.hawaii.edu

    1
    A direct infrared image of the HIP 99770 star system captured with W. M. Keck Observatory’s NIRC2 instrument [below] paired with the Keck II Telescope Adaptive Optics system. The bright host star is masked, as marked by the yellow star icon. The dashed circle shows the size of Jupiter’s orbit around the sun for scale. The white arrow points to the extrasolar planet HIP 99770 b. Credit: T. Currie/W. M. Keck Observatory/UTSA.

    Astronomers have developed a new method for finding exoplanets whose portraits can be taken from Earth using large ground-based telescopes, one that has proven successful after this technique resulted in a direct image of a Jupiter-like gas giant located 132.8 light-years away in the constellation Cygnus.

    The planet, called HIP 99770 b, is the first one beyond our solar system found using a powerful combination of astrometry and direct imaging.

    Two Mauna Kea Observatories on Hawaiʻi Island – W. M. Keck Observatory and Subaru Telescope – performed the direct imaging, snapping infrared photos of the planet directly.

    The astrometry, which measured the position and motion of HIP 99770 b’s home star, came from the European Space Agency’s Gaia space observatory and its predecessor Hipparcos.

    The study is published in the journal Science [below] on Friday, April 14.

    “Performing both direct imaging and astrometry allows us to gain a full understanding of an exoplanet for the first time: measure its atmosphere, weigh it, and track its orbit all at once,” said Thayne Currie, an affiliated researcher at Subaru Telescope and lead author of the study. “This new approach for finding planets prefigures the way we will someday identify and characterize an Earth-twin around a nearby star.”

    Detecting HIP 99770 b is tough; because the planet is faint, it can get lost in the glare of its bright host star.

    “This is the kind of discovery that really could have only been done from Mauna Kea,” said Currie. “We are extremely grateful for the privilege of being able to study the heavens from this mountain.”

    This new way of combing for nearby exoplanets is a major improvement to traditional, ground-based means; for the past 14 years, astronomers have been using so-called ‘blind’ surveys to scour the sky for stars that show potential for housing giant planets we can directly image from Earth based on the star system’s age and distance. However, this technique has a low yield. Precision astrometry on the other hand detects the movement of stars, which allows researchers to zero in on the ones tugged by the gravitational pull of an unseen companion such as a planet, then capture a picture of the star systems that are close enough to directly image.

    “Our discovery really changes the way we do exoplanet science,” said Currie. “Direct imaging is very exciting but also really challenging, with many nights devoted to looking for planets around other stars from so many programs only to come up empty. By fine-tuning our technique with astrometry, we now know exactly where to look.”

    2
    A movie showing the orbital motion of HIP 99770 b, a super-Jupiter in this exoplanetary system marked in the white circle. Credit: T. Currie/Subaru Telescope, UTSA

    HIP 99770 b serves as proof of concept, developed by an international research team led by Subaru Telescope, University of Tokyo, University of Texas-San Antonio, and the Astrobiology Center of Japan. From the Subaru Telescope and Keck Observatory data, they determined HIP 99770 b is 14-16 times the mass of Jupiter and orbits a star that is nearly twice as massive as the Sun. However, it receives nearly the same amount of sunlight as Jupiter because its host star is far more luminous than the Sun.

    The team also characterized the nature of HIP 99770 b’s atmosphere, namely its temperature, gravity, clouds, and chemistry. Using Keck Observatory’s second generation Near-Infrared Camera (NIRC2)[below] paired with the Keck II telescope adaptive optics system, they found the gas giant has a slightly higher temperature and is less cloudy than the HR 8799 planets – the very first directly imaged exoplanetary system discovered in 2008 by two Maunakea Observatories – Keck Observatory and Gemini Observatory. The planet’s atmosphere also has signs of water and carbon monoxide.

    Furthermore, the HIP 99770 star system is surrounded by a disk of icy dust, similar to the Kuiper Belt in our own solar system.

    “This is the first of many discoveries from our Keck and Subaru imaging program that uses astrometry to select targets. We already have additional discoveries that will be announced later this year and next year,” said Currie.

    Science

    See the full article here .

    Comments are invited and will be appreciated, especially if the reader finds any errors which I can correct. Use “Reply”.


    five-ways-keep-your-child-safe-school-shootings
    Please help promote STEM in your local schools.


    Stem Education Coalition

    Mission
    To advance the frontiers of astronomy and share our discoveries with the world.

    The W. M. Keck Observatory operates the largest, most scientifically productive telescopes on Earth. The two, 10-meter optical/infrared telescopes on the summit of Mauna Kea on the Island of Hawaii feature a suite of advanced instruments including imagers, multi-object spectrographs, high-resolution spectrographs, integral-field spectrometer and world-leading laser guide star adaptive optics systems. Keck Observatory is a private 501(c) 3 non-profit organization and a scientific partnership of the California Institute of Technology, the University of California and NASA.

    Today Keck Observatory is supported by both public funding sources and private philanthropy. As a 501(c)3, the organization is managed by The California Association for Research in Astronomy(CARA), whose Board of Directors includes representatives from the California Institute of Technologyand the University of California with liaisons to the board from The National Aeronautics and Space Agency and the Keck Foundation.


    Keck UCal

    Instrumentation

    Keck 1

    HIRES – The largest and most mechanically complex of the Keck’s main instruments, the High Resolution Echelle Spectrometer breaks up incoming starlight into its component colors to measure the precise intensity of each of thousands of color channels. Its spectral capabilities have resulted in many breakthrough discoveries, such as the detection of planets outside our solar system and direct evidence for a model of the Big Bang theory.

    Keck High-Resolution Echelle Spectrometer (HIRES), at the Keck I telescope.
    LRIS – The Low Resolution Imaging Spectrograph is a faint-light instrument capable of taking spectra and images of the most distant known objects in the universe. The instrument is equipped with a red arm and a blue arm to explore stellar populations of distant galaxies, active galactic nuclei, galactic clusters, and quasars.

    UCO Keck LRIS on Keck 1.

    VISIBLE BAND (0.3-1.0 Micron)

    MOSFIRE – The Multi-Object Spectrograph for Infrared Exploration gathers thousands of spectra from objects spanning a variety of distances, environments and physical conditions. What makes this huge, vacuum-cryogenic instrument unique is its ability to select up to 46 individual objects in the field of view and then record the infrared spectrum of all 46 objects simultaneously. When a new field is selected, a robotic mechanism inside the vacuum chamber reconfigures the distribution of tiny slits in the focal plane in under six minutes. Eight years in the making with First Light in 2012, MOSFIRE’s early performance results range from the discovery of ultra-cool, nearby substellar mass objects, to the detection of oxygen in young galaxies only 2 billion years after the Big Bang.

    Keck/MOSFIRE on Keck 1.

    OSIRIS – The OH-Suppressing Infrared Imaging Spectrograph is a near-infrared spectrograph for use with the Keck I adaptive optics system. OSIRIS takes spectra in a small field of view to provide a series of images at different wavelengths. The instrument allows astronomers to ignore wavelengths where the Earth’s atmosphere shines brightly due to emission from OH (hydroxl) molecules, thus allowing the detection of objects 10 times fainter than previously available.
    Keck OSIRIS on Keck 1.

    Keck 2

    DEIMOS – The Deep Extragalactic Imaging Multi-Object Spectrograph is the most advanced optical spectrograph in the world, capable of gathering spectra from 130 galaxies or more in a single exposure. In ‘Mega Mask’ mode, DEIMOS can take spectra of more than 1,200 objects at once, using a special narrow-band filter.

    Keck/DEIMOS on Keck 2.

    NIRSPEC – The Near Infrared Spectrometer studies very high redshift radio galaxies, the motions and types of stars located near the Galactic Center, the nature of brown dwarfs, the nuclear regions of dusty starburst galaxies, active galactic nuclei, interstellar chemistry, stellar physics, and solar-system science.

    NIRSPEC on Keck 2.

    ESI – The Echellette Spectrograph and Imager captures high-resolution spectra of very faint galaxies and quasars ranging from the blue to the infrared in a single exposure. It is a multimode instrument that allows users to switch among three modes during a night. It has produced some of the best non-AO images at the Observatory.

    KECK Echellette Spectrograph and Imager (ESI).

    KCWI – The Keck Cosmic Web Imager is designed to provide visible band, integral field spectroscopy with moderate to high spectral resolution, various fields of view and image resolution formats and excellent sky-subtraction. The astronomical seeing and large aperture of the telescope enables studies of the connection between galaxies and the gas in their dark matter halos, stellar relics, star clusters and lensed galaxies.

    Keck Cosmic Web Imager on Keck 2 schematic.

    Keck Cosmic Web Imager on Keck 2.

    NEAR-INFRARED (1-5 Micron)

    ADAPTIVE OPTICS – Adaptive optics senses and compensates for the atmospheric distortions of incoming starlight up to 1,000 times per second. This results in an improvement in image quality on fairly bright astronomical targets by a factor 10 to 20.

    LASER GUIDE STAR ADAPTIVE OPTICS [pictured above] – The Keck Laser Guide Star expands the range of available targets for study with both the Keck I and Keck II adaptive optics systems. They use sodium lasers to excite sodium atoms that naturally exist in the atmosphere 90 km (55 miles) above the Earth’s surface. The laser creates an “artificial star” that allows the Keck adaptive optics system to observe 70-80 percent of the targets in the sky, compared to the 1 percent accessible without the laser.

    NIRC-2/AO – The second generation Near Infrared Camera works with the Keck Adaptive Optics system to produce the highest-resolution ground-based images and spectroscopy in the 1-5 micron range. Typical programs include mapping surface features on solar system bodies, searching for planets around other stars, and analyzing the morphology of remote galaxies.

    Keck NIRC2 Camera on Keck 2.
    ABOUT NIRES
    The Near Infrared Echellette Spectrograph (NIRES) is a prism cross-dispersed near-infrared spectrograph built at the California Institute of Technology by a team led by Chief Instrument Scientist Keith Matthews and Prof. Tom Soifer. Commissioned in 2018, NIRES covers a large wavelength range at moderate spectral resolution for use on the Keck II telescope and observes extremely faint red objects found with the Spitzer and WISE infrared space telescopes, as well as brown dwarfs, high-redshift galaxies, and quasars.


    Future Instrumentation

    KCRM – The Keck Cosmic Reionization Mapper will complete the Keck Cosmic Web Imager (KCWI), the world’s most capable spectroscopic imager. The design for KCWI includes two separate channels to detect light in the blue and the red portions of the visible wavelength spectrum. KCWI-Blue was commissioned and started routine science observations in September 2017. The red channel of KCWI is KCRM; a powerful addition that will open a window for new discoveries at high redshifts.

    KCRM – Keck Cosmic Reionization Mapper KCRM on Keck 2.

    KPF – The Keck Planet Finder (KPF) will be the most advanced spectrometer of its kind in the world. The instrument is a fiber-fed high-resolution, two-channel cross-dispersed echelle spectrometer for the visible wavelengths and is designed for the Keck II telescope. KPF allows precise measurements of the mass-density relationship in Earth-like exoplanets, which will help astronomers identify planets around other stars that are capable of supporting life.

    KPF Keck Planet Finder on Keck 2.

     
  • richardmitnick 11:58 am on April 9, 2023 Permalink | Reply
    Tags: "First Detection of Hot Molecular Cloud Cores in the Small Magellanic Cloud", , , , , Ground based Astronomy, Researchers have previously detected hot molecular cloud cores in the Milky Way and in several nearby galaxies   

    From AAS NOVA: “First Detection of Hot Molecular Cloud Cores in the Small Magellanic Cloud” 

    AASNOVA

    From AAS NOVA

    4.7.23
    Kerry Hensley

    1
    Webb captured this near-infrared view of the star-forming region NGC 346 in the Small Magellanic Cloud. [SCIENCE: Olivia C. Jones (UK ATC), Guido De Marchi (ESTEC), Margaret Meixner (USRA)/NASA/ESA/CSA; IMAGE PROCESSING: Alyssa Pagan (STScI), Nolan Habel (USRA), Laura Lenkić (USRA), Laurie E. U. Chu (NASA Ames)]

    Researchers have detected hot molecular cloud cores in the Small Magellanic Cloud for the first time. This discovery enhances our understanding of star formation in the nearby universe and will guide future explorations of extragalactic star-forming regions.

    From Cold Cloud to Hot Core

    2
    A view of the Small Magellanic Cloud from the European Southern Observatory’s Visible and Infrared Survey Telescope for Astronomy.

    New stars form in massive clouds of molecular hydrogen gas. As the cloud swirls, gas collects in cold, dense clumps, creating the conditions for star formation. When a massive star begins to form in one of these clumps, the gas heats up, creating a hot molecular cloud core. Researchers have previously detected hot molecular cloud cores in the Milky Way and in several nearby galaxies, but they have remained elusive in one of our nearest neighbors: the Small Magellanic Cloud.

    The Small Magellanic Cloud is an interesting place to search for hot cores because this small, irregularly shaped galaxy is poor in metals — elements heavier than helium — compared to galaxies like the Milky Way. If we find hot cores in such a metal-poor galaxy, we can study how the formation of massive stars varies between metal-rich and metal-poor galaxies in the universe today. This can also help us understand star formation billions of years ago, when the universe was substantially less metal rich than it is now.

    Core Candidates

    3
    Locations of the two protostars/hot core candidates, S07 and S09, within the Small Magellanic Cloud. The observations were made at infrared wavelengths. [Shimonishi et al. 2023]

    Takashi Shimonishi (Niigata University) and collaborators began their search for hot cores with two sources in the Small Magellanic Cloud that had been flagged as high-mass protostars. Previous observations found that these two soon-to-be stars are swathed in clouds containing dust and ice, which suggests that the protostars might be embedded within dense gas.

    The team combined new and archival data from the Atacama Large Millimeter/submillimeter Array (ALMA) to determine the properties of the gas surrounding the two sources.

    They detected spectral lines from numerous molecules and molecular ions, including carbon monoxide, methanol, and sulfur dioxide. The data suggested that the gas surrounding the protostars is dense, hot (here, “hot” means warmer than 100K), and concentrated in a small region around each protostar — exactly the characteristics of a hot core!

    Testing Molecular Tracers

    Finding hot cores in the metal-poor Small Magellanic Cloud suggests that hot core formation is an expected part of massive star formation for galaxies with a wide range of metal abundances. Specifically, Shimonishi and collaborators have shown that hot cores can form in galaxies in which metals are 80% less abundant relative to hydrogen than they are in the gas from which the Sun formed.

    4
    Comparison of the sulfur dioxide (SO2) and methanol (CH3OH) emission for the hot core S07. The source region of the sulfur dioxide emission is more compact and warmer. [Adapted from Shimonishi et al. 2023]

    Interestingly, the team found key differences between the Small Magellanic Cloud hot cores and those in other galaxies. Generally, researchers use methanol emission to find hot cores, but the methanol emission from the newly found cores was extended and cool — not what we’d expect for a hot core. Instead, it was sulfur dioxide emission that traced the cores effectively. Why might methanol be a poor core tracer in the Small Magellanic Cloud when it’s so effective in other environments? This might point to differences in how methanol and sulfur dioxide form in metal-poor hot cores, making sulfur dioxide a better indicator of hot cores in these regions.

    Citation

    “The Detection of Hot Molecular Cores in the Small Magellanic Cloud,” Takashi Shimonishi et al 2023 ApJL 946 L41.
    https://iopscience.iop.org/article/10.3847/2041-8213/acc031/pdf
    See the science paper for instructive material with images.

    See the full article here .

    Comments are invited and will be appreciated, especially if the reader finds any errors which I can correct. Use “Reply”.


    five-ways-keep-your-child-safe-school-shootings

    Please help promote STEM in your local schools.


    Stem Education Coalition

    1

    The mission of the American Astronomical Society is to enhance and share humanity’s scientific understanding of the Universe.

    The Society, through its publications, disseminates and archives the results of astronomical research. The Society also communicates and explains our understanding of the universe to the public.
    The Society facilitates and strengthens the interactions among members through professional meetings and other means. The Society supports member divisions representing specialized research and astronomical interests.
    The Society represents the goals of its community of members to the nation and the world. The Society also works with other scientific and educational societies to promote the advancement of science.
    The Society, through its members, trains, mentors and supports the next generation of astronomers. The Society supports and promotes increased participation of historically underrepresented groups in astronomy.
    The Society assists its members to develop their skills in the fields of education and public outreach at all levels. The Society promotes broad interest in astronomy, which enhances science literacy and leads many to careers in science and engineering.

    Adopted June 7, 2009

    The society was founded in 1899 through the efforts of George Ellery Hale. The constitution of the group was written by Hale, George Comstock, Edward Morley, Simon Newcomb and Edward Charles Pickering. These men, plus four others, were the first Executive Council of the society; Newcomb was the first president. The initial membership was 114. The AAS name of the society was not finally decided until 1915, previously it was the “Astronomical and Astrophysical Society of America”. One proposed name that preceded this interim name was “American Astrophysical Society”.

    The AAS today has over 7,000 members and six divisions – the Division for Planetary Sciences (1968); the Division on Dynamical Astronomy (1969); the High Energy Astrophysics Division (1969); the Solar Physics Division (1969); the Historical Astronomy Division (1980); and the Laboratory Astrophysics Division (2012). The membership includes physicists, mathematicians, geologists, engineers and others whose research interests lie within the broad spectrum of subjects now comprising contemporary astronomy.

    In 2019 three AAS members were selected into the tenth anniversary class of TED Fellows.

    The AAS established the AAS Fellows program in 2019 to “confer recognition upon AAS members for achievement and extraordinary service to the field of astronomy and the American Astronomical Society.” The inaugural class was designated by the AAS Board of Trustees and includes an initial group of 232 Legacy Fellows.

     
  • richardmitnick 9:49 am on April 6, 2023 Permalink | Reply
    Tags: "Study Finds A Strange Streak of Young Stars is Evidence of a Runaway Supermassive Black Hole", , , , , Ground based Astronomy, ,   

    From The W.M. Keck Observatory: “Study Finds A Strange Streak of Young Stars is Evidence of a Runaway Supermassive Black Hole” 

    W.M. Keck Observatory two ten meter telescopes operated by California Institute of Technology and The University of California, at Mauna Kea Observatory, Hawai’i, altitude 4,207 m (13,802 ft). Credit: Caltech.

    Keck Laser Guide Star Adaptive Optics on two 10 meter Keck Observatory telescopes, Mauna Kea Hawai’i, altitude 4,207 m (13,802 ft). Credit: Caltech.

    Mauna Kea Observatories Hawai’i altitude 4,213 m (13,822 ft).

    From The W.M. Keck Observatory

    4.6.23

    Mari-Ela Chock (She/Her/Hers)
    Communications Officer
    808.554.0567
    mchock@keck.hawaii.edu

    1
    A Hubble Space Telescope image of a never-before-seen 200,000 light-year long trail of newborn stars with twice the diameter of our milky way galaxy. this streak is likely a wake behind a fleeing supermassive black hole, astronomers say. Credit: NASA, ESA, P. van Dokkum (Yale), J. DePasquale (STScI).

    Astronomers have spotted a candidate supermassive black hole running away from its home galaxy, hurtling through space at a velocity of about 4 million miles per hour for the past 39 million years.

    A Yale University-led team using NASA’s Hubble Space Telescope and W. M. Keck Observatory on Maunakea in Hawaiʻi discovered an unusual, very thin, almost straight streak of young stars and shocked gas – possibly the trail the black hole left behind as it escaped.

    The findings are outlined in a study published in today’s issue of The Astrophysical Journal Letters [below].

    “Something like this has never been seen anywhere in the universe,” said Pieter van Dokkum, professor of astronomy and physics at Yale University and lead author of the study. “We’ve known for a long time that supermassive black holes exist and it had been predicted for about 50 years that they could sometimes be ejected from galaxies. If confirmed, this would be the first evidence of a runaway supermassive black hole, proving this prediction.”

    Van Dokkum’s team first detected the long feature with NASA’s Hubble Space Telescope.

    To get a closer look, they conducted follow-up observations using Keck Observatory’s Low Resolution Imaging Spectrometer (LRIS) [below] and Near Infrared Echellette Spectrograph (NIRES) [below].

    The Keck Observatory data revealed the streak of stars measured a remarkable 200,000 light-years in length and extended from a compact, active star-forming galaxy whose light took about 7.6 billion years to reach Earth. The trail is almost half as bright as the host galaxy it is linked to, indicating it contains an abundance of new stars.

    “We think we’re seeing a wake behind the black hole where the gas cools and is able to form stars. So, we’re looking at star formation trailing the black hole,” said van Dokkum. “What we’re seeing is the aftermath. Like the wake behind a ship, we’re seeing the wake behind the black hole.”

    2
    An artist’s impression of a runaway supermassive black hole that was ejected from its host galaxy as a result of a tussle between it and two other black holes. As the black hole plows through intergalactic space, it compresses tenuous gas in front of it. This precipitates the birth of hot blue stars. This illustration is based on Hubble Space Telescope observations of a 200,000-light-year-long “contrail” of stars behind an escaping black hole. Credit: Leah Hustak (STScI)/NASA/ESA.

    Keck Observatory also showed a bright knot of ionized gas at the top of the wake – likely the site of the black hole itself. Also, the linear feature’s home galaxy appears to be missing a black hole at its center, or at least does not have one that is actively feasting on material and generating powerful jets of energy that telescopes can detect.

    If the narrow wake of stars and gas was indeed created by a black hole dislodged from its home galaxy, astronomers have a likely explanation for its origin story. First, two galaxies, both containing a supermassive black hole inside their cores, merge. Next, as the black holes whiz around each other in a binary dance at the center of the newly- merged galaxy, a third supermassive black hole inside another galaxy intrudes on the couple. The trio’s interaction with one another then creates an unstable situation that generates enough velocity to torpedo one of the three black holes out.

    3
    A panel showing sections of spectra captured with W. M. Keck Observatory’s LRIS instrument, revealing the unusual linear feature extended from a galaxy whose light took about 7.6 billion years to reach Earth. Credit: V. Dokkum (Yale)/W. M. Keck Observatory.

    As a next step, van Dokkum and his team are now seeking to confirm whether their discovery is in fact a runaway black hole; they’ve applied for time on NASA’s James Webb Space Telescope and Chandra X-ray Observatory to conduct follow-up observations.

    Because the linear streak of newborn stars and shocked gas is so striking, van Dokkum says it should be straightforward to find other objects like it in current and future data, such as with NASA’s upcoming Nancy Grace Roman Space Telescope.

    “Much of what we do is hypothesis testing, or refining previous measurements, but sometimes there is this bolt out of the blue of a completely unanticipated discovery. That is rare, but it is the best!” said van Dokkum.

    “Going from noticing the streak and thinking ʻhey that’s weird’ to this paper was so incredibly fun and satisfying as we were all learning every step of the way,” said co-author Imad Pasha, a Yale University graduate student on van Dokkum’s research team.

    The Astrophysical Journal Letters
    See the science paper for instructive material with images.
    ___________________________________________________________________________
    ABOUT LRIS

    The Low Resolution Imaging Spectrometer (LRIS) is a very versatile and ultra-sensitive visible-wavelength imager and spectrograph built at the California Institute of Technology by a team led by Prof. Bev Oke and Prof. Judy Cohen and commissioned in 1993. Since then it has seen two major upgrades to further enhance its capabilities: the addition of a second, blue arm optimized for shorter wavelengths of light and the installation of detectors that are much more sensitive at the longest (red) wavelengths. Each arm is optimized for the wavelengths it covers. This large range of wavelength coverage, combined with the instrument’s high sensitivity, allows the study of everything from comets (which have interesting features in the ultraviolet part of the spectrum), to the blue light from star formation, to the red light of very distant objects. LRIS also records the spectra of up to 50 objects simultaneously, especially useful for studies of clusters of galaxies in the most distant reaches, and earliest times, of the universe. LRIS was used in observing distant supernovae by astronomers who received the Nobel Prize in Physics in 2011 for research determining that the universe was speeding up in its expansion.

    ABOUT NIRES

    The Near Infrared Echellette Spectrograph (NIRES) is a prism cross-dispersed near-infrared spectrograph built at the California Institute of Technology by a team led by Chief Instrument Scientist Keith Matthews and Prof. Tom Soifer. Commissioned in 2018, NIRES covers a large wavelength range at moderate spectral resolution for use on the Keck II telescope and observes extremely faint red objects found with the Spitzer and WISE infrared space telescopes, as well as brown dwarfs, high-redshift galaxies, and quasars. Support for this technology was generously provided by the Mt. Cuba Astronomical Foundation.

    See the full article here .

    Comments are invited and will be appreciated, especially if the reader finds any errors which I can correct. Use “Reply”.


    five-ways-keep-your-child-safe-school-shootings
    Please help promote STEM in your local schools.


    Stem Education Coalition

    Mission
    To advance the frontiers of astronomy and share our discoveries with the world.

    The W. M. Keck Observatory operates the largest, most scientifically productive telescopes on Earth. The two, 10-meter optical/infrared telescopes on the summit of Mauna Kea on the Island of Hawaii feature a suite of advanced instruments including imagers, multi-object spectrographs, high-resolution spectrographs, integral-field spectrometer and world-leading laser guide star adaptive optics systems. Keck Observatory is a private 501(c) 3 non-profit organization and a scientific partnership of the California Institute of Technology, the University of California and NASA.

    Today Keck Observatory is supported by both public funding sources and private philanthropy. As a 501(c)3, the organization is managed by The California Association for Research in Astronomy(CARA), whose Board of Directors includes representatives from the California Institute of Technologyand the University of California with liaisons to the board from The National Aeronautics and Space Agency and the Keck Foundation.


    Keck UCal

    Instrumentation

    Keck 1

    HIRES – The largest and most mechanically complex of the Keck’s main instruments, the High Resolution Echelle Spectrometer breaks up incoming starlight into its component colors to measure the precise intensity of each of thousands of color channels. Its spectral capabilities have resulted in many breakthrough discoveries, such as the detection of planets outside our solar system and direct evidence for a model of the Big Bang theory.

    Keck High-Resolution Echelle Spectrometer (HIRES), at the Keck I telescope.
    LRIS – The Low Resolution Imaging Spectrograph is a faint-light instrument capable of taking spectra and images of the most distant known objects in the universe. The instrument is equipped with a red arm and a blue arm to explore stellar populations of distant galaxies, active galactic nuclei, galactic clusters, and quasars.

    UCO Keck LRIS on Keck 1.

    VISIBLE BAND (0.3-1.0 Micron)

    MOSFIRE – The Multi-Object Spectrograph for Infrared Exploration gathers thousands of spectra from objects spanning a variety of distances, environments and physical conditions. What makes this huge, vacuum-cryogenic instrument unique is its ability to select up to 46 individual objects in the field of view and then record the infrared spectrum of all 46 objects simultaneously. When a new field is selected, a robotic mechanism inside the vacuum chamber reconfigures the distribution of tiny slits in the focal plane in under six minutes. Eight years in the making with First Light in 2012, MOSFIRE’s early performance results range from the discovery of ultra-cool, nearby substellar mass objects, to the detection of oxygen in young galaxies only 2 billion years after the Big Bang.

    Keck/MOSFIRE on Keck 1.

    OSIRIS – The OH-Suppressing Infrared Imaging Spectrograph is a near-infrared spectrograph for use with the Keck I adaptive optics system. OSIRIS takes spectra in a small field of view to provide a series of images at different wavelengths. The instrument allows astronomers to ignore wavelengths where the Earth’s atmosphere shines brightly due to emission from OH (hydroxl) molecules, thus allowing the detection of objects 10 times fainter than previously available.
    Keck OSIRIS on Keck 1.

    Keck 2

    DEIMOS – The Deep Extragalactic Imaging Multi-Object Spectrograph is the most advanced optical spectrograph in the world, capable of gathering spectra from 130 galaxies or more in a single exposure. In ‘Mega Mask’ mode, DEIMOS can take spectra of more than 1,200 objects at once, using a special narrow-band filter.

    Keck/DEIMOS on Keck 2.

    NIRSPEC – The Near Infrared Spectrometer studies very high redshift radio galaxies, the motions and types of stars located near the Galactic Center, the nature of brown dwarfs, the nuclear regions of dusty starburst galaxies, active galactic nuclei, interstellar chemistry, stellar physics, and solar-system science.

    NIRSPEC on Keck 2.

    ESI – The Echellette Spectrograph and Imager captures high-resolution spectra of very faint galaxies and quasars ranging from the blue to the infrared in a single exposure. It is a multimode instrument that allows users to switch among three modes during a night. It has produced some of the best non-AO images at the Observatory.

    KECK Echellette Spectrograph and Imager (ESI).

    KCWI – The Keck Cosmic Web Imager is designed to provide visible band, integral field spectroscopy with moderate to high spectral resolution, various fields of view and image resolution formats and excellent sky-subtraction. The astronomical seeing and large aperture of the telescope enables studies of the connection between galaxies and the gas in their dark matter halos, stellar relics, star clusters and lensed galaxies.

    Keck Cosmic Web Imager on Keck 2 schematic.

    Keck Cosmic Web Imager on Keck 2.

    NEAR-INFRARED (1-5 Micron)

    ADAPTIVE OPTICS – Adaptive optics senses and compensates for the atmospheric distortions of incoming starlight up to 1,000 times per second. This results in an improvement in image quality on fairly bright astronomical targets by a factor 10 to 20.

    LASER GUIDE STAR ADAPTIVE OPTICS [pictured above] – The Keck Laser Guide Star expands the range of available targets for study with both the Keck I and Keck II adaptive optics systems. They use sodium lasers to excite sodium atoms that naturally exist in the atmosphere 90 km (55 miles) above the Earth’s surface. The laser creates an “artificial star” that allows the Keck adaptive optics system to observe 70-80 percent of the targets in the sky, compared to the 1 percent accessible without the laser.

    NIRC-2/AO – The second generation Near Infrared Camera works with the Keck Adaptive Optics system to produce the highest-resolution ground-based images and spectroscopy in the 1-5 micron range. Typical programs include mapping surface features on solar system bodies, searching for planets around other stars, and analyzing the morphology of remote galaxies.

    Keck NIRC2 Camera on Keck 2.
    ABOUT NIRES
    The Near Infrared Echellette Spectrograph (NIRES) is a prism cross-dispersed near-infrared spectrograph built at the California Institute of Technology by a team led by Chief Instrument Scientist Keith Matthews and Prof. Tom Soifer. Commissioned in 2018, NIRES covers a large wavelength range at moderate spectral resolution for use on the Keck II telescope and observes extremely faint red objects found with the Spitzer and WISE infrared space telescopes, as well as brown dwarfs, high-redshift galaxies, and quasars.


    Future Instrumentation

    KCRM – The Keck Cosmic Reionization Mapper will complete the Keck Cosmic Web Imager (KCWI), the world’s most capable spectroscopic imager. The design for KCWI includes two separate channels to detect light in the blue and the red portions of the visible wavelength spectrum. KCWI-Blue was commissioned and started routine science observations in September 2017. The red channel of KCWI is KCRM; a powerful addition that will open a window for new discoveries at high redshifts.

    KCRM – Keck Cosmic Reionization Mapper KCRM on Keck 2.

    KPF – The Keck Planet Finder (KPF) will be the most advanced spectrometer of its kind in the world. The instrument is a fiber-fed high-resolution, two-channel cross-dispersed echelle spectrometer for the visible wavelengths and is designed for the Keck II telescope. KPF allows precise measurements of the mass-density relationship in Earth-like exoplanets, which will help astronomers identify planets around other stars that are capable of supporting life.

    KPF Keck Planet Finder on Keck 2.

     
  • richardmitnick 10:23 am on April 3, 2023 Permalink | Reply
    Tags: "Roman Space Telescope and Rubin Observatory scientists collaborate on a giant testbed of simulated galaxies", , , , Ground based Astronomy, ,   

    From The DOE’s SLAC National Accelerator Laboratory: “Roman Space Telescope and Rubin Observatory scientists collaborate on a giant testbed of simulated galaxies” 

    From The DOE’s SLAC National Accelerator Laboratory

    3.13.23 [Just today in social media.]

    1
    This simulated Roman deep field image, containing hundreds of thousands of galaxies, represents just 1.3 percent of the synthetic survey, which is itself just one percent of Roman’s planned survey. The galaxies are color coded – redder ones are farther away and whiter ones are nearer. Credits: M. Troxel and Caltech-IPAC/R. Hurt.

    The synthetic galaxy catalog will help test Roman’s capabilities and foster collaboration with the Rubin project.

    Scientists have created a gargantuan synthetic survey that shows some of what we can expect from NASA’s Nancy Grace Roman Space Telescope, slated to launch in the mid-2020s, and the Vera C. Rubin Observatory’s Legacy Survey of Space and Time (LSST), funded by the National Science Foundation and the Department of Energy.

    Though it represents just a small chunk of the real future surveys, this simulated version contains a staggering number of galaxies – 33 million of them, along with 200,000 foreground stars in our home galaxy.

    The team drew data from a mock universe [The Astrophysical Journal Supplement Series (below)] originally developed to support science planning [The Astrophysical Journal Supplement Series (below)] with the Vera C. Rubin Observatory, which is located in Chile and set to begin full operations in 2024, and the Rubin/LSST Dark Energy Science Collaboration. Because the Roman and Rubin/LSST simulations use the same source data, astronomers can compare them and see what they can expect to learn from pairing the telescopes’ observations once they’re both actively scanning the universe.

    The work put in now will also help both teams make the most of the data they collect in the future. “The idea there was to use the same simulated data, so that downstream we can foster more collaboration,” said James Chiang, a lead scientist at the Department of Energy’s SLAC National Accelerator Laboratory and a researcher on the project. “I’m excited to work with everyone and see things come together.”

    2
    This animation shows the type of science that astronomers will be able to do with future Roman deep field observations. The gravity of intervening galaxy clusters and dark matter can lens the light from farther objects, warping their appearance as shown in the animation. By studying the distorted light, astronomers can study elusive dark matter, which can only measured indirectly through its gravitational effects on visible matter. As a bonus, this lensing also makes it easier to see the most distant galaxies whose light they magnify. (Caltech-IPAC/R. Hurt)

    A paper describing the results, led by Duke University assistant professor Michael Troxel, is published in MNRAS [below].

    Cosmic Construction

    Roman’s High Latitude Wide Area Survey will consist of both spectroscopy and imaging, which is the focus of the new simulation. Roman’s imaging will reveal precise positions and shapes of hundreds of millions of faint galaxies that will be used to map dark matter. That data – as well as data from Rubin and other projects – will in turn help researchers understand how the universe evolved into what we see today and fill in more of the gaps in our understanding of dark matter.

    “Theories of cosmic structure formation make predictions for how the seed fluctuations in the early universe grow into the distribution of matter that can be seen through gravitational lensing,” said Chris Hirata, a physics professor at Ohio State University in Columbus, and a co-author of the paper. “But the predictions are statistical in nature, so we test them by observing vast regions of the cosmos. Roman, with its wide field of view, will be optimized to efficiently survey the sky, complementing observatories such as the James Webb Space Telescope that are designed for deeper investigation of individual objects.”

    3
    This graphic compares the relative sizes of the synthetic image (inset, outlined in orange), the whole area astronomers simulated (the square in the upper-middle outlined in green), and the size of the complete future survey astronomers will conduct (the large square in the lower-left outlined in blue). The background, from the Digitized Sky Survey, illustrates how much sky area each region covers. The synthetic image covers about as much sky as a full moon, and the future Roman survey will cover much more area than the Big Dipper. While it would take the Hubble Space Telescope or James Webb Space Telescope around a thousand years to image an area as large as the future survey, Roman will do it in just over seven months. (NASA’s Goddard Space Flight Center and M. Troxel)

    Ground and Space

    The synthetic survey covers 20 square degrees of the sky, which is roughly equivalent to 95 full moons. The actual survey will be 100 times larger, unveiling more than a billion galaxies. Rubin will scan an even greater area – 18,000 square degrees, nearly half of the entire sky – but with lower resolution since it will have to peer through Earth’s turbulent atmosphere.

    Pairing the Roman and Rubin/LSST simulations offers the first opportunity for scientists to try to detect the same objects in both sets of images. That’s important because ground-based observations aren’t always sharp enough to distinguish multiple, close sources as separate objects. Sometimes they blur together, which affects weak lensing measurements. Now, scientists can determine the difficulties and benefits of “deblending” such objects in Rubin images by comparing them with Roman ones.

    With Roman and Rubin’s colossal cosmic view, astronomers will be able to accomplish far more than the survey’s primary goals, which are to study the structure and evolution of the universe, map dark matter, and discern between the leading theories that attempt to explain why the expansion of the universe is speeding up. Scientists can comb through the new simulated data to get a taste of the bonus science that will come from seeing so much of the universe in such exquisite detail.

    “We anticipate many different scientific opportunities, but we will also have to learn to expect the unexpected,” said Julie McEnery, the senior project scientist for the Roman mission at NASA’s Goddard Space Flight Center in Greenbelt, Maryland. “The mission will help answer critical questions in cosmology while potentially revealing brand new mysteries for us to solve.”

    The research was funded in part by the DOE Office of Science. Portions of the research were conducted at the National Energy Research Scientific Computing Center, a DOE Office of Science user facility.

    The Astrophysical Journal Supplement Series
    The Astrophysical Journal Supplement Series
    MNRAS
    See the science papers for instructive material with images.

    See the full article here .

    Comments are invited and will be appreciated, especially if the reader finds any errors which I can correct. Use “Reply”.


    five-ways-keep-your-child-safe-school-shootings
    Please help promote STEM in your local schools.

    Stem Education Coalition

    DOE’s SLAC National Accelerator Laboratory campus

    The DOE’s SLAC National Accelerator Laboratory originally named Stanford Linear Accelerator Center, is a Department of Energy National Laboratory operated by Stanford University under the programmatic direction of the Department of Energy Office of Science and located in Menlo Park, California. It is the site of the Stanford Linear Accelerator, a 3.2 kilometer (2-mile) linear accelerator constructed in 1966 and shut down in the 2000s, which could accelerate electrons to energies of 50 GeV.
    Today SLAC research centers on a broad program in atomic and solid-state physics, chemistry, biology, and medicine using X-rays from synchrotron radiation and a free-electron laser as well as experimental and theoretical research in elementary particle physics, astroparticle physics, and cosmology.

    Founded in 1962 as the Stanford Linear Accelerator Center, the facility is located on 172 hectares (426 acres) of Stanford University-owned land on Sand Hill Road in Menlo Park, California—just west of the University’s main campus. The main accelerator is 3.2 kilometers (2 mi) long—the longest linear accelerator in the world—and has been operational since 1966.

    Research at SLAC has produced three Nobel Prizes in Physics

    1976: The charm quark—see J/ψ meson
    1990: Quark structure inside protons and neutrons
    1995: The tau lepton

    SLAC’s meeting facilities also provided a venue for the Homebrew Computer Club and other pioneers of the home computer revolution of the late 1970s and early 1980s.

    In 1984 the laboratory was named an ASME National Historic Engineering Landmark and an IEEE Milestone.

    SLAC developed and, in December 1991, began hosting the first World Wide Web server outside of Europe.

    In the early-to-mid 1990s, the Stanford Linear Collider (SLC) investigated the properties of the Z boson using the Stanford Large Detector [below].

    As of 2005, SLAC employed over 1,000 people, some 150 of whom were physicists with doctorate degrees, and served over 3,000 visiting researchers yearly, operating particle accelerators for high-energy physics and the Stanford Synchrotron Radiation Laboratory (SSRL) [below] for synchrotron light radiation research, which was “indispensable” in the research leading to the 2006 Nobel Prize in Chemistry awarded to Stanford Professor Roger D. Kornberg.

    In October 2008, the Department of Energy announced that the center’s name would be changed to SLAC National Accelerator Laboratory. The reasons given include a better representation of the new direction of the lab and the ability to trademark the laboratory’s name. Stanford University had legally opposed the Department of Energy’s attempt to trademark “Stanford Linear Accelerator Center”.

    In March 2009, it was announced that the SLAC National Accelerator Laboratory was to receive $68.3 million in Recovery Act Funding to be disbursed by Department of Energy’s Office of Science.

    In October 2016, Bits and Watts launched as a collaboration between SLAC and Stanford University to design “better, greener electric grids”. SLAC later pulled out over concerns about an industry partner, the state-owned Chinese electric utility.

    Accelerator

    The main accelerator was an RF linear accelerator that accelerated electrons and positrons up to 50 GeV. At 3.2 km (2.0 mi) long, the accelerator was the longest linear accelerator in the world, and was claimed to be “the world’s most straight object.” until 2017 when the European x-ray free electron laser opened. The main accelerator is buried 9 m (30 ft) below ground and passes underneath Interstate Highway 280. The above-ground klystron gallery atop the beamline, was the longest building in the United States until the LIGO project’s twin interferometers were completed in 1999. It is easily distinguishable from the air and is marked as a visual waypoint on aeronautical charts.

    A portion of the original linear accelerator is now part of the Linac Coherent Light Source [below].

    Stanford Linear Collider

    The Stanford Linear Collider was a linear accelerator that collided electrons and positrons at SLAC. The center of mass energy was about 90 GeV, equal to the mass of the Z boson, which the accelerator was designed to study. Grad student Barrett D. Milliken discovered the first Z event on 12 April 1989 while poring over the previous day’s computer data from the Mark II detector. The bulk of the data was collected by the SLAC Large Detector, which came online in 1991. Although largely overshadowed by the Large Electron–Positron Collider at CERN, which began running in 1989, the highly polarized electron beam at SLC (close to 80%) made certain unique measurements possible, such as parity violation in Z Boson-b quark coupling.


    Presently no beam enters the south and north arcs in the machine, which leads to the Final Focus, therefore this section is mothballed to run beam into the PEP2 section from the beam switchyard.

    The SLAC Large Detector (SLD) was the main detector for the Stanford Linear Collider. It was designed primarily to detect Z bosons produced by the accelerator’s electron-positron collisions. Built in 1991, the SLD operated from 1992 to 1998.

    SLAC National Accelerator Laboratory Large Detector

    PEP

    PEP (Positron-Electron Project) began operation in 1980, with center-of-mass energies up to 29 GeV. At its apex, PEP had five large particle detectors in operation, as well as a sixth smaller detector. About 300 researchers made used of PEP. PEP stopped operating in 1990, and PEP-II began construction in 1994.

    PEP-II

    From 1999 to 2008, the main purpose of the linear accelerator was to inject electrons and positrons into the PEP-II accelerator, an electron-positron collider with a pair of storage rings 2.2 km (1.4 mi) in circumference. PEP-II was host to the BaBar experiment, one of the so-called B-Factory experiments studying charge-parity symmetry.

    SLAC National Accelerator Laboratory BaBar

    SLAC National Accelerator Laboratory SSRL

    Fermi Gamma-ray Space Telescope

    SLAC plays a primary role in the mission and operation of the Fermi Gamma-ray Space Telescope, launched in August 2008. The principal scientific objectives of this mission are:

    To understand the mechanisms of particle acceleration in AGNs, pulsars, and SNRs.
    To resolve the gamma-ray sky: unidentified sources and diffuse emission.
    To determine the high-energy behavior of gamma-ray bursts and transients.
    To probe dark matter and fundamental physics.

    National Aeronautics and Space Administration Fermi Large Area Telescope

    National Aeronautics and Space Administration Fermi Gamma Ray Space Telescope.

    KIPAC


    KIPAC campus

    The Stanford PULSE Institute (PULSE) is a Stanford Independent Laboratory located in the Central Laboratory at SLAC. PULSE was created by Stanford in 2005 to help Stanford faculty and SLAC scientists develop ultrafast x-ray research at LCLS.

    The Linac Coherent Light Source (LCLS)[below] is a free electron laser facility located at SLAC. The LCLS is partially a reconstruction of the last 1/3 of the original linear accelerator at SLAC, and can deliver extremely intense x-ray radiation for research in a number of areas. It achieved first lasing in April 2009.

    The laser produces hard X-rays, 10^9 times the relative brightness of traditional synchrotron sources and is the most powerful x-ray source in the world. LCLS enables a variety of new experiments and provides enhancements for existing experimental methods. Often, x-rays are used to take “snapshots” of objects at the atomic level before obliterating samples. The laser’s wavelength, ranging from 6.2 to 0.13 nm (200 to 9500 electron volts (eV)) is similar to the width of an atom, providing extremely detailed information that was previously unattainable. Additionally, the laser is capable of capturing images with a “shutter speed” measured in femtoseconds, or million-billionths of a second, necessary because the intensity of the beam is often high enough so that the sample explodes on the femtosecond timescale.

    The LCLS-II [below] project is to provide a major upgrade to LCLS by adding two new X-ray laser beams. The new system will utilize the 500 m (1,600 ft) of existing tunnel to add a new superconducting accelerator at 4 GeV and two new sets of undulators that will increase the available energy range of LCLS. The advancement from the discoveries using these new capabilities may include new drugs, next-generation computers, and new materials.

    FACET

    In 2012, the first two-thirds (~2 km) of the original SLAC LINAC were recommissioned for a new user facility, the Facility for Advanced Accelerator Experimental Tests (FACET). This facility was capable of delivering 20 GeV, 3 nC electron (and positron) beams with short bunch lengths and small spot sizes, ideal for beam-driven plasma acceleration studies. The facility ended operations in 2016 for the constructions of LCLS-II which will occupy the first third of the SLAC LINAC. The FACET-II project will re-establish electron and positron beams in the middle third of the LINAC for the continuation of beam-driven plasma acceleration studies in 2019.

    SLAC National Accelerator Laboratory FACET

    SLAC National Accelerator Laboratory FACET-II upgrading its Facility for Advanced Accelerator Experimental Tests (FACET) – a test bed for new technologies that could revolutionize the way we build particle accelerators.

    The Next Linear Collider Test Accelerator (NLCTA) is a 60-120 MeV high-brightness electron beam linear accelerator used for experiments on advanced beam manipulation and acceleration techniques. It is located at SLAC’s end station B

    SLAC National Accelerator Laboratory Next Linear Collider Test Accelerator (NLCTA)

    SLAC National Accelerator LaboratoryLCLS

    SLAC National Accelerator LaboratoryLCLS II projected view

    Magnets called undulators stretch roughly 100 meters down a tunnel at SLAC National Accelerator Laboratory, with one side (right) producing hard x-rays and the other soft x-rays.

    SSRL and LCLS are DOE Office of Science user facilities.

    Stanford University campus

    Leland and Jane Stanford founded Stanford University to “promote the public welfare by exercising an influence on behalf of humanity and civilization.” Stanford opened its doors in 1891, and more than a century later, it remains dedicated to finding solutions to the great challenges of the day and to preparing our students for leadership in today’s complex world. Stanford, is an American private research university located in Stanford, California on an 8,180-acre (3,310 ha) campus near Palo Alto. Since 1952, more than 54 Stanford faculty, staff, and alumni have won the Nobel Prize, including 19 current faculty members.

    Stanford University, officially Leland Stanford Junior University, is a private research university located in Stanford, California. Stanford was founded in 1885 by Leland and Jane Stanford in memory of their only child, Leland Stanford Jr., who had died of typhoid fever at age 15 the previous year. Stanford is consistently ranked as among the most prestigious and top universities in the world by major education publications. It is also one of the top fundraising institutions in the country, becoming the first school to raise more than a billion dollars in a year.

    Leland Stanford was a U.S. senator and former governor of California who made his fortune as a railroad tycoon. The school admitted its first students on October 1, 1891, as a coeducational and non-denominational institution. Stanford University struggled financially after the death of Leland Stanford in 1893 and again after much of the campus was damaged by the 1906 San Francisco earthquake. Following World War II, provost Frederick Terman supported faculty and graduates’ entrepreneurialism to build self-sufficient local industry in what would later be known as Silicon Valley.

    The university is organized around seven schools: three schools consisting of 40 academic departments at the undergraduate level as well as four professional schools that focus on graduate programs in law, medicine, education, and business. All schools are on the same campus. Students compete in 36 varsity sports, and the university is one of two private institutions in the Division I FBS Pac-12 Conference. It has gained 126 NCAA team championships, and Stanford has won the NACDA Directors’ Cup for 24 consecutive years, beginning in 1994–1995. In addition, Stanford students and alumni have won 270 Olympic medals including 139 gold medals.

    As of October 2020, 84 Nobel laureates, 28 Turing Award laureates, and eight Fields Medalists have been affiliated with Stanford as students, alumni, faculty, or staff. In addition, Stanford is particularly noted for its entrepreneurship and is one of the most successful universities in attracting funding for start-ups. Stanford alumni have founded numerous companies, which combined produce more than $2.7 trillion in annual revenue, roughly equivalent to the 7th largest economy in the world (as of 2020). Stanford is the alma mater of one president of the United States (Herbert Hoover), 74 living billionaires, and 17 astronauts. It is also one of the leading producers of Fulbright Scholars, Marshall Scholars, Rhodes Scholars, and members of the United States Congress.

    Stanford University was founded in 1885 by Leland and Jane Stanford, dedicated to Leland Stanford Jr, their only child. The institution opened in 1891 on Stanford’s previous Palo Alto farm.

    Jane and Leland Stanford modeled their university after the great eastern universities, most specifically Cornell University. Stanford opened being called the “Cornell of the West” in 1891 due to faculty being former Cornell affiliates (either professors, alumni, or both) including its first president, David Starr Jordan, and second president, John Casper Branner. Both Cornell and Stanford were among the first to have higher education be accessible, nonsectarian, and open to women as well as to men. Cornell is credited as one of the first American universities to adopt this radical departure from traditional education, and Stanford became an early adopter as well.

    Despite being impacted by earthquakes in both 1906 and 1989, the campus was rebuilt each time. In 1919, The Hoover Institution on War, Revolution and Peace was started by Herbert Hoover to preserve artifacts related to World War I. The Stanford Medical Center, completed in 1959, is a teaching hospital with over 800 beds. The DOE’s SLAC National Accelerator Laboratory (originally named the Stanford Linear Accelerator Center), established in 1962, performs research in particle physics.

    Land

    Most of Stanford is on an 8,180-acre (12.8 sq mi; 33.1 km^2) campus, one of the largest in the United States. It is located on the San Francisco Peninsula, in the northwest part of the Santa Clara Valley (Silicon Valley) approximately 37 miles (60 km) southeast of San Francisco and approximately 20 miles (30 km) northwest of San Jose. In 2008, 60% of this land remained undeveloped.

    Stanford’s main campus includes a census-designated place within unincorporated Santa Clara County, although some of the university land (such as the Stanford Shopping Center and the Stanford Research Park) is within the city limits of Palo Alto. The campus also includes much land in unincorporated San Mateo County (including the SLAC National Accelerator Laboratory and the Jasper Ridge Biological Preserve), as well as in the city limits of Menlo Park (Stanford Hills neighborhood), Woodside, and Portola Valley.

    Non-central campus

    Stanford currently operates in various locations outside of its central campus.

    On the founding grant:

    Jasper Ridge Biological Preserve is a 1,200-acre (490 ha) natural reserve south of the central campus owned by the university and used by wildlife biologists for research.

    SLAC National Accelerator Laboratory is a facility west of the central campus operated by the university for the Department of Energy. It contains the longest linear particle accelerator in the world, 2 miles (3.2 km) on 426 acres (172 ha) of land. Golf course and a seasonal lake: The university also has its own golf course and a seasonal lake (Lake Lagunita, actually an irrigation reservoir), both home to the vulnerable California tiger salamander. As of 2012 Lake Lagunita was often dry and the university had no plans to artificially fill it.

    Off the founding grant:

    Hopkins Marine Station, in Pacific Grove, California, is a marine biology research center owned by the university since 1892., in Pacific Grove, California, is a marine biology research center owned by the university since 1892.
    Study abroad locations: unlike typical study abroad programs, Stanford itself operates in several locations around the world; thus, each location has Stanford faculty-in-residence and staff in addition to students, creating a “mini-Stanford”.

    Redwood City campus for many of the university’s administrative offices located in Redwood City, California, a few miles north of the main campus. In 2005, the university purchased a small, 35-acre (14 ha) campus in Midpoint Technology Park intended for staff offices; development was delayed by The Great Recession. In 2015 the university announced a development plan and the Redwood City campus opened in March 2019.

    The Bass Center in Washington, DC provides a base, including housing, for the Stanford in Washington program for undergraduates. It includes a small art gallery open to the public.

    China: Stanford Center at Peking University, housed in the Lee Jung Sen Building, is a small center for researchers and students in collaboration with Beijing University [北京大学](CN) (Kavli Institute for Astronomy and Astrophysics at Peking University(CN) (KIAA-PKU).

    Administration and organization

    Stanford is a private, non-profit university that is administered as a corporate trust governed by a privately appointed board of trustees with a maximum membership of 38. Trustees serve five-year terms (not more than two consecutive terms) and meet five times annually.[83] A new trustee is chosen by the current trustees by ballot. The Stanford trustees also oversee the Stanford Research Park, the Stanford Shopping Center, the Cantor Center for Visual Arts, Stanford University Medical Center, and many associated medical facilities (including the Lucile Packard Children’s Hospital).

    The board appoints a president to serve as the chief executive officer of the university, to prescribe the duties of professors and course of study, to manage financial and business affairs, and to appoint nine vice presidents. The provost is the chief academic and budget officer, to whom the deans of each of the seven schools report. Persis Drell became the 13th provost in February 2017.

    As of 2018, the university was organized into seven academic schools. The schools of Humanities and Sciences (27 departments), Engineering (nine departments), and Earth, Energy & Environmental Sciences (four departments) have both graduate and undergraduate programs while the Schools of Law, Medicine, Education and Business have graduate programs only. The powers and authority of the faculty are vested in the Academic Council, which is made up of tenure and non-tenure line faculty, research faculty, senior fellows in some policy centers and institutes, the president of the university, and some other academic administrators, but most matters are handled by the Faculty Senate, made up of 55 elected representatives of the faculty.

    The Associated Students of Stanford University (ASSU) is the student government for Stanford and all registered students are members. Its elected leadership consists of the Undergraduate Senate elected by the undergraduate students, the Graduate Student Council elected by the graduate students, and the President and Vice President elected as a ticket by the entire student body.

    Stanford is the beneficiary of a special clause in the California Constitution, which explicitly exempts Stanford property from taxation so long as the property is used for educational purposes.

    Endowment and donations

    The university’s endowment, managed by the Stanford Management Company, was valued at $27.7 billion as of August 31, 2019. Payouts from the Stanford endowment covered approximately 21.8% of university expenses in the 2019 fiscal year. In the 2018 NACUBO-TIAA survey of colleges and universities in the United States and Canada, only Harvard University, the University of Texas System, and Yale University had larger endowments than Stanford.

    In 2006, President John L. Hennessy launched a five-year campaign called the Stanford Challenge, which reached its $4.3 billion fundraising goal in 2009, two years ahead of time, but continued fundraising for the duration of the campaign. It concluded on December 31, 2011, having raised a total of $6.23 billion and breaking the previous campaign fundraising record of $3.88 billion held by Yale. Specifically, the campaign raised $253.7 million for undergraduate financial aid, as well as $2.33 billion for its initiative in “Seeking Solutions” to global problems, $1.61 billion for “Educating Leaders” by improving K-12 education, and $2.11 billion for “Foundation of Excellence” aimed at providing academic support for Stanford students and faculty. Funds supported 366 new fellowships for graduate students, 139 new endowed chairs for faculty, and 38 new or renovated buildings. The new funding also enabled the construction of a facility for stem cell research; a new campus for the business school; an expansion of the law school; a new Engineering Quad; a new art and art history building; an on-campus concert hall; a new art museum; and a planned expansion of the medical school, among other things. In 2012, the university raised $1.035 billion, becoming the first school to raise more than a billion dollars in a year.

    Research centers and institutes

    DOE’s SLAC National Accelerator Laboratory
    Stanford Research Institute, a center of innovation to support economic development in the region.
    Hoover Institution, a conservative American public policy institution and research institution that promotes personal and economic liberty, free enterprise, and limited government.
    Hasso Plattner Institute of Design, a multidisciplinary design school in cooperation with the Hasso Plattner Institute of University of Potsdam [Universität Potsdam](DE) that integrates product design, engineering, and business management education).
    Martin Luther King Jr. Research and Education Institute, which grew out of and still contains the Martin Luther King Jr. Papers Project.
    John S. Knight Fellowship for Professional Journalists
    Center for Ocean Solutions
    Together with UC Berkeley and UC San Francisco, Stanford is part of the Biohub, a new medical science research center founded in 2016 by a $600 million commitment from Facebook CEO and founder Mark Zuckerberg and pediatrician Priscilla Chan.

    Discoveries and innovation

    Natural sciences

    Biological synthesis of deoxyribonucleic acid (DNA) – Arthur Kornberg synthesized DNA material and won the Nobel Prize in Physiology or Medicine 1959 for his work at Stanford.
    First Transgenic organism – Stanley Cohen and Herbert Boyer were the first scientists to transplant genes from one living organism to another, a fundamental discovery for genetic engineering. Thousands of products have been developed on the basis of their work, including human growth hormone and hepatitis B vaccine.
    Laser – Arthur Leonard Schawlow shared the 1981 Nobel Prize in Physics with Nicolaas Bloembergen and Kai Siegbahn for his work on lasers.
    Nuclear magnetic resonance – Felix Bloch developed new methods for nuclear magnetic precision measurements, which are the underlying principles of the MRI.

    Computer and applied sciences

    ARPANETStanford Research Institute, formerly part of Stanford but on a separate campus, was the site of one of the four original ARPANET nodes.

    Internet—Stanford was the site where the original design of the Internet was undertaken. Vint Cerf led a research group to elaborate the design of the Transmission Control Protocol (TCP/IP) that he originally co-created with Robert E. Kahn (Bob Kahn) in 1973 and which formed the basis for the architecture of the Internet.

    Frequency modulation synthesis – John Chowning of the Music department invented the FM music synthesis algorithm in 1967, and Stanford later licensed it to Yamaha Corporation.

    Google – Google began in January 1996 as a research project by Larry Page and Sergey Brin when they were both PhD students at Stanford. They were working on the Stanford Digital Library Project (SDLP). The SDLP’s goal was “to develop the enabling technologies for a single, integrated and universal digital library” and it was funded through the National Science Foundation, among other federal agencies.

    Klystron tube – invented by the brothers Russell and Sigurd Varian at Stanford. Their prototype was completed and demonstrated successfully on August 30, 1937. Upon publication in 1939, news of the klystron immediately influenced the work of U.S. and UK researchers working on radar equipment.

    RISCARPA funded VLSI project of microprocessor design. Stanford and University of California- Berkeley are most associated with the popularization of this concept. The Stanford MIPS would go on to be commercialized as the successful MIPS architecture, while Berkeley RISC gave its name to the entire concept, commercialized as the SPARC. Another success from this era were IBM’s efforts that eventually led to the IBM POWER instruction set architecture, PowerPC, and Power ISA. As these projects matured, a wide variety of similar designs flourished in the late 1980s and especially the early 1990s, representing a major force in the Unix workstation market as well as embedded processors in laser printers, routers and similar products.
    SUN workstation – Andy Bechtolsheim designed the SUN workstation for the Stanford University Network communications project as a personal CAD workstation, which led to Sun Microsystems.

    Businesses and entrepreneurship

    Stanford is one of the most successful universities in creating companies and licensing its inventions to existing companies; it is often held up as a model for technology transfer. Stanford’s Office of Technology Licensing is responsible for commercializing university research, intellectual property, and university-developed projects.

    The university is described as having a strong venture culture in which students are encouraged, and often funded, to launch their own companies.

    Companies founded by Stanford alumni generate more than $2.7 trillion in annual revenue, equivalent to the 10th-largest economy in the world.

    Some companies closely associated with Stanford and their connections include:

    Hewlett-Packard, 1939, co-founders William R. Hewlett (B.S, PhD) and David Packard (M.S).
    Silicon Graphics, 1981, co-founders James H. Clark (Associate Professor) and several of his grad students.
    Sun Microsystems, 1982, co-founders Vinod Khosla (M.B.A), Andy Bechtolsheim (PhD) and Scott McNealy (M.B.A).
    Cisco, 1984, founders Leonard Bosack (M.S) and Sandy Lerner (M.S) who were in charge of Stanford Computer Science and Graduate School of Business computer operations groups respectively when the hardware was developed.[163]
    Yahoo!, 1994, co-founders Jerry Yang (B.S, M.S) and David Filo (M.S).
    Google, 1998, co-founders Larry Page (M.S) and Sergey Brin (M.S).
    LinkedIn, 2002, co-founders Reid Hoffman (B.S), Konstantin Guericke (B.S, M.S), Eric Lee (B.S), and Alan Liu (B.S).
    Instagram, 2010, co-founders Kevin Systrom (B.S) and Mike Krieger (B.S).
    Snapchat, 2011, co-founders Evan Spiegel and Bobby Murphy (B.S).
    Coursera, 2012, co-founders Andrew Ng (Associate Professor) and Daphne Koller (Professor, PhD).

    Student body

    Stanford enrolled 6,996 undergraduate and 10,253 graduate students as of the 2019–2020 school year. Women comprised 50.4% of undergraduates and 41.5% of graduate students. In the same academic year, the freshman retention rate was 99%.

    Stanford awarded 1,819 undergraduate degrees, 2,393 master’s degrees, 770 doctoral degrees, and 3270 professional degrees in the 2018–2019 school year. The four-year graduation rate for the class of 2017 cohort was 72.9%, and the six-year rate was 94.4%. The relatively low four-year graduation rate is a function of the university’s coterminal degree (or “coterm”) program, which allows students to earn a master’s degree as a 1-to-2-year extension of their undergraduate program.

    As of 2010, fifteen percent of undergraduates were first-generation students.

    Athletics

    As of 2016 Stanford had 16 male varsity sports and 20 female varsity sports, 19 club sports and about 27 intramural sports. In 1930, following a unanimous vote by the Executive Committee for the Associated Students, the athletic department adopted the mascot “Indian.” The Indian symbol and name were dropped by President Richard Lyman in 1972, after objections from Native American students and a vote by the student senate. The sports teams are now officially referred to as the “Stanford Cardinal,” referring to the deep red color, not the cardinal bird. Stanford is a member of the Pac-12 Conference in most sports, the Mountain Pacific Sports Federation in several other sports, and the America East Conference in field hockey with the participation in the inter-collegiate NCAA’s Division I FBS.

    Its traditional sports rival is the University of California, Berkeley, the neighbor to the north in the East Bay. The winner of the annual “Big Game” between the Cal and Cardinal football teams gains custody of the Stanford Axe.

    Stanford has had at least one NCAA team champion every year since the 1976–77 school year and has earned 126 NCAA national team titles since its establishment, the most among universities, and Stanford has won 522 individual national championships, the most by any university. Stanford has won the award for the top-ranked Division 1 athletic program—the NACDA Directors’ Cup, formerly known as the Sears Cup—annually for the past twenty-four straight years. Stanford athletes have won medals in every Olympic Games since 1912, winning 270 Olympic medals total, 139 of them gold. In the 2008 Summer Olympics, and 2016 Summer Olympics, Stanford won more Olympic medals than any other university in the United States. Stanford athletes won 16 medals at the 2012 Summer Olympics (12 gold, two silver and two bronze), and 27 medals at the 2016 Summer Olympics.

    Traditions

    The unofficial motto of Stanford, selected by President Jordan, is Die Luft der Freiheit weht. Translated from the German language, this quotation from Ulrich von Hutten means, “The wind of freedom blows.” The motto was controversial during World War I, when anything in German was suspect; at that time the university disavowed that this motto was official.
    Hail, Stanford, Hail! is the Stanford Hymn sometimes sung at ceremonies or adapted by the various University singing groups. It was written in 1892 by mechanical engineering professor Albert W. Smith and his wife, Mary Roberts Smith (in 1896 she earned the first Stanford doctorate in Economics and later became associate professor of Sociology), but was not officially adopted until after a performance on campus in March 1902 by the Mormon Tabernacle Choir.
    “Uncommon Man/Uncommon Woman”: Stanford does not award honorary degrees, but in 1953 the degree of “Uncommon Man/Uncommon Woman” was created to recognize individuals who give rare and extraordinary service to the University. Technically, this degree is awarded by the Stanford Associates, a voluntary group that is part of the university’s alumni association. As Stanford’s highest honor, it is not conferred at prescribed intervals, but only when appropriate to recognize extraordinary service. Recipients include Herbert Hoover, Bill Hewlett, Dave Packard, Lucile Packard, and John Gardner.
    Big Game events: The events in the week leading up to the Big Game vs. UC Berkeley, including Gaieties (a musical written, composed, produced, and performed by the students of Ram’s Head Theatrical Society).
    “Viennese Ball”: a formal ball with waltzes that was initially started in the 1970s by students returning from the now-closed Stanford in Vienna overseas program. It is now open to all students.
    “Full Moon on the Quad”: An annual event at Main Quad, where students gather to kiss one another starting at midnight. Typically organized by the Junior class cabinet, the festivities include live entertainment, such as music and dance performances.
    “Band Run”: An annual festivity at the beginning of the school year, where the band picks up freshmen from dorms across campus while stopping to perform at each location, culminating in a finale performance at Main Quad.
    “Mausoleum Party”: An annual Halloween Party at the Stanford Mausoleum, the final resting place of Leland Stanford Jr. and his parents. A 20-year tradition, the “Mausoleum Party” was on hiatus from 2002 to 2005 due to a lack of funding, but was revived in 2006. In 2008, it was hosted in Old Union rather than at the actual Mausoleum, because rain prohibited generators from being rented. In 2009, after fundraising efforts by the Junior Class Presidents and the ASSU Executive, the event was able to return to the Mausoleum despite facing budget cuts earlier in the year.
    Former campus traditions include the “Big Game bonfire” on Lake Lagunita (a seasonal lake usually dry in the fall), which was formally ended in 1997 because of the presence of endangered salamanders in the lake bed.

    Award laureates and scholars

    Stanford’s current community of scholars includes:

    19 Nobel Prize laureates (as of October 2020, 85 affiliates in total)
    171 members of the National Academy of Sciences
    109 members of National Academy of Engineering
    76 members of National Academy of Medicine
    288 members of the American Academy of Arts and Sciences
    19 recipients of the National Medal of Science
    1 recipient of the National Medal of Technology
    4 recipients of the National Humanities Medal
    49 members of American Philosophical Society
    56 fellows of the American Physics Society (since 1995)
    4 Pulitzer Prize winners
    31 MacArthur Fellows
    4 Wolf Foundation Prize winners
    2 ACL Lifetime Achievement Award winners
    14 AAAI fellows
    2 Presidential Medal of Freedom winners

     
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