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  • richardmitnick 9:29 pm on October 17, 2018 Permalink | Reply
    Tags: , , , , Gemini Near-Infrared Spectrograph on Gemini North, , , Hawaii USA, Mauna Kea, Sierra Remote Observatory, The core-collapse supernova 2017eaw   

    From Gemini Observatory: “Nearby Supernova Sheds Light on Ancient Dust” 

    NOAO

    Gemini Observatory
    From Gemini Observatory

    October 16, 2018

    Thanks to two allocations of Director’s Discretionary Time and a successful Fast-Turnaround program, an international team (including Gemini Emeritus Astronomer Tom Geballe, who wrote this summary on behalf of the team) used Gemini North/GNIRS to follow the evolution of the near-infrared spectrum of the core-collapse supernova 2017eaw (ccSN 2017eaw) over three semesters.

    Gemini Near-Infrared Spectrograph on Gemini North, Mauna Kea, Hawaii USA

    The data obtained from this relatively nearby event may help us to better understand the existence of dusty galaxies in the early, much more distant Universe.

    One of the unexpected discoveries in studies of the very early Universe is that many high redshift galaxies are “dusty.” These dusty galaxies exist as recently as several hundred million to a billion years after the Big Bang. The origin of this dust is somewhat of a mystery, because stars with masses similar to the Sun, which constitute the vast majority of stars in a galaxy, would not have evolved to the dust-producing stage in such a short time. Thus, there must be another source of dust in these very distant and very young galaxies.

    __________________________________________________
    Where Does Interstellar Dust Originate?

    Interstellar dust constitutes about 1% of the mass of interstellar matter in our Milky Way and in many other galaxies. It is generally understood that the origin of most of that dust is stars with masses roughly similar to that of our Sun, that became red giants and ejected their outer layers into space. Although initially almost entirely hydrogen and helium, during the red giant phase the outer layers of those stars are polluted by heavier elements such as carbon, nitrogen, oxygen, silicon, magnesium, and many others that are produced by thermonuclear reactions deep inside the stars and then mixed into the outer layers. Once the ejecta cool to temperatures lower than about 2,000 K, dust particles inevitably start to form out of these heavy elements. However, it is billions of years after these stars formed when this happens. On the other hand, core collapse supernovae live only a few millions to a few tens of millions of years before they explode, during which time they turn most of their hydrogen-rich and helium-rich interiors into vast reservoirs of heavy elements. Thus, unlike stars like the Sun, massive stars are potential dust-producers in the early Universe.
    __________________________________________________

    One possible source is the ejecta from massive stars that explode after only a few millions to a few tens of millions of years after they form, the so-called core-collapse supernovae (ccSNe).

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    Figure 1. Image of spiral galaxy NGC 6946 and SN 2017eaw indicated by arrow. Photo courtesy of Damian Peach, obtained on May 28th, 2017, at 10:31 UTC from the Sierra Remote Observatory, California.

    Sierra Remote Observatory in the Sierra Nevada Mountains, a mountain range in the Western United States, between the Central Valley of California and the Great Basin

    2
    The Great Basin is the largest area of contiguous endorheic watersheds in North America. It spans nearly all of Nevada, much of Oregon and Utah, and portions of California, Idaho, and Wyoming.

    While we cannot study individual supernovae in such distant galaxies, we can find examples of them in the nearby Universe. Infrared- and millimeter-wave observations of several “local” examples have revealed that ccSNe can produce copious amounts of dust — up to one solar mass for each event. Until now, however, detailed evolution of dust production in such supernovae, which can take place over several years, has only been followed in one object: the very nearby, famous, and rather unusual ccSN 1987A in the Large Magellanic Cloud. Fortuitously, our recent observations of ccSN 2017eaw in the nearby galaxy NGC 6946 provided another rare opportunity to follow that evolution in detail over an extended period. NGC 6946 is located about 7 megaparsecs away and is popularly known as the Fireworks Galaxy, because it is a prodigious supplier of supernovae (see Figure 1 and a pre-SN 2017eaw Gemini Legacy Image of NGC 6946).

    SN 2017eaw was discovered on May 14, 2017, just as its host galaxy, NGC 6946, became observable in the eastern sky before dawn. Because of its high northerly location, we saw an opportunity to follow SN 2017eaw continuously from May until December (before it became too low in the western sky to observe from Maunakea) and proposed the idea to Gemini Observatory. Thanks to two allocations of Director’s Discretionary Time and a successful Fast-Turnaround program, the team led by Jeonghee Rho (SETI Institute) was able to follow the evolution of the supernova’s near-infrared (0.84-2.52 micron) spectrum in Semesters 2017A, 2017B, and 2018A. The team also includes Tom Geballe (Gemini Observatory), Dipankar Banerjee and Vishal Joshi (Physical Research Laboratory, Ahmedabad, India), Nye Evans (Keele University, U.K.), and Luc Dessart (Universidad de Chile).

    During 2017-18, we obtained Gemini North/GNIRS (Gemini Near-InfraRed Spectrometer) data on ten dates between 22 and 387 days after the discovery. It is believed that these data represent the highest quality and most extensive near-infrared time-sequence of spectra ever obtained for a Type II-P SN, the most common type of ccSN, whose light curve has a distinctive flat stretch (called a plateau).

    The first nine of these spectra, obtained in 2017, are shown in Figure 2. While they are a goldmine of information — revealing details on elemental abundances, nucleosynthesis, changes in ionization, and velocities of the ejecta — our major goal was to witness and model the formation of the molecule carbon monoxide (CO) and dust, which is quite hot when it forms. Information on these species is contained only at the long wavelength end of the spectra, from 2.0 to 2.5 microns.

    CO is important because it is a powerful coolant of the ejecta, which aids in making dust formation possible. Its presence is clearly detected on day 124 by the sharp increase in signal near 2.30 microns, and we think it was already marginally present at day 107. The dust signature also begins at day 124, and is the flattening slope of the continuum from 2.1 microns to longer wavelengths, compared to the steadily decreasing continuum signal at shorter wavelengths, and across the entire spectrum at earlier times.

    We have used the spectra to estimate the CO mass produced by SN 2017eaw and find that it is qualitatively matched by models in the literature of a progenitor star of mass roughly 15 times that of the Sun. Fits to the continuum indicate that the temperature of the dust emitting at 2.1-2.5 microns is ~ 1,300 K and that the dust is mainly graphitic, which, unlike amorphous carbon, can condense at higher temperatures than this. Discussion of these and other results and analysis are reported in Rho et al., The Astrophysical Journal Letters, 864: L20, 2018.

    We are continuing our monitoring of SN 2017eaw in Semester 2018B; thereafter it will be too faint. In future semesters, we hope to measure additional nearby ccSNe that occur in order to estimate the frequency of CO and dust production by such SNe, as well as the masses of CO and dust produced by each.

    See the full article here .


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    Gemini/North telescope at Maunakea, Hawaii, USA,4,207 m (13,802 ft) above sea level

    Gemini South telescope, Cerro Tololo Inter-American Observatory (CTIO) campus near La Serena, Chile, at an altitude of 7200 feet

    AURA Icon

    Gemini’s mission is to advance our knowledge of the Universe by providing the international Gemini Community with forefront access to the entire sky.

    The Gemini Observatory is an international collaboration with two identical 8-meter telescopes. The Frederick C. Gillett Gemini Telescope is located on Mauna Kea, Hawai’i (Gemini North) and the other telescope on Cerro Pachón in central Chile (Gemini South); together the twin telescopes provide full coverage over both hemispheres of the sky. The telescopes incorporate technologies that allow large, relatively thin mirrors, under active control, to collect and focus both visible and infrared radiation from space.

    The Gemini Observatory provides the astronomical communities in six partner countries with state-of-the-art astronomical facilities that allocate observing time in proportion to each country’s contribution. In addition to financial support, each country also contributes significant scientific and technical resources. The national research agencies that form the Gemini partnership include: the US National Science Foundation (NSF), the Canadian National Research Council (NRC), the Chilean Comisión Nacional de Investigación Cientifica y Tecnológica (CONICYT), the Australian Research Council (ARC), the Argentinean Ministerio de Ciencia, Tecnología e Innovación Productiva, and the Brazilian Ministério da Ciência, Tecnologia e Inovação. The observatory is managed by the Association of Universities for Research in Astronomy, Inc. (AURA) under a cooperative agreement with the NSF. The NSF also serves as the executive agency for the international partnership.

     
  • richardmitnick 11:56 am on November 30, 2015 Permalink | Reply
    Tags: , , Mauna Kea,   

    From NASA Earth: “Mauna Kea Volcano, Hawaii” 

    NASA Earth Observatory

    NASA Earth Observatory

    1
    acquired November 1, 2015

    Mauna Kea (“White Mountain”) is the only volcano on the island of Hawaii that has evidence of glaciation. This photograph of Mauna Kea was taken by an astronaut as the International Space Station (ISS) passed over at approximately 5 p.m. local time. The late-afternoon lighting and oblique viewing angle accentuates the shadows, highlighting the white domes of the observatories along the crater rims.

    The major observatories
    Keck Observatory
    Keck

    CFHT
    Canada France Hawaii Telescope

    NAOJ Subaru Telescope
    NAOJ/Subaru

    The angle also accentuates the numerous cinder cones and lava flows. Astronauts are often deprived of a three-dimensional sense of mountains because the ISS flies so far above Earth’s surface. But the low Sun angle here gives a strong sense of the domed shape of this immense volcano.

    Several observatories appear as small white dots on the rim of Mauna Kea. As the highest volcano on the island of Hawaii (summit elevation 4,205 meters or 13,800 feet above sea level), it is an ideal location for the astronomical observatories set up by several countries and academic consortiums.

    Although Mauna Kea last erupted in 2460 BCE, the potential for renewed activity is high. Neighboring Mauna Loa volcano has erupted approximately every six years for the past 3,000 years.

    See the full article here .

    Please help promote STEM in your local schools.

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    The Earth Observatory’s mission is to share with the public the images, stories, and discoveries about climate and the environment that emerge from NASA research, including its satellite missions, in-the-field research, and climate models. The Earth Observatory staff is supported by the Climate and Radiation Laboratory, and the Hydrospheric and Biospheric Sciences Laboratory located at NASA Goddard Space Flight Center.

     
  • richardmitnick 7:45 am on August 7, 2015 Permalink | Reply
    Tags: , , , Mauna Kea   

    From ABC: “A Look at the Science on Hawaii’s Mauna Kea” 

    ABC News bloc

    ABC News

    Aug 7, 2015
    CALEB JONES, Associated Press

    Atop Hawaii’s Mauna Kea, where some Native Hawaiians have been peacefully protesting the construction of what would be one of the world’s largest telescopes, astronomers have spent the last 40 years observing our universe and helping make some of the most significant discoveries in their field.

    If the highly contested Thirty Meter Telescope {TMT] is constructed on the site, scientists say they will be able to explore more of the universe’s unsolved mysteries.

    TMT
    Proposed TMT

    Many Native Hawaiians, however, consider the land sacred.

    Looking back billions of years in time, astronomers on Mauna Kea continue to peer into the most distant reaches of our early universe, allowing them to see the time immediately following the cosmic dark ages and the big bang.

    Here’s a look at what makes Mauna Kea such a valuable place for both science and the Hawaiian culture.

    WHAT KIND OF SCIENCE IS CURRENTLY BEING DONE ON MAUNA KEA?

    The 13 telescopes currently in place on the summit of Mauna Kea, Hawaii’s highest point, have played major roles in discoveries considered among the most significant to astronomy.

    Keck Observatory
    Keck Observatory Interior
    Keck Observatory

    CFHT Telescope
    CFHT nterior
    Canada France Hawaii Telescope
    Above, two of the most important science machines on Mauna Kea

    While astronomers often use many different telescopes in locations around the world to draw their conclusions, Guenther Hasinger, director of Mauna Kea’s Institute for Astronomy, said “there is almost no major astronomical discovery where there was not very important input from the telescopes on Mauna Kea.”

    Scientists at Mauna Kea have helped identify the presence of dark energy, discover a black hole in our galaxy and learn about potentially habitable planets in other solar systems, just to name a few.

    “The fact that there are other planets out there at some point will change our perspective in a similar way, as the first picture of the Earth taken from the moon did,” said Hasinger. “We might be able to fly to them at some point.”

    Mike Brown, an astronomer and professor at the California Institute of Technology, used Mauna Kea telescopes to help reclassify Pluto as a dwarf planet.

    WHY IS MAUNA KEA SO PERFECT?

    In order to tap the full potential of the kind of telescopes being used on Mauna Kea and other similar sites, scientists say you must have a number of conditions present. First, the summit of Mauna Kea, on the Big Island, is nearly 14,000 feet above sea level, above 50 percent of the Earth’s atmosphere. It is very dark, nestled in the crater of a dormant volcano far away from any large cities that would create light pollution. The consistently warm ocean water that surrounds the island helps keep the atmosphere stable.

    According to award-winning astronomer Andrea Ghez, a professor at the University of California Los Angeles who has published the most compelling proof of black holes to date, Mauna Kea is “the best place in the world to do astronomy.”

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    Andrea Ghez

    “Being in the middle of the ocean is geographically perfect,” she said.

    It also helps to be located somewhere with easy access to technology.

    “Places that are not developed tend not to be near places that can support technological endeavors,” she said. “Hawaii is one of the few places where you hit all three, which is why everybody in the world wants to build their telescopes there.”

    See the full article here.

    Please help promote STEM in your local schools.

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