Tagged: CFH Telescope Toggle Comment Threads | Keyboard Shortcuts

  • richardmitnick 5:23 pm on May 26, 2015 Permalink | Reply
    Tags: , , CFH Telescope   

    From CFHT: “Faint Galaxies found Hiding in the Virgo Cluster” 

    CFHT icon
    Canada France Hawaii Telescope

    May 26, 2015

    Science Contact information
    James Taylor
    University of Waterloo
    taylor@uwaterloo.ca

    Dr. Laura Ferrarese
    NGVS Principal Investigator
    laura.ferrarese@nrc-cnrc.gc.ca

    Media Contact information
    Leslie Sage
    CASCA Press Officer
    cascapressofficer@gmail.com

    Mary Beth Laychak
    CFHT Outreach Program Manager
    mary@cfht.hawaii.edu

    1
    Example of a Low Surface Brightness Galaxy in the Virgo cluster. These galaxies are very hard to detect and the LSB mode on MegaCam enabled the possibility of such detections.

    A recent survey using the Canada-France-Hawaii Telescope has discovered hundreds of new galaxies in the Virgo Cluster, the nearest large cluster of galaxies.

    2
    Virgo Cluster showing the diffuse light between member galaxies. Messier 87 is the largest galaxy (lower left)

    Most are extremely faint “dwarf” galaxies, objects hundreds of thousands of times less massive than our own galaxy, the Milky Way, and amongst the faintest galaxies known in the Universe. The Virgo cluster appears to be home to far more of such faint systems than the “Local Group” of galaxies to which the Milky Way belongs, suggesting that galaxy formation on small scales may be more complicated than previously thought, and that our Local Group may not be a typical corner of the universe.

    3
    The Local Group of galaxies. The Milky Way and Andromeda are the most massive galaxies by far.

    The discovery has been announced by the “Next Generation Virgo Cluster Survey” (NGVS) team and is based on data collected, over the course of 6 years, with Megacam, a 340 Megapixel camera operating at the Canada France Hawaii Telescope and capable of observing, in a single shot, a one square degree field of view (equivalent to 4 full moons). Taking advantage of MegaCam’s wide angle coverage, the NGVS team was able to observe the Virgo cluster in its entirety, covering an area of the sky equivalent to over 400 full moons, at a depth and resolution that significantly exceed those of any existing surveys of the cluster. The resulting mosaic, comprising nearly 40 billion pixels, is the deepest, widest contiguous field ever seen is such detail.

    To exploit the full power of the data, Laura Ferrarese, Lauren McArthur and Patrick Cote of the National Research Council of Canada developed a sophisticated data analysis technique that allowed them to discover many times more galaxies than were known previously, including some of the faintest and most diffuse objects ever detected.

    Virgo is the nearest large cluster of galaxies, roughly 50 Million light-years away from us. Whereas the Milky Way forms part of a relatively small group of galaxies, the “Local Group”, spread over the nearest few million light-years, Virgo contains dozens of bright galaxies and thousands of fainter ones. In the Local Group, the current theories of galaxy formation suggest there should be hundreds or thousands of dwarf galaxies, but fewer than 100 have been detected. Clusters such as Virgo were known to be richer hunting grounds for dwarfs, but only recently has the NGVS made it possible to set firm constraints on their numbers.

    To understand the implications of these new discoveries, Jonathan Grossauer and James Taylor at the University of Waterloo ran computer simulations of clusters like Virgo, to see how many bound concentrations of dark matter they should contain at the present day. Comparing the numbers and masses of dark matter clumps to the population of galaxies discovered by the NGVS, they find a very simple pattern, where the ratio of stellar to dark matter mass changes slowly going from the smallest to the largest galaxies. It seems that in Virgo, there could be a simple relationship between dark matter mass and galaxy brightness, valid over a factor of 100,000 in stellar mass.

    This is not the case in the Local Group: the low mass dark matter clumps that would be occupied by galaxies in Virgo, do not seem to have been capable of forming galaxies in the Local Group. So why are the two environments so different? A follow-up study with higher-resolution simulations by the NGVS survey team will explore how galaxies are spatially distributed throughout the cluster, to seek more clues to the mystery of dwarf galaxy formation.

    See the full article here.

    Please help promote STEM in your local schools.

    STEM Icon

    Stem Education Coalition

    The CFH observatory hosts a world-class, 3.6 meter optical/infrared telescope. The observatory is located atop the summit of Mauna Kea, a 4200 meter, dormant volcano located on the island of Hawaii. The CFH Telescope became operational in 1979. The mission of CFHT is to provide for its user community a versatile and state-of-the-art astronomical observing facility which is well matched to the scientific goals of that community and which fully exploits the potential of the Mauna Kea site.

     
  • richardmitnick 5:39 am on July 19, 2014 Permalink | Reply
    Tags: , , , CFH Telescope,   

    From CFH: “Fingerprinting the formation of giant planets” 

    CFHT icon
    Canada France Hawaii telescope

    July 17th 2014
    Media contact
    Dr. Daniel Devost
    Canada-France-Hawaii Telescope
    (808) 885-3163
    devost@cfht.hawaii.edu

    Science contacts
    Marcelo Tucci Maia
    Universidade do São Paulo
    marcelotuccimaia@usp.br

    Prof. Jorge Meléndez
    Universidade de São Paulo
    jorge.melendez@iag.usp.br

    Dr. Ivan Ramírez
    University of Texas
    ivan@astro.as.utexas.edu

    A team of Brazilian and American astronomers used CFHT observations of the system 16 Cygni to discover evidence of how giant planets like Jupiter form.

    Canada-France-Hawaii Telescope
    CFH

    16 cygni

    One of the main models to form giant planets is called “core accretion”. In this scenario, a rocky core forms first by aggregation of solid particles until it reaches a few Earth masses when it becomes massive enough to accrete a gaseous envelope. For the first time, astronomers have detected evidence of this rocky core, the first step in the formation of a giant planet like our own Jupiter.

    chart
    Difference in chemical composition between the stars 16 Cyg A and 16 Cyg B, versus the condensation temperature of the elements in the proto-planetary nebula. If the stars had identical chemical compositions then the difference (A-B) would be zero. The star 16 Cyg A is richer in all elements relative to star 16 Cyg B. In other words, star 16 Cyg B, the host star of a giant planet, is deficient in all chemical elements, especially in the refractory elements (those with high condensation temperatures and that form dust grains more easily), suggesting evidence of a rocky core in the giant planet 16 Cyg Bb. Credits: M. Tucci Maia, J. Meléndez, I. Ramírez.

    The astronomers used the Canada-France-Hawaii Telescope (CFHT) to analyze the starlight of the binary stars 16 Cygni A and 16 Cygni B. The system is a perfect laboratory to study the formation of giant planets because the stars were born together and are therefore very similar, and both resemble the Sun. However, observations during the last decades show that only one of the two stars, 16 Cygni B, hosts a giant planet which is about 2.4 times as massive as Jupiter. By decomposing the light from the two stars into their basic components and looking at the difference between the two stars, the astronomers were able to detect signatures left from the planet formation process on 16 Cygni B.

    The fingerprints detected by the astronomers are twofold. First, they found that the star 16 Cygni A is enhanced in all chemical elements relative to 16 Cygni B. This means that 16 Cygni B, the star that hosts a giant planet, is metal deficient. As both stars were born from the same natal cloud, they should have exactly the same chemical composition. However, planets and stars form at about the same time, hence the metals that are missing in 16 Cygni B (relative to 16 Cygni A) were probably removed from its protoplanetary disk to form its giant planet, so that the remaining material that was falling into 16 Cygni B in the final phases of its formation was deficient in those metals.

    The second fingerprint is that on top of an overall deficiency of all analyzed elements in 16 Cygni B, this star has a systematic deficiency in the refractory elements such as iron, aluminum, nickel, magnesium, scandium, and silicon. This is a remarkable discovery because the rocky core of a giant planet is expected to be rich in refractory elements. The formation of the rocky core seems to rob refractory material from the proto-planetary disk, so that the star 16 Cygni B ended up with a lower amount of refractories. This deficiency in the refractory elements can be explained by the formation of a rocky core with a mass of about 1.5 – 6 Earth masses, which is similar to the estimate of Jupiter’s core.

    “Our results show that the formation of giant planets, as well as terrestrial planets like our own Earth, leaves subtle signatures in stellar atmospheres”, says Marcelo Tucci Maia (Universidade de São Paulo), the lead author of the paper. “It is fascinating that our differential technique can measure these subtle differences in chemical abundances; we achieve a precision that was unthinkable until now”, adds team member Jorge Meléndez (Universidade de São Paulo). Ivan Ramírez (University of Texas) concludes: “16 Cyg is a remarkable system, but certainly not unique. It is special because it is nearby; however, there are many other binary stars with twin components on which this experiment could be performed. This could help us find planet-host stars in binaries in a much more straightforward manner compared to all other planet-finding techniques we have available today.”

    The team is composed of the PhD student Marcelo Tucci Maia, Prof. Dr. Jorge Meléndez (Universidade de São Paulo) and Dr. Iván Ramírez (University of Texas at Austin). This research will appear in the paper High precision abundances in the 16 Cyg binary system: a signature of the rocky core in the giant planet, by M. Tucci Maia, J. Meléndez and I. Ramírez, in the Astrophysical Journal Letters.

    The CFH observatory hosts a world-class, 3.6 meter optical/infrared telescope. The observatory is located atop the summit of Mauna Kea, a 4200 meter, dormant volcano located on the island of Hawaii. The CFH Telescope became operational in 1979. The mission of CFHT is to provide for its user community a versatile and state-of-the-art astronomical observing facility which is well matched to the scientific goals of that community and which fully exploits the potential of the Mauna Kea site.


    ScienceSprings is powered by MAINGEAR computers

     
  • richardmitnick 5:09 am on March 30, 2014 Permalink | Reply
    Tags: , , , CFH Telescope, ,   

    From NASA: “Stephan’s Quintet Plus One” A Real Beauty 

    NASA

    The first identified compact galaxy group, Stephan’s Quintet is featured in this remarkable image constructed with data drawn from Hubble Legacy Archive and the Subaru Telescope on the summit of Mauna Kea. The galaxies of the quintet are gathered near the center of the field, but really only four of the five are locked in a cosmic dance of repeated close encounters taking place some 300 million light-years away. The odd man out is easy to spot, though. The interacting galaxies, NGC 7319, 7318A and 7318B, and 7317 have a more dominant yellowish cast. They also tend to have distorted loops and tails, grown under the influence of disruptive gravitational [galactic] tides. The mostly bluish galaxy, NGC 7320, is in the foreground about 40 million light-years distant, and isn’t part of the interacting group. Still, captured in this field above and to the left of Stephan’s Quintet is another galaxy, NGC 7320C, that is also 300 million light-years distant. Of course, including it would bring the four interacting galaxies back up to quintet status. Stephan’s Quintet lies within the boundaries of the high flying constellation Pegasus. At the estimated distance of the quintet’s interacting galaxies, this field of view spans over 500,000 light-years.

    sq
    Image Credits Optical: Subaru October 26, 2011
    Image Credits: X-ray: NASA/CXC/CfA/E. O’Sullivan Optical: Canada-France-Hawaii-Telescope/Coelum
    15 February 2006

    From Spitzer
    sq2
    Date 2006-03-02
    Credit NASA/JPL-Caltech/Max-Planck Institute/P. Appleton (Spitzer Science Center/Caltech)
    Observers
    Spitzer data: P. Appleton (SSC/Caltech) K. Xu (SSC/Caltech) W. Reach (SSC/Caltech) M. Dopita (Australian National University) Y. Gao (Purple Mountain Observatory, China) N. Lu (SSC/Caltech) C. Popescu (Max Planck Institut fuer Kernphysik, Heidelberg, Germany) J. Sulentic (University of Alabama) R. Tuffs (Max Planck Institut fuer Kernphysik, Heidelberg, Germany) M. Yun (University of Massachusetts)

    region
    The galaxies in the vicinity of Stephan’s Quintet. The rectangle indicates the area covered by the 1998–99 Hubble Space Telescope image.

    NASA Spitzer Telescope
    NASA/Spitzer

    NAOJ Subaru Telescope
    NAOJ/Subaru

    NASA Chandra Telescope
    NASA/Chandra

    Canada-France-Hawaii Telescope
    Canada-France-Hawaii Telescope

    See the full article here.

    The National Aeronautics and Space Administration (NASA) is the agency of the United States government that is responsible for the nation’s civilian space program and for aeronautics and aerospace research.

    President Dwight D. Eisenhower established the National Aeronautics and Space Administration (NASA) in 1958 with a distinctly civilian (rather than military) orientation encouraging peaceful applications in space science. The National Aeronautics and Space Act was passed on July 29, 1958, disestablishing NASA’s predecessor, the National Advisory Committee for Aeronautics (NACA). The new agency became operational on October 1, 1958.

    Since that time, most U.S. space exploration efforts have been led by NASA, including the Apollo moon-landing missions, the Skylab space station, and later the Space Shuttle. Currently, NASA is supporting the International Space Station and is overseeing the development of the Orion Multi-Purpose Crew Vehicle and Commercial Crew vehicles. The agency is also responsible for the Launch Services Program (LSP) which provides oversight of launch operations and countdown management for unmanned NASA launches. Most recently, NASA announced a new Space Launch System that it said would take the agency’s astronauts farther into space than ever before and lay the cornerstone for future human space exploration efforts by the U.S.

    NASA science is focused on better understanding Earth through the Earth Observing System, advancing heliophysics through the efforts of the Science Mission Directorate’s Heliophysics Research Program, exploring bodies throughout the Solar System with advanced robotic missions such as New Horizons, and researching astrophysics topics, such as the Big Bang, through the Great Observatories [Hubble,
    Chandra, Spitzer ]and associated programs. NASA shares data with various national and international organizations such as from the Greenhouse Gases Observing Satellite.


    ScienceSprings is powered by MAINGEAR computers

     
c
Compose new post
j
Next post/Next comment
k
Previous post/Previous comment
r
Reply
e
Edit
o
Show/Hide comments
t
Go to top
l
Go to login
h
Show/Hide help
shift + esc
Cancel
Follow

Get every new post delivered to your Inbox.

Join 462 other followers

%d bloggers like this: