Telescope Projects at Steward Observatory Work in Progress Astronomical Society of New York Union College Saturday, 24 October 2009 Peter Wehinger Steward.

Slides:

Advertisements

Similar presentations

Chapter 6: Telescopes – Portals of Discovery. Visible light is only one type of electromagnetic radiation emitted by stars Each type of EM radiation travels.

Advertisements

Light and Telescopes Please pick up your assigned transmitter

Debris Disk Science with GMT Inseok Song, University of Georgia for “Opening New Frontiers with the Giant Magellan Telescope” in Oct 2010 Zodiacal light:

Laser Launch System for the LBT Richard Davies Sebastian Rabien Max Planck Institute for Extraterrestrial Physics  Approaches of other observatories 

Light and Telescopes Chapter 5. Traditional Telescopes The 4-m Mayall Telescope at Kitt Peak National Observatory (Arizona)

Imaging Science Fundamentals Chester F. Carlson Center for Imaging Science Astronomical Imaging Telescopes and Detectors.

Aug-Nov, 2008 IAG/USP (Keith Taylor) ‏ Instrumentation Concepts Ground-based Optical Telescopes Keith Taylor (IAG/USP) Aug-Nov, 2008 Aug-Sep, 2008 IAG-USP.

Astronomical Research at TAMU Faculty Future facilities and projects.

Current Status of Lulin Observatory Hung-Chin Lin Taiwan.

The SOAR Telescope MSU’s Laboratory for Astronomical Discovery.

A Few Ways of Acquiring Telescope Time Telescope Committee Astronomical Society of New York October 23, 2009 Peter Wehinger Steward Observatory University.

Extremely Large Telescopes and the Epoch of Reionization Xiaohui Fan(Arizona) with help from Pat McCarthy and GMT Science Working Group July 11, 2008,

January 24, 2006Astronomy Chapter 5 Astronomical Instruments How do we learn about objects too far away for spacecraft? How do telescopes work? Do.

An Introduction to Adaptive Optics Mike Hein PH 464 – Applied Optics Winter 2005.

Mexican Sites: San Pedro Martir Vladimir Vassiliev Alberto Carramiñana Rene Ong.

Modern Telescopes and Ancient Skies New Views of the Universe An IU Lifelong Learning Class Tuesdays, May 10, 17, 24 III. 30-meters and beyond.

1 The Thirty-Meter Telescope (TMT) Richard Ellis, Steele Professor and California Institute of Technology TMT Board member Michael Bolte, Director, University.

Observational Astronomy. Astronomy Primary Goal: Understanding the nature of the universe and its constituents Means: Equipment building, research, teaching.

Studying space from Earth Tele = distance Scopos = to watch Light and radiation How astronomers gather info about space.

Light and Telescopes Chapter 6. Previous chapters have described the sky as it appears to our unaided eyes, but modern astronomers turn powerful telescopes.

The KPNO 4m “Mayall” Telescope Arjun Dey (NOAO). National Optical Astronomy Observatory Mission: provide the best ground-based astronomical capabilities.

The Giant Magellan Telescope AAS San Diego January 11, 2005 Matt Johns.

Adaptive Optics in the VLT and ELT era

H205 Cosmic Origins  Telescopes (Ch. 6)  Visit Kirkwood Obs  Time for Reflection  Hand in EP1 APOD.

Page 1 AO in AO A daptive O ptics in A stronomical O bservations Diana R. Constantin ASTRONOMICAL INSTITUTE OF THE ROMANIAN ACADEMY.

4. Telescopes Light gathering power and resolution Optical and radio telescopes Limitations of Earth’s atmosphere and satellite missions. Instruments (prism.

Telescopes. Act as “electromagnetic radiation catchers” Capture as much as possible Focus Magnifies images Telescopes that “catch” visible light are called.

How do we study the Universe?. SPECTROSCOPY Uses visible wavelength split into colors.

A visible-light AO system for the 4.2 m SOAR telescope A. Tokovinin, B. Gregory, H. E. Schwarz, V. Terebizh, S. Thomas.

Announcements No lab this week due to observing night last night There will be a lab after class next week. If the skies are clear expect to stay out until.

{ Telescopes Jon Holtzman NMSU Astronomy.  Telescopes are light buckets: bigger buckets collect more light, and faint (far away) objects don’t produce.

Telescope Technologies

2013 Survey Science Group Workshop, Feb High-1 Resort.

1 The LOFT group Who we are Where we came from Where we are going Large Optics Fabrication and Testing ?

Chile Sky Background at ESO/la Silla in the Visible and Near IR Leonardo Vanzi -Olivier R. Hainaut European Southern Observatory La Silla - Chile.

Viewing the Universe through distorted lenses: Adaptive optics in astronomy Steven Beckwith Space Telescope Science Institute & JHU.

Early scientific goals for the MMT’s multi-laser-guided adaptive optics Michael Lloyd-Hart, Thomas Stalcup, Christoph Baranec, N. Mark Milton, Matt Rademacher,

Telescopes Portals of Discovery. Telescope A telescope is an instrument designed to aid the observation of remote objects by collecting some form of electromagnetic.

6.3 Telescopes and the Atmosphere 6.4 Eyes and Cameras: Everyday Light Sensors Our goals for learning How does Earth’s atmosphere affect ground-based observations?

Light, Mirrors and Telescopes Rajesh Gupta University of California, San Diego. Mr. Smith’s Class.

Telescopes continued… Why is bigger better? Two reasons…

Chinese- international collaboration solved the central question: ”How common are planets like the Earth”

The Taiwanese-American Occultation Survey (TAOS) Matthew Lehner ASIAA.

Telescopes. Light Hitting a Telescope Mirror huge mirror near a star * * * small mirror far from 2 stars In the second case (reality), light rays from.

A105 Stars and Galaxies  News Quiz Today  1 st NovaSearch homework due Thursday  First Exam on Thursday, Sept. 28 Today’s APODAPOD.

The Large Synoptic Survey Telescope: The power of wide-field imaging Michael Strauss, Princeton University.

LSST and Dark Energy Dark Energy - STScI May 7, 2008 Tony Tyson, UC Davis Outline: 1.LSST Project 2.Dark Energy Measurements 3.Controlling Systematic Errors.

Adaptive Optics for Astronomy Kathy Cooksey. AO Basics Photons –Travel in straight lines Wavefront –Line perpendicular to all photons’ paths Atmospheric.

Light, Optics and Telescopes The Electromagnetic Spectrum.

Telescopes Lecture. Standards Understand how knowledge about the universe comes from evidence collected from advanced technology (e.g., telescopes, satellites,

The Large Synoptic Survey Telescope and Precision Studies of Cosmology David L. Burke SLAC C2CR07 Granlibakken, California February 26, 2007 Brookhaven.

Page 1 Adaptive Optics in the VLT and ELT era basics of AO Neptune François Wildi Observatoire de Genève Credit for most slides : Claire Max (UC Santa.

Opening New Frontiers with the GMT, Seoul, October Giant Magellan Telescope How does an adaptive secondary mirror support the unique qualities of.

ISP Astronomy Gary D. Westfall1Lecture 7 Telescopes Galileo first used a telescope to observe the sky in 1610 The main function of a telescope is.

Giant Magellan Telescope Project Status and Relationship with the NSF Astronomy and Astrophysics Advisory Committee February 8, 2007 Patrick McCarthy -

The Very Large Array (VLA) in New Mexico. Observations at wavelengths other than visible light are revealing previously invisible sights Visible light.

Light, Optics and Telescopes The Electromagnetic Spectrum.

Page 1 Adaptive Optics in the VLT and ELT era François Wildi Observatoire de Genève Credit for most slides : Claire Max (UC Santa Cruz) Basics of AO.

Gina Moraila University of Arizona April 21, 2012.

A Tour of the Largest Ground-Based Telescopes Being Developed

The GMT Project The Giant Magellan Telescope (GMT)

DIRECT DETECTION OF GRAVITATIONAL WAVES FROM NEUTRON STARS

6.3 Telescopes and the Atmosphere

The Giant Magellan Telescope

Modern Observational/Instrumentation Techniques Astronomy 500

Telescopes Lecture.

Review When is Orion visible in Arizona?

The Richard F. Caris Mirror Lab

How Stars are Seen… Astronomy - Ch.20.

Presentation transcript:

Telescope Projects at Steward Observatory Work in Progress Astronomical Society of New York Union College Saturday, 24 October 2009 Peter Wehinger Steward Observatory University of Arizona

Casting a 6.5-m Mirror for San Pedro Martir Steward Observatory Mirror Lab A World Class Site: San Pedro Martir Baja California, Mexico Peter Wehinger

Hexagonal Columns of Al 2 SiO 5 Honeycomb Structure Light-weight Spun-cast Mirrors

Casting in Progress – 26 Aug 2009 SPM 6.5-m Mirror The Principals UNAM INAOE UC Berkeley UC Santa Cruz U Arizona

San Pedro Martir A World Class Site Peter Wehinger Steward Observatory SOML Casting Event – 6.5-m Mirror 26 August 2009

SPM Tucson Ensenada San Diego ~ 600 km Baja California and the Sonoran Desert 380 km

SPM Obs Pico del Diablo Meling Ranch Airfield Road to San Pedro Martir 60 km 40 km

Climatic & Seeing Conditions Clear Sky Statistics Photometric ~ 63% (Tapia et al) Satellite Imaging~ 73% (Erasmus et al.) Spectroscopic ~ 81% (Tapia et al.) Seeing Statistics Median Seeing ~ 0.48 arc sec Mean Seeing ~ 0.57 arc sec (FWHM) 25 th Percentile ~ 0.37 arc sec

LBT Kitt Peak Lick Palomar MMT Lowell NIGHT SKY IN THE DESERT SPM Sky brightness B ~ 22.3 mag/sec 2 PHX LA TUC HER N San Pedro Martir

Ensenada Yuma San Felipe San Diego Tijuana SPM Sky Brightness at San Pedro Martir Darker than B ~ 22.3 mag/sec km N

Night Sky Spectrum on San Pedro Martir Intensity (erg/s/cm 2 /A)  (A)

Remarks about SPM Night Sky Integrated Light of Night Airglow Green Line [OI] 5577 visible to ~10-15 deg above horizon Arcturus – steady, no scintillation (twinkling) Naked-eye limit at least ~ 7th magnitude of brightest galaxies in Virgo Cluster - visible SPM has darkest night sky – Compared with other sites Arizona, Chile, Hawaii, Himalayas

Possible Air Field at Vallecitos ~ 5-6 km from telescopes 2425 m 2434 m 2 km

LBT LARGE BINOCULAR TELESCOPE Site: Mt Graham, Arizona Two 8.4-m f/1.1 Mirrors

Steward Observatory Mirror Lab Casting Bay 6.5-m 8.4-m

LBT Edge-to-Edge ~ 22.4 m, Equivalent Circular Aperture ~ 11.8 m 30 m

NGC 6946 with 8.2-m Subaru

NGC 6946 with 8.4-m LBT

GMT GIANT MAGELLAN TELESCOPE Site: Las Campanas, Chile

GMT seven 8.4-m Mirrors 21.5-m Circular Aperture 25.5-m Edge to Edge Graphics by Todd Mason

GMT Partners as of Oct Carnegie Institution of Washington University of Texas at Austin Texas A & M University University of Arizona Australian National University Astronomy Australia Ltd. Harvard University Smithsonian Institution Korea Astronomy & Space Institute others considering joining

Mirror Lab Founder, Roger Angel inspects 8.4-m mirror for GMT

GMT-1– polishing at ~ ± 0.5  Oct 2009 Final figure will be ±10-20 nm, 400x smoother

When GMT is completed in ~ years What will be found…? Remember Hale & Wickliffe Rose Again there will be many surprises..!

Three Planets b, c, & d Imaged around Star HR 8799 Light from central star is suppressed Discovery Announced 14 Nov 2008 Gemini 8.2 m

Phil Hinz et al. Steward Observatory

LSST LARGE SYNOPTIC SURVEY TELESCOPE Site: Cerro Pachon, Chile

Founding Partners (2003) University of Arizona Research Corporation University of Washington NOAO + 18 other institutions (as of 2008)

Large Synoptic Survey Telescope

LSST Optical Layout 8.36 m 6.28m 4.96 m 3.4 m 64 cm Primary f/1.25 Secondary Tertiary f/0.8 Focal Plane Design: L. Seppala, LLNL Filters Field Flattener

Large Synoptic Survey Telescope Project Overview & Goals 10-sec exposures ~ 24 mag. 3.5 Gpix/image – 10 sq. deg Terabytes per night Entire sky surveyed in 4 nights Search for Near-Earth Objects Survey the Kuiper Belt Probe dark matter Many Surprises Serendipitous Discoveries 64 cm

LSST 8.4-m Primary Mirror 22 October 2008 Lifting off oven floor Weight ~ 52 tons Glass ~ 26 tons

LSST 8.4-m Primary Mirror 22 October 2008 During move from oven to holding ring Weight ~ 103,000 lbs Glass ~ 52,000 lbs

Ground-Layer Adaptive Optics Recent Results on MMT

Planet found around the Nearby star  Pictoris ESO 8.1-m Telescope

The MMT multi-laser GLAO system Laser type2 x doubled YAG (15 W each) Wavelength532 nm Pulse rep rate5.2 kHz Average power30 W Launch locationBehind secondary mirror Number of beacons5, arranged like a pentagon Enclosed field of view2 arc minutes Beacon typeRayleigh scattering Range gate20-29 km, dynamic refocusing

MMT results: M3 Open loop, K s filter, seeing 0.70” Logarithmic scale 110”

MMT results: M3 Closed loop GLAO, K s filter, seeing 0.30” Logarithmic scale 110”

NGC 2770 – First Light Binocular Image with LBT 11 Jan 2007 Supernova Gamma-Ray Burst

Magellan m Telescope (Baade) Las Campanas Observatory VLT UT1 8-m Telescope & FORS 1: ESO Paul Groot, Harvard-Smithsonian Center for Astrophysics Jerome Orosz, University of Utrecht 11 Optical Images of X-ray Nova XTE J