Modern Observational/Instrumentation Techniques Astronomy 500

Slides:



Advertisements
Similar presentations
NIR INSTRUMENT FOR GLAO Takashi Hattori, Iwata Ikuru (Subaru Telescope)
Advertisements

1 Astronomical Observational Techniques and Instrumentation RIT Course Number Professor Don Figer Telescopes.
Optical Astronomy Imaging Chain: Telescopes & CCDs.
Optics and Telescopes Chapter Six.
Astronomy for beginners Telescopes By Aashman Vyas.
Announcements No lab tonight due to Dark Sky Observing Night last night Homework: Chapter 6 # 1, 2, 3, 4, 5 & 6 First Quarter Observing Night next Wednesday.
VLBI: Visible Light Broadband Imager Instrument Conceptual Design Presentation Tom Berger Lockheed Martin Solar and Astrophysics Lab.
ENERGY a proposal for a Multi-channel Cmos Camera F. Pedichini, A. Di Paola, R. Speziali INAF Oss. Astr. Roma h e-
Astronomical Spectroscopy
Your Observing Challenge: White Dwarfs in Open Star Clusters.
Unit 1 Physics Detailed Study 3.1 Chapter 10: Astronomy.
Science Specification of SOLAR-C payload SOLAR-C Working Group 2012 July 23.
Telescope Notes 1. Objectives To know the general types of telescopes and the advantages and disadvantages of each one. To know the primary parts and.
OPTICAL TELESCOPES Optical telescopes gather the visible light to observe distant objects. There are Three Basic Types of Optical Telescopes A.Refracting.

Photography. View Camera 8 x 10 4 x 5 Camera is usually referred to by the size of film.
STATUS REPORT OF FPC SPICA Task Force Meeting March 29, 2010 MATSUMOTO, Toshio (SNU)
Telescopes & recent observational techniques ASTR 3010 Lecture 4 Chapters 3 & 6.
© 2004 Pearson Education Inc., publishing as Addison-Wesley Telescopes.
15 October Observational Astronomy Direct imaging Photometry Kitchin pp ,
Astronomy 1020-H Stellar Astronomy Spring_2015 Day-21.
Telescopes: Portals of Discovery
NORDFORSK Summer School, La Palma, June-July 2006 NOT: Telescope and Instrumentation Michal I. Andersen & Heidi Korhonen Astrophysikalisches Institut Potsdam.
Telescopes come in three basic styles. Refracting telescopes use lenses Refractors are either achromatic (some color distortion) or apochromatic (very.
Reflecting Telescopes. Mirrors A flat mirror reflects light in straight lines. A curved mirror can focus light to a point. A perfect parabolic mirror.
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.
Dirk Soltau Kiepenheuer-Institut für Sonnenphysik Synoptic Network Workshop, Boulder Some General Considerations on Wide Field Telescopes.
Telescopes Chapter 3. Objectives To know the general types of telescopes and the advantages and disadvantages of each one. To know the primary parts and.
Charge-Coupled Devices Astrophysics Lesson 5. Learning Objectives Describe and explain the structure and operation of the charge coupled device State.
NIC3 FOM Dithered Observations of the Orion Nebula Eddie Bergeron, STScI.
Telescope Desiderata. Various Goals Imagery / surveys - discovery, census – Consider scales, POSS vs HST, etc Astrometry / motions / distances Photometry.
Astronomical Spectroscopic Techniques. Contents 1.Optics (1): Stops, Pupils, Field Optics and Cameras 2.Basic Electromagnetics –Math –Maxwell's equations.
 From the ground the atmosphere distorts images.  Light pollution from streetlights, city lights, car lights, and more hinders the seeing conditions.
Telescopes Overview MAS April 20, 2017.
VERTICAL SCANNING INTERFEROMETRY VSI
Telescopes come in three basic styles
Astronomical Spectroscopic Techniques
“Whether they ever find life there or not, I think Jupiter should be considered an enemy planet.” Jack Handy HW2 is due on Wednesday. How’s that going?
Astronomy 04 The Solar System
Telescopes.
Telescopes Chapter 3 Objectives To know the general types of telescopes and the advantages and disadvantages of each one. To know the primary parts.
Telescopes.
Dioptrics, catoptrics, and more!
The Aperture acts like an iris
Telescopes.
Astronomy 920 Commissioning of the Prime Focus Imaging Spectrograph
Introduction to Spectroscopy
Observational Astronomy
C2PU TELESCOPES Version 02, 28/08/2016 Jean-Pierre Rivet CNRS, OCA,
Lecture 2: Basic Astronomical Optics
Modern Observational/Instrumentation Techniques Astronomy 500
Optical Design For a 32 Inch, All-Spherical Relay Cassegrain Telescope
4. Telescopes Light gathering power and resolution
OPTICAL TELESCOPES Optical telescopes gather the visible light to observe distant objects. There are Three Basic Types of Optical Telescopes Refracting.
Announcements Lab tonight: planetarium
LSST Photometric Calibration
Modern Observational/Instrumentation Techniques Astronomy 500
C2PU TELESCOPES Version 02, 28/08/2016 Jean-Pierre Rivet CNRS, OCA,
Optics and Telescopes Chapter Six.
Astronomical Observational Techniques and Instrumentation
Modern Observational/Instrumentation Techniques Astronomy 500
Modern Observational/Instrumentation Techniques Astronomy 500
Telescopes Chapter 3.
Modern Observational/Instrumentation Techniques Astronomy 500
Modern Observational/Instrumentation Techniques Astronomy 500
Modern Observational/Instrumentation Techniques Astronomy 500
Observational Astronomy
Optics Alan Title, HMI-LMSAL Lead,
Telescopes come in three basic styles
Presentation transcript:

Modern Observational/Instrumentation Techniques Astronomy 500 Andy Sheinis, Sterling 5520,2-0492 sheinis@astro.wisc.edu MW 2:30, 6515 Sterling Office Hours: Tu 11-12

Hardware

Telescopes What parameters define telescopes? Spectral range Area Throughput FOV Image Quality Plate scale/Magnification Pointing/tracking

Telescopes Examples of telescopes? Refracting Galilean (1610) Keplerian (1611, 1834) Astronomical Terrestrial Reflecting (4x harder to make!) Newtonian Gregorian (1663) Cassegrain (1668) Ritchey-Cretien (1672) Catadioptric Schmidt (1931) Maksutov (1944)

Some Everyday Concepts (1) Specular and Diffuse Reflection Refraction Specular Diffuse Retro

Some Everyday Concepts (2) Imaging Object Image Object Image Rays Wavefronts The Observer The Observer

High-School Optics F’ Image Object F

Imaging Cameras Imagers can be put at almost any focus, but most commonly they are put at prime focus or at cassegrain.

The scale of a focus is given by S=206265/(D x f#) (arcsec/mm) Examples: 3m @f/5 (prime) 13.8 arcsec/mm (0.33”/24µpixel) 1m @f/3 (prime) 68.7 arcsec/mm (1.56”/24µpixel) 1m @f/17 (cass) 12.1 arcsec/mm (0.29”/24µpixel) 10m @f/1.5 (prime) 11.5 arcsec/mm (0.27”/24µpixel) 10m @f/15 (cass) 1.15 arcsec/mm (0.03”/24µpixel) Classical cassegrain (parabolic primary + convex hyperbolic in front of prime focus) has significant coma.

For a classical cassegrain focus or prime focus with a parabolic primary you need a corrector. The Richey-Chretien design has a hyperbolic primary and secondary designed to balance out coma and astigmatism in the focal plane.

Direct Camera design/considerations LN2 can Dewar CCD dewar window Preamp Shielded cable to controller baffles shutter Filter wheel Field corrector/ADC Primary mirror

Shutters The standard for many years has been multi-leaf iris shutters. As detectors got bigger and bigger, the finite opening time and non-uniform illumination pattern started to cause problems. 2k x 2k 24µ CCD is 2.8 inches along a diagonal. Typical iris shutter - 50 milliseconds to open. Center of a 1s exposure is exposed 10% longer than the corners.

Shutter vignetting pattern produced by dividing a 1 second exposure by a 30 second exposure.

Double-slide system The solution for mosaic imagers and large-format CCD has been to go to a 35mm camera style double-slide system.

Filter Wheel Where do you put the filter? There is a trade off between filter size and how well focused dust and filter imperfections are.

Drift Scanning An interesting option for imaging is to park the telescope (or drive it at a non-sidereal rate) and let the sky drift by. Clock out the CCD at the rate the sky goes by and the accumulating charge ``follows’’ the star image along the CCD.

Drift Scanning End up with a long strip image of the sky with a `height’ = the CCD width and a length set by how long you let the drift run (or by how big your disk storage is). The sky goes by at 15 arcseconds/second at the celestial equator and slower than this by a factor of 1/cos(d) as you move to the poles. So, at the equator, PFCam, with 2048 x 0.3” pixels you get an integration time per object of about 40 seconds.

Drift Scanning What is the point? Problem: Superb flat-fielding (measure objects on many pixels and average out QE variations) Very efficient (don’t have CCD readout, telescope setting) Problem: Only at the equator do objects move in straight lines, as you move toward the poles, the motion of stars is in an arc centered on the poles. Sloan digital survey is a good example Zaritsky Great Circle Camera is another

Direct Imaging Filter systems Photometry Point sources Aperture PSF fitting Extended sources (surface photometry) Star-galaxy separation

Filter Systems There are a bunch of filter systems Broad-band (~1000Å wide) Narrow-band (~10Å wide) Some were developed to address particular astrophysical problems, some are less sensible.

1.1µ silicon bandgap 3100Å is the UV atmospheric cutoff

Filter Choice: Example Suppose you want to measure the effective temperature of the main-sequence turnoff in a globular cluster. color relative time to reach dTeff=100 B-V 4.2 V-R 11.5 B-I 1.0 B-R 1,7

Narrow-band Filters Almost always interference filters and the bandpass is affected by temperature and beam speed: DCWL = 1Å/5˚C DCWL = 17Å; f/13 f/2.8