004 Jan15 ITS Paul Boltwood

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Information about 004 Jan15 ITS Paul Boltwood

Published on January 10, 2008

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Slide1:  TECHNIQUES FOR IMAGING VERY FAINT OBJECTS NO MAGIC, JUST DO EVERYTHING RIGHT (or at least try to!) by Paul Boltwood ITS November 8, 2002 Salem Oregon This talk is on the conference CDR Copyright (C) 1996-2002 Paul Boltwood Slightly updated January 15, 2006 SKY & TELESCOPE DEEP FIELD CONTEST:  SKY & TELESCOPE DEEP FIELD CONTEST one of the reasons I was invited here was that I won this contest with an image that reached mag. 24.1 see Bradley Schaefer’s articles S&T May 1998 and May 1999 I should not have won because I had: suburban skies a CCD with 40% peak quantum efficiency 16" aperture done a crude reduction many amateurs surpass me in all of these departments as soon as I heard that I won, I re-reduced the image carefully and reached mag. 24.5 – but too late for S&T in this talk I will tell you how I did this PHILOSOPHY BEHIND THE TECHNIQUES:  PHILOSOPHY BEHIND THE TECHNIQUES when I started in 1989, I wanted to do some publishable science and I ended up doing photometry of blazars, ~100,000 images having my data accepted by scientists was my motivating force and my strategy was: “try to do everything right” most professionals in North America assume that an amateur is incompetent until proven otherwise when I design something, I try to learn the theory behind my equipment & techniques and be very thorough WHY IS SO MUCH HOMEMADE?:  WHY IS SO MUCH HOMEMADE? during this talk you will see that most of my equipment and software is homemade. Everything in this talk that does not have a brand name, I have designed, and either built or had built. I like designing and building this stuff, and I know how to do it I started before much of today’s equipment was available to keep costs down, I used my labour rather than money for the scientific work especially, I needed to know that everything works properly and in a known way. Equipment manufactured for amateurs is deficient in this regard: optical performance data is not available, esp. non-visual software source code is not available mechanical performance is usually inadequate database handling is not provided wrong approach taken for scientific work WHY DO I HAVE AN OBSERVATORY?:  WHY DO I HAVE AN OBSERVATORY? allows use of superior, non-portable, equipment avoids losing alignment and collimation has electrical power observing in the Frozen North near Ottawa, Canada makes an insulated heated equipment room especially desirable: makes long exposures feasible allows use of long winter nights even at -35°C protects computers and electronics stores books and accessories allows money earning activities while waiting for exposures BOLTWOOD OBSERVATORY (1):  BOLTWOOD OBSERVATORY (1) In The Far Backyard At Home BOLTWOOD OBSERVATORY (2):  BOLTWOOD OBSERVATORY (2) Roof Rolled Off To The South BOLTWOOD OBSERVATORY (3):  BOLTWOOD OBSERVATORY (3) Telescope Room, Old Homemade Camera BOLTWOOD OBSERVATORY (4):  BOLTWOOD OBSERVATORY (4) Telescope Room, AP7p Camera telescope room is cool in the sun because double skinned and ventilated, including between skins. Thermal design by Rob Dick biggest fault is no dome. Cannot observe if windy walls are black because original use was visual with a refractor. Roll-off roof ceiling is white to provide light while working on equipment convenient access more important than dark skies for my work so I located at home MOUNT:  MOUNT Byers Series 2 (sort of), with modifications: backlash removal stiffened DEC drive (15* better than Byers) stiffened mounting plate overloaded with 180 lb optical tube assembly tracking error in 2 minute exposure is imperceptible periodic error correction not used or needed no guiding either stepping motors limited to 15 times siderial rate OPTICAL TUBE ASSEMBLY (1):  OPTICAL TUBE ASSEMBLY (1) focus flap motors, no longer used rotating secondary, 4 ports eyepiece focuser S.S. angle stiffeners epoxied on 11*80 finder square wooden tube: allows home carpentry supports extensive baffling corners allow tube currents to escape away from light path easy to mount items on corner spaces are useful allowed a demountable primary cell OPTICAL TUBE ASSEMBLY (2):  OPTICAL TUBE ASSEMBLY (2) Primary Cell – Designed And Built By Max Stuart collimation adj. using a rod end OPTICAL TUBE ASSEMBLY (3):  OPTICAL TUBE ASSEMBLY (3) Primary Mirror Support holes for rod ends OPTICAL TUBE ASSEMBLY (4):  OPTICAL TUBE ASSEMBLY (4) Spider Assembly And Baffling BAFFLING:  BAFFLING no non-imaging light should get to the focal plane or intermediate optical surfaces optics often have light-scattering dust on them baffles at right angles to the light are the primary defence. Black paint is a secondary defence unbaffled focusers, extension tubes, cameras are major sources of flare you should be able to work near the moon as long as it is not actually shining on your primary you should be able to turn on the observatory lights with little impact while CCD observing OPTICS:  OPTICS 16" f/4.7 primary on Astro Sitall zero expansion substrate by Peter Ceravolo 2 times better than diffraction limit zero expansion substrate replaced a previous pyrex primary for a several times reduction in focus drift 3.1" Newtonian secondary by Galaxy, RMS .016 wave Televue 2" Big Barlow normally used Televue Paracorr used for wide field Televue 5X Powermate intended for narrow field but not fully tested UBVRI filters for photometry by Omega, RGB filters for astrophotography by Custom Scientific OPTICS PROBLEMS:  OPTICS PROBLEMS amateur optics don't cover CCD spectral extremes refractive optics suffer from chromatic aberrations, and filters may pass unexpected UV or IR. Do not use photographic filters wish I had a Ritchey-Chretien Cassegrain matched to camera before buying your 4096*4096 CCD, check your optical aberrations in the corners, and alignment and focus capability. This stuff is hard enough at 512*512 before using multicoated optics, check what happens at the spectral extremes design such that all optical surfaces are far from focus. Then dust will not affect your flat fields very much black anodizing is clear in the near IR, so paint it I use Krylon Ultra Flat Black spray FOCUSER & CAMERA ASSEMBLY:  FOCUSER & CAMERA ASSEMBLY anti-backlash umbilical focuser frame focus sled optics tube collet AP7p camera filter wheel fan for 3°C cooler CCD tarp on ceiling FOCUSER:  FOCUSER 5.5 inch range to allow for magnifying optics stepping motor and limit switches linear bearings the camera is always at same rotation on sky EXPLODED CAMERA ASSEMBLY:  EXPLODED CAMERA ASSEMBLY magnifiers with buttress thread baffling Collet filter wheel Apogee AP7p extra filter holder camera clamps filter disk motor FILTER WHEEL:  FILTER WHEEL 10 positions for 1" filters microstepped stepping motor wheel is carefully balanced 2 optical switches for positioning wheel: one with 1 hole, other with 10 holes switches are checked to be sure that the correct filter is in place at each move AP7p not fastened in the normal way – clamps are used AP7p penetrates into face of housing filter is very close to housing permits the use of 1" filters – 2" is normal note the baffle to correct shiny ring in the camera CCD CAMERA:  CCD CAMERA current camera Apogee AP7p with SiTe 502A chip has blue sensitivity and 80% peak quantum efficiency, more thermal noise and hot pixels, poor temperature control, 512*508 pixels old homemade camera with Thomson TH7883 chip in vacuum, liquid cooled, chip at -72°C, low thermal noise and very few hot pixels has little blue sensitivity, 40% peak quantum efficiency, excellent flatness, good temperature control, 382*574 pixels. Used for S&T Deep Field CALIBRATION FLAT FIELD LIGHT SOURCE:  CALIBRATION FLAT FIELD LIGHT SOURCE purpose is to flood telescope entrance aperture to simulate a sky background: puts diffuser across full aperture and in contact. Need exactly the same light path as for sky background diffuser needs to be evenly lit spectra to match night sky (not likely!) four 35W tungsten halogen lamps with blue-green and IR cut filters on each regulated power required inside covered with crumpled Al foil clips onto front of OTA, 40"*40"*11.5" 4% variation across diffuser - best I could do in an 11.5" thick package BOLTWOOD OBSERVATORY (5):  BOLTWOOD OBSERVATORY (5) Equipment Room ELECTRONICS (1):  ELECTRONICS (1) power and switch panel rack of microprocessor boards flat fielder power supply modular use Microchip PIC microcontrollers, one per function complex stepping motor control firmware in 4 of them all time critical functions are done in the microcontrollers almost electronics all are in equipment room to ease repairs and reduce thermal wear & tear ELECTRONICS (2):  ELECTRONICS (2) control of telescope fans & heaters, button box sound, temp. readouts RA & DEC stepping motor drives, button box filter wheel & focuser motor drives serial backplane controller with parallel port interface to PC ELECTRONICS (3):  ELECTRONICS (3) Rack Backplane For Microcontroller Boards COMPUTER AND SOFTWARE SUMMARY:  COMPUTER AND SOFTWARE SUMMARY observatory computer is a Pentium II 333 MHz, 256 MB RAM, 60 GB hard drive 17" 1600*1200 display software: Windows 2000 because it allows simultaneous star mapping, data base, observing, reduction, and non-astronomical work telescope control image data base reduction MaxIm star mapping: Guide 8.0 with A2.0 catalog to mag 20 - 526,280,881 stars and a million galaxies DSS available at house over web TELESCOPE CONTROL SOFTWARE:  TELESCOPE CONTROL SOFTWARE VB and C++ software position & exposure info. usually from “.aux” files or script uses MaxIm for camera driver, auto- focus, mount jogger, image display corrects for refraction and flexure for position and focus corrects for temperature for focus optionally runs scripts in my own language images are rotated to have north at the top immediately upon readout often not attended for 90 minutes normal exposure is 2 minutes with many frames merged in reduction DATA BASE:  DATA BASE has index to 120,000 images, all FITS with extensive headers allows semi-automatic data reduction observations are grouped by “group files” to aid reduction observing and reduction software updates data base automatically user interface package: searches data base in several ways uses MaxIm to display images allows display and editing of FITS headers (singly or in bulk) allows display and editing of “group files” VB and C++ software DATA BASE USER INTERFACE:  DATA BASE USER INTERFACE CALIBRATION FRAMES:  CALIBRATION FRAMES I do 16 frames each of bias, deferred charge and flat fields which are then averaged to reduce noise deferred charge frame was used for my old homemade TH7883 camera, not yet for AP7p: was several times more important than bias frame added to image to compensate for trapped electrons 10+ hours of 1000 sec. dark frames for each CCD temperature: calibrated and summed to form thermal frame prorated by exposure time when used – assumes good camera quality is dependant upon camera temperature regulation normal image reduction procedures are used to create master calibration frames from raw calibration frames bad pixels in master calibration frames are marked and not used in image reduction REDUCTION SOFTWARE (1):  REDUCTION SOFTWARE (1) produces master calibration, astrophoto and photometric reductions runs scripts all pixel computations are 32 bit floating point, 16 bits inadequate reduced images have a large dynamic range due to merging C++ software REDUCTION SOFTWARE (2):  REDUCTION SOFTWARE (2) automatic, driven by: "group" file listing image files and FITS headers control file giving star, sky, and exclusion zone locations merges images interpolating between pixels to correct for translation, scale, and rotation cosmic rays removed from calibration and image frames during: overscan averaging raw frame calibration frame merging bad pixels (due to many sources) are marked and avoided – merge is corrected for these missing pixels variance frames are maintained (primarily for photometry) REDUCTION PROCEDURE SUMMARY:  REDUCTION PROCEDURE SUMMARY manually delete bad images from the group file reduction software then: calibrates each raw image pixel by pixel measures each calibrated image merges calibrated images based on those measurements into buffers. Each image is multiplied by a weight that is larger for better images completes the merge optionally flatten the image to correct errors in flat field calibration optional MaxIm deconvolution and other fiddling will use S&T Deep Field image as the example in what follows CALIBRATE EACH RAW IMAGE:  CALIBRATE EACH RAW IMAGE scan lines have 32 overscan pixels beyond the real pixels average these along the line subtract overscan from each pixel to remove certain camera problems apply bias, deferred charge, thermal, and flat master calibration frames for each pixel: cal = (raw-overscan- bias+defchg- (prorated_therm))/flat bad pixels are marked and not used S&T Deep Field Raw Frame MEASURE EACH CALIBRATED IMAGE:  MEASURE EACH CALIBRATED IMAGE using pattern matching, locate the "key" star measure: sky background centers for each of 2 "locating" stars shape of "locating" stars reject any calibrated image where "location" star elongation is too large estimate the variance of a faint object in this image: est_var = sky_var * exp(key_mag - key_min_mag) * (fwhm*fwhm) is proportional to it weight for frame when merging is 1/est_var compute translation, scale, and rotation required for registration compute weighted sky estimate and add to sum MERGE EACH CALIBRATED IMAGE:  MERGE EACH CALIBRATED IMAGE merge this calibrated image into 12 merging buffers 12 needed to handle variance, weight, and cosmic ray removal later bad pixels are skipped subpixel merge into the image buffers using bilinear interpolation subtract sky from each pixel because it is so dominant weight each pixel by 1/(est_var) add weight to the sum_of_weights buffer for each pixel for each pixel location, remember max and next_to_max value seen in buffers for cosmic ray removal later COMPLETE MERGE:  COMPLETE MERGE remove cosmic rays. For a pixel: use merged image value excluding max and next_to_max values statistically decide whether max is a cosmic ray, ditto next_to_max if cosmic ray, remove from sum and sum_of_weights buffers compute for frame: sky = weighted_sky_sum / sum_of_sky_weights compute for each pixel: pixel = (weighted_sum / sum_of_weights) + sky S&T Deep Field Merged FLATTENING THE IMAGE:  FLATTENING THE IMAGE why isn't it flat now? I did flat field every raw frame but there is an extreme sensitivity to flat field errors due to light pollution range of image is 1.444e6 to 1.459e6 photons/pixel, just 1% image is 99% light pollution sky flatness failure is 6000 photons/pixel, just .4%, but that is 40% of the total image range flattening method: separate sky from stars and other objects examine sky near each final image pixel to get a sky estimate for that pixel for each pixel subtract off local sky estimate, add on overall sky average only works with small objects, and fails with nebulosity S&T DEEP FIELD FINISHED IMAGE:  S&T DEEP FIELD FINISHED IMAGE Mag. 24.5 Objects Have SNR Of 3 According To Bradley Schaefer FAINT TARGET URBAN CCD PROBLEM:  FAINT TARGET URBAN CCD PROBLEM flattening the sky background is the #1 problem any spectrally independent lack of flatness in the CCD chip does not matter as long as your master calibration frame is good (this does require care) what matters is any spectrally dependant lack of flatness spectral variation of each pixel’s sensitivity creates the problem because sky background, target, and the flat field light source all have a different spectral content back illuminated chips are especially bad due to interference effects CCD FLATNESS COMPARISON:  CCD FLATNESS COMPARISON Thomson CSF TH7883 and SiTe 502A were compared used master flat calibration frames for B, V, R, and I photometric filters where the average pixel value was 1. measured standard deviations of flat differences between filters: TH7883 SiTe 502A B-V 0.0144 V-R 0.0027 0.0052 R-I 0.0058 0.0168 the TH7883 should be able, ultimately, to go substantially deeper, but with much longer exposures. SPECIAL URBAN REQUIREMENTS:  SPECIAL URBAN REQUIREMENTS high flat field quality proper baffling perhaps filtering for light pollution. I have not tried this except to use a photometric I filter to darken sky my skies are suburban at <19.3 mag./sq.arcsec (dark is 22) so my advice may not be entirely appropriate the ability with the CCD to subtract the sky makes the big urban difference in comparison with film or eyesight unfortunately, due to higher sky noise and flat fielding failure, an urban site still cannot match a dark site ASTROPHOTO SUGGESTIONS:  ASTROPHOTO SUGGESTIONS when doing astrophotos, avoid the hackneyed objects, or at least do some different view of them pick suitable targets: that fit the chip well are overhead at the middle of the observing session do long exposures get in close EXAMPLE OF CLOSE IN - CORE OF M31 (1):  EXAMPLE OF CLOSE IN - CORE OF M31 (1) usual amateur picture covers 3 degrees and the center 15 arcmin is burned out this has .47 arcsec pixels, 3.0*4.5 arcmin 7" refractor, homemade CCD camera, no filter 54 min. exposure some interesting dark patches on the left EXAMPLE OF CLOSE IN - CORE OF M31 (2):  EXAMPLE OF CLOSE IN - CORE OF M31 (2) same image, different stretch center of the reduced image was not saturated and this shows that M31 has a very bright point-like center - not evident in most photos EXAMPLE OF CLOSE IN - CORE OF M31 (3):  EXAMPLE OF CLOSE IN - CORE OF M31 (3) same image unsharp masked in MaxIm (but the official way failed) mask made using low pass FFT filter with 2.5% cutoff and 100% weight image - mask + 10000 using pixel math 10000 added because MaxIm does not understand negative numbers EXAMPLE OF CLOSE IN - CORE OF M31 (4):  EXAMPLE OF CLOSE IN - CORE OF M31 (4) deconvolved using MaxIm in this image the background is not the sky – it is the star clouds of M31 EXAMPLE OF A DIFFERENT VIEW - NGC 206 IN M31:  EXAMPLE OF A DIFFERENT VIEW - NGC 206 IN M31 I R V photometric filtered images rendered as R G B faintest star visible limited by confusion - more resolution is needed to do better, not more exposure pixel size 1.09 arcsec exposures: I 348 min. R 562 min. V 434 min. 16" Newtonian, homemade CCD camera weighted merge was tuned to enhance sharpness ALIGNMENT FOR GERMAN EQUATORIALS (1):  ALIGNMENT FOR GERMAN EQUATORIALS (1) I use Project Pluto's Guide for map of the polar region mark refracted pole location do rough alignment some other way have RA drive on use low CCD magnification aim telescope at pole with telescope on one side of pier start 1 min. exposure after 30 sec. pull counterweight shaft around 180 degrees slowly in 30 sec. ALIGNMENT FOR GERMAN EQUATORIALS (2):  ALIGNMENT FOR GERMAN EQUATORIALS (2) Center of half circles is where the polar axis is pointing. Adjust mount elevation and azimuth until correct. Sorry – these pictures are not mates Shim OTA on saddle and adjust DEC to center the half circles. Set DEC circle to 90° ALIGNMENT FOR GERMAN EQUATORIALS (3):  ALIGNMENT FOR GERMAN EQUATORIALS (3) Doing Precision Adjustment Of Elevation And Azimuth OPTICAL ALIGNMENT TOOL:  OPTICAL ALIGNMENT TOOL fits into vane holder in place of secondary to first align the spider fits into eyepiece focusers 1.25" & 2" fits into collet on front of filter wheel HeNe for 1/2 sized spot aluminized center dot on primary with clear donut around it instead of a gummed reinforcement. Gum will streak when washing mirror with alcohol Homemade HeNe Laser Collimator Slide55:  TECHNIQUES FOR IMAGING VERY FAINT OBJECTS Paul Boltwood, paul@boltwood.ca 1655 Stittsville Main St., Stittsville, Ont., Canada K2S 1N6 (613) 836-6462 More at ottawa.rasc.ca under the Astronomy button. A more technical talk on the S&T Deep Field image given at Starfest 2000 is on the CDR and the web site. The techniques in it are somewhat different.

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