Quasars: Imaging the Visible Edge of the Universe. David Haworth Copyright 2010
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1 Quasars: Imaging the Visible Edge of the Universe David Haworth Copyright 2010
2 Imaging Equipment OSP 2008 QSI 532ws-M1 camera 9.7mm x 14.9mm Tele Vue NP-101is APO refractor 4 inch dia., focal length = 540, f/5.4 Focal reducer: Tele Vue NPR X Focal length = 432, f/4.3, 3.24 arcsec/pix Astronomik Type IIc Luminance filter Orion Atlas EQ-G Mount GoTo Controller Losmandy G-11 tripod Orion StarShoot AutoGuider Guide scope: 40mm dia., 250mm focal length Guiding software: Stark Labs PHD Guiding 2
3 3 Eye Candy: NGC253
4 4 Brain Candy: 17 QSOs Near NGC253
5 Quasars & QSOs Quasi-Stellar Radio Source & Quasi-Stellar Objects 1959 Third Cambridge Catalogue of Radio Sources C 48 first optical observation C 273 first identification of z=.158 Maarten Schmidt solved the unknown broad emission lines Credit en.wikipedia.org/wiki/redshift 5 Credit 1&Ns=p_date_range%7C1&Ntt=Maarten+Schmidt +&x=4&y=60,16641, ,00.html
6 Quasar 3C 273 Redshift Z = (503.2 nm 434 nm)/434 nm = nm nm H-alpha nm nm H-alpha nm 6
7 Quasar 3C 273 NASA/IPAC EXTRAGALACTIC DATABASE 7
8 Today Quasar 3C 273 Age of Universe H o = km/sec/mpc, Ω matter = 0.27, Ω vacuum = 0.73 Cosmic microwave background radiation Age of the Solar System 3C Age of Universe Gyears 8
9 9 17 QSOs Near NGC253
10 17 QSOs Near NGC QSOs Light Travel > Solar System Age ~4.5Gyr 10
11 BRI J [WHO91] [HB89] [HB89] [WHB96] [HB89] LBQS LBQS [WHO91] [HB89] LBQS [HB89] Today Imaging at Visible Edge of Universe Age of Universe H o = km/sec/mpc, Ω matter = 0.27, Ω vacuum = Age of Universe Gyears 11
![QSO [WHO91] 0043-259 Redshift 3.](/docs-images/86/93972128/images/12-1.jpg "309050 Positive Image Negative Image Negative &")
12 QSO [WHO91] Redshift Positive Image Negative Image Negative & Markers NED Image 12
13 QSO BRI J Redshift Positive Image Negative Image Negative & Markers NED Image 13
14 Exposure Image 61 images x 2 minutes per image 122 minutes total CCD-TEMP: -30 C Statistics Signal to Noise of the background with no stars Background average /background Std Dev = Signal to Noise
15 NP127is Driveway Imaging miles East-North-East from the center of Portland 15
16 Driveway Imaging 16 miles from the center of Portland 16
17 17 QSOs Near NGC3079
18 18 QSOs Near NGC3079
19 Twin Quasar Q Redshift
20 Twin Quasar Q Gravitational lens at magnitude
21 Image Statistics S/N= Background Ave/Std Dev = /0.592 = images x 2 minutes per image (98 minutes total) 21
22 22 Tele Vue NP127is at ARGO
23 QS0 SDSS J Dave Rowe PlateSolveXP 23
24 QS0 SDSS J DSS Image 24
25 QS0 SDSS J DSS Image 25
26 QS0 SDSS J SDSS Image 26
27 QS0 SDSS J min x 25 Images = 50 Minutes Image 27
28 QS0 SDSS J R Band Magnitudes
29 QS0 SDSS J Profile Curve 29
30 QS0 SDSS J S/N= Background Ave/Std Dev = /0.414 =
31 Today Gyears Age at Redshift SDSS J z = % of the Age of Universe
32 32
33 33 QS0 SDSS J
34 34 Galaxy R 20.16
35 Galaxies R Band Magnitudes
36 Stars R Band Magnitudes
37 Quasar 3C 273 Redshift Z = (503.2 nm 434 nm)/434 nm = nm nm H-alpha nm nm H-alpha nm 37
38 Star Spectroscope $249 38
39 Driveway Imaging 16 miles East-North-East from the center of Portland 39
40 Star Spectroscope, NP127is & QSI532 Vega Spectrum, 0.2 sec Diffraction Grating Orders M M = (Grating Interval Distance)sinθ Blazed 2 40
41 H H H H Star Spectroscope, NP127is & QSI532 Focus is between H & H Intensity peak is between H & H 41
42 H H H H Star Spectroscope, NP127is & QSI532 Focus is between H & H Intensity peak is between H & H 42
43 H H H H H Star Spectroscope, NP127is & QSI532 Focus is at H Intensity peak is at H 43
44 H H H H Star Spectroscope, NP127is & QSI532 Focus is just beyond H towards H Intensity peak is between H & H 44
45 H H H H Star Spectroscope, NP127is & QSI532 Focus is between H & H Intensity peak is between H & H 45
46 Radial Velocity Spectra Credit Quasar 3C 273 Redshift Measurement 46
47 Quasar 3C 273 Redshift Credit One 300 second image 3C
48 Star Spectroscope, NP127is & QSI532 MaxIm DL V5.07 Create master Darks Flat darks Flats Stacked calibrated image Graph window to determine wavelength calibration 48
49 Quasar 3C x 5 min Credit One 300 second image 49
50 Quasar 3C 273 Redshift Credit 16 x 300 second images H-beta H-alpha 50 3C 273
51 Quasar 3C 273 Redshift Credit Star BD , F5 used for calibration H-beta H-gamma H-alpha BD C 273
52 Wavelength Calibration H at 266 pixels 52
53 200 lines/mm grating Wavelength Calibration = (d)sinθ θ = arcsin(h /(200 lines/mm)) Tanθ = 266 pixels/distance Distance = 266 pixels/tanθ Distance = 18.24mm θ QSI532 CCD H at 266 pixels Å 53 =SIN (ATAN ( *(pixel distance) / ))* * Diagram not to scale
54 Quasar 3C 273 Redshift Credit Redshift z =
55 Quasar 3C 273 Redshift Credit Quasar 3C 273 Spectrum UV IR-A 55
56 Quasar 3C 273 Credit Observed Spectrum Redshift
57 57
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Sources of Noise. Noise can come from a variety of sources but can generally be grouped under three headings.
Noise The next factor to be investigated is noise. (It is a common misconception that the more sensitive a camera is the fainter the object you can detect. In fact it is the amount of noise, both from
Spectral Interferometry for Broadband UV / Optical Astronomy
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