Home

DADOS Spektrograph Tutorial

1. R Balmer neh doa 3645 6 I M Ca Seon 47 Ca II 3935 66 K H 3600 3800 4000 6200 6400 6600 ew 9 s a PAL a mi TI v1 Y Y mw A w Wy cal 6162 00 I Ho 6562 82 Ca I Telluric O 6102 72 6280 40 d mere Hs 4101 74 Ca I 4226 73 9 4400 4340 47 SF MA md vi Y 4600 di A ECTROGRAPH M spectrum 4800 Fe I 46886 00 f Aty AAAY MP Ww 1 Hp 4861 33 F 4200 6800 I 4400 7000 w Fraunhofer B Absorption 6067 6944 B 7 Any H O Absorption 4600 DADOS 900 L mm und ALccd 5 2 CCD Kamera Spektrum Tom Schnee und Johannes Schnepp 2012 200 4800 7400 WN tuse Wi 7160 7394 AA 5200 5000 5400 AA ALccd Li JM 5600 5800 5 2 CCD Camera ORIAL E 6000 Vu ANC WM APP YY W AIR Aag av IN VT NK Ke Y M au AN Mw Nw eg he Y M V yn 4057 60 ue weih p LN 5857 00 183 en 5328 00 e rie NI I 5753 38 5476 91 Mg I Na I 5172 68 5889 95 Fel Mg I 5270 00 5000 5200 5400 5600 5800 6000 WA 7600 7800 8000 B200 8400 8600 A i Ti Hi w ow i we A e nm Fh W Mb wer a 4 aA Y i N i d MIN m Wil A a n d id V i li Ca II y 8498 07 i Ca II d HA 8542 02 i Absorption 8320 8385 Ca II Fraunhofer A 8662 93 OO Absorption Al 7594 7684 DADOS 9oo lines mm and ALccd 5 2 CCD camer
2. gsx e f Se by Jon Lomberg Radius 5 5P Ra Luminosity 4 169l Lo Temperature 15 5005 K Rotational velocity v sin i 125 km s Age 225226 Myr t Tau B Mass 0 940 Mo Other designations 123 Tauri HR 1910 HD 37202 BD 21 908 FKS 211 HIP 26451 SAO 77336 GC 6985 Ne I 6506 5277A Ha Ne I 6598 9528A Ne I 6532 8824A Zeta Tauri al LI a 4 e Be eng i 1 dc e x gaus A A e e er en e u BA Observation data Epoch J2000 0 Equinox J2000 0 ICRS Constellation Taurus Right ascension 05 37 38 685425 Declination 21 08 33 158271 Apparent magnitude V 3 01 ol Characteristics Spectral type B2 lip U B color index BK B V color index _0 164 2 Astrometry Radial velocity Rv 20 4 kms RA 1 78 mas yr Proper motion y Parallax m 7 33 0 82 mas Distance approx 440 ly approx 140 pc Orbit Period P 132 987 days Semi major axis a 1 17 AU Eccentricity e 0 0 assumed Inclination i 92 8 Longitude of the node IO 58 0 Periastron epoch T 2 447 025 6 HJD Argument of periastron 0 0 assumed bal secondary Semi amplitude K1 7 43 km s primary Date 2014 03 10 mid exposure 23 30 UT 0 3m aperture f 10 DADOS 1200 lines mm grating CCD camera SBIG ST 8300M total exposure 3x300s with darkframe subtraction without flatfielding Spectral resolution about 1 49 A Calibration with Xenon Neon plasma tub
3. DADGS sur srectrocrary TUTORIAL El Dado 1 Field of view at slit viewing port Guiding camera View through the guiding eyepiece Simulation TT DT ee Guiding eyepiece IP Slit viewer Slit viewer Os Slit viewing port zm i eil Pleiades Star Cluster Pentax 75 500mm e Central slit 25 um gives best spectral resolution e The 50 um slit provides the brightest visual stellar spectra e Spectral resolution is independent of the telescope s focus e Perfect telescope focus maximizes contrast of spectral lines e Guiding is possible at the slit viewing port The slit s length should be parallel to Declination 6 direction 2 Nosepiece Slit illuminator V3 5E Bernd Koch b koch baader planetarium de 12 Td c EH IINE to ET it dm 3 O Ge gr 7 am O gt V3 5E Bernd Koch b koch baader planetarium de DAD C 3 SPECTROGRAPH UTC RIAL CA Dado ctroscopy The Aristarchus Plateau DMK 41 Ze Q O A TI E oD c un of Un N iem af Ka rj r Video Jonas Niepmann V3 5E Bernd Koch b koch baader planetarium de s J ZA LL 1 S PECTROGRAPH UIC RIAL _ E Dado 2 The blazed reflection grating Resolving power AA on camera objective axis and 25 um slit Grating of 200 lines mm Theoretical Measured nm 396 542 416 606 647 616 668 723 697 Gra
4. Step 1 Image Browser Check the quality of spectral images Step 2 Fitswork Download and check settings Step 3 Fitswork The stacking process Create an averaged color spectrum Step 4 Fitswork Rotate crop convert to monochrome spectrum amp save Step 5 Visual Spec VSpec Spectrum calibration w o instrumental response Step 6 Visual Spec VSpec Visualize Profile as synthetic color profile Step 7 VisualSpec VSpec Spectrum calibration by instrumental response and calculation of the effective temperature of Betelgeuse from its spectrum Step 8 Visual Spec VSpec Visualize profile as a synthetic color profile V3 5E Bernd Koch b koch baader planetarium de 36 DADOS SLIT SPECTROGRAPH TUTORIA ee T MMM 9 Stacking calibration of stellar spectra from a Canon DSLR camera Step 1 Check the quality of spectral images in an image browser Dataset Betelgeuse 200L 2010 312 15 1 Spectra JPG gt Note the image numbers of the perfectly imaged spectra with regard to exposure time and sharpness of spectral features Ignore imperfect spectra V3 5E Bernd Koch b koch baader planetarium de 37 p DADOS sspe UTORIA Em Stacking caltbresior_of stella ep et RUIT anon DSLR camera Step 2 Spectrum stacking with Fitswork Download Fitswork at http www fitswork de software softw en php Start Fitswork Fi
5. No need for a color camera Synthetic color spectra can be created with Vspec Difficult to handle for beginners in astrophotography and astrospectroscopy V3 5E Bernd Koch b koch baader planetarium de 32 pbagder DIE a V I a RIAL E non DSLR camera T 96 Ha 100 ca 98 80 Baader BCF filter Canon filter A ep EO NO Credit Bernd Koch Axel Martin 200 400 600 800 Wavelength nm http www baader planetarium de sektion s45 canon_astroupgrade english htm V3 5E Bernd Koch b koch baader planetarium de 33 SS EE ee Exercise 1 a Orionis Betelgeuse Date 2010 12 15 Pentax 75 SDHF 500mm Canon EOS 450D Baader BCF Filter ISO 800 Spectrograph DADOS Grating 200 l mm Spectral resolution 12 A 5500 A Scale 2 1 A Pixel Betelgeuse Spectral Class M2lab Apparent magnitude 0 7 mag Set of 11 spectra each 8 s exposed Darkframes not used Flatflields not used Images Betelgeuse 200L 2010 12 15 V3 5E Bernd Koch b koch baader planetarium de 34 Stacking calibration of stellar spectra from a Canon DSLR camera a Orionis Betelgeuse M2Iab 1x8s 11x8s DADOS 200 lines mm Canon EOS 450D BCF filter 11x8s Improved SNR signal to noise ratio due to stacking V3 5E Bernd Koch b koch baader planetarium de DADA C S A tacana T SPEcTROGRAPH U IL RIAL E stellar spectra from a Canon DSLR camera
6. sey NEC V The Coathanger Altair PNV J20233073 2046041 or Nova Delphini Nova 2013 is a brightinova star in the constellation From Wikipedia the free encyclopedia Delphinus Itwas discovered on 14 August 2013 by amateur astronomer Koichi Itagaki in m A nova plural novae or novas is a cataclysmic nuclear explosion in a white dwarf which causes a Japan and confirmed by the Liverpool sudden brightening of the star Novae are notto be confused with other brightening phenomena Telescope on La Palma The nova appeared such as supernovae or luminous red novae A nova is caused by the accretion of hydrogen on to the with a magnitude 6 8 when it was discovered surface of the star which ignites and starts nuclear fusion in a runaway manner Novae are thought d to occur on the surface of a white dwarf in a binary system If the two stars are close enough and peaked at magnitude 4 5 on 16 August material can be pulled from the companion stars surface onto the white dwarf For other uses see Nova disambiguation and Novas disambiguation V3 5E Bernd Koch b koch baader planetarium de 03 DADOS SLIT BPECTROGRAPH TUTORIAL Ges Nova Delphini 2013 August 16 2013 A LI o Le 2013 08 16 23 22 UT 23 55 UT mid Exposure August 16 985 UT 0 3m aperture f 7 8 f22340mm SBIG ST 8300M Baader RGB Filter Nova maximum Aug 16 45 0 V 4 3 mag Image amp Processing Bernd Koch Sorth Ge
7. Ad A 17390 4570 4840 5110 5380 5650 5920 6190 6450 6730 7000 7270 V3 5E Bernd Koch b koch baader planetarium de 55 Stacking calibration of anon DSLR camera Step 5 Visual Spec VSpec Continuum extraction from the raw profile 5 11 Press point courbe sic set 20 to 50 points actually green crosses along the continuum upper limit euze summenspektrum mon File Edit ve Operations Spectrometry Radiometry Tools Assistant Window Options 5 sei NM 0 x2i 3 4307 17 I 5923 852 7 2 1532 A pixel a Ori Betelgeuse Class M2lab DES ck DI cot V3 5E Bernd Koch b koch baader planetarium de 56 PavAs Stacking calibration of stellar spectra from a Canon DSLR camera Step 5 Visual Spec VSpec Continuum extraction from the raw profile 5 12 Press Execute The resulting continuum is the orange red line i Visual Spec beteigeuze enspektrum mono wavecal spc EI rie Ed rormat a A So romet et Tochs Assistare a Ori Betelgeuse Class M2lab 156510 139120 86950 69560 4570 4840 5110 5380 5650 5920 6190 6460 6730 7000 7270 V3 5E Bernd Koch b koch baader planetarium de T SPECTROGRAP H A 48010 mmm DES ck DOE GzZk a a EUM SES VER Ph LJ B Stacking calibration of stellar spectra from a Canon DSLR camera Step 5 Visual Spec VSpec Cont
8. Bernd Koch b koch baader planetarium de 41 DAD DC 3 ET Stacking calibre ion ofs Step 3 Fitswork The stacking process Create an averaged color spectrum Dataset Betelgeuse 200L 2010 12 15 2 Spectra raw images CR2 PECTROGRAPH mm B TORIAL Ez3 a Canon DSLR camera tellar spectra fr 2 Step of Processing sic gt Add to destination image gt Planet Moon gt Crosscorrelation gt Number of Marks gt Function Mid means average gt Press start button Batch Processing a H D J o oO 2 Step of Processing 1 SPECIFY FILES Start File C QDokurmnente und Einstellungen astrofato D esktop Betelgeu se 2L 2010 12 01 5 2 5pektra raw ima ges CH2 Betelgeuse LDT LRZ Destination File I Edge All Files in Folder doe Detect 30 0 12 ADD TO DESTINATION IMAGE of white Crosscorrelation Humber of Marks 1 Function Mid l V3 5E Bernd Koch b koch baader planetarium de 42 sas jLIT BPECTROGRAPH TUT RIAL CG e EE ru Stacking caim nan Arat spectra a from a Step 3 Fitswork The stacking process Create an averaged color spectrum Dataset Betelgeuse_200L_2010 12 15 2_Spectra_raw_images_CR2 anon DSLR camera Draw a tight frame around the first spectrum Skip bad images which are not properly focused or exposed Load the next frame
9. V3 5E Bernd Koch b koch baader planetarium de 9 prc A gg irror and slit illuminator DAD sl SLIT SPECTROGRAPH Slit viewing port guiding port Slit plate EX The slit plate contains three slits of different Sh a I widths 25 um 35 um and 50 um Mirror The small mirror allows the observer at the slit viewing port to keep an object s image exactly on one the slits Slit illuminator To be visible against a dark sky background the slits can be illuminated by an adjustable red LED Please note Mirror Don t forget to switch off the slit illuminator before starting the exposure of the spectrum Otherwise the red LED stray light will be superimposed on the image of the spectrum To save battery energy always be sure to switch off the illuminator while not in use The illuminator holds two 1 5V batteries LR41 Slit illuminator V3 5E Bernd Koch b koch baader planetarium de 10 Guiding camera the guiding eyepice es 4560 wi U i E SNIN e Guiding eyepiece 25 um f Slit viewer Slit viewer Bright background Point the 2 nosepiece at a bright light source Look through the guiding eyepiece Each of the three slits has a different width The width of a slit is crucial for spectral resolution The length of a slit is irrelevant 2 Nosepiece VNNN Slit illuminator Y V3 5E Bernd Koch b koch baader planetarium de DI
10. 5800A Bernd Koch 2013 09 16 Xe 4500 978 Xe 4524 6805 Xe 4582 7472 Xe 4624 2756 Xe 4671 2258 Blend Xe 4690 970 Xe 4697 0208 Xe 4734 1518 Xe 4792 619 Xe 4807 0190 Xe 4829 708 Xe 4843 2934 Blend Xe 4916 51 Xe 4923 152 Xe 5028 2794 Ne 5400 5616 4400 4500 4600 4700 4800 4900 5000 5100 5200 5300 5400 5500 5600 5700 5800 V3 5E O Bernd Koc 91 b koch baader planetarium de A EDLLI Gg Geh BELLO UL y Tu EE Oo Ne 5852 4878 o e Ne 5881 8950 Ta Ne 5944 8340 7 Ne 5975 5343 Xe 8231 6336 Xe 8280 1162 S ES Ne 6029 9968 x gt x lt Ne 6074 3376 Ne 7032 41 Ne 6096 1630 y Ne 6143 0627 x Ne 6163 59 amp Xe 6182 420 x Ne 6217 2812 Ne 6266 4952 Ne 6304 7893 Xe 6318 062 Ne 6334 4276 Ne 6382 9914 ec POSTER Xe 7119 598 S Xe 6469 705 Ne 7173 9380 X Ne 6506 5277 S Ne 6532 8824 p ac Xe 8346 8217 x e s Ne 7245 1665 Xe 8409 1894 Ne 6678 2766 Xe 7284 34 Xe 8206 336 Ne 6717 0430 Xe 7393 793 Xe 7386 003 Xe 6827 315 Ne 7438 8970 Xe 7967 342 Xe 6882 15 Ne 7488 8712 Ne 692314672 Ne 7535 7738 Xe 6976 182 Xe 7642 024 5800 5900 6000 6100 6200 6300 6400 6500 6600 6700 6800 6900 7000 7100 7200 7300 7400 7500 7600 7700 7800 8200 8400 V3 5E Bernd Koch b koch baader planetarium de DADOS SLIT BPECTROGRAPH TUTORIAL al Nova Delphini 2013 Discovery August 14 8174 UT NELP HENUS Et A SAG TTA
11. Cal 9893 Na D 5889 95 5895 92 og 29 2 97 7 az prez 0 maze ave Antares a Sco gt S aS 2035 P Ses EXO 38 alee 9 lab g Co i 4861 33 e Piin Ms LE T I ff E S T e al m y GL 2 9o 9 n mo o 2 o 5 9 2 Hp 2s EARS e kein gg 35 2 98 o I e fie n 90 Tees A o IIl IV WUR iy TN U M UN wA a o 2 AL VEY AN UNI uv PU wild a 8 8 H mm v I V 1 l d al e NNI T HPV WW UST qm Wa amp z BEL MIL IN fl WI 3 telluric z TI ll x re mma nm S A A E o 3 o 350 4000 ioo sap 4900 4400 4500 eo poo eoo 4900 shoo SI00 00 300 S404 oo S600 700 sod poop ooo 6100 pzo0 soq poo esoo eod jejoo poo esoo 7009 ipo 1400 Suggested reference Spectroscopic Atlas for Amateur Astronomers by Swiss amateur astronomer Richard Walker http www ursusmajor ch downloads spectroscopic atlas 4 0 pdf V3 5E Bernd Koch b koch baader planetarium de 53 z PECTROGRAPH L RIAL G ma Canon DSLR camera Stacking calibration of stellar s Step 5 Visual Spec VSpec From pixel to ngstrom Wavelength calibration of the x axis _ d Get 5 peki e Jj d id a 4561 33 1 252 5258 0 0181 ecce 5125 2 481 0345 0 1738 ES 5270 3 5438752 0 3745 Hi P 9371 43 4 598 4399 0 228 Load 5893 5 849 6815 0 0103 Degre 3 B5EB2 82 B 1154 228 0 001 t Deore 1 181440 NV _ Save Degre 2 Degre 3 1 l
12. Credit Thomas Schrofl 22 10 2013 17 40 UT DADOS 200L mm amp SBIG STF 8300M x ar dq SEUTUSFISPOT A EE CFG AMAL ta x veqs_l0sec_id absolut spc intensity Calibration by Bernd Koch V3 5E Bernd Koch b koch baader planetarium de 111 st AL LU S SPECTROGRAPH ORIAL E 3 8200 Stacking 8 ull calibration of spectra taken CCD camera In an upcoming release the subject e cee and full calibration of spectra obtained with a monochrome CCD camera will be described Stay tuned isual Spec DV File Edit Format Operations Spectrometry Radiometry Tools Assistant Window Options DADOS 200 lines mm amp SBIG ST 8300M Bernd Koch glia H Ox z179 sasiz zk 2 1648 A pixel BUS ER 03 6106 77 666 74 Rett efen F um l t 21 QL OC ED n Ss o6 4t 6 le 2b atair 1x1 20c 60 004 wavecal pseudocontinuum normiert spc 20 a Aql Altair Spectral Class A7V H9 H8 T E Telluric lines 40 p H Hy Earth s atmosphere Calll K 3933 66 4465 5230 5995 6760 7525 8290 hs atair 1x1 20c 60 004 wavecal pseudocontinuum normiert spc intensity 2013 09 13 19 20 UT Stack of 10 x 1s exposure time 10s Autodark DADOS 200 lines mm SBIG ST 8300M Image and calibration Bernd Koch V3 5E Bernd Koch b koch baader planetarium de 112 DADOS SLIT SPECTROGRAPH TUTORIAL References amp recommended reading by B
13. Ok go on Check if the area is marked yellow frame is still in place Go through all images with or without controlling image quality The final image the stacked spectrum will be saved after a while as Result image fit Create a new folder 5 Results and save copy of Result image fit 3 Results is your new working directory SERGE Add to Destination Image Please mark an amp rea and dto d g click afterwards on Dk go on Skip Image W_images_CR2 Betelgeuse_01 CR2 No more Controlling Cancel Pause Cancel Please note The quality of the final spectrum depends on recognizing spectral lines in each single image Spectra with short exposure times and consequently low contrast may not stack properly V3 5E Bernd Koch b koch baader planetarium de 43 DADOS Site EST COGRAPH TUT RIAL E Ee M Stacking calibration of stellar spectra froma Canon DSLR camera Step 4 Fitswork Rotate and save again as Result image fit Rotate Result image fit to achieve a perfectly leveled spectrum Processing gt Image Geometry gt Rotate image with Subsidiary Line met PPM a E LIETE ER File Processing Image Combining Settings Window Help E Add Borders Ctri4R T F R is Ext w A i WF er Tt Resize Image Cl tS CON CN CCCRNE lx Pixel Arithmetic Sharpen Filter d m E Blur Filter Correct Image Distortion Ba
14. also be calculated by the broadening of the emission lines measured at Ha rwHM L 267A FWHM km Vp Z Co 1220 5 FWHM 26 7A Absorption Emission FWHM 26 7A Ay 6562 82 co 299792 Ref www ursusmajor ch downloads analysis and interpretation of astronomical sp pdf V3 5E Bernd Koch b koch baader planetarium de DADOS s rsreecreossae TUTORIAL ES Nova Delphini 2013 08 19 23 amp 2013 09 05 summary All spectra taken with DADOS 200 lines mm with 0 3m Telescope by Bernd Koch 19 8 2013 20 07 UT 20 33 UT Voc odio det mm hae e OI 6300 304A OI 8446A 23 8 2013 22 30 UT 23 00 UT He HI 4861 33 HI 6562 85 5 9 2013 21 03 UT 21 40 UT Nova Delphini database www astrosurf com aras novae Nova2013Del html V3 5E Bernd Koch b koch baader planetarium de 100 VV VV VV VV N V Celestron 1 DADOS goo lines mm STF 8300M CCD camera Pentax 75 2x Converter DADOS goo I mm STF 8300M CCD camera Spectrum recording amp video camera guiding MaxIm DL Win XP 7 32 bit tested Set y Cas on the middle of the three slits 25 um for highest resolution The slit s length should be parallel to Deklination 8 direction Center spectrum on Ha by turning the micrometer adjustment Keep exposure time well below the saturation level of the sensor 1s 60s Guiding Video camera Skyris 274M TIS DMK 41 or else Number of images per spectrum Minimum 20
15. 0 0615 Lambda S o 6594 361 5 476 2359 0 0488 Degre Save C Dege d C Degre 2 y Cassiopeise win rita adc e Degre 3 Observation data Reset C Degre4 Epoch J2000 Equinox J2000 Constellation Cassiopeia nonet D Bm Calibration with telluric H20 lines Declination 60 43 00 2984 Apparent magnitude V 2477 Characteristics Spectral type B0 5 Ive U B color index 1 02 B V color index 20 1512 Variable type Gamma Cas Astrometry Radial velocity Rv 8 8 4 kms Proper motion p RA 25 KAN mas yr Dec 3 92 mas yr Parallax m 5 94 0 121 mas Distance 550 10 ly 168 3 pc e e 1 1 em Telluric lines Telluric lines Mass 19 3 0 13 M ms S SA keen Ve i l int v barn gf M AN MOST mm mM Luminosity 55 000 Lo Surface gravity log g 3 50 cgs m H20 H2O Temperature 30 900 K Rotational velocity v sin 3007 kms Date 2011 04 19 882 UT Cu EdgeHD 0 28m aperture f 10 DADOS goo lines mm grating CCD camera Alccd 5 2 QHY6 Single exposure 120s Average of 20 exposures Darkframe subtraction no flatfielding Spectral resolution 2 3 at 6563 Calibration with VisualSpec telluric HO FWHM 7 9A EW 23 4A 6520A 6605A RV 5 2 km s Spectrum obtained at a spectroscopy workshop at the College CFG Wuppertal Germany Calibration amp results Bernd Koch V3 5E Bernd Koch b koch baader planetarium de
16. 16bit Create a spectrum profile gt Identify spectral lines gt Calibrate wavelength nad NM ON PEN al ZS ep C OWNONS S a i les ke Betelgeuse profile MalIab i 4390 4480 4570 4660 4750 4840 4930 5020 5110 5200 5290 5380 5470 5560 5650 5740 5830 5920 6010 6100 6190 6280 6370 6460 6550 6640 6730 6820 6810 7000 7090 7180 7270 7360 7450 V3 5E Bernd Koch b koch baader planetarium de 7O Stacking calibra eege T anon DSLR camera Step 7 Visual Spec VSpec Spectrum calibration by removing the instrumental profile 74 File Open profile Result image wavecal spc 208680 191290 173900 156510 139120 121730 104340 86950 69560 52170 34780 a Ori Betelgeuse Class M2Iab 4840 5110 5380 5650 5920 6190 6460 6730 7000 7270 V3 5E Bernd Koch b koch baader planetarium de 71 Step 7 Visual Spec VSpec Spectrum calibration by removing the instrumental profile 7 2 Assistant Instrumental response sic assistant 7 3 Pickles gt Press on green arrow button gt Open mzai dat Class Mal m Instrumental response assistant Image result wavecal spc optional Spectral type Search spectral ype on SIMBAD b Select reference spectrum Ge Pickles UVES Miles C Elodie Milles 2 optional shift Wavelength shift D Response Division and extraction EI Save Save response in file reponse g iv
17. A BA g sina Path difference of reflected beam A AC g sin p A mA A A g sina sin D with m o 1 2 Grating equation V3 5E Bernd Koch b koch baader planetarium de 2 s ST GN Grating normal FN Face normal g Groove spacing o Blaze angle a Angle of the incident light p Angle of reflected light Grating equation mA g sina sinB gt sina sin B nl Derivative with respect to p d gcosB d p m d m Angular dispersion Pe oup Linear dispersion p yt FA ey f is the focal length of the objective lens oP o 0 M m arcsin Sin Q Blaze angle p 7 ub F V3 5E Bernd Koch b koch baader planetarium de 28 SspectRocraPH TUTORIAL E OS with blazed 200 lines mm grating Calculatio A B E D E F G H I J eee M N 1 SIMSPEC V4 0 english version by Ken Harrison original version by Christian Buil Latest Revision Apr 12 2 3 Enter data in highlighted cells Data Entry 4 5 Celestron Cu Diameter D Collimator pixel sizel p T 2 g 0 Focal length f Collimator Focal length f1 number of X pixels Nx 0 8 F D F Collimator Required Focal ratio Fc quantum efficiency m e escope aperture i mm 9 Central obstruction ei Collimator Minimum diameter d1 Read noise RON z 10 Teles th hput Reso
18. Visual Spec File Edit Form Operations amp iu o 4 al O x i 93 4500 96 I f2asse 161 7 2 1532 A pixel eso ZJ ckhue v F uaa me E HAR we AS toe HEA db O amp m bue See ea ree image_result_wavecal spc pectrometry Radiometry Tools Assistant Window Options lai E VE EI p Ej c lt gt m Selection Division image_result_wavecal spe intiByeiticantinuum spe intensity Olt gt E DE gt 7 kk p El EE spc Oe continuum spc A IE image result wavecal s B A Intensity V3 5E Bernd Koch b koch baader planetarium de 61 Infos 2 153177 pisel OF de 4302 97 7541 25 TESI Normalize and replace Lr nd c d E E Ge me Stacking calibration of stellar spectra from a Canon DSLR camera Step 5 Visual Spec VSpec Dataset division 5 18 The green profile is the result of division Now prepare to save the result i Visual Spec image result wavecal spc El File Edit Format Operations Spectrometry Radiometry Tools Assistant Window Options SIM ox 1502 I p18796 519V 2 1532 A pixel s Divisi ivision M EE vi J He DE cp 273540 250745 H0315 1 IE 4 j BP zen 15956 136770 113975 91180 68385 45590 a Ori Betelgeuse Class M2lab 4570 4840 5110 5380 5650 5920 6190 6460 6730 7000 7270 V3 5E Bernd Koch b koch b
19. another master of the art http stars astro illinois edu sow spectra html Dr Kaler also has a website on the same subjects as his book above This specific web address is one entry port into a trio of websites about stars and their spectra V3 5E Bernd Koch b koch baader planetarium de 114 f DADO Su ORIAL E N SPECTROGRAPH II d SAFETY RULES 1 NEVER look directly at the Sun with your eyes You can burn a hole in your retina resulting in partial blindness 2 NEVER change how solar observing equipment is set up for you Doing so may result in permanent blindness for yourself or others 3 If weare using the spectral calibration lamp take care not to touch the bulb as it gets hot enough to burn fingers 4 If you see a yellowish green indistinct fog while using the solar spectroscope in the deep blue end of the spectrum you have gone too far and ultraviolet in the sunlight is causing the vitreous humor in your eye to fluoresce This is not the best thing for your eye adjust the spectroscope to head away from the deep blue until the fog disappears 5 Avoid mashing your eye into the eyepiece Doing so is unnecessary and raises the risk of spreading conjunctivitis pink eye It also makes the telescope jiggle and observation harder 6 Dont play around with the batteries They can give you a serious electrical jolt 7 If you are unsure about anything ask OTHER RULES 1 Apply only light pressure to m
20. dat gaiv dat g8v dat km det kOiv dat kOv dat kD1ii dat k1iii dat kliv dat k2i dat Es k2iii dat lk det e k3i dat lat det V3 5E Bernd Koch b koch baader planetarium de k3iv dat k3v dat k4i dat kil dat kv det kat det k5v dat k7v dat k34ii dat mOiii dat mOv dat mili dat miv dat El CFI F E mzin dat m2v dat m3ii dat len at det m3v dat m4iii dat E m4v dat m det m5v dat m iii dat Ie m amp v dat rg v dat rg5iii dat rg5v dat km det rkOv dat rk1iii dat rk2iii dat m ion of stellar spectra from a Canon DSLR camera Step 7 Visual Spec VSpec Spectrum calibration by removing the instrumental profile The red profile is the reference spectrum of a star of similar spectral class ix Visual Spec image result wavecal spc el File Edit Format Operations Spectrometry Radiometry Tools Assistant Window Options x SG ij Ed Ed Dx 1500 7530 48 I 774 32 1532 A pixel s mai dat v amp M pupeF JS m m AQAA EXER ot 2 Sf oe ax b E 8 AE dp Y instrumental response assistant x amp 2 75 c optional Spectral type EE Search spectral type on SIMBAD E3 Select refe id E N 2 5 Pickles L Milles EI Mi A i5 optional shift Wavelength shift b 2 25 d esponse ivision and extraction 2 Save ave response in file 1 75 1 5 d U 1 25 1 0 75 0 5 3 H 4570 4840 5110 5380 5650 5920 6190 6460 6730 7000 7270 V3 5E
21. ex c 3 astrofoto X Desktop File gt Open image Result image mono pb Dr File Edt Format Operations Spectrometry Tools Assistant Window Options amp eai d ox 11953 E i F7 0 e ab ss ossoec GG SS 7 nena sl n v F m nal E ZOE Z o6 4 s VR Dj db V3 5E Bernd Koch b koch baader planetarium de 3 Dokumente und Einstellungen ECTROGRAPH TUT RIAL p um Lg anon DSLR camera beteigeuze summenspektru beteigeuze summenspektru Beteigeuze Summenspektn Betelgeuse final spectrum continuum spc Result image wavecal n Result image wavecal n Result image color 15bit f Result image color2 16bit Result image mono 15bit Result image mono 165bit Result image wavecal spc Image pic pic Profil fits fit crcl 50 DADOS Sure mmt TUTORIAL SS EE SS Kaesch P Step 5 VisualSpec VSpec Create a spectrum profile 5 4 Profile extraction gt All set to Auto gt OK gt Close a O x y 1546 5 Img D n Dm Et uP m a i mmo Wei w Ges O PP Tie SALSA 317 4 zz VB TT am S SS a uto pectrum position H 83 Yl 233 r 158 Tilt angle 2e Heigth 15 Sup Ti 0 Inf vi rit r Ok V3 5E Bernd Koch b koch baader planetarium de 51 DADUS 5 Suv Seecrrograrn TUTORIAL El SEH Stacking calibre ic 3 of s ellar e PEOR from a Canon DSLR camera Step 5 VisualSpec VSpec Save t
22. planetarium de 106 Credit Gemini Observatory Illustration by Jon Lomberg 25 Fa B 20 H oll X wg Ss xe A Stober 396 10 e d B Fontaine et al Ht x Andrillat iFehrenbach a 4 D Schanne 3 o Hanisch Prism 596 e Desnoux 3 5 Guarro 43 amp Garrel 396 Ha CTau Charbonnel 3 Gorodenski EW Angstr T gn a Heidbg Ondrejov Li 0 42500 45000 47300 20000 JD 2400000 V3 5E Bernd Koch b koch baader planetarium de n m Guo et al A Sletteb Reyn o Pollmann Prism 396 D Mauclaire 396 B cke 3 Kalbermatten 3 Buil 396 o Ubaud 396 D Sawicki f o Koch 92500 A A Pollmann Grating 396 i 55000 D 107 Credit Ernst Pollmann Credit Gemini Observatory Illustration by Jon Lomberg i Visual Spec S ia HAG o 1 24526 4924 78 0 97 30 05 pixel 4728 36 4730 4 1 2 04 intensity X r m blue SE oan m m HQ CH MRN Ela X Ton e E bPt kU Date 2014 03 14 817 UT o 3m aperture f 10 DADOS 1200 lines mm grating 120s exposure CCD camera SBIG ST 8300 5 4 Micron Pixel Spectral resolution 1 5A Calibration and creation of a synthetic colour spectrum with VisualSpec software Image and calibration by Bernd Koch V3 5E Bernd Koch b koch baader planetarium de 108 i Visual Spec File
23. 000D 1200 lines mm exposure 5 s 900 lines mm Exposure 1s Unsharp masking Se AG 1200 lines mm Exposure 5 s Ai 1 6 fully resolved Eet Unsharp masking V3 5E Bernd Koch b koch baader planetarium de 16 e DADOS sut srectrocrarH TUTORIAL Daylight spectrum of goo lines mm grating and 1200 lines mm grating DADOS 900 lines mm Spectral resolution 2 5 A O 75 px EOS 10D 7 211m Bernd Koch DADOS 1200 lines mm Spectral Resolution1 7 A O 47 px EOS 1000D 5 7117 Bernd Koch O 23 A px 0 088 A p x www lightfrominfinity org HIRSS HIRRS htm V3 5E Bernd Koch b koch baader planetarium de 17 A 2 Grating replacement Touching the grating will destroy it beyond repair Do not attempt to remove dust by breathing or blowing air onto the grating Small droplets of moisture and saliva can permanently damage the grating as well Do not use compressed or canned air This will likewise transport moisture grease or propellant onto the grating Any exchange of grating holders should always be performed in clean surroundings free of dust and static build up Arrange your workplace for ensure a quick and clean grating exchange V3 5E Bernd Koch b koch baader planetarium de 18 Have the 900 lines mm grating with holder readily available Loosen the grating angle locking screw 9 by one turn only Rotate the micrometer backwards to show an 8mm settin
24. 168480 i nun Emm Ze Degre 4 155520 7 935 3000 eg Sia 3230 3290 1350 1426 SIS 3540 M CG user SHES 608 4120 4 95 620 470 s TE 1 M 49 3 E 4790 amu ew Oo S tie 1230 p Ke Ee d E 7u SM 120 D hl t130 wa su aun MIC 142560 Fel WW IF 125600 2 5270 AN dh PA e V d X 116640 5893 j d V Ma D A La IE 103680 n 6562 82 Wits 5889 95 f H a 50720 J 5895 92 d n 77760 Ay M U 64800 4861 33 r Hp 51840 MV telluric o 38880 j e b ay a Ori Betelgeuse Class M2Iab AY A send KI Bed 350 70 1050 1400 Viren i V3 5E Bernd Koch b koch baader planetarium de 54 Lo EE Wi Stacking calibration of stellar spectra from a Canon DSLR camera Step 5 Visual Spec VSpec Continuum extraction from the raw profile 5 40 Compute continuum Visual Spec beteigeuze summenspe um mono wavecal spc t ag File Edit Format Operations Spectraffetry IE un tions 3 x g Lei A Dx z ampute Continuum L intensity Qe blue D oM Continuum Division Continuum Subtraction 208580 H20 correction H20 correction real spectrum e Auto H20 correcto QU UTI etelgeuse aSs Ala Verif Cal Atm 9 191290 Auto Planck Planck Extinction Compute flux of reference star 173900 Compute absolute flux 156510 139120 121730 104340 esso jeoseo 52170 34780 Oo
25. 40 5110 5380 5650 5920 6190 6460 6730 7000 V3 5E Bernd Koch b koch baader planetarium de poi spectra from a Canon DSLR camera Step 5 Visual Spec VSpec Calibration summary beteigruze sasmmenspektnam mono wavecal spe Raw profile Sk Dn Gr Ei Wavelength calibrated Pseudo continuum to be divided 4390 4480 4570 4660 4750 4840 4930 5020 5110 5200 5290 5380 5470 5560 5650 5740 5830 5920 6010 6100 6190 6280 6370 6460 6550 6640 6730 6820 6910 7000 7090 7180 7270 7360 7 5650 5740 5830 5920 6010 6100 6190 6280 6370 6460 6550 6640 6730 6820 6810 7000 7090 7180 7270 7360 7 4390 4570 4750 4840 4930 5020 5110 5200 5290 5380 5470 5560 4482 4660 YN A n WAT f A PEU MNA CL Normalization to 1 MP d A P A A huh 4 d j A h n f A Dal yj v A A A al LA Li A iV Y A M i A IW A d Waffe UU P MAPA Tu well Wm Aua AN Jk Vi l k j AM f i N E y H MN i v Y gt Final result but not corrected for the instrumental profile a Ori Betelgeuse Class M2Iab 4480 4570 4660 4750 4040 4930 5020 5110 5200 5290 5380 5470 5560 5650 5740 5830 5920 6010 6100 6190 6250 6370 6460 6550 6640 6730 6820 6010 7000 7090 7180 7270 7360 7450 99 V3 5E Bernd Koch b koch baader planetarium de 66 O 2LIT PECTRC a Stacking calibrati
26. 709 nm 712 3 nm 404 6565 nm 435 8335 nm 487 7 nm 2 e 707 nm 611 6 nm 533 45 nm 541 15 nm 546 0750 nm J 576 9610 nm f 579 0670 nm TL 580 3782 nm bs 541 eee 650 8 nm o 59 Ss nn i m DADOS 200 L mm amp EOS 450D mod Weblink to article on fluorescent substances 2003 http www electrochem org dl interface sum sum03 IF6 03 Pages48 5 1 pdf D 7 ORMALIGHT M 1 I 118 9 V3 5E Bernd Koch b koch baader planetarium de gt Stacking amp calibration of spectra obtained with a DSLR camera If you already have a DSLR camera please practice with it by recording a daylight spectrum solar spectrum G2V Cheaper than any CCD camera with a similar big sensor APS C Easier handling than a CCD camera LiveView mode for easy focusing at a bright light source e g ESL You can easily find your way through the spectrum red blue Easy identification of spectral features due to color Autodark improves SNR at the cost of exposure time Low signal to noise ratio images Low sensitivity at less than 4000A means the Ca II lines are barely visible Non modified DSLRs have low sensitivity above 6000A Stacking amp calibration of spectra obtained with a cooled b amp w CCD camera Sensitive from about 3500A Balmer Jump at 3646A to about 10000A IR High signal to noise ratio images Separate dark frames useful dark frame library
27. BAADER DA D Lj c TUTORIAL by Bernd Koch SLIT SPECTROGRAPH Ha Be Star y Cas V3 5E Bernd Koch b koch baader planetarium de X DADOS N Contents Workshop on stellar spectroscopy at the college CFG Wuppertal DADOS amp accessories DADOS layout Spectrum photography amp visual guiding Optical path Dado 1 the guiding port Slit plate mirror and slit illuminator Dado 1 Field of view at the slit viewing port Dado 1 a CMa Sirius close to 25 um Slit DMK41 video camera Dado 1 Lunar Spectroscopy The Aristarchus Plateau DMK 41 Dado 2 The blazed reflection grating Daylight spectrum of 900 lines mm grating and 1200 lines mm grating Dado 2 Grating replacement Part 1 to 4 Diffraction of light transmission Transmission grating Blazed transmission grating vs blazed reflection grating Blazed reflection grating Blazed grating theory Definition of parameters Blazed grating theory Calculation example DADOS with blazed 200 lines mm grating Energy saving lamp ORMALIGHT 9W DADOS with 200 lines mm grating Spectrum of Energy Saving Lamp ESL Ormalight 9W V3 5E Bernd Koch b koch baader planetarium de ur SrectrosrarH TUTORIAL ES 11 12 13 14 15 16 17 18 21 22 23 24 25 26 27 28 20 30 31 pr cc m A gg e See DAD C e a g T SPECTROGRAPH 9 Stacking calibration of stellar spectra 32 Stacking calib
28. Bernd Koch b koch baader planetarium de 73 JKIA ADi 0 Stacking calibration of si ellar sp ectra from anon DSLR camera d Step 7 Visual Spec VSpec Spectrum calibration by removing the instrumental profile 7 4 Press green arrow button Division and extraction Result The orange profile is the unsmoothed instrumental profile i Visual Spec File Edit Format Operations Spectrometry Radiometry Tools Assistant Window Options amp ic Elf Gd Dx isos 7536 94 1 e826 581 272 1532 A pixel AX Se pe image result wavecal spc Ele 736380 675015 613650 Instrumental response assistant EM image result wavecal spc 552285 r optional Spectral type Search spectral type on SIMBAD m Select reference spectrum 490920 Pickles C UVES Milles C Elodie Milles 2 429555 P optional shift Wavelength shift 368190 r Response Division and extraction 306825 Save Save response in file 245460 reponse 184095 mur me o H 365 A A 4570 4840 5110 5380 5650 5920 6190 6460 6730 7000 7270 V3 5E Bernd Koch b koch baader planetarium de 74 JKIA Di NES 0 y f anon DSLR camera lic la Stacking calibration of Step 7 Visual Spec VSpec Spectrum calibration by removing the instrumental profile 7 5 Smooth the instrumental profile Press button point cur
29. CAOS data Length of the spectrum y Ca x 8 mm 53 SNRcalculations amended to follow CAOS formulae 54 Bowen magnitude now based on spectrum width and units corrected http www astrosurf com buil us compute SimSpec V4 o xls V3 5E Bernd Koch b koch baader planetarium de 2Q p ann DADUS SLIT GPECTROGRAPH TUTORIAL Energy saving lamp ORMALIGHT 9W DADOS with 200 lines mm grating Ze A EN to Er WE _ E M 4 ist Order m 1 is most efficient Can be used for stellar spectroscopy from 3500 A to about 10 000 A with an ultraviolet and infrared sensitive CCD camera ist order in the infrared beyond 8500 A overlaps the 2nd order You may check this by taking the sun s spectrum daylight spectrum with your camera A DSLR camera modified with a Baader UV IR cut filter is only sensitive between roughly 4000 A and 7000 A Higher Orders than the first can be used for spectroscopy only in a smaller wavelength range But the higher spectral resolution is bought dearly due to low efficiency A grating with 900 lines mm or 1200 lines mm is recommended to achieve higher spectral resolution V3 5E Bernd Koch b koch baader planetarium de 30 DA D C 5 E Einb FSIS BOT TUTO RIAL Spectrum of Energy Saving Lamp ESL ORMALIGHT 9W Ce Tb CeMgAl 10 5 Fluorescence lines of Eu2 Y gt 03 Mercury Hg Excited by Hg UV line 254 nm Yttrium oxide doped with Europium 587 6 nm nm 631 1 nm
30. Edit Format Operations Spectrometry Radiometry Tools Assistant Window Options d a mAH nx 21827 4790 42 ka intensity m blue Sa m m 4t QC E wt Bleu 6 4 2A beta aur 03 cropped wavecal pseudocont resample spc 0 99 me 30 05 A pixel EA 2014 03 14 817 UT 4490 4520 3 beta aur 03 cropped wavecal pseudocont resample spc intensity 4550 4580 4610 4640 4670 4730 EJE Line splitting AA approximately 1 9A in the covered spectral range due to Doppler shift caused by the stars combined rotational velocity v AA A v c c 299792 5 km s average v 126 3 km s 6 2 km s V3 5E Bernd Koch b koch baader planetarium de 109 ADOS SLIT BPECTROGRAPH TUTORIAL Project Emission nebula M42 E Credit Bernd Koch DADOS 200 lines mm 0 3m Telescope Central slit 254m V3 5E Bernd Koch b koch baader planetarium de 110 pit ue EE en ge e cp DADO S suin srectrocraPH TUTORIAL amp Stacking amp full calibration of spectra taken by a STF 8300M CCD camera In an upcoming release the subject of stacking and full calibration of spectra obtained with a monochrome CCD camera will be described Stay tuned a Lyr Vega Spectral Class AoV 2013 10 22 17 40 UT Exposure time 10s with Autodark DADOS 200 lines mm SBIG STF 8300M Student astronomical observatory at Carl Fuhlrott College in Wuppertal Germany
31. LR camera Step 7 Visual Spec VSpec Spectrum calibration by removing the instrumental profile The green must be converted to a blue profile before it can be saved 7 12 Erase graphic ol gt Edit gt Replace Intensity 7 13 File gt Save as gt Betelgeuse_final_spectrum spc o Ori Betelgeuse Class M2lab V3 5E Bernd Koch b koch baader planetarium de 80 JIU A Stacking calibration of anon DSLR camera Step 7 Visual Spec VSpec Spectrum calibration by removing the instrumental profile 7 14 Use left mouse button and select area around 5500A a Ori Betelgeuse Class M2Iab V3 5E Bernd Koch b koch baader planetarium de O1 m d A Eo B Re T SPECTROGRAPH EUIVANIAL _ Stacking ca ibration of ste lar spectra from a Canon DSLR camera Step 7 Visual Spec VSpec Spectrum calibration by removing the instrumental profile 7 15 Normalize to 1 Press button vi 7 16 File gt Save as gt Betelgeuse final spectrum spc a Ori Betelgeuse Class M2Iab A A 4840 5110 5380 5650 5920 6190 6460 V3 5E Bernd Koch b koch baader planetarium de 82 Lm DADOS s rseccreossaes TUTORIAL El e Stacking calibration of stellar spectra from a Canon DSLR camera Step 7 Visual Spec VSpec Using the spectrum to estimate temperature 7 17 Calculation of the effective temperature of Betelgeuse from its spectrum We assume thermal radiat
32. Planetarium DADOS 200 L mm and CCD Camera SBIG ST 8300M Dispersion appr 2A px Identification of spectral lines amp Calibration of Xenon Spectrum 4500A 5028A Kniazev 2009 Ne Xe Plasma Tube www conrad de ce de product 591136 Magic Plasma Roehre Lichteffekt queryFromSuggest true NIST Atomic Spectra Database Lines Form Note Blended spectral lines can be resolved with a high res grating and then also be used for calibration The wavelengths of observed lines of groud state Xenon Xe I and Neon Ne I have been obtained from NIST Database http physics nist gov PhysRefData ASD lines form html Best wewed wih the latest versions of Web browsers and JavaScript enabled Title Author s Doc number Version Date ABSTRACT Keywords Approved Atlas of Reference Spectra for RSS Observations Alexei Y Kniazev SALT Ref 2252AA0001 v2 0 pdf f r Xenon 2252A A0001 2 0 July 12 2009 Reference spectra David Buckley Ast Ops Manager Date Signature In this document current version of SALT atlases of reference spectra is pre sented Spectra of Ar CuAr Ne ThAr and Xe lamps are collected and iden tified for many RSS setups For each setup the best lines are shown with their wavelengths Calulated accuraces are also shown V3 5E Bernd Koch b koch baader planetarium de OO tube from d Electronic Ne Xe Plasma Tube Conrad Electronic 4400A
33. R km it anon DSLR camera Step 5 VisualSpec VSpec Spectrum calibration without correction for the instrumental profile Betelgeuse Result image mono obt NEN Eee Create a spectrum profile gt Identify spectral lines gt Calibrate wavelength a Mrs p Py i y Fun w j bo pm P9 gen d h 4 L uer NINE B 7 V Raw profile Ae pet FE dm i T l j 4390 4480 4570 4660 4750 4840 4930 5020 5110 5200 5290 5360 5470 5560 5650 5740 5830 5920 6010 6100 6190 6280 6370 6460 6550 6640 6730 6820 6810 7000 7090 7190 7270 7360 7450 Divide a continuum O d ch was extrai yav Tom the raw profile Continuum Normalize intensity to 1 Measure Doppler shifts or Equivalent Widths EW of lines Hh i Ai iM J fu i i rh du IT MW y A m AN KG A A 4 p hl V d d 6562 3253 4061 450 5092 5209 WR 6923 64 oa Spectrum profile normalized to 1 4 4390 4480 4570 4660 4750 4640 4930 5020 5110 5200 5290 380 5470 5560 S650 5740 58630 5920 6010 6100 6190 6280 6370 6460 6550 6640 6730 6620 6910 7000 7090 7180 7270 7360 7450 V3 5 Bernd Koch b koch baader planetarium de 49 p SS gt pu Stacking calibration of stellar spectra froma Step 5 VisualSpec VSpec Preferences 5 1 5 2 Options gt Preferences gt Working directory 3_ Results Image gt fits and Profile gt spc 5 3 Preferences Open VSpec
34. Save in folder gamma Cas Expose 20 darks of same exposure time and sensor temperature Folder darks Optional Flat fields with auto darksubtraction Folder flats Dark Flat calibration with MaxIm DL stacking with FITSWORK Spectrum calibration with Visual Spec VSpec V3 5E Bernd Koch b koch baader planetarium de 101 Credit Gemini Observatory Illustration by Jon Lomberg b 7 e A E O Spectroscopy of Be star y Cas gt Celestron u DADOS 900 200 lines mm EOS 450D ISO 800 Autodark Pentax 75 2x Converter DADOS 900 200 lines mm EOS 450D ISO 800 Spectrum recording amp video camera guiding MaxIm DL Win XP 7 32 bit tested The slit s length should be parallel to Deklination 8 direction Center spectrum on Ha or Hp by turning the micrometer adjustment Keep exposure time well below saturation of sensor 1s to about 60s Guiding Video camera Skyris 274M TIS DMK 41 or else Number of images per spectrum Minimum 20 Save in folder gamma Cas Stacking with FITSWORK Spectrum calibration with Visual Spec VSpec V3 5E Bernd Koch b koch baader planetarium de 102 VV VV VV WV Credit Gemini Observatory Illustration by Jon Lomberg w Non linear calibration KL as r Liste de raies wi al lambda rae _ pixel 1 d_lambda M76 Ce 310 0547 0 0835 E 549386 2 32712 01201 IN 6517 1 3 357 2144 0 0488 r Delta Lond 6586 596 4 466 1803
35. Spectra Database 2 1 www conrad de ce de product 591136 Magic Plasma Roehre Lichteffekt queryFromSuggest true 2 http physics nist gov PhysRefData ASD lines form html Bernd Koch 2013 09 16 V TE d di NJ ech N n W M IP I 3 9x V3 5E Bernd Koch b koch baader planetarium de 97 DADOS sur srecreocesrn TUTORIAL E TT OrlzuL L e C hASn LDDLDLDP E e _ Re Em TN E EE nova del 2013 9x120s spektralfaden 16bit stretched wavecal continuum spc P Cygni Profile 2013 08 19 20 01 UT 20 33 UT Mid exposure August 19 84722 UT DADOS 200 lines mm Stacking FITSWORK with 9 x 120s Calibration VisualSpec Ha The expansion velocity v of the nova s envelope is calculated by the P Cygni profile method measured at Ha A km E De 1005 p AA 22 0 Ay 6562 82 cy 299792 22 n 22 0A S Absorption Emission Ref www ursusmajor ch downloads analysis and interpretation of astronomical sp pdf V3 5E Bernd Koch b koch baader planetarium de _ DADOS sur srectrocraeH TUTORIAL _ E NS er m Re MH TN E EE nova del 2013 9x120s spektralfaden 16bit stretched wavecal continuum spc P Cygni Profile M xi 2013 08 19 20 01 UT 20 33 UT Mid exposure August 19 84722 UT DADOS 200 lines mm Stacking FITSWORK with 9 x 120s Calibration VisualSpec Efi The expansion velocity v of the nova s envelope can
36. a Paper by students Tom Schnee and Johannes Schnepp CFG Wuppertal 2012 V3 5E Bernd Koch b koch baader planetarium de 83 Calibration spectra with a Ne Xe plasma um T E cto ur Student astronomical observatory at CFG College in Wuppertal Germany T Ek th Pi B e E 4 py X s rm de Ki De UY Gel un Wei ie m A SS T ege ue Pos ectronic Ne 5852 4878 onra ectronic E S Ne 5881 8950 e 6 k N Ne 5944 8340 Z Pa Ne 5975 5343 Xe 8231 6336 Xe 8280 1162 E asma tude e e Ne 6029 9968 e e Ne 6074 3376 Ne 7032 41 Ne 6096 1630 S Xe 4500 978 Ne 6143 0627 g Xe 4524 6805 RRS cmd Xe 6182 420 C Xe 4582 7472 manc Xe 4624 2756 He 62604934 Ne 6304 7893 Xe 4671 2258 Xe 6318 062 Blend Xe 4690 970 Xe 4697 0208 Ne 6334 4276 E y npe Ne 6382 9914 pe Xe 4792 619 Xe 4807 0190 Xe 6469 705 Ne 7173 9380 p Xe 4829 708 Ne 6506 5277 S Ne 6532 8824 Xe 4843 2934 NA Xe 8346 8217 Ei e Ne 7245 1665 Xe 8409 1894 Ne 6678 2766 Xe 7284 34 e le Ne 6717 0430 Xe 7393 793 Xe 7386 003 i Xe 6827 315 Ne 7438 8970 Blend Xe 4916 51 Xe 4923 152 l Xe 7967 342 d Xe 6882 15 Ne 7488 8712 Xe 5028 2794 Ne 6929 4672 Ne 7535 7738 Xe 6976 182 Xe 7642 024 Ne 5400 5616 8200 8400 8800 8900 4400 4500 4600 4700 4800 4900 5000 5100 5200 5300 5400 S500 S600 5700 5800 5900 6000 6100 6200 6300 6400 6500 6600 6700 6800 6900 7000 7100 7200 7300 7400 7500 7600 7700 7800 Spectrograph Baader
37. aader planetarium de 62 p Em Stacking calibration of stellar spectra from a Canon DSLR camera Step 5 Visual Spec VSpec The normalized profile of Betelgeuse 5 19 Edit Replace Intensity 5 20 Save as gt Result image wavecal normalized spc 273540 a Ori Betelgeuse Class M2lab 250745 279560 nhs 5S WP 36D 15956p 136770 113975 91180 68385 45590 22795 N A V3 5E Bernd Koch b koch baader planetarium de 62 4570 4840 5110 5380 5650 5920 6190 6460 6730 7000 7270 RIZ 48116 wm ECTRO EH Stacking calibration of stellar spectra from a Canon DSLR camera Step 5 Visual Spec VSpec The normalized profile of Betelgeuse CC amp 8 5 21 Indicate middle area with left mouse button to become 1 in intensity 5 22 Press button Normalize A 273540 a Ori Betelgeuse Class M2Iab 250745 15956p 136770 113975 91180 68385 45590 22795 N A 4570 4840 5110 5380 5650 5920 6190 6460 6730 7000 7270 V3 5E Bernd Koch b koch baader planetarium de 64 SC Stacking calibration of stellar spectra from a Canon DSLR camera Step 5 Visual Spec VSpec The normalized profile of Betelgeuse 5 23 Result Wavelength calibrated and intensity normalized profile of Betelgeuse 5 24 Save as Result image wavecal normalized to 1 spc a Ori Betelgeuse Class M2Iab O 4570 48
38. ake allowed adjustments focusing for example Less force means less jiggling and thus easier observation 2 This equipment is expensive in the thousands of dollars Treat it carefully and don t horse around near it 3 Minor accidents do happen should you bump something let the docent know so he can get the observed object back in view 4 Dont touch any of the glass optics with your hands This can damage the optical coatings Please ENJOY YOUR OBSERVATIONS and ASK LOTS OF QUESTIONS about anything you don t understand or about which you wish to know more e V3 5E Bernd Koch b koch baader planetarium de 115 ZS DADOS sursrecersossae TUTORIAL E LL Disclaimer TIS While the methods shown in this tutorial work well they assume an underlying knowledge of astrophotography not covered here The user must be able to specify purchase operate and maintain appropriate equipment for the task at hand optical tube assemblies eyepieces equatorial mounts autoguiding equipment cameras spectroscopes computers image processing software and astronomical accessories The user must know skills such as cleaning and collimation of optics physical balancing of the system polar alignment setting periodic error correction and gear backlash for the mount in use dew control navigating across the sky operation of a computer and its programs to collect and reduce data etc The equipment used in this tutorial is expensive well over ten t
39. ckground Flatten Shift Image k Imagesize x2 hi f tri Video d Imagesize x2 hi f tri Backpropagation El Bayer Interpolation j Imagesize x2 hi f sinc Special Filter d Imagesize x2 NN directdial FW FFT K i Imagesize x2 Neuronal Network dass gina xm Train Neuronal Network for Resizing Expand Image to RGB V3 5E Bernd Koch b koch baader planetarium de 44 DADOS sur srectracraey TUTORIAL Si EE e mg Deg P zee Been spectra from a Canon DSLR camera Step 4 Fitswork Rotate Result image fit 2 perfectly leveled spectrum e Please mark a line exactly along the spectrum with the left mouse button e then gt Ok gt Whole Image i Please mark an oblique Line then click Ok V3 5E Bernd Koch b koch baader planetarium de 45 DA DOS sut Srectrocrary TUTO RIAL E El te ccc mmm Stacking calibration of stellar spectra froma Canon DSLR camera Step 4 Fitswork Crop amp save Result image colour 1 amp bit fit gt Draw a yellow frame around the spectrum gt Cut off gt Save as Result image color pb fr V3 5E Bernd Koch b koch baader planetarium de 46 DADOS SLIT BPECTROGRAPH TUTORIAL ee Se Stacking calibration of stellar spectra from a Canon DSLR camera Step 4 Fitswork Convert to black amp white image and save Processing gt Color image to b w luminance File Processing Image Combining Set
40. diffracted zeroth order gt A blazed transmission grating will improve things V3 5E Bernd Koch b koch baader planetarium de 25 ORIAL ES lazed reflection grating SpectrocraPH TU e SES VS Although in some cases transmission gratings are applicable or even desirable they are not often used Reflection gratings are much more prevalent in spectroscopic and laser systems due primarily to the following advantages Reflection gratings can be used in spectral regions where glass substrates and resins absorb light e g the ultraviolet erating normal incident ligh Reflection gratings provide much higher resolving power than equivalent transmission gratings since the path difference between neighboring beams Le separated by a single groove is aS Rx higher in the case of the reflection CONS grating Therefore transmission gratings must be wider so that more grooves are illuminated to obtain comparable resolving power fas diffracted light Figure 12 1 Diffraction by a plane transmission grating A beam of Reflection grating systems are generally monochromatic light of wavelength is incident on a grating at angle a to the IIS grating normal and diffracted along several discrete paths bm for diffraction smaller than transmission grating orders m The incident and diffracted rays lies on opposite sides ofthe grating systems because the reflection erating The con
41. e and VisualSpec software Image processing amp spectrum calibration Bernd Koch V3 5E Bernd Koch b koch baader planetarium de 104 DADOS 1200 lines mm SBIG ST 8300M 1 x1 Binning Ne I 6506 5277A Ne I 6532 8824A e Ha intensity in the red R and violet wing V of the Ha line 6402248 1 1276519 0 6506 528 2 1503454 6532882 3 156068 6598 953 4 1703 958 6717 043 5 1858568 Spectrum calibration VisualSpec RMS 005355 Delta Lambda Degre Dege 1 Degre 2 e Degre 3 Dege 4 Date 2014 03 10 JD 2456727 386 Spectral resolution 1 5A Radial velocity v 30 9 km s EW 3 9A 6540A 6590A V R 1 00 by Bernd Koch and Ernst Pollmann V3 5E Bernd Koch b koch baader planetarium de 105 by Jon Lomberg Credit Gemini Observatory Poll 1072000 0372001 B Poll 12 2001 0472002 A Poll 0142003 0472003 Poll 08 2004 047 2005 Poll 08 2005 04 2006 x Stober o Bjorkman et al 2000 E Buil 4 Ondrejov V to R mo nito rng Heidelberg 9 Kalbermatten Bucke A Thizy o Desnouz 4 Mauclaire 0 Schanne D Dubs Garrel Poll 08 2007 0472014 9 Sawicki Guarro d o Gorodenski x Koch E Ha V R Credit Ernst Pollmann 48000 50000 52000 54000 26000 JD 2400000 Multi epoch Near Infrared Interferometry of the Spatially Resolved Disk Around the Be Star Tau Schaefer et al http arxiv org abs 1009 5425 V3 5E Bernd Koch b koch baader
42. ernd Koch DADOS Spectrograph s user manual Richard Walker s astronomical spectroscopy spectroscopic Atlas 4 0 11487 KB Practical Aspects of Astronomical spectroscopy 2 0 4209 KB Analysis and Interpretation of Astronomical Spectra 9 1 5330 KB The Spectrum of Quasar 3c275 1 2 745 KB Atomic Emission Spectroscopy 2 0 F963 KB SQUES RELCO SC480 Calibration Lines 2 0 2210 KB V3 5E Bernd Koch b koch baader planetarium de 115 as DADOS sur srectrocraeH TUTORIAL E a ss f __ ae ZS Ra e References amp recommended reading by Matthew Buynoski Introduction to Astronomical Spectroscopy by Immo Appenzeller ISBN 978 1 107 60179 6 Wonderful little book by a master of the art of spectroscopy and contains interesting topics atmospheric dispersion compensators volume phase gratings etc Observation and Analysis of Stellar Photospheres by David Gray ISBN 978 0 521 06681 5 Parts of this book are highly technical and suitable only for those with physical science degrees but other portions of it describing equipment and how it works e g detectors spectroscopes telescopes are suitable by everyone Dr Gray is also a master of the art of spectroscopy Stars and Their Spectra by James Kaler ISBN 0 521 30494 6 This book is a good introduction to stars and what their spectra reveal about them It is not too technical and suitable for any amateur astronomer Dr Kaler is
43. f Vienna Austria who attended our October 21 25 2013 workshop all pages in German http www waa at bericht 2013 10 20131021sfloo html http www waa at bericht 2013 10 20131022sf117 html If you are interested in a workshop please have a look at our website www schuelerlabor astronomie de or contact Mr Michael Winkhaus head of the observatory Michael Winkhausqt online de Please address inquiries about the DADOS spectrograph directly Mr Bernd Koch b koch baader planetarium de Bernd Koch 4 V3 5E Bernd Koch b koch baader planetarium de A LEAL UO sLr SPECTROGRAPH TUTORIAL m Workshop on cies spectroscopy at the college CFG Wuppertal Guiding Pentax 75 SDHF Camera cae ih DADOS m d EdgeH 3 Magi Interested in a workshop Please contact Michael Winkhaus Workshop April 2011 V3 5E Bernd Koch b koch baader planetarium de 5 DADOS Spektrograph DADOS Spectrograph 2456313 T2 Quick changer 42456320 T2 Quick change ring 2458556 Blaze reflection m E grating 900 lines mm i gt 1 2958027 Canon T2 Ring umma j 11A 2 Stop Ring 1304110 Kellner 10 mm f S suiding eyepiece idi 3 a Slit Viewer 1304120 Kellner 20mm yl positioning eyepiece p e AX User s Manual BE D EL ES 2458550 DADOS slit spectrograph 2458590 Neon di calibrat
44. figuration shown in which the transmission grating is illuminated from the back is most common acts as a folding mirror http gratings newport com information handbook chapteri2 asp 12 2 V3 5E Bernd Koch b koch baader planetarium de 24 First order Intensity Zero order First order Second order Third order First Order Advantages The highest efficiency is in first order with the correct blaze angle gt The reflectivity is higher than the throughput of a blazed transmission grating V3 5E Bernd Koch b koch baader planetarium de 25 1 C K OP LS Pe aa Uo i N SOS a Ml Q be Wm n w Q Wm 5 R8mRR8 Th HH V3 5E Bernd Koch b koch baader planetarium de GN Grating normal FN Face normal g Groove spacing 9 Blaze angle a Angle of the incident light p Angle of reflected light 26 GN Grating normal FN Face normal g Groove spacing A gt 9 Blaze angle TM Mh Mh SS Ml Ba Ml Sa Ml Dia D Ml Ml Ml Ml MM Ml MM 077 lt meta Eid EE ee d a Angle of the incident light p Angle of reflected light ils ie Sa Mi us Ba S S2 Additive interference occurs when the total path difference A of light from adjacent slits S1 and S2 is an integer multiple of the wavelength A The phase is then the same so the beams intensity add Path difference of incident beam
45. g At any given point in space through which diffracted light may pass the path length to each slit in the grating will vary So will the phases of the waves at that point from each of the slits and thus will add or subtract from one another to create peaks and valleys through the phenomenon of additive and destructive interference When the path difference between the light from adjacent slits is equal to half the wavelength A 2 the waves will all be out of phase and thus will cancel each other to create points of minimum intensity Similarly when the path difference is A the phases will add together and maxima will occur Reference http en wikipedia org wiki Diffraction grating Grating a E Ic E i TS B _ I CR sin A CES 7 sin f Z l T sin p Diffraction term Interference term of a slingle slit width b of N slits at distance d Diffraction Interference pattern Reference Nos Monochromatoren d BAneu doc 2 21 V3 5E Bernd Koch b koch baader planetarium de 22 _ MSS _ lt m BEE Ee First order Zero order First order Second order Third order YA DOS sur seecrroceapH TUTORIAL E Intensity Maximum intensity in zero order Disadvantages of a transmission grating gt Light is dispersed among the various diffraction orders leading to low intensity in the higher ones Transmission losses are due to selective absorption in the glass Maximum intensity is the un
46. g on the Vernier scale Use the 1 5mm Allen wrench to remove the four hex head screws V3 5E Bernd Koch b koch baader planetarium de Take off the side plate grating holder assembly Be careful not to touch the grating Release the headless set screw inside of the pressure plate by 2 full turns counterclockwise using the 1 5mm Allen wrench Remove the grating holder from the pressure plate Take the 900 lines mm grating holder out of the storage container and store the 200 lines mm grating in it 39 19 40 Place the 900 lines mm grating holder into the pressure plate Rotate the grating holder to adjust the proper position in regard to the markings in the pressure plate Each mark indicates the position of a specific grating Be sure to use the proper one to achieve the optimal throughput Example of position 200 lines mm grating V3 5E Bernd Koch b koch baader planetarium de Example of position 900 lines mm grating Lock the pressure plate by tightening the headless set screw clockwise Carefully replace the side plate grating holder assembly Replace and tighten the 4 screws that secure the side plate 41 2O De E _ So C dn a SW J TI Adjust the micrometer to a Vernier position of approximately 2 5 Lock the grating tilt mechanism by rotating the grating angle locking screw clockwise DADOS wi
47. ge frame SNR Calculations Number of photons E 1 63E 02 photons cm2 s Sky background Ed 4 09E 04 photons cm2 s arc sec Final Efficiency R 0 12 96 Useful signal Nm 8856 e pixel Background noise Ns 131 e pixel Noise c 237 e Signal Noise by interval AA 96 e pixel Noise from Signal Noise from Electronics 216 e pixel Angle of incidence a Angle of reflected light B 40 78 Anamorphic factor SY 3 x o diffraction limit grating FWHMd Dispersion 2 05 A px Siit image width on CCD FWHMt Spectral resolution 13 62 A at 5200 A Resolving power 382 Transmission efficiency guide system Transmission efficiency Littrow mirror Transmission efficiency Collimator lens To Transmission efficiency Camera lens Tc Transmission efficiency Grating Tg Entrance slit transmission Tf otal Transmission of Spe S T O O 1 47 V4 0 April 2012 New layout Added Data Page Updated comments Blaze angle p c 4 2 2 E 4 1 3 48 V3 3a Jan 2012 Collimator focal ratio set to match telescope Camera focal ratio no longer an input S S x o 49 V3 3 May 2011 Corrections to the equation for FWHMt incorrectly calculated for slit lt star Linear dispersion 394 37 A mm 50 V3 2c Oct 2010 Slit width now in micron 51 V3 2b July 2010 Transmission efficiencies added for guider and Littrow mirror e 52 V3 2a April 2010 Fixed slit width v s star size for resolution calculation Based on
48. he spectrum profile 5 5 Press z to display pixel positions and intensity The result is a spectrum profile with x y pixel positions intensity Tilt Spectrum is not perfectly leveled angle 0 01 so the spectral lines are not perfectly perpendicular This has no measurable effect on the calibration 5 6 Save Result image 16bit spc Due to a different stacking procedure and color conversion the spectrum intensities on the following pages differ somehow This has no effect on the final profile as it is being calibrated continuum removed or instrumental profile used Result_image_mono_16bit spc 173985 115990 aye n e lt ES Pixel 100 200 300 400 500 600 700 DUU DUU 1000 1100 1200 E 300 1400 1500 V3 5E Bernd Koch b koch baader planetarium de 52 e LIT Fm Stacking calibration of stellar spectra from a Canon D camera Step 5 Visual Spec VSpec Identification of spectral features 5 7 Print the raw profile and note the wavelengths of precisely known spectral lines of a star of similar class 207360 194400 181440 F 168480 142560 129600 116640 103680 L90720 L 77760 54800 51840 38880 25920 12960 a Ori Betelgeuse Class M2lab 5371 49 Fe 5125 5270 Fely Fel Cri
49. housand US per student set up Expect that equipment of similar value must be used in order to achieve good results All that said please accept our best wishes for your success in astrospectroscopy The author thanks Michael Winkhaus head of the Student Astronomical Observatory of the college Carl Fuhlrott Gymnasium in Wuppertal Germany for the opportunity to give workshops in astronomy astrophotography and astrospectroscopy These workshops are held in collaboration with Ernst Pollmann of Leverkusen Ernst is the head of Active Spectroscopy in Astronomy ASPA http www astrospectroscopy de and well known for his expertise in high resolution stellar spectroscopy The author thanks Matthew Buynoski buynoski batnet com who does visual spectroscopy for presentation to schoolchildren for his helpful review and proofreading of this tutorial COPYRIGHT NOTICE This document is proprietary and for use of the intended recipient only Baader Planetarium GMBH reserves all rights Certain parts of this document were contributed and are also copyrighted by one or more of the following authors Baader Planetarium Bernd Koch Michael Winkhaus Ernst Pollman Matthew Buynoski All information contained in this document is subject to Baader Planetariums s copyright Permission is granted for educators in astronomy and astrophysics to make this tutorial available to their students for no more than the direct cost of making the copies to hand out Permis
50. ight 7 10 Operations gt Divide profile by profile Select intensity below response spc Lei SS P 1 Li IRE 276 4894 99 I 104330 683 2 1532 Mbixel Fee amp m blue BR an op m Ai Q MERO eZ SO lat d sss us qp ox i A d Kai t i v a PN ae VM y d S m KE w Selection ivision image result wavecal spc intBysityresponse spc intensity Infos 2 153177 A pixel de 4302 87 7541 25 Normalize and replace EbG 7 amp crE is EEE C i oN o Ay V3 5E Bernd Koch b koch baader planetarium de 79 Stacking calibration of stellar spectra from a Canon D camera Step 7 Visual Spec VSpec Spectrum calibration by removing the instrumental profile Result The green profile is the calibrated true spectrum profile of Betelgeuse corrected for instrumental profile 7 11 Close response spc File Edit Format Operations Spectrometry Radiometry Tools Assistant Window Options ic E Ed Dx 276 4894 59 I f104930 683 2 1532 A pixel s Division amp m greenF SE p pi HER RUAK Ae 2 se at X Hz RE dq ve N I image_result_wavecal spc Secs Tm V3 5E Bernd Koch b koch baader planetarium de 79 Fa lt gt DES ek D IBiG kLE o 1 4 1 SE 29PECTFE JAPH EX JRIAL G z Stacking calibration of stellar spectra from a Canon DS
51. inuum extraction from the raw profile 5 13 Edit Replace Intensity at Operations Spectrometry Radiometry Tools Assistant Window Options iN t Edit Pi ej i pee 1498 7526 17 I 2 1532 A pixel Paste Ctrl V ring Jee Soles J F n sa m HAAA wt 2 oe lat v AE cp Clear Maj Del Pixel ce 1 line T Header Ctrl 4H N V3 5E Bernd Koch b koch baader planetarium de 58 ORIA mESIT m 5 R camera Bone Step 5 Visual Spec VSpec Continuum extraction from the raw profile 5 14 Save as gt Continuum spc 208680 191290 173900 156510 139120 121730 104340 86950 69560 52170 34780 17390 4570 4840 5110 5380 5650 5920 6190 6460 6730 7000 7270 V3 5E Bernd Koch b koch baader planetarium de 59 Ee gece EK mem lt T pit ccu a Stacking calibration of stellar spectra from a Canon DSLR camera Step 5 Visual Spec VSpec Continuum division 5 15 File gt Open profile gt Continuum spc and Result image wavecal spc 5 16 Highlight the window Result image wavecal spc image result wavecal spc Y A Le b V3 5E Bernd Koch b koch baader planetarium de 60 Jm um gt A ORIA ON Stacking calibration of anon DSLR camera Step 5 Visual Spec VSpec Pda division 5 17 Operations gt Divide profile by profile gt Click on continuum spc gt intensity i
52. ion lamp 2452110 Carrying case for DADOS and accessories V3 5E Bernd MeN cord NO y re augeetel tarium de 6 1 2 3 4 5 6 7 8 9 10 11 12 13 14 2 Nosepiece gt Telescope Adjustable red LED slit illuminator incl two 1 5V LR 41 batteries c 114 Slit viewer port for guiding eyepiece 11 or camera e CN i 114 Stop ring for guiding eyepiece 11 or camera Micrometer adjustment for scanning the spectrum 1 LE a N Rotation stage counter spring do not touch Focuser Focuser locking screws Grating angle locking screw Optional goo lines mm grating Guiding eyepiece for viewing the spectrograph s slit Quick changer optional but not for DSLR i Focusing eyepiece holder T2 gt 11 4 10 mm or 20 mm Kellner eyepieces for viewing a spectrum V3 5E Bernd Koch b koch baader planetarium de 7 Adjustable red LED slit El dado1 illuminator slit plate 2 Nosepiece gt Telescope Ss a Slit viewer b N F A assembly S p J k j e El E 22 dps Focuser Grating angle locking screw pl ase loosen this screw before urning the micrometer adjustment sch Micrometer adjustment Guiding eyepiece spectrum scanning to keep object on slit ICH V3 5E Bernd Koch b koch baader planetarium de Collimator P e 7 s DLL ant uid Grating Slit Des Mirror Objective
53. ion of a black body according to Planck s Law Radiometry gt Auto Planck black line A Planck spectrum with Tef f 3000K best fit is fitted by VSpec gt mas xl a NN RENT 800 z E 3 a Ori Betelgeuse Class M2lab D d z E E z lt 400 B 5 e E S 200 T 4000K E E E CMS E 0 e 0 500 1000 1500 2000 nm V3 5E Bernd Koch b koch baader planetarium de 83 PECTRO JTORIAL E ilar spectra from a Canon DSLR camera Stacking calibration of Step 7 Visual Spec VSpec Using the spectrum to estimate temperature 7 18 Wien s law 99000 1034 K max Toff max Wavelength of the maximum of the assumed black body emission Teff Effective Temperature K o Ori Betelgeuse Class M2lab VSpec result T 3000K black line gt Amax 9700A 7 officially adopted value T ff 3450K Iw o e e JI e e ui 4 k nm 200 0 500 1000 1500 2000 A nm V3 5E Bernd Koch b koch baader planetarium de 84 E i w A ed Stacking calibration C f oi ellar sp ectra fr om anon DSLR camera d Step 8 Visual Spec VSpec Visualize profile as synthetic profile 8 1 Synthese sic gt Creates a synthetic black amp white spectrum glia eS E nox TU 4302 ka 32 1532 Avpixe1 03 5543 1 43 06 intensi uem erus EIEBPPIEFTYT WA E SE uelut ses Ve EI do betelgeuse_final_s
54. lution of Collimation lens FWHMo Dark noise Nd Telescope focal length 2800 mm Keesen Ee 2 E e B 12 Camera Focal length 12 Binning Y axis fy Grating groove density 200 lines mm 13 Camera Distance to grating T i 14 Atmospheric transmission Ta Camera Minimum lens diameter d 2 E 1 15 Sky magnitude mag arc sec 2 Camera Maximum focal ratio Fo Subs exposure time ts Gro ove Sp acing g mm 16 Star size at focus FWHM Resolution of Camera lens FWHMc number of subframes n 200 17 Total exposure time t 3600 d Oo 18 Collimator Camera Total angle y B Total deflection angle a 6 90 19 NOTES microns h o 20 See www astrosurf org buil us spe2 hresol htm Grating e E 21 www astrosurf org buillus stage calcul design us bim Grating Lines mm n Centra wave engt A 5 2 0 nm 5 2 0 0 A 22 lanatory notes and worked example Grating Diffraction order k Magnitude m Grating Minimum height H Effective temperature Te Diffraction order m 1 Grating Minimum width W Bolometric Correction BC e e Dispersion p i SNR Slit width 25 um Resolving power R Spectral resolution AA Limiting Mag Limiting Mag Bowen mod 15 36 Dispersion r Camera Canon EOS 450D SimSpec Results e 3g Angle of incident light 49 22 Wavelength Range Reference wavelength 7 0 EOS 450D 185 19 px mm Lambda min 7 1 Lambda max 72 gth range ima
55. on of stellar spectra from a Canon DSLR camera Step 6 Visual Spec VSpec Visualize profile as nade profile 6 1 Tools gt Synthese sic Creates a synthetic black amp white spectrum me nsity gt amp m bue eS See err ere SF d image_result_wavecal_normalized to 1 spc o Ori Betelgeuse Class M2Iab r A DER 4570 4840 5110 5380 5650 5920 6190 6460 6730 7000 7270 IINE IE 5 1l V3 5E Bernd Koch b koch baader planetarium de 67 SF pectTRoGRAPH TU OTR DRLAL E Stacking calibration of stellar RES rom a Canon DSLR camera Step 6 Visual Spec VSpec Visualize profile as synthetic profile 6 2 Synthese sic Colorer sic creates a colored synthetic spectrum a Ori Betelgeuse Class M2Iab HD Mg Triplet Na D Ha V A V3 5E Bernd Koch b koch baader planetarium de 68 asp T ay DADOS s rseecreossae TUTORIAL E3 Stacking calibration of stellar spectra from a Canon DSLR camera Comparison of spectral resolution of Betelgeuse spectra DADOS 200 lines mm and 9oo lines mm ni Mg pret Na P 200 lines mm 5890 5896A 900 lines mm Na D well resolved V3 5E Bernd Koch b koch baader planetarium de 69 p sy JI Pi C e pE gp Be E oe e TI ng BEL ADOS s TUTORIAL E anon DSLR camera Step 7 Visual Spec VSpec Spectrum calibration by removing the instrumental profile Betelgeuse Result Image mono
56. pectrum s S o Ori Betelgeuse Class M2lab 4570 4840 5110 5380 5650 5920 6190 6460 6730 7000 7270 sf betelgeuse final spectrum spc intensity V3 5E Bernd Koch b koch baader planetarium de 95 ee Stacking cali Step 8 Visual Spec VSpec Visualize profile as synthetic profile 8 2 Synthese sic gt Colorer sic gt Creates a synthetic color spectrum for presentation 32 1532 A pixel T ssoo 5 1043 SD eb betelgeuse_final_spectrum spc a Ori Betelgeuse Class M2Iab 4570 5650 5920 a betelgeuse final spectrum spc intensity V3 5E Bernd Koch b koch baader planetarium de 86 L SPECTROGRAPH T yu ORIAL E ee ee spectrum A A 4400 4600 4800 5000 5200 5400 5600 5800 6000 6200 6400 6600 A EOS 450D Baader BCF filter 1 5 1 25 1 00 0 75 0 5 0 25 0 00 eme Hy HB Mg I Fe I Mg I Na I Cal Telluric O o 4340 47 Fe I 4861 33 5167 32 5328 00 5528 40 5889 95 6102 72 2 6562 82 Das Sonnenspektrum 4688 00 Jl Fe I Mg I Na I 4957 60 5172 68 5895 92 Mg I 5183 60 Projektarbeit in Astronomie 4400 4600 4800 5000 5200 5400 5600 5800 6000 6200 6400 6600 DADOS 900 lines mm and DSLR camera Canon EOS 450Da BCF Paper by Tom Schnee and Johannes Schnepp CFG Wuppertal 2012 V3 5E Bernd Koch b koch baader planetarium de 37 1 5 1 4 1 3 1 2 1 1 1 0 0 9 og 0 7 0 6 0 5 0 4 0 3 0 2 0 1 0 0 W ge T ell
57. ration of stellar spectra from a Canon DSLR camera 33 86 The solar spectrum 87 88 Calibration of Spectra with a Ne Xe Plasma Tube from Conrad Electronic 89 92 Nova Delphini 2013 93 100 Spectrum of Be star y Cas 101 103 Spectrum of Be star C zeta Tau 104 107 Spectroscopic binary star B Aur 108 109 Emission nebula M42 110 Stacking amp full calibration of spectra taken by a STF 8300M CCD camera 111 112 References amp recommended reading 113 114 Safety and other rules 115 Disclaimer 116 V3 5E Bernd Koch b koch baader planetarium de AD m FI aimant TORIAL E i RSR spec py at the cc FG Wuppertal The student astronomical observatory on the roof of the college Carl Fuhlrott Gymnasium in Wuppertal Germany is well equipped with six identical telescope units We provide astronomy and astrophysics education for larger groups of students from other colleges and the nearby Bergische Universitaet Wuppertal Equipment Astro Physics 900GTO mount Celestron u EdgeHD telescope Pentax 75 SDHF refractor Celestron ED 80 600mm refractor Canon EOS 450D DSLR camera SBIG STF 8300M CCD camera and lot of accessories Special workshops on the topic of stellar spectroscopy are held with six units of the DADOS spectrograph Gratings with 200 900 1200 lines mm are available as well as spectral calibration lamps Tutors Michael Winkhaus Bernd Koch and Ernst Pollmann Please look at the report of Dr Thomas Schroefl o
58. rmany V3 5E Bernd Koch b koch baader planetarium de 94 DADOS sucv srectrocrary TUTORIAL ES Nova Delphini 2013 2013 09 05 9 UT Spectrum DADOS 200 lines mm amp SBIG ST 8300M CCD camera 0 3m Telescope V3 5E Bernd Koch b koch baader planetarium de 95 DADOS sur srecreocraen TUTORIAL Ez3i Nova Delphini 2013 2013 09 05 9 UT Calibration with a Ne Xe plasma tube from Conrad Electronic Spectrum DADOS 200 lines mm amp SBIG ST 8300M CCD camera 0 3m Telescope Ne Xe plasma tube in front of the telescope and spectrum superimposed during exposure Note the changes in spectral resolution due to the different slit widths V3 5E Bernd Koch b koch baader planetarium de 96 e DAD C c3 SLIT SPECTROGRAPH TUTORIAL SE 7 Nova Delphini 2013 09 05 88785 UT Calibration with a Ne Xe plasma tube from Conrad Electronic I 1743890 Xe18862 32 mS Xe 18930 83 REEL 14671 2258 Ne 15852 49 Nei enen Ne 1 6678 28 Ne1 7032 41 Ne17245 17 Ne Xe 19799 697 Xe 19923 198 Xe 1 7642 02 17967 342 Xe 18206 336 Xe I 8231 6336 Xe 18280 1162 Xe 18819 4106 if Xe 18952 2509 Xe 1 8346 8217 Xe 1 8409 1894 111742 236 Xe X Xe Kalibrierung mit Ne Xe Plasmarohre 1 und NIST Atomic
59. sion is also granted to each individual astronomer student amateur or professional to make and keep one copy for his or her personal use Any unauthorized copying any publishing of it s content in the internet or intranet any use of this information by third parties and or its dissemination to third parties without the expressed written consent of Baader Planetarium GMBH is a serious infringement Under international copyright laws any reproduction or dissemination of this document by the recipient is expressly prohibited Any transfer of this document in original or copied form to competitors or other third parties violates applicable public copyright laws Violations of copyright or public procurement laws will be prosecuted under the law Baader Planetarium GMBH 2014 V3 5E Bernd Koch b koch baader planetarium de 116
60. tep 3 Fitswork The stacking process Create an averaged color spectrum Dataset Betelgeuse_200L_2010 12 15 2_Spectra_raw_images_CR2 File gt Batch Processing Fitswork Settings Window Help Batch Processing amp IF Image Registration Make User Raw Format Last Processings Exit Program V3 5E Bernd Koch b koch baader planetarium de 40 Stacking calibration of stellar S ctra from from a Canon DSLR camera Step 3 Fitswork The stacking process Create an averaged color spectrum Dataset Betelgeuse_200L_2010 12 15 2_Spectra_raw_images_CR2 1 Step of Processing sic 1 File gt Select first raw image file 2 All files in folder 3 Press right arrow button to proceed ffnen Batch Processing ES fe 1 Step of Processing specity Files 1 SPECIFY FILES Start File Destination File Suchenin TE 2 Speldra raw magesCR2 s f pk Ede All Files in Folder eee i E A Gr e Typ 2145 x 1428 Pixel Iw Start File Ed 11 278KB Maxim DL Image m 11 277KB Maxim DL Image Destination File lem 2 3 C e All Files in Folder 5 ka 11 269KB Maxim DL Image CU 2 11 267KB Maxim DL Image 11 274KB Maxim DL Image 11 279KB Maxim DL Image A s Er 11 276 KB Maxim DL Image 11 278KB Maxim DL Image 11 266KB Maxim DL Image 11 273KB Maxim DL Image 11 278KB Maxim DL Image h SEM EN ries Hom seres Stark Cancel V3 5E
61. th grating exchanged Copyright DADOS Spectrograph s User s Manual by Baader Planetarium GmbH V3 5E Bernd Koch b koch baader planetarium de 21 141114114 action ote t transmission Single Slit Diffraction Diffraction is described by the Huygens Fresnel principle and the principle of superposition of waves The propagation of a wave can be visualized by considering every point on a wavefront as a point source for a secondary spherical wave The wave displacement at any subsequent point is the sum of these secondary waves When waves are added together their sum is determined by the relative phases as well as the amplitudes of the individual waves so that the summed amplitude of the waves can have any value between zero and the sum of the individual amplitudes Hence diffraction patterns usually have a series of maxima and minima Reference http en wikipedia org wiki Diffraction Single slit_diffraction TH cos i 04 0b V o ee Diffraction grating An idealized grating is made up of a set of slits of spacing d that must be wider than the wavelength to cause diffraction When a plane wave of wavelength A with normal incidence perpendicular to the grating each slit in the grating acts as a quasi point source from which light propagates in all directions After light interacts with the grating the diffracted light is composed of the sum of interfering wave components emanating from each slit in the gratin
62. ting of 900 lines mm Theoretical Measured A nm 2038 2000 371 3910 3000 561 5376 5000 800 Limiting magnitude for a 30 cm telescope with S N 50 and 20 minutes of exposure time For the 200 lines mm grating m 8 To avoid damage please change the grating G tt strictly according to DADOS user manual Also be careful with the tiny set screws and don t touch the optical surface of the grating Credit DADOS Spectrograph User Manual Two blazed reflection gratings are recommended by the designers of the DADOS spectrograph Low resolution 200 lines mm linear dispersion 2 16 A px 0 2 nm px 6563 A 5 4 micron pixel Medium resolution 90o lines mm linear dispersion 0 59 A px 0 059 nm px Optional High resolution 1200 lines mm linear dispersion 0 46 A px 0 046 nm px A modified DSLR Camera with an 18 mm x 22 mm APS size sensor covers the whole spectrum about 400 nm 700 nm only if used with the 200 lines mm grating The camera field should be aligned parallel to the spectrum to minimize aliasing errors due to rotation of the spectrum This can be achieved by loosening three set screws at the T2 adapter rotating the inner T2 ring and tightening the set screws V3 5E Bernd Koch b koch baader planetarium de 15 DADOS sour srectrosraPH TUTORIA Daylight spectrum of 900 I mm grating and 1200 mm grating Me Triplet EOS 10D 900 lines mm exposure 15 unprocessed unsharp masking EOS 1
63. tings Window Help G E Add Borders Ctrl R 400 RGB RGB an eg Exit EN of a m EE Sage Geometry we_Results zweite Fassung Mittelmed Result_image_colour_16bit fit iix Pixel Arithmetic d Sharpen Filter Blur Filter Zool Background Flatten Color Functions Resize Image Ctrl 4G Video E Ba yer Interpolation Special Filter M FFT Mare Functions Tr F e OF OF e F F F Adjust Colorlayers Hi Split Color Image to 3 B W Images Color Image to B W Luminance Color Image to B W Luma C Dokumente und Einstellungen astrofoto Desktop Betelgeuse_200L_2010 12 15 2_Spektra_raw_images_CR2 Result_image fit Result image _mono_16bit fit FITS 16 bit Integer ped Save as Result image mono a16bit V3 5E Bernd Koch b koch baader planetarium de 47 DA Been TUTORIAL _ E Stacking calibration of stellar spectra from a Canon DSLR camera Step 5 VisualSpec VSpec Spectrum calibration VSpec Software Download http valerie desnoux free fr Please note VisualSpec accepts monochrome 16 bit files only A4 VIELE File Edit Format Operations Spectrometry Tools Assistant Window Options amp Le El E ox 31s85 si I 5 o 0 A pixel 32766 SC 9 5 ZS Ea As SS Se SS p intensity QN blue F u nk as SHA A EL AE AU w qp EUG gt V3 5E Bernd Koch b koch baader planetarium de 48 p ee Paya UTO
64. tswork File Processing Image Combining Settings Window Help ie Ld P4 m B US SS a V3 5E Bernd Koch b koch baader planetarium de 38 Settings Load Save Math Image display Various Syg Show Image Preview Convert Color Images to VU after Loading v Loading and Saving FITS Files Flip Image Camera Raw W Debayer Raw Images Dont RGB Scale not Debayered Raw Images Settings Load Save Math Image display Various Syg General Interpolation dee C Linear NoHalo C Neuronal alow C EE Image Division and Multiplication Iw Scale Result standard Scale PSF Images Automatic Hotel Removement in Image Subtraction Sigma 40 Network Initialization Fandom Automatic 2D FFT Interference Filter Sigma 20 FFT outer Border for reducing Artefacts Piel SR 34 B8 RIAI Ed n a Canon E camera Settings Load Save Math Image display Various Sps Save FITS Files as Extention af FITS Files C 32 bit Floating Point e Ej 32 bit Integer f 1B bit Integer Pis JPEG Ctrl J 0 9 Higher Better Compression are Scale TIFF Images Automatic Settings Load Save Math Image display Various Sps Automatic Histogram Scaling Block BD 1x White 99 99 Z from Histagram Set Blacklevel always to D Adjust Gamma on Images with more than Bit V3 5E Bernd Koch b koch baader planetarium de 39 anon DSLR camera S
65. ve x and set about 60 green crosses along the continuum a Ori Betelgeuse Class M2Iab 413210 236120 V3 5E Bernd Koch b koch baader planetarium de 75 Stacking calibration of a Canon DSLR camera Step 7 Visual Spec VSpec Spectrum calibration by removing the instrumental profile 7 6 Press button OK and press eyecute PASTES File Edit Format Operations i Visual Spec image_result_wavecal spc eee ls x a El File Edit Format Operations Spectrometry Radiometry Tools Assistan Window Options AE g a HAB nx 1498 7526 17 I Z0 418 aon me 1532 A pixel a Ori Betelgeuse Class M2Iab At d NL MAC As V 4840 5110 5380 5650 5920 6190 6460 V3 5E Bernd Koch b koch baader planetarium de 76 CTR RAF Stacking calibration of stellar spectra from a Canon DSLR camera Step 7 Visual Spec VSpec Spectrum calibration by removing the instrumental profile 7 7 Erase graphic ES gt Edit gt Replace Intensity intensity gt eh blue S 7 8 File gt Save as gt response spc V3 5E Bernd Koch b koch baader planetarium de 7 7 TUTORIAL E ing calibrati af stellar ea spectra From a Canon DSLR camera Step 7 Visual Spec VSpec Spectrum calibration by removing the instrumental profile 7 9 While response spc is still open File gt open profile Result image wavecal spc please highl

DADOS Spektrograph Tutorial

Contents

Download Pdf Manuals

Related Search

Related Contents