"Science, Faculty of"@en . "Physics and Astronomy, Department of"@en . "DSpace"@en . "UBCV"@en . "Scharein, Robert Glenn"@en . "2010-05-16T05:04:41Z"@en . "1984"@en . "Master of Science - MSc"@en . "University of British Columbia"@en . "This thesis describes the first incarnation of an automated photometry program AOLP, acronym for Automatic Object Location Program. This program is designed to search through an image and to find, catalogue, and (eventually) classify all objects found. The primary aim is for use in a faint galaxy survey. The program has also proven useful in other areas, such as photometry of globular clusters and relatively nearby, bright galaxies."@en . "https://circle.library.ubc.ca/rest/handle/2429/24767?expand=metadata"@en . "AOLP : AN AUTOMATIC OBJECT LOCATION PROGRAM by ROBERT GLENN SCHAREIN B.Sc. (Hon), U n i v e r s i t y of Manitoba, 1981 A THESIS SUBMITTED IN PARTIAL FULFILMENT OF THE REQUIREMENTS FOR THE DEGREE OF MASTER OF SCIENCE in THE FACULTY OF GRADUATE STUDIES (Department of Geophysics and Astronomy) We accept t h i s t h e s i s as conforming to the r e q u i r e d standard THE UNIVERSITY OF BRITISH COLUMBIA October, 1984 \u00C2\u00A9 Robert Glenn S c h a r e i n , 1984 In p r e s e n t i n g t h i s t h e s i s i n p a r t i a l f u l f i l m e n t of the requirements f o r an advanced degree at the U n i v e r s i t y o f B r i t i s h Columbia, I agree t h a t the L i b r a r y s h a l l make i t f r e e l y a v a i l a b l e f o r r e f e r e n c e and study. I f u r t h e r agree t h a t p e r m i s s i o n f o r e x t e n s i v e copying of t h i s t h e s i s f o r s c h o l a r l y purposes may be granted by the head o f my department or by h i s or her r e p r e s e n t a t i v e s . I t i s understood t h a t copying or p u b l i c a t i o n o f t h i s t h e s i s f o r f i n a n c i a l g a i n s h a l l not be allowed without my w r i t t e n p e r m i s s i o n . Department ,of (j^op hyji (.5 CL^<4 ^SWO^OW.^ The U n i v e r s i t y of B r i t i s h Columbia 1956 Main Mall Vancouver, Canada V6T 1Y3 Date DE-6 (.3/81) Abstract T h i s t h e s i s d e s c r i b e s the f i r s t i n c a r n a t i o n of an automated photometry program AOLP, acronym f o r Automatic Object L o c a t i o n Program. T h i s program i s designed to search through an image and to f i n d , c atalogue, and ( e v e n t u a l l y ) c l a s s i f y a l l o b j e c t s found. The primary aim i s f o r use i n a f a i n t galaxy survey. The program has a l s o proven u s e f u l i n other areas, such as photometry of g l o b u l a r c l u s t e r s and r e l a t i v e l y nearby, b r i g h t g a l a x i e s . i i Table of Contents Chapter Page A b s t r a c t i i L i s t of Tables i v L i s t of F i g u r e s v Acknowledgements v i i I. I n t r o d u c t i o n 1 A. F a i n t Galaxy Counting 1 B. Moment I n v a r i a n t s i n Astronomy 8 I I . Hardware and Software D e s c p r i p t i o n 13 A. The I 2 S Image Processor 13 B. The Automatic Object L o c a t i o n Program 17 I I I . A p p l i c a t i o n to A r t i f i c i a l F i e l d s 20 A. E f f e c t of Shape 21 IV. Mixed Star and Galaxy F i e l d s 25 V. Photometric A p p l i c a t i o n s 29 A. G l o b u l a r C l u s t e r s 32 M92 32 M13 36 B. G a l a x i e s 39 Colours and Magnitudes of Compact Group g a l a x i e s 39 Luminosity P r o f i l e s of Compact Group G a l a x i e s 41 VI. C o n c l u s i o n 67 B i b l i o g r a p h y 68 i i i L i s t of Tables I A n a l y t i c a l Values f o r Moment I n v a r i e n t s 22 II C a l i b r a t i o n S t a r s i n M92 31 III Colours and Magnitudes of Compact Group G a l a x i e s 40 i v L i s t of Figures 1 F a i n t galaxy counts 4 2 Data path i n 1 2S 14 3 R v i . C 2 f o r gaussians 23 4 C\u00E2\u0080\u009E v s . C 2 f o r gaussians 23 5 C 2 vs. magnitude f o r E9 f i e l d \u00E2\u0080\u00A2 26 6 R vs. C 2 f o r E9 f i e l d 27 7 R v s . C 2 f o r E9 f i e l d 27 8 C\u00E2\u0080\u009E vs. C 2 f o r E9 f i e l d 28 9 C 2 vs. magnitude f o r M92 34 10 R v s . C 2 f o r M92 35 11 C\u00E2\u0080\u009E v s . C 2 f o r M92 35 12 B v s . B-R CM diagram f o r M92 37 13 V vs. B-V CM diagram f o r M92 37 14 B vs. B-R CM diagram for M13 38 15 V v s . B-V CM diagram f o r M1 3 38 16 Luminosity p r o f i l e s f o r galaxy HCG73a 43 17 Luminosity p r o f i l e s f o r galaxy HCG73b 44 18 Luminosity p r o f i l e s f o r galaxy HCG73c 45 19 Luminosity p r o f i l e s f o r galaxy HCG73d.. 46 20 Luminosity p r o f i l e s f o r galaxy HCG76a 47 21 Luminosity p r o f i l e s f o r galaxy HCG76b 48 22 Luminosity p r o f i l e s f o r galaxy HCG76b... 49 23 Luminosity p r o f i l e s f o r galaxy HCG76c 50 24 Luminosity p r o f i l e s f o r galaxy HCG76c 51 25 Luminosity p r o f i l e s f o r galaxy HCG76d 52 v 26 ' Luminosity p r o f i l e s f o r galaxy HCG76e 53 27 Luminosity p r o f i l e s f o r galaxy HCG76f 54 28 Luminosity p r o f i l e s for galaxy HCG88a 55 29 Luminosity p r o f i l e s for galaxy HCG88b 56 30 Luminosity p r o f i l e s f o r galaxy HCG88c 57 31 Luminosity p r o f i l e s f o r galaxy HCG88d 58 32 Luminosity p r o f i l e s f o r galaxy HCG92a 59 33 Luminosity p r o f i l e s f o r galaxy HCG92bd 60 34 Luminosity p r o f i l e s f o r galaxy HCG92c 61 35 Luminosity p r o f i l e s for galaxy HCG92e 62 36 Luminosity p r o f i l e s f o r galaxy HCG97a 63 37 Luminosity p r o f i l e s f o r galaxy HCG97a 64 38 Luminosity p r o f i l e s f o r galaxy HCG97b 65 39 Luminosity p r o f i l e s f o r galaxy HCG97c 66 v i Acknowledgements I would l i k e to thank my a d v i s o r , Dr. Greg Fahlman f o r suggesting t h i s p r o j e c t and p r o v i d i n g help when needed. His p a t i e n c e and encouragement were most welcome. I would a l s o l i k e to thank Dr. Paul Hickson f o r access to h i s CCD images of compact groups and g l o b u l a r c l u s t e r s . To my f r i e n d s and c o l l e g u e s i n the Astronomy Dept, I o f f e r my g r a t i t u d e . I'd e s p e c i a l l y l i k e to thank John N i c o l , f o r always p r o v i d i n g c h e e r f u l a s s i s t a n c e with a myriad of computer problems. For a l l my dear f r i e n d s in Winnipeg and Calgary, thanks f o r standing behind me when the going got rough. To my very c l o s e f r i e n d s i n Vancouver (and those who have l e f t ) , I owe a great d e a l . Thank-you for a l l that you have shown me over the past three y e a r s . To my brother Don, h i s wife Debbie and t h e i r daughter who was born as t h i s t h e s i s was being completed I extend my love. And most of a l l I would l i k e to thank my parents, my mother with her joyous, wonderful f r e e - f l o w i n g s p i r i t , who has been a r e a l gem a l l these years; and my f a t h e r , that most b r i l l i a n t man who taught me the love of nature, wherever he may be. v i i I. Introduction A. Faint Galaxy Counting Two important and as of yet, unanswered q u e s t i o n s i n cosmology are: 1) Is the u n i v e r s e r e a l l y homogeneous? and 2) E x a c t l y how do g a l a x i e s evolve? To answer these q u e s t i o n s r e q u i r e s that we look f a r enough out i n the u n i v e r s e so that we are w e l l w i t h i n the uniform Hubble flow, and f a r enough back in time so that we can see g a l a x i e s over a s i g n i f i c a n t f r a c t i o n of t h e i r l i f e t i m e s . Thus we are i n the realm of the very f a i n t g a l a x i e s (B > 22) where, due to the l a r g e numbers i t may become necessary to have an automated means of c o u n t i n g and measuring the g a l a c t i c images. I t i s f o r t h i s purpose that the program AOLP (Automatic Object L o c a t i o n Program) has been developed. I t w i l l become p o s s i b l e with equipment p r e s e n t l y being b u i l t at the U n i v e r s i t y of B r i t i s h Columbia to o b t a i n a complete sample of f a i n t g a l a x i e s down to magnitude 25 together with r e d s h i f t i n f o r m a t i o n f o r s e v e r a l r e g i o n s of the sky. Such a sample w i l l g r e a t l y enhance our c u r r e n t understanding of these q u e s t i o n s . I t i s u s e f u l then to examine what i n f o r m a t i o n we c o u l d expect to f i n d from f a i n t galaxy counts and a l s o to see what o t h e r s have done in t h i s a r ea. F a i n t galaxy counts appear to be r e l a t i v e l y i n s e n s i t i v e to d i f f e r e n t values of the Hubble constant H0 and the d e c e l e r a t i o n parameter q0 for a s p e c i f i c c o s m o l o g i c a l model. The reason f o r t h i s i s , as shown by T i n s l e y (1977,1980), 1 2 that number-magnitude r e l a t i o n s f o r d i f f e r e n t models are im p e r c e p t i b l y d i f f e r e n t ( i g n o r i n g e v o l u t i o n ) at c o n c e i v a b l y a t t a i n a b l e magnitudes. Once we i n c l u d e g a l a c t i c e v o l u t i o n , the i n t e r p r e t a t i o n of galaxy counts i s com p l i c a t e d by many unknown parameters. A l s o , the d i s t i n c t i o n between d i f f e r e n t types of g a l a x i e s i s g e n e r a l l y not a v a i l a b l e at f a i n t magnitudes. The observed d i f f e r e n t i a l count i s t h e r e f o r e a sum over the expected number N (m) f o r each c l a s s of galaxy. The number of g a l a x i e s of a given type i n an i n t e r v a l Am of apparent magnitude i s given by, N (m) Am = J N (m, z) dl ogz Am where Zy = \"formation\" r e d s h i f t (when s t a r formation s t a r t e d ) N = (number of ga l a x i e s ) / m a g n i t u d e / u n i t logz = W(z) n0 *(M0) here W(z) =-4-nRlr 2 r7 \/(l-kr2) dr d I ogz i s the comoving volume/unit logz i n a Robertson-Walker cosmology with the standard metric ds2 = c 2 d t 2 - R2(t)[dr2/(1-kr2) + r2dd2 + r2si n28d*-*\u00E2\u0080\u00A2 a Figure 10: Scatter p l o t of R vs. C 2 for objects in M92. 50000 r 20000 -10000 -5000 L 1000 -500 L 0.5 2 5 10 20 50 100 Figure 11: Scatter p l o t of C\u00C2\u00AB vs. C 2 for objects in M92. 36 The p l o t of C 4 vs. C 2 shown i n f i g u r e 11 proves to more i n t e r e s t i n g than i t was e a r l i e r . S t a r s l i e on an extremely narrow l i n e , and there i s a l s o c o n s i d e r a b l e d e v i a t i o n from t h i s l i n e f o r n o n - s t e l l a r o b j e c t s . Two colour-magnitude diagrams are show here. F i g u r e 12 shows a J? vs. B-R diagram obtained with data from the f i r s t o bserving s e s s i o n . A V vs. B-V diagram i s shown i n f i g u r e 13 with data from the second s e s s i o n . M13 Exposures of M13 were taken only on the second observing s e s s i o n . The f i e l d surveyed i s l o c a t e d f i v e arc-minutes d i r e c t l y north of the c e n t e r . Shown i n f i g u r e s 14 and 15 are B vs. B-R and V vs. B-V diagrams. T h i s approach i n determining colour-magnitude diagrams i s probably not the best one a v a i l a b l e , although i t does y i e l d i n t e r e s t i n g r e s u l t s . A b e t t e r technique i s to f i t s t e l l a r p r o f i l e s to the o b j e c t s i n the f i e l d . T h i s a l l o w s merged o b j e c t s to be i n c l u d e d i n the survey. In the approach taken here, merged o b j e c t s are d e l i b e r a t e l y avoided. 37 16 17 18 19 m 20 21 22 h 23 \u00E2\u0080\u00A2 * \ ^ + \u00E2\u0080\u00A2H- + , + + 4+ + + \u00E2\u0080\u00A2 \u00E2\u0080\u00A2 24 0.5 16 h 17 r 18 h 1.0 1.5 2.0 B - R : M92 Figure 12: C o l o u r magnitude d i a g r a m of M92 from f i r s t o b s e r v i n g s e s s i o n . i \"i 1 \u00E2\u0080\u0094 i I I T I I I 2.5 19 20 21 22 23 -0.4 0.0 + + + 4-. +\"7+ + \u00E2\u0080\u00A2V* 4* 0.4 1.6 0.8 1.2 B - V : M92 Figure 13: C o l o u r magnitude d i a g r a m of M92 from second o b s e r v i n g s e s s i o n . 2.0 19 r 20 r 21 r 22 23 1.2 1.6 B - R : M13 2.0 2.4 Figure Ml 3. 14: Colour magnitude diagram of i _ + i i i i i i - + *\u00E2\u0080\u00A2 - + + + A + -4-4- 4. 4. * + -ft* \u00E2\u0080\u00A2 \u00E2\u0080\u00A2 + + ** f 4- * * ** + i 4. \u00E2\u0080\u00A2 *-\ j. \* * 1 * * 4+ 4* + *+ * + + + 4 -1 1 1 1 1 1 18 19 20 21 22 0.4 0.8 1.6 1.2 B - V : M13 Figure 15: Colour magnitude diagram of Ml 3. 39 B. Galaxies AOLP was a l s o used determine the magnitudes and c o l o u r s of g a l a x i e s i n Hickson's compact group c a t a l o g u e . The data was obtained during the summer of 1983 o b s e r v i n g s e s s i o n . Exposures were made in red and blue l i g h t f o r each f i e l d . The photometry was done using the ISOPHOT command in AOLP. The i s o p h o t a l i n t e n s i t y was measured at each isophote from 255 ( i n ADC u n i t s ) down to j u s t above the sky. T h i s allowed the i n t e n s i t y p r o f i l e s to be determined i n a d d i t i o n to c o l o u r s and magnitudes for each galaxy. Colours and Magnitudes of Compact Group galaxies The c o l o u r s and magnitudes for the s e l e c t e d g a l a x i e s are shown in Table I I I . In order to determine the c o l o u r s , the two images taken through the R and B f i l t e r s had to be matched up. A number of a l t e r n a t i v e s were c o n s i d e r e d . One p o s s i b i l i t y was to d e f i n e an area by a given isophote on one image, a l i g n the images c a r e f u l l y and measure the i n t e n s i t y w i t h i n the corresponding region on the other image (note i t i s not n e c e s s a r i l y an i s o p h o t e ) . T h i s method does not f i t n a t u r a l l y i n t o the type of output generated by AOLP. The ISOPHOT command g i v e s the i n t e n s i t y w i t h i n the isophote and the area of the isophote ( i n p i x e l s ) . The technique used was to match up each measurement in one c o l o u r ( i n t h i s case blue, but the choice i s a r b i t r a r y ) with the measurement i n the other c o l o u r that c o n t a i n e d the same number of p i x e l s ( i n t e r p o l a t i n g i f n e c e s s a r y ) . A p o t e n t i a l disadvantage of 40 Table I II; Colours and Magnitudes of Compact Group Galaxies Galaxy -\u00E2\u0080\u00A223.5 (B-R) 2 3 5 &2\u00C2\u00AB.0 (B-R) 2 a o Comments 73a 14.74 1.17 14.43 1.14 s p i r a l 73b 17.76 2.30 17.47 2.26 s p i r a l f 73c 17.22 1 .69 17.14 1 .69 le n t i c 73d 19.11 2.44 18.94 2.43 s p i r a l f 76a 16.11 1 .79 16.05 1 .78 spi r a l 76b 15.47 1 .58 15.33 1 .57 e l l i p 76c 1 5.70 1 .66 15.53 1 .65 e l l i p 76d 16.16 1 .60 15.97 1 .56 e l l i p 76e 17.73 1 .54 17.55 1 .54 s p i r a l 88a 14.38 1 .53 1 4.29 1 .53 s p i r a l 88b 14.51 1 .53 1 4.39 1 .52 spi r a l 88c 1 5.56 1.11 15.37 1.11 spi r a l 88d 15.87 0.78 ***** **** spi r a l 92a 13.53 1 .08 ***** **** spi r a l 92bd 14.08 1 .65 13.96 1 .65 spi r a l 92c 15.44 1 .82 14.74 1 .62 s p i r a l 92e 15.46 * * * * ***** **** ellip t -97a 14.74 1 .65 14.59 1 .65 e l l i p 97b 16.12 1 .57 16.01 1 .58 spi r a l 97c 15.26 1 .45 15.17 1 .45 lent ic t Blue photometry probably in error $ Bright star subtracted this method i s that the same region might not be measured on each image, eventhough they are of the same size area. This effect would generally be s i g n i f i c a n t only in the inner region of a galaxy where the colour along a given isophote 41 might not be constant. For measurements i n the outer regions of a galaxy, where the co l o u r i s f a i r l y uniform around an isophote, t h i s technique i s r e l i a b l e . The r e s u l t s quoted i n the t a b l e are f o r t h i s case. Luminosity P r o f i l e s of Compact Group Galaxies The ISOPHOT command i s very u s e f u l f o r determining l u m i n o s i t y p r o f i l e s of g a l a x i e s . The method used here i s somewhat d i f f e r e n t from usual techniques of a r r i v i n g at lu m i n o s i t y p r o f i l e s , but i s p o t e n t i a l l y as u s e f u l . Luminosity p r o f i l e s are u s u a l l y determined from r a d i a l c u t s , e i t h e r along the minor or major a x i s or at some angle to i t . Aperture photometry i s a l s o used with c i r c u l a r a p e r t u r e s or e l l i p t i c a l a p e r t u r e s t a i l o r e d to f i t a given g a l a x y . A l l of these methods s u f f e r from the problem that they are not g e n e r a l . R a d i a l cuts c o n t a i n i n f o r m a t i o n only from one par t of the galaxy. With aperture photometry i t i s d i f f i c u l t to accommodate p e c u l i a r i t i e s i n i n d i v i d u a l galaxy shapes. I t i s worthwhile to develop an approach that i s holistic i n the sense that i t d e s c r i b e s the e n t i r e galaxy, and general i n that i t can be a p p l i e d to a l l g a l a x i e s i n a c o n s i s t e n t manner. We d e f i n e here the effective radius of an isophote to be re=\/(A/n) where A i s the area w i t h i n the i s o p h o t e . For an e l l i p s e of e l l i p t i c i t y e t h i s corresponds to a r a d i a l cut at an angle 4>=arccos {(1 - e)'05} to the major a x i s . For d i s r u p t e d g a l a x i e s there i s no such correspondence between the e f f e c t i v e radius and a r a d i a l c u t . These g a l a x i e s o f t e n 42 have no c l e a r l y d e f i n e d major a x i s and the e f f e c t i v e r a d i u s seems to be the most meaningful r a d i a l parameter. Many of the g a l a x i e s s t u d i e d here are of t h i s type. F o l l o w i n g are the d i f f e r e n t i a l and i n t e g r a t e d l u m i n o s i t y p r o f i l e s for 2. of the compact group g a l a x i e s . Magnitude i s p l o t t e d as a f u n c t i o n of r f o r each galaxy, and a l s o as a f u n c t i o n of r e \u00C2\u00B0 ' 2 S f o r e l l i p t i c a l g a l a x i e s . The magnitudes shown are instrumental blue magnitudes. 43 2 0 I 1 1 1 1 1 1 1 -2 5 i i i i i i i I 0.0 5 10 15 2 0 2 5 3 0 3 5 Eff. Radius (arc-sec) : HCG73a 14- I 1 1 1 1 1 r 0.0 5 10 15 2 0 2 5 3 0 3 5 Eff. Radius (arc-sec) : HCG73a Figure 16: D i f f e r e n t i a l and integrated magnitude p r o f i l e s for galaxy HCG73a. Open faced Sc s p i r a l . 44 21 0.0 5 10 15 Eff. Radius (arc-sec) : HCG73b 0.0 5 10 15 Eff. Radius (arc-sec) : HCG73b Figure 17: D i f f e r e n t i a l and i n t e g r a t e d magnitude p r o f i l e s f o r galaxy HCG73b. S p i r a l galaxy. The blue photometry i s probably in e r r o r . Figure 18: D i f f e r e n t i a l and integrated magnitude p r o f i l e s for galaxy HCG73c. Lenticular galaxy. 46 T 1 1 1 1 1 1 1 1 1 0.0 2 4 6 8 10 Eff. Radius (arc-sec) : HCG73d i 1 1 i i i i i i i I 0.0 2 4 6 8 10 Eff. Radius (arc-sec) : HCG73d Figure 19: D i f f e r e n t i a l and integrated magnitude p r o f i l e s for galaxy HCG73d. S p i r a l galaxy. Photometry probably in error. 47 0.0 18 r 0.0 5 10 15 Eff. Radius (arc-sec) : HCG76a 5 10 15 Eff. Radius (arc-sec) : HCG76a Figure 20: D i f f e r e n t i a l and integrated magnitude p r o f i l e s for galaxy HCG76a. S p i r a l galaxy. J I L 0.0 5 10 15 20 25 30 Eff. Radius (arc-sec) : HCG76b i 1 1 1 1 1 1 0.0 5 10 15 20 25 30 Eff. Radius (arc-sec) : HCG76b Figure 21: D i f f e r e n t i a l and integrated magnitude p r o f i l e s for galaxy HCG76b. E l l i p t i c a l galaxy. cd S 15 16 17 1.0 1.5 2.0 2.5 (Eff. Rad.)* 5 (arc-sec)\" 2 5 : HCG76b Figure 22: D i f f e r e n t i a l and integrated magnitude p r o f i l e s for galaxy HCG76b. E l l i p t i c a l galaxy. \u00E2\u0080\u00A24-3 d CO S OJ 16 17 0.0 Eff. 5 10 15 Radius (arc-sec) : HCG76c Figure 23: magnitude E l l i p t i c a l 20 D i f f e r e n t i a l p r o f i l e s f o r galaxy. and i n t e g r a t e d galaxy HCG76c. 1 1.5 2 2.5 (Eff. Rad)\"86 (arc-sec)\"* : HCG76c i - 1 1 1 \u00E2\u0080\u00A2 \u00E2\u0080\u0094 i i I I i i i i 1 1 1 1.5 2 2.5 (Eff. Rad)* 8 (arc-sec)\"* : HCG76c Figure 24: D i f f e r e n t i a l and integrated magnitude p r o f i l e s for galaxy HCG76c. E l l i p t i c a l galaxy. 20 Eff. Radius (arc-sec) : HCG76d Figure 25: D i f f e r e n t i a l and integrated magnitude p r o f i l e s for galaxy HCG76d. E l l i p t i c a l galaxy. Sharp jump in p r o f i l e due to presence of bright st a r . 5 3 l i I I I I I i i I I 0.0 2 4 6 8 10 Eff. Radius (arc-sec) : HCG76e Figure 26: D i f f e r e n t i a l and integrated magnitude p r o f i l e s for galaxy HCG76e. S p i r a l galaxy. CD -*-> ti S 18 19 20 0.0 2 4 6 8 10 Eff. Radius (arc-sec) : HCG76f 12 Figure 27: D i f f e r e n t i a l magnitude p r o f i l e s for Lenticular galaxy. and integrated galaxy HCG76f. 55 I i i i i 1 1 1 0.0 5 10 15 20 25 30 35 Eff. Radius (arc-sec) : HCG88a Figure 28: D i f f e r e n t i a l and integrated magnitude p r o f i l e s for galaxy HCG88a. S p i r a l galaxy. 56 . I 1 1 i i i i I 0.0 5 10 15 20 25 30 35 Eff. Radius (arc-sec) : HCG88b 14 I 1 1 1 1 1 1 . 1 15 -i-j fl ca \u00C2\u00AB! 16 fl 0.0 5 10 15 20 25 30 35 Eff. Radius (arc-sec) : HCG88b Figure 29: D i f f e r e n t i a l and in t e g r a t e d magnitude p r o f i l e s f or galaxy HCG88b. S p i r a l galaxy. 57 0.0 5 10 15 20 25 30 Eff. Radius (arc-sec) : HCG88c T 1 1 1 r j i i i L \u00C2\u00B0 0 5 10 15 20 25 30 Eff. Radius (arc-sec) : HCG88c Figure 30: D i f f e r e n t i a l and i n t e g r a t e d magnitude p r o f i l e s f o r galaxy HCG88c. S p i r a l galaxy. 58 Figure 31: D i f f e r e n t i a l and integrated^ magnitude p r o f i l e s for galaxy HCG88d. S p i r a l galaxy. 59 20 I 1 1 1 1 1 1 1 24 I 1 1 1 1 1 1 1 0.0 5 10 15 20 25 30 35 Eff. Radius (arc-sec) : HCG92a 13 I i 1 1 1 1 r 22 1 1 i i i i i I 0.0 5 10 15 20 25 30 35 Eff. Radius (arc-sec) : HCG92a Figure 32: D i f f e r e n t i a l and i n t e g r a t e d magnitude p r o f i l e s f o r galaxy HCG92a. S p i r a l galaxy. B r i g h t e s t . member in Stephen's Q u i n t e t . Galaxy with d i s c r e p e n t r e d s h i f t . Sharp jump i n p r o f i l e due to presence of b r i g h t s t a r . 20 | 1 1 1 1 1 r 0.0 5 10 15 20 25 30 35 Eff. Radius (arc-sec) : HCG92bd I r 1 1 1 1 i I -\u00E2\u0080\u00A2-< a aj SS si C ~ 15 I i I i i i i l 0.0 5 10 15 20 25 30 35 Eff. Radius (arc-sec) : HCG92bd Figure 33: D i f f e r e n t i a l and i n t e g r a t e d magnitude p r o f i l e s f o r galaxy HCG92bd. P a i r of i n t e r a c t i n g s p i r a l g a l a x i e s i n Stephen's Q u i n t e t . 61 20 0.0 5 10 15 20 25 30 Eff. Radius (arc-sec) : HCG92c J L 0.0 5 10 15 20 25 30 Eff. Radius (arc-sec) : HCG92c Figure 34: D i f f e r e n t i a l and integrated magnitude p r o f i l e s for galaxy HCG92c. S p i r a l galaxy in Stephen's Quintet. Eff. Radius (arc-sec) : HCG92e CD c cd 3 S CD 14 15 16 0.0 5 10 15 20 Eff. Radius (arc-sec) : HCG92e 25 Figure 35: D i f f e r e n t i a l and i n t e g r a t e d magnitude p r o f i l e s f o r galaxy HCG92e. E l l i p t i c a l galaxy i n Stephen's Q u i n t e t . The sharp jump in the p r o f i l e i s due the presence of a b r i g h t s t a r . 63 I 1 1 I I i i I 0.0 5 10 15 20 25 30 35 Eff. R a d i u s ( a r c - s e c ) : HCG97a 0.0 5 10 15 20 25 30 35 Eff. R a d i u s ( a r c - s e c ) : HCG97a Figure 36: D i f f e r e n t i a l and in t e g r a t e d magnitude p r o f i l e s for galaxy HCG97a. E l l i p t i c a l galaxy. I I I I I I I 1.0 1.5 2.0 2.5 ( E f f . R a d . ) * 6 ( a r c - s e c ) * * : HCG97a Figure 37: D i f f e r e n t i a l and i n t e g r a t e d magnitude p r o f i l e s f o r galaxy HCG97a. E l l i p t i c a l galaxy. 0.0 5 10 15 Eff. Radius (arc-sec) : HCG97b 20 Figure 38 magnitude galaxy. D i f f e r e n t i a l and p r o f i l e s f o r galaxy i n t e g r a t e d HCG97b. S p i r a l 15 cd s OJ 16 0.0 5 10 15 20 Eff. Radius (arc-sec) : HCG97c Figure 39: D i f f e r e n t i a l and i n t e g r a t e d magnitude p r o f i l e s f o r galaxy HCG97c. L e n t i c u l a r galaxy. VI. Conclusion The f i r s t stages of AOLP have shown i t to be useful in a number of d i f f e r e n t applications. It is a r e l i a b l e method of obtaining colour-magnitude diagrams for globular clusters although i t is probably not the best approach. Luminosity p r o f i l e s of galaxies are quickly and e f f i c i e n t l y determined with the program. More research s t i l l needs to be done in the application to mixed star and galaxy f i e l d s . This w i l l have to wait u n t i l the proper data base can be assembled. The i n i t i a l work with moment invarients looks promising, the technique proved helpful in discriminating stars from other objects when applied to the globular cluster f i e l d s . 67 "@en . "Thesis/Dissertation"@en . "10.14288/1.0085789"@en . "eng"@en . "Astronomy"@en . "Vancouver : University of British Columbia Library"@en . "University of British Columbia"@en . "For non-commercial purposes only, such as research, private study and education. Additional conditions apply, see Terms of Use https://open.library.ubc.ca/terms_of_use."@en . "Graduate"@en . "Aolp : an automatic object location program"@en . "Text"@en . "http://hdl.handle.net/2429/24767"@en .