Study photometric properties of spiral galaxy NGC 4448 using CCD camera with multiband filters الوزدوج وهرشحات هتعذدة الحزم
|
|
- Ursula Pope
- 5 years ago
- Views:
Transcription
1 Iraqi Journal of Physics, 2017 ol.15, No.35, PP Study photometric properties of spiral galaxy NGC 4448 using CCD camera with multiband filters Department of Astronomy and Space, College of Science, University of Baghdad Abstract The goal of our study is to perform detailed multiband surface photometry of the spiral galaxy NGC 4448 and its brightest starforming regions. The structure and composition of the stellar population in the surface brightness galaxy NGC 4448 was studied using B CCD photometry. The observations were obtained on the 1.88 m optical telescope of Kottamia Astronomical Observatory (KAO), Egypt. A two-dimensional decomposition of the galaxy bulge and disk components is carried out. A powerful star forming region is observed near the galactic center. Based on the positions of the various components of the galaxy in two color diagrams. From the observations, the surface brightness profiles, Ellipticity profiles, position angle profiles and color indices profiles are described and studied. Key words Spiral galaxy, surface photometry, ellipticity, color index. Article info. eceived: Mar Accepted: May Published: Dec دراسة الخصائص الضوئية للوجرة الحلزو ية NGC 4448 الوزدوج وهرشحات هتعذدة الحزم س اى حسي علي بأستخذام كاهيرة الشحي قسن الفلك والفضاء, كلية العلوم, جاهعة بغذاد الخالصة تن دراسة تركية وتنية الجوهرة النجوية في اللوعاى السطحي للوجرة )4448 )NGC بىاسطت أخز أسصاداث فىتىيتشيت باستخذاو كاييشة انشحن ان ضدوج camera( )CCD يع ان ششحاث )B,,( وتاستخذام تلسكىب تصري قطره 8811 يتش في يشصذ انقطاييت انفهكي في ج هىسيت يصش انعشبيت 8 تى تحهيم يشكبتي ان جشة )disk( و 8)bulge( تى يالحظت ينطقت فعانت نتكىين اننجىو بانقشب ين يشكض ان جشة وباالستناد انى يشكباث يختهفت نه جشة نهشسىو انبيانيت راث انهىنين وين خالل االرصادات تن دراسة ووصف لوعانية السطح brightness) (surface هقذار التفلطح )ellipticity) صاويت ان ىضع angle) (position ودليل االلىاى 8)color indices) Introduction The surface photometry of galaxies provides the fundamental and essential information for the study of their structures and dynamics. The recent advances in CCD device technology and image processing techniques allow us to deal the photometric data of faint objects of great deal with high precision. In this study, we performed the multiband surface photometry of galaxies with a CCD camera equipped on 1.88 m optical telescope of Kottamia Astronomical Observatory (KAO) Egypt. The specific characteristics of their photometric structures will provide the essential information not only of the relations of stellar kinematics to configurations but also of the origin of the bar structure. Surface photometry is an important tool in the understanding of galaxy mass and structure. Obtaining the structural 8
2 Iraqi Journal of Physics, 2017 characteristics and the total luminosity of a galaxy requires knowledge of its surface brightness profile to a significant depth. During a surface photometry project to explore the structure of galaxies by morphological type (Schombert & Smith 2011) [1]. Most of the current knowledge about the structure of galaxies came from the analysis of the photographic plates. ecently, this technique has been enhanced by the replacement of digital imaging. This new technology improves sensitivity by a factor of 100 and provides greater dynamic range. The 1980s saw the rise of the CCD cameras, it is a device consists of light sensitive photoelectric cells, or pixels, that transfer incoming light particles into electric current [2]. The pixels can also be digitally combined, which increases light sensitivity at the expense of resolution [3]. The light observed in the visual wavelengths from a galaxy arises from all its stars, with the radiation contribution from the brightest hot stars competing with the light from the more numerous fainter cool stars. In this sense, we can infer a galaxy s stellar composition and age by observing its color [4]. Photometry can be defined as the determination of the amount and temporal nature of the flux emitted by an astronomical object as a function of wavelength [5]. By taking images of a galaxy at different wavelengths, and then analyzing the intensity distribution in each image, one can determine the distribution of stars, dust, and gas within the object. In order to obtain images of objects at different wavelengths for photometric study, a series of filters are introduced into the light path of the instrument being used. In order to be scientifically useful for the resultant images, it is important that a standard set of filters be used. One such standard is the Cousins set. The set contains five filters UBI filters. It is not necessary to use all five filters in order to gather photometric data [6]. In this paper we use only three filters (B). Surface photometry is an important tool in understanding the galaxy mass and structure. Obtaining the structural characteristics and the total luminosity of a galaxy requires knowledge of a surface brightness profile. During a surface photometry project to explore the structure of galaxies by morphological type [1]. Observations, data reduction and photometric calibration In this section we will concentrate on the kind of optical telescope, the processing that implied to manipulate the data and photometric calibration. Observations The observations were obtained in March 2011at the Newtonian focus of the (1.88 m) reflector telescope which has a focal length of (9.15 m) at KAO Egypt. With broadband B,, and this CCD array realizes a photometric system close to the standard Johnson Cousins UBI system. The array was cooled with liquid nitrogen. The size of the array is x pixels, providing an image scale of arcsec/pixel. Table 1 illustrates an observing log. 9
3 Iraqi Journal of Physics, 2017 ol.15, No.35, PP Table 1: Log of observations. Date of observation The name of the Galaxy Filters Time exposure (sec) 2011/3/25-26 NGC 4448 B 5 x x x 600 Seeing air mass 1.81" Data reduction We performed the preliminary reduction of the images. To correct for electron bias and the effect of hot pixels and bad columns of the CCD array, a dark frame that was the average of several exposures taken with a closed shutter and the same integration time as for the object subtracted. Summed frames of the twilight sky are used, then divided each image by its flat field to correct for the nonuniform sensitivity of the detector pixels. To performed the subsequent data reduction by using a standard procedure incorporating Astronomical Image Processing Packages software IAF [7-11]. Photometric calibration The photometric calibration of the galaxies NGC 4448 is based on standard stars PG ; from the list of the Landolt standard stars [12] observed on the each night, the instrumental magnitudes were transformed to the standard Johnson- Cousins UBI system. The images of galaxies NGC 4448 is recorded on CCD camera using B, and filters. These images are demonstrated in Fig.1. a b c Fig.1: CCD image of NGC 4448 before reduction (a) B filter (b) filter (c) filter. 10
4 Iraqi Journal of Physics, 2017 The output of the data reduction process for the galaxies NGC 4448 are shown in Fig. 2. The results illustrate a clean background a b c Fig. 2: CCD image of NGC 4448 after reduction (a) B filter (b) filter (c) filter. Data analysis and results NGC 4448 is a barred spiral galaxy with a prominent inner ring structure in the constellation Coma Berenices. Fig.3 represents the photometric profiles along the major axis of the galaxy NGC 4448 using B, and filters which are symmetric about the center. It s so clear that the galaxy possesses a large bright core. From this figure the diameter of the nucleus and the bulge are estimated and they were found to be 8 and 14 arcsec respectively. A way from the center of the bulge, the emission is purely dominated by the contribution of the disc of the galaxy. The far end of Fig. 3 represents the emission of the contribution of the arms of the galaxy. The maximum surface brightness at the center of the nucleus (, and ). The eastern part of the galaxy is brighter than the western part by ( ) in the band ( ) as opposed to ( ). 11
5 Ellipticity P.A ( Degree ) B,, ( Mag/arcsec 2 ) Iraqi Journal of Physics, 2017 ol.15, No.35, PP B adius ( arcsec ) Fig.3: Photometric profiles along the major axis of NGC Figs.(4a) and (4b) show the unusual dependence for the ellipticity and position angle of the isophotes on distance from the center. The circumnuclear region has nearly circular isophotes ( ) oriented in position angle Further variations in the position angle and, in part, the ellipticity of the isophotes are associated with the fact that the center of the bright ring does not coincide with the center of the galaxy s nucleus at distances r > from the center B a b B adius ( arcsec ) adius ( arcsec ) Fig. 4: (a) Isophote ellipticity (b) position angle of the galaxy P. A as a function of the distance r to the center of NGC Fig. 5 shows the (B-) and (-) color indices along the major axis of NGC The galaxy becomes bluer with distance from the center, most strongly in (B-). (B-) varies from in the nucleus to at the periphery of the galaxy; the corresponding indices for (-) are 0.85 mag and 0.35 mag respectively. The color indices in the bar for (B-) is 1.05 mag, and for (-) is 0.77 mag. 12
6 Color Indices ( Mag ) Iraqi Journal of Physics, B adius ( arcsec ) Fig.5: Profiles of the color indices along the major axis of the galaxy NGC Conclusions The eastern part of the galaxy NGC 4448 is brighter than the western part. This means that the brighter part have many constellations of young stars than that of lower brightness. NGC 4448 is one of the bluest galaxies in its class, and star formation has actively occurred. The star formation rate in the nucleus and spiral arms has remained virtually constant in time (as we can conclude from their positions in twocolor diagrams). This means that either the efficiency of star formation has increased in time in these regions or there is a constant input of gas to the nucleus and spiral arms of the galaxy. eferences: [1] J. Schombert and A.K. Smith, Systematic Bias in 2MASS Galaxy Photometry. astroph.im.arxiv: v1 [2] P.A.Martinez. "A Practical Guide to CCD Astronomy". Cambridge University, [3].Wodaski. on. "The New CCD Astronomy" New Astronomy Press., [4] Zeilik, Michael and Stephen Gregory. "Astronomy and Astrophysics".4 th ed. Saunders College Publishing, [5] S. B. Howell, "Handbook of CCD Astronomy". Cambridge: Cambridge University Press [6] W. J. Kaufman and G. A. Freedman, "Universe" (5 th Ed.). New York: W. H. Freeman and Company, [7] S.H. Ali and S.A. Albakri, Iraqi Journal of Physics, 12, 24 (2014) [8] A. Halton, "Atlas of Peculiar Galaxies". Astronomy and Astrophysics Journal, 14 (1966) 1A. [9] H.M. Hernandez, J.D. Zendejas,.. Avila, The Astronomical Journal, 134 (2007) [10] A.S. Gusev and S.S. Kaisin, Astronomy eports, 46, 9 (2002) [11] S.H. Ali, Iraqi Journal of Science, 56, 3A (2015) [12] Landolt, Astronomy Journal, 104, 340 (1992). 13
STRUCTURE OF GALAXIES
STRUCTURE OF GALAXIES 2., classification, surface photometry Piet van der Kruit Kapteyn Astronomical Institute University of Groningen the Netherlands February 2010, classification, surface photometry
More informationReduction procedure of long-slit optical spectra. Astrophysical observatory of Asiago
Reduction procedure of long-slit optical spectra Astrophysical observatory of Asiago Spectrograph: slit + dispersion grating + detector (CCD) It produces two-dimension data: Spatial direction (x) along
More informationA Tour of the Messier Catalog. ~~ in ~~ Eight Spellbinding and Enlightening Episodes. ~~ This Being Episode Three ~~
A Tour of the Messier Catalog ~~ in ~~ Eight Spellbinding and Enlightening Episodes ~~ This Being Episode Three ~~ Globulars and Galaxies Warm-up for The Realm M83 Spiral Galaxy Constellation Hydra
More informationFigure 1: (Image Credit)
Ricky Leon Murphy HET609 Semester 1 2005 Project 83 May 30, 2005 Spiral Galaxy Morphology and a Comparison of Four Spiral Galaxies Stars are grouped into island universes called galaxies and there are
More informationAstronomical imagers. ASTR320 Monday February 18, 2019
Astronomical imagers ASTR320 Monday February 18, 2019 Astronomical imaging Telescopes gather light and focus onto a focal plane, but don t make perfect images Use a camera to improve quality of images
More informationProblem Solving. radians. 180 radians Stars & Elementary Astrophysics: Introduction Press F1 for Help 41. f s. picture. equation.
Problem Solving picture θ f = 10 m s =1 cm equation rearrange numbers with units θ factors to change units s θ = = f sinθ fθ = s / cm 10 m f 1 m 100 cm check dimensions 1 3 π 180 radians = 10 60 arcmin
More informationModern Image Processing Techniques in Astronomical Sky Surveys
Modern Image Processing Techniques in Astronomical Sky Surveys Items of the PhD thesis József Varga Astronomy MSc Eötvös Loránd University, Faculty of Science PhD School of Physics, Programme of Particle
More informationGalaxy classification
Galaxy classification Questions of the Day What are elliptical, spiral, lenticular and dwarf galaxies? What is the Hubble sequence? What determines the colors of galaxies? Top View of the Milky Way The
More informationInfra-red imaging of perpendicular nested bars in spiral galaxies with the Infra-red Camera at the Carlos Sanchez Telescope
Infra-red imaging of perpendicular nested bars in spiral galaxies with the Infra-red Camera at the Carlos Sanchez Telescope S.N. Kemp (skemp@ll.iac.es) Instituto de Astrofísica de Canarias, E-38200 La
More informationCorotation Resonance of Nonbarred Spiral Galaxies. A Research work By Arjun Karki with Prof. Marc Seigar (Research advisor)
Corotation Resonance of Nonbarred Spiral Galaxies A Research work By Arjun Karki with Prof. Marc Seigar (Research advisor) Outline Motivation / Objective Introduction - Density Wave Theory - Corotation
More informationCorotation Resonance of Non-barred Spiral Galaxies
Corotation Resonance of Non-barred Spiral Galaxies A Research work By Arjun Karki Kark with Prof. Marc Seigar (Research advisor) Outline Motivation / Objective Introduction - Density wave theory - Corotation
More informationAstronomy 114. Lecture 27: The Galaxy. Martin D. Weinberg. UMass/Astronomy Department
Astronomy 114 Lecture 27: The Galaxy Martin D. Weinberg weinberg@astro.umass.edu UMass/Astronomy Department A114: Lecture 27 18 Apr 2007 Read: Ch. 25,26 Astronomy 114 1/23 Announcements Quiz #2: we re
More informationSTUDIES OF SELECTED VOIDS. SURFACE PHOTOMETRY OF FAINT GALAXIES IN THE DIRECTION OF IN HERCULES VOID
STUDIES OF SELECTED VOIDS. SURFACE PHOTOMETRY OF FAINT GALAXIES IN THE DIRECTION OF 1600+18 IN HERCULES VOID G.Petrov [1], A.Y.Kniazev [2], and J.W. Fried [2] 1 Institute of Astronomy, Bulgarian Academy
More informationYou, too, can make useful and beautiful astronomical images at Mees: Lesson 3
You, too, can make useful and beautiful astronomical images at Mees: Lesson 3 Calibration and data reduction Useful references, besides Lessons 1 and 2: The AST 142 Projects manual: http://www.pas.rochester.edu/~dmw/ast142/projects/project.pdf
More informationThe Milky Way. Overview: Number of Stars Mass Shape Size Age Sun s location. First ideas about MW structure. Wide-angle photo of the Milky Way
Figure 70.01 The Milky Way Wide-angle photo of the Milky Way Overview: Number of Stars Mass Shape Size Age Sun s location First ideas about MW structure Figure 70.03 Shapely (~1900): The system of globular
More informationSKINAKAS OBSERVATORY. Astronomy Projects for University Students PROJECT GALAXIES
PROJECT 7 GALAXIES Objective: The topics covered in the previous lessons target celestial objects located in our neighbourhood, i.e. objects which are within our own Galaxy. However, the Universe extends
More informationActive Nuclei and their Host Galaxies: Observations of Seyfert Galaxies
Active Nuclei and their Host Galaxies: Observations of Seyfert Galaxies Samuel Harrold 1 and Joel Kajubi 1 1 Department of Physics and Astronomy, University of Rochester, Rochester, NY 14627 Abstract We
More informationLaboratory: Milky Way
Department of Physics and Geology Laboratory: Milky Way Astronomy 1402 Equipment Needed Quantity Equipment Needed Quantity Milky Way galaxy Model 1 Ruler 1 1.1 Our Milky Way Part 1: Background Milky Way
More informationFoundations of Astronomy 13e Seeds. Chapter 6. Light and Telescopes
Foundations of Astronomy 13e Seeds Chapter 6 Light and Telescopes Guidepost In this chapter, you will consider the techniques astronomers use to study the Universe What is light? How do telescopes work?
More information* All those going out on the roof at night must carry a torch.
University of Exeter Observatory User Note: Observatory safety Tim Harries, September 2003 Observatory Safety Working at night in proximity to moving equipment is potentially hazardous, and safety is our
More informationA Random Walk Through Astrometry
A Random Walk Through Astrometry Astrometry: The Second Oldest Profession George H. Kaplan Astronomical Applications Department Astrometry Department U.S. Naval Observatory Random Topics to be Covered
More informationOBSERVING THE VARIABILITY OF AGN: APERTURE PHOTOMETRY VS. PSF FITTING. Eric C. Allan. A senior thesis submitted to the faculty of
OBSERVING THE VARIABILITY OF AGN: APERTURE PHOTOMETRY VS. PSF FITTING by Eric C. Allan A senior thesis submitted to the faculty of Brigham Young University in partial fulfillment of the requirements for
More informationBV R photometry of comparison stars in selected blazar fields
ASTRONOMY & ASTROPHYSICS JUNE I 1998, PAGE 305 SUPPLEMENT SERIES Astron. Astrophys. Suppl. Ser. 130, 305 310 (1998) BV R photometry of comparison stars in selected blazar fields I. Photometric sequences
More informationChapter 15 The Milky Way Galaxy. The Milky Way
Chapter 15 The Milky Way Galaxy The Milky Way Almost everything we see in the night sky belongs to the Milky Way We see most of the Milky Way as a faint band of light across the sky From the outside, our
More informationCitation for published version (APA): Fathi, K. (2004). Dynamics and morphology in the inner regions of spiral galaxies Groningen: s.n.
University of Groningen Dynamics and morphology in the inner regions of spiral galaxies Fathi, Kambiz IMPORTANT NOTE: You are advised to consult the publisher's version (publisher's PDF) if you wish to
More informationAstronomical "color"
Astronomical "color" What color is the star Betelgeuse? It's the bright star at upper left in this picture of Orion taken by a student at the RIT Observatory. Orange? Red? Yellow? These are all reasonable
More informationWHAT PHOTOMETRIC PRECISION CAN I ACHIEVE? DAVID BOYD
WHAT PHOTOMETRIC PRECISION CAN I ACHIEVE? DAVID BOYD If you start using a CCD camera to carry out photometry on variable stars, this is a question that sooner or later you will ask yourself. Prompted by
More informationPhotometric Calibration of the CCD Camera of 1-m Telescope at VBO
J. Astrophys. Astr.(1991) 12, 319 331 Photometric Calibration of the CCD Camera of 1-m Telescope at VBO Y. D. Mayya* Indian Institute of Astrophysics, Bangalore 560034 Received 1991 July 7; accepted 1991
More informationSurface Photometry Quantitative description of galaxy morphology. Hubble Sequence Qualitative description of galaxy morphology
Hubble Sequence Qualitative description of galaxy morphology Surface Photometry Quantitative description of galaxy morphology Galaxy structure contains clues about galaxy formation and evolution Point
More informationThe Optical Microvariability and Spectral Changes of the BL Lacertae Object S
J. Astrophys. Astr. (2011) 32, 97 103 c Indian Academy of Sciences The Optical Microvariability and Spectral Changes of the BL Lacertae Object S5 0716+714 H. Poon 1,, J.H.Fan 2 & J.N.Fu 1 1 Astronomy Department,
More informationAstroBITS: Open Cluster Project
AstroBITS: Open Cluster Project I. Introduction The observational data that astronomers have gathered over many years indicate that all stars form in clusters. In a cloud of hydrogen gas, laced with helium
More informationBV RI photometric sequences for nine selected dark globules
ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES Astron. Astrophys. Suppl. Ser. 126, 73-80 (1997) NOVEMBER II 1997, PAGE73 BV RI photometric sequences for nine selected dark globules J.F. Lahulla 1, A. Aguirre
More informationarxiv: v1 [astro-ph.im] 31 Jul 2014
A new method of CCD dark current correction via extracting the dark information from scientific images arxiv:1407.8279v1 [astro-ph.im] 31 Jul 2014 Bin Ma 1, Zhaohui Shang 2,1, Yi Hu 1, Qiang Liu 1, Lifan
More informationLecture 25 The Milky Way Galaxy November 29, 2017
Lecture 25 The Milky Way Galaxy November 29, 2017 1 2 Size of the Universe The Milky Way galaxy is very much larger than the solar system Powers of Ten interactive applet 3 Galaxies Large collections of
More informationImaging with SPIRIT Exposure Guide
Imaging with SPIRIT Exposure Guide SPIRIT optical telescopes utilise extremely sensitive cameras to record the light from distant astronomical objects. Even so, exposures of several seconds up to a few
More informationCCD Double-Star Measurements at Altimira Observatory in 2007
Page 27 CCD Double-Star Measurements at Altimira Observatory in 2007 Robert K. Buchheim Altimira Observatory (G76) 18 Altimira Coto de Caza, CA 92679 Email: RBuchheim@earthlink.net Abstract: CCD measurements
More informationASTRO 310: Galac/c & Extragalac/c Astronomy Prof. Jeff Kenney. Class 17 Mar 30, 2016 Starlight Distribu/ons in Disk Galaxies
ASTRO 310: Galac/c & Extragalac/c Astronomy Prof. Jeff Kenney Class 17 Mar 30, 2016 Starlight Distribu/ons in Disk Galaxies reminder no class next Monday, April 3!! 3 Color op/cal image of spiral galaxy
More informationOPTICAL PHOTOMETRY. Observational Astronomy (2011) 1
OPTICAL PHOTOMETRY Observational Astronomy (2011) 1 The optical photons coming from an astronomical object (star, galaxy, quasar, etc) can be registered in the pixels of a frame (or image). Using a ground-based
More informationOpen Cluster Photometry: Part II
Project 4 Open Cluster Photometry: Part II Observational Astronomy ASTR 310 Fall 2005 1 Introduction The objective of this and the previous project is to learn how to produce color-magnitude diagrams of
More informationPHYSICS Observing Guide
PHYSICS 123-253 Observing Guide v1.4 November 2013 TEAMWORK Working in pairs or groups is quite common in science labs, and this lab is no exception. Teamwork can be quite effective; it's often possible
More informationAnalyzing Spiral Galaxies Observed in Near-Infrared
Analyzing Spiral Galaxies Observed in Near-Infrared Preben Grosbøl European Southern Observatory Karl-Schwarzschild-Str. 2, D-85748 Garching, Germany Abstract A sample of 54 spiral galaxies was observed
More informationSpitzer Space Telescope
Spitzer Space Telescope (A.K.A. The Space Infrared Telescope Facility) The Infrared Imaging Chain 1/38 The infrared imaging chain Generally similar to the optical imaging chain... 1) Source (different
More information1 Lecture, 2 September 1999
1 Lecture, 2 September 1999 1.1 Observational astronomy Virtually all of our knowledge of astronomical objects was gained by observation of their light. We know how to make many kinds of detailed measurements
More informationThe HII Regions of Sextans A
Publications of the Astronomical Society of the Pacific 6: 765-769, 1994 July The HII Regions of Sextans A Paul Hodge 1 Astronomy Department, University of Washington, Seattle, Washington 98195 Electronic
More informationStudy of Physical Characteristics of High Apogee Space Debris
Study of Physical Characteristics of High Apogee Space Debris Yongna Mao, Jianfeng Wang, Xiaomeng Lu, Liang Ge, Xiaojun Jiang (National Astronomical Observatories, Beijing, 100012, China) Abstract Date
More informationThe Extragalactic Distance Database: Hawaii Photometry Catalog
The Extragalactic Distance Database: Hawaii Photometry Catalog Hélène M. Courtois Université Lyon, CNRS/IN2P3/INSU, Institut de Physique Nucléaire, Lyon, France and Institute for Astronomy, University
More informationChapter 6: Transforming your data
Why is transformation necessary? Chapter 6: Transforming your data The AAVSO International Database is composed of data collected from many different observers, at different times, from around the globe.
More informationLow Surface Brightness Galaxies Erwin de Blok. Encyclopedia of Astronomy & Astrophysics P. Murdin
eaa.iop.org DOI: 10.1888/0333750888/2620 Low Surface Brightness Galaxies Erwin de Blok From Encyclopedia of Astronomy & Astrophysics P. Murdin IOP Publishing Ltd 2006 ISBN: 0333750888 Institute of Physics
More informationIntroduction to SDSS -instruments, survey strategy, etc
Introduction to SDSS -instruments, survey strategy, etc (materials from http://www.sdss.org/) Shan Huang 17 February 2010 Survey type Status Imaging and Spectroscopy Basic Facts SDSS-II completed, SDSS-III
More informationChapter 5: Telescopes
Chapter 5: Telescopes You don t have to know different types of reflecting and refracting telescopes. Why build bigger and bigger telescopes? There are a few reasons. The first is: Light-gathering power:
More informationEnergy Sources of the Far IR Emission of M33
Energy Sources of the Far IR Emission of M33 Hinz, Reike et al., ApJ 154: S259 265 (2004). Presented by James Ledoux 24 µm 70 µm 160 µm Slide 1 M33 Properties Distance 840kpc = 2.7 Mlyr (1'' ~ 4 pc) Also
More informationDOME C AS A SETTING FOR THE PERMANENT ALL SKY SURVEY (PASS)
Title : will be set by the publisher Editors : will be set by the publisher EAS Publications Series, Vol.?, 2005 DOME C AS A SETTING FOR THE PERMANENT ALL SKY SURVEY (PASS) H.J. Deeg, J.A. Belmonte, R.
More information11 days exposure time. 10,000 galaxies. 3 arcminutes size (0.1 x diameter of moon) Estimated number of galaxies in observable universe: ~200 billion
11 days exposure time 10,000 galaxies 3 arcminutes size (0.1 x diameter of moon) Estimated number of galaxies in observable universe: ~200 billion Galaxies with disks Clumpy spiral shapes Smooth elliptical
More informationStellar Photometry: II. Transforming. Ast 401/Phy 580 Fall 2015
Stellar Photometry: II. Transforming Ast 401/Phy 580 Fall 2015 Summary We ve learned how to measure instrumental magnitudes for a star using aperture photometry or PSF-fitting: (a) Add up all of the counts
More informationCross-Talk in the ACS WFC Detectors. I: Description of the Effect
Cross-Talk in the ACS WFC Detectors. I: Description of the Effect Mauro Giavalisco August 10, 2004 ABSTRACT Images acquired with the Wide Field Channel (WFC) of the Advanced Camera for Surveys (ACS) are
More informationAn Introduction to Galaxies and Cosmology. Jun 29, 2005 Chap.2.1~2.3
An Introduction to Galaxies and Cosmology Jun 29, 2005 Chap.2.1~2.3 2.1 Introduction external galaxies normal galaxies - majority active galaxies - 2% high luminosity (non-stellar origin) variability
More informationExploring Data. Keck LRIS spectra. Handbook of CCD Astronomy by Steve Howell Chap. 4, parts of 6
Exploring Data Keck LRIS spectra Handbook of CCD Astronomy by Steve Howell Chap. 4, parts of 6 FITS: Flexible Image Transport System Digital file format used to store astronomical images, data, and catalogs.
More informationInfrared Mass-to-Light Profile Throughout the Infall Region of the Coma Cluster
Infrared Mass-to-Light Profile Throughout the Infall Region of the Coma Cluster K. Rines 1, M.J. Geller 2, M.J. Kurtz 1, A. Diaferio 3, T.H. Jarrett 4, and J.P. Huchra 1 ABSTRACT Using a redshift survey
More information1 A photometric probe for Pan-STARRS
The Pan-STARRS Imaging Sky Probe B.R. Granett, K.C. Chambers, E.A. Magnier, K. Fletcher and the Pan-STARRS Project Team University of Hawai i Institute for Astronomy Abstract Photometric performance is
More informationChapter 5. Telescopes. Dr. Tariq Al-Abdullah
Chapter 5 Telescopes The Tools of Astronomy Dr. Tariq Al-Abdullah Learning Goals: 5.1 Optical Telescopes (The Hubble Space Telescope) 5.2 Telescope Size 5.3 Images and Detectors 5.4 High-Resolution Astronomy
More informationExtra Gal 9: Photometry & Dynamics
Extra Gal 9: Photometry & Dynamics Two books, among many others, that can be used by the studenys for extensive references and details are: Binney and Merrifield: Galactic Astronomy Binney and Tremaine
More informationExponential Profile Fitting on the Unusual SAB(s)bc galaxy M106 Alex K Chen Astronomy Department, University of Washington
Exponential Profile Fitting on the Unusual SAB(s)bc galaxy M106 Alex K Chen Astronomy Department, University of Washington Abstract M106 is a late type spiral galaxy with an inclination of 64 degrees.
More informationView of the Galaxy from within. Lecture 12: Galaxies. Comparison to an external disk galaxy. Where do we lie in our Galaxy?
Lecture 12: Galaxies View of the Galaxy from within The Milky Way galaxy Rotation curves and dark matter External galaxies and the Hubble classification scheme Plotting the sky brightness in galactic coordinates,
More informationJournal Club Presentation on The BIMA Survey of Nearby Galaxies. I. The Radial Distribution of CO Emission in Spiral Galaxies by Regan et al.
Journal Club Presentation on The BIMA Survey of Nearby Galaxies. I. The Radial Distribution of CO Emission in Spiral Galaxies by Regan et al. ApJ, 561:218-237, 2001 Nov 1 1 Fun With Acronyms BIMA Berkely
More informationOptics and Telescopes
Optics and Telescopes Guiding Questions 1. Why is it important that telescopes be large? 2. Why do most modern telescopes use a large mirror rather than a large lens? 3. Why are observatories in such remote
More informationSKINAKAS OBSERVATORY Astronomy Projects for University Students COLOUR IN ASTRONOMY
P R O J E C T 3 COLOUR IN ASTRONOMY Objective: Explain what colour means in an astronomical context and its relationship with the temperature of a star. Learn how to create colour-colour diagrams and how
More informationOptical and Near- Infrared Photometric Study of NGC 6724
Research in Astron. Astrophys. Vol.0 (201x) No.0, 000 000 http://www.raa-journal.org http://www.iop.org/journals/raa Research in Astronomy and Astrophysics Optical and Near- Infrared Photometric Study
More informationIN REPORT: Plate Scale and FOV of CCD for Each Telescope using Albireo Stars
USE ASTROIMAGEJ NOT AIP4WIN To download ALL the public data from Canvas, go to Files, then click the 3 dots next to the Public Data Folder and click Download. It will download all the files at once. 6.1
More informationDetermining colours of NGC 1073 Sjoerd Hardeman and Thijs Coenen University of Amsterdam Faculty of Science
Determining colours of NGC 1073 Sjoerd Hardeman and Thijs Coenen University of Amsterdam Faculty of Science Determining colours of NGC 1073 Sjoerd Hardeman and Thijs Coenen University of Amsterdam Faculty
More informationTNG photometry of the open cluster NGC 6939
Mem. S.A.It. Vol. 75, 19 c SAIt 2004 Memorie della TNG photometry of the open cluster NGC 6939 G. Andreuzzi 1, A. Bragaglia 2, M. Tosi 2 and G. Marconi 3 1 INAF Osservatorio Astronomico di Roma, via Frascati
More informationActive Galaxies & Quasars
Active Galaxies & Quasars Normal Galaxy Active Galaxy Galactic Nuclei Bright Active Galaxy NGC 5548 Galaxy Nucleus: Exact center of a galaxy and its immediate surroundings. If a spiral galaxy, it is the
More informationThe Milky Way Galaxy. Some thoughts. How big is it? What does it look like? How did it end up this way? What is it made up of?
Some thoughts The Milky Way Galaxy How big is it? What does it look like? How did it end up this way? What is it made up of? Does it change 2 3 4 5 This is not a constant zoom The Milky Way Almost everything
More information1. Give short answers to the following questions. a. What limits the size of a corrected field of view in AO?
Astronomy 418/518 final practice exam 1. Give short answers to the following questions. a. What limits the size of a corrected field of view in AO? b. Describe the visibility vs. baseline for a two element,
More informationLecture 15: Galaxy morphology and environment
GALAXIES 626 Lecture 15: Galaxy morphology and environment Why classify galaxies? The Hubble system gives us our basic description of galaxies. The sequence of galaxy types may reflect an underlying physical
More informationLecture 12: Distances to stars. Astronomy 111
Lecture 12: Distances to stars Astronomy 111 Why are distances important? Distances are necessary for estimating: Total energy released by an object (Luminosity) Masses of objects from orbital motions
More informationASTR 2310: Chapter 6
ASTR 231: Chapter 6 Astronomical Detection of Light The Telescope as a Camera Refraction and Reflection Telescopes Quality of Images Astronomical Instruments and Detectors Observations and Photon Counting
More informationTelescopes, Observatories, Data Collection
Telescopes, Observatories, Data Collection Telescopes 1 Astronomy : observational science only input is the light received different telescopes, different wavelengths of light lab experiments with spectroscopy,
More informationThe Milky Way Galaxy (ch. 23)
The Milky Way Galaxy (ch. 23) [Exceptions: We won t discuss sec. 23.7 (Galactic Center) much in class, but read it there will probably be a question or a few on it. In following lecture outline, numbers
More informationarxiv: v1 [astro-ph] 3 Oct 2007
Peremennye Zvezdy 27, No.4, 2007 Variable Stars 27, No.4, 2007 SAI, INASAN, Astronet.ru Moscow, Russia 3 October 2007 arxiv:0710.0765v1 [astro-ph] 3 Oct 2007 PHOTOMETRIC OBSERVATIONS OF SUPERNOVA 2002hh
More informationLecture Outlines. Chapter 24. Astronomy Today 8th Edition Chaisson/McMillan Pearson Education, Inc.
Lecture Outlines Chapter 24 Astronomy Today 8th Edition Chaisson/McMillan Chapter 24 Galaxies Units of Chapter 24 24.1 Hubble s Galaxy Classification 24.2 The Distribution of Galaxies in Space 24.3 Hubble
More informationChapter 6 Light and Telescopes
Chapter 6 Light and Telescopes Guidepost In the early chapters of this book, you looked at the sky the way ancient astronomers did, with the unaided eye. In chapter 4, you got a glimpse through Galileo
More informationAn analogy. "Galaxies" can be compared to "cities" What would you like to know about cities? What would you need to be able to answer these questions?
An analogy "Galaxies" can be compared to "cities" What would you like to know about cities? how does your own city look like? how big is it? what is its population? history? how did it develop? how does
More informationA PRELIMINARY CLASSIFICATION SCHEME FOR THE CENTRAL REGIONS OF LATE-TYPE GALAXIES
A PRELIMINARY CLASSIFICATION SCHEME FOR THE CENTRAL REGIONS OF LATE-TYPE GALAXIES SIDNEY VAN DEN BERGH* Dominion Astrophysical Observatory, National Research Council 5071 West Saanich Road, Victoria, B.C.,
More informationLab 7: The H-R Diagram of an Open Cluster
Lab 7: The H-R Diagram of an Open Cluster Due Date: 2007 Nov 27 (after thanksgiving) 1 Introduction: The HR Diagram In this two week project you will do absolute (not differential) photometry with a CCD
More informationHigh quality seeing V, I and Gunn z imaging of Terzan 4: a blue horizontal branch bulge globular cluster
Astron. Astrophys. 319, 850 854 (1997) ASTRONOMY AND ASTROPHYSICS High quality seeing V, I and Gunn z imaging of Terzan 4: a blue horizontal branch bulge globular cluster S. Ortolani 1, B. Barbuy 2, and
More informationUrban Observer. Loose Core Globular Clusters NGC 288 & by David Nakamoto
Urban Observer Loose Core Globular Clusters NGC 288 & 2419 by David Nakamoto dinakamoto@hotmail.com Star clusters make for nice objects for urban observers, both visually and photographically. I think
More information3D Spectroscopy to Dissect Galaxies Down to Their Central Supermassive Black Holes. Kambiz Fathi. Stockholm University, Sweden
3D Spectroscopy to Dissect Galaxies Down to Their Central Supermassive Black Holes Kambiz Fathi Stockholm University, Sweden Towards a better understanding of the Hubble Diagram Towards a better understanding
More informationGalaxies. The majority of known galaxies fall into one of three major classes: spirals (78 %), ellipticals (18 %) and irregulars (4 %).
Galaxies Collection of stars, gas and dust bound together by their common gravitational pull. Galaxies range from 10,000 to 200,000 light-years in size. 1781 Charles Messier 1923 Edwin Hubble The distribution
More informationVRI photometry of stars in the fields of 12 BL Lacertae objects
ASTRONOMY & ASTROPHYSICS MAY I 1996, PAGE 403 SUPPLEMENT SERIES Astron. Astrophys. Suppl. Ser. 116, 403-407 (1996) VRI photometry of stars in the fields of 12 BL Lacertae objects M. Fiorucci and G. Tosti
More informationarxiv:astro-ph/ v1 20 Feb 2004
Discovery of Face-On Counterparts of Chain Galaxies in the Tadpole ACS Field arxiv:astro-ph/42477v1 Feb 4 Debra Meloy Elmegreen Vassar College, Dept. of Physics & Astronomy, Box 745, Poughkeepsie, NY 1264;
More informationPart two of a year-long introduction to astrophysics:
ASTR 3830 Astrophysics 2 - Galactic and Extragalactic Phil Armitage office: JILA tower A909 email: pja@jilau1.colorado.edu Spitzer Space telescope image of M81 Part two of a year-long introduction to astrophysics:
More informationVariable Stars Advanced Lab
Variable Stars Advanced Lab Introduction In this lab, you will be observing several variable stars to determine the period and classification of the star. A variable star is considered any star which goes
More informationA survey of the ISM in early-type galaxies
ASTRONOMY & ASTROPHYSICS APRIL II 1999, PAGE 269 SUPPLEMENT SERIES Astron. Astrophys. Suppl. Ser. 136, 269 284 (1999) A survey of the ISM in early-type galaxies II. The dust F. Ferrari 1, M.G. Pastoriza
More informationPhotometric Studies of GEO Debris
Photometric Studies of GEO Debris Patrick Seitzer Department of Astronomy, University of Michigan 500 Church St. 818 Dennison Bldg, Ann Arbor, MI 48109 pseitzer@umich.edu Heather M. Cowardin ESCG/Jacobs
More informationThe magnitude system. ASTR320 Wednesday January 30, 2019
The magnitude system ASTR320 Wednesday January 30, 2019 What we measure: apparent brightness How bright a star appears to be in the sky depends on: How bright it actually is Luminosity and its distance
More informationBright Quasar 3C 273 Thierry J-L Courvoisier. Encyclopedia of Astronomy & Astrophysics P. Murdin
eaa.iop.org DOI: 10.1888/0333750888/2368 Bright Quasar 3C 273 Thierry J-L Courvoisier From Encyclopedia of Astronomy & Astrophysics P. Murdin IOP Publishing Ltd 2006 ISBN: 0333750888 Institute of Physics
More informationBHS Astronomy: Galaxy Classification and Evolution
Name Pd Date BHS Astronomy: Galaxy Classification and Evolution This lab comes from http://cosmos.phy.tufts.edu/~zirbel/ast21/homework/hw-8.pdf (Tufts University) The word galaxy, having been used in English
More informationCapturing and Processing Deep Space Images. Petros Pissias Eumetsat Astronomy Club 15/03/2018
Capturing and Processing Deep Space Images Petros Pissias Eumetsat Astronomy Club 15/03/2018 Agenda Introduction Basic Equipment Preparation Acquisition Processing Quick demo Petros Pissias Eumetsat Astronomy
More informationIntroduction and Background:
Introduction and Background: Often times identifying the characteristics of extreme examples of galaxy morphology and properties (e.g. Perseus A, Malin 1, NGC 1569) provides very important constraints
More informationSetting UBVRI Photometric Zero-Points Using Sloan Digital Sky Survey ugriz Magnitudes
University of Nebraska - Lincoln DigitalCommons@University of Nebraska - Lincoln Martin Gaskell Publications Research Papers in Physics and Astronomy 10-1-2007 Setting UBVRI Photometric Zero-Points Using
More information