LSB Galaxies Detection Using Markovian Segmentation on Astronomical Images
|
|
- Nathan Arnold
- 5 years ago
- Views:
Transcription
1 LSB Galaxies Detection Using Markovian Segmentation on Astronomical Images Mireille Louys 1, Benjamin Perret 1 Bernd Vollmer 2, François Bonnarel 2 Sebastien Lefèvre 1, Christophe Collet 1 1 Laboratoire des Sciences de l Informatique, de l Image et de la Télédétection 2 Centre de donnees astronomiques de Strasbourg,
2 Rationale Surface brightness is highly variable from one galaxy to another (Disney, 1976) Low surface brightness galaxies are close to the image background level and satisfy: SB > 22.5 mag.arcsec -2 Found inside and outside galaxy clusters How complete are our detections? More understanding in the baryonic fraction of the Dark Matter in the universe 2
3 Noise and background Easy case More difficult 3
4 Overview Original Image Segmentation Map Objects list Segmentation Objects Profiles Fitting Selection Visual Inspection and Validation Markovian Quadtree 3D mathematical morphology DetectLSB Ellipse parameters Fit error Magnitude profile LinLog, LinLin Measured Surface brightness Estimated Surface brightness Scale length VO Objects list VOTable XML
5 Markovian segmentation The goal is to classify pixel values and discriminate bright objects, sky background and faint sources to be considered later as LSB candidates. It works as an inverse method : Try to find the Bayesian estimate of the most likely class partition that maps the observation We make 2 assumptions : on the noise and inner class statistics (here gaussian), on the statistical phenomenon: Markovian quadtree. 5
6 Markovian quadtree The succesive tree levels correspond to increasing scales of the image. We want to compute the a posteriori probability of having site s in one class c, knowing the observation Ys and the class number of the parent node within the Markov tree. The Quadtree provides an in-scale regularisation framework, providing exact and non iterative solution It is fully applicable to multiband observations 6
7 Steps achieved with DetectLSB For each detection map: Identify pixel connected components Remove very extended components : > 300 pixels Remove components at the edges of the image Ellipse fitting Luminosity profile analysis Selection criteria: Sort out stars according to their profile (steep slope, etc.) Remove bad centered and/or overlaping objects (crowded regions) Check for central surface brightness 7
8 Luminosity profile analysis For each object in the detection map: Average profile along each ellipse radius f(r)=u 0 *exp( r/r 0 ) At least 3 points aligned above background level
9 Source Measurements Fitted SB Surface Brightness Radius Profile Fit Error
10 Data set B-images of a region of the Virgo cluster obtained with the Isaac Newton Telescope WFCS (Wild Field Camera Survey) Analysed by Sabina Sabatini et coll. in SABATINI S.; DAVIES J.; SCARAMELLA R.; SMITH R.; BAES M.; LINDER S.M.; ROBERTS S.; TESTA V. Mon. Not. R. Astron. Soc., 341, (2003). and provided to us as a test set Full data set = 80 images of 4096x2048 pixels Analysed: 18 images with X-match with the detection lists provided by the authors 10
11 Results on the INT data set Found 79 % of our LSB candidates are confirmed by Sabatini et al. 23 (Markov+detectLSB) compared to 29 (Sabatini) Found new LSB candidates The validation on the full data set is still an on-going collaboration effort with S. Sabatini and W. van Driel. 11
12 Conclusion The Markovian segmentation approach allows to study LSB candidates even in a noisy environment Multiband image analysis is beeing currently applied to the same data set in B band completed with I band First tests are promising Such a procedure has been implemented in the AIDA image processing workflow project at CDS (Cf Schaaff et al, this conference) 12
13 2 detections for the same object
Astronomical Object Detection with a Robust Hit-or-Miss Transform
Astronomical Object Detection with a Robust Hit-or-Miss Transform Benjamin Perret, Sébastien Lefèvre, Christophe Collet, Bernd Vollmer To cite this version: Benjamin Perret, Sébastien Lefèvre, Christophe
More informationA Robust Hit-or-Miss Transform For Template Matching Applied to Very Noisy Astronomical Images.
A Robust Hit-or-Miss Transform For Template Matching Applied to Very Noisy Astronomical Images. B. Perret S. Lefèvre Ch. Collet Laboratoire des Sciences de l Image, de l Informatique et de la Télédétection
More informationInferring Galaxy Morphology Through Texture Analysis
Inferring Galaxy Morphology Through Texture Analysis 1 Galaxy Morphology Kinman Au, Christopher Genovese, Andrew Connolly Galaxies are not static objects; they evolve by interacting with the gas, dust
More informationMultiband Segmentation of a Spectroscopic Line Data Cube: Application to the HI Data Cube of the Spiral Galaxy NGC 4254
EURASIP Journal on Applied Signal Processing 25:15, 2546 2558 c 25 Hindawi Publishing Corporation Multiband Segmentation of a Spectroscopic Line Data Cube: Application to the HI Data Cube of the Spiral
More informationObserving Dark Worlds
Observing Dark Worlds Project Overview In this project, we analyze images showing galaxies in space to predict the location of Dark Matter Halos (DMH), which by definition cannot be observed directly.
More informationMore Galaxies. Scaling relations Extragalactic distances Luminosity functions Nuclear black holes
More Galaxies Scaling relations Extragalactic distances Luminosity functions Nuclear black holes Tully-Fisher relation velocity profile of gas Luminosity vs velocity width WR In spirals, luminosity L ~
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 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 informationSTRUCTURE AND DYNAMICS OF GALAXIES
STRUCTURE AND DYNAMICS OF GALAXIES 3., classification of galaxies Piet van der Kruit Kapteyn Astronomical Institute University of Groningen, the Netherlands www.astro.rug.nl/ vdkruit Beijing, September
More informationSTRUCTURE 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 informationGSC : an RR Lyrae star with a ceasing Blazhko effect and three new variables in the field.
GSC 02626-00896: an RR Lyrae star with a ceasing Blazhko effect and three new variables in the field. Rainer Gröbel 1, 2 1) DE- 90542 Eckental, Germany rainer.groebel@web.de 2) Bundesdeutsche Arbeitsgemeinschaft
More informationClusters of galaxies
Clusters of galaxies Most galaxies belong to some larger bound structure. Conventionally consider groups and clusters, with characteristic properties: Groups Clusters Core radius 250 h -1 kpc 250 h -1
More informationStructure of the Milky Way. Structure of the Milky Way. The Milky Way
Key Concepts: Lecture 29: Our first steps into the Galaxy Exploration of the Galaxy: first attempts to measure its structure (Herschel, Shapley). Structure of the Milky Way Initially, star counting was
More informationDiscovery of eight lensing clusters of galaxies
. Article. SCIENCE CHINA Physics, Mechanics & Astronomy September 2014 Vol. 57 No. 9: 1809 1815 doi: 10.1007/s11433-014-5544-8 Discovery of eight lensing clusters of galaxies LIANG SuMing 1,2, WEN ZhongLue
More informationD4.2. First release of on-line science-oriented tutorials
EuroVO-AIDA Euro-VO Astronomical Infrastructure for Data Access D4.2 First release of on-line science-oriented tutorials Final version Grant agreement no: 212104 Combination of Collaborative Projects &
More informationTHE HUBBLE SEQUENCE. This use case explores the morphology of galaxies and their classification according to the Hubble Sequence.
THE HUBBLE SEQUENCE G. Iafrate (a), M. Ramella (a) e V. Bologna (b) (a) INAF - Astronomical Observatory of Trieste (b) Istituto Comprensivo S. Giovanni - Sc. Sec. di primo grado M. Codermatz" - Trieste
More informationThe dwarf LSB galaxy population of the Virgo Cluster I. The faint-end slope of the Luminosity Function.
Mon. Not. R. Astron. Soc. 000, 1 12 (2002) Printed 12 November 2018 (MN LATEX style file v1.4) The dwarf LSB galaxy population of the Virgo Cluster I. The faint-end slope of the Luminosity Function. S.
More informationGalaxies. Hubble's measurement of distance to M31 Normal versus other galaxies Classification of galaxies Ellipticals Spirals Scaling relations
Galaxies Hubble's measurement of distance to M31 Normal versus other galaxies Classification of galaxies Ellipticals Spirals Scaling relations Cepheids in M31 Up to 1920s, the Milky Way was thought by
More informationSUPPLEMENTARY INFORMATION
doi:10.1038/nature10669 Observations and data reduction The data used for this work were taken as part of the Strong-lensing at High Angular Resolution Program (SHARP) and will be discussed in detail by
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 informationREU Final Presentation: VERITAS Update. Summer 2011 Advisors: John Finley and Glenn Sembroski Purdue University By: Kara Ponder
REU Final Presentation: VERITAS Update Summer 2011 Advisors: John Finley and Glenn Sembroski Purdue University By: Kara Ponder Very Energetic Radiation Imaging Telescope Array System Ground-based gamma-ray
More informationHubVis: Software for Gravitational Lens Estimation and Visualization from Hubble Data
HubVis: Software for Gravitational Lens Estimation and Visualization from Hubble Data Sam L. Shue, Andrew R. Willis, and Thomas P. Weldon Dept. of Electrical and Computer Engineering University of North
More informationSpatial inference for astronomical data sets with INLA
Spatial inference for astronomical data sets with INLA EWASS - 5 April 2018 - Liverpool, UK S6 - Software in Astronomy Emille E. O. Ishida Laboratoire de Physique de Clermont - Université Clermont-Auvergne
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 informationQuasars and Active Galactic Nuclei (AGN)
Quasars and Active Galactic Nuclei (AGN) Astronomy Summer School in Mongolia National University of Mongolia, Ulaanbaatar July 21-26, 2008 Kaz Sekiguchi Hubble Classification M94-Sa M81-Sb M101-Sc M87-E0
More informationDetection of Artificial Satellites in Images Acquired in Track Rate Mode.
Detection of Artificial Satellites in Images Acquired in Track Rate Mode. Martin P. Lévesque Defence R&D Canada- Valcartier, 2459 Boul. Pie-XI North, Québec, QC, G3J 1X5 Canada, martin.levesque@drdc-rddc.gc.ca
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 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 informationMULTIPLE EXPOSURES IN LARGE SURVEYS
MULTIPLE EXPOSURES IN LARGE SURVEYS / Johns Hopkins University Big Data? Noisy Skewed Artifacts Big Data? Noisy Skewed Artifacts Serious Issues Significant fraction of catalogs is junk GALEX 50% PS1 3PI
More informationIdentifying High Redshift Dropouts. Abstract
Identifying High Redshift Dropouts Jeffrey Gerber Physics REU, University of California at Davis, Davis, CA, 95616 Dr. Benjamin Cain and Dr. Marusa Bradac Cosmology Department, University of California
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 informationARTEFACT DETECTION IN ASTROPHYSICAL IMAGE DATA USING INDEPENDENT COMPONENT ANALYSIS. Maria Funaro, Erkki Oja, and Harri Valpola
ARTEFACT DETECTION IN ASTROPHYSICAL IMAGE DATA USING INDEPENDENT COMPONENT ANALYSIS Maria Funaro, Erkki Oja, and Harri Valpola Neural Networks Research Centre, Helsinki University of Technology P.O.Box
More informationGalaxy Luminosity Function. Galaxy Luminosity Function. Schechter Function. Schechter Function by environment. Schechter (1976) found that
Galaxy Luminosity Function Count the number of galaxies as a function of luminosity (or absolute magnitude) Useful for: Understanding galaxy formation (distribution by luminosity implies distribution by
More informationThe Combined effects of ram pressure stripping, and tidal influences on Virgo cluster dwarf galaxies, using N body/ SPH simulation
The Combined effects of ram pressure stripping, and tidal influences on Virgo cluster dwarf galaxies, using N body/ SPH simulation Author: Rory Smith, Cardiff University Collaborators: Jonathon Davies,
More informationIMPROVING THE DECONVOLUTION METHOD FOR ASTEROID IMAGES: OBSERVING 511 DAVIDA, 52 EUROPA, AND 12 VICTORIA
IMPROVING THE DECONVOLUTION METHOD FOR ASTEROID IMAGES: OBSERVING 511 DAVIDA, 52 EUROPA, AND 12 VICTORIA Z Robert Knight Department of Physics and Astronomy University of Hawai`i at Hilo ABSTRACT Deconvolution
More informationLocal Group cosmology with ngcfht
Local Group cosmology with ngcfht Nicolas Martin (Strasbourg Observatory & MPIA, Heidelberg) Cosmology on galaxy scales the new frontier observed halo kpc Large scale cosmology is now largely understood
More informationTwo Transiting Exoplanet Candidates in Cygnus from the MASTER Project
Peremennye Zvezdy (Variable Stars) 33, No. 2, 2013 Received 13 February; accepted 22 February. Two Transiting Exoplanet Candidates in Cygnus from the MASTER Project A. Y. Burdanov 1, A. A. Popov 1, V.
More information1.4 Galaxy Light Distributions
26 1.4 Galaxy Light Distributions List of topics Hubble classification scheme see Binney & Merrifield text Galaxy surface brightness profiles (JL 2.3.1, plus additional material) Galaxy luminosity function
More informationImaging with Micado at the E-ELT. WORKSHOP: Imaging at the E-ELT
Imaging with Micado at the E-ELT Renato Falomo INAF Observatory of Padova, Italy WORKSHOP: Imaging at the E-ELT 29 May 2009, Garching Resolved stellar population in Virgo (high SB) Detailed View of high
More informationMulti-instrument, multiwavelength. energy sources with the Virtual Observatory
Multi-instrument, multiwavelength study of high energy sources with the Virtual Observatory Caroline Bot 1,2, François Bonnarel 1,2, René Goosmann 2 and Françoise Genova 1,2 1: Centre de Données astronomiques
More informationRandom Field Models for Applications in Computer Vision
Random Field Models for Applications in Computer Vision Nazre Batool Post-doctorate Fellow, Team AYIN, INRIA Sophia Antipolis Outline Graphical Models Generative vs. Discriminative Classifiers Markov Random
More informationPhotometry with Iris Photometry with Iris
Author: Daniel Duggan & Sarah Roberts - Faulkes Telescope Project Introduction Photometry is the measurement of the intensity or brightness of an astronomical object, such as a star or galaxy by adding
More informationTransiting Hot Jupiters near the Galactic Center
National Aeronautics and Space Administration Transiting Hot Jupiters near the Galactic Center Kailash C. Sahu Taken from: Hubble 2006 Science Year in Review The full contents of this book include more
More informationLESSON 1. Solar System
Astronomy Notes LESSON 1 Solar System 11.1 Structure of the Solar System axis of rotation period of rotation period of revolution ellipse astronomical unit What is the solar system? 11.1 Structure of the
More informationDust properties of galaxies at redshift z 5-6
Dust properties of galaxies at redshift z 5-6 Ivana Barisic 1, Supervisor: Dr. Peter L. Capak 2, and Co-supervisor: Dr. Andreas Faisst 2 1 Physics Department, University of Zagreb, Zagreb, Croatia 2 Infrared
More informationDeep fields around bright stars ( Galaxies around Stars )
Deep fields around bright stars ( Galaxies around Stars ) Scientific context: the morphological evolution of faint field galaxies Near-IR observations ground-based observations with AO: PUEO/CFHT deep
More informationData Processing in DES
Data Processing in DES Brian Yanny Oct 28, 2016 http://data.darkenergysurvey.org/fnalmisc/talk/detrend.p Basic Signal-to-Noise calculation in astronomy: Assuming a perfect atmosphere (fixed PSF of p arcsec
More informationWhat is the solar system?
Notes Astronomy What is the solar system? 11.1 Structure of the Solar System Our solar system includes planets and dwarf planets, their moons, a star called the Sun, asteroids and comets. Planets, dwarf
More informationADAS Guide to choosing the right Telescope. Produced by Members of the Society, Nov 2017
ADAS Guide to choosing the right Telescope Produced by Members of the Society, Nov 2017 Choosing a Telescope Telescope Types Telescope Features Visual or Astrophotography use? Telescope Package or Separate
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 information1 Introduction. 2 Observations. HD , an Eccentric Ellipsoidal System
Peremennye Zvezdy (Variable Stars) 33, No. 7, 2013 Received 24 August; accepted 30 August. HD 305629, an Eccentric Ellipsoidal System S. A. Otero 1,2, G. Di Scala 3,4 1 Buenos Aires, Argentina 2 American
More informationHW#4 is due next Monday Part of it is to read a paper and answer questions about what you read If you have questions, ask me!
Sep 21, 2015 Elliptical galaxies overview Shapes: evidence for triaxiality, isophotal twists, structure What causes flattening in ellipticals? Classes of ellipticals: Disky vs boxy Flat core vs cuspy/power-law
More informationarxiv:astro-ph/ v1 26 Jul 2005
A High Resolution HI Study of Selected Virgo Galaxies - Preliminary Results on Gas Morphology & Extra-Planar Gas arxiv:astro-ph/0507592v1 26 Jul 2005 Aeree Chung and J. H. van Gorkom Department of Astronomy,
More informationBasics of Photometry
Basics of Photometry Photometry: Basic Questions How do you identify objects in your image? How do you measure the flux from an object? What are the potential challenges? Does it matter what type of object
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 informationEvidence for/constraints on dark matter in galaxies and clusters
Nov 11, 2015 Evidence for/constraints on dark matter in galaxies and clusters HW#9 is due; please hand in your summaries; then you get to talk (I have slides of the different facilities/telescopes. HW#10
More informationSun Building Activity 2 The Signature of the Stars
Sun Building The Signature of the Stars Rainbows reveal that white light is a combination of all the colours. In 1666, Isaac Newton showed that white light could be separated into its component colours
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 informationDRM Update Joe Liske
DRM Update Joe Liske ETC Update Bug fix in spectroscopic mode: ETC used to calculate S/N per spectral pixel, not per resolution element. Correction and clarification of ETC document. In progress: update
More informationGalaxies in Pennsylvania. Bernstein, Jarvis, Nakajima, & Rusin: Implementation of the BJ02 methods
Galaxies in Pennsylvania Bernstein, Jarvis, Nakajima, & Rusin: Implementation of the BJ02 methods Bases of our methods: Shapes with geometric meaning: No empirical polarizabilities; simple optimizations
More informationCOLOR SEPARATION OF GALAXY TYPES IN THE SLOAN DIGITAL SKY SURVEY IMAGING DATA
COLOR SEPARATION OF GALAXY TYPES IN THE SLOAN DIGITAL SKY SURVEY IMAGING DATA Strateva et al. 2001, AJ, 122, 1861 Presenter: Ken Mawatari Date: 2011 October 31 2011/10/31 1 Outline Abstruct : roughly Introduction
More informationCONFIRMATION OF A SUPERNOVA IN THE GALAXY NGC6946
CONFIRMATION OF A SUPERNOVA IN THE GALAXY NGC6946 G. Iafrate and M. Ramella INAF - Astronomical Observatory of Trieste 1 Introduction Suddenly a star runs out its nuclear fuel. Its life as a normal star
More informationObtain one of the laminated sheets, and classify the numbered objects by color (hopefully obvious) and by shape:
Astronomy 100 Name(s): Exercise 8: Galaxies and the Hubble Law The large-scale structure of the universe is governed by gravity. The Sun orbits the center of our galaxy, the Milky Way. The Milky Way, in
More informationOverlapping Astronomical Sources: Utilizing Spectral Information
Overlapping Astronomical Sources: Utilizing Spectral Information David Jones Advisor: Xiao-Li Meng Collaborators: Vinay Kashyap (CfA) and David van Dyk (Imperial College) CHASC Astrostatistics Group April
More informationLecture Three: Observed Properties of Galaxies, contd.! Hubble Sequence. Environment! Globular Clusters in Milky Way. kpc
Hubble Sequence Lecture Three: Fundamental difference between Elliptical galaxies and galaxies with disks, and variations of disk type & importance of bulges Observed Properties of Galaxies, contd.! Monday
More informationTHE PLEIADES OPEN CLUSTER
THE PLEIADES OPEN CLUSTER G. Iafrate (a), M. Ramella (a) and P. Padovani (b) (a) INAF - Astronomical Observatory of Trieste (b) ESO - European Southern Observatory 1 Introduction Open star clusters are
More informationFinding Black Holes Left Behind by Single Stars
Finding Black Holes Left Behind by Single Stars Finding Black Holes "Yesterday upon the stair I met a man who wasn't there. He wasn't there again today. I wish that man would go away." Hughes Mearns (1875-1965)
More informationarxiv: v4 [astro-ph] 18 Jun 2008
Chinese Journal of Astronomy and Astrophysics manuscript no. (L A TEX: chjaa.tex; printed on April 18, 2017; 6:18) Chin. J. Astron. Astrophys. Vol. 8 (2008), No. 3, 362 Received 2007 May 31; accepted 2008
More informationClusters and groups of galaxies: internal structure and dynamics
Clusters and groups of galaxies: internal structure and dynamics Strong constraints on cosmological theories and on the nature of dark matter can be obtained from the study of cluster masses, mass distribution,
More informationPoS(extremesky2009)013
Correlating the WFC and the IBIS hard X-ray surveys IASF-Roma INAF. Via Fosso del Cavaliere, 100 00133 Rome Italy E-mail: fiamma.capitanio@iasf-roma.inaf.it A. J. Bird School of Physics and Astronomy,
More informationProtoplanetary discs of isolated VLMOs discovered in the IPHAS survey
Protoplanetary discs of isolated VLMOs discovered in the IPHAS survey Luisa Valdivielso Casas Collaborators: E. Martín, H. Bouy, E. Solano,J. Drew,R. Greimel 1 IAC - ULL 14 de septiembre 2010 Outline Introduction
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 informationSurface Brightness of Spiral Galaxies
Surface Brightness of Spiral Galaxies M104: SA N4535: SAB LMC: dwarf irregular,barred Normal 1/4-law+exp fits An example of surface brightness profile. The top curve is the sum of exp disk+1/4-bulge. The
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 information2 F. PASIAN ET AL. ology, both for ordinary spectra (Gulati et al., 1994; Vieira & Ponz, 1995) and for high-resolution objective prism data (von Hippe
AUTOMATED OBJECTIVE PRISM SPECTRAL CLASSIFICATION USING NEURAL NETWORKS F. PASIAN AND R. SMAREGLIA Osservatorio Astronomico di Trieste Via G.B.Tiepolo 11, 34131 Trieste, Italy AND P. HANZIOS, A. DAPERGOLAS
More informationBrief update (3 mins/2 slides) on astrophysics behind final project
Nov 1, 2017 Brief update (3 mins/2 slides) on astrophysics behind final project Evidence for Dark Matter Next Wed: Prelim #2, similar to last one (30 mins). Review especially lecture slides, PEs and non-project
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 informationLarge Area Imaging Survey of Near-Infrared Sky with Korean Compact Space Telescopes
Large Area Imaging Survey of Near-Infrared Sky with Korean Compact Space Telescopes Science & Technology Satellite Series (KARI) (2000 ~ 2013. 02) 1 st Satellite: FIMS (Far-ultraviolet IMaging Spectrograph)
More informationWFC3 IR Blobs, IR Sky Flats and the measured IR background levels
The 2010 STScI Calibration Workshop Space Telescope Science Institute, 2010 Susana Deustua and Cristina Oliveira, eds. WFC3 IR Blobs, IR Sky Flats and the measured IR background levels N. Pirzkal 1 Space
More informationTHE HUBBLE SEQUENCE. Information and contacts: -
THE HUBBLE SEQUENCE G. Iafrate (a), M. Ramella (a) e V. Bologna (b) (a) INAF - Astronomical Observatory of Trieste (b) Istituto Comprensivo S. Giovanni - Sc. Sec. di primo grado M. Codermatz" - Trieste
More informationThe Milky Way, Hubble Law, the expansion of the Universe and Dark Matter Chapter 14 and 15 The Milky Way Galaxy and the two Magellanic Clouds.
The Milky Way, Hubble Law, the expansion of the Universe and Dark Matter Chapter 14 and 15 The Milky Way Galaxy and the two Magellanic Clouds. Image taken from the European Southern Observatory in Chile
More informationRed giants in the halo of the SO galaxy NGC 3115: a distance and a bimodal metallicity distribution
Mon. Not. R. Astron. Soc. 286, 771-776 (1997) Red giants in the halo of the SO galaxy NGC 3115: a distance and a bimodal metallicity distribution Rebecca A. W. Elson* Institute of Astronomy, Madingley
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 Star Images: On the Determination of Moffat s PSF Shape Parameters
J. Astrophys. Astr. (1988) 9, 17 24 CCD Star Images: On the Determination of Moffat s PSF Shape Parameters O. Bendinelli Dipartimento di Astronomia, Via Zamboni 33, I-40126 Bologna, Italy G. Parmeggiani
More informationPart I. C. M. Bishop PATTERN RECOGNITION AND MACHINE LEARNING CHAPTER 8: GRAPHICAL MODELS
Part I C. M. Bishop PATTERN RECOGNITION AND MACHINE LEARNING CHAPTER 8: GRAPHICAL MODELS Probabilistic Graphical Models Graphical representation of a probabilistic model Each variable corresponds to a
More informationA photometric catalogue of galaxies in the cluster Abell 85,
ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES Astron. Astrophys. Suppl. Ser. 128, 67-73 (1998) FEBRUARY II 1998, PAGE67 A photometric catalogue of galaxies in the cluster Abell 85, E. Slezak 1, F. Durret
More informationDo we know all the Milky Way Globular Clusters? Dirk Froebrich
Do we know all the Milky Way Globular Clusters? Dirk Froebrich People 1) Candidates from the FSR Cluster Sample A. Scholz H. Meusinger C.J. Davis C.L. Raftery 2) Candidates from the GPS and Mercer list
More informationPhotometry of Supernovae with Makali i
Photometry of Supernovae with Makali i How to perform photometry specifically on supernovae targets using the free image processing software, Makali i This worksheet describes how to use photometry to
More informationastro-ph/ Feb 95
Search for Intra-Cluster Machos by Pixel Lensing of M87 Andrew Gould 1 Dept of Astronomy, Ohio State University, Columbus, OH 43210 e-mail gould@payne.mps.ohio-state.edu astro-ph/9501104 1 Feb 95 Abstract
More informationDetection ASTR ASTR509 Jasper Wall Fall term. William Sealey Gosset
ASTR509-14 Detection William Sealey Gosset 1876-1937 Best known for his Student s t-test, devised for handling small samples for quality control in brewing. To many in the statistical world "Student" was
More informationThe effect of large scale environment on galaxy properties
The effect of large scale environment on galaxy properties Toulouse, June 2017 Iris Santiago-Bautista The LSS baryonic component is composed by substructures of gas and galaxies embedded in dark matter
More informationClassification of Galaxies
Name: Partner(s): 1102 or 3311: Desk # Date: Classification of Galaxies Purpose Study and classify galaxies Learn how to measure their distance, mass and radius. Equipment Pictures from online lab manual
More informationOutline: Galaxy groups & clusters
Outline: Galaxy groups & clusters Outline: Gravitational lensing Galaxy groups and clusters I Galaxy groups and clusters II Cluster classification Increasing rareness Intermission: What are you looking
More informationImage Segmentation: Definition Importance. Digital Image Processing, 2nd ed. Chapter 10 Image Segmentation.
: Definition Importance Detection of Discontinuities: 9 R = wi z i= 1 i Point Detection: 1. A Mask 2. Thresholding R T Line Detection: A Suitable Mask in desired direction Thresholding Line i : R R, j
More informationDiscovery of Primeval Large-Scale Structures with Forming Clusters at Redshift z=5.7
Discovery of Primeval Large-Scale Structures with Forming Clusters at Redshift z=5.7 Sadanori Okamura Department of Astronomy, and Research Center for the Early Universe, University of Tokyo Collaborators
More informationScaling Relations of late-type galaxies
Scaling Relations of late-type galaxies - an observational perspective - Lecture I Lecture II Trends along the Hubble sequence Galaxy rotation curves Lecture III Tully-Fisher relations Marc Verheijen Kapteyn
More informationClusters of Galaxies " High Energy Objects - most of the baryons are in a hot (kt~ k) gas." The x-ray luminosity is ergs/sec"
Clusters of Galaxies! Ch 4 Longair Clusters of galaxies are the largest gravitationally bound systems in the Universe. At optical wavelengths they appear as over-densities of galaxies with respect to the
More informationWORKSHOP ULXs AND THEIR ENVIRONMENT June 13th 16th, 2016 Strasbourg, France
WORKSHOP ULXs AND THEIR ENVIRONMENT June 13th 16th, 216 Strasbourg, France I GEDE PUTU MAHADIPA PRIAJANA COLLABORATORS: HESTI RETNO TRI WULANDARI KIKI VIERDAYANTI PREMANA W PREMADI SULISTYOWATI Affiliation:
More informationPHY323:Lecture 7 Dark Matter with Gravitational Lensing
PHY323:Lecture 7 Dark Matter with Gravitational Lensing Strong Gravitational Lensing Theory of Gravitational Lensing Weak Gravitational Lensing Large Scale Structure Experimental Evidence for Dark Matter
More informationHubble s Law and the Cosmic Distance Scale
Lab 7 Hubble s Law and the Cosmic Distance Scale 7.1 Overview Exercise seven is our first extragalactic exercise, highlighting the immense scale of the Universe. It addresses the challenge of determining
More information