Lab 4: Stellar Spectroscopy

Size: px
Start display at page:

Download "Lab 4: Stellar Spectroscopy"

Transcription

1 Name:... Astronomy 101: Observational Astronomy Fall 2006 Lab 4: Stellar Spectroscopy 1 Observations 1.1 Objectives and Observation Schedule During this lab each group will target a few bright stars of different spectral types and record their spectra. All our observations will be done using an SBIG Self-Guiding spectrograph mounted onto the Whitney 14 Celestron telescope at Brackett Observatory. You will observe in groups of 2-3, and each group will take spectra of at least three stars in the target list. At the end of the lab, different groups will most likely have to share their data, so keep good logs. The current labs times are Tuesday 6:00pm and Thursday 7:00pm & 9:00pm. These may change depending on the weather, so stay in contact with the lab instructor. 1.2 Picking Targets For this lab, your lab instructor has pre-selected a target list of stars that span the range of spectral types. For this lab, brighter is better, so as you can see in Table 1, your targets were chosen to have V 2-3 mag. Star Name RA (1996.5) Dec (1996.5) Magnitude Alderamin (α Cep) Markab (α Peg) Ruchbah (δ Cas) v Alphirk (β Cep) v Alpheratz (α And) v Algenib (γ Peg) v NoName (γ Cas) v Scheat (β Peg) v Mirach (β And) Alrai (γ Cep) Schedar (η Cas) Matar (η Peg) Caph (β Cas) v Table 1: Potential spectroscopy targets. Different spectral types are separated by double lines. 1.3 Background Telescope, Spectrograph and Camera We will be using SBIG self-guiding spectrograph, mounted onto the 14 Celestron. By now you are already familiar with this telescope and the Sky software that we use to operate it. The spectrograph is connected 1

2 to the ST-7E CCD camera. The descriptions of the spectrograph, and the CCD camera are on the web (see Overview of Telescopes and Instruments on the course webpage). I have also posted operating instructions for the spectrograph on the same web page where you downloaded this lab manual. In preparation for the lab, please read section 5.0 of the instructions. The wavelength range of the spectrograph extends roughly from 3800 Å to 7500 Å. The spectrograph has two gratings. Their main parameters are summarized in the table below. To change gratings one needs simply to turn the black toggle switch on the spectrograph. Flip the lever up (away from the handles on the spectrograph box) to use low resolution mode and down to use high resolution mode. High Resolution Low Resolution Grating Grating Dispersion 1.07 Å/pixel 4.3 Å/pixel Resolution (FWHM) 2.2 Å 8 Å Spectral Coverage per Frame 750 Å 3200 Å Table 2: Parameters of the spectrograph. The central wavelength of the spectrum can be set using the micrometer adjustment. The numbers on the micrometer correspond quite well to center wavelength of the spectrum in high resolution mode. For example, when the micrometer reads 5.45, the spectrum is centered around 5450 Å. The micrometer scale is of course incorrect for the low resolution grating. To center the desired wavelength you will have to read the required micrometer setting from the figure below. Figure 1: Micrometer setting for the low resolution grating is plotted as a function of the desired center frequency. The locations of the three Balmer lines of H are also shown on the figure. 1.4 Procedure Between you and your partner, choose four stars with different spectral types for your observation Positioning the Star in the Slit and Taking Spectra As you know, pointing has not been the strong point of Brackett telescopes. It might be even more difficult to find your targets this time around, since the tracking CCD on the spectrograph is quite small ( mm vs mm for AP47p). To point the telescope, send it to your target and use the flip mirror to view your star through the eye-piece. Use the paddle to center your target and then flip back the mirror. You are now ready to check whether or not the star appears on the tracking CCD on the spectrograph. Once your star is visible on the guide camera all you need to do is position the star in the slit using the telescope controls and then take your science exposure. To control the spectrograph we will be using Maxim DL again. Your instructor will show you how to choose the tracking CCD and take images. The instructions outlined in section 5.0 of the spectrograph manual are written for the program called CCDOPS, but they are easily adaptable for Maxim DL. If your stars are bright and positioned exactly on the slit, exposure times of about 10 sec should be sufficient. With such a short exposure you will not need to use the auto-guider (software package that takes short images of the target using the tracking CCD and adjusts the tracking of the telescope to keep the target 2

3 centered on the same spot on the chip). It might become necessary, however, for longer exposures. If you decide you need to use it, you instructor will show you how to activate it. We will not be taking flat frames (they would simply give us the spectrum of the sky), Make sure to use automatic dark subtraction for the final images. It might also be useful to take images of the sky. We will not be able to use them as flats, since they will give us the spectrum of the sky, but you can treat them as a background, which can them be subtracted from your stellar images to get rid of the sky lines Calibrating Spectra The micrometer is sufficiently well calibrated for rough positioning of the spectra. However, to identify spectral lines, and especially to measure Doppler shifts of lines due to stellar radial motion we need to use calibration lamps. We have hydrogen and neon lamps available. To collect calibration data, place the lamp a few inches away from opal circular window on the bottom of the spectrograph and either leave the window open and the lamp on while taking stellar spectra, or take a separate exposure after you are done with the stellar spectrum. Experiment using both methods to see which will work best. With the hydrogen lamp, you should see H α, H β, and H γ lines at 6563 Å, 4861 Å, and 4340 Å, respectively. You might also see H δ at 4103 Å. With the neon lamp, you should see series of intermediate strength lines around 6000 Å Nebula Spectra It is a lot of fun to take emission line spectra of nebula. If you have time at the end of your observing run, try to locate the Ring nebula (early teams) or the Orion nebula (late teams). It might be rather tricky to place these on the slit, because the pointing is not very reliable, but the eye-piece will help. You might need to use the auto-guider to take these spectra. 1.5 Summary Ideally, at the end of your observation you should have the following data: spectra of a couple of stars from your target list; spectrum of one or both of the calibration lamps for each of your target spectra. 2 Data Analysis 2.1 Data Access Your data will be transferred from Brackett to: Fall2006/Lab4 data/ 2.2 Extracting Slit Spectra with IRAF The procedure for analyzing spectra is explained very clearly in the IRAF manual you will find in the astro lab. The instructions are quite straight-forward, and we will go over the entire procedure in class on Monday. Below I summarize the differences between what you will be doing and the procedure described in the manual. 1. The parameter dispaxi, which determines whether the dispersion axis is along lines or columns, belongs to the entire package (e.g. kpnoslit, ctioslit, or kpnocoude), not to the apall task. So to set it, type eparam kpnoslit, and set dispaxi to 1. 3

4 2. Background subtraction should not be important for any of our targets, so you can simply ignore it, set the parameter background to none. If you decide to subtract the background anyways, make sure to choose background region close to the spectrum, because the sky emission lines are not perpendicular to the dispersion axis. 3. Set weights parameter to none and clean parameter to no, since we do not know well the noise characteristics of our CCD. 4. For simplicity, set format to onedspec and extras to no. 5. Use the command splot to examine your final spectrum Calibration and Line Centroids To convert from pixel number to wavelength we need to calculate the dispersion solution for our spectrograph using the calibration lamp spectra. The calibration can be done in two ways. Method 1: You can use either the mercury or hydrogen spectrum to do the calibration by hand. First compute the comparison spectrum following instructions on pp on the IRAF manual. The key point to keep in mind is that if there is a slant to your slit you need to extract the calibration spectrum from the same exact rows of the CCD chip as you stellar spectrum. (Note: If your calibration was taken on the same exposure as your data, you can measure your calibration lines at the same time you measure your stellar emission lines below.) Once it is done, use the command splot to examine the calibration spectrum and to compute the peak positions of the prominent lines. To do that, place the cursor to the left of the line and type e, then place it to the right of the line and type e again. On the bottom of the display window you will see the computed information. You will need to record this to obtain the dispersion solution for your spectrum. Now go back to your stellar spectrum and using the same method compute the centroids for the most prominent absorption lines. Finally, use the listpix command to write the flux data into text files. Now you can use your favorite number crunching program to convert from pixel # s to Å for all the spectral lines you identified in the stellar spectrum. Do not forget that in our images red is to the left, and blue is to the right. Make sure to comment on the uncertainties in your line centroids. You can get some idea for this by considering the resolution of the spectrograph, and by comparing calibration spectra taken at different times during the night to each other. Since we did not take spectrophotometric standard stars, you will not be flux calibrating your spectra to get rid of the CCD response. Method 2: You use the task identify provided in IRAF, on the hydrogen and/or neon spectra. Follow the instructions in the manual. Once this is done, your spectra will have the form flux vs. wavelength, and splot will allow you to determine line wavelength, rather than pixel location. Linelists for most standard calibration lines are included in the IRAF linelists directory; however, hydrogen lines are not. Since you re probably only identifying 3 lines in the hydrogen spectrum, you can create this text file by hand using the table below. 2.3 Identifying Stellar Spectral Types First, you need to identify spectral lines. The table below shows some prominent lines; a more complete table of common spectral lines can be found in the Handbook of Space Astronomy and Astrophysics. You might also find useful Jacoby et al. (1984) paper and an online catalog run by IPAC at Caltech. The links to all of these are provided on our website together with this lab manual. 4

5 λ (Å) Element Comments 6563 H H α 4861 H H β 4341 H H γ 4102 H H δ 3970 H H ɛ 3889 H H ζ 3835 H H η 3968 Ca II prominent in cooler stars 3934 Ca II prominent in cooler stars 5890 Na I doublet line, strong in M type 5896 Na I doublet line, strong in M type Now you come to the really hard part trying to guess at the spectral type of your stars. Justify your answer based on which spectral lines you are able to identify. Start by comparing the two spectra. Can you tell which one is redder? Keep in mind that the continuum shape is largely determined by the shape of the CCD quantum efficiency curve, so take this into account. Your goal is to determine the spectral type of your objects to the nearest letter and justify your answer. Then look up the correct spectral type and check your answers. 2.4 What to Include in Your Report Here is the minimum of what needs to be included in your report. 1. Observations: Include a summary of observing logs, and instrument specifications. 2. Data Reduction: Include examples of your calibration spectra (flux vs. pixel #) as well as computed centroids for spectral lines. Try to use tables as much as possible, it makes the whole thing much neater. 3. Data Analysis and Interpretation: Include your dispersion solution(s), list lines that you were able to identify, show the final spectra (flux vs. Å) and label lines on them. Explain your logic on determining the final spectral types for your stars. 5

Department of Physics and Astronomy University of Iowa 29:137 Astronomical Laboratory Fall 2011 Lab 4: Stellar Spectroscopy

Department of Physics and Astronomy University of Iowa 29:137 Astronomical Laboratory Fall 2011 Lab 4: Stellar Spectroscopy Department of Physics and Astronomy University of Iowa 29:137 Astronomical Laboratory Fall 2011 Lab 4: Stellar Spectroscopy 1 Introduction Throughout your astronomy education, you have read about stellar

More information

Objectives: (a) To understand how to display a spectral image both as an image and graphically.

Objectives: (a) To understand how to display a spectral image both as an image and graphically. Texas Tech University Department of Physics & Astronomy Astronomy 2401 Observational Astronomy Lab 8:- CCD Image Analysis:- Spectroscopy Objectives: There are two principle objectives for this laboratory

More information

Measuring the Redshift of M104 The Sombrero Galaxy

Measuring the Redshift of M104 The Sombrero Galaxy Measuring the Redshift of M104 The Sombrero Galaxy Robert R. MacGregor 1 Rice University Written for Astronomy Laboratory 230 Department of Physics and Astronomy, Rice University May 3, 2004 2 Abstract

More information

Lab 6: Spectroscopy Due Monday, April 10

Lab 6: Spectroscopy Due Monday, April 10 Lab 6: Spectroscopy Due Monday, April 10 The aim of this lab is to provide you with hands-on experience obtaining and analyzing spectroscopic data. In this lab you will be using a spectrograph to obtain

More information

College of San Mateo Observatory

College of San Mateo Observatory College of San Mateo Observatory Stellar Spectra Catalog SGS Spectrograph Spectra taken from CSM observatory using SBIG Self Guiding Spectrograph (SGS) A work in progress compiled by faculty, staff, and

More information

Open Cluster Photometry: Part II

Open 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 information

Model SGS Dual CCD Self-Guiding Spectrograph

Model SGS Dual CCD Self-Guiding Spectrograph .. Model SGS Dual CCD Self-Guiding Spectrograph The Self-Guiding Spectrograph is designed to be used with the ST-7XE/XME camera. For convenience, it can also be used with any dual sensor ST/7/8/9/10/2000

More information

Introduction: Objectives: (a) To understand how to compile a list of objects for imaging with a CCD.

Introduction: Objectives: (a) To understand how to compile a list of objects for imaging with a CCD. Texas Tech University Department of Physics Astronomy 2401 Observational Astronomy Lab 2:- Planning Observations Introduction: Observing time at the telescope is generally very limited. Therefore, in order

More information

Reduction procedure of long-slit optical spectra. Astrophysical observatory of Asiago

Reduction 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 information

Mimir NIR Spectroscopy Data Processing Cookbook V2.0 DPC

Mimir NIR Spectroscopy Data Processing Cookbook V2.0 DPC Mimir NIR Spectroscopy Data Processing Cookbook V2.0 DPC - 20111130 1. Fetch and install the software packages needed a. Get the MSP_WCT, MSP_CCS, MSP_SXC packages from the Mimir/Software web site: http://people.bu.edu/clemens/mimir/software.html

More information

AstroBITS: Open Cluster Project

AstroBITS: 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 information

Astronomical frequency comb for calibration of low and medium resolution spectrographs

Astronomical frequency comb for calibration of low and medium resolution spectrographs Astronomical frequency comb for calibration of low and medium resolution spectrographs innofspec at AIP has several years expertise in astronomical instrumentation. innofspec succesfully developed a new

More information

Open Cluster Research Project

Open Cluster Research Project Open Cluster Research Project I. Introduction The observational data indicate that all stars form in clusters. In a cloud of hydrogen gas, laced with helium and a trace of other elements, something triggers

More information

Observing Night 1 DON T FORGET TO KEEP NOTES ON YOUR PROCEDURE AND KEEP AN OBSERVING LOG FOR THE NIGHT!!!!!

Observing Night 1 DON T FORGET TO KEEP NOTES ON YOUR PROCEDURE AND KEEP AN OBSERVING LOG FOR THE NIGHT!!!!! Observing Night 1 Objects : Name RA (2000) Dec V B-V V-R R-I MK source HD 5015 00 53 04 +61 07 26 5.34 0.54 0.48 0.30 F9V Ducati 2002 HD 30197 4 46 17 +18 44.1 6.01 1.21 0.620 0.533 K4III J66/T86 HD 7615

More information

Hubble's Law and the Age of the Universe

Hubble's Law and the Age of the Universe Hubble's Law and the Age of the Universe Procedure: Name: 1. Login into the network using your user ID and your password. 2. Double click on the Astronomy shortcuts folder on the desktop. 3. Double click

More information

Note on OSIRIS Wavelength Calibrations D. Le Mignant, Oct. 5, 2007

Note on OSIRIS Wavelength Calibrations D. Le Mignant, Oct. 5, 2007 Note on OSIRIS Wavelength Calibrations D. Le Mignant, Oct. 5, 2007 1. Observations and data reduction In this short note, we report on some on-going analysis of OSIRIS data in an effort to document our

More information

Exploring 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 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 information

APAS Laboratory { PAGE } Spectroscopy SPECTROSCOPY

APAS Laboratory { PAGE } Spectroscopy SPECTROSCOPY SPECTROSCOPY SYNOPSIS: In this lab you will eplore different types of emission spectra, calibrate a spectrometer using the spectrum of a known element, and use your calibration to identify an unknown element.

More information

Astro 500 A500/L-15 1

Astro 500 A500/L-15 1 Astro 500 A500/L-15 1 Lecture Outline Spectroscopy from a 3D Perspective ü Basics of spectroscopy and spectrographs ü Fundamental challenges of sampling the data cube Approaches and example of available

More information

NAOYUKI TAMURA Subaru Instrument Astronomer Subaru Telescope, NAOJ

NAOYUKI TAMURA Subaru Instrument Astronomer Subaru Telescope, NAOJ FMOS status tt report Science workshop 2011.02.2802 28-03.0202 NAOYUKI TAMURA Subaru Instrument Astronomer Subaru Telescope, NAOJ * Overview * Recent history & current status t * Schedule & future plan

More information

Lecture 8. October 25, 2017 Lab 5

Lecture 8. October 25, 2017 Lab 5 Lecture 8 October 25, 2017 Lab 5 News Lab 2 & 3 Handed back next week (I hope). Lab 4 Due today Lab 5 (Transiting Exoplanets) Handed out and observing will start Friday. Due November 8 (or later) Stellar

More information

Southern African Large Telescope. Prime Focus Imaging Spectrograph. Instrument Acceptance Testing Plan

Southern African Large Telescope. Prime Focus Imaging Spectrograph. Instrument Acceptance Testing Plan Southern African Large Telescope Prime Focus Imaging Spectrograph Instrument Acceptance Testing Plan Eric B. Burgh University of Wisconsin Document Number: SALT-3160AP0003 Revision 1.0 18 February 2003

More information

Investigating the Efficiency of the Beijing Faint Object Spectrograph and Camera (BFOSC) of the Xinglong 2.16-m Reflector

Investigating the Efficiency of the Beijing Faint Object Spectrograph and Camera (BFOSC) of the Xinglong 2.16-m Reflector Research in Astron. Astrophys. Vol. (xx) No., http://www.raa-journal.org http://www.iop.org/journals/raa Research in Astronomy and Astrophysics Investigating the Efficiency of the Beijing Faint Object

More information

ASTRONOMY 460: PROJECT INTRO - GALACTIC ROTATION CURVE

ASTRONOMY 460: PROJECT INTRO - GALACTIC ROTATION CURVE ASTRONOMY 460: PROJECT INTRO - GALACTIC ROTATION CURVE Snežana Stanimirović, October 6, 2014 1. Introduction This project has two goals: we want to measure the Milky Way (or Galactic) rotation curve by

More information

PROJECT GLOBULAR CLUSTERS

PROJECT GLOBULAR CLUSTERS PROJECT 5 GLOBULAR CLUSTERS Objective: The objective of this exercise is the calculation of the core and tidal radius of a globular cluster in the Milky Way. Measure the tidal radius of a globular cluster

More information

UNIVERSITY COLLEGE LONDON. Measuring a Stellar Spectrum

UNIVERSITY COLLEGE LONDON. Measuring a Stellar Spectrum University Of London Observatory 1 Introduction UNIVERSITY COLLEGE LONDON Measuring a Stellar Spectrum 1B30 Practical Astronomy 1B13 Frontiers of Astronomy The primary way astronomers find out about physical

More information

IN REPORT: Plate Scale and FOV of CCD for Each Telescope using Albireo Stars

IN 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 information

Measuring the Age of the Universe

Measuring the Age of the Universe Measuring the Age of the Universe Activity Guide Author: Sarah Eve Roberts HUBBLE DIAGRAM: STUDENT WORKSHEET 1 Introduction The discovery of the expanding Universe was one of the greatest revelations in

More information

Millimagnitude Accuracy Photometry of Extra solar Planets Transits using Small Telescopes

Millimagnitude Accuracy Photometry of Extra solar Planets Transits using Small Telescopes Millimagnitude Accuracy Photometry of Extra solar Planets Transits using Small Telescopes S. Kozłowski 1, 2, A. Szary 1, M. Zub 1, G. Melikidze 1, K. Maciesiak 1, J. A. Gil 1 1 Institute of Astronomy University

More information

The Hubble Redshift Distance Relation

The Hubble Redshift Distance Relation The Hubble Redshift Distance Relation Student Manual A Manual to Accompany Software for the Introductory Astronomy Lab Exercise Document SM 3: Version 1 Department of Physics Gettysburg College Gettysburg,

More information

The Challenge of AZ Cas-Part 1. John Menke Barnesville, MD Abstract

The Challenge of AZ Cas-Part 1. John Menke Barnesville, MD Abstract The Challenge of AZ Cas-Part 1 John Menke Barnesville, MD 20838 john@menkescientific.com www.menkescientific.com Abstract This is an interim report on observations of the spectrum of AZCas taken during

More information

Extraction of Point Source Spectra from STIS Long Slit Data

Extraction of Point Source Spectra from STIS Long Slit Data 1997 HST Calibration Workshop Space Telescope Science Institute, 1997 S. Casertano, et al., eds. Extraction of Point Source Spectra from STIS Long Slit Data J. R. Walsh Spect Telescope European Coordinating

More information

Operating the Celestron 14 Telescope

Operating the Celestron 14 Telescope Operating the Celestron 14 Telescope 1. The Telescope and Its Controls The Celestron 14-inch telescope is located in the east bay of the observatory (Fig. 1). It is a Schmidt-Cassegrain type instrument;

More information

PHYS/ASTR 2060 Popular Observational Astronomy(3) Syllabus

PHYS/ASTR 2060 Popular Observational Astronomy(3) Syllabus PHYS/ASTR 2060 Popular Observational Astronomy(3) Syllabus Instructor: Prof. Wayne Springer (wayne.springer@utah.edu) Office: 226 INSCC (Office Hours: T 3PM-5PM or by appt.) Phone: 801-585-1390 TA: Jinqi

More information

A Search for Dark Matter in an Edge on Spiral Galaxy

A Search for Dark Matter in an Edge on Spiral Galaxy UNIVERSITY OF CALIFORNIA - SANTA CRUZ DEPARTMENT OF PHYSICS PHYS 136 PROFESSOR: PROCHASKA A Search for Dark Matter in an Edge on Spiral Galaxy Benjamin Stahl Team: A. Callahan (PI) & J. Gillette August

More information

Optical/IR Observational Astronomy Spectroscopy. David Buckley, SALT

Optical/IR Observational Astronomy Spectroscopy. David Buckley, SALT David Buckley, SALT 1 Background is really just monochromatic photometry History 1637 Descartes explained the origin of the rainbow. 1666 Newton s classic experiments on the nature of colour. 1752 Melvil

More information

A Stellar Spectra 3. Stars shine at night (during the day too!). A star is a self-luminous sphere of gas. Stars are held together by gravity.

A Stellar Spectra 3. Stars shine at night (during the day too!). A star is a self-luminous sphere of gas. Stars are held together by gravity. Stellar Spectra Relativity and Astrophysics Lecture 12 Terry Herter Outline What is a star? Stellar Spectra Kirchhoff s Laws Spectral Classification Spectral Types: O B A F G K M L T Stellar Photometry

More information

TEACHING OBSERVATIONAL METHODS IN ASTROPHYSICS: REMOTE OBSERVATIONS FROM THE SCHOOL

TEACHING OBSERVATIONAL METHODS IN ASTROPHYSICS: REMOTE OBSERVATIONS FROM THE SCHOOL TEACHING OBSERVATIONAL METHODS IN ASTROPHYSICS: REMOTE OBSERVATIONS FROM THE SCHOOL Paolo Santin, INAF - Astronomical Observatory of Trieste, Trieste, Italy Abstract The traditional way of teaching Astrophysics

More information

Buy-back points tallied and added: 750 points bought-back. Last Withdrawal date: this friday, Oct 31st.

Buy-back points tallied and added: 750 points bought-back. Last Withdrawal date: this friday, Oct 31st. Announcements HW #3: Available online now. Due in 1 week, Nov 3rd, 11pm. Buy-back points tallied and added: 750 points bought-back. Last Withdrawal date: this friday, Oct 31st. Evening Observing: next

More information

Emission Spectrum of Atomic Gases. Prelab Questions

Emission Spectrum of Atomic Gases. Prelab Questions Emission Spectrum of Atomic Gases Prelab Questions Before this coming to this lab, please review your text for the physics of the spectrum of visible light and of diffraction grating spectrometer.. Which

More information

Building your own Pizza-Box Spectroscope. *You will need to bring in a medium- sized sturdy cardboard pizza box, shoe box, or similar from home.

Building your own Pizza-Box Spectroscope. *You will need to bring in a medium- sized sturdy cardboard pizza box, shoe box, or similar from home. Building your own Pizza-Box Spectroscope Experimental Notes *You will need to bring in a medium- sized sturdy cardboard pizza box, shoe box, or similar from home. Color, Light, and Atomic Spectroscopy

More information

Lab 4 Radial Velocity Determination of Membership in Open Clusters

Lab 4 Radial Velocity Determination of Membership in Open Clusters Lab 4 Radial Velocity Determination of Membership in Open Clusters Sean Lockwood 1, Dipesh Bhattarai 2, Neil Lender 3 December 2, 2007 Abstract We used the Doppler velocity of 29 stars in the open clusters

More information

Introduction to SDSS -instruments, survey strategy, etc

Introduction 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 information

PHYSICS Observing Guide

PHYSICS 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 information

125-Day Spectral Record of the Bright Nova Delphini 2013 (V339 Del)

125-Day Spectral Record of the Bright Nova Delphini 2013 (V339 Del) Mooers and Wiethoff, JAAVSO Volume 42, 2014 161 125-Day Spectral Record of the Bright Nova Delphini 2013 (V339 Del) Howard D. Mooers Department of Geological Sciences, University of Minnesota Duluth, Duluth,

More information

Astronomy 102: Stars and Galaxies Exam 2

Astronomy 102: Stars and Galaxies Exam 2 October 13, 2004 Name: Astronomy 102: Stars and Galaxies Exam 2 Instructions: Write your answers in the space provided; indicate clearly if you continue on the back of a page. No books, notes, or assistance

More information

Atomic Spectra. Eric Reichwein David Steinberg Department of Physics University of California, Santa Cruz. August 30, 2012

Atomic Spectra. Eric Reichwein David Steinberg Department of Physics University of California, Santa Cruz. August 30, 2012 Atomic Spectra Eric Reichwein David Steinberg Department of Physics University of California, Santa Cruz August 30, 0 Abstract To observe helium spectral lines we used a spectrometer. From a table of known

More information

WHAT DO RADIAL VELOCITY MEASUREMENTS TELL ABOUT RV TAURI STARS?

WHAT DO RADIAL VELOCITY MEASUREMENTS TELL ABOUT RV TAURI STARS? Dig Sites of Stellar Archeology: Giant Stars in the Milky Way Ege Uni. J. of Faculty of Sci., Special Issue, 2014, 113-120 WHAT DO RADIAL VELOCITY MEASUREMENTS TELL ABOUT RV TAURI STARS? Timur Şahin 1*,

More information

INTRODUCTION TO THE TELESCOPE

INTRODUCTION TO THE TELESCOPE AST 113/114 Fall 2014 / Spring 2016 NAME: INTRODUCTION TO THE TELESCOPE What will you learn in this Lab? For a few of the labs this semester, you will be using an 8-inch Celestron telescope to take observations.

More information

Any first year text, sections on atomic structure, spectral lines and spectrometers

Any first year text, sections on atomic structure, spectral lines and spectrometers Physics 33 Experiment 5 Atomic Spectra References Any first year text, sections on atomic structure, spectral lines and spectrometers Any modern physics text, eg F.K. Richtmeyer, E.H. Kennard and J.N.

More information

Life Cycle of Stars. Photometry of star clusters with SalsaJ. Authors: Daniel Duggan & Sarah Roberts

Life Cycle of Stars. Photometry of star clusters with SalsaJ. Authors: Daniel Duggan & Sarah Roberts Photometry of star clusters with SalsaJ Authors: Daniel Duggan & Sarah Roberts Photometry of star clusters with SalsaJ Introduction Photometry is the measurement of the intensity or brightness of an astronomical

More information

Color-Magnitude Diagram Lab Manual

Color-Magnitude Diagram Lab Manual Color-Magnitude Diagram Lab Manual Due Oct. 21, 2011 1 Pre-Lab 1.1 Photometry and the Magnitude Scale The brightness of stars is represented by its value on the magnitude scale. The ancient Greek astronomer

More information

Physics 476LW Advanced Physics Laboratory Atomic Spectroscopy

Physics 476LW Advanced Physics Laboratory Atomic Spectroscopy Physics 476LW Atomic Spectroscopy 1 Introduction The description of atomic spectra and the Rutherford-Geiger-Marsden experiment were the most significant precursors of the so-called Bohr planetary model

More information

Pizza Box Spectrometer Data & Report

Pizza Box Spectrometer Data & Report Pizza Box Spectrometer Data & Report Team Name: Members: Section or lab meeting time: Data & Observations: 1. How do you think the grating works? Explain in several sentences. 2. If you were to use your

More information

Astronomy 122. Lunar Eclipse. Make sure to pick up a grating from Emily! You need to give them back after class.

Astronomy 122. Lunar Eclipse. Make sure to pick up a grating from Emily! You need to give them back after class. Astronomy 122 Make sure to pick up a grating from Emily! You need to give them back after class. This Class (Lecture 11): Twinkle, Twinkle, Little Star Next Class: Stellar Evolution: The Main Sequence

More information

The Wolf-Rayet + O binary WR 140 in Cygnus

The Wolf-Rayet + O binary WR 140 in Cygnus The Wolf-Rayet + O binary WR 140 in Cygnus http://spektroskopie.fg-vds.de Fachgruppe SPEKTROSKOPIE 1. The system The archetype of colliding-wind binary (CWB) systems is the 7.9-year period WR+O binary

More information

DIFFRACTION GRATING. OBJECTIVE: To use the diffraction grating in the formation of spectra and in the measurement of wavelengths.

DIFFRACTION GRATING. OBJECTIVE: To use the diffraction grating in the formation of spectra and in the measurement of wavelengths. DIFFRACTION GRATING OBJECTIVE: To use the diffraction grating in the formation of spectra and in the measurement of wavelengths. THEORY: The operation of the grating is depicted in Fig. 1 on page Lens

More information

COLOR MAGNITUDE DIAGRAMS

COLOR MAGNITUDE DIAGRAMS COLOR MAGNITUDE DIAGRAMS What will you learn in this Lab? This lab will introduce you to Color-Magnitude, or Hertzsprung-Russell, Diagrams: one of the most useful diagnostic tools developed in 20 th century

More information

A Fast Algorithm for Cosmic Rays Removal from Single Images

A Fast Algorithm for Cosmic Rays Removal from Single Images A Fast Algorithm for Cosmic Rays Removal from Single Images Wojtek Pych David Dunlap Observatory, University of Toronto P.O. Box 360, Richmond Hill, Ontario, Canada L4C 4Y6 and Copernicus Astronomical

More information

ADVANCED CCD PHOTOMETRY AND EXOPLANET TRANSIT PHOTOMETRY. By : Kenny A. Diaz Eguigure

ADVANCED CCD PHOTOMETRY AND EXOPLANET TRANSIT PHOTOMETRY. By : Kenny A. Diaz Eguigure ADVANCED CCD PHOTOMETRY AND EXOPLANET TRANSIT PHOTOMETRY By : Kenny A. Diaz Eguigure KELT: THE KILODEGREE EXTREMELY LITTLE TELESCOPE Robotic Survey for Transiting Exoplanets KELT-North Deployed 2005 to

More information

EXPERIMENT 14. The Atomic Spectrum of Hydrogen

EXPERIMENT 14. The Atomic Spectrum of Hydrogen Name: Laboratory Section: Laboratory Section Date: Partners Names: Grade: Last Revised on March 18, 2003 EXPERIMENT 14 The Atomic Spectrum of Hydrogen 0. Pre-Laboratory Work [2 pts] 1. You will be using

More information

Lecture Outline: Spectroscopy (Ch. 4)

Lecture Outline: Spectroscopy (Ch. 4) Lecture Outline: Spectroscopy (Ch. 4) NOTE: These are just an outline of the lectures and a guide to the textbook. The material will be covered in more detail in class. We will cover nearly all of the

More information

KEELE UNIVERSITY SCHOOL OF CHEMICAL AND PHYSICAL SCIENCES Year 1 ASTROPHYSICS LAB. WEEK 1. Introduction

KEELE UNIVERSITY SCHOOL OF CHEMICAL AND PHYSICAL SCIENCES Year 1 ASTROPHYSICS LAB. WEEK 1. Introduction KEELE UNIVERSITY SCHOOL OF CHEMICAL AND PHYSICAL SCIENCES Year 1 ASTROPHYSICS LAB WEEK 1. Introduction D. E. McLaughlin January 2011 The purpose of this lab is to introduce you to some astronomical terms

More information

Measuring Radial Velocities of Low Mass Eclipsing Binaries

Measuring Radial Velocities of Low Mass Eclipsing Binaries Measuring Radial Velocities of Low Mass Eclipsing Binaries Rebecca Rattray, Leslie Hebb, Keivan G. Stassun College of Arts and Science, Vanderbilt University Due to the complex nature of the spectra of

More information

Starlight in the university lab: Astrolab

Starlight in the university lab: Astrolab Starlight in the university lab: Astrolab Project report (Phase 1) (2- year project, started in 2013, to be completed in 2014) 1. Short summary of the completed project that we can place on the website

More information

Lab 5: Spectroscopy & the Hydrogen Atom Phy248 Spring 2009

Lab 5: Spectroscopy & the Hydrogen Atom Phy248 Spring 2009 Lab 5: Spectroscopy & the Hydrogen Atom Phy248 Spring 2009 Name Section Return this spreadsheet to your TA that will use it to score your lab. To receive full credit you must use complete sentences and

More information

Textbook: Explorations: An Introduction to Astronomy, 4 th Edition by: Thomas T. Arny

Textbook: Explorations: An Introduction to Astronomy, 4 th Edition by: Thomas T. Arny Instructor: Brian Harker Office: SER 309 ( 797-2397 ) Email Address: brian.harker@gmail.com Class Hours: TR, 1:30pm 2:45pm in BUS 215 Office Hours: After class or by appointment Textbook: Explorations:

More information

Report on the new EFOSC2 VPH grisms

Report on the new EFOSC2 VPH grisms Report on the new EFOSC2 VPH grisms Ivo Saviane Lorenzo Monaco v 1.0 March 01, 2008 1 Introduction In January 2008 the ULTRASPEC project delivered two volume-phased holographic grisms (VPHG) to be used

More information

Astro 3 Lab Exercise

Astro 3 Lab Exercise Astro 3 Lab Exercise Lab #4: Measuring Redshifts of Galaxies Dates: August 5 6 Lab Report due: 5 pm Friday August 15 Summer 2014 1 Introduction This project involves measuring the redshifts of distant

More information

Chapter 6: Transforming your data

Chapter 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 information

Physics 1C OPTICAL SPECTROSCOPY Rev. 2-AH. Introduction

Physics 1C OPTICAL SPECTROSCOPY Rev. 2-AH. Introduction Introduction In this lab you will use a diffraction grating to split up light into its various colors (like a rainbow). You will assemble a spectrometer, incorporating the diffraction grating. A spectrometer

More information

The IRS Flats. Spitzer Science Center

The IRS Flats. Spitzer Science Center Spitzer Science Center Table of Contents The IRS Flats 1 Chapter 1. The Purpose of this Document... 3 Chapter 2.... 4 2.1 Make a finely-spaced map of a star....4 2.2 Simulate an extended source...6 2.3

More information

Studies of diffuse UV radiation

Studies of diffuse UV radiation Bull. Astr. Soc. India (2007) 35, 295 300 Studies of diffuse UV radiation N. V. Sujatha and Jayant Murthy Indian Institute of Astrophysics, Bangalore 560 034, India Abstract. The upcoming TAUVEX mission

More information

Galaxy Metallicity: What Oxygen Tells Us About The Lifecycles of Galaxies Designed by Prof Jess Werk, modified by Marie Wingyee Lau

Galaxy Metallicity: What Oxygen Tells Us About The Lifecycles of Galaxies Designed by Prof Jess Werk, modified by Marie Wingyee Lau Introduction Galaxy Metallicity: What Oxygen Tells Us About The Lifecycles of Galaxies Designed by Prof Jess Werk, modified by Marie Wingyee Lau Before stars and galaxies came into existence, the very

More information

LAB: Photometry of the Pleiades Cluster

LAB: Photometry of the Pleiades Cluster LAB: Photometry of the Pleiades Cluster ASTR 203 - Instructors Olszewski & Rigby Due IN CLASS on Oct. 30 You may work with 1 partner. If you do, only turn in 1 assignment with both your names on it! You

More information

Data Processing in DES

Data 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 information

Data Reduction - Optical / NIR Imaging. Chian-Chou Chen Ph319

Data Reduction - Optical / NIR Imaging. Chian-Chou Chen Ph319 Data Reduction - Optical / NIR Imaging Chian-Chou Chen (T.C.) @ Ph319 Images at different wavelengths... Images at different wavelengths... However, the raw data are always not as pretty Why? The total

More information

Lab 3: Open Star Cluster Age and Distance Determination

Lab 3: Open Star Cluster Age and Distance Determination Name:... Astro 101: Observational Astronomy Fall 2009 Lab 3: Open Star Cluster Age and Distance Determination 1 Observations 1.1 Objectives During this lab you will integrate some of the skills you learned

More information

arxiv: v2 [astro-ph.ep] 2 Nov 2017

arxiv: v2 [astro-ph.ep] 2 Nov 2017 Palomar Optical Spectrum of Hyperbolic Near-Earth Object A/2017 U1 Joseph R. Masiero 1 ABSTRACT arxiv:1710.09977v2 [astro-ph.ep] 2 Nov 2017 We present optical spectroscopy of the recently discovered hyperbolic

More information

NIRSpec Multi-Object Spectroscopy of Distant Galaxies

NIRSpec Multi-Object Spectroscopy of Distant Galaxies NIRSpec Multi-Object Spectroscopy of Distant Galaxies Pierre Ferruit & the NIRSpec GTO team & the NIRCam-NIRSpec galaxy assembly collaboration Proposal Planning Workshop STScI 15 May 2017 ESA UNCLASSIFIED

More information

Sky Brightness at the Hobby-Eberly Telescope

Sky Brightness at the Hobby-Eberly Telescope Sky Brightness at the Hobby-Eberly Telescope D. Austin Belknap August 15, 2008 Abstract The Hobby-Eberly Telescope (HET) at McDonald Observatory has a 9.2 m effective aperture, and has been in operation

More information

Astronomical "color"

Astronomical 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 information

Making an H-R diagram Earth & Sky

Making an H-R diagram Earth & Sky Making an H-R diagram Earth & Sky Name: Introduction Astronomers have discovered relationships between the surface temperatures and luminosities (brightnesses) of stars. These relationships are often presented

More information

Photometric and spectroscopic observations of the 2014 eclipse of the complex binary EE Cephei

Photometric and spectroscopic observations of the 2014 eclipse of the complex binary EE Cephei Photometric and spectroscopic observations of the 2014 eclipse of the complex binary EE Cephei David Boyd Variable Star Section, British Astronomical Association, [davidboyd@orion.me.uk] Abstract We report

More information

Astronomy 101 Lab: Spectra

Astronomy 101 Lab: Spectra Name: Astronomy 101 Lab: Spectra You will access your textbook in this lab. Pre-Lab Assignment: In class, we've talked about different kinds of spectra and what kind of object produces each kind of spectrum.

More information

Spectrometers. Materials: Easy Spectrometer. Old CD Razor Index card Cardboard tube at least 10 inches long

Spectrometers. Materials: Easy Spectrometer. Old CD Razor Index card Cardboard tube at least 10 inches long Spectrometers Overview: Spectrometers (spectroscopes) are used in chemistry and astronomy to measure light. In astronomy, we can find out about distant stars without ever traveling to them, because we

More information

The Grating Spectrometer and Atomic Spectra

The Grating Spectrometer and Atomic Spectra PHY 192 Grating Spectrometer 1 The Grating Spectrometer and Atomic Spectra Introduction In the previous experiment diffraction and interference were discussed and at the end a diffraction grating was introduced.

More information

10 - Celestron Telescope II: Operation

10 - Celestron Telescope II: Operation 10 - Celestron Telescope II: Operation Purpose: Gain more experience setting up a 6 Celestron telescope, familiarize yourself with the software interface, and acquire an image with the CCD camera. Due:

More information

INTRODUCTION TO THE TELESCOPE

INTRODUCTION TO THE TELESCOPE INTRODUCTION TO THE TELESCOPE What will you learn in this Lab? For a few of the labs this semester, you will be using an 8-inch Celestron telescope to take observations. This lab will introduce you to

More information

The Grating Spectrometer and Atomic Spectra

The Grating Spectrometer and Atomic Spectra PHY 192 Grating Spectrometer Spring 2012 1 The Grating Spectrometer and Atomic Spectra Introduction In the previous experiment diffraction and interference were discussed and at the end a diffraction grating

More information

ATOMIC SPECTRA. Objective:

ATOMIC SPECTRA. Objective: 1 ATOMIC SPECTRA Objective: To measure the wavelengths of visible light emitted by atomic hydrogen and verify the measured wavelengths against those predicted by quantum theory. To identify an unknown

More information

SEQUENCING THE STARS

SEQUENCING THE STARS SEQUENCING THE STARS ROBERT J. VANDERBEI Using images acquired with modern CCD cameras, amateur astronomers can make Hertzsprung-Russell diagrams from their own images of clusters. In this way, we can

More information

Experiment 7: Spectrum of the Hydrogen Atom

Experiment 7: Spectrum of the Hydrogen Atom Experiment 7: Spectrum of the Hydrogen Nate Saffold nas2173@columbia.edu Office Hour: Mondays, 5:30-6:30PM INTRO TO EXPERIMENTAL PHYS-LAB 1493/1494/2699 Introduction The physics behind: The spectrum of

More information

Detection of Exoplanets by Amateur Astronomers

Detection of Exoplanets by Amateur Astronomers Detection of Exoplanets by Amateur Astronomers September 17, 2015 by Dennis M. Conti email: dennis_conti@hotmail.com 1 Background Exoplanet (Extrasolar Planet) a planet orbiting a distant host star First

More information

arxiv:astro-ph/ v1 12 Nov 2003

arxiv:astro-ph/ v1 12 Nov 2003 A Fast Algorithm for Cosmic Rays Removal from Single Images Wojtek Pych arxiv:astro-ph/0311290v1 12 Nov 2003 David Dunlap Observatory, University of Toronto P.O. Box 360, Richmond Hill, Ontario, Canada

More information

Name: Partner(s): 1102 or 3311: Desk # Date: Spectroscopy Part I

Name: Partner(s): 1102 or 3311: Desk # Date: Spectroscopy Part I Name: Partner(s): 1102 or 3311: Desk # Date: Spectroscopy Part I Purpose Investigate Kirchhoff s Laws for continuous, emission and absorption spectra Analyze the solar spectrum and identify unknown lines

More information

Starry Night Version 5.7 Features What s new and how to use them!

Starry Night Version 5.7 Features What s new and how to use them! Starry Night Version 5.7 Features What s new and how to use them! New Features Overview 1. Space Missions (Probe Paths) 2. 3-D Object Models 3. Advanced Telescope Control panel 4. Google Maps Integration

More information

10/31/2018. Chapter 7. Atoms Light and Spectra. Thursday Lab Announcement. Topics For Today s Class Black Body Radiation Laws

10/31/2018. Chapter 7. Atoms Light and Spectra. Thursday Lab Announcement. Topics For Today s Class Black Body Radiation Laws Phys1411 Introductory Astronomy Instructor: Dr. Goderya Chapter 7 Atoms Light and Spectra Thursday Lab Announcement Jonah will start the Lab at 6:00 PM. Two pieces of Glass and HST Lunar Phases Topics

More information

ACS CCDs UV and narrowband filters red leak check

ACS CCDs UV and narrowband filters red leak check Instrument Science Report ACS 2007-03 ACS CCDs UV and narrowband filters red leak check Marco Chiaberge and Marco Sirianni May 01, 2007 ABSTRACT We present results of the observations of the star 15 Mon,

More information

NORTHERN ILLINOIS UNIVERSITY PHYSICS DEPARTMENT. Physics 211 E&M and Quantum Physics Spring Lab #9: Diffraction Spectroscopy

NORTHERN ILLINOIS UNIVERSITY PHYSICS DEPARTMENT. Physics 211 E&M and Quantum Physics Spring Lab #9: Diffraction Spectroscopy NORTHERN ILLINOIS UNIVERSITY PHYSICS DEPARTMENT Physics 211 E&M and Quantum Physics Spring 2018 Lab #9: Diffraction Spectroscopy Lab Writeup Due: Mon/Wed/Thu/Fri, April 30/ May 2/3/4, 2018 Background All

More information