IMACS Multi-Object Echelle B. Sutin, T. Hare & A. McWilliam & many others N *Not yet released *

Slides:



Advertisements
Similar presentations
EIS/Solar-B: EIS information that was sent to System Side EIS subsystems: EIS consists of three EIS subsystems. (a) STR: Structure, (b) HAR: Harness, (c)
Advertisements

Echelle Spectroscopy Dr Ray Stathakis, AAO. What is it? n Echelle spectroscopy is used to observe single objects at high spectral detail. n The spectrum.
CRIRES+ The CRIRES Upgrade Project. CRIRES+: The CRIRES Upgrade Project What is CRIRES? High resolution infrared spectrograph Installed at VLT UT1 R~100,000.
9/24/05LDP Prism description A Low Dispersion Prism for IMACS f/2 (LDP) A lower dispersion element affords more slits per mask at the expense of resolution.
Spectral Characterization of calibration lamps: STIS An improved list of emission lines for STIS Calibration Enhancement Florian Kerber, ST-ECF TIPS Meeting.
Science Case for Multi-object High Resolution Spectroscopy at Keck R. Michael Rich (UCLA) Judy Cohen (Caltech)
Spectroscopic Data ASTR 3010 Lecture 16 Textbook Ch. 11.
Echelle spectra reduction with IRAF*
FMOS Observations and Data 14 January 2004 FMOS Science Workshop.
AURA New Initiatives Office S.C. Barden, M. Liang, K.H. Hinkle, C.F.W. Harmer, R.R. Joyce (NOAO/NIO) September 17, 2001 Instrumentation Concepts for the.
Grism Spectroscopy with FLITECAM Erin C. Smith (UCLA) Ian S. McLean (UCLA)
5 th SECCHI Tam Meeting.1 COR2 Status Angelos Vourlidas.
Spectrographs. Spectral Resolution d 1 2 Consider two monochromatic beams They will just be resolved when they have a wavelength separation of d Resolving.
Astronomical Spectroscopy
Berkeley workshop summary Redundancy : dual detector Field of view : 3”x6” Spectrograph length goal: < 400 mm Isostatic mount on the base plate with control.
VOLUME-PHASE HOLOGRAPHIC GRATINGS FOR ASTRONOMICAL SPECTROGRAPHS James A. Arns, Willis S. Colburn, & Mark Benson (Kaiser Optical Systems, Inc.) Samuel.
Gemini Multi-Object Spectrograph (GMOS)
Naoyuki Tamura (University of Durham) Expected Performance of FMOS ~ Estimation with Spectrum Simulator ~ Introduction of simulators  Examples of calculations.
2.4m Telescope Group Yunnan Observatory of CAS Status of LiJET Project & The Coude Echelle Spectrograph for the Lijang 1.8m Telescope China-Japan Collaboration.
Physical Modelling of Instruments Activities in ESO’s Instrumentation Division Florian Kerber, Paul Bristow.
Memorandam of the discussion on FMOS observations and data kicked off by Ian Lewis Masayuki Akiyama 14 January 2004 FMOS Science Workshop.
Michigan/MIKE Fiber System (MMFS) – Update Apr 2005.
The Michigan/Magellan Fiber System (M2FS): An MRI Instrument Development Proposal to NSF.
AAO Fibre Instrument Data Simulator 10 October 2011 ROE Workshop 2011 Michael Goodwin Tony Farrell Gayandhi De Silva Scott Smedley Australian Astronomical.
18/19 January 2003IMACS SAC meeting update1 IMACS: Inamori-Magellan Areal Camera and Spectrograph Magellan SAC Status Report 18/19 January 2003 OCIW, Pasadena,
SALT HRS Lisa Crause for Durham CfAI & SALT Ops SALT Board Meeting #35, Chapel Hill, 5 June 2014.
2009 Aug 20 — SAC update WFOS/MOBIE1 WFOS/Multi-Object Broadband Imaging Echellette MOBIE Team, to date: PI / optical designer: Rebecca Bernstein Project.
STIS Closeout Plan Paul Goudfrooij 2005 HST Calibration Workshop, 10/26/2005.
17/18 May 2003IMACS SAC meeting update1 IMACS: Inamori-Magellan Areal Camera and Spectrograph Magellan SAC Status Report 17/18 May 2003 Univ. of Michigan,
NGC 2506 – a try for a spectroscopic study Ekaterina Atanasova Petr Kabath Christine Oppegaard Mª Carmen Sánchez Gil Tutor: Frédéric Royer 2nd NEON Archive.
14 October Observational Astronomy SPECTROSCOPY and spectrometers Kitchin, pp
Spectroscopic Observations (Massey & Hanson 2011, arXiv v2.pdf) Examples of Spectrographs Spectroscopy with CCDs Data Reduction and Calibration.
High Resolution Echelle Spectrograph for Chinese Weihai 1m Telescope. Leiwang, Yongtian Zhu, Zhongwen Hu Nanjing institute of Astronomical Optics Technology.
Near Infrared Spectro-polarimeter (NIRSP) Conceptual Design Don Mickey Jeff Kuhn Haosheng Lin.
First results of the tests campaign in VISIBLE in VISIBLE for the demonstrator 12 October 2007 SNAP Collaboration Meeting Paris Marie-Hélène Aumeunier.
Astrophotography The Basics. Image Capture Devices Digital Compact cameras Webcams Digital SLR cameras Astronomical CCD cameras.
GMTNIRS (Giant Magellan Telescope Near-IR Spectrograph) Survey Science Group Workshop 3 조 김상혁 김재영 최나현
18 October Observational Astronomy SPECTROSCOPY and spectrometers Kitchin, pp
Integral Field Spectroscopy. David Lee, Anglo-Australian Observatory.
NIRSpec Operations Concept Michael Regan(STScI), Jeff Valenti (STScI) Wolfram Freduling(ECF), Harald Kuntschner(ECF), Robert Fosbury (ECF)
Exoplanet Transit Observations at Weihai Observatory of Shandong University Chen CAO
XRT’s Observational Parameters R. Kano (NAOJ). Contents FOV & Full Disk Imaging Time Cadence & Observation Table New Items as Solar X-ray Telescopes –Pre-flare.
Oct 30, 2003PFIS - Student Wkshop1 The Prime Focus Imaging Spectrograph – Old Challenges and New Ones K. Nordsieck, Principal Investigator Jeff Percival,
September 16, 2008LSST Camera F2F1 Camera Calibration Optical Configurations and Calculations Keith Bechtol Andy Scacco Allesandro Sonnenfeld.
Data products of GuoShouJing telescope(LAMOST) pipeline and current problems LUO LAMOST Workshop.
Oct 26, 2007SALT Workshop UKZN1 Robert Stobie Prime Focus Imaging Spectrograph Science Rationale Modes –Fabry-Perot Spectral Imaging –Grating Spectroscopy;
Binospec - Next Generation Optical Spectrograph for the MMT
Multiobject Spectroscopy: Preparing and performing Michael Balogh University of Durham.
MOS Data Reduction Michael Balogh University of Durham.
Practical applications: CCD spectroscopy Tracing path of 2-d spectrum across detector –Measuring position of spectrum on detector –Fitting a polynomial.
14 January Observational Astronomy SPECTROSCOPIC data reduction Piskunov & Valenti 2002, A&A 385, 1095.
Paul Bristow (ESO Instrumentation) Thanks to: Andrea Modigliani, Joël Vernet & Florian Kerber, Sabine Moehler (ESO) Paolo Goldoni, Frédéric Royer & Régis.
Experiments and Design of a wavelength calibration procedure for MOSFIRE Principal Investigator: David Guerrero, Cal Poly SLO Research Advisor: Ian McLean,
Oct 17, 2001SALT PFIS Preliminary Design Review1 Operation Concepts Definition Document (OCDD) Chip Kobulnicky University of Wisconsin.
Visible Spectro-polarimeter (ViSP) Conceptual Design David Elmore HAO/NCAR
F. Pepe Observatoire de Genève Optical astronomical spectroscopy at the VLT (Part 2)
The Prime Focus Imaging Spectrograph for the Southern African Large Telescope: Operational Modes Chip Kobulnicky – Instrument Scientist, University of.
2. Diffraction Grating Basic principles: Diffraction
Astronomical Observation part II. Spectometry Jubee Sohn
Spatially Resolved Spectroscopy ASTR 3010 Lecture 17 Textbook Ch. 11.
From the NGSL to Absolute Flux Sara Heap, NASA/Goddard Space Flight Center Don Lindler, Sigma Space Corporation Phase 1: NGSL observations + in situ calibration.
Single Object Spectroscopy and Time Series Observations with NIRSpec
A.Zanichelli, B.Garilli, M.Scodeggio, D.Rizzo
NIRSpec Time Series Observations
TEMPO Instrument Update
Onboard Instruments of ASTROSAT
Introduction to Spectroscopy
BASIC HYPER SPECTRAL IMAGING
Spectroscopy Workshop
MIRI Low Resolution Spectroscopy
Presentation transcript:

IMACS Multi-Object Echelle B. Sutin, T. Hare & A. McWilliam & many others N *Not yet released *

● IMACS Multi-Object Echelle (MOE) F/4 focus

● Grating + Prism cross-disperser in grating module ● Grating: 245 l/mm, 37-degree blaze?,160x214mm ( 20% overfill loss) ● Prism: fused silica, 13-degree apex angle,300x200mm, 63mm base

MOE Characteristics ● Wavelength range:  (10 orders) ● ~ objects ● Resolving power (0.6 arc sec): R=21,000 ● Slit length: 5 arc seconds ● 15x15 arc min. field ● ~900 counts/pixel in 1hr at H  for V~17.0 (~1400 counts/pix/hr at 7600A) ● Cost: Parts~$35K, Labor~$20K

MOE Engineering ● October/November 2004 ● Th-Ar lamp system installed & calibrated ● Problem #1: mechanical clash! (-3mm) IMACS model off by 9mm Solution: move prism

Slide the prism down. Minimum distance now 1-2 mm.

MOE Engineering ● Problem #2: very tight fit Solution: move cables & mill the prism mounting ● Problem #3: spectral clash! Design “feature” of grating roll Solution: unique software for mask cutting (empirical vs predicted) ● Problem #4: some spectra fell between CCD gaps Solution: software

MOE Engineering ● Problem #5: blaze not centered on CCD Design flaw or grating blaze 3 degrees off Solution: in progress

Off-center Blaze for central object HH O 2 B-band Carina star #1386 V=17.88 (1 hour exposure)

Object at edge of field HH O 2 B-band Carina Star # 1107 V=17.79

MOE Science ● 1 st Science/Engineering run Dec ● Collaborators: A.Koch (Basel) & V.Smith (Gemini) ● Carina dSph mask 20 objects 12 hrs ● Fornax dSph mask 20 (10) objects 8 hrs ● A blocking filter (4 orders) ● 1 st night seeing 1.1'' fwhm ● Problem?: Nod & Shuffle mode Solution: software

HH EuII NiI FeI VI CoI Chip #2

Procedural difficulties ● Re-alignment, after each exposure, results in a shift of the spectra on the array; requires quartz spectra to be taken each time MOE is moved. ● Number of spectra: 20 obj x 4 orders x 4 ccd x 12 exp = 3840 spectra => Pipeline reduction required

Summary ● MOE works, but the blaze problem needs to be resolved. ● Pipeline reduction is essential. ● MOE complements MIKE and MIKE+fibers. ● MOE can compete with VLT/UVES+GIRAFFE and enhances our ability to study the chemical evolution of nearby systems.