SPIRE Spectrometer data analysis
|
|
- Paul Dean
- 6 years ago
- Views:
Transcription
1 SPIRE Spectrometer data analysis Rosalind Hopwood SPIRE Instrument and Calibration Scientist 26 th October 2016 Exploiting the Herschel Science Archive
2 Outline Documentation & literature Examining spectra Identifying problems Understanding the route cause of issues Problem case 1: point-like source in high Galactic cirrus Problem case 2: point-like source with a pointing offset Problem case 3: partially extended source Problem case summary Analysing the corrected data Spectral line fitting Estimating the spectral noise Mapping observations R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/2016 2
3 SpireCalibrationWeb/FTS-flyer.pdf The flyer THE FTS ICC# Spe The SPIRE Fourier Transform Spectrometer SSW c Herschel Pho tro to SPATIAL DOMAIN: INTERFEROGRAM SLW SLW KEY LITERATURE SPIRE Handbook, SPIRE Data Reduction Guide Swinyard et al., 2014 Hopwood et al., 2015 WAVELENGTH COVERAGE SSW GHz µm GHz µm INSTRUMENTAL kms kms-1 LINE WIDTH HR 1.2 GHz 1.2 GHz Frequency dependent beam CALIBRATION ACCURACY Point-source : 6% Extended-source : 1% sparse mode & 7% mapping mode AVG. CONTINUUM OFFSET (additive): Point-source calibration Extended calibration MAPPING MODES 2.6 FoV Sparse: single pointing Intermediate: 4 point jiggle Full: 16 point jiggle SPARSE OR MAPPING RASTER PATTEREN User defined FoV Fringing Glitches SLW SSW 0.4 Jy 0.3 Jy 9.4x x10-19 Wm-2Hz-1sr-1! Wm-2Hz-1sr-1! SLW CUBE SSW CUBE Small-scale shape in the spectrum Beats : strong CO ladder in the spectrum SPECTRAL DOMAIN: SPECTRUM SLW LINE PROFILE J=12-11 J=11-10 J=10-9 HR J=9-8 J=8-7 J=7-6 J=5-4 J=6-5 SSW SPECTRAL RESOLUTION HIGH (HR) 1.2 GHz, LOW (LR) 25 GHz Herschel Science Archive Level-2 SPARSE naming example for HR Point-source calibrated Spectra! HR_spectrum_point Extended calibrated! HR_spectrum_ext MAPPING naming example for HR SLW Spectral cubes! HR_SLW_cube / HR_SLW_cube_convol spectra! HR_SLW_spectrum2d R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/2016 3
4 Reference material SPIRE DRG: Chapter 7 for the Spectrometer SPIRE Handbook: FTS calibration: Swinyard et al (arxiv: ) FTS calibration program: Hopwood et al (arxiv: ) LR calibration: Marchili et al (arxiv: ) Extended-source calibration: Valtchanov et al. (in preparation) Spectrometer pipeline: Fulton et al (arxiv: ) FTS Mapping: Benielli et al (arxiv: )* Experimental Astronomer, Volume 37, Issue 2, July 2014 Five FTS papers (*including the mapping paper above) Ø Ø Ø Ø Fulton et al. FTS RSRFs arxiv: Hopwood et al. Telescope model correction arxiv: Lu et al. Bright source mode arxiv: Valtchanov et al. Relative pointing offsets arxiv: SECT: Wu et al (arxiv: ) Beam profile: Makiwa et al (Applied Optics, Vol. 52, Issue 16, p ) R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/2016 4
5 This analysis is HIPE based All Spectrometer data products are provided as FITS files and can be accessed using your preferred software See the SPIRE Spectrometer pipeline products presentation for the archive tar file folder structure and FITS file structure for Level-2 products R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/2016 5
6 Useful scripts Within HIPE there is a set of Useful scripts These are designed to: help facilitate FTS data processing/analysis be easily understood be easy to edit to compliment each other These scripts are written in Jython and some could be easily transferable to Python Suggested workflow for Spectrometer data R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/2016 6
7 Useful scripts A few more details Compares with a photometer map Subtracts extended emission using the off-axis detectors. HPDPs will be in the HSA soon. Ask the helpdesk if there is one for your observation in the interim POCT: estimates and corrects for pointing offset R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/2016 7
8 Identifying problems Looking for problem -> documentation is your first port of call SPIRE Data Reduction Guide (SDRG): Chapter 7 for the Spectrometer Relevant sections for this session are: 7.4 Pointing considerations 7.5 Recipes for faint and medium strength sources 7.6 Recipes for semi-extended sources 7.11 Spectral Analysis Does my spectrum need correcting? R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/2016 8
9 Identifying problems 1 Point- source embedded in extended emission 2 Point- source observed with a significant poin8ng offset 3 A source with par8ally extended morphology Does my spectrum need correcting? All three issues lead to a jump between SLW and SSW: Separa8ng the cause of the jump is necessary This may be difficult and some8mes not possible R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/2016 9
10 Inspecting your data Inspecting an observation in the HSA Check out the summary information provided in the search results Click on the Postcard R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
11 Inspecting your data Inspecting an observation in the HSA Check out the summary information provided in the search results This is the Browse Product image For a sparse single pointed observation this is the spectra from the centre detectors R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
12 Inspecting your data Inspecting an observation in the HSA Check out the summary information provided in the search results This is the Browse Product image For a sparse single pointed observation this is the spectra from the centre detectors ANY PROBLEMS? Not for this one R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
13 Problem case 1 1 Point-source embedded in extended emission AFGL4106: post-red supergiant binary; medium source (> 10Jy) ANY PROBLEMS? R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
14 Problem case 1 1 Point-source embedded in extended emission AFGL4106: post-red supergiant binary; medium source (> 10Jy) ANY PROBLEMS? Yes, there s a jump between the bands R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
15 Problem case 1 1 Point-source embedded in extended emission Useful script: Spectrometer array footprint plot Plots the FTS footprint over a SPIRE photometer map If no photometer map inputted then photobsids used (if there are any) Photometer map should be FIR/ submm Use to identify a background/ foreground Use to check for contaminating neighbours Hopwood et al Script edited for plot colours R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
16 SPIRE spectrometer data analysis Problem case 1 ① Point-source embedded in extended emission Useful script: Spectrometer array footprint plot Point-like Point-like sitting in Galactic Cirrus (IRAS 100 µm) Adapted from Hopwood et al figure 2 R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/ Partially extended morphology
17 Problem case 1 1 Point-source embedded in extended emission AFGL4106: post-red supergiant binary; medium source (> 10Jy) ANY PROBLEMS? The extended background is pointsource calibrated leading to a poor continuum shape and extra fringing SLW is more strongly affected due to larger beam size (~2 SSW) Large-scale continuum shape can be corrected SLWC3 Poor shape < 750 GHz Fringing > 850 GHz for SLW SSWD4 Jump between the bands R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
18 Problem case 1 1 Point-source embedded in extended emission AFGL4106: post-red supergiant binary; medium source (> 10Jy) ANY PROBLEMS? The extended background is pointsource calibrated leading to a poor continuum shape and extra fringing SLW is more strongly affected due to larger beam size (~2 SSW) Large-scale continuum shape can be corrected SLWC3 Poor shape < 750 GHz Fringing > 850 GHz for SLW SSWD4 Jump between the bands The background subtracted HPDP could be your solution if not R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
19 Problem case 1 1 Point-source embedded in extended emission SLW 1 st ring Background subtraction script results Shape improved < 750 GHz Fringing > 850 GHz for SLW still there SSW 2 nd ring Jump between the bands is corrected R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
20 Problem case 1 1 Point-source embedded in extended emission Background subtraction using the off-axis detectors A word of caution There is real flux in the detector rings See Hopwood et al for more details For a point source (Uranus/Neptune) bang on the centre there is around 1.9% in SLW 1 st ring Only 0.1% in SSW 2 nd ring (1.4% SSW 1 st ring: not used) Point source calibration accounts for this missing bit Lots more flux for semi-extended sources For AFGL4106 the results are worth the loss: fitting is easier SLW 1 st ring SSW 1 st ring SSW 2 nd ring BGS script results Jump is corrected Hopwood et al AFGL4106 R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
21 Problem case 2 2 Point-source observed with a significant pointing offset AFGL2688: point-like source See the DRG 7.4. Pointing Considerations R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
22 Problem case 2 2 Point-source observed with a significant pointing offset AFGL2688: point-like source Jump between the bands See the DRG 7.4. Pointing Considerations R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
23 Problem case 2 2 Point-source observed with a significant pointing offset AFGL2688: point-like source Check the metadata Jump between the bands See the DRG 7.4. Pointing Considerations R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
24 Problem case 2 2 Point-source observed with a significant pointing offset AFGL2688: point-like source radecoffset The offset between the commanded position and the actual reconstructed pointing, which includes any systematic BSM offset (bsmoffset), but not the APE. Jump bsmoffset BSM offset position (0.0 or 1.72 between arcsec), which is corrected for Check the metadata the bands by the point-source calibration. This systematic offset is included in the radecoffset value. radecoffset and bsmoffset give info on KNOWN pointing See the DRG offset. The APE is still associated to the pointing Pointing Considerations R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
25 Problem case 2 2 Point-source observed with a significant pointing offset Useful script: Pointing Offset Corrector (POCT) Assesses the jump between SLW and SSW bands to deduce and correct pointing offset For point-source calibrated spectra only For the centre detectors only Only use POCT to correct point-like sources The SPIRE calibration is required The method: SECT is used to create a grid of overlap ratios by offsetting the source model on a grid of pointing offsets The pointing offset is derived by interpolating the initial overlap ratio from the grid The spectra are corrected for pointing offset with SECT Input your observation ID at the top of the script and let POCT run it can take a while R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
26 Problem case 2 2 Point-source observed with a significant pointing offset Useful script: Pointing Offset Corrector (POCT) For this observation POCT finds an offset to the requested pointing of 6.08 ± > known (relative method) offset = 6.21 ± 0.32 Corrected results are the green and brown spectra Optimal offset Jump is corrected R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
27 Problem case 3 3 A source with partially extended morphology NGC6302: the Butterfly nebula with FWHM 18 See the DRG 7.6. Recipes for semi-extended sources R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
28 Problem case 3 3 A source with partially extended morphology NGC6302: the Butterfly nebula with FWHM 18 Large jump between the bands See the DRG 7.6. Recipes for semi-extended sources R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
29 Problem case 3 3 A source with partially extended morphology NGC6302: the Butterfly nebula with FWHM 18 Check the metadata See the DRG 7.6. Recipes for semi-extended sources - radecoffset is minimal (0.25 ) - OD is > 1011 so bsmoffset is 0 So what s the issue? R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
30 SPIRE spectrometer data analysis Problem case 3 ③ A source with partially extended morphology SPIRE Spectrometer calibration Point-like Semi-extended Extended Point-like Semi-extended Extended See the DRG 7.6. Recipes for semi-extended sources R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
31 SPIRE spectrometer data analysis Problem case 3 ③ A source with partially extended morphology SPIRE Spectrometer calibration Point-like Semi-extended Extended Point-like Semi-extended Extended NGC6302 See the DRG Point-source calibrated spectra 7.6. Recipes for of a semi-extended source semi-extended sources R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
32 SPIRE spectrometer data analysis Problem case 1 ① Point-source embedded in extended emission Useful script: Spectrometer array footprint plot Point-like Point-like Adapted from Hopwood et al figure 2 R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/ Partially extended morphology
33 Problem case 3 3 see Wu et al DRG Section 7.6 & the Handbook A source with partially extended morphology SECT: correcting the data for extent The SECT algorithm is based on the forward coupling efficiency to the source distribution: so a good knowledge of the source distribution is key Here we use the default SECT settings with: - a basic elliptical Gaussian - FWHM of 18 - Eccentricity of No x- or y-offset And setting the source model diameter to be optimised (optimisediameter=true) HOWEVER the correction efficiency (η c ) is assumed to be 1, which may not be true and can introduce extra uncertainties R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
34 Problem case 3 3 A source with partially extended morphology NGC6302: the Butterfly nebula with FWHM 18 Optimum diameter calculated as 18.5 SECT plots the uncorrected and corrected spectra Jump is corrected see Wu et al DRG Section 7.6 & the Handbook R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/ There is room for improvement: Needs better knowledge of the source model
35 Summary Three key problems that SPIRE Spectra can suffer have been addressed 1. High extended background: background subtracted HPDPs will be available in the HSA soon for this issue soon contact the Helpdesk to see if there is such an HPDP already created for your observation subtracting the off-axis detectors subtracts some real signal weigh up the benefit relative to this 2. Unknown pointing offset: the offset can be estimated using the overlap region not easy to correct in this way for semi-extended sources, unless you have good knowledge of the source distribution 3. Partial source extent: the SECT method should be used a good knowledge of the source distribution is needed η c may not be 1 R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
36 Workflow on corrected data The corrected spectra are ready for scientific analysis Spectral line fitting: there is a useful script for line fitting, but if using a fitter outside of HIPE, a few things to remember: The line shape is well represented by a sinc profile Due to asymmetry in the line profile, there is a 2.6% shortfall in line flux calculated from the fitted sinc parameters See DRG Section 7.11 R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
37 Workflow on corrected data The corrected spectra are ready for scientific analysis Spectral line fitting: there is a useful script for line fitting, but if using a fitter outside of HIPE, a few things to remember: Apodized data may help when searching for faint lines, but fit and take measurement from the standard spectra See DRG Section 7.11 R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
38 Workflow on corrected data The corrected spectra are ready for scientific analysis Spectral line fitting: there is a useful script for line fitting, but if using a fitter outside of HIPE, a few things to remember: Fit to the lines and continuum simultaneously to achieve the best fit See DRG Section 7.11 R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
39 Analysing the corrected data The corrected spectra are ready for scientific analysis Estimating the spectral noise: there is a useful script for noise estimation, but the method is straightforward and easy to perform outside of HIPE, a few things to remember: Lines should be removed before taking the noise the sinc wings cause ringing across the frequency range, which is the dominant noise source for spectra with strong features See DRG Section 7.11 R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
40 Analysing the corrected data The corrected spectra are ready for scientific analysis Estimating the spectral noise: there is a useful script for noise estimation, but the method is straightforward and easy to perform outside of HIPE, a few things to remember: Lines should be removed before taking the noise the sinc wings cause ringing across the frequency range, which is the dominant noise source for spectra with strong features Correcting semi-extended data or correcting for pointing offset will increase the noise estimate because the data are corrected for lost flux by a multiplicative factor See DRG Section 7.11 R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
41 Analysing the corrected data The corrected spectra are ready for scientific analysis Estimating the spectral noise: there is a useful script for noise estimation, but the method is straightforward and easy to perform outside of HIPE, a few things to remember: Lines should be removed before taking the noise the sinc wings cause ringing across the frequency range, which is the dominant noise source for spectra with strong features Correcting semi-extended data or correcting for pointing offset will increase the noise estimate because the data are corrected for lost flux by a multiplicative factor The next two slides illustrate these points for problem case 3 NGC6302 See DRG Section 7.11 R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
42 Analysing the corrected data The corrected spectra are ready for scientific analysis Estimating the spectral noise for problem case 3 NGC6302 (Method: standard deviation of baseline subtracted data in frequency bins) Green dashed is noise estimate for the data straight from the archive Blue is the noise estimate for SECT corrected. Which goes up after data is corrected up Lines dominate the noise NGC6302 See DRG Section 7.11 R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
43 Analysing the corrected data The corrected spectra are ready for scientific analysis Estimating the spectral noise for problem case 3 NGC6302 (Method: standard deviation of baseline subtracted data in frequency bins) Blue is the noise estimate for SECT corrected The noise is above HSpot due to SECT Orange is after first fitting to the strongest lines Red is noise estimate for the SECT corrected and line subtracted data NGC6302 R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
44 Mapping: spatial resolution From the SPIRE instrument introduction presentation 4-jiggle pattern 16-jiggle pattern R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
45 Mapping: coverage SLW inter, 35 SSW inter, 19 SLW full, 17.5 SSW full, 9.5 Cube Image Error Coverage (naïve cube) R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
46 Mapping SSW cubes for NGC 7023 ( ) LR, fully sampled, special calibration raster from OD 261 Naïve cube mean of spectra within a pixel CP cube Gaussian weighted mean of spectra within kernel Integrated maps over GHz CP cube is smoother (lower noise) Convolved spatially, so no difference in line shape Naïve cubes suffer from holes : no coverage CP cubes can have partial spectra at the edges: low coverage They have the same WCS See DRG Sections 7.8 & 7.12 R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
47 Mapping SSW cubes for the Orion Bar ( ) LR, fully sampled, special calibration raster from OD 261 There are a number of tools & scripts in HIPE that are geared for Herschel cube analysis Integrated line flux plot from the Spectrometer Cube Fitting script See DRG Sections 7.8 & 7.12 R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
48 Q&A Not all of the useful scripts available in HIPE were covered If you have any questions on these, or the ones that were, or any other Spectrometer problems, send them to the helpdesk for the afternoon Q&A Thanks for attending! R. Hopwood Exploiting the Herschel Science Archive: SPIRE Spectrometer data analysis ESAC 26/10/
esac Release Note for the Herschel SPIRE Fourier-Transform Spectrometer Background Subtracted Spectra
esac European Space Astronomy Centre (ESAC) P.O. Box, 78 28691 Villanueva de la Cañada, Madrid Spain Release Note for the Herschel SPIRE Fourier-Transform Spectrometer Background Subtracted Spectra Prepared
More informationIvan Valtchanov Herschel Science Centre European Space Astronomy Centre (ESAC) ESA. ESAC,20-21 Sep 2007 Ivan Valtchanov, Herschel Science Centre
SPIRE Observing Strategies Ivan Valtchanov Herschel Science Centre European Space Astronomy Centre (ESAC) ESA Outline SPIRE quick overview Observing with SPIRE Astronomical Observation Templates (AOT)
More informationPACS spectroscopy Data Analysis
PACS spectroscopy Data Analysis Elena Puga Herschel Science Centre ESA 27/10/2016 Exploiting the Herschel Science Archive E. Puga Exploiting the Herschel Science Archive: PACS Spectrometer Data Analysis
More informationSPIRE In-flight Performance, Status and Plans Matt Griffin on behalf of the SPIRE Consortium Herschel First Results Workshop Madrid, Dec.
SPIRE In-flight Performance, Status and Plans Matt Griffin on behalf of the SPIRE Consortium Herschel First Results Workshop Madrid, Dec. 17 2009 1 Photometer Herschel First Results Workshop Madrid, Dec.
More informationSPIRE FTS Pipelines and Data Products Trevor Fulton
SPIRE FTS Pipelines and Data Products Trevor Fulton Blue Sky Spectroscopy Lethbridge, Alberta, Canada SPIRE FTS Pipelines and Data Products Data Products Observation Context Levels 0-2 Data Processing
More informationOpen Research Online The Open University s repository of research publications and other research outputs
Open Research Online The Open University s repository of research publications and other research outputs Calibration of Herschel SPIRE FTS observations at different spectral resolutions Journal Item How
More informationChris Pearson: RAL Space. Chris Pearson: April
Chris Pearson: RAL Space 1 2 Young Star Dust Clouds Infra Red Light 3 Starlight reprocessed to infrared wavelengths 4 1983: The Dawn of Infrared Astronomy Infra-Red Astronomical Satellite (IRAS) All sky
More informationCalibration of the Herschel SPIRE Fourier Transform Spectrometer
doi:10.1093/mnras/stu409 Calibration of the Herschel SPIRE Fourier Transform Spectrometer B. M. Swinyard, 1,2 E. T. Polehampton, 2,3 R. Hopwood, 4 I. Valtchanov, 5 N. Lu, 6 T. Fulton, 3,7 D. Benielli,
More informationarxiv: v1 [astro-ph.im] 9 Jan 2014
Noname manuscript No. (will be inserted by the editor) Herschel SPIRE FTS telescope model correction Rosalind Hopwood Trevor Fulton Edward T. Polehampton Ivan Valtchanov Dominique Benielli Peter Imhof
More informationHIFI webinar: News, Calibrations, and Data Processing Updates
NHSC HIFI Webinar December 17, 2012 HIFI webinar: News, Calibrations, and Data Processing Updates Pat Morris, Adwin Boogert, Colin Borys with contributions from D. Teyssier & C. McCoey Outline 1. Observatory
More informationPACS Wavelength Switching AOT release note
PACS Wavelength Switching AOT release note 1 Prepared by the PACS ICC 20 January 2010 Wavelength switching release note version of 03-dec-2009 updated with full dynamic range saturation limits. Differences
More informationHerschel Calibration Report for HUG#9.
Herschel Calibration Report for HUG#9. Anthony Marston, Herschel Instrument and Calibration Scientist Team Lead, HSC, ESAC, Spain. To Herschel User s Group #9, 18-19 June 2015. - page 1 Outline of Presentation
More informationAnnouncement of Opportunity for Open Time. SPIRE PACS Parallel Mode Observers' Manual
Announcement of Opportunity for Open Time SPIRE PACS Parallel Mode Observers' Manual HERSCHEL-HSC-DOC-0883, Version 2.1 4-October-2011 SPIRE PACS Parallel Mode Observers' Manual Published version 2.1,
More informationarxiv: v1 [astro-ph.im] 5 Mar 2014
Mon. Not. R. Astron. Soc. 000, 1 18 (2013) Printed 6 March 2014 (MN LATEX style file v2.2) Calibration of the Herschel SPIRE Fourier Transform Spectrometer arxiv:1403.1107v1 [astro-ph.im] 5 Mar 2014 B.
More informationSUBJECT: SPIRE Spectrometer Detector Thermal Time Constant Derivation Procedure
SUBJECT: PREPARED BY: Time Constant Derivation Procedure Trevor Fulton DOCUMENT No: SPIRE-BSS-NOT- ISSUE: Draft 0.2 APPROVED BY: Date: Page: 2 of 11 Distribution Name Sarah Leeks Edward Polehampton Trevor
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 informationHerschel/SPIRE FTS View of M82 Probing the molecular ISM in M82 starburst
Herschel/SPIRE FTS View of M82 Probing the molecular ISM in M82 starburst Pasquale Panuzzo (CEA Saclay Irfu/SAp) and SAG2: N. Rangwala, A. Rykala, K. G. Isaak, J. Glenn, C. D. Wilson, L. Spinoglio, M.
More informationNew RSRF ( #49) Corrects Resident PACS Lines for the Red Order Leak Steve Lord, NHSC Caltech. Steve Lord
New RSRF ( #49) Corrects Resident PACS Lines for the Red Order Leak Steve Lord, NHSC Caltech Understanding the Problem (I/II): Summary: The PACS spectrometer suffers an "order light leak" where flux from
More informationVisualisation and Manipulation Tools for Herschel Spectra. Russell Shipman
Visualisation and Manipulation Tools for Herschel Spectra Russell Shipman Outline Goal of Spectral Tools Why develop common tools Guidelines for functionality/requirements Answering user scenario: our
More informationPACS Spectroscopy performance and calibration PACS Spectroscopy performance and calibration
1 of 18 PACS Spectroscopy performance and Prepared by Bart Vandenbussche With inputs by Alessandra Contursi Helmut Feuchtgruber Katrina Exter Christophe Jean Albrecht Poglitsch Elena Puga Pierre Royer
More informationPACS Spectroscopy performance and calibration PACS Spectroscopy performance and calibration
1 of 18 PACS Spectroscopy performance and PICC-KL-TN-041 Prepared by With inputs by Bart Vandenbussche Joris Blommaert Alessandra Contursi Helmut Feuchtgruber Christophe Jean Albrecht Poglitsch Pierre
More informationThe data processing pipeline for the Herschel SPIRE Fourier Transform Spectrometer
Advance Access publication 2016 February 25 doi:10.1093/mnras/stw343 The data processing pipeline for the Herschel SPIRE Fourier Transform Spectrometer T. Fulton, 1,2 D. A. Naylor, 1 E. T. Polehampton,
More informationSPIRE Observers Manual
SPIRE Observers Manual HERSCHEL-DOC-0798, version 2.4, June 7, 2011 2 SPIRE Observers Manual Version 2.4, June 7, 2011 This document is based on inputs from the SPIRE Consortium and the SPIRE Instrument
More informationExtraction 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 informationesac Herschel/HIFI Spectral Map Highly Processed Data Products Release Notes
esac European Space Astronomy Centre (ESAC) P.O. Box 78 28691 Villanueva de la Cañada, Madrid Spain NHSC NASA Herschel Science Center IPAC, Caltech 1200 E. California Blvd, Pasadena, CA, USA Herschel/HIFI
More informationPACS Spectrometer Wavelength Calibration
PACS Spectrometer Wavelength Calibration H. Feuchtgruber Max-Planck-Institut für extraterrestrische Physik, Garching PACS WaveCal 1 Description of the Calibration Problem - Blue array: 400 pixels - Red
More informationContinuum Submillimetre Astronomy from UKIRT. Ian Robson UK ATC
Continuum Submillimetre Astronomy from UKIRT Ian Robson UK ATC Submillimetre means high - how high can we get? let s s go to Hawaii! (1975,( 76) We need a submillimetre photometer! Lots of lessons learned
More informationPlanetary Models updates
Planetary Models updates Raphaël Moreno Observatoire de Paris-Meudon (LESIA) HIFI cross-calibration measurements: Uranus & Neptune Neptune/CO (SPIRE) TITAN Planet splinter summary (Dec. 2010 ) Herschel
More informationFIRST carrier spacecraft
FIRST carrier spacecraft Height 9 m Width 4.5 m Launch mass 3300 kg Power 1 kw Launch vehicle Ariane 5 Orbit Lissajous around L2 Science data rate 100 kbps Telescope diametre 3.5 m Telescope WFE 10 µm
More informationarxiv: v1 [astro-ph.im] 17 Jun 2009
Astronomy & Astrophysics manuscript no. sps paper accepted c ESO 2018 October 19, 2018 SPS: A software simulator for the Herschel-SPIRE photometer B. Sibthorpe 1, P. Chanial 2, and M. J. Griffin 3 1 UK
More informationSurface brightness comparison of PACS blue array with IRAS and Spitzer/MIPS images. Babar Ali, NHSC
Extended Source Photometry Page 1 Surface brightness comparison of PACS blue array with IRAS and Spitzer/MIPS images Babar Ali, NHSC Document change record Version Date Changes 1.01 12-April-2011 Version
More informationTHE LAST SURVEY OF THE OLD WSRT: TOOLS AND RESULTS FOR THE FUTURE HI ABSORPTION SURVEYS
F. Maccagni; R. Morganti; T. Oosterloo; K. Geréb; N. Maddox, J. Allison THE LAST SURVEY OF THE OLD WSRT: TOOLS AND RESULTS FOR THE FUTURE HI ABSORPTION SURVEYS A SURVEY BEFORE THE BLIND SURVEYS During
More informationNAOYUKI 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 informationEarly-Science call for observing time with SAM-FP
Early-Science call for observing time with SAM-FP 1. General description SOAR is opening a call for proposals for early-science with SAM-FP in 2016B, for 4 nights (September 29 October 2, 2016). SAM-FP
More informationHerschel Spectroscopy Crosscalibration
Herschel Spectroscopy Crosscalibration Herschel Science Centre E.Puga D. Teyssier A. Marston 1 Spectral Wavelength Overlap SPIRE leak ~190.0-220.0 microns 2 Routine Calibration Programmes Post-AGB AFGL
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 informationOpen 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 informationComparing Ultraviolet and Infrared Star Formation Tracers
Comparing Ultraviolet and Infrared Star Formation Tracers George J. Bendo and Rebecca Freestone Jodrell Bank Centre for Astrophysics, The University of Manchester 15 February 2018 Overview The DS9 image
More informationThe Herschel/PACS Point Source Catalog
The Herschel/PACS Point Source Catalog G. Marton 1, Cs. Kiss 1, R. Paladini 2, L. Calzoletti 3, B. Altieri 3, J. Rector 2, E. Verebélyi 1 1. Konkoly Observatory, Budapest, Hungary 2. IPAC, Pasadena, CA,
More informationORBS and ORCS. Reduction and analysis of SITELLE's data
ORBS and ORCS Reduction and analysis of SITELLE's data omas Martin (Université Laval) Laurent Drissen (Université Laval) Laurie Rousseau-Nepton (Université Laval), Alexandre Alarie (Université Laval),
More informationThe Herschel-SPIRE Point Source Catalog Feasibility Study Report
1 The Herschel-SPIRE Point Source Catalog Feasibility Study Report Bernhard Schulz 1, Gabor Marton 2, Kevin Xu 1, Nanyao Lu 1, David Shupe 1, Ivan Valtchanov 3, Babar Ali 1, Chris Pearson 4, John Rector
More informationBINGO simulations and updates on the performance of. the instrument
BINGO simulations and updates on the performance of BINGO telescope the instrument M.-A. Bigot-Sazy BINGO collaboration Paris 21cm Intensity Mapping Workshop June 2014 21cm signal Observed sky Credit:
More informationContinuum Observing. Continuum Emission and Single Dishes
July 11, 2005 NAIC/NRAO Single-dish Summer School Continuum Observing Jim Condon Continuum Emission and Single Dishes Continuum sources produce steady, broadband noise So do receiver noise and drift, atmospheric
More informationThe HIFI Beam: Release #1 Release Note for Astronomers
The HIFI Beam: Release #1 Release Note for Astronomers Michael Mueller, Willem Jellema (SRON Netherlands Institute for Space Research, The Netherlands), Michael Olberg (Onsala Space Observatory, Sweden)
More informationFourier transform spectroscopy: an introduction. David Naylor University of Lethbridge
Fourier transform spectroscopy: an introduction David Naylor University of Lethbridge Outline History Ideal vs real FTS Pros/cons Extension to ifts Examples: Sitelle, SPIRE, Safari Michelson s original
More informationUpdated flux calibration and fringe modelling for the ACS/WFC G800L grism
Updated flux calibration and fringe modelling for the ACS/WFC G800L grism H. Kuntschner, M. Kümmel, J. R. Walsh January 25, 2008 ABSTRACT A revised flux calibration is presented for the G800L grism with
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 informationSpectral Analysis of High Resolution X-ray Binary Data
Spectral Analysis of High Resolution X-ray Binary Data Michael Nowak, mnowak@space.mit.edu X-ray Astronomy School; Aug. 1-5, 2011 Introduction This exercise takes a look at X-ray binary observations using
More informationSubmillimetre astronomy
Sep. 20 2012 Spectral line submillimetre observations Observations in the submillimetre wavelengths are in principle not different from those made at millimetre wavelengths. There are however, three significant
More informationIRAM Memo IRAM-30m EMIR time/sensitivity estimator
IRAM Memo 2009-1 J. Pety 1,2, S. Bardeau 1, E. Reynier 1 1. IRAM (Grenoble) 2. Observatoire de Paris Feb, 18th 2010 Version 1.1 Abstract This memo describes the equations used in the available in the GILDAS/ASTRO
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 informationLab 4: Stellar Spectroscopy
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
More informationSPIRE/PACS Parallel Mode
SPIRE/PACS Parallel Mode Herschel Observation Planning Workshop ESAC, 20 21 September 2007, Sarah Leeks Herschel Science Centre European Space Astronomy Centre Research and Scientific Support Department
More informationGemini Integration Time Calculators
Gemini Integration Time Calculators Phil Puxley SPE-C-G0076 Version 1.1; June 1998 Version History: 1.0 June 1998; first draft. 1.1 June 1998; following comments from Ted von Hippel and Joe Jensen. 1.
More informationCHARA Collaboration Year-Eight Science Review. VLTI update. F. Delplancke
VLTI update F. Delplancke Summary Infrastructure Current instruments: MIDI, AMBER, PIONIER Under test & commissioning: PRIMA 2 nd generation instruments Long Range Plan Infrastructure Infrastructure 4
More informationObserving with the Infrared Spectrograph
Observing with the Infrared Spectrograph C. Grillmair, L. Armus GO Workshop 21-22 November 2002 Outline 1) Meet the IRS IST 2) Basic IRS capabilities 3) Observing and readout modes 4) Data products and
More informationCOS FUV Focus Determination for the G140L Grating
Instrument Science Report COS 2012-01 COS FUV Focus Determination for the G140L Grating Parviz Ghavamian 1 Space Telescope Science Institute, Baltimore, MD October 03, 2012 ABSTRACT The procedures for
More informationPublic Release of NIKA Sunyaev-Zel'dovich Data
Public Release of NIKA Sunyaev-Zel'dovich Data Explanatory supplement Contact : Remi Adam (radam@cefca.es) NIKA was used to image galaxy clusters using the Sunyaev-Zel dovich (SZ) effect. A total of six
More informationarxiv: v3 [astro-ph.im] 18 Aug 2016
Astronomy & Astrophysics manuscript no. DarioFadda c ESO 2018 October 10, 2018 Transient effects in Herschel/PACS spectroscopy Dario Fadda 1,, Jeffery D. Jacobson 2, and Philip N. Appleton 2 arxiv:1601.07729v3
More informationSPIRE Spectrometer Pipeline Description
SPIRE Spectrometer Pipeline Description SPIRE-BSS-DOC-002966 Trevor Fulton Issue 1.2 05 December 2008 SPIRE Spectrometer Pipeline Description Trevor Fulton Table of Contents 1. Introduction... 1 1.1. Acronyms...
More informationESO Phase 3 Data Release Description. Data Collection ATLASGAL Release Number 1 Data Provider
ESO Phase 3 Data Release Description Data Collection ATLASGAL Release Number 1 Data Provider Frederic Schuller, K. Immer, Y. Contreras, T. Csengeri, J. S. Urquhart Date 19.01.2016 Abstract The APEX Telescope
More informationThe in-orbit wavelength calibration of the WFC G800L grism
The in-orbit wavelength calibration of the WFC G800L grism A. Pasquali, N. Pirzkal, J.R. Walsh March 5, 2003 ABSTRACT We present the G800L grism spectra of the Wolf-Rayet stars WR45 and WR96 acquired with
More informationASTRONOMY 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 informationCorrecting the extended-source calibration for the Herschel-SPIRE Fourier-transform spectrometer
Advance Access publication 2017 December 9 doi:10.1093/mnras/stx3178 Correcting the extended-source calibration for the Herschel-SPIRE Fourier-transform spectrometer I. Valtchanov, 1 R. Hopwood, 1,2 G.
More informationNICMOS Status and Plans
1997 HST Calibration Workshop Space Telescope Science Institute, 1997 S. Casertano, et al., eds. NICMOS Status and Plans Rodger I. Thompson Steward Observatory, University of Arizona, Tucson, AZ 85721
More informationThe ALMA Observing Preparation Tool
The ALMA Observing Preparation Tool Atacama Large Millimeter/submillimeter Array Expanded Very Large Array Robert C. Byrd Green Bank Telescope Very Long Baseline Array For a video version of this material:
More informationFORCAST: Science Capabili2es and Data Products. William D. Vacca
FORCAST: Science Capabili2es and Data Products William D. Vacca Faint Object infrared Camera for the SOFIA Telescope (FORCAST) SWC (blue) Light from telescope LWC (red) Facility Instrument PI: Terry Herter
More informationPrinciples of Interferometry. Hans-Rainer Klöckner IMPRS Black Board Lectures 2014
Principles of Interferometry Hans-Rainer Klöckner IMPRS Black Board Lectures 2014 acknowledgement Mike Garrett lectures James Di Francesco crash course lectures NAASC Lecture 5 calibration image reconstruction
More informationCan we do this science with SKA1-mid?
Can we do this science with SKA1-mid? Let s start with the baseline design SKA1-mid expected to go up to 3.05 GHz Proposed array configuration: 133 dishes in ~1km core, +64 dishes out to 4 km, +57 antennas
More informationDiffuse AME emission in Perseus
Diffuse AME emission in Perseus A strange beast Bob Watson, JBCA Summary Tenerife experiment first hint COSMOSOMAS Leading to Perseus SED Less filtered data (1 harmonic removal) Component separation VSA
More informationOptimal resolutions for optical and NIR spectroscopy S. Villanueva Jr.* a, D.L. DePoy a, J. L. Marshall a
Optimal resolutions for optical and NIR spectroscopy S. Villanueva Jr.* a, D.L. DePoy a, J. L. Marshall a a Department of Physics and Astronomy, Texas A&M University, 4242 TAMU, College Station, TX, USA
More informationA software simulator for the Herschel-SPIRE imaging photometer
A software simulator for the Herschel-SPIRE imaging photometer Bruce Sibthorpe *, Adam Woodcraft, Matthew Griffin, Steven Lloyd Watkin Department of Physics & Astronomy, Cardiff University, Cardiff CF24
More information1 General Considerations: Point Source Sensitivity, Surface Brightness Sensitivity, and Photometry
MUSTANG Sensitivities and MUSTANG-1.5 and - Sensitivity Projections Brian S. Mason (NRAO) - 6sep1 This technical note explains the current MUSTANG sensitivity and how it is calculated. The MUSTANG-1.5
More informationShort-Spacings Correction From the Single-Dish Perspective
Short-Spacings Correction From the Single-Dish Perspective Snezana Stanimirovic & Tam Helfer (UC Berkeley) Breath and depth of combining interferometer and single-dish data A recipe for observing extended
More informationAnalysis of wavelength shifts reported for X-shooter spectra
Analysis of wavelength shifts reported for X-shooter spectra S. Moehler (SDP) June 15, 2015 Executive Summary I investigated the causes for wavelength offsets seen in telluric lines and sky lines of extracted
More informationSPIRE: Herschel s Submillimetre Camera and Spectrometer
SPIRE: Herschel s Submillimetre Camera and Spectrometer Matt Griffin, Alain Abergel, Peter Ade, Philippe André, Jean-Paul Baluteau, James Bock, Alberto Franceschini, Walter Gear, Jason Glenn, Douglas Griffin,
More informationLab 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 informationEvolution of Telescope Background with Time (OD)
Evolution of Telescope Background with Time (OD) Best sampling with HD161796, no absolute flux -- Express telescope in units of source (3x3 co-added, no pointing or point source correction) Second-best
More informationAbsolute Flux Calibration for STIS First-Order, Low-Resolution Modes
Instrument Science Report STIS 97-14 Absolute Flux Calibration for STIS First-Order, Low-Resolution Modes Ralph Bohlin, Space Telescope Science Institute Nicholas Collins, Hughes STX/LASP/GSFC Anne Gonnella,
More informationA survey of the 6.7 GHz methanol maser emission from IRAS sources
ASTRONOMY & ASTROPHYSICS APRIL II 2000, PAGE 269 SUPPLEMENT SERIES Astron. Astrophys. Suppl. Ser. 143, 269 301 (2000) A survey of the 6.7 GHz methanol maser emission from IRAS sources I. Data? M. Szymczak,
More informationABSTRACT. a Institute for Space Imaging Science, University of Lethbridge, Alberta, T1K 3M4, Canada; b Joint
The spectral response of the SCUBA-2 850 and 450 micron photometric bands David A. Naylor* a, Brad G. Gom a, Sherif AbdElazim a, Per Friberg b, Daniel Bintley b, Wayne S. Holland c, Michael J. MacIntosh
More informationThe Relation Between Gas Density and Star Formation Rate in the Spiral Galaxy M100
The Relation Between Gas Density and Star Formation Rate in the Spiral Galaxy M100 George J. Bendo and Rebecca Freestone Jodrell Bank Centre for Astrophysics, The University of Manchester 04 January 2018
More informationarxiv: v2 [astro-ph.im] 2 Jan 2018
Preprint 3 January 2018 Compiled using MNRAS LATEX style file v3.0 arxiv:1708.09203v2 [astro-ph.im] 2 Jan 2018 Correcting the extended-source calibration for the Herschel-SPIRE Fourier-Transform Spectrometer
More informationGIS Data Processing. Eddie Breeveld MSSL/UCL
GIS Data Processing Eddie Breeveld MSSL/UCL erb@mssl.ucl.ac.uk GIS Data Processing Introduction and status of the GIS system Planning GIS Observations Displaying GIS Data Correcting Instument Effects Fixed
More informationTime Variability of Molecular Line Emission in IRC+10216
Time Variability of Molecular Line Emission in IRC+10216 David Teyssier, ESA-ESAC, Spain J. Cernicharo, G. Quintana-Lacaci, M. Agúndez, M. Barlow, E. de Beck, F. Daniel, L. Decin, P. GarciaLario, M. Groenewegen,
More informationALMA Science Verification Program. Martin Zwaan ALMA Regional Centre ESO, Garching
ALMA Science Verification Program Martin Zwaan ALMA Regional Centre ESO, Garching Science Verification The process by which ALMA demonstrates that it is capable of producing data of the required quality
More informationIntroduction to the Sloan Survey
Introduction to the Sloan Survey Title Rita Sinha IUCAA SDSS The SDSS uses a dedicated, 2.5-meter telescope on Apache Point, NM, equipped with two powerful special-purpose instruments. The 120-megapixel
More informationThe H.E.S.S. Standard Analysis Technique
The H.E.S.S. Standard Analysis Technique Wystan Benbow for the H.E.S.S. Collaboration Max Planck Institut für Kernphysik Postfach 103980 D-69029 Heidelberg, Germany The High Energy Stereoscopic System
More informationCommon questions when planning observations with DKIST Jan 30, 2018
Common questions when planning observations with DKIST Jan 30, 2018 1. Can the DKIST instruments work together? All instruments except Cryo-NIRSP can work together and with Adaptive Optics (AO). All can
More informationMALATANG THOMAS R. GREVE UNIVERSITY COLLEGE LONDON. MApping the dense molecular gas in The strongest star-forming Galaxies
MALATANG MApping the dense molecular gas in The strongest star-forming Galaxies www.eaobservatory.org/jcmt On behalf of the MALATANG team: THOMAS R. GREVE UNIVERSITY COLLEGE LONDON Seoul National University,
More informationData analysis of massive data sets a Planck example
Data analysis of massive data sets a Planck example Radek Stompor (APC) LOFAR workshop, Meudon, 29/03/06 Outline 1. Planck mission; 2. Planck data set; 3. Planck data analysis plan and challenges; 4. Planck
More informationThe Cornell Atlas of Spitzer Spectra (CASSIS) and recent advances in the extraction of complex sources
The Cornell Atlas of Spitzer Spectra (CASSIS) and recent advances in the extraction of complex sources V. Lebouteiller (CEA & Cornell University) D.J. Barry, G.C. Sloan, H.W.W. Spoon, D.W. Weedman, J.R.
More informationCommissioning of the Hanle Autoguider
Commissioning of the Hanle Autoguider Copenhagen University Observatory Edited November 10, 2005 Figure 1: First light image for the Hanle autoguider, obtained on September 17, 2005. A 5 second exposure
More informationPossibilities for handling SRF variation in the MTG-IRS detector array
Possibilities for handling SRF variation in the MTG-IRS detector array Nigel Atkinson (Met Office) ECMWF / EUMETSAT / NWP-SAF Workshop on the assimilation of high temporal resolution satellite data May
More informationThe ALMA Observing Preparation Tool
The ALMA Observing Preparation Tool Atacama Large Millimeter/submillimeter Array Expanded Very Large Array Robert C. Byrd Green Bank Telescope Very Long Baseline Array Video versions of this material:
More informationObjectives: (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 informationPysynphot: A Python Re Implementation of a Legacy App in Astronomy
Pysynphot: A Python Re Implementation of a Legacy App in Astronomy Vicki Laidler 1, Perry Greenfield, Ivo Busko, Robert Jedrzejewski Science Software Branch Space Telescope Science Institute Baltimore,
More informationDetermining the Specification of an Aperture Array for Cosmological Surveys
Determining the Specification of an Aperture Array for Cosmological Surveys P. Alexander University of Cambridge, Department of Physics, Cavendish Laboratory, Cambridge, UK. A. J. aulkner Jodrell Bank
More informationFIFI-LS Commissioning
FIFI-LS Commissioning March April 2014 Dr. Randolf Klein FIFI-LS Instrument Scientist USRA 1 The Team S. Beckmann A. Bryant S. Colditz C. Fischer F. Fumi N. Geis R. Hönle R. Klein A. Krabbe (PI) L. Looney
More informationCONFUSION NOISE AND BACKGROUND
Konkoly Infrared & Space Astronomy Group CONFUSION NOISE AND BACKGROUND Csaba Kiss Introduction Confusion noise was very important for the recent infrared space instruments (e.g. those of IRAS, ISO and
More information