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Outline 1.  Introduction: what this is about 2.  Line intensity extraction in HIFI spectra – Demo 3.  Continuum intensity extraction in HIFI spectra – Demo 4.  Best practice for cross-comparison with other instruments/observatories
– Demo
On-line Spectroscopy WS – 23-25 April 2014 - page 2
Introduction
•  This session focuses on line intensity and continuum level extraction in the framework of single pointing observations (point mode and spectral scan observations)
•  For mapping observations, similar concepts and rules will apply but additional tools are available in HIPE, that shall be presented at a later stage
On-line Spectroscopy WS – 23-25 April 2014 - page 3
Line intensity/area extraction •  For simple line profiles, the preferred approach should be to use the
Spectrum Fitter GUI (SFG)
–  Can be applied as interactive GUI –  Can be run as a command line code, written from scratch or based on
a GUI session export –  Detailed documentation at: http://herschel.esac.esa.int/hcss-doc-12.0/load/dag/html/Dag.Ch.SpectralFitting.SEII.html
•  When line profiles are too complex to be well represented by (multi-)line model fit, it is more accurate to simply sum up (integrate) all intensity channels within a given frequency range –  A task called integrator can be used for that matter –  It allows to take a simple baseline model into account based on
channels neighbouring the targeted line
DEMO: CO 6-5 line area extraction in NGC6302
On-line Spectroscopy WS – 23-25 April 2014 - page 4
Continuum level extraction (1) •  To first order, the continuum level is well represented by the mean
baseline intensity over the 4 GHz IF bandwidth •  However the following considerations need to be taken into account:
•  HIFI is Double-Sideband in nature so it measures the sum of the two sideband continua. Also it applies a SBR correction correct only for lines
•  Standing waves will not strictly cancel out if the IF bandwidth is not exactly a multiple of the number of cycles
•  There are known unruly IF ranges hitting at given LO tunings, that can affect the overall continuum level via baseline distortion
•  Strong/broad lines need to be properly ignored •  The error applying to this continuum will depend on efficiency of
rebinning on the radiometric noise •  Continuum levels in HEB data are strongly affected by Electrical
Standing Waves, so they must be corrected first •  Some observing modes are better suited for accurate continuum
estimate (DBS, preferably with continuum optimisation) – some others can actually NOT provide continuum info at all, e.g. FSW
•  Beware of continuum in OFFs !
On-line Spectroscopy WS – 23-25 April 2014 - page 5
On-line Spectroscopy WS – 23-25 April 2014 - page 6
Continuum level extraction (2)
Intermediate Frequency (MHz) ESW amplitude (K)
Inte
nsity
(K)
Con
tinuu
m le
vel
(K)
WBS-H WBS-V
Spurious continuum signal and ESW amplitude
Unruly IF ranges - examples
Band 6 resonances
Baseline distortion in band 3b
Continuum level extraction (3) •  Based on this, the following recommendations apply:
•  In HEB bands, ALWAYS correct from ESW first (see dedicated session in this workshop) – inspect the outcome in case of correction hiccups
•  In applicable bands (now 2a, 5a, 5b), undo the sideband ratio correction •  Wherever applies, remove fringes using FitHifiFringe, WITHOUT
baseline subtraction or division of any kind – one has to live with the residual baseline slopes…(they are part of the uncertainty)
•  Avoid ranges of the spectrum affected by either enhanced noise or very distorted baseline
•  In order to circumvent sideband ratio consideration, the continuum in the SSB spectrum at level 2 can be simply divided by 2, and considered to apply at the LO frequency
•  The noise in rebinned data may not decreased radiometrically for very large smoothing widths •  At large bin sizes, IF amplifiers will ingest noise that is expected to limit
the effective radiometric bandwidth •  Presently, we recommend to not smooth data with kernel width larger
than 100 MHz
On-line Spectroscopy WS – 23-25 April 2014 - page 7
Continuum level extraction (4) •  The mkRms task will perform some statistics computation on a given
spectrum, providing mean, median, RMS, etc, per sub-band: •  One of the strength of the task is an automatic line masking (a la FHF) •  It will also apply boxcar smoothing of a given width •  Alternatively, the pipeline will automatically compute and store spectra
statistics in obs > trendAnalysis > Statistics (no line masking though) •  H/V average is then up to the User – imbalance may always persist…
DEMO: Continuum around CH line in band 7a in W51
Before ESW correction Before ESW correction After ESW+FHF correction After ESW+FHF correction After ESW+FHF correction - V
After ESW+FHF correction - H
On-line Spectroscopy WS – 23-25 April 2014 - page 8
Comparison with PACS/SPIRE (1) •  Comparison with PACS and SPIRE data involves the conversion to flux
units •  This conversion can be performed using the task convertK2Jy, or
using analytical formulae •  An assumption on the source size must however be made •  For non point-like sources, analytical treatment exists for pure
Gaussian beams – for a more realistic beam the use of convertK2Jy is needed (note: this is not yet available in 12.0)
•  Further conversion to other unit can be done with the task convertUnits •  Analytical treatment:
S = (TA*×ηl/ηA) × (2kB/Ageom) × (ΩS/ΩΣ)
•  For point-like sources, K = ΩΣ/ΩS = 1 •  For non point-like sources, and a pure Gaussian beam of HPBW θb
•  K = (1-exp(-x2))/x2, where x=√ln2 (θS/θb), for a disk source of diam θS
•  K = 1/(1+x2), where x = (θS/θb) for a Gaussian source of HPBW θS
On-line Spectroscopy WS – 23-25 April 2014 - page 9
On-line Spectroscopy WS – 23-25 April 2014 - page 10
Comparison with PACS/SPIRE (2) •  PACS and SPIRE also have their tricks…
•  The source extend matters greatly for the accurate calibration of PACS or SPIRE data – see corresponding sessions in this workshop – the source morphology assumption must be consistent for all instruments
•  The very different spectral resolution compared to HIFI can imply line blending, which must be taken into account
•  PACS comparison in the red leak region is possible on line but not likely on continuum
•  Line flux extraction in SPIRE spectra is better done with sinc function fit on unapodized data. On top of that, multi-line, multi-species fitting is working better to account for the sinc side-lobe ringing and baselines
IRC+10216: CO-only fit
CO 6-5: 2.5e-15 W/m2
CO 7-6: 3.2e-15 W/m2
IRC+10216: multi-species fit
CO 6-5: 2.6e-15 W/m2
CO 7-6: 3.3e-15 W/m2
Comparison with other radio-tel. •  Comparison with other observatories using antenna temperature
scaling can in principle be done in temperature scale: •  Different dish size however implies a different beam dilution that must
be corrected – remember that Tmb is not Tb ! source morphology assumption kicks in again
•  Transiting to Jy may again be a better option since the antenna gain (Jy per K) will scale with the dish area
On-line Spectroscopy WS – 23-25 April 2014 - page 11