pacs nhsc spire point source spectroscopy webinar 21 march 2012 david shupe, bernhard schulz, kevin...

PACS

NHSC SPIRE Point Source Spectroscopy Webinar21 March 2012

David Shupe, Bernhard Schulz, Kevin Xu

on behalf of the SPIRE ICC

Extracting Photometryfrom SPIRE Maps

PACS

NHSC SPIRE Point Source Photometry Webinar21 March 2012

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SPIRE Point Source Photometry

• SPIRE Calibration and Map Units• Fitting Functions to Point Sources• Considerations for Aperture Photometry

• Source Extraction• Summary: Checklists for Astronomers

• Demos of the HIPE Photometry Tools

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• SPIRE Calibration and Map Units– How Calibration is Defined– Units and Beam Areas

• Fitting Functions to Point Sources• Considerations for Aperture Photometry

• Source Extraction• Summary: Checklists for Astronomers• Demos of the HIPE Photometry Tools

SPIRE calibration is defined by the peak deflection when scanning

• When a detector is scanned directly over a point source, the peak deflection of the signal timeline equals the brightness of the source.

Scan of detector PSWE8 over Neptune,obsid 1342187440

The timeline-based definitionleads to some accounting corrections

• Units are in Janskys per beam• Most software wants Jy/pixel or MJy/sr

• Map-making lowers the peaks…• …relative to the timelines

• Calibration is for point source peaks• Some detectors have bigger areas

• Calibration is for nu*Fnu = constant• Color correction for other spectral shapes

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Use the “fine-scale” beam areasto convert Jy/beam to other units

• The fine-scale beam areas were measured from Neptune maps with 1-arcsec pixels– 250um: 423 sq arcsec– 350um: 751 sq arcsec– 500um: 1587 sq arcsec

• These values may change slightly in the near future (by a few percent)

• The “convertImageUnit” task willchange maps to Jy/pixel or MJy/sr

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Divide peaks measured in mapsby the pixelization correction

• See Sec 5.2.11 of the SPIRE Observer’s Manual

• For nominal pixel sizes, divide by factors of:– 0.951 (250)– 0.931 (350)– 0.902 (500)

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250 350

500

Curves obtained by integrating skybins/pixelsover Gaussian approximations to the average beam

Pixel size in arcseconds

1.0

0.9

0.8

6” 10” 14”

Applying the Relative Gains equalizesthe detector areas (instead of the peaks)

• Gains are provided in the SPIRE cal tree• These gains are applied before

destriping and map-making• More details when we talk about

Aperture Photometry

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Single-detector Neptune maps show the gains reduce the spread in aperture photometry

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Timeline-fitting

Aperture Photometry

Measured Flux (Jy)

Neptune, Operational Day 168, PSW (250 microns)

Aperture radius = 150”Aperture correction = 1.027

Color corrections are described in the SPIRE Observers’ Manual & Data Reduction Guide

• See Sec 5.2.8 • Multiply by the

value appropriate for your source

• For specific cases, compute your own correction from the filter RSRFs

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250

350500

Color Correction Factor vs. AssumedSource Spectral Index (Point Source)

Source Spectral Index (in frequency)

1.0

0.94

0.98

30.90

-2 -1 0 1 2-3

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• SPIRE Calibration and Map Units• Fitting Functions to Point Sources

– Peak-fitting techniques– Estimating uncertainties

• Considerations for Aperture Photometry

• Source Extraction• Summary: Checklists for Astronomers• Demos of the HIPE Photometry Tools

Peak-fitting is recommendedfor point sources

• Fitting Gaussians to timelines is the best method for sources visible on the maps– Jython script: bendoSourceFit_v0.9.py– Java task: timelineSourceFitterTask

• Gaussian-fitting on maps is serviceable as a second choice– Java task: sourceFitting– Gaussian is good approximation for radii up to

(22, 30, 42) arcsec

To estimate the total uncertainty in flux,combine these terms in quadrature

• Uncertainty in the fitted amplitude– Includes the instrument and confusion

noise (minimum of about 5 mJy)

• 7% of flux density for calibration uncertainty– 2% statistical reproducibility– 5% absolute level of Neptune model

(this term does not apply to SPIRE colors)

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• SPIRE Calibration and Map Units• Fitting Functions to Point Sources• Considerations for Aperture Photometry– Applying the relative gains– Aperture corrections

• Source Extraction• Demos of the HIPE Photometry Tools

The relative gains may be applied using a Useful Script, or the SPIA

• SPIRE official pipeline scripts– applyExtendedEmissionGains option

• SPIRE Useful Script: Photometer Baseline Removal and Destriper– Example is at the end (5th one)

• spiaLevel2 task– Relative gains are applied by default

• In the last 2 cases, the original Level 1 timelines are left untouched– The point-source calibration still based on peaks– The best of both worlds: timeline-fitting on

Level 1, and aperture photometry on maps15

Official aperture corrections are now in the SPIRE Data Reduction Guide!

• Available in the online HIPE 8 docshttp://herschel.esac.esa.int/hcss-doc-8.0/load/spire_drg/html/ch05s07.html

• Not in the docs that come with HIPE 8.1• Values in Photometry Recipe:

– 1.2750 (250μm) 22” radius, sky 60”-90”– 1.1933 (350μm) 30” radius, sky 60”-90”– 1.2599 (500μm) 42” radius, sky 60”-90”– Uncertainties at 5% level16

http://herschel.esac.esa.int/hcss-doc-8.0/load/spire_drg/html/ch05s07.html

http://herschel.esac.esa.int/hcss-doc-8.0/load/spire_drg/html/ch05s07.html

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• Source Extraction– Inside HIPE: DAOPhot & Sussextractor– DAOPhot Demo

• Summary: Checklists for Astronomers• Demos of the HIPE Photometry Tools

Two source extractors are availablewithin HIPE

• sourceExtractorDaophot– Algorithms from IDL AstroLib– FIND for detection– APER for photometry (not PSF-fitting!)

• sourceExtractorSussextractor– Sussextractor algorithm

(Savage & Oliver 2007)– Flux density is peak of smoothed image– Good for detecting sources

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The simplest operation of extractorsuses the FWHM of each band

• Averages for nominal pixels:– 250um: 18.2 arcsec– 350um: 24.9 arcsec– 500um: 36.3 arcsec

• You can supply your own PRF image• The fine-scale beam areas are needed

(or the images must be converted)– (423, 751, 1587) sq arcsec

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Corrections are still neededfor extractor outputs

• For sourceExtractorDaophot, need an aperture correction appropriate to radius supplied

• For sourceExtractorSussextractor, the correction seems to be flux-dependent

• A nice combination for sources 20 mJy and brighter, is to use Sussextractor for detection and timeline-fitting for the photometry (see demo)

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Checklist for timeline-fitting photometry

Use the Level 1 timelines without relative gains applied

Perform first-order baseline correctionSupply a starting positionRun the bendoSourceFit or the

timelineSourceFittingTaskApply color correction as needed

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Checklist for fitting on the map

Use the map made without relative gains applied

Run the sourceFitting taskDivide by the pixelization correctionApply color correction as needed

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Checklist for aperture photometry

Make the map with relative gains applied (destriping recommended also)

Convert to Jy/pixel using “convertImageUnit” task

Run the annularSkyAperturePhotometry task

Apply an appropriate aperture correction

Apply color correction as needed24

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Demos of the photometry tools in HIPE

• Fitting Gaussians on the map (Bernhard)

• Timeline-fitting of Gaussians (Bernhard)• Aperture Photometry (Kevin)• Source detection with Sussextractor

combined with timeline-fitting (David)

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pacs nhsc spire point source spectroscopy webinar 21 march 2012 david shupe, bernhard schulz, kevin...

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