Spectrometer Wavelength Calibration XHSPOT Proposal: PVSpecWave H. Feuchtgruber

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Spectrometer Wavelength CalibrationXHSPOT
Proposal PVSpecWave H. Feuchtgruber
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Description of the Calibration Problem
47 x 47

• Blue array 400 pixels
• Red array 400 pixels
• 2 different blue filters
• 3 grating orders
• - Grating range
• 32000-1064000 positions
• Spectral resolution elements
• 3650 (x sampling x time)

2x
1st order
2nd order
3rd order
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PCD Requirements

• PCD sec. 4.2.1
• Required accuracy Peak position to within
  10-20 of a spectral resolution element

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XHSPOT Proposal PVSpecWave (1)
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XHSPOT Proposal PVSpecWave (2)
. more to be filled in according to actual
target visibilities !
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Wavelength Calibration Targets (1)

• Suitable target list containing strong molecular
  lines
• - PICC-ME-TN-013, Use of late type stars for
  PACS wavelength calibration, (D. Lutz)
• Photometric and Spectroscopic Calibration of
  Herschel Instruments with Planets and
  Satellites, (Th. Encrenaz, R. Moreno, A.
  Coustenis)
• Uranus(H2O), Neptune(H2O, CO), Saturn(H2O, NH3,
  PH3)
• Jupiter (H2O, NH3, PH3 fills entire 5x5 field
  of view !)
• Justtanont et al., AA, 360, 1117-1125 (2000),
  ISO-LWS observations of rotational CO lines from
  C-rich objects

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Wavelength Calibration Targets (2)

• Suitable target list containing strong atomic
  fine-structure lines
• 19 selected Planetary Nebulae
• IC418, IC2501, NGC5315, He2-131, NGC6210,
  NGC6543, NGC 6572,
• SwSt1, BD 30 3639, NGC6826, IC4997, NGC7027,
  NGC7662, NGC40,
• NGC3242, NGC3918, NGC5882, NGC6302, NGC6905
• - Atomic fine-structure lines within the PACS
  wavelength range
• OIII51.8145µm NIII57.317µm OI63.184µm
  OIII88.356µm
• NII121.898µm OI145.525µm
  CII157.741µm NII205.178µm
• - References
• 1) ISO 95-015, Planetary nebulae to be used as
  ISO-SWS Astronomical Calibration Sources, H.W.W.
  Spoon, K.A. van der Hucht, D. Lutz
• 2) An Infrared Spectral Line List of
  Astrophysical Interest (2.4-200µm) and its use in
  the SWS and LWS ISO Central Program
• 3) www.mpe.mpg.de/ir/ISO/linelists/FSlines.html
• 4) Liu et al., MNRAS, 323, 343, (2001), ISO LWS
  observations of planetary nebula fine-structure
  lines provides also observed line fluxes

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PVSpecWave The spatial situation
Diameter of Jupiter Mid-Jun-09 as seen from L2
43.9
White crosses indicate location of all PACS
spectrometer spatial pixels
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PVSpecWave Spatial Information about Targets

• Fluxes of moons and faint ring are being
  neglected
• Roll-angle will be important for assigning
  rotational velocity shifts
• separately for each spatial pixel (max. ??
  11km/s)
• Check that no other bright targets come close to
  Jupiter at actual
• observation date/time.
• Require Herschel velocity towards target and
  doppler shifts

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Status of Analysis and Uplink Preparation

• For the overall calibration strategy and
  formalism see presentation at the Herschel
  Calibration Workshop2
• Uplink (1st version) is defined in X-HSPOT
  proposal PVSpecWave
• No relevant SOVT data available for analysis

• Analysis code (or CAP) is unchanged from FM ILT
• - Operating system MS WinXP
• - Use HIPE to generate L0 products
• - Use IDL code to derive new
• calibration parameters
• - Output ASCII files of polynomial
• coefficients for inclusion into pipeline
• Updated input model spectra for
• all giant planets are available now covering the
  entire PACS wavelength range and convolved to the
  PACS spectral resolution, inclusion of HD
• lines in progress

Semi-Automatic calibration procedure
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Calculated fluxes for 1 spatial pixel
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Calibration Targets for Molecular Lines
Start PV
Start Routine Ops
Target visibilities (HSPOT)
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Calibration on bright PNs
Start Routine Ops
Start PV
Target visibilities (HSPOT)
Monitoring for roll angle/time dependencies etc.
selected out of Ref. (1)