NHSC HIFI DP workshop Caltech, 7-9 February 2011

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Pat MorrisPat Morris Steve Lord, Adwin Boogert, Colin Borys (NHSC)

Carolyn McCoey (Univ. of Waterloo)Emmanuel Caux, IRAP (ex-CESR)

Thanks – Frank Helmich, HIFI PI, and the HIFI Consortium

The HIFI InstrumentThe HIFI InstrumentStatus, AOTs, and CalibrationsStatus, AOTs, and Calibrations

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Welcome

NHSC teamNHSC teamScienceAdwin Boogert

Herschel DP Training “Champions” Group

Colin Borys NHSC rep Herschel DP Mgt Group

Steve LordPat Morris

NHSC rep Herschel DP User Group

ApplicationsJoan XieAnnie Hoac

NHSC teamNHSC teamScienceAdwin Boogert

Herschel DP Training “Champions” Group

Colin Borys NHSC rep Herschel DP Mgt Group

Steve LordPat Morris

NHSC rep Herschel DP User Group

ApplicationsJoan XieAnnie Hoac

Carolyn McCoey, U. WaterlooHerschel DP Training “Champions” Group

Emmanuel Caux, IRAPHIFI Co-PIHIFI rep Herschel DP User GroupHIFI Users Group

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Outline

• Part I: Expectations & Goals, Preliminaries, Data Access• Part II: Instrument Status and Health• Part III: Calibrations• Part IV: Cross-Calibrations (HIFI vs APEX, SPIRE)• Part V: AOT Status

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Expectations & Goals

• Learn HIPEBecome familiar with the GUI concepts and usage, how to

execute pipelines and explore your data

• Learn where to find templates data reduction scripts and how to use them... and import and execute custom scripts

• Learn how to read/ingest your data in HIPE• Learn how to process HIFI data to Level 2+ products• Learn about resources and support NHSC can

provide• Processing ➫ science in HIPE with CASSIS (joint

session)• Sessions will use public data for demo and practice

purposes.

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Preliminaries

• Do you have the right version of HIPE installed?• Where are the data?

– Should I have them already?– What if I don’t?– How do I ensure I’m ready to go?

• Where are the scripts?• What are tutorials?

• The next two presentations will answer these questions.

☕ We have allowed for some time to be used for testing your setup (before/during coffee)

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Data access this week

HSA

ESA Mission Ops Center

ESAC, Madrid

HIFI ICCDB

NHSC/HIFI DB

You @ NHCS

HIPE

NHSC/HIFI has reprocessed data in

HIPE 5.1, and provided in local stores

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Data access at t > this week

HSA

ESA Mission Ops Center

ESAC, Madrid

You @ home

HIPE

The HSA is the only repository of observations and calibrations that can be accessed by the observing community.

Help from NHSC and HSC always available.

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Part IIInstrument health and status

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HIFI Single Event Upsets

• An SEU in August 2009 attributed to CR on a sensitive memory chip in the LO control unit caused premature power-off of the LOU, killing HIFI’s Prime side (DC/DC converter failure)

• HIFI runs on its REDUNDANT side since February 2010, with new intensive fault protection S/W.

• SEU occurring statistically every 12 days

• Recovery now well established and rapid.

• One full power cycle (last resort) has been required, when HIFI stopped reacting to commands.

• ~2 ODs lost to LCU SEUs

• 5 ODs lost to ICU SEUs but PACS rescheduled so no observatory time lost.

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LSU OXCO Anomaly

• HIFI’s 10 MHz signal (for locking LO chains, LSU, WBS and HRS) is generated by a crystal.

• Crystal is heated to 100º C for best performances– The heater circuit is not working well. Temperatures began

spiking in June 2010, investigation concluded that the circuit is reacting to LSU temperature control switching to an on/off mode.

• The LSU and HIFI are operating within design specifications, and the crystal temperature is within the nominal tolerances so science observations are not affected.

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LSU OXCO scenarios

We cannot change anything in software or by commanding. We have to wait and see what happens, three scenarios are possible :

• Situation remains stable– Currently science data are not affected– Keep operating HIFI as is

• Heater circuit dies, but crystal keeps working– Drift of HIFI frequency expected that needs to be

characterized, especially at the “jump” (may then stabilize)– Dedicated characterization + observing known lines every OD

• Heater circuit dies, takes crystal with it End of HIFI

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WBS-V comb fade

• WBS-V comb has a failed component, already discovered in 2007– The WBS-V could not be removed and repaired.

• Comb power continued to drop– Steep decay between OD 320 and OD 420, lighter since– No remaining attenuation in subband 4 (2-3 dB in others)

• Comb line intensity dropped to < 40 counts, much lower than specs.

Possible reduction of accuracy in determining comb line positions, reduced frequency calibration accuracy expected

S/N still > 400 in sub-band 4

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HRS-WBS cross calibration

• Measure pair of spectra with WBS and HRS at any input (preferentially from internal 100 K hot load)

• Compute mutual correlation as function of relative shift

• HRS can be positioned to cover almost the full WBS scale

• Some On-Board S/W bugs to use this being worked out.

• Accuracy of about 100kHz (best case 30kHz)

• No issues with WBS-H so far.

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Reality Check

• The HIFI team has been working through so-called Failure Mode Effects and Critical Analysis (FMECA) since assembly and test phases.– A lot of things are related to problems anticipated at launch– Secondary are all the power supplies, which are supposed to be

robust, however, not guaranteed

• Tens of items exist that say “switch to redundant” – that option was required already during PV, thus is no longer available and thus we operate with numerous possible single point failures

• The FMECA is on functional level Hundreds of components can cause a functional problem.

Chance that HIFI survives the remaining mission is not close to 100% anymore

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Part IIICalibrations

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LO Spurs and Spurious Response

• Impurity features in HIFI are manifest as ~25MHz, Gaussian-shaped features in hot, cold, on, and off data.

• Both WBS and HRS are affected.– Because they look a lot like astronomical lines, they can

fool users.

• The repeatable ones are tabulated in PHS (HSpot) and pipeline tables.– In the pipeline, the hot/cold loads are searched in all science

observations, and spurs are flagged.

Hot and Cold Loads from an observation in band 1a

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Spur clean-up at instrument level

Many of the most troublesome impurities (e.g. near key lines) have been cleaned up, by (time/labor intensive) tests and changes to multiplier settings and bias voltages.

Band 1a spur eliminated (557 GHz H2O line region)

System temperature increased at upper 1.5 GHz of band

Sensitivity in band 1a is better than that in band 1b for LO frequencies up to 551.9 GHz.

V

H

V

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Band 5b purification

• LO-band 5B had several LO spikes at the same time– Result is that the IF consists of several frequency bands

superposed on each other. Calibration of all frequencies within the IF was unknown

– Purification efforts took many weeks.– AORs in 5b were released in December 2010.

• Band 5B was not alone in impurities but in the diplexer bands the diplexer can moved and the signal evaluated at each setting to give purest signal more efficiently (in observing terms).– Purification in bands 3b/7b done this way (Band 5 has no

diplexing).

• Purification is a major triumph for modeling of the LO chains!

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Sensitivities

• Sensitivities are driven mainly by System Temperatures and Aperture (or beam) Efficiencies.

• Tsys remains essentially as measured just before launch --- some small changes at specific frequencies to mitigate impurities and unstable tunings.

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Beam Calibrations

• H/V beam sizes and co-alignment

• Measured mainly from Saturn, Uranus, Mars

• Beam offsets are taken into account in the HIFI pipeline since 5.0

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Efficiencies

• Beam efficiencies measured on Mars

+ Overall ~10% better than pre-launch estimates

o Data taken before Nov 2010 should have somewhat better noise performance (HSpot 5.2 uses updated effciencies).

– Band 5a/b are an exception, ~10% lower.

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Error Budget

Error source B1/B2 B3/B4 B5 B6/B7

Sideband ratio <10% <30% <10% <30%

Hot Load Coupling <1% < 1% < 1% < 1%

Cold Load Coupling <1% < 1% < 1% < 1%

Hot Load Temperature < 1% < 1% < 1% < 1%

Cold Load Temperature < 1% < 1% < 1% < 1%

Beam efficiency 5-10% 5-10% 5-10% 5-10%

Pointing (APE+co-alignement) < 5% < 5% < 5% < 5%

Standing Wave 2-4% ? ? ?

Total (quadratic sum) <16 % <32 % <15% <32%

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Part IVCross Calibrations

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HIFI / Ground

• Comparison made of HIFISTARS spectra with APEX spectra (CHAMP+ SRON/NOVA mixers in MPIfR instrument)

• Scaling consistent with different beam sizes

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HIFI - SPIRE

From HIFISTARS program

Good agreement in continuum at low frequencies

CO 10-9 in CRL618

Continuum less reliable for HIFI at higher frequencies (drift)

Observations not optimized for continuum measurements

HIFI-VHIFI-H

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Part VAOT Status

(Not an Intro to the AOTs)

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HIFI AOTs in OT1(mid-November 2010)

Relative distribution of SScan and Map times is ~reversed from GT/OK KPs.

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Band requests in accepted OT1 programs

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General Status

• All HIFI Observing Modes released and being scheduled.Certain restrictions and recommendations remain in place:– FSwitch with Spectral Scans is forbidden in Bands 6 and 7.

• LO power is difficult to stabilize between ON and OFF (throw). • If FastDBS can’t be used, LChop is the alternative.

– FSwitch with OTF maps is forbidden in Bands 6 and 7, except over a range of frequencies around 1897 GHz (C+ tuning).

– Fast(chop)DBS is recommended over DBS in Bands 6 and 7.

– All FSwitch and LChop with all modes should be taken with sky reference, esp in the diplexer Bands 3,4,6,7.

• Data which were taken inconsistent with these recommendations (mainly AOT tests and some early PSP/SDP data) to be dealt with in IA.

Not quite… see next

slide!

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Some systematic issuesSpectral Scans

WBS-V leveling/saturations

• Certain LO tunings in Spectral Scans lead to strong IF instabilities, as a result of saturating the WBS-V on the hot load.

• First noticed over ~1061 – 1090 GHz; investigation reveals other isolated ranges over most all bands. 4a and 6a most affected (SScans there on hold), 3a/b least affected.

• Several problems lead to this behavior … e.g. initial power levels deduced from the cold loads.

…will be corrected by increasing the WBS attenuator tuning grid and update to power level tables where not sufficiently covered AOT validation (remember HIFI went on a “fast-track” release after loss of Prime side). Testing in progress.

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Some Systematic IssuesSpectral Maps

• OTF mapping modes were the last ones to release, could not receive detailed attention during HIFI’s “time-out”.

• Several changes were necessary:– Sky sampling definitions (Nyquist

vs “half-beam”)• Density: Maps taken < OD 280 uses

Nyquist = HPWB/2. (half-beam), > 280 Nyquist ~ /2D.

• DBS Raster affected also.

– Compensation for a “zig-zag” effect

• Slight timing mis-correlations due to command timing in the uplink system, scan speed granularity. Overall not major problems but could affect what the user expected vs sees in the data. OTF only.

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More details on Observing Mode performances…

• Are in the HIFI AOT Release Notes at HSC:http://herschel.esac.esa.int/AOTsReleaseStatus.shtml

– Update to the AOT Release Notes for OTF modes is pending (next week!)

• The site also contains informational notes about– Beam efficiency calibrations, and effects in HSpot and the pipeline.– H/V beam pointing in the pipeline.

• More info on the data by mode will be covered by Carolyn (Level 1 and 2 pipeline overview), and in the mode-specific presentations and demos.

• Further resources (pages, online and video tutorials, science tools) will be explained during the workshop, and summarized at the end to take all inputs into account.

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Questions?