Annual Instrument UpdatesThe Support Astronomers W. M. Keck Observatory 2010 February 24photo B. Schaefer

ESIGreg Wirth

ESI Current StatusGood newsESI working well overallMechanical stages AOKMAGIQ software now on ESIBad newsMotor controller software can no longer be compiled from source

ESI Usage

ESI Integral Field Unit (IFU)Delivered and tested in 1994target acquisition problematicCommissioning completed 2010-Jan-17target acquisition solvedNow released for useDocumentation underway

DEIMOSGreg Wirth

DEIMOS Current StatusDEIMOS continues to perform well overall; no major problemsSignal dropouts on CCD1 became a problemTraced faults to bad cable; now fixedConcerns:Grating tilt stages show occasional unrepeatability; possible mechanical problem with encoder mountSlitmask system generates metal dust in focal plane requiring regular cleanup; no easy fix

DEIMOS Mask in Focal Plane

DEIMOS Slitmask Debris

DEIMOS Future PrioritiesReplace rotator control hostConcern about obsolescence of Linux boxUpgrade instrument control hostNew hardwareRebuild software for greater maintainabilityRevamp DEIMOS web pages

DEIMOS/LRIS Slitmask Milling

Slitmask Mill

DEIMOS/LRIS Slitmask MillingSlit quality remains unevenSummit staff are improving operation:Using new tool for more accurate depth calibrationDoubling tabletop thickness for better stability and flatnessIncreasing vacuum for better suctionImplementing regular mill PM program

NIRSPECJim Lyke

NIRSPECExtended AO capabilityReplaced Br- filter with AO pupil stopAccess to KL, M-wide filters behind AOSCAM reading all 4 quadrantsSince September 2009 serviceServer CrashesOne crash every four nights20 min average per crash

NIRSPEC ServiceUCLA fabricated pupil I. McLean, G. Brims, J. Canfield, T. AliadoAccess port allowed in situ swapSmooth serviceServicing teamG. Hill, M. Wagner, A. Agliam, J. Lyke (I. McLean by phone)

NIRSPEC AOAO pupils are alignedEasily switch between the two filter wheelsSoftwareNew scriptsEFS updated (no change for observers)XNIRSPEC needs updatingTest data look goodMars methane measurements coming in early April.

NIRSPEC SCAMWires found pressed against radiation shieldConsultation with PI, Ian McLeanCarefully relocated wiresFour good quadrants since September

NIRSPEC Server CrashesCausesFiber degradationOTDR inspection shows marginal performanceCleaning generally helpsConnectors sensitive to alignmentXNIRSPEC blocks serverServer unresponsiveExiting XNIRSPEC cures crash

NIRSPEC Server CrashesMitigationFiber degradationOptimizing fiber assignmentMore frequent cleaningImprove tech trainingXNIRSPEC blocks serverUpdate recover script

OSIRISJim Lyke

OSIRISFourth service successfulTemperatures nominalDetector temps stableGood image qualityPrevious three servicesReplaced cold headFixed image motion with scale changeCalibration updatesWavelength calibration as function of temperatureRectification matrix improvements

OSIRIS TempsCurrentLast Year

OSIRIS Near FutureMove to K1 planned for late 2010BDRP v2.3 comingFewer RecMat spikesWavelength solution as function of TNew AO dichroicLots of work by Shelley Wright and James Larkin

OSIRIS Upgrades?Grating~30% efficientPossible to double this in J-bandDetector/Electronics

AO bench temps 57 K above telescope

Read-noiseDark currentOSIRIS10 e0.056 e/sMOSFIRE4 eunmeasured

OSIRIS UpgradesSimulations based upon D. Laws IFsim_v2 codeEmission line sourceHa flux = 1016 erg/cm2/sz = 2.3, FWHM = 80 km/s2.16 mm

NIRC2Al Conrad

Time Lost to Faults(A good year for NIRC2) ~1 hour time lost in 74.5 nights Pointing Origin (April; 22 min.) Server Problem (May; 18 min.) Frozen GUI (July; 15 min.) < 0.2% of total time

Pump Repair February 2009: The CCR system went off-line for approx. 2 hours due to a glycol system failure.This triggered the NIRC2 auto-pump mechanism:But the pump did not spin up.The system protected itself perfectly (i.e., the pump-to-dewar valve solenoid was never energized).view from below

Pump Repair The pump was repaired and re-installed during spring 2009Pump system was tested end-to-end (5 x 10-8 millibars).The NIRC2 PI (Keith) was included during all critical steps.Annual testing of the system has been added to the PM schedule.

Monitoring NIRC2 ThroughputTTTNew AO DichroicPPPP P are photometric standards. T are LGSAO Tycho stars. Post-dichroic improvement is ~15% at Kp.

Service Mission Three critical components are required: An L-Filter: In hand. A Y-Filter: Being fabricated at Barr. Cost shared 50/50 between AO ops and external support (M. Liu). The Wollaston Prism: Procurement negotiations are ongoing between UC and the vendor.We will schedule a time to install these components once we know more about the expected arrival of the prism.We must factor into this decision Galactic Center season, plans for the OSIRIS move to Keck 1, and the MOSFIRE commissioning schedule.We are also consulting with the AOWG regarding the potential impact of the delay.

LGSAO Differential TrackingLong exposures of Solar System objects, until recently, were only possible with AO when observing on-axis (R < 15 for NGS; R < 18 for LGS)Following the recent commissioning of LGS differential tracking, faint solar system objects passing near suitably bright guide stars (R < 18) can now be searched for companions (Grundy/Roe, Dec. 2009)

When bright moons or passing stars are available, this mode can be used in regimes with high scattered light (e.g., near Jupiter or Mars)

LGSAO Differential Tracking ExampleTwo images of the Kuiper Belt triple system 1999 TC36. The ~2 day orbital motion of the two, barely resolved inner components can be seen in these images separated by 3-1/2 hours. The faint outer component has a 50 day period. These observations confirmed the orbital solution of the inner pair.

HIRESScott Dahm

Current HIRES DemandHIRES use statistics: 2009155 nights (135 HIRESr / 20 HIRESb)102 nights (66%) exoplanet searches 2010 (Jan.Jul.)82 nights (74 HIRESr / 8 HIRESb)68 nights (83%) exoplanet searchesKepler/CoRoT Followup2009: 24 nights2010 (Jan.- Jul): 22 nights

HIRES Update FTS scans of HIRES iodine cell completed at PNNL and NIST in March 2009. Utility board problem reported to the SSC likely resolved no recurrence since March 2009 Shutter replaced in September 2009 after indications of failure Replacement shutter failed on second day of use 3 spare shutters remaining Guider electronics box replaced in December 2009 2 spares remaining MAGIQ camera upgrade Bias jumps: correlated with CCD electronics heat exchanger fan.

HIRES Future PlansImproved exoplanet slit guiding algorithm being developed by Keck software group.Development of HIRES fiber scrambler for PSF stabilityProposed by Marcy, Fischer & collaborators Two design conceptsOptical breadboard located underneath the echelleRod lens assembly near the decker plateMAGIQ camera upgradeRecent donation receivedPossibly slated for installation during FY11.

LRISMarc Kassis

LRIS-MAGIQ Offset Guider CommissionedOffset Guider FOV modest increase from 1.36x1.0 to 2.93x2.93Fixed optical systemPhotometric filters (BVRI)Old movable guider will be removed in 2010A.Image quality element testingFocus calibrations completeTip-Tilt calibrations ongoingMIRA vs. IQM with observer permissionOffset guider image of M99: BVR, 20sMovable guider FOV

Red Upgrade completedUpgraded LRIS Red in June 2009Wrote data reduction routines Modified focusing software Modified and improved slitmask alignment software.Updated script libraryImplemented electronics temperature regulationCharacterized performanceRevised most LRIS web documentation Immediately released for observer use

Upgrade was nearly seamless to observers

Minor ProblemsBlue side data slightly noisier following repair of a video boardCapacitors replaced by Bob LeachPursuing solutions as time permitsRed side noise resulting from temperature changes in external controller electronicsUCSC isolated noise to a clock driver board Acquired new boardsTemperature regulating hardware will be removed

LRIS Red CCDsData smearing

Limped through September & October runs

Determine problem was internal to dewar

LRIS Red CCDsShipped to UCSC for repair

Recovered 1-12 Left with reduced performance

Full FOV possible with 1 amp (left) readouts

Sept 2009LRLR Nov 2009

LRIS Red CCDs

1-12 L went bad

Science limited to CCD 1-13 Dec 2009 Sept 2009LRLR

LRIS Red CCDs Dec 2009

1-13 L went bad

Correlated faults with power cycling

Temperature excursions below -150 degrees C may be the cause Sept 2009 Jan 2010LRLR

LRIS Red RepairsImplemented continuous power mode for LRISNew software keeps CCD temperature at or above -150 CRewrote LRIS/telescope installation procedures Added automatic power transfer switch & breakout box

Software modifications to handle one amp readoutsDS9XPOSE XFOCUS

Observers receiving updates viaNine news updatesE-mails sent to observers with upcoming runsObservatory Newsletter article

LRIS Red CCDs StabilizedTwo Amp ModeLong slit modePerformance of 1-13 R unchanged since commissioningOne Amp R Mode

Minor Planned UpgradesNew Slitmask frames tested 22 JanAstrometry analysis completed 18 FebRelease for use in MarchLRIS Calibration LampsWill follow removal of old movable guiderDEIMOS-style slitmask alignmentMore efficient alignmentsDifferential flexure data acquired 22 Jan

NIRCMarc Kassis

NIRCNIRCs Last Ride2010 Jan 30P.I. SoiferMatthews observingCooling fan died (lost 1 science night)Warmed to ambient tempsBackfilled with dry nitrogenWill not be scheduled in 2010B

InterferometerSam Ragland

Presentation sequenceIntroductionScience highlightsWhat is new?KI performance summaryASTRA status update

1. IntroductionKeck Interferometer provides milli-arcsecond angular resolution through fringe contrast measurements12 observing runs in 2009 19 science nightsNASA key science program completed in Jan/09Demonstrated good reliability of the instrument (~ 90% uptime); lost ~ to bad weatherNSF-funded ASTRA project in process of delivering new capabilitiesK1 inK2 inLong delay linesFast delay linesSwitchyardBeam combiners

7 refereed publications since start of 2009Spatially resolved spectroscopic observations of 15 young stars in the K-band (Eisner et al. 2009)Detect hot hydrogen gas through Br g emission lineObservations suggest the presence of water vapor and CO gas in the inner disk of several objectsInterferometric evidence for resolved warm dust in the DQ Tau system (Boden et al. 2009)Suggests the IR excess from this PMS binary system is distributed on the physical scale of the binary orbit (0.1-0.2 AU)First L-band observations of a YSO disk (Ragland et al. 2009)Studied the temperature structures of the inner disks a Herbig AeBe star though simultaneous K & L measurementsPress release in Dec 2009: http://www.keckobskeck_telescopes_take_deeper_look_at_planetary_nurseries; http://www.nasa.gov/topics/universe/features/keck-life-zone.html2. Science Highlights (slide 1 of 2)

2. Science Highlights (slide 2 of 2)51 Oph: A possible Beta Pictoris analog measured with the Keck Interferometer Nuller (Stark et al. 2009)A two component model: inner disk of blackbody grains and outer disk of small grains was essential to explain the observed KI measurements in conjunction with VLTI-MIDI & Spitzer observationsExploring the inner region of type 1 AGNs with the KI (Kishimoto et al. 2009)Four Type I AGNs thanks to the recent angle tracking improvement; these observations partially resolved the dust sublimation regionPress release in Dec 2009: http://keckobservatorkeck_observatorys_interferometer_takes_closer_look_at_supermassive_black_ho/Transitional Disks with KI (Pott et al. 2010)Rule out binary companions within specific parameter range

3. What is new? (Slide 1 of 3)Completed operational transition of the ASTRA Self-phase referencing (SPR) mode and offered as a fully operational science instrument for semester 2010BSpectral resolution of ~ 1700 in K-band for K < 7Science beam

3. What is new? (Slide 2 of 3)Offering ASTRA Dual-field Phase Referencing (DFPR) mode for shared-risk science in 2010B Measurements up to K ~ 12 when suitable nearby reference star is availablePrimary FTSecondary FTFBFFFB Fast Servo Closed loop feed-back Open loop feed-forward Slow Servo Limited feed-back Long integration times Fainter magnitude limitsFieldSeparatorsBrightreference beamFaint science beamTip/tiltMetrologyPrimary FDLSecondary FDLNew sub-systems

3. What is new? (Slide 3 of 3)Validated V2 observations in ASTRA-DSM configuration Easy reconfiguration between modesEnables split observing with ASTRA and standard V2 instruments on the same nightUpgraded to a SMC-based sequencers for easy maintenancePerformed a performance validation test for H-band visibility modeValidated science with newly implemented AO/IF dichroicWorked on L-band instrument to improve operational efficiency

4. KI performance summary V2 Science modesK5/H4 sensitivities: K < 10.3; H < 9K42 sensitivity: K < 7.6K330 (R ~ 1700) sensitivity: K < 7L-band sensitivity: L < 6K/L split pupil mode: K < 8.7 & L < 4.8DFPR mode: K < 12.3 for when bright reference star (K < 8) within 5-15; K < 11.3 for 15-25 fieldNuller Science modeN-band flux > 1.7 JyAdaptive optics and Angle tracking limitsAO sensitivity: R < 12KAT sensitivity: J/H < 10.5 ( H < 9 for SPR & H < 13 for DFPR)

KI is the most sensitive IR interferometer by over 2 (operational modes) to 4 (shared-risk modes) magnitudes

*5. ASTRA status update - J. WoillezAstrometry Known exoplanets and galactic center Astrometry review on Oct 29, 2009 Currently developing the astrometry subsystems: astrometric metrology + transverse internal baseline monitor First astrometric tests starting in July 2010 Qualification campaign through 10BDual field phase referencingImproving the limiting magnitude of the interferometer to K>14 First fringes on a bright target pair obtained on Dec 29. In process of completing the DFPR subsystems (dual field subsystem after AO & tip/tilt metrology) 1.5 engineering nights to complete commissioning (March & April) with July night as backup

AO OperationsRandy Campbell

*Recent ChangesOperating Model1 spotter mode with Night Attendant G10-T safety standards committee met at Keck No laser coordinatorOAs fully trained on LGSAO operationsPrimary SA reduced hoursNo need for additional secondary SALaser/satellite keep out cone reduced from 0.5 to 0.1 (Keck II only)

*LGSAO MetricsHours

*LGSAO Lost Time MetricsHours

*Things Were Working On Frequent Faults:Laser PointingSupervisory Control, SC, offloadingEfficiencyMauna Kea Laser Operations Group, MLOGNSF and DoD representatives to visit Keck and Gemini to review impact of LCH.Blanket closures, ToO coordination.Future aircraft safety solutionsK1LGS support

Keck Observatory ArchiveHien Tran

KOA StatusExtracted spectra for single-chip legacy data released August 2009NIRSPEC data release agreement signedAll NIRSPEC PIs notifiedSimple User Interface released Access data for a given night or targetSpecial protection of HIRES data taken in support of Kepler2302 nights of HIRES data (236,154 files) ingested63% of the data are publicly releasedOver 140,000 queries (~4 TB downloads) since public opening July 2006Three refereed papers

KOA Future PlansNIRSPEC data released spring 2010Directors review March/April 2010Extracted spectra for NIRSPEC dataVisualization tool for extracted spectraPI-specific user interface; interface for selecting officials (SOs)

Mainland ObservingGreg Wirth

Mainland Observing Sites:Old

Mainland Observing Sites:New

Mainland Observing Sites:Future

Mainland Observing Sites:Mainland-only Mode

Mainland Observing Sites:External Use Allowed

Instrument PM* ProjectGrant Hill

* Preventive Maintenance* Predictive Maintenance* Performance Monitoring

Instrument PM ProjectSince last report:Project provided good earned value to the observatory in FY09 and is continuing through FY10.To date:Database of PMs created and ingesting task information.Scheduling software automatically generating work orders.Wide variety of PMs being developed, documented and performedSeveral Web-based interface GUIs written and in regular use.Many problems found and most addressed.Effort to script some tasks of particular interest to observers is now underway.

Instrument ThroughputThe Support Astronomer Group

General NotesUse existing data or procedures when possible.Minimize impact to science observing.In all case, we need to identify photometric nights. (SkyProbe)LGS-AO: leverage use of laser alignment stars (OSIRIS, NIRC2, NIRSPAO)

Throughput Monitoring Summary

DEIMOS Throughput GUISuggests a starSingle button data-takingSingle button analysis

Next StepsFinish commissioning DEIMOS throughput acquisition tool.Implement tool on LRIS.NIRC2, OSIRIS, HIRES:Write data-taking scriptsWrite data-analysis scriptsDetermine magnitudes of LGS-AO checkout starsNIRSPECWrite and test KOA queries.Write analysis softwareAll: integrate into IPM

Mask repair occurred on Jan 20-21 2009Compares to one to two crashes each night at its worst in the past.

The AO system could lock on some features on Mars, like Syrtis Major, shortly before the Mars methane observations, but it could not lock onto anything on the face of Mars with known high methane concentration.OTDR = optical time delay reflectometerNote the different temperature scales on the two plots: 67.570.5 on the left, 6976 on the right.End of October run LRIS shipped to UCSC for Repair and Inspection of internal components.1-12 R , non linear, 12 e- noise.1-12 L linear to 50K , gain 1.2 instead of 1.0, RN went from 4.5 to 6.5 e-. Still useful.

1-12 R , non linear, 12 e- noise.1-12L linear to 50K , gain 1.2 instead of 1.0, RN went from 3.5 to 5 DN. Still useful.

1-12 R , non linear, 12 e- noise.1-12L linear to 50K , gain 1.2 instead of 1.0, RN went from 3.5 to 5 DN. Still useful.

1-12 R , non linear, 12 e- noise.1-12L linear to 50K , gain 1.2 instead of 1.0, RN went from 3.5 to 5 DN. Still useful.

**Implementing a more lean operationWe went from 2 spotters on-station to 1, which reduces the number of people from 5 to 2 per night, and were using NAs to accomplish Hosted meeting at Keck Communicated observatory issues directly to committee, Credit to Paul Stomski, on committeeSafety officer Steve Shimko, Bob Goodrich, Management and administration support

No longer using a laser operator at night, just doing spot checking of the laser system.

The OAs are excellent LGSAO operators and thus the SAs are able to reduce their role during night operations and we no longer have a the second SA on hand, as one SA can do both the instrument and the AO system.In Jan of this year, USStratCom, formerly USSpace Command reduced our keep out cone to 0.1 degrees following a series of documents, reports, and tests of our avoidance system.Resulted in a significant closure reductions:Now averaging less than two closures per target per night of 20 sec duration.However, blanket closures continue to be significant, 10 blanket closure events totaling about 7 hr, 22 min

*Categorized time accounting of AO metrics, hours over the past 5 years of of LGSAO operations.

FY 2009 is the nearest row, science time is the second column from the left. We continue to improveAlthough the faults and overheads stayed about the same. The weather was better and of course we take full credit for that.

We had hoped to improve the efficiency and we have two changes upcoming that should improve acquisition and dithering, that we think we can shave close to an hour off of some NIRC2 nights that have several targets and many dithers.

Regarding the faults

*Laser faults worse this past year. 5 fault events out of the 114 nights. Launch system, water cooling leak, Yag 6 flash lamp (cant run with out Y1 or 6)

Theres the space command already discussed, LTCS about the same

A slight improvement in AO faults, maturation of the NGWFC, but still to much time lost. The laser steering is part of AO Fault another source were targeting is the supervisor control, loops not closing, and loss of TT star during dithers.* those two faults are our current focus of effort, the laser pointing issues seem to be nearly solved, found rigidity problems with L3/L4.

As mentioned, two changes upcoming to make acquisition and dithering more efficient

The MLOG is a group tasked by the MK directors to coordinate efforts on laser issues and pick up where the MKLWG left off. The first meeting to be held March 10.

Dr. Steve Kramer on behalf of the NSF From theScience and Technology Policy Institute Institute for Defense Analyses

Is visiting Gemini and Keck in the next week to understand the LCH impact on science. Well spend two days with him, one at HQ and one on the summit.

Working toward no spotter with either the ASCAM and/or passive radar, Paul Stomski attending G-10 T meetings to help set aircraft avoidance policies.

And of course were supporting K1LGS development and preparing to transition to science operations

*Selecting Officials are those people at each institution (university, NASA, NOAO, etc.) who have the authority to grant proprietary period extensions. We look for existing procedures or data in order to minimize the extra on-sky overhead.CFHTs SkyProbe is a good source of photometric-quality nights, but not for all.DEiMOS and LRIS will use a standard grating. The large number of gratings available for LRIS will limit the number of LRIS nights during which data can be collected.There is a GUI being developed for DEIMOS and LRIS. This will greatly simplify data-taking, for observers, OAs, and SAs.