DetectorandReadout•  Micro-XTESsareMo/Aubilayerswithtransi<on

temperaturesof120mK•  Absorbersarecomposedofa0.5µmthicklayerof

Auanda3.1µmlayerofBi•  Thedetectorshaveadesignresolu<onof3eVat1

keVandhavedemonstrated4.5eVresolu<ononanon-mul<plexinglabsystemat6keV

•  DetectorreadoutisachievedwithaNISTdesigned,rocketflightqualified,varia<onona<medivisionmul<plexingcircuit

AcknowledgementsThisworkwassupportedbyaNASASpaceTechnologyResearchFellowship.TheMicro-XprojectisconductedunderNASAgrantNNX10AE25G.

DetectorCalibra<onoftheMicro-XSoundingRocketX-rayTelescope1,2D.C.Goldfinger,3,4J.S.Adams,3R.Baker,3S.R.Bandler,2N.Bas<don,2M.E.Danowski,5W.B.Doriese,3M.E.Eckart,2E.Figueroa-Feliciano,1S.N.T.Heine,5G.C.Hilton,2A.J.F.Hubbard,3R.L.Kelley,3C.A.Kilbourne,2R.Manzagol,6D.McCammon,3T.Okajima,3F.S.Porter,5C.D.Reintsema,3P.Serlemitsos,3,4S.J.Smith,1,7P.Wikus1MassachusebsIns<tuteofTechnology,2NorthwesternUniversity,3NASAGoddardSpaceFlightCenter,4UniversityofMaryland,5Na<onalIns<tuteofStandardsandTechnology,6UniversityofWisconsin,7nowatBrukerBioSpinAG

Micro-XIntroduc<onThisisasoundingrocketborneimagingspectrometerthatusesanarrayofTransi<onEdgeSensors(TES)toperformmicrocalorimetryonincomingX-rays.ThetemperaturecontrolisachievedwithanAdiaba<cDemagne<za<onRefrigerator.ItsfirstflightisplannedtotargetthePuppisAsupernovaremnanttomeasureelementalabundancesandtocompareplasmadiagnos<csfromresolvedemissionlines.

•  Apogeeof299km•  Observa<on<meof

300sec•  128pixelarray•  Effec<veareaof

300cm2•  Woltertypeop<c

•  2.6arcminPSF•  11.8arcminFieldof

View•  Basetemperatureof75

mK

UpdatesonStatus•  Cryostatmovedtonew,fullyopera<onalMicro-X

labatNorthwesternUniversity•  PassedtheNASAdesignreview;currentdesignis

approvedforflight•  Beginningthefinalassemblyofthecryostatwith

filtersinlaunchconfigura<on

Micro-Xdetectorplane

DetectorArray

MUXChipControlThermometers

Noisespectrumwithoutan<-aliasfiltering.Thisdataisinastatemoresimilartotheenergyspectrabelow

EnergyResolu<on•  Directmeasurementsoftheenergyresolu<on

weremadewithourflightcalibra<onsource.•  Thebestmeasuredresolu<onwiththeflight

systemis9.88eVwhichinferiortotheNEP.•  Shijsinthebaselinethataretoosharpforourdrij

correc<onhadcontributedtothisdifference,butthiscanbemademorestablewithSQUIDtuning.

•  Lowfrequencylinesthatproduceoscilla<onsvisibleinthe<medomainprovidetheremainderofthegap.

•  Filteringtheselinesinthe<medomainpriortotheimplementa<onofthephase-insensi<veop<malfiltermayimprovetheenergyresolu<on.

DetectorNoise•  WehavemodeledourTESswiththeknowndesign

parametersandgetagoodfittoX-raypulses.•  Inordertofitthenoisespectrum,excessnoise

needstobeaddedtothemodel,andtheexcessphonon-likenoiseisthedominantcomponentoftheintegratednoiseequivalentpower(NEP).

•  Totalmul<plexedelectronicsnoiseis40pA//√Hz,whichisbelowthelevelofthedetectornoise

RadioFrequencyPickup•  Webelievethattheexcessphononnoiseis

generatedbyRFpickupintothecryostatwhichmanifestsashea<nginthedetector.

•  Theflightboxthatinterfacesbetweenthecryostatandroomtemperatureelectronicsallowsmorepickupthanthelaboratoryequivalent.Weareinves<nghowtogeneratea<ghterelectricalseal.

•  Suscep<bilitytothisnoisetypevariesfrompixeltopixel.Thereisnopabernofwhichpixelsareworsewithinthereadoutwiringscheme,sothenoisehastoenterthedetectorsdirectly.

EnergyspectrumofdatatakenonaMicro-Xpixel,zoomedinontheKK-αline.

PixelYB01PotassiumK-αlineFWHM=9.88±0.2eVΧ2=1.03

Timelineofremainingworkun<lflight.LaunchscheduledforFebruary2018.

6/24/17 7/24/17 8/23/17 9/22/17 10/22/17 11/21/17 12/21/17 1/20/18

GSE built Optics

Clean/reassembly FEA wirebond

Avionics assembly Science electronics testing

Get avionics vibed Flight configuration tests

PIR Travel to WFF

Integration tests MRR

Ship to WSMR Travel to WSMR

WSMR tests Launch

PixelYB01NoiseTracesFWHM=7.01±0.067eVΧ2=0.55

EnergyspectrumofdatatakenonaMicro-Xpixel,zoomedinonnoisetraces.

Noisespectrumforarepresenta<veTESintheMicro-Xarray,biased30%intothetransi<on.Thesuddendropinthenoiseat8.4kHzistherollofffrequencyofthedigitalan<-aliasfilterthatcorrectsfortheeffectsfromthedecima<onofdata.