Kepler Data Release 17 Notes Q12 · 2012-08-28 · MJD midTime MJD midTime UT midTime UT midTime...

Kepler Data Release 17 Notes

Q12

KSCI-19057-001Data Analysis Working Group (DAWG)

Susan E. Thompson (Editor)

KSCI-19057-001: Kepler Data Release 17 Notes

Document Control

OwnershipThis document is part of the Kepler Project Documentation that is controlled by the Kepler Project Office,NASA/Ames Research Center, Moffett Field, California.

Control LevelThis document will be controlled under KPO @ Ames Configuration Management system. Changes to thisdocument shall be controlled.

Physical LocationThe physical location of this document will be in the KPO @ Ames Data Center.

Distribution RequestsTo be place on the distribution list for additional revisions of this document, please address your request tothe Kepler Science Office:

Michael R. HaasKepler Science Office DirectorMS 244-30NASA Ames Research CenterMoffett Field, CA [email protected]

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The Data Characteristics Handbook and accompanying Data Release Notes are the collective effort ofthe Data Analysis Working Group (DAWG), composed of Science Office (SO), Science Operations Center(SOC), and Guest Observer (GO) Office members as listed below:

Jon Jenkins*, ChairDoug Caldwell*, Co-ChairBarclay, ThomasBryson, Stephen T.Burke, Christopher J.Christiansen, Jessie L.Clarke, Bruce D.Cote, Miles T.Girouard, ForrestHaas, Michael R.Hall, JenniferIbrahim, KhadeejahKinemuchi, KarenKlaus, ToddKolodziejczak, Jeffery (MSFC)Li, JieMcCauliff, Sean D.Morris, RobMullally, FergalQuintana, Elisa V.Rowe, JasonSeader, ShawnSmith, Jeffrey ClaiborneStill, MartinStumpe, Martin C.Tenenbaum, Peter G.Thompson, Susan E.Twicken, JoeUddin, Akm KamalVan Cleve, Jeffrey

The correct citation for this document is: S. E. Thompson, J. L. Christiansen, J. M. Jenkins, D. A.Caldwell, T. Barclay, S. T. Bryson, C. J. Burke, B. D. Clarke, M. T. Cote, F. Girouard, M. R. Haas, J.R. Hall, K. Ibrahim, K. Kinemuchi, T. C. Klaus, J. J. Kolodziejczak, J. Li, S. D. McCauliff, R. Morris, F.Mullally, E. V. Quintana, J. Rowe, S. Seader, J. C. Smith, M. D. Still, M. C. Stumpe, P. G. Tenenbaum, J.D. Twicken, A. K. Uddin, and J. E. Van Cleve, 2012, Kepler Data Release 17 Notes (KSCI-19057-001).

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Contents

1 Introduction 71.1 Dates, Cadence Numbers, and Units . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 7

2 Release Description 8

3 Evaluation of Performance 83.1 Overall . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 8

4 Historical Events 104.1 Kepler Mission Timeline to Date . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 104.2 Safe Mode . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 104.3 Loss of Fine Point . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 104.4 Attitude Tweaks . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 114.5 Variable FGS Guide Stars . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 114.6 Module 3 Failure . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 114.7 NEW – A Few Corrupted Targets on Module 2.1 . . . . . . . . . . . . . . . . . . . . . . . . . 12

5 Ongoing Phenomena 135.1 Image Motion . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 145.2 Focus Changes . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 145.3 Momentum Desaturation . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 145.4 Reaction Wheel Zero Crossings . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 145.5 Downlink Earth Point . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 145.6 Manually Excluded Cadences . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 145.7 Incomplete Apertures Give Flux and Feature Discontinuities at Quarter Boundaries . . . . . 145.8 Argabrightening . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 145.9 Background Time Series . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 155.10 Pixel Sensitivity Dropouts . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 155.11 Short Cadence Requantization Gaps . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 165.12 Spurious Frequencies in SC Data . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 165.13 Propagation of Uncertainties . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 165.14 Onboard Spacecraft Errors . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 165.15 Anomaly Summary Tables . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 175.16 NEW – Data Loss and Detector Changes from Coronal Mass Ejections . . . . . . . . . . . . . 19

6 UPDATED – Time and Time Stamps 21

7 Ensemble Cotrending Basis Vectors 21

8 Contents of Supplement 228.1 Short Supplement Package . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 22

9 References 23

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A Word of Caution to Users

The Simple Aperture Photometry (SAP) product generated by the PA (Photometric Analysis) pipelinemodule and the PDC (Pre-search Data Conditioning) processed data are designed for automated photome-try on over 160,000 stars. Although significant effort has been expended to make these products robust andreliable, they do not produce the best photometry for every target. To mitigate the impact of non-optimalapertures, Kepler is now providing target pixel files so that users can perform their own photometry. Keplerhas also completely reworked the PDC software module, which is now producing significantly improved re-sults for most long-cadence targets. All data processed after Data Release 12 (Q9) has taken advantage ofthe new PDC module. Additionally, Q0–Q4 were reprocessed in March 2012 (Data Release 14) and Q5–Q8were reprocessed in July 2012 (Data Release 16). Also, cotrending basis vectors (see Section 7.0) are beingprovided for all quarters so that users can better remove systematics from the simple-aperture-photometry(SAP) light curves generated by the pipeline or custom light curves self-extracted from the target pixel files.

Investigators are strongly encouraged to study the Data Characteristics Handbook and Data ReleaseNotes for all data sets that they intend to use. We advise against publication of results based on Kepler lightcurves without careful consideration and due diligence by the end user, and dialogue with the Science Officeor Guest Observer Office where appropriate.

Users are encouraged to notice and document artifacts or issues with the processing and report them tothe Science Office at [email protected].

Like Waldseemuller’s 1507 map, the Maximum A Priori (MAP) method for PDC and other improvementsto light curve correction implemented in Kepler Pipeline 8.0 will show us more of the light-curve world thanwe knew before, while leaving some hazards to navigation around the edges. Far-ranging light curve marinerswill be given the tools to help navigate in such perilous circumstances by the Guest Observer Office.

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1 Introduction

These Data Release Notes provide information specific to the release of Q12 data, processed with SOCPipeline 8.1. These Notes contain the summary figures and tables for this quarter—the companion text canbe found in the Kepler Data Characteristics Handbook (KSCI-19040). The sections are numbered in thesame order in these Notes and the Handbook to assist the reader.

1.1 Dates, Cadence Numbers, and Units

No changes from the Data Characteristics Handbook.

Contents of Data Release 17.

Q.m First Cadence Last Cadence First Cadence Last Cadence Num Start EndMJD midTime MJD midTime UT midTime UT midTime CINs CIN CIN

12 LC 55931.9097 56014.5227 05-Jan-2012 21:49:54 28-Mar-2012 12:32:43 4044 48473 5251612.1 SCM1 55931.8998 55958.4015 05-Jan-2012 21:35:41 01-Feb-2012 09:38:08 38910 1442650 148155912.2 SCM2 55959.1173 55986.4977 02-Feb-2012 02:48:58 29-Feb-2012 11:56:40 40200 1482610 152280912.3 SCM3 55987.3975 56014.5326 01-Mar-2012 09:32:20 28-Mar-2012 12:46:56 39840 1524130 1563969

Contents of Data Release 17–Full Frame Images.

Q Class Filename UT Start UT End

12 FFI KPLR2012032101442 2012-02-01 09:45:16 2012-02-01 10:14:4212 FFI KPLR2012060123308 2012-02-29 12:03:42 2012-02-29 12:33:0812 FFI KPLR2012088132324 2012-03-28 12:53:58 2012-03-28 13:23:24

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2 Release Description


3 Evaluation of Performance

3.1 Overall

Figure 1: 6.5-h Temporal Median (TM) of the CDPP time series calculated by the TPS pipeline module. Themedian (circles) and 10th percentile value (diamonds) for all dwarf stars between Kp=11.75–12.25 are given.The 6-h TMCDPPs have been divided by sqrt(13/12) = 1.041 to approximate 6.5-h TMCDPPs. A detaileddiscussion of the CDPP values is given in the Kepler Data Characteristics Handbook and in Christansen etal. (2012, arXiv:1208.0595). The 6.x, 7.0 and 8.0 labels given in the legend refer to the version of the SOCpipeline used.

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Table 1: Aggregate statistics for the TMCDPPs by magnitude. Column Definitions: (1) Kepler Magnitudeat the center of the bin. Bins are ± 0.25 mag, for a bin of width 0.5 mag centered on this value. (2) Numberof dwarfs (log g > 4) in the bin. (3) 10th percentile TMCDPP for dwarfs in the bin. (4) Median TMCDPPfor dwarfs in the bin. (5) Number of all stars in the bin. (6) 10th percentile TMCDPP of all observed starsin the bin. (7) Median TMCDPP for all stars in the bin. (8) Simplified noise model CDPP.

Kp mag No. dwarfs 10th prctile Median No. stars 10th prctile Median Noise model

9.0 53 9.6 24.4 182 11.3 48.6 3.810.0 161 12.8 31.9 585 14.3 59.1 6.011.0 637 18.4 31.6 1775 20.3 66.9 9.512.0 2231 25.1 35.6 4293 26.5 53.4 15.213.0 7037 36.5 47.0 10193 37.5 54.0 24.414.0 14300 57.0 71.7 16568 57.7 73.9 40.115.0 28675 101.6 129.4 28679 101.6 129.4 68.816.0 15006 187.9 236.8 15006 187.9 236.8 127.8

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4 Historical Events

In this Section, we discuss cadences that may not be useful for high-precision photometry due to planned orunplanned spacecraft events.

4.1 Kepler Mission Timeline to Date

Kepler Mission TimelineJanuary February March April May June July August September October November December

SM 6/15 SM 7/2 LOFP LOFP LOFP SM 11/19

2009

Launch Science 7/20 8/20 10/19 11/19 12/17Mod 3 SM - 2/2 3/6/09 FSW patch 5/12/09 6/18 9/17 SM 12/22

LOFP 12/13

2010

1/19 2/18 3/19 4/21 5/20 7/21 8/22 9/22 10/23 11/23 12/21

SM - 2/1 SM 3/14 SM 12/7

2011

1/24 2/23 3/19 4/26 5/25 6/26 7/27 8/29 9/29 10/31 12/1You are here

2012

2/1 2/29 4/30 5/31 7/30 8/30 11/4 12/61/4 3/28 6/28 10/1

Commissioning Q2-Summer Q3-Fall Q1-Spr

Quarterly roll Monthly

Symbol Key

Safe Mode Event

Loss of Fine-Point

Module 3 anomaly

Q5-Spring Q6-Summer Q7-Fall Q4-Winter

Q9-Spring Q10-Summer Q11-Fall Q8

Q13-Spring Q14-Summer Q12-Winter

Chart update date

Winter

Q15-Fall

Figure 2: Kepler Mission Timeline as of the end of Q12.

4.2 Safe Mode

There were no Safe Modes in Q12.

4.3 Loss of Fine Point

The cadences obtained when the spacecraft was not in fine point are listed in Tables 4 and 5, the LC and SCanomaly summary tables respectively.

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Figure 3: Attitude Error in Q12, calculated by PAD using Long Cadence data. The large spike nearMJD=55994 is caused by the CME.

4.4 Attitude Tweaks

The pointing history is shown in Figure 3; there were no attitude tweaks over the course of Q12.

4.5 Variable FGS Guide Stars


4.6 Module 3 Failure


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4.7 NEW – A Few Corrupted Targets on Module 2.1

Targets whose photometric apertures include pixels that lie in columns 632-638 on mod.out 2.1 have incorrectsmear correction, corrupting the data on these targets. The bright variable star CH Cyg (KIC 11913210)has increased in brightness during quarter 12, causing these columns to be affected by charge bleeding intothe masked smear region on mod.out 2.1 (channel 1, skygroup 1). These affected columns were not excludedduring calibration causing targets that fall near the columns occupied by CH Cyg to have an incorrect smearcorrection. The high values in these masked smear columns exceed the pixel data storage range on thespacecraft, causing the smear data values to wrap through zero. For some columns this wrapping occursseveral times during the quarter. Due to the highly-varying and incorrect smear values used, calibratedpixel values, and all calculated time series for targets on these columns are not valid. This problem will becorrected in future processing of the data.

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5 Ongoing Phenomena

In this Section, we document the systematic errors arising in nominal on-orbit operations, most of which areremoved from the PDC flux time series by the science pipeline. An overview of the events which impacteddata collection in Q12 are shown in Figure 4.

Figure 4: An overview of the location of the data anomalies flagged in Q12.

The flags shown in Figure 4 are explained in the Data Characteristics Handbook and Archive Manual. Fur-ther details on certain flags are listed here:

• NO DATA indicates cadences where no data was collected (e.g during Earth-point or Safe Mode events).

• ARGABRIGHTENING refers to cadences where the multiple-channel Argabrightening flag (flag 0x07,decimal value 64) was set. The single channel flag (0x0D, decimal value 4096) is not represented on thisplot. No cadences exceeded the multiple-channel, argabrightening threshold this quarter. See Table 3for a list of cadences identified at a lower threshold in multiple channels.

• COARSE POINT refers to cadences where the pointing of the telescope drifted by more than 0.5 millip-ixels from the nominal value. NOT FINE POINT refers to cadences where the telescope’s fine guidancesensor reported that the telescope was not in fine point mode. These flags are combined as flag 0x03(decimal value 3) in the FITS files.

• EXCLUDE corresponds to flag 0x09 (decimal value 256). It is set when another, unspecified, eventdegrades data quality. In Q12, this flag was set to mark cadences during coronal mass ejection events.See Sections 5.6 and 5.16.

• LDE FLAG refers to flags set by the Spacecraft when a error was detected in the Local DetectorElectronics (LDE) on the on-board memory. The pipeline does not process these cadences, so only rawpixels are available.

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5.1 Image Motion


5.2 Focus Changes


5.3 Momentum Desaturation

Tables of the Long and Short Cadences affected by momentum desaturations in the reaction wheels areprovided in the Data Release Notes Supplement; the cadences are also indicated in the quality flag columnin the FITS files at MAST.

5.4 Reaction Wheel Zero Crossings

The cadences of the reaction wheel zero crossings are marked in the SAP QUALITY and QUALITY columnof the light curve and target pixel files, respectively.

5.5 Downlink Earth Point

The cadences occurring during spacecraft Earth Point are listed in Tables 4 and 5.

5.6 Manually Excluded Cadences

Data quality during Q12 was affected by three coronal mass ejections (CMEs) discussed in Section 5.16.Users are strongly discouraged from using the data collected during these events, see Table 2 for cadencesthat were affected by the CME.

Table 2: Cadences affected by the CME are marked with the Manual Exclude flag (0x09, decimal 256) in theSAP QUALITY column of the light-curve files (and the QUALITY column in the target pixel files).

Q.m First Cadence Last Cadence First Cadence Last CadenceLC LC SC SC

12.1 49319 49423 1468030 147117912.1 49544 49589 1474780 147615912.3 51465 51685 1532410 1539039

5.7 Incomplete Apertures Give Flux and Feature Discontinuities at QuarterBoundaries


5.8 Argabrightening

The cadences affected by Argabrightening events with amplitude TMAD > 10 are listed in Table 3 for LC.We no longer list the SC Argabrightening events in the data release notes. Since they are concurrent withthe LC events, use the LC Argabrightening events to determine those times when SC data are affected bythis phenomenon.

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Table 3: Q12 LC Argabrightening Events with amplitude TMAD > 10, and occurring on a number of channelsTMCE > 10. This threshold is lower than that set in the pipeline. The columns are (1) Cadence intervalnumber (CIN) for Argabrightening cadences, (2) Relative cadence index (RCI) for Argabrightening cadences,(3) Argabrightening cadence mid-times (MJD), (4) Mean Argabrightening statistic over channels includedin the Argabrightening event < SArg >FPA, (5) Number of channels exceeding threshold for this cadence(Nchan), (6) Number of channels exceeding the default pipeline threshold for this cadence (Npipe).

CIN RCI Mid-Times (MJD) < SArg >FPA Nchan Npipe

49138 666 55945.49801 7.2 19 049473 1001 55952.34327 20.7 78 049585 1113 55954.63183 6.1 15 050159 1687 55966.36072 7.2 14 050197 1725 55967.13720 6.5 12 050470 1998 55972.71557 5.6 23 050482 2010 55972.96077 8.0 24 050627 2155 55975.92365 22.9 23 550988 2516 55983.30018 3.5 13 050989 2517 55983.32061 5.0 16 050990 2518 55983.34105 6.4 26 050991 2519 55983.36148 7.5 29 050992 2520 55983.38191 8.4 32 050993 2521 55983.40235 8.8 34 050994 2522 55983.42278 9.2 34 050995 2523 55983.44321 9.3 29 050996 2524 55983.46365 9.1 31 050997 2525 55983.48408 11.2 48 050998 2526 55983.50451 8.9 40 050999 2527 55983.52495 6.8 25 051000 2528 55983.54538 4.6 15 051348 2876 55990.65628 10.3 43 051795 3323 55999.79010 11.0 43 051796 3324 55999.81053 9.3 30 051797 3325 55999.83096 9.3 32 051798 3326 55999.85140 10.1 36 051799 3327 55999.87183 9.5 34 051800 3328 55999.89227 9.5 33 051801 3329 55999.91270 7.3 23 052236 3764 56008.80132 12.2 48 052403 3931 56012.21373 18.0 65 052491 4019 56014.01189 8.0 14 0

5.9 Background Time Series

The background flux time series for Q12 is shown in Figure 5.

5.10 Pixel Sensitivity Dropouts

Some pixels lost sensitivity following the CMEs. See section 5.16 for further information regarding this lossof sensitivity.

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Figure 5: The background flux time series for Q12 showing the average over all the modules, and twoindividual modules. The narrow spikes are Argabrightening events. The large, broad spikes near MJD55950, 55954 and 55993 are a result of the CMEs.

5.11 Short Cadence Requantization Gaps


5.12 Spurious Frequencies in SC Data


5.13 Propagation of Uncertainties


5.14 Onboard Spacecraft Errors


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5.15 Anomaly Summary Tables

The list of cadences affected by data anomalies. LDE OUT of SYNC indicates a error flag set by the LocalDetector Electronics box. The full lists of affected cadence interval numbers (CINs) for Tables 4 and 5 beloware included in the Data Release 17 Supplement.

Table 4: Q12 LC Anomaly Summary Table

LC CIN start LC CIN end Anomaly Type Note

48473 48473 EARTH POINT48647 48647 LDE OUT OF SYNC48709 48709 COARSE POINT49007 49008 COARSE POINT49148 49148 COARSE POINT49319 49423 EXCLUDE49544 49589 EXCLUDE49654 49654 COARSE POINT49770 49805 EARTH POINT49805 49805 LDE OUT OF SYNC49974 49974 COARSE POINT50168 50168 COARSE POINT50222 50222 LDE OUT OF SYNC51145 51189 EARTH POINT51465 51685 EXCLUDE51495 51495 LDE OUT OF SYNC51498 51498 LDE OUT OF SYNC51500 51500 LDE OUT OF SYNC51503 51503 LDE OUT OF SYNC51508 51511 LDE OUT OF SYNC51513 51513 LDE OUT OF SYNC51518 51518 LDE OUT OF SYNC51738 51738 COARSE POINT51741 51741 COARSE POINT52023 52023 COARSE POINT52292 52292 COARSE POINT52361 52361 COARSE POINT

Table 5: Q12 SC Anomaly Summary Table

SC CIN start SC CIN end Anomaly Type Note

1442650 1442650 EARTH POINT1445508 1445521 COARSE POINT1449730 1449759 COARSE POINT1449888 1449901 COARSE POINT1454268 1454281 COARSE POINT1458648 1458661 COARSE POINT1458670 1458729 COARSE POINT1462900 1462929 COARSE POINT

Continued on next page

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Table 5 – continued from previous page

SC CIN start SC CIN end Anomaly Type Note

1463028 1463041 COARSE POINT1466859 1466891 COARSE POINT1467408 1467421 COARSE POINT1468030 1471179 EXCLUDE1471788 1471801 COARSE POINT1474780 1476159 EXCLUDE1476168 1476181 COARSE POINT1477389 1477421 COARSE POINT1478080 1478109 COARSE POINT1480548 1480561 COARSE POINT1482610 1482610 EARTH POINT1482610 1482639 LDE OUT OF SYNC1485978 1485991 COARSE POINT1487680 1487709 COARSE POINT1490358 1490371 COARSE POINT1493500 1493529 COARSE POINT1494738 1494751 COARSE POINT1499118 1499131 COARSE POINT1503498 1503511 COARSE POINT1507878 1507891 COARSE POINT1512258 1512271 COARSE POINT1516608 1516621 COARSE POINT1520988 1521001 COARSE POINT1524130 1524130 EARTH POINT1527228 1527241 COARSE POINT1531608 1531621 COARSE POINT1532410 1539039 EXCLUDE1540368 1540381 COARSE POINT1540600 1540629 COARSE POINT1540690 1540719 COARSE POINT1544748 1544761 COARSE POINT1549128 1549142 COARSE POINT1549150 1549179 COARSE POINT1553508 1553521 COARSE POINT1557220 1557249 COARSE POINT1557888 1557901 COARSE POINT1559290 1559319 COARSE POINT1562268 1562281 COARSE POINT

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5.16 NEW – Data Loss and Detector Changes from Coronal Mass Ejections

Data quality during Q12 was affected by three coronal mass ejections (CMEs). Cadences impacted by theCME were marked with the Manual Exclude flag (0x09, decimal 256) in the SAP QUALITY column of thelight-curve files (and the QUALITY column in the target pixel files). Users are strongly discouraged fromusing the data collected during these events, see Table 2 for cadences that were affected by the CME.

During these CMEs, the flux of charged particles from the sun impacting the spacecraft increased by manyorders of magnitude causing an increase in measured dark current, as well as the “cosmic ray” count. Thefine guidance sensors were also impacted, so the pointing of the spacecraft deviated from the nominal valueby many milli-pixels.

Users should note that the detector underwent some long-term changes after the CMEs. These effects areparticularly noticeable after the third, and most powerful, CME. In particular:

• The dark current rose slightly. This increase does not materially affect data quality.

• A small number of pixels show a pronounced drop in sensitivity after the largest CME. When a targetstar falls on one or more of these pixels, the mean measured flux will be lower after the CME thanbefore. In the majority of such cases, the pixel-sensitivity dropout corrector in PDC is confused bythese discontinuities because of the intervening gapped cadences. PDC-MAP can only correct globalsystematic errors and thus these sensitivity drop outs cannot be dealt with effectively by the algorithm.Hence, PDC fails to correct most of them and often introduces additional low-frequency artifacts intothe light curve (e.g., see Figure 6).

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Figure 6: Flux time series showing a discontinuity that can happen after the CME. The blue and red curvesshow the PA and PDC light curves, respectively. Notice that PDC is unable to satisfactorily correct thediscontinuities following the CME, and that the correction introduces a long term trend into the data.

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6 UPDATED – Time and Time Stamps

Kepler has some preliminary evidence that the absolute time in the archived data files are wrong by ap-proximately one minute. We have not identified the source of this discrepancy. If you have information, orevidence, related to this issue please email the Kepler Science Office at [email protected].

7 Ensemble Cotrending Basis Vectors

A plot highlighting the principal values for Q12 cotrending basis vectors is shown in Figure 7. There are noother changes from the Data Characteristics Handbook.

Figure 7: A representative set of principal values of SVD-extracted cotrending basis vectors for Q12, showingthat most of the systematic errors can be accounted for by the first 8 or fewer components. Users are providedwith the first 16 components for each mod.out in the files at MAST.

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8 Contents of Supplement

The Supplement is available as a full package (DataReleaseNotes17SupplementFull.tar), which contains thefiles described below. The thermal telemetry files have been removed from this release but can be obtainedfrom the Science Office upon request.

Pipeline Instance Detail Reports

q12-lc-from PA ksop1246-as-run-pipeline-instance-detail-report-120530.txtq12-sc3-ksop1246-as-run-pipeline-instance-detail-report-120604.txt

Data Anomaly Types

DataAnomalyTypes_Q12LC_LC_PID6758.txt

DataAnomalyTypes_Q12SCM1_SC_PID6775.txt



Mod.out central motion

Q12LC_central_column_motion.txt

Q12LC_central_row_motion.txt

Background Flux Time Series

Q12LC_background.txt

Q12SCM1_background.txt



Argabrightening Detections

Q12LC_LC_ArgAgg_Summary.txt

Out of Fine Point Cadence Lists

Q12LC_LC_isNotFinePoint.txt

Q12SCM1_SC_isNotFinePoint.txt



8.1 Short Supplement Package

The Supplement also contains a short package suitable for emailing (DataReleaseNotes17SupplementShort.tar).The small package does not contain the following files:

Q12LC_background.txt




Q12LC_central_column_motion.txt

Q12LC_central_row_motion.txt

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9 References

20. “The Derivation, Properties and Value of Kepler’s Combined Differential Photometric Precision”, Chris-tiansen, J. L. et al., arXiv:1208.0595 (2012)

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