STUC Meeting – May 2014 K. Sembach

Current Status

Infrared WFC3/IR 2014 • All science instruments are performing well – ACS, COS, STIS, and WFC3 are being used for science

• Cycle 21 is progressing as planned – October 1, 2013 – September 30, 2014

• Froner Fields program is in full swing – (Epoch 1: Oct-Nov 2013) – MACS J0416.1-2403 (Epoch 1: Jan-Feb 2014) – Abell 2744 (Epoch 2: May-Jun 2014) – MACS J0416.1-2403 (Epoch 2: Aug 2014) Visible WFPC2 2001 – MACS J0717.5+3745 (Epoch 1: Sep 2014)

• Loss of Gyro 5 in March 2014 – 17 orbits impacted – Science meline recovered within 30 hours

• 24th Anniversary on April 24, 2014 – Kicks off Hubble’s 25th year

STUC - May 2014 2 Long Range Observing Plan (D. Adler and the Planning & Scheduling Team)

• Observing efficiency remains high to date through Cycle 21

• Cycle Completeness: scheduled Cycle 21 84.0 (to date) • Cycle 17 completed in March 2013 • Cycle 18 completed in July 2013 Cycle 20 85.5 • Cycle 19 completed in March 2014 Cycle 19 83.2 • Cycle 20 has 19 orbits in the plan Cycle 18 83.4 Cycle 17 84.0 • Cycle 21 Subscripon: • Well subscribed through mid-August • May pull some Cycle 22 programs forward this summer to keep efficiency high

STUC - May 2014 3 Long Range Plan Status through calendar ending 05/18/14

Orbits Cycle Orbits Now Oct ’13 Visits not in current plan Now Oct ’13 19 0 4 Unschedulable 18 18 20 19 265 No plan windows 2 8 21 1595 3343 Cycle 20 miscellaneous 122 65 22 69(1) 72(1) Cycle 21 miscellaneous 99 134 Total 1683 3684 Total not yet in plan 241 225 Orbits Instrument Orbits Now Oct ’13 SNAPs Now Oct ’13 WFC3 590 1621 Cycle 20 810 854 COS 530 984 Cycle 21 494 646 ACS 354 593 Total 1304 1500 STIS 221 497 (1) Some Cycle 22 Froner Fields and DD observaons have windows FGS 2 3 opening in Cycle 21. Total(2) 1697 3698 (2) Some programs have more than one prime science instrument.

STUC - May 2014 4 Long Range Plan Progress of Froner Field Programs

Executed or Planned Orbits scheduled Froner Field Cycle alloc 10/1/14 10/1/15 < 5/18/14 < 9/30/14 - 9/30/15 - 9/30/16 Abell 2744 21 140 76 64 0 0 MACSJ0416.1-2403 21 140 70 70 0 0 MACSJ0717.5+3745 22 140 2 10 128 0 MACSJ1149.5+2223 22 140 4 0 136 0 Abell S1063 23 140 0 0 0 140 Abell 370 23 140 0 0 0 140

STUC - May 2014 5 WFC3 Infrared Persistence

• The WFC3 HgCdTe detector exhibits a complex set of persistence phenomena following exposure to significant levels of illuminaon.

• Scheduling system now defines: • Bad actors – bright IR sources; no other IR observaons can be taken within two orbits. • Sensive observaons – IR observaons that are sensive to residual persistence. • Worst actors – bright IR sources that generate persistence over large conguous regions (i.e., GRISM/spaal scans) – no other IR within two orbits; no sensive observaons within 10 orbits.

• There can be efficiency issues when there are worst actors and sensive observaons on the same flight calendar.

STUC - May 2014 6 Persistence in Froner Fields

• Persistence complicates: – Scheduling – Calibraon – Analysis

• Migaon: – Dither observaons to reduce “self-persistence” – Idenfy observaons likely to cause severe problems Residual from prior – Schedule with sufficient spaal scan intervals (a real challenge) – Predict persistence using me history of detector (another challenge) Froner Field MACS0416 with the imprint of a spaally scanned observed many hours prior to this observaon

STUC - May 2014 7 STUC - May 2014 8 Long Range Plan Cycle 20 Large and Treasury Programs

Cycle 20 Large Orbits Exec/sched Planned before Status & Treasury alloc by 05/18/14 9/30/14 Bean 60 60 0 Complete Bedin 120 120 0 Complete Cushing 125 125 0 Complete Gaensicke 122 163(1) 0 Complete Gladders 107 107 0 Complete Kirshner (ToO) 100 94 6 Ends July 2014 Riess 112 112 0 Complete Sabbi 60 60 0 Complete Sahu 64 64 0 Complete

(1) Total orbits > allocaon due to extra visits needed to set flags and check for bright objects.

STUC - May 2014 9 Long Range Plan Cycle 21 Large and Treasury Programs

Cycle 21 Large Orbits Exec/sched Planned before Planned aer Not in & Treasury alloc by 5/18/14 9/30/14 10/1/14 plan Ayres 230 144 58 25 3 Bean 152 103 33 16 0 Calze 154 144 10 0 0 Churchill 110 62 48 0 0 Peterson 179 108 71 0 0 Pioo 131 84 45 2 0 Treu 140 45 46 49 0

Peterson (Reverberaon mapping of NGC 5548): • One visit per day for 179 straight days • Missed three visits due to Gyro 5 safing (March 7) and the COS suspend event (March 25/26) • Missed four visits due to slew/OBAD issues • Science sll on track

STUC - May 2014 10 AGN-STORM: Mean Spectra

AGN – Space Telescope and Opcal Reverberaon Mapping (PI = B. Peterson)

G130M – cenwave: 1291, 1327 G160M – cenwave: 1600, 1623

Lyα CIV

STUC - May 2014 11 AGN-STORM: Preliminary Light Curves

Connuum Lyα red wing

Lyα

JD – 2450000 JD – 2450000

Length of the campaign: 179 nights Length of the campaign: 179 nights

STUC - May 2014 12 Science Instruments

STUC - May 2014 13 ACS Status Update (N. Grogin and the ACS Team)

• The ACS/WFC and ACS/SBC connue to perform well. – Nearly five years of revived WFC : longer than pre-failure WFC – ACS comprises ~17% of Cycle 21 GO usage (& 50% of HFFs)

• The CALACS pipeline has recently been streamlined by segregang the pixel-based CTE correcon stage and exploing parallel processing for a 60x speed enhancement.

• The ACS Team has been supporng the HFF implementaon and data- reducon efforts. Enhanced WFC calibraons, driven by HFF requirements, are being incorporated into CALACS and AstroDrizzle to benefit the enre ACS user community.

STUC - May 2014 14 Developments in CTE Migaon

• Connued detailed monitoring of CTE degradaon (see plot at lower le) – Refined coefficients for pixel-based (Anderson & Bedin) correcon used in CALACS – Refined coefficients for post-hoc correcon of stellar photometry (via ACS webtool)

• CTE-migang LED post-flash ISR recently published (ACS ISR 2014-1) – Refined understanding of use-cases & proper flash levels from CTE monitoring 2K sub-array image Direcon of worsening CTE WFC 2K sub-array correcon recently validated; soon to be included in CALACS

STUC - May 2014 15 Developments in CTE Migaon

STUC - May 2014 16 ACS Coming Aracons

• Comprehensive mapping of WFC scaered-light – Associaon of enre WFC full-frame image archive (~105 images) with GSC2 – “Dragon’s breath” and “Edge glow” danger zones to be displayed in APT/Aladin • WFC calibraon synergies with the HFF Program – Superior dark-current subtracon for highly-mulple image stacks (“self-cal”) – Improved full-frame bias de-striping via automated source-masking – Faster validaon and distribuon of improved geometric distoron soluon – Faster validaon and distribuon of improved flaields • Proper handling of WFC full-frame readout dark – Impacts all images; currently subsumed into superbias (but not a bias effect) – Ramps up to several-electron add’l pedestal for CTE; add’l Poisson noise term – Proper handling will result in reduced “bad-column” flagging and beer CTE correcon

STUC - May 2014 17 WFC3 Status (J. Mackenty and the WFC3 Team)

• WFC3 is operang nominally • CCD detectors performing well (radiaon damage growth on trend) – ~50% usage of PostFlash for CTE migaon (appropriate fracon; GOs understand opon) – Ongoing enhancements to post-observaon correcon code; fall install into OPUS • IR Detector Persistence – Connuing to refine our understanding/models; f(expme, flux, total illuminaon, me) – Emphasis on short exposures of bright objects to improve transit observaons • IR Background variaons – He 1.083 µm line is strong source (analogous to Lyα) from illuminated atmosphere – Impacts both grisms (G102 and G141 overlap at 1.083 µm) plus F110W and F105W – Observaons with mulple filters benefit from sequencing within each orbit (HFF changed) – Working to beer predict background for planning and also improve sky subtracon • Astrometry – CCD photolithographic paern and filter correcons (9 filters); errors 0.1 à 0.01 pixels – Spaal Scans for <30 micro arc second parallax measurements (Riess et al published) • PSF libraries – Experiments underway to extract extensive libraries of (~107) observed PSF – Improved focus monitoring/adjustment; PSF models and actuals to observers in future

STUC - May 2014 18 Froner Fields F105W Backgrounds

Higher He I emission Lower He I emission

STUC - May 2014 19 Channel Select Mechanism Usage

• Reduce usage to migate CSM risk without impacng science

STUC - May 2014 20 COS Status (C. Oliveira and the COS/STIS Team)

• COS is performing well at its FUV detector Lifeme Posion 2 (since July 2012)

• Work is proceeding for move to COS FUV Lifeme Posion 3 in February 2015 – Gain sag models originally indicated that would need to move to LP3 in September 2014 to overcome localized sensivity losses – LP3 will be located -2.5” from original lifeme posion • Blue modes (1055/1096 of G130M) will remain at current locaon (LP2); all other modes moved to LP3 • G140L and G130M/1222 will have to be operated at different high voltage values from all other modes. Blue modes at LP2 will also use different high voltages.

• COS FUV trending sll shows only low level decrease in sensivity (~3%/yr) 2010 2011 LP1 2012 2013 LP2 2014 1.0 1.0

0.9 0.9 Throughput

0.8 0.8

STUC - May 2014 21 COS/FUV Improved Extracon

• Current spectral extracon collapses spectrum over a rectangular box - Pixels at edges of profile might fall on regions sagged by a previous lifeme posion and the whole column is discarded - This is OK if effect on flux always < a few percent

• Strategy for Improved Extracon – Create library of spectral reference profiles – Align reference profile with observed spectrum to allow significance of any bad pixels to be evaluated

• Inial Implementaon – Two-zone extracon – In each column add up all counts within central 99% of encircled energy (EE) – Only discard column if inner 80% EE region contains flagged pixels – Technique close to current boxcar when no bad pixels are flagged – Should be more tolerant of mediocre alignment of profile with spectrum than a weighted or opmal extracon would be

STUC - May 2014 22 COS FUV Two-Zone Extracon

• Compute cumulave energy in profile as a funcon of Y in each column to idenfy outer (99% EE) and inner (80% EE) zones – Add up flux in full region, but only flag sagged pixels if located in inner zones

Old method Areas excluded from extracted spectrum when boxcar (old) extracon method is used

New method

STUC - May 2014 23 STIS Status (C. Oliveira and the COS/STIS Team)

• STIS/MAMA and STIS/CCD channels are working well (5 years aer SM4)

• Support for new STIS apertures implemented – Outsourced calibraon program 12567 (PI: Ayres) to make ND long slits (31x0.05NDA, 31x0.05NDB, 31x0.05NDC) slits fully supported (aenuaon of ~ 4x, 10x, and 25x) • Currently supported ND slits allow only aenuaon factors of 2x, 100x, or 1000x • New slits are especially important for studies of LISM and bright standard stars

• Spectroscopic ETC now supports small echelle slits with the CCD for ACQ/PEAK

• New coronographic locaons for STIS provide inner working angles of ~0.2” – Outsourced calibraon program 12923 (PI: Gaspar) explored new aperture locaons near corner of the coronographic bar (BAR10) as well as the “bent finger” wedge (BAR5) – New posions allow high contrast imaging at a minimum working angle of 0.15” with demonstrated performance at 0.2” close to 2x beer than WEDGE0.6 (smallest posion currently supported)

STUC - May 2014 24 Hubble Source Catalog

STUC - May 2014 25 HST Source Catalog Update (B. Whitmore and the HSC Team)

SDSS image and catalog Hubble footprint for M101 Example of potenal for supporng database astronomy at new level of detail

The Hubble Source Catalog:

– Combines tens of thousands of HLA visit-based source lists into a single master catalog

– Provides entry into the rapidly growing field of database astronomy

– Will be a fundamental reference for JWST users, and upcoming surveys (e.g., PanSTARRS, LSST) HSC sources STUC - May 2014 26

Three Reasons to Build the Catalog

1. Time-variable phenomena – The HSC supports 2. Mosaics – Accurate spaal me-variable studies over a >20 year baseline. offsets between observaons are needed to build the HSC. These can then be used to HSC photometry of dwarf make mosaics. IC 1613

124 ACS images 29 separate visits 3. Very large datasets – Replicang what is available in the HSC in seconds would take

Hubble images most researchers weeks, months, or years of the SMC to produce. STUC - May 2014 27

Symbiosis Between the HSC and HLA

WFPC2Magaper2HSCProc There is a symbioc relaonship WFPC2 Matched Pairs between the HSC and HLA. Some 106 before things are easier to detect and fix in bin the HSC database while other things 4 are easier in the HLA images and Pairs 10 source lists.

Matched 100

WFPC2Magaper2HSCDev WFPC2 Matched Pairs 1 106 0.01 0.02 0.05 0.10 0.20 aer frac diff bin

4 Pairs 10 Here is an example of a problem with WFPC2 magnitudes that was

Matched 100 first detected in the HSC and then fixed in the HLA. 1 0.01 0.02 0.05 0.10 0.20 frac diff STUC - May 2014 28 Hubble Source Catalog Timeline

June 2012 – Beta 0.1 release (Budavari + Lubow 2012 paper posted) • Included ACS/WFC and WFPC2 HLA source lists May 2013 – Beta 0.2 release • Improved source filtering and matching • Improved tools (plots, summary form, …) • Formaon of external HSC Working Group following release Mar 2014 – Beta 0.3 release • Included ACS/WFC, WFPC2, and WFC3 catalogs from HLA DR7 • Improved matching (i.e., from ~70 % to 95 % “good” catalogs)

~Fall 2014 – Version 1 of HSC • Improved ACS and WFPC2 catalogs (based on WFC3-type algorithms) • Integraon with the MAST Discovery Portal

Future Plans • Cross-matching with other projects (e.g., Spzer, Chandra, PanStarrs, …) • Pointers to existence of spectroscopic data (e.g., FOS, GHRS, STIS, COS, GRISMS) • More extensive tools (e.g., support SQL database queries)

STUC - May 2014 29 Hubble 2020 Vision

STUC - May 2014 30 ------Monday, May 25, 2009

Thursday, May 8, 2014

If all works as planned, Hubble should be able to peer even deeper into space and farther back in time than it has before. The telescope, circling some 350 miles above Earth, is expected to perform for at least five more years. That should be long enough to bridge the gap until its successor, the James Webb Space Telescope, is sent to a perch almost a million miles from Earth.

STUC - May 2014 31 Hubble 2020 Vision Statement

Operate Hubble out to 2020 or beyond so that there is at least one year of overlapping science observaons with the James Webb Space Telescope, performed in a manner that maximizes the science return of both observatories by taking full advantage of Hubble's unique capabilies and the astronomical community's scienfic curiosity.

How long will Hubble connue to • An operang observatory operate? • Capable science instruments

As long as it remains • Scienfic drivers (demand)

scienfically producve • Adequate staffing and user support

What is needed to keep Hubble • Appropriate funding scienfically producve? • Teamwork (mul-level)

STUC - May 2014 32 The Road to 2020+

Current Status Expectaons • Good reliability of science instruments and Observatory Excellent major systems through 2020 (NESC) Health • Known modes of degradaon Orbit Decay Nominal orbit • Orbit stable unl mid-2030s Scheduling • Efficiency declines to ~40-45% upon ~50%, near all-me high Efficiency transion to reduced-gyro mode Scienfic ~800 papers per year; • Publicaon rate remains high Producvity ~40 PhDs per year • New discoveries connue >1000 proposals per year; Demand • No near-term decrease expected 6:1 oversubscripon (me) • Work efficiencies are harder to achieve Staffing Lean operaons beyond FY16 without loss of capability Mission $98.3M/year total budget • Flat mission budget presents challenges Funding (~2/3 ops, ~1/3 grants+EPO) Grant $28.6M/year in grants to the • Grant funding is stable through FY15-FY16 Funding community • May decline as JWST grants start

STUC - May 2014 33 Subsystem Reliability

• NESC reliability esmates for Hubble’s instruments and primary subsystems support a 2020 vision for the observatory. • The recent failure of Gyro 5 does not substanvely change the overall gyro lifeme assessment. Instruments Subsystems

STUC - May 2014 34 Hubble Science Output

• 12,089 science papers based on HST data, with nearly 500,000 citaons • 13,122 individuals have (co)authored a paper based on HST data • More than 500 PhD theses have been based on HST data Refereed Papers per Year

Year of Publicaon

STUC - May 2014 35 Intense Proposal Pressure

• In Cycle 22 there were 1135 proposals submied • >6000 different invesgators have had approved programs to date

Post-SM4 Just received Number of Proposals per Cycle Cycle STUC - May 2014 36 HST Budget ($98.3M)

Grants to Observers GFSC Flight Operaons 29% Cy18 – $27.7M & Sustaining Engineering Cy19 – $28.4M 33% Cy20 – $30.1M Cy21 – $28.6M Operaons staff is STScI EPO half the size it was 4.5% ~12 years ago STScI Science Operaons 33.5%

Note: Even a flat funding profile of $98.3M per year will require reducons in personnel or cuts to science grant funding. Hubble may be 24 years old, but its best years are sll ahead…. No Scan

Scanned

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