Hubble Space Telescope 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
• Fron er Fields program is in full swing – Abell 2744 (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:
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 Fron er Fields and DD observa ons 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 Fron er Field Programs
Executed or Planned Orbits scheduled Fron er 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 illumina on.
• Scheduling system now defines: • Bad actors – bright IR sources; no other IR observa ons can be taken within two orbits. • Sensi ve observa ons – IR observa ons that are sensi ve to residual persistence. • Worst actors – bright IR sources that generate persistence over large con guous regions (i.e., GRISM/spa al scans) – no other IR within two orbits; no sensi ve observa ons within 10 orbits.
• There can be efficiency issues when there are worst actors and sensi ve observa ons on the same flight calendar.
STUC - May 2014 6 Persistence in Fron er Fields
• Persistence complicates: – Scheduling – Calibra on – Analysis
• Mi ga on: – Dither observa ons to reduce “self-persistence” – Iden fy observa ons likely to cause severe problems Residual from prior – Schedule with sufficient spa al scan intervals (a real challenge) – Predict persistence using me history of detector (another challenge) Fron er Field MACS0416 with the imprint of a spa ally scanned star observed many hours prior to this observa on
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 > alloca on 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 a er 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 Pio o 131 84 45 2 0 Treu 140 45 46 49 0
Peterson (Reverbera on 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 s ll on track
STUC - May 2014 10 AGN-STORM: Mean Spectra
AGN – Space Telescope and Op cal Reverbera on Mapping (PI = B. Peterson)
G130M – cenwave: 1291, 1327 G160M – cenwave: 1600, 1623
Lyα CIV
STUC - May 2014 11 AGN-STORM: Preliminary Light Curves
Con nuum 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 con nue 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 segrega ng the pixel-based CTE correc on stage and exploi ng parallel processing for a 60x speed enhancement.
• The ACS Team has been suppor ng the HFF implementa on and data- reduc on efforts. Enhanced WFC calibra ons, driven by HFF requirements, are being incorporated into CALACS and AstroDrizzle to benefit the en re ACS user community.
STUC - May 2014 14 Developments in CTE Mi ga on
• Con nued detailed monitoring of CTE degrada on (see plot at lower le ) – Refined coefficients for pixel-based (Anderson & Bedin) correc on used in CALACS – Refined coefficients for post-hoc correc on of stellar photometry (via ACS webtool)
• CTE-mi ga ng 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 Direc on of worsening CTE WFC 2K sub-array correc on recently validated; soon to be included in CALACS
STUC - May 2014 15 Developments in CTE Mi ga on
STUC - May 2014 16 ACS Coming A rac ons
• Comprehensive mapping of WFC sca ered-light – Associa on of en re WFC full-frame image archive (~105 images) with GSC2 – “Dragon’s breath” and “Edge glow” danger zones to be displayed in APT/Aladin • WFC calibra on synergies with the HFF Program – Superior dark-current subtrac on for highly-mul ple image stacks (“self-cal”) – Improved full-frame bias de-striping via automated source-masking – Faster valida on and distribu on of improved geometric distor on solu on – Faster valida on and distribu on of improved fla ields • 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 be er CTE correc on
STUC - May 2014 17 WFC3 Status (J. Mackenty and the WFC3 Team)
• WFC3 is opera ng nominally • CCD detectors performing well (radia on damage growth on trend) – ~50% usage of PostFlash for CTE mi ga on (appropriate frac on; GOs understand op on) – Ongoing enhancements to post-observa on correc on code; fall install into OPUS • IR Detector Persistence – Con nuing to refine our understanding/models; f(exp me, flux, total illumina on, me) – Emphasis on short exposures of bright objects to improve exoplanet transit observa ons • IR Background varia ons – 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 – Observa ons with mul ple filters benefit from sequencing within each orbit (HFF changed) – Working to be er predict background for planning and also improve sky subtrac on • Astrometry – CCD photolithographic pa ern and filter correc ons (9 filters); errors 0.1 à 0.01 pixels – Spa al Scans for <30 micro arc second parallax measurements (Riess et al published) • PSF libraries – Experiments underway to extract extensive libraries of (~107) observed PSF stars – Improved focus monitoring/adjustment; PSF models and actuals to observers in future
STUC - May 2014 18 Fron er Fields F105W Backgrounds
Higher He I emission Lower He I emission
STUC - May 2014 19 Channel Select Mechanism Usage
• Reduce usage to mi gate CSM risk without impac ng science
STUC - May 2014 20 COS Status (C. Oliveira and the COS/STIS Team)
• COS is performing well at its FUV detector Life me Posi on 2 (since July 2012)
• Work is proceeding for move to COS FUV Life me Posi on 3 in February 2015 – Gain sag models originally indicated that would need to move to LP3 in September 2014 to overcome localized sensi vity losses – LP3 will be located -2.5” from original life me posi on • Blue modes (1055/1096 of G130M) will remain at current loca on (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 s ll shows only low level decrease in sensi vity (~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 Extrac on
• Current spectral extrac on collapses spectrum over a rectangular box - Pixels at edges of profile might fall on regions sagged by a previous life me posi on and the whole column is discarded - This is OK if effect on flux always < a few percent
• Strategy for Improved Extrac on – Create library of spectral reference profiles – Align reference profile with observed spectrum to allow significance of any bad pixels to be evaluated
• Ini al Implementa on – Two-zone extrac on – 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 op mal extrac on would be
STUC - May 2014 22 COS FUV Two-Zone Extrac on
• Compute cumula ve energy in profile as a func on of Y in each column to iden fy 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) extrac on 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 a er SM4)
• Support for new STIS apertures implemented – Outsourced calibra on program 12567 (PI: Ayres) to make ND long slits (31x0.05NDA, 31x0.05NDB, 31x0.05NDC) slits fully supported (a enua on of ~ 4x, 10x, and 25x) • Currently supported ND slits allow only a enua on 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 loca ons for STIS provide inner working angles of ~0.2” – Outsourced calibra on program 12923 (PI: Gaspar) explored new aperture loca ons near corner of the coronographic bar (BAR10) as well as the “bent finger” wedge (BAR5) – New posi ons allow high contrast imaging at a minimum working angle of 0.15” with demonstrated performance at 0.2” close to 2x be er than WEDGE0.6 (smallest posi on 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 poten al for suppor ng 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 spa al me-variable studies over a >20 year baseline. offsets between observa ons are needed to build the HSC. These can then be used to HSC photometry of dwarf galaxy make mosaics. IC 1613
124 ACS images 29 separate visits 3. Very large datasets – Replica ng 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 symbio c rela onship 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 a er 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, …) • Forma on 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) • Integra on with the MAST Discovery Portal
Future Plans • Cross-matching with other projects (e.g., Sp zer, 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 observa ons 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 capabili es and the astronomical community's scien fic curiosity.
How long will Hubble con nue to • An opera ng observatory operate? • Capable science instruments
As long as it remains • Scien fic drivers (demand)
scien fically produc ve • Adequate staffing and user support
What is needed to keep Hubble • Appropriate funding scien fically produc ve? • Teamwork (mul -level)
STUC - May 2014 32 The Road to 2020+
Current Status Expecta ons • Good reliability of science instruments and Observatory Excellent major systems through 2020 (NESC) Health • Known modes of degrada on Orbit Decay Nominal orbit • Orbit stable un l mid-2030s Scheduling • Efficiency declines to ~40-45% upon ~50%, near all- me high Efficiency transi on to reduced-gyro mode Scien fic ~800 papers per year; • Publica on rate remains high Produc vity ~40 PhDs per year • New discoveries con nue >1000 proposals per year; Demand • No near-term decrease expected 6:1 oversubscrip on ( me) • Work efficiencies are harder to achieve Staffing Lean opera ons 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 es mates for Hubble’s instruments and primary subsystems support a 2020 vision for the observatory. • The recent failure of Gyro 5 does not substan vely change the overall gyro life me assessment. Instruments Subsystems
STUC - May 2014 34 Hubble Science Output
• 12,089 science papers based on HST data, with nearly 500,000 cita ons • 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 Publica on
STUC - May 2014 35 Intense Proposal Pressure
• In Cycle 22 there were 1135 proposals submi ed • >6000 different inves gators 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 Opera ons 29% Cy18 – $27.7M & Sustaining Engineering Cy19 – $28.4M 33% Cy20 – $30.1M Cy21 – $28.6M Opera ons staff is STScI EPO half the size it was 4.5% ~12 years ago STScI Science Opera ons 33.5%
Note: Even a flat funding profile of $98.3M per year will require reduc ons in personnel or cuts to science grant funding. Hubble may be 24 years old, but its best years are s ll ahead…. No Scan
Scanned
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