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Hubble Space Telescope Observer’S Guide Spring 2021

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Hubble Space Telescope Observer’S Guide Spring 2021 HUBBLE SPACE TELESCOPE OBSERVER’S GUIDE SPRING 2021 In 2021, the Hubble Space Telescope is celebrating 31 years in operation as a powerful observatory probing the astrophysics of the cosmos from Solar system studies to the high-redshift universe. The high-resolution imaging capability of HST spanning the IR, optical, and UV, coupled with spectroscopic capability will remain invaluable through the middle of the upcoming decade. HST coupled with JWST is poised to enable new innovative science and be will be key for multi-messenger investigations. Key Science Threads • Properties of the huge variety of exo-planetary systems: compositions and inventories, compositions and characteristics of their planets • Probing the stellar and galactic evolution across the universe: pushing closer to the beginning of galaxy formation and preparing for coordinated JWST observations • Exploring clues as to the nature of dark energy ACS SBC absolute re-calibration (Cycle 27) reveals 30% greater • Probing the effect of dark matter on the evolution sensitivity than previously understood. More information at of galaxies http://www.stsci.edu/contents/news/acs-stans/acs-stan- • Quantifying the types and astrophysics of black holes october-2019 of over 7 orders of magnitude in size WFC3 offers high resolution imaging in many bands ranging from • Tracing the distribution of chemicals of life in 2000 to 17000 Angstroms, as well as spectroscopic capability in the universe the near ultraviolet and infrared. Many different modes are available for high precision photometry, astrometry, spectroscopy, mapping • Investigating phenomena and possible sites for and more. robotic and human exploration within our Solar System COS COS2025 initiative retains full science capability of COS/FUV out to 2025 (http://www.stsci.edu/hst/cos/cos2025). Observing opportunities include coordination with JWST, Lifetime Position 5 will be introduced for Cycle 29. the UV initiative, archive research, and mid-cycle observing proposals. STIS Updates for CALSTIS include geometric distortion, time sensitivity and blaze shift.See stisblazefix, a tool for blaze fixing: https://github.com/spacetelescope/stisblazefix Cover: The giant nebula (NGC 2014) and its smaller blue neighbor (NGC 2020) are part of a vast star-forming region in the Large Magellanic Cloud. T Tauri stars and brown dwarfs within 8 star-forming regions in the ULLYSES Milky Way, including time-domain monitoring of 4 prototypical T Tauri CHARTING stars with well-known rotation periods and magnetic configurations. YOUNG STARS’ All targets are being observed with COS and/or STIS medium-resolution modes, as detailed in Table 2. ULTRAVIOLET LIGHT Region Instrumental modes WITH HUBBLE COS/G130M/1096 (brightest O stars) The Hubble Space Telescope’s Ultraviolet Legacy Library of Young LMC and COS/G130M/1291 + COS/G160M/1611 or STIS E140M SMC STIS/E230M/1978 (O9 I – B9 I only) Stars as Essential Standards (ULLYSES) is a Director’s Discretionary STIS/E230M/2707 or COS/G185M/1953 + 1986 (B5-9 I) program of approximately 1,000 orbits that will produce an ultraviolet Sextans-A and COS/G140L/800 spectroscopic library of young high- and low-mass stars in the local NGC 3109 universe. The ULLYSES program will uniformly sample the fundamental Survey T Tauri COS/G130M/1291 + COS/G160M/1611 astrophysical parameter space for each mass regime, including spectral stars STIS/G230L + STIS/G430L + STIS/G750L type, luminosity class, and metallicity for massive stars, and the mass, Monitoring T COS/G160M/1611 + COS/G230L/2635 + COS/ Tauri stars G230L/2950 age, and disk accretion rate in low-mass stars. The program is expected to execute over a three-year period, from Cycle 27 to Cycle 29. Region # ULLYSES # AR # ULLYSES targets targets orbits PROJECT MILESTONES LMC 98 34 225 February 2020 Target samples released SMC 65 41 220 First data release (LMC and SMC stars) November 2020 Sextans-A 3 6 ~37 ullyses.stsci.edu/ullyses-download.html NGC 3109 3 0 ~15 Observations of T Tauri stars in Ori and Ori OB1 November-December regions in coordination with TESS and LCOGT Lupus 27 4 142 2020 σ (programs 16113, 4, 5) Cha I 16 3 97 Data release 2 (LMC, SMC massive stars; Spring 2021 Cha 2 1 22 Orion T Tauri stars) ϵ Cha 5 3 20 Epoch 1 of HST monitoring observations of Spring 2021 TW Hya and RU Lup Orionη OB1 10 0 45 Observing Strategy and Technical Specifications ∑ Ori 3 0 13 The ULLYSES program is divided into two primary observational CrA 2 0 10 campaigns of high- and low-mass stars. The focus on high-mass TW Hydrae 1 0 2 stars includes observations of 65 stars in the SMC, 98 stars in the Monitoring CTTS 4 0 100 LMC, as well as 6 additional stars which are accessible in the even TOTAL 239 92 948 lower metallicity Local Group galaxies NGC 3109 and Sextans A. For low-mass stars, observations will focus on about 71 K- and M-type FOR MORE INFORMATION, VISIT https://ullyses.stsci.edu Massive Stars T Tauri Stars The massive star component of ULLYSES leverages on existing The 61 T Tauri stars to be surveyed in 8 Milky Way star-forming regions uniformly sample mass and disk accretion rate. The li- FUSE and HST archival data, to provide full UV coverage at medi- brary of UV-optical-NIR spectra from ULLYSES will enable studies um-resolution for ~240 targets uniformly sampling spectral type of the accretion and resulting UV radiation in those objects, which and luminosity class. affects the evolution of proto-planetary disks and the chemical The ULLYSES dataset for massive stars will enable transformative composition and atmospheric escape of young planets. science in the field of stellar astrophysics, and enable a legacy of studies of the interstellar and circum-galactic media. 3 1e 14 C IV 2 10 10 1 0 1545 1550 1555 10 11 F 1e 15 8 Mg II 6 12 10 4 2 0 2760 2780 2800 2820 2840 10 13 103 104 Wavelength WIDE FIELD CAMERA 3 (WFC3) Wide Field Camera 3 (WFC3) offers high resolution imaging in bands ranging from 2000 to 17000 Angstroms, as well as spectroscopic capability in the near ultraviolet and infrared. A variety of modes are available for high precision photometry, astrometry, spectroscopy, mapping and more: http://www.stsci.edu/sites/www/home/hst/instrumentation/wfc3.html UVIS IR 130'' (1013 pix) 162'' (4096 pix) Wavelength Ranges SPECTROSCOPIC MODES IMAGING MODES Select filters shown. UVIS/IR channels feature 62/15 filters, respectively, with varying bandwidths for many spectral features Direct Imaging Grism Spectroscopy High resolution, wide field imaging. Large complement of Using grisms instead of imaging filters allows low resolution filters for various photometric bands/spectral features. spectroscopy, while maintaining high spatial resolution. Disperse wavelengths 휆 Slew during Add exposure scanning Scan with grism Spatial Scanning Grism Scanning Slewing during exposure (spatial scanning) places Combining scanning and grism spectroscopy allows source flux on hundreds of pixels/avoids saturation, for extremely high SNR spectra. Useful for transit achieving extremely high SNR photometry. observations. WFC3 information: http://www.stsci.edu/sites/www/home/hst/instrumentation/wfc3.html Handbook: https://hst-docs.stsci.edu/display/WFC3IHB SPACE TELESCOPE IMAGING SPECTROGRAPH (STIS) FUV MAMA (Multi Anode Microchannel Array) STIS is one of the oldest active instruments on the Hubble Space • 1024 x 1024 CsI detector, TIME-TAG available Telescope (HST). • Imaging: 25’’ x 25’’ FOV, 0.025’’ pixels, 9 filters • large fraction of total HST observing time (10-15% GO • Spectroscopy: 2 first order and 2 echelle gratings observations in recent Cycles) = 1150 – 1740Å, R ~ 1000 - 200,000 − ~30 cen. • incredibly versatile and highly configurable instrument • Numerous filters, gratings, and apertures • λwave. configurations NUV MAMA • large variety of unique photometric and spectroscopic • 1024 x 1024 CS2Te detector, TIME-TAG available modes • Imaging: 25’’ x 25’’ FOV, 0.025’’ pixels, 12 filters • high spatial resolution in the UV and optical • Spectroscopy: 2 first order and 2 echelle gratings ACCESS TO UV = 1650 – 3100 Å, R ~ 500 - 200,000 • ~55λ cen. wave. Configurations • Prism Spectroscopy: = 1150 - 3620 Å, R ~ 10 – 2500 CCD • λ • 1024 x 1024 SITE CCD detector • Imaging: 52’’ x 52’’ FOV, 0.051’’ pixels, 9 filters • Spectroscopy: 6 first order gratings = 1650 – 11,000 Å, R ~ 500 - 10,000 • ~40 cen. wave. Configurations • λ CORONAGRAPHY • Usable with coronagraphic mask and occulting bars • Broadband imaging (2000 - 10,300 Å ) • Bar-occulted spectroscopy (2000 - 10,300 Å) SPATIALLY-RESOLVED SPECTROSCOPY UNIQUE USES OF STIS Spatial Scanning with the STIS CCD TIME-TAG Mode Spatial scanning is now an available-but-unsupported mode The STIS MAMA allows time-resolved observations through on STIS. TIME-TAG mode. • allows for more photons to be collected before reaching • tracks the collection time of each individual photon event at the CCD full-well saturation. a time resolution of 125 microseconds. • better averaging over variations in the flat field, • can lead to much better IR fringe removal than non-scanned images. • For example, Signal-to-Noise ratios of 600-800 have been achieved in 1D extracted G750M/9336 spectra For more information about STIS: www.stsci.edu/hst/instrumentation/stis If you have questions about STIS/HST/STScI: https://stsci.service-now.com/hst ADVANCED CAMERA FOR SURVEYS (ACS) Dust Pillars in Gravitational lensing Carina observed with in Abell 370 observed the ACS/WFC. with ACS/WFC. Uses filters F502N Uses filters ([O III], blue) F475W (blue), and F658N F625W (green), and (H + [N II], red). F814W (red ). Wide Field Channel (WFC) Solar Blind Channel (SBC) • FUV imaging and slitless spectroscopy (1,150–1,700 Å) • Optical imaging and slitless spectroscopy • High throughput, best for FUV imaging (3,500–11,000 Å) • 35'' x 31'' field of view • Highest throughput on HST in visible light • 5 longpass filters, 1 Lyman filter • 202'' x 202'' field of view, largest on HST • Two prisms; R ~ 79 and 96 at 1,500 Å • 13 wide, medium, and narrowband filters • 15 tunable wavelength filters • Grism (5,500–10,500 Å); R ~ 100 at 8,000 Å • Near-UV / visible linear polarization filters Please see the ACS Instrument Handbook for more de- tailed information on ACS capabilities.
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