The list of Investigators does not match the STScI records for this program. 0 ----- Attempting Submission 1 (Wed Apr 13 19:24:35 GMT 2022) ----- There has been an evolution of the CoIs over the course of the ULLYSES programs. The Space Telescope Science Institute (STScI) Director has decided to devote up to 1000 orbits of Director's Discretionary time in observing Cycles 27-29 to a new Hubble Ultraviolet Legacy program focused on star formation and associated stellar physics. This new program, ULLYSES (UV Legacy Library of Young Stars as Essential Standards), will provide a UV spectroscopic reference sample of young (< 10 Myr) high- and low-mass stars. It will target over ~150 OB stars in the Magellanic Clouds and lower metallicity galaxies in the Local Group, and ~40 T Tauri stars and brown dwarfs in the Milky Way. In addition, ULLYSES will monitor 4 typical T Tauri stars over different rotational phases through at least three rotation periods, and over timescales of months to years. The resulting library will provide template spectra of massive stars at metallicities substantially below the well studied, while the low mass sample will cover a wide range of ages, accretion rates, and masses, including objects down to well below 0.5 M_sun. The legacy of this large UV dataset on the first 10 Myr of stellar evolution will be enhanced by complementary datasets obtained by the scientific community. In addition to the core goals of the program related to stellar astrophysics of low and high mass stars, this data will also enable exciting science in the fields of ISM, CGM, jets, and exoplanets. ULLYSES will be modeled after the Frontier Fields program: all data obtained will be non-proprietary. The implementation team at STScI is developing high-level science data products and a sophisticated database and website for disseminating data from the ULLYSES program and ancillary datasets for the ULLYSES target sample from space and ground-based facilities. This proposal includes a subset of the massive ULLYSES stars being observed in the Magellanic clouds. Depending on target brightness, the main FUV spectral range will generally use either the STIS E140M setting or the combination of the COS c1291 + c1611 settings. Sufficiently bright stars without good FUSE data in the archive will also be observed with the COS c1096 setting to provide coverage at shorter wavelengths. Where time permits, stars of type O9 or later will also be observed with STIS E230M/1978, while for supergiants of spectral type B5 or later E230M/2707 may also be included. Where possible, targets of a given spectral type were selected to span both a range in extinction and in rotation rates to support a variety of stellar and ISM studies. Signal-to-noise requirements used to determine the desired exposures times were defined as follows: COS/G130M/c1096: 20 / nine-pixel resel at 1080 A COS/G130M/c1291: 30 / six-pixel resel at 1150 A COS/G160M/c1611: 30 / six-pixel resel at 1590 A COS/G185M/c1953: 30 / three-pixel resel at 1860 A COS/G185M/c1986: 30 / three-pixel resel at 1980 A STIS/E140M/c1425: 20 / two-pixel resel at 1200 A STIS/E230M/c1978: 20 / two-pixel resel at 1800 A STIS/E230M/c2707: 20 / two-pixel resel at 2800 A The actual implemented exposure times may be adjusted to efficiently use HST orbits, but should always provide at least 80% of the desired time as defined by the above requirements. Additional details about the scientific motivation and technical implementation strategy of the ULLYSES observations can be found at http://www.stsci.edu/stsci-research/research-topics-and-programs/ullyses. The ULLYSES program is based on the recommendations of a working group led by Sally Oey; the full text of that group's report can be found at http://www.stsci.edu/files/live/sites/www/files/home/stsci-research/research-topics-and-programs/ullyses/_documents/HSTUV-report-ULLYSES.pdf. 0 false SUPPORTED STAR SUPERGIANT O OF NO N11-ELS-020 : [ELS2006] N11 020 Previous name : N11-020 Input file: ULLYSES_Cycle29_MassiveStar_ProgramInput_v5.csv SpT = O5 Inf+p COS/G130M/c1096 : rn(PoWR-OB-new(PoWR_39000_3.80_m7.00_Z0.50.fits, lmc-ob-i 39-38, Z=0.500 solar, Teff=39000, log_lum=5.54, log_g=3.80, log_mdot=-7.00) (extinction lmcavg=0.060), flux1160 +- 2.0A flux=5.3e-13 Flam) Coordinate pedigree: Gaia DR2 Calculation performed 2021-10-25T00:58:05, v0.9 ------------------------------------------------------------------------------- tstatus; N11-ELS-020; P/COS approved for submission; S/ins not started; P/RP 11/04/22; S/xx DD/MM/YY tcheck; APT/SIMBAD target names: ; Yes tcheck; Target info verification status?; Yes tcheck; Coordinates & P.M. verified, epoch checked?; Yes tcheck; Adopted SED compared to Observations?; Yes ... Still using O5 I model, but extinction is increased to 0.18 to fit both the STIS data and the photometry. Flux = 5.2e-13 Flam at 1160A ELS2006-N11-020 J2000 SpT=O5 Inf+p; E(B-V)=0.06; B=12.96; V=13.18; F1160=5.310e-13; F1360=4.560e-13; F1700=3.630e-13 1649866731090 The scheduling data was generated by CASM 30.1. CASM was run in Phase II mode. vstatus; 1C; N11-ELS-020; P/COS approved for submission; P/RP 11/04/22 ; intrev: complete ; P/AF 12/04/22 vcheck; Enter targ name & Inst. & Resp. Sci.; N11-ELS-020 ; COS ; RP vcheck; ETC numbers entered in APT?; Yes vcheck; Any screening violations?; No vcheck; S/N ETC calcs done & documented?; Yes vcheck; Field images checked & saved?; Yes vcheck; Selected ACQ strategy?; Yes ... ACQ/IMAGE-BOA/MIRRORA vcheck; Possible ACQ or Sci spoilers?; No vcheck; Field BOT clear?; Yes ... The unknown stars in the field are most likely: - Gaia DR3 4662150750288097536 - K5V star with Gmag 17.98 - Gaia DR3 4662150754618470272 - A7V-A8V star with Gmag 18.66 - Gaia DR3 4662150754581323776 - G8V-G9V star with Gmag 18.69 vcheck; Visual BOT check for stars not in catalog?; Yes vcheck; Orbit packing finalized?; Yes vcheck; Buffer times optimized?; Yes vcheck; Verify visit grouping correct; N/A vcheck; Is visit ready for int. review?; Yes Allocated COS orbits = 2 (Tic-Visit :proposal-id 16817 :visit-id "1C" :proposal-version -1 :trans-version "20211222" :date "13-Apr-2022 12:18:51.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 1452496 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16817 :visit-id "1C" :obset-id "1C" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16817 :visit-id "1C" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2577 :al-overhead-at-end 0 :internal-dur-at-end 114 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2970 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16817 :visit-id "1C" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2578 :al-overhead-at-end 0 :internal-dur-at-end 439 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2970 :pcs-gap 0 ) true 2 0 Expected S/N of ~30 for imaging TA rn(PoWR-OB-new(PoWR_39000_3.80_m7.00_Z0.50.fits, lmc-ob-i 39-38, Z=0.500 solar, Teff=39000, log_lum=5.54, log_g=3.80, log_mdot=-7.00) (extinction lmcavg=0.060), flux1160 +- 2.0A flux=5.3e-13 Flam); cos,fuv,g130m,c1096,psa,mjd#59670; fp-pos=None, segment=None) From file ULLYSES_Cycle29_MassiveStar_ProgramInput_v5.csv Spectral type: O5 Inf+p SED = N11-ELS-20_COS_G130M_c1096_sed.fits For exptime=3251.1 s, spectral region: 1080.0 +- 0.5 A achieves SNR=20.0/resel global countrate (brightest segment): 5515.4 cts/s/segment brightest pixel: 0.108 cts/s/pix at 1220.0 A Calculation performed 2021-10-25T00:58:11, v0.9 --------- Expected S/N ~20 at 1180 A using the combined FPPOS. The exposure time was calculated using a new model with an extinction=0.18. This change much better reflects the existing STIS data and U, B photometry. rn(PoWR-OB-new(PoWR_39000_3.80_m7.00_Z0.50.fits, lmc-ob-i 39-38, Z=0.500 solar, Teff=39000, log_lum=5.54, log_g=3.80, log_mdot=-7.00) (extinction lmcavg=0.060), flux1160 +- 2.0A flux=5.3e-13 Flam); cos,fuv,g130m,c1096,psa,mjd#59670; fp-pos=None, segment=None) From file ULLYSES_Cycle29_MassiveStar_ProgramInput_v5.csv Spectral type: O5 Inf+p SED = N11-ELS-20_COS_G130M_c1096_sed.fits For exptime=3251.1 s, spectral region: 1080.0 +- 0.5 A achieves SNR=20.0/resel global countrate (brightest segment): 5515.4 cts/s/segment brightest pixel: 0.108 cts/s/pix at 1220.0 A Calculation performed 2021-10-25T00:58:11, v0.9 --------- Expected S/N ~20 at 1180 A using the combined FPPOS. The exposure time was calculated using a new model with an extinction=0.18. This change much better reflects the existing STIS data and U, B photometry. rn(PoWR-OB-new(PoWR_39000_3.80_m7.00_Z0.50.fits, lmc-ob-i 39-38, Z=0.500 solar, Teff=39000, log_lum=5.54, log_g=3.80, log_mdot=-7.00) (extinction lmcavg=0.060), flux1160 +- 2.0A flux=5.3e-13 Flam); cos,fuv,g130m,c1096,psa,mjd#59670; fp-pos=None, segment=None) From file ULLYSES_Cycle29_MassiveStar_ProgramInput_v5.csv Spectral type: O5 Inf+p SED = N11-ELS-20_COS_G130M_c1096_sed.fits For exptime=3251.1 s, spectral region: 1080.0 +- 0.5 A achieves SNR=20.0/resel global countrate (brightest segment): 5515.4 cts/s/segment brightest pixel: 0.108 cts/s/pix at 1220.0 A Calculation performed 2021-10-25T00:58:11, v0.9 --------- Expected S/N ~20 at 1180 A using the combined FPPOS. The exposure time was calculated using a new model with an extinction=0.18. This change much better reflects the existing STIS data and U, B photometry. rn(PoWR-OB-new(PoWR_39000_3.80_m7.00_Z0.50.fits, lmc-ob-i 39-38, Z=0.500 solar, Teff=39000, log_lum=5.54, log_g=3.80, log_mdot=-7.00) (extinction lmcavg=0.060), flux1160 +- 2.0A flux=5.3e-13 Flam); cos,fuv,g130m,c1096,psa,mjd#59670; fp-pos=None, segment=None) From file ULLYSES_Cycle29_MassiveStar_ProgramInput_v5.csv Spectral type: O5 Inf+p SED = N11-ELS-20_COS_G130M_c1096_sed.fits For exptime=3251.1 s, spectral region: 1080.0 +- 0.5 A achieves SNR=20.0/resel global countrate (brightest segment): 5515.4 cts/s/segment brightest pixel: 0.108 cts/s/pix at 1220.0 A Calculation performed 2021-10-25T00:58:11, v0.9 --------- Expected S/N ~20 at 1180 A using the combined FPPOS. The exposure time was calculated using a new model with an extinction=0.18. This change much better reflects the existing STIS data and U, B photometry.