09/30/21: Update to the STIS ORIENT to exclude a nearby bright star that doesn't clear for the G230L NUV MAMA observations. The nearby M-dwarf will likely no longer be in the slit.
11/04/21: Update to the PEAKD centering algorithm from FLUX-WT-FLR to FLUX-WT to be consistent with expected values for NUMPOS=3 and STEPSIZE=1.3
11/11/21: Update to timing requirements from sequence to grouping to make it less time constrained-1812578639----- Attempting Submission 1 (Tue Sep 14 01:11:29 GMT 2021) -----
HST Phase II Proposal 16599 successfully submitted.
Receipt: # 16599-1
----- Attempting Submission 2 (Thu Sep 30 17:04:38 GMT 2021) -----
HST Phase II Proposal 16599 successfully submitted.
Receipt: # 16599-2
----- Attempting Submission 3 (Thu Nov 04 21:46:41 GMT 2021) -----
HST Phase II Proposal 16599 successfully submitted.
Receipt: # 16599-3
----- Attempting Submission 4 (Thu Nov 11 15:09:22 GMT 2021) -----ULLYSES T Tauri Survey Star HD 104237E in Eps ChaThe 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 low mass ULLYSES survey stars. Each target will be observed with the COS c1291 + c1589 + c1623 settings, as well as with STIS G230L, G430L, and G750L. All observations will normally be constrained to occur within 1 day.
Signal-to-noise requirements used to determine the desired exposures times were defined as follows:
COS/G130M/c1291: N V 1239 +- 1 A -- S/N=10/6-pix-resel at the peak of the line
COS/G160M/c1589: C IV 1549 +- 1 A -- S/N=20/6-pix-resel at the peak of the line (combined c1589 & c1623)
COS/G160M/c1623: C IV 1549 +- 1 A -- S/N=20/6-pix-resel at the peak of the line (combined c1589 & c1623)
STIS/G230L/52X2: Mg II 2800 +-15 A -- S/N=20/2-pix-resel at the peak of the line
STIS/G430L/52X2: continuum average 4000 +-5 A -- S/N=20/2-pix-resel (2 reads)
STIS/G750L/52X2: continuum average 5700 +-5 A -- S/N=20/2-pix-resel (2 reads)
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.0falseSUPPORTEDSTART TAURI STARPRE-MAIN SEQUENCE STARNOHD-104237E : eps Cha 7, J12000931-7811424
Region: eps Cha
Simbad: https://simbad.u-strasbg.fr/simbad/sim-id?Ident=HD+104237E&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id
Target coordinates are from Gaia DR3.
Spectral type: K5.5 ; A_V: 1.0 ; Distance (pc): 114
M*: 0.9 ; log(dm/dt): -9.07
Input file: targets_up_to_May30-2022.csv
hd104237e_lya2_etc_scaled_pAV0.50.txt
Calculation performed 2021-06-18T15:05:41, 0.24
-------------------------------------------------------------------------------
tstatus; HD-104237E; P/COS approved for submission; S/STIS internal review complete; P/DJS 30/09/21; S/RP 30/09/22
tcheck; APT/SIMBAD target names: ; [FLG2003] eps Cha 7 & 2MASS J12000931-7811424
tcheck; Target info verification status?; Yes. Photometry is scarce; Our model of the target was checked against U=15.279 V=13.674 B=15.912
tcheck; Coordinates & P.M. verified, epoch checked?; Yes. Correct against Gaia DR3
tcheck; Adopted SED compared to Observations?; YesEPS-CHA-7J12000931-7811424J2000SpT=K5.5; A_V=1.00; V=12.1STARA0-A3 III-INOHD-104237 is going to be an offset target about 11" away from HD-104237E because of an M-dwarf in the field that isn't safe to observe with the COS/PSA.
All ETC runs used archival HST/STIS data of this target.
V-magnitude and Spectral type pulled from Simbad
Coordinates, proper motion, and parallax are from GAIA DR3 release
Spectroscopic TA clears with the PSA in the ETC: COS.sa.1530325DX-CHAJ2000Timing link suitability includes constraints ([Group (1C 1D 1S) Within 1.0 days])The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode./Users/rplesha/Box/ullyses_tech/ullyses_proposals/survey_c29/16599/OP-cache/ULLYSES_16599-v1C.xmlvstatus; 1C; HD-104237E; P/COS approved for submission; P/RP 30/09/21 ; internal review complete ; P/DJS 30/09/21
vcheck; Enter targ name & Inst. & Resp. Sci.; HD-104237E ; COS ; RP
vcheck; ETC numbers entered in APT?; Yes
vcheck; Any screening violations?; No
vcheck; M-dwarf check complete and added to box folder?; Yes...
PSA: COS.sp.1532254
Global count rate: 1,421.82 counts/s
Brightest pixel: 0.012 counts /s at 1302.53 A
vcheck; S/N ETC calcs done & documented?; Yes
vcheck; Field images checked & saved?; Yes
vcheck; Selected ACQ strategy?; Offset target PEAKD & PEAKXD
vcheck; Possible ACQ or Sci spoilers?; Yes. HD104237D ~4" away. M3 star
vcheck; Field BOT clear?; No, but everything is cleared for the settings we are using...
BOA (science): COS.sp.1530431
PSA (science): COS.sa.1530014
PSA (acq): COS.sa.1530325
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; 1C, 1D, 1S within 1 days
vcheck; phase constraint for ground based observations added?; N/A
vcheck; BETWEENS for coordinated observations added?; Yes
vcheck; Is visit ready for int. review?; Yes
Allocated COS orbits = 5(Tic-Visit
:proposal-id 16599
:visit-id "1C"
:proposal-version -1
:trans-version "20210514"
:date "04-Nov-2021 17:45:07.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 3
:saa-model "31"
:si-bright-earth-limb-angle 20.0
:data-volume 391472
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 16599
:visit-id "1C"
:obset-id "1C"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 16599
:visit-id "1C"
:orbit-number 1
:pcs-time 393
:si-vis-utilization 2615
:al-overhead-at-end 0
:internal-dur-at-end 67
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3008
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 16599
:visit-id "1C"
:orbit-number 2
:pcs-time 392
:si-vis-utilization 2616
:al-overhead-at-end 0
:internal-dur-at-end 95
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3008
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 16599
:visit-id "1C"
:orbit-number 3
:pcs-time 392
:si-vis-utilization 2616
:al-overhead-at-end 0
:internal-dur-at-end 391
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3008
:pcs-gap 0
)true30Because of M-dwarf flaring rules, a offset target acq is used. We are using a spectroscopic acq because the offset target is too bright to be observed with the PSA, so we do not want to have to worry about the difference in the sky of the BOA and PSA.
ETC calculations were done to obtain a S/N of 40 using a HST/STIS G140L spectrum of HD-104237.Because of M-dwarf flaring rules, a offset target acq is used. We are using a spectroscopic acq because the offset target is too bright to be observed with the PSA, so we do not want to have to worry about the difference in the sky of the BOA and PSA.
ETC calculations were done to obtain a S/N of 40 using a HST/STIS G140L spectrum of HD-104237.Because of an M-dwarf in the field, only G130M/1222 can be used with COS.
We aim to get a total S/N of 10/resel at the peak of the N V line at 1239 A.
Additional observations will be done with STIS/G140L to obtain the remaning goals of S/N of 20/resel at the peak of the C IV line at 1549 A.
Updated Calculations:
COS.sp.1530070 for the exposure time.
global countrate (brightest segment): 60.218 cts/s (FUVA)
brightest pixel: 0.009 cts/s/pix at 1301.98 A
S/N ~ 10 at 1239A
COS.sp.1530071 for bright object checks & buffer times
global countrate (brightest segment): 136.675 cts/s (FUVA)
brightest pixel: 0.014 cts/s/pix at 1301.98 A
Buffer fill time = 12,536s * (2/3) =8357.33, so anything less is fine; using 1500 to be safe
COS.sp.1530073 for M-dwarf clearing
global countrate (brightest segment): 899.888 cts/s (FUVA)
brightest pixel: 0.011 cts/s/pix at 1302.53 A
No warnings, so we are safe to observe with 1222 even if there is an M-dwarf flareBecause of an M-dwarf in the field, only G130M/1222 can be used with COS.
We aim to get a total S/N of 10/resel at the peak of the N V line at 1239 A.
Additional observations will be done with STIS/G140L to obtain the remaning goals of S/N of 20/resel at the peak of the C IV line at 1549 A.
Updated Calculations:
COS.sp.1530070 for the exposure time.
global countrate (brightest segment): 60.218 cts/s (FUVA)
brightest pixel: 0.009 cts/s/pix at 1301.98 A
S/N ~ 10 at 1239A
COS.sp.1530071 for bright object checks & buffer times
global countrate (brightest segment): 136.675 cts/s (FUVA)
brightest pixel: 0.014 cts/s/pix at 1301.98 A
Buffer fill time = 12,536s * (2/3) =8357.33, so anything less is fine; using 1500 to be safe
COS.sp.1530073 for M-dwarf clearing
global countrate (brightest segment): 899.888 cts/s (FUVA)
brightest pixel: 0.011 cts/s/pix at 1302.53 A
No warnings, so we are safe to observe with 1222 even if there is an M-dwarf flareBecause of an M-dwarf in the field, only G130M/1222 can be used with COS.
We aim to get a total S/N of 10/resel at the peak of the N V line at 1239 A.
Additional observations will be done with STIS/G140L to obtain the remaning goals of S/N of 20/resel at the peak of the C IV line at 1549 A.
Updated Calculations:
COS.sp.1530070 for the exposure time.
global countrate (brightest segment): 60.218 cts/s (FUVA)
brightest pixel: 0.009 cts/s/pix at 1301.98 A
S/N ~ 10 at 1239A
COS.sp.1530071 for bright object checks & buffer times
global countrate (brightest segment): 136.675 cts/s (FUVA)
brightest pixel: 0.014 cts/s/pix at 1301.98 A
Buffer fill time = 12,536s * (2/3) =8357.33, so anything less is fine; using 1500 to be safe
COS.sp.1530073 for M-dwarf clearing
global countrate (brightest segment): 899.888 cts/s (FUVA)
brightest pixel: 0.011 cts/s/pix at 1302.53 A
No warnings, so we are safe to observe with 1222 even if there is an M-dwarf flareTiming link suitability includes constraints ([Group (1C 1D 1S) Within 1.0 days])The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode./Users/rplesha/Box/ullyses_tech/ullyses_proposals/survey_c29/16599/OP-cache/ULLYSES_16599-v1D.xmlvstatus; 1C; HD-104237E; P/COS approved for submission; P/RP 30/09/21 ; internal review complete ; P/DJS 30/09/21
vcheck; Enter targ name & Inst. & Resp. Sci.; HD-104237E ; COS ; RP
vcheck; ETC numbers entered in APT?; Yes
vcheck; Any screening violations?; No
vcheck; M-dwarf check complete and added to box folder?; Yes...
PSA: COS.sp.1532254
Global count rate: 1,421.82 counts/s
Brightest pixel: 0.012 counts /s at 1302.53 A
vcheck; S/N ETC calcs done & documented?; Yes
vcheck; Field images checked & saved?; Yes
vcheck; Selected ACQ strategy?; Offset target PEAKD & PEAKXD
vcheck; Possible ACQ or Sci spoilers?; Yes. HD104237D ~4" away. M3 star
vcheck; Field BOT clear?; No, but everything is cleared for the settings we are using...
BOA (science): COS.sp.1530431
PSA (science): COS.sa.1530014
PSA (acq): COS.sa.1530325
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; 1C, 1D, 1S within 1 days
vcheck; phase constraint for ground based observations added?; N/A
vcheck; BETWEENS for coordinated observations added?; Yes
vcheck; Is visit ready for int. review?; Yes
Allocated COS orbits = 5(Tic-Visit
:proposal-id 16599
:visit-id "1D"
:proposal-version -1
:trans-version "20210514"
:date "30-Sep-2021 12:08:12.0"
: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 252304
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 16599
:visit-id "1D"
:obset-id "1D"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 16599
:visit-id "1D"
:orbit-number 1
:pcs-time 393
:si-vis-utilization 2615
:al-overhead-at-end 0
:internal-dur-at-end 67
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3008
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 16599
:visit-id "1D"
:orbit-number 2
:pcs-time 392
:si-vis-utilization 2616
:al-overhead-at-end 0
:internal-dur-at-end 391
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3008
:pcs-gap 0
)true20Because of M-dwarf flaring rules, a offset target acq is used. We are using a spectroscopic acq because the offset target is too bright to be observed with the PSA, so we do not want to have to worry about the difference in the sky of the BOA and PSA.
ETC calculations were done to obtain a S/N of 40 using a HST/STIS G140L spectrum of HD-104237.Because of M-dwarf flaring rules, a offset target acq is used. We are using a spectroscopic acq because the offset target is too bright to be observed with the PSA, so we do not want to have to worry about the difference in the sky of the BOA and PSA.
ETC calculations were done to obtain a S/N of 40 using a HST/STIS G140L spectrum of HD-104237.Because of an M-dwarf in the field, only G130M/1222 can be used with COS.
We aim to get a total S/N of 10/resel at the peak of the N V line at 1239 A.
Additional observations will be done with STIS/G140L to obtain the remaning goals of S/N of 20/resel at the peak of the C IV line at 1549 A.
Updated Calculations:
COS.sp.1530070 for the exposure time.
global countrate (brightest segment): 60.218 cts/s (FUVA)
brightest pixel: 0.009 cts/s/pix at 1301.98 A
S/N ~ 10 at 1239A
COS.sp.1530071 for bright object checks & buffer times
global countrate (brightest segment): 136.675 cts/s (FUVA)
brightest pixel: 0.014 cts/s/pix at 1301.98 A
Buffer fill time = 12,536s * (2/3) =8357.33, so anything less is fine; using 1500 to be safe
COS.sp.1530073 for M-dwarf clearing
global countrate (brightest segment): 899.888 cts/s (FUVA)
brightest pixel: 0.011 cts/s/pix at 1302.53 A
No warnings, so we are safe to observe with 1222 even if there is an M-dwarf flareBecause of an M-dwarf in the field, only G130M/1222 can be used with COS.
We aim to get a total S/N of 10/resel at the peak of the N V line at 1239 A.
Additional observations will be done with STIS/G140L to obtain the remaning goals of S/N of 20/resel at the peak of the C IV line at 1549 A.
Updated Calculations:
COS.sp.1530070 for the exposure time.
global countrate (brightest segment): 60.218 cts/s (FUVA)
brightest pixel: 0.009 cts/s/pix at 1301.98 A
S/N ~ 10 at 1239A
COS.sp.1530071 for bright object checks & buffer times
global countrate (brightest segment): 136.675 cts/s (FUVA)
brightest pixel: 0.014 cts/s/pix at 1301.98 A
Buffer fill time = 12,536s * (2/3) =8357.33, so anything less is fine; using 1500 to be safe
COS.sp.1530073 for M-dwarf clearing
global countrate (brightest segment): 899.888 cts/s (FUVA)
brightest pixel: 0.011 cts/s/pix at 1302.53 A
No warnings, so we are safe to observe with 1222 even if there is an M-dwarf flare/Users/rplesha/Box/ullyses_tech/ullyses_proposals/survey_c29/16599/OP-cache/ULLYSES_16599-v1S.xmlTiming link suitability includes constraints ([Group (1C 1D 1S) Within 1.0 days])The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.vstatus; 1S; HD-104237E; S/STIS approved for submission; P/RP 30/09/21 ; internal review complete; S/DW 29/09/21
vcheck; Enter targ name & Inst. & Resp. Sci.; HD-104237E ; STIS ; RP
vcheck; ETC numbers entered in APT?; Yes
vcheck; Any screening violations?; No
vcheck; M-dwarf check complete and added to box folder?; Yes
FUV MAMA: STIS.sp.1532255
NUV MAMA: STIS.sp.1532256
vcheck; S/N ETC calcs done & documented?; Yes
vcheck; Field images checked & saved?; Yes
vcheck; Selected ACQ strategy?; Yes
vcheck; Possible ACQ or Sci spoilers?; Yes. HD104237D ~4" away. M3 star
vcheck; Field BOT clear?; No...
NUV MAMA: HD-104237A does not clear the field; STIS.sp.1537639
An orient was set to avoid ~6" away from HD-104237A, which means we cannot constrain the slit to also include the M-dwarf.
HD-104237A does clear for the FUV MAMA using previous STIS/G140L data: STIS.sp.1530432
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; 1C, 1D, 1S within 1 days
vcheck; phase constraint for ground based observations added?; N/A
vcheck; BETWEENS for coordinated observations added?; Yes & additional ORIENT to avoid HD-104237A in the slit
vcheck; Is visit ready for int. review?; Yes
Allocated STIS orbits = 3(Tic-Visit
:proposal-id 16599
:visit-id "1S"
:proposal-version -1
:trans-version "20210514"
:date "30-Sep-2021 12:08:14.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 3
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 917024
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 16599
:visit-id "1S"
:obset-id "1S"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 16599
:visit-id "1S"
:orbit-number 1
:pcs-time 393
:si-vis-utilization 2615
:al-overhead-at-end 0
:internal-dur-at-end 263
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3008
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 16599
:visit-id "1S"
:orbit-number 2
:pcs-time 0
:si-vis-utilization 2616
:al-overhead-at-end 0
:internal-dur-at-end 178
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3008
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 16599
:visit-id "1S"
:orbit-number 3
:pcs-time 0
:si-vis-utilization 2616
:al-overhead-at-end 116
:internal-dur-at-end 1231
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3008
:pcs-gap 0
)true30With a 0.5s exposure we get a S/N of 182.0992
The bright object check for this target acq was done in ETC run STIS.ta.1529279, which had a saturation time of 0.78s, so we want to stay under that time because we will get plenty of S/N with a 0.5s exposure.Because of an M-dwarf in the field, we are observing with G140L instead of COS/G160M.
We aim to get a total S/N of 10/resel at the peak of the N V line at 1239 A and S/N of 20/resel at the peak of the C IV line at 1549 A.
Additional observations will be done with STIS/G140L to obtain the remaning goals of S/N of 20/resel at the peak of the C IV line at 1549 A.
ETC Calculations:
STIS.sp.1531287 for the exposure time.
global countrate: 278.636 cts/s
brightest pixel: 0.162 cts/s/pix at 1304.70 A
S/N ~ 12 at 1239A & S/N ~22 at 1549A
STIS.sp.1531288 for bright object checks & buffer times
global countrate: 362.029 cts/s
brightest pixel: 0.690 cts/s/pix at 1304.70 A
Buffer fill time = 5,524.42s * 0.80 = 4419.5, so using half exposure time instead (1095)
STIS.sp.1532255 for M-dwarf clearing
global countrate: 3725.156 cts/s
brightest pixel: 71.778 cts/s/pix at 1548.3 A
A global count rate of ~3700 is less than the limit of 120,000 cnts/s, so we are safe to observe even if there is an M-dwarf flareBecause of an M-dwarf in the field, we are observing with G140L instead of COS/G160M.
We aim to get a total S/N of 10/resel at the peak of the N V line at 1239 A and S/N of 20/resel at the peak of the C IV line at 1549 A.
Additional observations will be done with STIS/G140L to obtain the remaning goals of S/N of 20/resel at the peak of the C IV line at 1549 A.
ETC Calculations:
STIS.sp.1531287 for the exposure time.
global countrate: 278.636 cts/s
brightest pixel: 0.162 cts/s/pix at 1304.70 A
S/N ~ 12 at 1239A & S/N ~22 at 1549A
STIS.sp.1531288 for bright object checks & buffer times
global countrate: 362.029 cts/s
brightest pixel: 0.690 cts/s/pix at 1304.70 A
Buffer fill time = 5,524.42s * 0.80 = 4419.5, so using half exposure time instead (1095)
STIS.sp.1532255 for M-dwarf clearing
global countrate: 3725.156 cts/s
brightest pixel: 71.778 cts/s/pix at 1548.3 A
A global count rate of ~3700 is less than the limit of 120,000 cnts/s, so we are safe to observe even if there is an M-dwarf flareBecause of an M-dwarf in the field, we are observing with G140L instead of COS/G160M.
We aim to get a total S/N of 10/resel at the peak of the N V line at 1239 A and S/N of 20/resel at the peak of the C IV line at 1549 A.
Additional observations will be done with STIS/G140L to obtain the remaning goals of S/N of 20/resel at the peak of the C IV line at 1549 A.
ETC Calculations:
STIS.sp.1531287 for the exposure time.
global countrate: 278.636 cts/s
brightest pixel: 0.162 cts/s/pix at 1304.70 A
S/N ~ 12 at 1239A & S/N ~22 at 1549A
STIS.sp.1531288 for bright object checks & buffer times
global countrate: 362.029 cts/s
brightest pixel: 0.690 cts/s/pix at 1304.70 A
Buffer fill time = 5,524.42s * 0.80 = 4419.5, so using half exposure time instead (1095)
STIS.sp.1532255 for M-dwarf clearing
global countrate: 3725.156 cts/s
brightest pixel: 71.778 cts/s/pix at 1548.3 A
A global count rate of ~3700 is less than the limit of 120,000 cnts/s, so we are safe to observe even if there is an M-dwarf flarehd104237e_lya2_etc_scaled_pAV0.50.txt; stis,nuvmama,g230l,c2376,52x2,mjd#59670
Input file: targets_up_to_May30-2022.csv
Spectral type: K5.5 ; A_V: 1.0 ; Distance (pc): 114
M*: 0.9 ; log(dm/dt): -9.07
For exptime=185.8 s, spectral region:
2800.0 +- 15.0 A achieves SNR=20.0 / 2-pix-resel
A factor of 2.0 has been applied to the exptime in each exposure.
global countrate (brightest segment): 2359.7 cts/s/segment
brightest pixel: 0.446 cts/s/pix at 2796.8 A
Calculation performed 2021-06-18T15:05:41, v0.24
STIS.sp.1529572 for the exposure time.
global countrate: 2367.777 cts/s
brightest pixel: 0.446 cts/s/pix at 2796.8 A
S/N ~ 18 at 2800A
STIS.sp.1529574 for bright object checks & buffer times
global countrate: 2769.19 cts/s
brightest pixel: 4.216 cts/s/pix at 2796.80 A
Buffer fill time = 722.23s * 0.80 = 577.784, so using half exposure time instead (186)
STIS.sp.1532256 for M-dwarf clearing
global countrate: 92,558.916 cts/s
brightest pixel: 53.941 cts/s/pix at 2692.80 A
A global count rate of ~90,000 is less than the limit of 120,000 cnts/s, so we are safe to observe even if there is an M-dwarf flarehd104237e_lya2_etc_scaled_pAV0.50.txt; stis,ccd,g430l,c4300,52x2,mjd#59670
WARNING: operating mode = ACCUM
Input file: targets_up_to_May30-2022.csv
Spectral type: K5.5 ; A_V: 1.0 ; Distance (pc): 114
M*: 0.9 ; log(dm/dt): -9.07
For exptime=50.2 s, n_reads=2, spectral region:
4000.0 +- 5.0 A achieves SNR=20.0 / 2-pix-resel
A factor of 2.0 has been applied to the exptime in each exposure.
global countrate (brightest segment): 46110.2 cts/s/segment
brightest pixel: 23.498 cts/s/pix at 4560.5 A
Calculation performed 2021-06-18T15:05:41, v0.24hd104237e_lya2_etc_scaled_pAV0.50.txt; stis,ccd,g750l,c7751,52x2,mjd#59670
WARNING: operating mode = ACCUM
Input file: targets_up_to_May30-2022.csv
Spectral type: K5.5 ; A_V: 1.0 ; Distance (pc): 114
M*: 0.9 ; log(dm/dt): -9.07
For exptime=3.3 s, n_reads=2, spectral region:
5700.0 +- 5.0 A achieves SNR=20.0 / 2-pix-resel
A factor of 2.0 has been applied to the exptime in each exposure.
global countrate (brightest segment): 127415.6 cts/s/segment
brightest pixel: 242.239 cts/s/pix at 6563.9 A
Calculation performed 2021-06-18T15:05:41, v0.24