0Assigned ID: 664
----- Attempting Submission 1 (Fri Apr 05 19:38:07 GMT 2019) -----
HST Phase I Proposal 664 (GalBStarsHST27.apt) successfully submitted.
Receipt: # 664-1
----- Attempting Submission 2 (Fri Apr 05 23:11:51 GMT 2019) -----Now includes visit 60, a partial duplicate of visit 50 (which was a duplicate of visit 10), but with changes to account for partial success of visit 50
Removed successful c1817 observation.
Changed c1222 observation to only repeat failed FP-POS=4 exposure.
Changed to SCHED=100.
Expanded NUV exposures to fill available SCHED100 visibility in first orbit,
but made only modest increases in FUV exposures to keep within this proposal's phase 2 S/N requirements
and limit charge extraction from the FUV detectors, even though this leaves a good bit of unused time in the 2nd orbit.
As we discussed with our CS, Andrew Fox, we made some changes in the NUV grating cenwave selection from what was in the phase 1.
This includes substituing the 1850 CENWAVe for 1835, and occaisionallly using more of the NUV settings than we had originally proposed to use.
This counts as a minor change and has already been approved by the CS.
Note that there appear to be some issues with the finding charts. Several come up blank, and for a couple of others (e.g., LS 5130 and CPD -57 3485),
the stellar image in the finding chart is significantly misaligned despite using GAIA coordinates.
The alignment is good for these coordinates when displaying 2MASS images in Aladin, so perhaps there are issues with the astrometry used in the GSC2 based finding chart images?
This should be fixed.-1967712607----- Attempting Submission 1 (Wed Jul 24 21:09:11 GMT 2019) -----
----- Attempting Submission 2 (Wed Mar 25 16:14:30 GMT 2020) -----The Galactic Abundance Gradient for the Fe Group Elements in Early B StarsWe propose HST spectroscopic observations of twelve sharp-lined early B main-sequence stars with galactocentric distances ranging from 3-14 kpc in order to determine the metallicity gradient for the Fe group elements (Ti, V, Cr, Mn, Fe, Co, Ni) in our galaxy. This will be the first attempt to establish abundance gradients for all of the Fe-peak elements found in these young stars, that were formed <100 Myr ago. The result will be an assessment of the chemical evolution of our galaxy. Whereas the light elements are mostly delivered to the ISM by core-collapse supernovae (CCSNe), the Fe group elements are believed to primarily come from low/intermediate mass binaries containing white dwarfs that undergo SNe Ia explosions. According to some references, a single SNe Ia can deliver as much as 0.5 solar masses of pure Fe and Mn to the ISM compared with about 0.07 solar masses from a CCSNe. The older stellar populations were formed from an ISM that was enriched primarily by CCSNe, but the Fe group elements in B stars probably owe their origin mostly to SN Ia. Recently there has been a great deal of interest in using the observed Mn/Fe ratio to determine the progenitors of SNe Ia. Since the SNe models predict that Mn/Fe varies with metallicity, a good determination of the Mn abundance across our galaxy would also be useful for SN science. For each Fe group element we will determine its abundance relative to H and Fe. The unique spectra will have legacy value, as strong lines from the Fe group elements (except for a very few features of Fe itself) are found only in the FUV/NUV. Both COS and STIS will be used. The analysis will be carried through with TLUSTY/SYNSPEC.The twelve program stars (cf. Table 1) fall into two brightness categories. The more distant B stars, most of which are quite reddened, can be observed with COS (G130M, G185M gratings), but some of the brighter stars need to be observed with STIS (E140M, E230M gratings) as they exceed the COS bright limit. COS will provide spectra of higher S/N but at a slightly lower spectral resolution than STIS.
COS observations: LS 5130, DSH279-8, DSH393-3, NGC6611-ESL30, NGC3293- ESL43, Rup44-27, S285-6, S289-13, and ALS 45 will be observed with COS. The implemen- tation of the COS2025 initiative makes it somewhat more costly to get the best resolution and S/N over the full range of the COS FUV detector. While using the 1291 setting would obtain the best resolution over our desired wavelength range, having only 2 FP-POS posi- tions available with this setting would limit the obtainable S/N and make it more difficult to identify and remove detector artifacts. The longer G130M settings are now allowed only with the B segment, limiting wavelength coverage. We've chosen to use the COS G130M/1222 + G160M/1533 to maximize the S/N and wavelength coverage in the FUV region, although this means accepting somewhat lower spectra resolution in the 1300-1500 angstrom range. For our ETC calculations we assume Kurucz models of the spectral type and E(B-V) as specified in Table 2, normalizing to a UV measurement where available and to V otherwise. We targeted a baseline S/N of 30:1 at 1350 Angstroms for the 1222 setting, and at 1550 for the 1533 setting. These FUV observations should provide S/N > 30:1 between 1250 and 1550 A, covering numerous Ti iii, V iii, Cr iii, and Mn iiilines, and > 20:1 over the whole range from about 1130 to 1700 A, with lower S/N down to 1070 A. In addition, we will use the G185M grating with central wavelengths of 1786 and 1817 to extend almost complete cover- age at S/N 30 up to 1933 A; this adds observations of many critical Co iii , N iii , Ni iii , and many strong Fe iii features. For some of our brighter targets where there is additional time in an orbit, we will also use the 1850 setting to fill in the remaining gaps in the NUV range and extend observations up to 1968 A. For a few of our fainter targets, we will reduce the baseline S/N requirements to 20:1-25:1 and/or omit the 1850 setting to keep down the overall orbit request. These cases are noted in Table 2.
STIS observations: The STIS E140M and E230M gratings will be used to observe CD-41 11034, HD 14476, and BD -21 1882 from 1150-2400 A, and will cover all of the spectral features/species mentioned above. The 0.2 x 0.2 arcsec aperture will be employed to eliminate light contamination from nearby cluster stars.
For ETC calculations, interpolate Kurucz SED to adopted spectral type, apply best estimate E(B-V), and then normalize to the available measurement closest to the observation band.
Exception are stars with IUE LGAP data, where the IUE observations are used instead. Details and raferences for the assumed ETC input parameters are discussed in the comments for each target.PI Geraldine Peters has been an expert on B stars and interacting binaries with B-type primaries since the 1970s. Her specializations include determining photospheric abundances and modeling activity in Be and Be-binary stars. She has presented several invited talks at IAU symposia and other meetings, published about 150 papers in refereed journals and major conference proceedings, written an invited chapter in the Planets, Stars, and Stellar Systems series, and co-edited an IAUS Proceedings volume.
Co-Is Jean-Claude Bouret and Thierry Lanz are experts in the modeling of the atmosphere and winds of massive stars with the state-of-the-art codes CMFGEN, and TLUSTY. These codes are crucial tools for analyses of UV data to determine the stars fundamental parameters, especially surface abundances at the core of this proposal.'
Co-I Charles Proffitt has worked for many years as an instrument scientist supporting the HST COS and STIS spectrographs, and now supports the JWST NIRSpec Instrument. He is an expert on observations with COS and STIS and has published papers on the abundances of boron and of the s-process elements in early B stars.Stellar Physics6falsefalsetruefalsefalsefalsefalseSUPPORTEDSTARB0-B2 V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
Updated to Gaia ICRS coordinates as given in SIMBAD.
Default SIMBAD name = LS IV -13 88
Has STIS G230M 2095 observations to normalize NUV flux (data sets O63O01*); STIS TA image in F28X50LP shows only one source, as does 2MASS image, despite apparent confusion in GSC2 image and finding chart.
Reference for spectral type of B2IV is Smartt et al 2001 A&A 367, 86 who gives
Teff=21200, logg=3.5, vsini=35km/s, and B-V=0.24, implying E(B-V)=0.45
The "unknown" star in BOT listings is the target itself. It is listed as "not a star" in GSC2, although it appears to be a point source in 2MASS and STIS ACQ images.J2000J2000FLAMHST(2050)=3.0e-14, SpT=B2IVSTARB0-B2 V-IVNOUpdated to GAIA Coordinates
[DSH2001] 279-8
Galex catalog lists NUV abmag of 13.02; applying local linearity correction gives a corrected mag of 12.668.
This causes GALEX BOT to flag as unsafe assuming it is an unreddened O5 star. But we know this is a B2 star, and even adopting B1 in the ETC without any extinction shows this is safe (COS.sp.1365335), while adopted B2 and the estimated E(B-V) gives the ETC results linked in each exposure.
Geier et al 2019 estimates E(B-V)=0.1282 from Gaia data
Munn et al 2003 A&A 419, 713 gives V=12.48, B-V=-0.127, T=20000, logg=4.5, vsini<10
So adopt B2V spectral type and E(B-V) about 0.1TYC-8357-911-1J2000J2000Galex NUV (Uncorrected)=13.02, Galex NUV(corrected for non-linearity)=12.668, V(TYC)=12.1STARB0-B2 V-IVNOSimbad Name [DSH99] 393-3
Munn et al 2003 A&A 419, 713 found V=12.49, B-V=0.214, vsini=30, Teff=23000K, log g = 4.5,
implies SpT=B1.6V, B-V = -0.24, E(B-V) about 0.45
3 unknowns in BOT - look up in GSC 2.4.1 at http://gsss.stsci.edu/webservices/GSC2/WebForm.aspx
All are very faint
S8BJ192511, Gaia G =17.11, Nplate=16.9283
S8BJ192559, Gaia G = 18.13, Nplate = 17.6085
S8BJ192571, Gaia G = 17.76, Nplate = 17.3887
N plate is very close to Cousins I bandJ2000J2000SpT=B1.5VSTARB0-B2 V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
Coordinates updated to Gaia DR2 numbers in SIMBAD
SpT=B2V
Only object flagged by BOT is the target. See detailed ETC calculations
Trundle et al found B1.5V, implying E(B-V)=0.61 with SIMBAD B, V values
http://vizier.u-strasbg.fr/viz-bin/VizieR-3?-source=J/A%2bA/471/625/starsNGC6611-ESL30J2000J2000STARB0-B2 V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
PPM coordinates are listed in SIMBAD; we have substituted 2MASS coordinates from II/246/out as these should be significantly more accurate and proper motion, which PPM incluldes but 2MASS does not, should be small
Cl* NGC 6231 SBL 403
IUE spectra SWP19380 + LWR15416
Updated coordinates to Gaia DR2. (For some reason SIMBAD doesn't pick up the GAIA ID and measurements for this one, but the star is clearly in Gaia.
GSC2 BOT returns no stars, so as substitute for default BOT look for other 2MASS and Gaia entries within 10" of target and use these magnitudes to check safety
Target has J=8.796 and J-K=+0.041
field star at 7.07" has J=13.957 and J-K=+0.814
field star at 8.00" has J=14.479 and J=K=+0.981
GAIA search finds one closer star to target.
Target has Gmag=9.28
field star at 1.36" has Gmag=12.06 (no color info, but would have been in IUE LGAP aperture, so flux already included)
field star at 7.60" has Gmag=16.38
field star at 7.60" had Gmag=19.15
field star at 9.06" has Gmag=19.61
field star at 9.55" has Gmag=19.55
field star at 10.02"has Gmag=18.67
So all close stars are are much fainter than the target.2MASS-J16541130-4148538NGC6231-SBL403J2000J2000STARB3-B5 V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
Updated with GAIA DR2 coordinates from SIMBAD
BOT lists the target itself as unknown, but otherwise clear - see detailed ETC calcualtions for each exposureJ2000J2000SpT=B3VSTARB0-B2 V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
2MASS ICRS coordinates, also a TYCHO target
Cl* NGC 884 LAV 2049
BOT with GALEX shows target safe, no other concerns
V=8.75, B1V, E(B-V)=0.552 from Currie et al, 2010
http://vizier.u-strasbg.fr/viz-bin/VizieR-3?-source=J/ApJS/186/191/table3
V=8.776, B0.5III, E(B-V)=0.600 from Wegner 2003
http://vizier.u-strasbg.fr/viz-bin/VizieR-3?-source=J/AN/324/219/table1
SIMBAD: B=9.13, V=8.1914, B1.5I2MASS-J02221695+5716189NGC884-LAV2049J2000J2000FLAM_IUE(1450)=1.75e-12, V=8.1914, SpT=B1IVSTARB0-B2 V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
Updated to GAIA DR2 coordinates taken from SIMBAD
BOT shows target as safe with no concerns
V=10.32, B2IV, E(B-V)=0.33, vsini=17km/s from Garmany et al 2015, AJ, 150, 41
http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/AJ/150/41NGC2367-3J2000J2000SpT=B2IVSTARB0-B2 V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
Coordianates updated to GAIA DR2 as taken from SIMBAD
Cl Ruprecht 44 27
BOT only flags target. See detailed ETC calculations.
V=11.91, B0.5V E(B-V)=0.63, vsini=4km/s, from Garmany et al 2015, AJ, 150, 41
http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/AJ/150/41RUPRECHT44-27J2000J2000SpT=B0.5V, U=11.72STARB0-B2 V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
Updated to GAIA DR2 coordinates in SIMBAD
BOT only flags target. See detailed ETC calcuations using IUE spectra
V=11.17, E(B-V)=0.50, B0V, vsin(i)=6 km/s from Garmany et al 2015, AJ, 150, 41
http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/AJ/150/41
But primary ETC input is IUE swp35501 + lwp07914
For LWP 07914 used 2X SMAP to patch saturated wavelengths in LGAP.ALS9209J2000J2000FLAMIUE(1300)=5.0e-13, U=11.66, SpT=B0.5VSTARB0-B2 V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
MFJ SH 2-289 13
BOT only flags target. See detailed ETC calcuations.
Adopted E(B-V)=0.50, SpT=B0.5V, v sin(i)=4km/s from Garmany et al 2015, AJ, 150, 41
http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/AJ/150/41MFJ-SH-2-289-13TYC-4812-3777-1J2000J2000U=10.8, SpT=B0.5VSTARB0-B2 V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
Updated to GAIA DR2 coordinates from SIMBAD
Bo1-SLS45
BOT clears field, but see detailed ETC calcuations.
Adopted V=12.59 B1.5V E(B-V)=0.49, v sin(i)=11km/s, from Garmany et al 2015, AJ, 150, 41
http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/AJ/150/41BO1-SLS45J2000J2000U=12.29, SpT=B1.5VCOS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/NUVSpectroscopicNoNoG185M1786COS/NUVSpectroscopicNoNoG185M1817COS/NUVSpectroscopicNoNoG185M1835COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/NUVSpectroscopicNoNoG185M1786COS/NUVSpectroscopicNoNoG185M1817COS/NUVSpectroscopicNoNoG185M1835COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/NUVSpectroscopicNoNoG185M1786COS/NUVSpectroscopicNoNoG185M1817COS/NUVSpectroscopicNoNoG185M1835COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/NUVSpectroscopicNoNoG185M1786COS/NUVSpectroscopicNoNoG185M1817COS/NUVSpectroscopicNoNoG185M1835STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/NUV-MAMASpectroscopicNoNoE230M1978COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/NUVSpectroscopicNoNoG185M1786COS/NUVSpectroscopicNoNoG185M1817COS/NUVSpectroscopicNoNoG185M1835STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/NUV-MAMASpectroscopicNoNoE230M1978STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/NUV-MAMASpectroscopicNoNoE230M1978COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/NUVSpectroscopicNoNoG185M1786COS/NUVSpectroscopicNoNoG185M1817COS/NUVSpectroscopicNoNoG185M1835COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG160M1533COS/NUVSpectroscopicNoNoG185M1786COS/NUVSpectroscopicNoNoG185M1817COS/NUVSpectroscopicNoNoG185M1835COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/NUVSpectroscopicNoNoG185M1786COS/NUVSpectroscopicNoNoG185M1817COS/NUVSpectroscopicNoNoG185M1835COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/NUVSpectroscopicNoNoG185M1786COS/NUVSpectroscopicNoNoG185M1817COS/NUVSpectroscopicNoNoG185M1835The scheduling data was generated by CASM 28.0.CASM was run in Phase II mode./private/var/folders/c1/kkl4zqqs11g637_3q3f43f2m000400/T/OPVisit431888038374673759.xmlThe "unknown" star in BOT listings is the target itself. It is listed as "not a star" in GSC2, although it appears to be well resolved in 2MASS images1584550028000264.8(Tic-Visit
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)true30Spectra=B2V, E(B-V)=0.46, norm F2050=3.5e-14S/N=27@1817, Spectra=B2V, E(B-V)=0.46, norm F2050=3.5e-14S/N=26@1817, Spectra=B2V, E(B-V)=0.46, norm F2050=3.5e-14S/N=30@1350, Spectra=B2V, E(B-V)=0.46, norm F2050=3.5e-14S/N=26@1545, Spectra=B2V, E(B-V)=0.46, norm F2050=3.5e-14The scheduling data was generated by CASM 28.0.CASM was run in Phase II mode./private/var/folders/c1/kkl4zqqs11g637_3q3f43f2m000400/T/OPVisit16697981350137778280.xml1584651622000268.0(Tic-Visit
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)true20Spectra=B2V, E(B-V)=0.1, B=12.1Spectra=B2V, E(B-V)=0.1, B=12.1
Galex catalog lists NUV abmag of 13.02; applying linearity correction gives a corrected mag of 12.668.
This causes BOT to flag as unsafe assuming an unreddened O5 star. But we know this is a B2 star, and even adopting B1 in the ETC without any extinction shows this is safe (COS.sp.1365335)Spectra=B2V, E(B-V)=0.1, Galex(NUV)=12.668
S/N=30 at 1700
Galex catalog lists NUV abmag of 13.02; applying linearity correction gives a corrected mag of 12.668.
This causes BOT to flag as unsafe assuming an unreddened O5 star. But we know this is a B2 star, and even adopting B1 in the ETC without any extinction shows this is safe (COS.sp.1365335)Spectra=B2V, E(B-V)=0.1, Galex(NUV)=12.668
S/N=34@1817
Galex catalog lists NUV abmag of 13.02; applying linearity correction gives a corrected mag of 12.668.
This causes BOT to flag as unsafe assuming an unreddened O5 star. But we know this is a B2 star, and even adopting B1 in the ETC without any extinction shows this is safe (COS.sp.1365335)Spectra=B2V, E(B-V)=0.1, B=12.1
Galex catalog lists NUV abmag of 13.02; applying linearity correction gives a corrected mag of 12.668.
This causes BOT to flag as unsafe assuming an unreddened O5 star. But we know this is a B2 star, and even adopting B1 in the ETC without any extinction shows this is safe (COS.sp.1365335)Spectra=B2V, E(B-V)=0.1, Galex(NUV)=12.668
Galex catalog lists NUV abmag of 13.02; applying local linearity correction gives a corrected mag of 12.668.
This causes GALEX BOT to flag as unsafe assuming it is an unreddened O5 star. But we know this is a B2 star, and even adopting B1 in the ETC without any extinction shows this is safe (COS.sp.1365335), while adpopting B2 and the estimated E(B-V) gives the ETC results linked in each exposure.
Munn et al 2003 A&A 419, 713 gives V=12.48, B-V=-0.127, T=20000, logg=4.5, vsini<10
So adopt B2V spectral type and E(B-V) about 0.1Spectra=B2V, E(B-V)=0.1, Galex(NUV)=12.668
S/N=25.8@1550
Galex catalog lists NUV abmag of 13.02; applying linearity correction gives a corrected mag of 12.668.
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)true30B2V, E(B-V)=0.31, V=12.45B2V, E(B-V)=0.31, V=12.45B2V, E(B-V)=0.31, V=12.45B2V, E(B-V)=0.31, V=12.45B2V, E(B-V)=0.31, V=12.45B2V, E(B-V)=0.31, V=12.45B2V, E(B-V)=0.31, V=12.45The scheduling data was generated by CASM 28.0.CASM was run in Phase II mode./private/var/folders/c1/kkl4zqqs11g637_3q3f43f2m000400/T/OPVisit13330700723750454920.xml1585332480000267.64222145251404(Tic-Visit
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)true30V=11.42, B1.5V, E(B-V)=0.61V=11.42, B1.5V, E(B-V)=0.61V=11.42, B1.5V, E(B-V)=0.61V=11.42, B1.5V, E(B-V)=0.61V=11.42, B1.5V, E(B-V)=0.61V=11.42, B1.5V, E(B-V)=0.61The scheduling data was generated by CASM 28.0.CASM was run in Phase II mode./private/var/folders/c1/kkl4zqqs11g637_3q3f43f2m000400/T/OPVisit10321291116379750601.xml1585704082000285.3284421564334(Tic-Visit
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)true10B1V, V=9.28, E(B-V)=0.43, F(2050)=3.5e-13B1V, V=9.28, E(B-V)=0.43
IUE spectra SWP19380 + LWR15416 have this target name listed by GO, but the IUE listed coordinates are off by ~15" so the data bases do not link these observations to this star despite it being listed as the target. These have mean F(2050) flux of 1.1e-12
STIS.sp.1366028 (e140m) + STIS.sp.1366029 (E230M 1978) give good S/N in 1000 s each.
Fitzpatrick 2007 used these IUE spectra to derive Teff=26418, logg=4.15, E(B-V)=0.42.
Normalizing to these parameters and optical V=9.275, gives very similar results STIS.sp.1366033 + STIS.sp.1366030 to using IUE spectra
THis suggests IUE observed the correct star despite the error in the listed coordinates. Remember IUE pointing was done using a visual finding image several arc-minutes in extent
GSC2 BOT returns no stars, so as substitute for default BOT look for other 2MASS and Gaia entries within 10" of target and use these magnitudes to check safety
Target has J=8.796 and J-K=+0.041
field star at 7.07" has J=13.957 and J-K=+0.814
field star at 8.00" has J=14.479 and J=K=+0.981
GAIA search finds one closer star to target.
Target has Gmag=9.28
field star at 1.36" has Gmag=12.06 (no color info, but would have been in IUE LGAP aperture, so flux already included)
field star at 7.60" has Gmag=16.38
field star at 7.60" had Gmag=19.15
field star at 9.06" has Gmag=19.61
field star at 9.55" has Gmag=19.55
field star at 10.02"has Gmag=18.67
So all close stars are are much fainter than the target.UE spectra SWP19380 + LWR15416 have this target name listed by GO, but the supplied coordinates are off by ~15" so the data bases do not link these observations to this star despite it being listed as the target. These have mean F(2050) flux of 1 1e-12
STIS.sp.1366028 (e140m) + STIS.sp.1366029 (E230M 1978) give good S/N in 1000 s each.
Fitzpatrick 2007 used these IUE spectra to derive Teff=26418, logg=4.15, E(B-V)=0.42.
Normalizing to these parameters and optical V=9.275, gives very similar results STIS.sp.1366033 + STIS.sp.1366030 to using IUE spectraThe scheduling data was generated by CASM 28.0.CASM was run in Phase II mode./private/var/folders/c1/kkl4zqqs11g637_3q3f43f2m000400/T/OPVisit13590278582953511262.xml(Tic-Visit
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)true20V=11.32 B3 V E(B-V)=0.31
ETC gives ACQ time of 1.3 secondsV=11.32 B3 V E(B-V)=0.31
ETC gives ACQ time of 1.3 secondsV=11.32 B3 V E(B-V)=0.31V=11.32 B3 V E(B-V)=0.31V=11.32 B3 V E(B-V)=0.31The scheduling data was generated by CASM 28.0.CASM was run in Phase II mode./private/var/folders/c1/kkl4zqqs11g637_3q3f43f2m000400/T/OPVisit10892455431536566785.xml158553984100033.93954912684791(Tic-Visit
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(Tic-Obset
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)true10V=8.19, Spec=B1V, E(B-V)=0.63IUE SWP52232
HD 14476, B1IV, F(1450)=1.5e-12, F(1700) = 1.4e-12
SIMBAD: B=9.13, V=8.1914, B1.5IThe scheduling data was generated by CASM 28.0.CASM was run in Phase II mode./private/var/folders/c1/kkl4zqqs11g637_3q3f43f2m000400/T/OPVisit9882213936945040167.xml(Tic-Visit
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(Tic-Obset
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(Tic-Orbit
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)true10V=10.31, B0.5V E(B-V)=0.33V=10.32, B2IV, E(B-V)=0.33V=10.32, B2IV, E(B-V)=0.33The scheduling data was generated by CASM 28.0.CASM was run in Phase II mode./private/var/folders/c1/kkl4zqqs11g637_3q3f43f2m000400/T/OPVisit2818157672260148780.xml158586435400086.21982211389349(Tic-Visit
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)
(Tic-Obset
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(Tic-Orbit
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(Tic-Orbit
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(Tic-Orbit
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)true30V=11.91, B0.5V E(B-V)=0.63, ETC gives 4 seconds for spectroscopic ACQ S/N=40V=11.91, B0.5V E(B-V)=0.63, ETC gives 4 seconds for spectroscopic ACQ S/N=40V=11.91, B0.5V E(B-V)=0.63,V=11.91, B0.5V E(B-V)=0.63V=11.91, B0.5V E(B-V)=0.63V=11.91, B0.5V E(B-V)=0.63V=11.91, B0.5V E(B-V)=0.63The scheduling data was generated by CASM 28.0.CASM was run in Phase II mode./private/var/folders/c1/kkl4zqqs11g637_3q3f43f2m000400/T/OPVisit17664550593063974006.xml158198596100073.238878842721(Tic-Visit
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)true20IUE swp35501 + lwp07914
In LWP 07914 used 2X SMAP to patch saturated wavelengths in LGAP.IUE swp35501 + lwp07914
In LWP 07914 used 2X SMAP to patch saturated wavelengths in LGAP.IUE swp35501 + lwp07914
In LWP 07914 used 2X SMAP to patch saturated wavelengths in LGAP.IUE swp35501 + lwp07914
In LWP 07914 used 2X SMAP to patch saturated wavelengths in LGAP.IUE swp35501 + lwp07914
In LWP 07914 used 2X SMAP to patch saturated wavelengths in LGAP.IUE swp35501 + lwp07914
In LWP 07914 used 2X SMAP to patch saturated wavelengths in LGAP.IUE swp35501 + lwp07914
In LWP 07914 used 2X SMAP to patch saturated wavelengths in LGAP.
ETC buffer time is only 123 seconds. Almost too bright for time-tag!!!The scheduling data was generated by CASM 28.0.CASM was run in Phase II mode./private/var/folders/c1/kkl4zqqs11g637_3q3f43f2m000400/T/OPVisit14896825127401825566.xml158176612400066.44523814368421(Tic-Visit
:proposal-id 15869
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:date "25-Mar-2020 11:57:23.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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)
(Tic-Obset
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(Tic-Orbit
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)true20V=11.35 B0.5V E(B-V)=0.50 IUE SWP33406, LWP13138V=11.35 B0.5V E(B-V)=0.50 IUE SWP33406, LWP13138V=11.35 B0.5V E(B-V)=0.50 IUE SWP33406, LWP13138V=11.35 B0.5V E(B-V)=0.50 IUE SWP33406, LWP13138V=11.35 B0.5V E(B-V)=0.50 IUE SWP33406, LWP13138Recommeded buffer time of 2/3 * 123 is too small
Almost too bright for time-tag, but we have IUE spectra so flux should be reliableThe scheduling data was generated by CASM 28.0.CASM was run in Phase II mode./private/var/folders/c1/kkl4zqqs11g637_3q3f43f2m000400/T/OPVisit3437109885839796594.xml158200064600089.74612305225372(Tic-Visit
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)
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)true30V=12.59 B1.5V E(B-V)=0.49V=12.59 B1.5V E(B-V)=0.49V=12.59 B1.5V E(B-V)=0.49 from Garmany et al 2015, AJ, 150, 141
http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/AJ/150/41V=12.59 B1.5V E(B-V)=0.49V=12.59 B1.5V E(B-V)=0.49V=12.59 B1.5V E(B-V)=0.49The scheduling data was generated by CASM 28.0.CASM was run in Phase II mode./Users/proffitt/Documents/research/15869/OP-cache/15869-flight-revised-p2-v50.xmlDuplicate of visit 10158440307100088.38740762825608(Tic-Visit
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)
(Tic-Obset
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(Tic-Orbit
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)
(Tic-Orbit
:proposal-id 15869
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)true20IUE swp35501 + lwp07914
In LWP 07914 used 2X SMAP to patch saturated wavelengths in LGAP.IUE swp35501 + lwp07914
In LWP 07914 used 2X SMAP to patch saturated wavelengths in LGAP.IUE swp35501 + lwp07914
In LWP 07914 used 2X SMAP to patch saturated wavelengths in LGAP.IUE swp35501 + lwp07914
In LWP 07914 used 2X SMAP to patch saturated wavelengths in LGAP.IUE swp35501 + lwp07914
In LWP 07914 used 2X SMAP to patch saturated wavelengths in LGAP.IUE swp35501 + lwp07914
In LWP 07914 used 2X SMAP to patch saturated wavelengths in LGAP.IUE swp35501 + lwp07914
In LWP 07914 used 2X SMAP to patch saturated wavelengths in LGAP.
ETC buffer time is only 123 seconds. Almost too bright for time-tag!!!The scheduling data was generated by CASM 28.0.CASM was run in Phase II mode./Users/proffitt/Documents/research/15869/OP-cache/15869-flight-revised-p2-v60.xmlDuplicate of visit 50 (which was a duplicate of visit 10), with changes to account for partial success of visit 50
Removed successful c1817 observation
Changed c1222 observation to only repeat failed FP-POS=4 exposure
Changed to SCHED=100
Expanded NUV exposures to fill available SCHED100 visibility in first orbit, but made only modest increases in FUV exposures to keep within this proposal's phase 2 S/N requirements and limit charge extraction on the FUV detectors, even though this leaves a good bit of unused time in the 2nd orbit.(Tic-Visit
:proposal-id 15869
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:date "25-Mar-2020 11:13:07.0"
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)true20IUE swp35501 + lwp07914
In LWP 07914 used 2X SMAP to patch saturated wavelengths in LGAP.IUE swp35501 + lwp07914
In LWP 07914 used 2X SMAP to patch saturated wavelengths in LGAP.IUE swp35501 + lwp07914
In LWP 07914 used 2X SMAP to patch saturated wavelengths in LGAP.IUE swp35501 + lwp07914
In LWP 07914 used 2X SMAP to patch saturated wavelengths in LGAP.IUE swp35501 + lwp07914
In LWP 07914 used 2X SMAP to patch saturated wavelengths in LGAP.IUE swp35501 + lwp07914
In LWP 07914 used 2X SMAP to patch saturated wavelengths in LGAP.
ETC buffer time is only 123 seconds. Almost too bright for time-tag!!!The scheduling data was generated by CASM 28.0.CASM was run in Phase II mode./private/var/folders/c1/kkl4zqqs11g637_3q3f43f2m000400/T/OPVisit7645876588833995188.xmlDuplicate of visit 12158500937900072.0(Tic-Visit
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)true30V=12.59 B1.5V E(B-V)=0.49V=12.59 B1.5V E(B-V)=0.49V=12.59 B1.5V E(B-V)=0.49 from Garmany et al 2015, AJ, 150, 141
http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/AJ/150/41V=12.59 B1.5V E(B-V)=0.49V=12.59 B1.5V E(B-V)=0.49V=12.59 B1.5V E(B-V)=0.49