Assigned ID: 492
----- Attempting Submission 1 (Fri Feb 25 18:36:56 GMT 2011) -----All target coordinates should be sufficiently accurate that no ACQ/Search is needed.
BOT warnings are spurious as discussed in the "additional comments" in the proposal
description.----- Attempting Submission 1 (Mon Jun 27 22:25:44 GMT 2011) -----All target coordinates should be sufficiently accurate that no ACQ/Search is needed.
BOT warnings are spurious as discussed in the "additional comments" in the proposal
description.Testing Rotational Mixing in Massive Stars: Boron in the Galactic Open Cluster NGC 3293Recent observational advances have shown that chemical mixing in the envelopes of early-B stars is more complex than had previously been realized. The abundance patterns seen do not match the simple theoretically expected patterns, and there appear to be processes other than rotation that can also cause mixing. These complicating effects make it difficult to test or calibrate current stellar evolution models that include rotation with the currently available data, especially as most existing boron observations are biased towards intrinsically slow rotating stars. We have identified a sample of near-turnoff stars in the 10 Myr open cluster NGC 3293 which can now be efficiently observed with the COS G185M setting in which the earliest stages of rotationally driven mixing should have noticeably depleted the surface boron abundances. These observations will place stringent new constraints on models of rotationally driven mixing in early-B stars.One target will be observed in each of the ten visits.
The brightest target (#02) will be observed with STIS E230H 1963 in ACCUM mode.
The STIS ACQ will be done with F28X50OII, and the ACQ/PEAK with the G430L.
We will use four of the 0.2x0.06 stis FP-SPLIT slits for the observations and the 0.2x0.06FPB for the peakup.
We substitute a STIS GO wavecal at the end of the orbit for a standard auto-wavecal.
The other targets will be observed with the COS G185M using the 1971 setting and all four FP-POS positions.
Targets, 3, 4, 7, 8, 10, 12, & 19 will be observed using ACCUM mode, while targets 23 & 24 will use time-tag.
For the targets observed in COS ACCUM mode we will take two subexposures at each FP-POS position to minimize
the effects of OSM drift and/or photospheric velocity variations in the target.
COS acquisitions will use the same dispersed light G185M grating as the science. In principle, we could use
NUV imaging with the BOA, but that would leave a difficult BOP issue for the PSA aperture in this crowded cluster field.
To simplify the matching of targets and visits, we specify as the primary names for
all of our targets the designations given to stars in this cluster by Evans et al
2005 (A&A, 437, 467), and we set both the target # and the visit # to correspond
the Evans et al's number for that star. Simbad searches on these names can be
done with designations like "Cl* NGC 3293 ESL 2" for his star #2.
Many, if not most of these stars are beta Cepheid variables, but none of the
stars have large amplitudes.Target BOP
For most of our targets low-dispersion, large aperture IUE observations are available.
For stars with low-dispersion, large aperture IUE data we used the observed SWP+LWR or LWP spectra as
the ETC input. For all stars we also interpolated Kurucz models tailored to the Vmag, Teff, logg, & E(B-V) given by Dufton et al.
2006, A&A, 457, 265. Online data from Dufton is available at
http://vizier.cfa.harvard.edu/viz-bin/VizieR?-source=J/A+A/457/265
Stellar Parameters from Dufton et al,
Name Vmag B-V SpType Teff logg E(B-V)
mag K [cm/s2] mag
3293-002 6.73 0.07 B0.7 Ib 23000 2.80 0.27
3293-003 7.61 0.11 B1 III 21100 2.90 0.30
3293-004 8.03 0.02 B1 III 21500 3.00 0.21
3293-007 8.25 0.18 B1 III 22800 3.10 0.38
3293-008 8.59 0.05 B1 III 21500 3.25 0.24
3293-010 8.77 0.00 B1 III 21000 3.15 0.18
3293-012 8.95 0.06 B1 III 21500 3.30 0.25
3293-019 9.27 -0.04 B1 V 25000 3.85 0.18
3293-023 10.01 -0.05 B1.5 III 20500 3.40 0.13
3293-024 10.01 -0.01 B1.5 III 20500 3.50 0.17
For all stars where we have IUE data, the observed fluxes are always slightly less than the model predictions,
but in most cases differences are < 10% (for ESL003, the IUE observation is about 15% smaller).
So we are confident that all stars are within allowed limits, even though ESL003 and ESL004 are getting rather
close to the 30000 c/s per stripe limit for COS NUV spectra of some of our targets.
Results from Kurucz models tailored to Dufton's parameters above are
given below. We used synphot to interpolate the standard Kurucz solar
metallicty grid to the Teff and Logg values given, and also added Dufton's
listed amount of extinction. Below we report the predicted global
rate as well as the peak stripe rate and peak local rate, and the ETC ID #.
Spectral energy distrib ETC ID global stripe local
ngc3293esl002_kvnorm.dat STIS.sp.180644 81691 N/A 0.874
ngc3293esl003_kvnorm.dat COS.sp.180605 61856, 26133, 14.126
ngc3293esl004_kvnorm.dat COS.sp.180613 67965, 27603, 14.876
ngc3293esl007_kvnorm.dat COS.sp.180616 27511, 11995, 6.385
ngc3293esl008_kvnorm.dat COS.sp.180618 35288, 14421, 7.772
ngc3293esl010_kvnorm.dat COS.sp.180619 38255, 15136, 8.199
ngc3293esl012_kvnorm.dat COS.sp.180620 24364, 9901, 5.336
ngc3293esl019_kvnorm.dat COS.sp.180621 33494, 13586, 7.189
ngc3293esl023_kvnorm.dat COS.sp.180623 15419, 5764, 3.128
ngc3293esl024_kvnorm.dat COS.sp.180625 12789, 4831, 2.619
The ETC predictions for the IUE input spectra are given below
using the same format as table above.
IUE-SED file ETC ID global stripe local
ngc3293esl002.dat STIS.sp.180645 77123 N/A 1.045
ngc3293esl003.dat COS.sp.180632 52557 21052 13.017
ngc3293esl004.dat COS.sp.180633 65158 26873 15.870
ngc3293esl007.dat COS.sp.180637 24583 10232 5.617
ngc3293esl008.dat COS.sp.180634 32380 13490 7.726
010 N/A
ngc3293esl012.dat COS.sp.180638 24000 10107 5.834
ngc3293esl019.dat COS.sp.180640 32945 13804 7.507
023 N/A
024 N/A
Field BOP
For G185M 1971 BOA observations of an unreddened O star to
exceed the allowed global per stripe limits of 30000 counts/s
would require V<4.5. (COS.sp.181682). No star this bright is
within 0.5 degrees of NGC 3293, so there is no need to be concerned
about where the BOA is pointing during our PSA COS observations.
For the COS targets in the PSA, the field appears very crowded in
the GSC2; however, finding charts made using 2MASS images show
that there are no bright close companions. The BOT assumes that
most of these targets are unreddened O stars rather than the moderately
reddened B stars that they are and so produces spurious warnings.
The BOT also warns of a few unknown objects that might be in the
BOA aperture, but as noted above these are too faint to be of concern.HOT STARS12false0.00.0falsefalsefalsefalseAVAILABLESTARB0-B2 III-ICl* NGC 3293 ESL 2
Revised Hipparcos Coordinates and proper motions
IUE SWP10349 SWP21514 LWR 16227HD91943V513CARJ2000J2000FLAM(2070)=2.1e-11STARB0-B2 III-ICl* NGC 3293 ESL 3
Coordinates and PM from Tycho-2 Catalogue
FLAM(2070) from SWP21529, LWR16998CPD-57D3506ACD-57D3348J2000J2000FLAM(2070)=7.1e-12STARB0-B2 III-ICl* NGC 3293 ESL 4
Coordinates and proper motions from Tycho 2 catalog
FLAM(2070) from IUE data LWR16994, SWP21512 LGAP-LOCPD-57D3523J2000J2000FLAM(2070)=8.6e-12STARB0-B2 III-ICl* NGC 3293 ESL 7
Coordinates and proper motions from Tycho 2 catalog
FLAM(2070) from IUE data SWP21531 & LWR 17000HD092044J2000J2000FLAM(2070)=3.1e-12STARB0-B2 III-ICl* NGC 3293 ESL 8
Coordinates and proper motions from Tycho 2 catalog
FLAM(2070) from IUE swp21511.mxlo swp23569.mxhi lwr16993.mxloHD091983J2000J2000FLAM(2070)=4.1e-12STARB0-B2 III-ICl* NGC 3293 ESL 10
Coordinates and proper motions from Tycho 2 catalog
No IUE dataCPD-57D3500V403CARJ2000J2000FLAM(2070)=2.9e-12STARB0-B2 III-ICl* NGC 3293 ESL 12
Coordinates and proper motion from the Tycho 2 catalog
swp20307, lwr16228 (low disp, large aper)HD092007V380CARJ2000J2000FLAM(2070)=2.9e-12STARB0-B2 III-ICl* NGC 3293 ESL 19
Positions and proper motions from UCAC3
IUE swp21513 & LWR16995 low-large
Dufton gies 25000, 3.70,CPD-57D3507V405CARJ2000J2000FLAM(2070)=4.0e-12STARB0-B2 III-ICoordinates and proper motions from UCAC3 catalogue
No IUE data
From Dufton, V=10.01, Teff=20500, logg=3.4, E(B-V)=0.13
COS.sp.180188 gvies global 13578, globalA=5040, local, 2.73, S/N=142 in 2000 S, buffer=173CPD-57D3519J2000STARB0-B2 III-ICoordinates and proper motions from UCAC3 catalogue
No IUE data
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Global rate=77123
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)true10Used IUE spectra to provide input SED
Global rate of 52557 requires ACCUM mode
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:data-volume 174400
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(Tic-Obset
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:obset-id "07"
:pcs-mode "FGS"
)
(Tic-Orbit
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:dark-offset NIL
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:max-dark-utilization 1920
:low-sky "N"
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Global rate of 24582 requires ACCUM mode to allow sufficient margin against
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:data-volume 174400
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(Tic-Obset
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(Tic-Orbit
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Global rate of 32380 requires ACCUM mode
Combined exposure time of 2080 s
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(Tic-Obset
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(Tic-Orbit
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Global rate of 38254 requires ACCUM mode
Combined exposure time of 2080 s
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(Tic-Obset
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Global rate of 24000 requires ACCUM mode to provide sufficient margin against flux uncertainties
Combined exposure time of 2080 s
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Global rate of 32944 requires ACCUM mode
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Predicted global rate 15419 c/s/private/var/folders/M4/M4IdYzSyEVSMNp1iBl-i3E++2++/-Tmp-/OPVisit5239449108806493270.xmlThe scheduling data was generated by CASM 19.3.CASM was run in Phase II mode.(Tic-Visit
:proposal-id 12520
:visit-id "24"
:proposal-version -1
:trans-version "20110509"
:date "27-Jun-2011 18:24:11.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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(Tic-Obset
:proposal-id 12520
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)
(Tic-Orbit
:proposal-id 12520
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:max-dark-utilization 1920
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:pcs-visibility 3511
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)true10Used Kurucz spectra tailored to Dufton paramters to provide input SED
predicted global rate 12789 c/s