0Assigned ID: 271
----- Attempting Submission 1 (Thu Apr 07 20:02:44 GMT 2016) -----Adjusted some buffer times on the advice of the CS
The CS requested that the acquisitions be changed from 1971 to 1921 setting.
This change has been made and the ETC calculations for those exposures were updated.
Note that GSC2 is incomplete in this region and Galex is non-existent. PI has supplied CS with photometry from other sources for field BOP check.103661102----- Attempting Submission 1 (Mon Jul 11 14:32:18 GMT 2016) -----
----- Attempting Submission 2 (Tue Aug 16 21:10:57 GMT 2016) -----
----- Attempting Submission 3 (Thu Aug 18 22:12:53 GMT 2016) -----A Definitive Test of Rotational Mixing in Massive StarsCNO processed surface material found in OB stars may originate either from internal mixing or from binary interaction, but incomplete boron depletion is an unambiguous sign of internal mixing. Existing boron observations indeed suggest that internal mixing occurs in some stars at a level that is consistent with the low end of the efficiency range predicted by the different models of rotationally driven mixing. However, current results are too sparse to directly confirm the expected relation between boron depletion and rotation, and leave room to interpret boron depletion through other mixing processes. We propose to observe boron in ten rather rapidly rotating early-B stars in the 10 Myr old open cluster NGC 3293. Together with our previous data on stars in this cluster, this increased sample with an expanded range of V sin(i) values will provide a definitive test of rotational mixing, and --- assuming that rotation actually drives the expected mixing --- will allow for a tight calibration of its efficiency, which is of critical importance for modeling the interior of massive stars, with wide implications for their advanced evolutionary stages.All targets will be acquired with dispersed light acquisitions using the COS G185M 1971 PSA setting followed by science observations in the same mode.
Target names (ESL#'s) are from Evans, Smartt, Lee et al. (2005) A&A, 437, 467. To simplify tracking, we have set the APT target and visit numbers to match the ESL target numbers.
The four brightest targets will be observed with ACCUM mode as rates are too high for uninterupted TIME-TAG observations. The other six targets will be observed using TIME-TAG.
All observations will use all four FP-POS positions. For the ACCUM targets, the exposure at each FP-POS position will be split into two 255 s pieces to minimize OSM drift or smearing due to variations in the photospheric velocity during the observations.
Except for ESL 05 which has Hipparcos measurements, coordinates and proper motions are from the PPMXL Catalog. For our stars this seems to give proper motions with smaller errors and values more consistent with the mean cluster proper motion (-6.91+/-2.01 and +0.26+/-3.95 mas/yr) than does UCAC4.
For targets ESL 5 and 31 we have IUE LGAP LO data and so can make direct ETC calculations.
Use IUE spectra of ESL005 - SWP20323+LWR16247
COS.sp.820449
Get total 17160 in brightest stripe
Buffer time 56 c/s
Use IUE spectra of ESL031 - SWP20322+LWR16246
COS.sp.820450
Get total 1926 in brightest stripe
Buffer time = 427 s
Time to S/N=150 is 6129 s
We estimate acquisition times for our faintest target using the IUE spectrum for ESL031:
PEAKD COS.sa.820452 gives needed time of 0.4 s.
PEAKXD COS.sa.820453 gives time of 1.08 s for stripe B
Since these times are very short, we will adopt 1 s and 2 s for all PEAKD/PEAKXD exposure times for all of our targets..
For other ETC calculations we adopt V & E(B-V) from Dufton, P. L., Smartt, S. J., Lee, J. K., et al. 2006, A&A, 457, 265
For BOP ETC estimates we will adopt the Kurucz B1V spectrum (Teff=25400; log g =3.9), even though our targets are all a few thousand K cooler than this, and so the ETC calcuations should provide a firm upper limit to the possible count rates.
Below we give the adopted V & E(B-V) values used as input with B1V spectrum, along with the actual Teff & logg, and the ETC count rate for the brightest stripe and the ETC calculation #.
#ESL V Teff log g E(B-V) STRIPEA ETC#
005 8.12 21500 3.05 0.27 27863 821148 (see also COS.sp.820449 for IUE results)
006 8.21 21500 3.15 0.26 26826 821149
015 9.11 25000 3.80 0.21 14765 821150
016 9.21 19200 4.00 0.20 14092 821151
020 9.55 20500 3.15 0.21 9651 821152
025 10.01 21100 3.70 0.19 6907 821153
028 10.26 19400 3.65 0.18 5736 821154
030 10.51 19800 3.70 0.13 5692 821155
031 10.66 17400 3.45 0.21 3472 821156 (ee also COS.sp.820450 for IUE results)
038 11.00 20600 3.95 0.14 1882 820454
With the Kurucz B1 spectrum, targets 5 & 6 at 89% to 93% OF THE 30000 c/s/stripe limit on STRIPEA, but the more realistic IUE spectrum for ESL 005 shows only 17160 c/s/stripe and ESL 6 has almost identical parameters to ESL 5.
Note that for target 20, a more realistic flux estimate with a slightly cooler SED (COS.sp.820432) gives an ETC buffer time estimate of 130 s, so OK to use time-tag with a 110 s buffer time for this one instead of ACCUM.
CS requested that acq exposures change to 1921 setting
The CENWAVE=1921 ETC #s
#ESL V Teff log g E(B-V) STRIPEA ETC#
005 8.12 21500 3.05 0.27 19840 831885 (adopts IUE spectrum)
006 8.21 21500 3.15 0.26 29050 831888
015 9.11 25000 3.80 0.21 15744 831889
016 9.21 19200 4.00 0.20 14993 831890
020 9.55 20500 3.15 0.21 10498 831891
025 10.01 21100 3.70 0.19 7493 831897
028 10.26 19400 3.65 0.18 6128 831892
030 10.51 19800 3.70 0.13 5692 831893
031 10.66 17400 3.45 0.21 3777 831894
038 11.00 20600 3.95 0.14 3737 831895Stellar Physics12falsetruefalsefalsefalsefalseSUPPORTEDSTARB0-B2 III-INOVmag, coordinates, proper motions, and errors from UCAC4 catalogCPD-57-3521J2000J2000STARB0-B2 III-INOCoordinates and proper motion from PPMXL catalogCPD-57-3526BJ2000J2000STARB0-B2 III-INOCooridnates and proper motion from UCAC4V-V440-CARJ2000J2000STARB0-B2 V-IVNOCoordinates and proper motion from PPMXL catalogMCW-1182J2000J2000STARB0-B2 V-IVNOCoordinates and proper motion from PPMXL catalogV-V401-CARJ2000J2000STARB0-B2 III-INOCoordinates and proper motion from PPMXL catalogCPD-57-3504J2000J2000STARB0-B2 V-IVNOCoordinates and proper motion from PPMXL catalogCPD-57-3520J2000J2000STARB0-B2 V-IVNOCoordinates and proper motion from PPMXL catalogCPD-57-3514J2000J2000STARB0-B2 V-IVNOCoordinates and proper motion from PPMXL catalogCPD-57-3528J2000J2000STARB0-B2 V-IVNOCoordinates and proper motion from PPMXL catalogCL-NGC-3293-ESL-38J2000J2000COS/NUVSpectroscopicNoNoG185M1971COS/NUVSpectroscopicNoNoG185M1971COS/NUVSpectroscopicNoNoG185M1971COS/NUVSpectroscopicNoNoG185M1971COS/NUVSpectroscopicNoNoG185M1971COS/NUVSpectroscopicNoNoG185M1971COS/NUVSpectroscopicNoNoG185M1971COS/NUVSpectroscopicNoNoG185M1971COS/NUVSpectroscopicNoNoG185M1971COS/NUVSpectroscopicNoNoG185M1971The scheduling data was generated by CASM 24.2.CASM was run in Phase II mode./private/var/folders/8k/sxlgy5ts2xdbykzf_vw6jrfw0001c5/T/OPVisit5183389340910949659.xmlThe BOT reports the target as "unsafe" because it assumes that it is an unreddened O star. In reality it is a significantly reddened early-B star with IUE LGAP-LO observations.
Using SWP20323+LWR16247 in ETC COS.sp.820449 predicts total 17160 counts/second in the brightest stripe.(Tic-Visit
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)true10The BOT reports the target as "unsafe" because it assumes that it is an unreddened O star. In reality it is a significantly reddened early-B star with IUE LGAP-LO observations.
Using SWP20323+LWR16247 in ETC COS.sp.820449 predicts total 17160 counts/second in the brightest stripe.The BOT reports the target as "unsafe" because it assumes that it is an unreddened O star. In reality it is a significantly reddened early-B star with IUE LGAP-LO observations.
Using SWP20323+LWR16247 in ETC COS.sp.820449 predicts total 17160 counts/second in the brightest stripe.The BOT reports the target as "unsafe" because it assumes that it is an unreddened O star. In reality it is a significantly reddened early-B star with IUE LGAP-LO observations.
Using SWP20323+LWR16247 in ETC COS.sp.820449 predicts total 17160 counts/second in the brightest stripe.The scheduling data was generated by CASM 24.2.CASM was run in Phase II mode./private/var/folders/8k/sxlgy5ts2xdbykzf_vw6jrfw0001c5/T/OPVisit3867293483964165820.xmlBOT finds no targets in PSA(Tic-Visit
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(Tic-Obset
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(Tic-Obset
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(Tic-Orbit
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)true10The scheduling data was generated by CASM 24.2.CASM was run in Phase II mode./private/var/folders/8k/sxlgy5ts2xdbykzf_vw6jrfw0001c5/T/OPVisit5521495265342563928.xmlBOT finds no objects in PSA(Tic-Visit
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:coron NIL
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(Tic-Obset
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(Tic-Orbit
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:low-sky "N"
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)true10The scheduling data was generated by CASM 24.2.CASM was run in Phase II mode./private/var/folders/8k/sxlgy5ts2xdbykzf_vw6jrfw0001c5/T/OPVisit4845520078690230191.xmlBOT labels the target as "UNKNOWN". See BOP comments in observation description(Tic-Visit
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:date "24-Aug-2016 10:45:17.0"
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(Tic-Obset
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)true10The single "unknown" star reported by the BOT is the target.The single "unknown" star reported by the BOT is the target.The single "unknown" star reported by the BOT is the target.The scheduling data was generated by CASM 24.2.CASM was run in Phase II mode./private/var/folders/8k/sxlgy5ts2xdbykzf_vw6jrfw0001c5/T/OPVisit1988001012663459790.xmlBOT does not find target(Tic-Visit
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(Tic-Obset
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(Tic-Orbit
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)true10/private/var/folders/8k/sxlgy5ts2xdbykzf_vw6jrfw0001c5/T/OPVisit5020660115867654287.xmlThe scheduling data was generated by CASM 24.2.CASM was run in Phase II mode.(Tic-Visit
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)true20/private/var/folders/8k/sxlgy5ts2xdbykzf_vw6jrfw0001c5/T/OPVisit5998863944930734058.xmlThe scheduling data was generated by CASM 24.2.CASM was run in Phase II mode.(Tic-Visit
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:number-of-orbits 2
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:data-volume 3931008
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:coron NIL
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(Tic-Orbit
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)true20/private/var/folders/8k/sxlgy5ts2xdbykzf_vw6jrfw0001c5/T/OPVisit8486754052002216146.xmlThe scheduling data was generated by CASM 24.2.CASM was run in Phase II mode.(Tic-Visit
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:date "24-Aug-2016 10:45:25.0"
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(Tic-Obset
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(Tic-Orbit
:proposal-id 14673
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(Tic-Orbit
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)true20The BOT shows three unknows for this field.
The unknown in the PSA is the target. See the observation description for the notes on the target ETC calcuation.
Two "unknowns" are reported in the BOA. These are stars with no catalog magnitude listed.
However an unreddened O star would need V=4.2 to reach 40,000 c/s/stripe for G185M/1971/BOA,
COS.sp.820600, and it is obvious there are no stars this bright in this cluster. The integrated light of the entire open cluster only reaches V=4.7.