0Assigned ID: 1048
----- Attempting Submission 1 (Fri Apr 11 23:26:38 GMT 2014) -----Resubmission of observing plan. Responses were summarized in e-mail from Van Dixon to Andrew Fox on Dec 4.( Take 3 for submission)2088490797----- Attempting Submission 1 (Thu Jul 17 20:04:56 GMT 2014) -----
----- Attempting Submission 2 (Fri Dec 05 17:55:30 GMT 2014) -----The Windy Milky Way GalaxyThe Milky Way is the only galaxy in which we can directly measure the three dimensional density, kinematics, metallicity, and multi-phase structure of a Galactic wind. There are two major outflow regions suspected to exist in the Galaxy: a nuclear outflow associated with the Fermi Bubble and an annular wind associated with the star formation activity in the Molecular Ring/Scutum-Centaurus spiral arm. We request 14 orbits to observe five UV-bright sources in globular clusters in front of and behind the Scutum-Centaurus spiral arm. The interstellar absorption data will provide unique constraints on the vertical outflow velocity and radial extent of this outflow. We will combine these results with archival data to develop the next generation of multiphase, rotating wind models and use these models to estimate the energetics, mass outflow, and angular momentum flux of this galactic outflow. We expect that the insights gained here will be valuable in understanding the nature of local systems and the ubiquitous winds present in the universe at z=2. An analysis of the sources themselves will also provide valuable insights into the late stages of stellar evolution in low-metallicity populations.This program aims to obtain FUV spectra of five UV-bright stars in globular clusters using the G130M and G160M gratings of COS. Exposure times are sufficient to obtain S/N ~ 30 in each spectrum.
Three of our stars are in the GSC2 or the 2MASS Point-Source Catalog, so we use their GSC2 or 2MASS coordinates and employ an ACQ/IMAGE acquisition. Coordinates for the other two stars are determined from GALEX observations, so are uncertain at the 0.5 arcsec level. We begin their target acquisitions with a small ACQ/SEARCH.
NGC7099-214018-231323 and NGC5024-131310+180735 have been observed only with GALEX, so we have a weak handle on the stellar color -- and thus temperature. To compute exposure times suffient to achieve the required S/N, we assume that the star is cool (18,700 K) when modeling the G130M spectrum and warm (44,500 K) when modeling the G160M spectrum. For the other three stars, we use published temperatures or archival FUV spectra.ISM AND CIRCUMSTELLAR MATTERDefaultfalsetruefalsefalsefalseSUPPORTEDSTARB6-B9.5 III-IPOST-AGB STARStar is 67981 from the catalog of Anderson et al. (2008, AJ, 135, 2055), retrieved from the HLA.
The star is 0.5" from a redder companion, so we use an FUV spectroscopic TA.
Teff = 11,000 K, log g = 2.5, E(B-V) = 0.04, F(1300) = 4E-13, F(1600) = 4E-13
Using data from HUT235505 and IUE LWR07507:
G130M/1291 gives S/N = 30 in 303 s (COS.sp.615190)
G160M/1600 gives S/N = 30 in 601 s (COS.sp.615191)
Both generate warnings that count rate is too bright for an irregularly-variable source, but target is not variable.
Bright-Object Check: GSC2 reports 2 stars, both safe. GALEX reports one star of unknown brightness. It is in fact the target, with bad coordinates. Catalog of Schiavon et al. (2012; retrieved from Cosmic Lab) includes no GALEX sources within 45" of target. FUSE observed the star with a 30"x30" aperture; there is no evidence for a second UV-bright star in the field.NGC104-BRIGHT-STARJ2000J2000GALEX FUV=13.069STARB0-B2 III-IPOST-AGB STARUsing 2MASS coordinates, which are consistent with those listed in the GALEX UV photometric database of globular clusters (cosmic-lab.eu).
Teff = 27,000 K, log g = 3.6 (Mooney et al. 2004), E(B-V) = 0.28 (Harris 1996/2010)
Using Kurucz Models B1V 25400 3.9, E(B-V) = 0.28, scaled to GALEX FUV mag:
G130M/1291 gives S/N = 30 in 745 s (COS.sp.615356)
G160M/1600 gives S/N = 30 in 2216 s (COS.sp.615357)
Bright-Object Check: GSC2 has no data for this field. GALEX reports two objects, both safe, but they combine to raise global count rate on side B above limit. Both objects are copies of the target, with bad coordinates. Catalog of Schiavon et al. (2012; retrieved from Cosmic Lab) shows that nearest GALEX source is 17" from target.2MASS-J16570924-0404243J2000J2000GALEX FUV=13.876STARB0-B2 III-IPOST-AGB STARTarget is NGC7099-10 from Schiavon et al. (2012, AJ, 143, 121).
Coordinates from the GALEX UV photometric database of globular clusters (cosmic-lab.eu).
GALEX colors imply Teff = 24,000 K, but uncertainty is large. To guarantee S/N = 30, assume that star is 18,700 K when observing through G130M and 44,500 K when observing through G160M. VMAG is estimated from Kurucz model scaled to GALEX FUV. E(B-V) = 0.03 (Harris 1996/2010).
G130M/1291 gives S/N = 30 in 1500 s (COS.sp.615595)
G160M/1600 gives S/N = 30 in 5563 s (COS.sp.615598)
Bright-Object Check: GSC2 has no data for this field. GALEX reports one object and declares it safe. Aladin shows two GALEX sources with slightly different coordinates and similar magnitudes. Both are copies of the target.J2000J2000GALEX FUV=14.763STARPOST-AGB STARSDOTarget is 2MJF17RF in the GSC2; it was imported from 2MASS.
Teff = 58,800 K, log g = 5.15 (Moehler et al. 1998)
E(B-V) = 0.35 (Harris 1996/2010), Rv = 4.0 (Peterson, Rees, & Cudworth 1995)
Note: the extinction is variable across M4, but Mochejska et al. (2002) find that the NW quadrant, which includes our target, has relatively uniform extinction that is slightly higher [E(B-V) = 0.4) than the mean cluster value quoted by Harris.
Using Lanz & Hubeny OSTAR2002 model T5500g475v10 with Z/Zo = 10, E(B-V) = 0.35, and Rv = 4.0, scaled to UIT flux:
NUV/PSA/MIRRORB gives S/N = 40 in 9.4 s (COS.ta.649827)
G130M/1291 gives S/N = 30 in 2148 s (COS.sp.649829)
G160M/1600 gives S/N = 30 in 6270 s (COS.sp.649830)
Bright-Object Check: GSC2 reports 23 stars, all safe. GALEX has no information for this field.2MASS-J16232230-2628035J2000J2000UIT F(1620) = 4.3+/-0.5 E-14STARB0-B2 III-IPOST-AGB STARTarget is NGC5024-7 from Schiavon et al. (2012, AJ, 143, 121). Galex FUV and NUV magnitudes quoted in this proposal are from this paper. See also the GALEX UV photometric database of globular clusters (cosmic-lab.eu).
Using coordinates and VMAG of star N5IG002352 in the GSC2.
GALEX colors imply Teff = 25,000 K, but uncertainty is large. To guarantee S/N = 30, assume that star is 18,700 K when observing through G130M and 44,500 K when observing through G160M. E(B-V) = 0.02 (Harris 1996/2010).
NUV/PSA/MIRRORB gives S/N = 40 in 13.9 s (COS.ta.618717)
G130M/1291 gives S/N = 30 in 2940 s (COS.sp.615639)
G160M/1600 gives S/N = 30 in 11,122 s (COS.sp.615646)
Bright-Object Check: GSC2 reports 16 stars, all safe. GALEX reports 2 stars, both safe.J2000J2000GALEX FUV=15.506, GALEX NUV = 15.832COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG160M1600The scheduling data was generated by CASM 22.2.CASM was run in Phase II mode.(Tic-Visit
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:date "25-Nov-2014 12:02:15.0"
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)true10S/N = 40 in 0.3 s for Segment A, 0.1 s for A + B.See previous commentSee previous commentS/N = 30 in 303 s (G130M+1291, BT=2/3*204 = 136)S/N = 30 in 601 s (G160M+1600, BT=2/3*243 = 162)
Use BT=97 to reduce overheads.The scheduling data was generated by CASM 22.2.CASM was run in Phase II mode.(Tic-Visit
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)true20S/N = 40 in 0.9 s for Segment A, 0.4 s for A + BSee previous commentSee previous commentS/N = 30 in 745 s (G130M+1291, BT=2/3*465 = 310)S/N = 30 in 2216 s (G160M+1600, BT=2/3*786 = 524)The scheduling data was generated by CASM 22.2.CASM was run in Phase II mode.(Tic-Visit
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)true30S/N = 40 in 1.8 s for Segment A, 0.8 s for A + BSee previous commentSee previous commentS/N = 30 in 1500 s (G130M+1291, BT=2/3*805 = 537)S/N = 30 in 5563 s (G160M+1600, BT=2/3*1674 = 1116)The scheduling data was generated by CASM 22.2.CASM was run in Phase II mode.(Tic-Visit
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)true30S/N = 40 in 9.4 s (NUV, MIRRORB, PSA)S/N = 30 in 2148 s (G130M+1291, BT=2/3*1057 = 705)
Current plan yields 95% of required exposure time.S/N = 30 in 6270 s (G160M+1600, BT=2/3*2012 = 1341)
Current plan yields 89% of required exposure time.
Use BT = 900 to reduce overheads.The scheduling data was generated by CASM 22.2.CASM was run in Phase II mode.(Tic-Visit
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)true50S/N = 40 in 13.9 s (NUV, MIRRORB, PSA)
We scale this model to GALEX NUV, which better matches COS NUV bandpass.S/N = 30 in 2940 s (G130M+1291, BT=2/3*1400 = 933)
Current plan yields 97% of required exposure time in each band.S/N = 30 in 11,122 s (G160M+1600, BT=2/3*3030 = 2020)
Current plan yields 97% of required exposure time in each band.