0Assigned ID: 922
----- Attempting Submission 1 (Fri Apr 10 22:11:52 GMT 2015) -----
HST Phase I Proposal 922 (bhbprop.apt) successfully submitted.
Receipt: # 922-1
----- Attempting Submission 2 (Fri Apr 10 23:18:25 GMT 2015) -----
HST Phase I Proposal 922 (bhbprop.apt) successfully submitted.
Receipt: # 922-2
----- Attempting Submission 3 (Fri Apr 10 23:47:25 GMT 2015) -----
HST Phase I Proposal 922 (bhbprop.apt) successfully submitted.
Receipt: # 922-3For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.0----- Attempting Submission 1 (Mon Jul 20 20:27:08 GMT 2015) -----This is a one-orbit observation, and we use only three FP-POS settings to maximize the S/N. If we use all four positions, the buffer dumps cause us
to lose too much S/N.Using UV-bright Milky Way Halo Stars to Probe Star-Formation Driven Winds as a Function of Disk Scale HeightGalactic-scale winds driven by star formation are a common feature of galaxy formation models, and are observed ubiquitously from the local Universe to z~6. However, empirical constraints on the radial density profile and total spatial extent of these winds have been very challenging to obtain. We have devised a simple experiment using blue horizontal branch (BHB) stars in the halo of the Milky Way that will directly map the extent and density of diffuse, ionized outflows from the Galactic disk to the halo. We propose to take COS FUV spectra of 7 BHB stars that evenly sample the range of scale heights from 3 - 13 kpc, lying perpendicular to the disk of the Milky Way, extending from the position of the sun. This study will allow us to unambiguously track inflowing and outflowing material from the Milky Way via absorption component blueshifts and redshifts, respectively. This program will yield the first direct observational determination of the scale height to which star-formation-driven winds propagate in the halo. We will additionally probe the change in the gas density as it extends into the halo, and approximate a mass of metals as they leave the disk and become integrated into the halo. Our proposed experiment will yield the most detailed constraints on the physical state and energetics of gas in a large-scale galactic wind to date. Such constraints are fundamental to understanding the impact of feedback processes on galaxies and in fueling the buildup of their gaseous environments.From Phase I:
---------------
We are targeting blue horizontal branch stars in the halo of the Milky Way along a straight line perpendicular to the disk extending from the sun out to 13 kpc into the halo. Our catalog of blue horizontal branch stars comes from Xue et al. (2011), who selected these stars from SDSS DR8 stars with fiber spectra. Halo blue horizontal branch stars are good COS targets for four primary reasons: (1) They are blue point sources and therefore have bright continua in the UV, (2) their UV spectra are characterized by a fairly featureless bright continuum with broad Lyman series lines (Brown et al. 2012) because they are quite metal poor, (3) many of them are moving with |vrad| > 100 km/s which allows us to cleanly distinguish any absorption features intrinsic to the star and its atmosphere, and (4) They are approximate standard candles since their distances can be estimated from multi-band photometry with an accuracy of 10% (Deason et al. 2011).
There are two primary requirements that define our seven-star sample: 1) The stars must have GALEX FUV magnitudes that are bright enough to achieve our required S/N in a reasonable number of orbits (see below; mFUV < 18.5); and 2) The stars must have heliocentric radial velocites < -100 km/s to minimize confusion of features redshifted with respect to the MW with stellar absorption lines (although the halo stars are metal poor, and unlikely to exhibit significant contaminating atmospheric lines). Criterion 1 limits us to ~800 stars and criterion 2 winnows the group to ~200 potential stellar targets. Finally, we choose stars that lie along a continuous line of sight roughly perpendicular to the disk extending to the most distant star (z = 13 kpc) that remains after the aforementioned cuts. We sample the distance perpendicular to the plane in 1- 2 kpc increments, with a narrow range of x, y values (coordinates in the 2D plane of the disk) such that we are probing lines of sight within 500 pc of each other to minimize variations due to differing locations above the disk. These final criteria are crucial for a direct measure of how the properties of gas outside the disk depend on scale height, and leave us with 7 stars that satisfy our experimental design.
To achieve our primary goal of detecting the weak FUV absorption features redshifted (or perhaps blueshifted) with respect to strong Galactic absorption features, we require a S/N of 15 - 20 over our wavelength range, and the highest spectral resolution of COS (G160M) with a central wavelength of 1577 A. These requirements are to ensure an accurate measurement of this weak component and to avoid blending with the disk of the Milky Way. We expect to detect 15 mA features of CIV 1548 at 3sigma, consistent with previous detections of this transition in the halo of the Milky Way (Lehner & Howk 2011). For reference, a CIV 1548 line with an EW of 15 mA has a column density of 3 x10^12 cm^2, and a physically interesting limit based on detections in the halos of normal, star-forming galaxies (Bordoloi et al. 2014). To assess the signatures of gas inflow and outflow may require an analysis of the absorption line profiles by constructing two-component models which include the ISM component of the Galaxy (Rubin+2012), which is another reason we require S/N of at least 15 across our spectral range.
The key transitions we will probe will be SiII (1526), FeII (1608, 1611), AlII (1670),SiIV (1393, 1402), and CIV (1548, 1550). From this range of transitions, especially via comparisons of SiII and SiIV, we will be able to probe the ionization state of the gas as a function of distance from the galactic plane. Our stars range in GALEX FUV magnitudes from 16.3 - 18.5 . The Cycle 23 COS ETC tells us that we will require between 1 and 8 orbits for each BHB star (modeled as an AOIII star) to reach a S/N of 15 - 20 over the full spectral range (see: COS.sp.697859,697885, 697894, 697898, 697902, 697909). The most stringent requirement setting the exposure time is that we cover the CiIV doublet (1548, 1550) at the minimum S/N of 15. This calculation includes 14 minutes of overhead for the first orbit, and 6 minutes of overhead for each additional orbit. All exposure time calculations assume 2800 seconds of useful exposure averaged in each orbit (i.e., acquisition takes longer on the first orbit). Standard COS guide star and target acquisition, minimal readouts, and other overheads are factored in. None of these stars will pose a bright limit threat to COS and we have no timing or orientation constraints.
Phase II Observing Strategy:
-----------------------
We are taking COS/FUV spectra of blue horizontal branch stars with G160M centered at 1577 Angstroms. We require only one CENWAVE setting for this experiment since we are targeting specific absorption lines that will not fall near the gap between segments. Because we have coordinates that are accurate to within 0.1", we skip the ACQ/SEARCH step, and acquire the targets with a PEAKXD exposure followed by a PEAKD exposure. The Exposure times for these acquisitions are set by requiring a S/N in FUV-A segment only of 25, and a S/N of 40 for both segments, respectively.
For each of our four brightest targets that require four or fewer orbits to reach our desired S/N, we pack the exposures into a single visit. For the brightest star in our sample, we use a single orbit, and only three FP-POS settings to reduce overheads from buffer dumps. In general, the buffer times are quite long, and we thus set the buffer time in the exposure manually to be 100 seconds shorter than the target's exposure time. We proceed by attempting to maximize exposure times while keeping to a minimum of four FP-POS settings per visit (Except for visit 1, noted above, which is only one orbit). In four-orbit visits, we are able to use all four FP-POS settings with no loss from buffer dumps.
In our final set-up we achieve S/N of between 13 - 22 across our full wavelength range for all of our targets, which is generally in line with the requirements we outlined in the science case of Phase 1.ISM AND CIRCUMSTELLAR MATTER12falsetruefalsefalseSUPPORTEDSTARHALOHORIZONTAL BRANCH STARNOThis object was generated by the targetselector and retrieved from the SIMBAD database. z = 3.4J2000J2000GALEX FUV = 16.3STARHALOHORIZONTAL BRANCH STARNOThis object was generated by the targetselector and retrieved from the SIMBAD database. z = 4.1J2000J2000GALEX FUV = 16.9STARHALOHORIZONTAL BRANCH STARNOThis object was generated by the targetselector and retrieved from the SIMBAD database. z = 5.7SDSS-J134404.40+184259.1J2000J2000GALEX FUV = 17.3STARHALOHORIZONTAL BRANCH STARNOThis object was generated by the targetselector and retrieved from the SIMBAD database. z = 7.32MASS-J13255441+2232499J2000J2000GALEX FUV = 17.8STARHALOHORIZONTAL BRANCH STARNOThis object was generated by the targetselector and retrieved from the SIMBAD database. z = 9.22MASS-J14155712+3716582J2000J2000GALEX FUV = 18.0STARHALOHORIZONTAL BRANCH STARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.SDSS-J134119.85+282358.6J2000J2000GALEX FUV = 18.1STARHALOHORIZONTAL BRANCH STARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALEX FUV = 18.5COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1577The scheduling data was generated by CASM 23.2.CASM was run in Phase II mode.(Tic-Visit
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:internal-dur-at-end 331
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3307
:pcs-gap 0
)true40The scheduling data was generated by CASM 23.2.CASM was run in Phase II mode.The 7th target gets 8 orbits split over two visits of four orbits each.
With this set-up, we can get all four FP-POS per visit easily...
visits 9 and 10 are identical.(Tic-Visit
:proposal-id 14140
:visit-id "10"
:proposal-version -1
:trans-version "20150609"
:date "14-Jul-2015 00:33:09.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 4
:saa-model "31"
:si-bright-earth-limb-angle 20.0
:data-volume 348096
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 14140
:visit-id "10"
:obset-id "10"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 14140
:visit-id "10"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2974
:al-overhead-at-end 0
:internal-dur-at-end 38
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3307
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 14140
:visit-id "10"
:orbit-number 2
:pcs-time 222
:si-vis-utilization 3085
:al-overhead-at-end 0
:internal-dur-at-end 38
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3307
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 14140
:visit-id "10"
:orbit-number 3
:pcs-time 222
:si-vis-utilization 3085
:al-overhead-at-end 0
:internal-dur-at-end 38
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3307
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 14140
:visit-id "10"
:orbit-number 4
:pcs-time 222
:si-vis-utilization 3085
:al-overhead-at-end 0
:internal-dur-at-end 331
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3307
:pcs-gap 0
)true40