0Assigned ID: 291
----- Attempting Submission 1 (Thu Apr 06 20:18:28 GMT 2017) -----
HST Phase I Proposal 291 (SFGs.apt) successfully submitted.
Receipt: # 291-1INEFFICIENT ORDERING OF FP-POS POSITIONSI have submitted the repeats of the failed visits 54 (1 orbit) and 06 (3 orbits) after HOPR submission and approval by the TTRB. The two new visits are called 94 (repeat of visit 54) and 56 (repeat of visit 06).
Thanks.
Ale-1139300453----- Attempting Submission 1 (Thu Jul 20 22:58:06 GMT 2017) -----
----- Attempting Submission 2 (Tue Feb 27 00:10:08 GMT 2018) -----
HST Phase II Proposal 15193 (15193.apt) successfully submitted.
Receipt: # 15193-2
----- Attempting Submission 3 (Tue Feb 27 00:10:40 GMT 2018) -----
----- Attempting Submission 4 (Wed Jan 09 19:02:59 GMT 2019) -----
----- Attempting Submission 5 (Wed Jul 03 01:27:19 GMT 2019) -----I want to submit as is, since the warning is irrilevant and the visit planner has been run on the 2 new visits (94 qnd 56).
AleAddressing Ionization and Depletion in the ISM of Nearby Star-Forming GalaxiesMeasuring galaxy metallicity with cosmic time is of paramount importance to understand galaxy formation. ISM abundances are typically determined using emission-line spectroscopy of HII regions. However, HII regions may be self-enriched and not typical of the whole galaxy. This is particularly true for star-forming galaxies (SFGs) where the bulk of metals may be in the neutral gas. Quantifying metals in the ISM is thus important to assess how reliably HII regions trace galaxy abundances at any redshift. We were awarded 34 HST orbits (Cycle 17) to measure abundances in the neutral ISM of 9 nearby SFGs using absorption lines in the COS G130M/1291 spectra of bright UV background sources within the galaxy itself. We found metallicities that differ by up to ~ 2 dex depending on the element. These variations could be real or due to observational effects. Here we request 22 orbits in the new G130M/1222 and in G160M/1623 to access new FUV spectral transitions that will help us characterize ionized-gas contamination and dust depletion, and ultimately nail down the abundances of the different elements. These new data will nicely complement our Cycle 17 COS and Gemini/GMOS IFU programs, the latter aimed at deriving nebular abundances along the same COS sightlines. This first detailed and spatially-accurate comparison between neutral- and ionized-gas abundances in local (z~0) SFGs will provide crucial insights into the metallicity of galaxies at any redshift. If this UV spectroscopic study is not undertaken before HST ceases operation, the (in)homogeneity of the ISM in galaxies of the local Universe will continue to remain uncertain for at least another decade.We propose to perform COS/FUV spectroscopic follow-up observations of several point-like sources within 9 nearby star-forming galaxies previously targeted with COS G130M @ 1291 A to infer the metal content of their neutral ISM and compare it to the abundances in the HII regions. The complementary observations here proposed will provide tighter constraints to the observational effects affecting our ISM abundances, particularly ionization and depletion, but also hidden saturation and edge-detector effects.
The newer G130M @ 1222 A setting available to GOs starting from Cycle 20 will cover the 1060-1150 A spectral region (this setting places Ly_alpha in the detector gap; however, this is not an issue, since we will use the HI column densities from our previous observations to infer abundances). COS is currently the only HST (and space-based) instrument that can perform medium-resolution spectroscopy below ~ 1150 A. The bluer G130M @ 1055 A setting (900-1200 A) would have been preferred for our COS follow-up if it was not for its much lower effective area (a factor ~ 100 lower than for the standard 1291 A setting) that makes the integration times prohibitive. We will also efficiently extend the spectral coverage of our sightlines to the redder 1430-1800 A spectral range by using the G160M @ 1623 A setting. In many cases these additional observations are easily included within the 1 orbit already allocated for target acquisition and G130M observations because of short integration times. Averaging over bright and faint targets, the overall increment in the number of additional orbits requested to include G160M is only ~ 30%. This number would triple if the observations in G160M @ 1623 A would be done independently (14 orbits).
COS is a spectrograph optimized for observations of point sources. Observations of extended sources may thus be degraded in terms of resolution and this may compromise our abundance analysis. However, we are confident that this is not a problem for the observations here proposed. We will use the same sightlines towards UV-bright sources that we carefully selected for our Cycle 17 program. Most of these sources resulted in a COS/FUV G130M resolution of ~ 18 km/s (typical of point sources) once their intrinsic spatial extension was considered. Only a few of the targets were slightly extended (~ 0.3"-0.5" ) and resulted in a final spectral resolution of ~ 20-30 km/s. From our past FUSE and COS experience, this resolution is still well suited for the kind of ISM analysis that we are proposing here with COS (see, e.g., Aloisi et al. 2003 and James et al. 2014).
The exposure times for the Phase 1 are based on the same assumptions used to prepare the Phase 2 of our COS observations in Cycle 17 (program ID: 11579). In that case, the ACS/SBC pre-acquisition images were used in conjunction with archival WFPC2 and ACS/WFC images in other filters to isolate the brightest UV point-like sources, estimate their brightness and infer their spectral type from their color for usage in the ETC calculations (the foreground reddening from NED was also considered for this purpose). For this proposal, the flux of the targets was normalized to the flux observed at 1350 A in our COS G130M @ 1291 A spectra, instead of using the photometry from our pre-imaging effort.
The COS spectroscopic ETC was used to estimate exposure times necessary to reach a S/N ~ 10 at 1350 A for G130M@1222 A, and at 1550 A for G160M@1623 A. Our experience suggests that this is a minimum requirement to estimate column densities with uncertainties <|0.1 dex through a multi-component fitting technique. We conservatively considered an HST orbit lasting 54 minutes minus overheads as suggested by the APT: guide star (re-)acquisition (5-6 min), target acquisition (5-6 min), and exposure overheads including FP-POS split (2-12 min). Taking into account all the pointings for all the galaxies in the sample, this amounts to 17 orbits in COS/FUV G130M @ 1222 A and 5 additional orbits in COS/FUV G160M @ 1623 A, for a total of 22 orbits. (For I Zw 18 G160M @ 1623 A observations already exist in the HST archive.)
The ETC reported no warnings for violations of the local and/or global bright object limits, so we expect the targets to be safe to observe (as also already confirmed by our G130M @ 1291 A observations). The spectroscopic exposures in each pointing will be executed with FP-split to mitigate flat-fielding uncertainties and improve the S/N. Since the targets of each pointing will be faint point-like sources we will use the same target acquisition (TA) strategy performed before, i.e., a standard peak-up TA in NUV imaging mode.
The spectroscopic data will be analyzed using the Fitlyman package in MIDAS, which fits individual absorption lines with Voigt profiles taking into account constraints from atomic physics and the spectral resolution of the data. For an accurate analysis we will thus need to know the actually achieved resolution and line-spread function (LSF). We will calibrate this similarly to what already done for the COS spectra acquired in G130M @ 1291 A, i.e., we will use the TA images to estimate the intrinsic UV extension of the sources to convolve with the LSF of the COS/FUV spectroscopic observations.
This study has not been possible with any other previous space-based mission or instrument. The unique FUV capabilities of COS on HST, coupled with the ground-based Gemini IFU capabilities that will constrain the metals in the nebular gas along the same sightlines, will now finally provide the opportunity to probe this subject with a completely new approach. If this UV study is not completed now that HST is available, many of the key questions related to the evolution of metals with cosmic time will continue to remain unanswered for at least another decade if not longer.
Coordinated Observations
Justify Duplications
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(Tic-Orbit
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)true30The scheduling data was generated by CASM 26.2.2.CASM was run in Phase II mode.Part 1 of integration on IZw18 target (we cannot schedule a 6-orbit visit, so this is visit 1 with first 3 orbits).1541982911000278.0(Tic-Visit
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)
(Tic-Obset
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)
(Tic-Orbit
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)true11The scheduling data was generated by CASM 26.2.2.CASM was run in Phase II mode.1525751841000168.44243856506017(Tic-Visit
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(Tic-Orbit
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)
(Tic-Orbit
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(Tic-Orbit
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)true32The scheduling data was generated by CASM 26.2.2.CASM was run in Phase II mode.1557748630000162.0(Tic-Visit
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(Tic-Obset
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(Tic-Orbit
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(Tic-Orbit
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)true30The scheduling data was generated by CASM 26.2.2.CASM was run in Phase II mode.1535556735000267.289383236513(Tic-Visit
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(Tic-Orbit
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(Tic-Orbit
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(Tic-Orbit
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)true43The scheduling data was generated by CASM 26.2.2.CASM was run in Phase II mode.155011157800077.02294052804473(Tic-Visit
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)
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)
(Tic-Orbit
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)
(Tic-Orbit
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(Tic-Orbit
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)true40