0Assigned ID: 1706
----- Attempting Submission 1 (Thu Mar 22 03:52:27 GMT 2018) -----INEFFICIENT ORDERING OF FP-POS POSITIONS
INEFFICIENT ORDERING OF FP-POS POSITIONS
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
INEFFICIENT ORDERING OF FP-POS POSITIONS
INEFFICIENT ORDERING OF FP-POS POSITIONS
INEFFICIENT ORDERING OF FP-POS POSITIONS
INEFFICIENT ORDERING OF FP-POS POSITIONS
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.We are getting a BOT error for the acquisition of our second target, however, this target was observed in the same manner for program 14628 with no complications.
Is it still preferred to do FP-POS=ALL when doing multiple orbits of the same target?-494690307----- Attempting Submission 1 (Thu May 31 08:29:52 GMT 2018) -----We are getting a BOT error for the acquisition of our second target, however, this target was observed in the same manner for program 14628 with no complications.Resolving Extreme High-Ionization UV Emission-Line Diagnostics in Preparation for JWSTThe recent observations of extreme ultraviolet (UV) emission lines with complex line profiles in a z~2 lensed galaxy (Berg et al. 2018a) suggest our ability to characterize sources using their UV emission lines may be biased by the unaccounted for stellar and interstellar medium (ISM) contributions. This is of particular concern for the imminent window onto reionization-era sources allowed by the James Webb Space Telescope (JWST), where extreme UV emission lines may be the only diagnostic probes available. Because the CIII], OIII], CIV, and HeII high-ionization emission lines are rarely seen in lower redshift galaxies (0<z<3), the promising UV diagnostic diagrams combining these lines (e.g., Feltre et al. 2016; Nakajima et al. 2017; Byler et al. 2018) lack observational confirmation or calibration. Fortunately, recent UV spectral campaigns have identified a sample of nearby galaxies with analogous emission-line features to reionization-era systems, including the strongest CIV (Berg et al. 2016) and HeII (Berg et al. 2018b) emitters in the local Universe. We therefore propose high resolution, high signal-to-noise HST/COS spectral observations of two reionization-era analogues that will allow us to robustly model the massive star populations and resolve the stellar and nebular components of the high-ionization emission lines. These data will provide the first stringent test of the high-ionization UV emission line diagnostics critical to the interpretation of distant sources accessible with JWST.Goal:
We will obtain NUV target aquisiton images and high-resolution, high signal-to-noise HST/COS spectral observations of two reionization-era analogues that will allow us to robustly model the massive star populations and resolve the stellar and nebular components of the high-ionization emission lines.
Targets:
Our targets were selected from previous low-resolution HST/COS obsevations for their large CIV and HeII equivalent widths. These targets have high [OIII] optical emission line surface brightnesses, large ionizations, low metallicities (12+log(O/H) < 8.0), and compact morphologies in order to achieve maximum flux through the 2.5" COS aperture. We use the coordinates from our target's SDSS optical spectra, which are in the ICRS reference frame.
Target Acquisition:
Since all sources have SDSS positions, which are generally accurate to 0.1", we do not do an ACQ/SEARCH routine. With such excellent input coordinates from the SDSS, we aquire our targets using the ACQ/IMAGE mode with the PSA aperture and MirrorA for the COS/NUV configuration. Following the successful target acquisition method of our previous HST-GO14628 program, we have determined integration times necessary to reach a S/N = 25 for our targets. We assume a flat spectral distribution normalized by the GALEX FUV surface brightnesses. Both galaxies are compact in the SDSS imaging with a FWHM PSF diameter of ~2". We then divide the GALEX FUV fluxes by the area of the 2" PSF to determine the FUV surface brightnesses. Note that Target 18 required us to use Mirror B to ensure safe levels when using the BOT.
Science Exposures:
We will use COS with the G160M grating with a central wavelength of 1589 angstroms in TIMETAG mode in order to simultaneously observe the CIV 1548,1550 and HeII 1640 spectra features. In order to resolve the stellar and nebular components of the CIV and HeII features, we use the ETC to determine the total science integration times necessary to achieve a S/N >~ 7 per resolution in the continuum for our targets using input continuum fluxes at 1500 A from our previous HST/COS observations. We will observe our targets for 3 and 5 orbits each though the PSA aperture with the COS/FUV configuration. With the G160M grating we use FP-POS=ALL, which takes 4 images offset from one another in the dispersion direction and increases S/N. These 4 positions allow a flat to be created and cosmic rays to be eliminated.CosmologyGalaxies and the IGM6falsefalsetruefalsetruefalsefalseSUPPORTEDGALAXYDWARF COMPACTYESJ2000J2000g = 17.49, r = 17.76GALAXYDWARF COMPACTYESJ2000J2000SDSS r-band = 17.65COS/FUVSpectroscopicNoNoG160M1589COS/FUVSpectroscopicNoNoG160M1589The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.(Tic-Visit
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