Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.
Justification may be needed for use of certain lifetime positions with G160M. See "Errors and Warnings" for more details.0Assigned ID: 3708
----- Attempting Submission 1 (Fri Mar 25 23:27:54 GMT 2022) -----
----- Attempting Submission 2 (Sun Mar 27 15:43:36 GMT 2022) -----Due to the updated guidelines, we will only use 2 FP-POS observations to decrease the on-orbit overheads.For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.This phase 2 resubmission follows the TTRB approval to repeat 3 orbits of visit 01 and 3 orbits of visit 02 which suffered a guide-star loss-of-lock, leading to partially degraded data.-1301613607----- Attempting Submission 1 (Thu Jul 14 20:45:15 GMT 2022) -----
HST Phase II Proposal 17148 successfully submitted.
Receipt: # 17148-1
----- Attempting Submission 2 (Tue Oct 11 15:28:32 GMT 2022) -----
----- Attempting Submission 3 (Wed Oct 11 14:56:13 GMT 2023) -----
----- Attempting Submission 4 (Wed Nov 22 22:14:49 GMT 2023) -----
----- Attempting Submission 5 (Tue Dec 12 22:36:39 GMT 2023) -----Repetition of 3 orbits of both visits 01 and 02 (totaling 6 orbits) after failed observations.
We ran the orbit and visit planners for the new visits only (62 and 63).Preparing to find the sources of the reionization: Testing MgII as a Lyman Continuum tracer using a unique mock JWST sampleUnderstanding how galaxies contributed to reionize the universe is one of the principal science goals of the James Webb space telescope (JWST). Because the IGM is neutral at high-redshift, and therefore optically thick to ionizing radiation (LyC), JWST needs indirect LyC diagnostics calibrated on low redshift sources to unveil the sources of reionization. Here we propose the first sample selected based off their Mg II emission properties to have predicted LyC escape fractions. These 35 orbits of COS/HST observations will stringently test the best current LyC escape tracer in exactly the conditions that JWST will use it to infer the sources of cosmic reionization. Our mock JWST sample is completely different than any LyC sample as it is selected to have low neutral gas column densities. By comparing the Lyman Alpha and Mg II profiles we will understand the conditions when Mg II is optically thin and inform when JWST observations can use Mg II to measure the LyC escape fraction. The diverse physical properties of our sample and predicted LyC escape fraction will enable us to constrain the impact of dust and gas-phase metallicity in the inferred LyC properties. Two proposed targets are predicted to be extremely rare strong LyC emitters, while being normal star forming galaxies. If confirmed, these objects will provide a novel window into the escape of LyC. Beyond a simple test of confirmation, we will treat these observations as if they were up-coming JWST observations to demonstrate whether future JWST observations can recover the LyC escape fraction.Our proposed targets are 7 confirmed Mg II emitters discovered in the ongoing HETDEX survey (Gebhardt et al. 2022). These galaxies were selected based on their Mg II emission strength and a comparison to the [O II] emission ([O II] has to be detected in the HETDEX spectrum to confirm the redshift, and therefore the Mg II identification). Follow-up observations using the HET/LRS2 IFS (private communication) were performed for 4 of our targets to obtain spectrally resolved optical + near IR lines (from Mg II to Ha). We extracted the lines within a 2.5 arcsecond diameter aperture, similarly to the COS aperture. The three other targets can be observe with IFS in the future; for this proposal we used the publicly available SDSS spectra to measure their optical lines and HETDEX spectra to measure their Mg II doublet. There are no previous HST observations of our proposed galaxies and no other bright galaxies within the COS safety limit.
NUV acquisition images of the targets will be obtained with the standard Mirror A and the ACQ/IMAGE mode to reach a S/N of 40 inside a 9x9 pixel box centered on the brightest part of the galaxy. We used the GALEX NUV magnitudes when available or the SDSS U-band to estimate exposure times. The galaxies are small with light concentrated in a 2" radius (in the HSC imaging), i.e. well within the 2.5" COS aperture. COS will observe the galaxy integrated properties. We therefore calculate the acquisition exposure times with the ETC for a S/N of 40, assuming a point-like source. To be conservative, we assume that half the GALEX NUV and SDSS/U flux is contained within this compact component by adding 0.75 magnitudes to the observed magnitudes. Since we plan to use the NUV imaging to estimate of the sizes of the UV-emitting regions, we then double the required acquisition exposure times to allow us to detect fainter emission. The total estimated acquisition times vary between 98s and 234s depending on the source.
The low-resolution G140L grating with central wavelength of 800A will be used to measure the LyC. The required number of orbits for each object is calculated to detect the LyC at the 3sigma significance level by binning in the spectral direction by 400-pixels at the observed wavelength of 912A*(1 + z). We estimated the LyC flux using the equation 5 of Izotov et al. (2016b) with EW(Hb)=[70, 38, 84, 30, 59, 78, 116] A and the extinction corrected Hb fluxes of [5.3, 3.5, 6.9, 22.1, 4.8, 12.1, 23.0]x10^-16 erg s-1 cm-2 for our 7 galaxies, respectively. We assumed an escape fraction of 5% (corresponding to the lower bounds of the cosmologically relevant escape fractions according to models) and took into account the attenuation of the Milky Way. Using this method, we estimated the observed LyC flux densities to vary between 2.6 and 11.7x10^-18 erg s-1 cm-2 for our 7 targets. From 0.5 to 6 orbits are needed to detect the LyC of our targets.
For the medium-resolution Lyman alpha (Lya) spectroscopy, the G160M grating on COS will be used. The central wavelengths are chosen to optimize the signal-to-noise (S/N) and ensure that the Lya does not fall in the detector gaps. When available, the GALEX NUV magnitude is used to calculate the required number of orbits needed to obtain a S/N>3 in the continuum near Lya line by binning by 400-pixels. We used the SDSS U magnitude with a UV slope of -1.5 to estimate the continuum near Lya for two objects. Given the large Mg II EW (>3A) we expect our targets to be Lya emitters (EW>20A). This S/N in the continuum is thus sufficient to determine the shape of the Lya profile with ample accuracy. Between 0.5 and 2 orbits per object are needed for the medium-resolution G160M Lya spectrum.
We follow the COS handbook guidelines to determine the buffer times. We first calculate the buffer time from the spectroscopic ETC and GALEX FUV magnitude and multiply by 2/3. For all our targets, this re-scaled buffer time is longer than an individual FP-POS exposure and longer than 110 seconds. As recommended by the COS handbook, we therefore adopt the ETC buffer time multiplied by 2/3.
We schedule all of the objects in 2-3 orbit visits. Galaxies that require more than 3 orbits and can also have their science carried out in multiple visits, have been broken up into multiple visits. Our spectra requiring S/N < 20, we use at least 3 FP-POS per configuration and per visit.
Reduced-gyro operations will impact the measured fluxes of our targets leading to larger flux uncertainties that will moderately impact the science goals of our program. Moreover, the fact that not all orientations will be possible is not an issue because we do not have position angle restriction.The team has expertise in all of the required areas of work to carry out the data reduction and analysis. Co-I John Chisholm has been PI of multiple HST/COS observing proposals (Chisholm et al. 2016, 2017, 2018) so we know how to reduce and optimally use the data. Co-I John Chisholm have expertise in measuring the stellar continuum properties of galaxies (Chisholm et al. 2019). The team will thus be able to determine the escape fraction of ionizing photons and test a variety of dust attenuation curves and stellar continuum models to be compare with the properties of the Lyman alpha (HST/COS) and MgII emission (HET/LRS2 data). The COS observations of the Lyman alpha lines will be analyzed by PI Floriane Leclercq who has extensive
expertise on Lya observations and modeling (Leclercq et al. 2017, 2020).Galaxies6falsefalsetruefalsefalsefalsefalsefalseSUPPORTEDGALAXYDWARF COMPACTSTARBURSTNOJ2000J2000NUV=20.92GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000GALAXYDWARF COMPACTSTARBURSTNOJ2000J2000COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG160M1577The scheduling data was generated by CASM 31.0.CASM was run in Phase II mode.J022512+001560 requires 8 orbits. Thus, we split the object up into two visits. We use the standard SNR = 40 exposure times for the acquisition images, instead of the twice duration that we use for the objects that require a single visit.170038831900043.03844000000001(Tic-Visit
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