0Assigned ID: 376
----- Attempting Submission 1 (Fri Apr 05 09:01:22 GMT 2019) -----
HST Phase I Proposal 376 (LyCMgII_unsubmitted.apt) successfully submitted.
Receipt: # 376-1
----- Attempting Submission 2 (Fri Apr 05 14:42:26 GMT 2019) -----0----- Attempting Submission 1 (Thu Jul 18 13:45:53 GMT 2019) -----Deciphering Cosmic Reionization with Mg II Emission: Uncovering the most Promising Tracer of LyC Escape for JWSTThe Universe was reionized at z~6, but it is unknown what sources instigated cosmic reionization. Theory argues that either accretion onto black holes or massive stars reionized the Universe. JWST and ELTs will soon usher in the needed observations to determine the sources of reionization, but the neutral high-z IGM precludes a direct detection of ionizing photons (LyC). Further, the community does not yet have a flawless method to indirectly infer the fraction of LyC that escapes star-forming galaxies. Without such a calibrated method, JWST will struggle to determine the source of reionization. Here we propose new HST/COS observations to directly measure the LyC emission from 8 galaxies drawn from the SDSS that have a diverse sample of Mg II emission properties. Mg II emission possesses many strengths that other indirect indicators do not; chiefly the Mg II escape fraction tentatively correlates with the LyC escape fraction. However, this tentative correlation is only with 6 local confirmed leakers. If confirmed by our proposed observations, JWST and ELTs will use this relation to infer the LyC escape fraction within the Epoch of Reionization. To aid in the interpretation of LyC transmission, we also propose Lyman-alpha observations to perform simultaneous radiative transfer simulations of Mg II and Lyman-alpha to provide vital physical context for why Mg II traces LyC escape. In total, we request 32 orbits to fully-develop the most promising proposed method for determining the LyC escape fraction during the Epoch of Reionization. These observations may be the key for JWST to accomplish one of its primary science goal: determining the source of cosmic reionization.We selected star-forming galaxies from the SDSS DR14 sample using the following criteria: (1) compact and similar angular sizes in the SDSS photometric bands to ensure the FUV light is within the 2.5'' diameter COS aperture, (2) z > 0.3 to ensure that Mg II is within the SDSS bandpass and the LyC is on the sensitive portion of the COS detector, (3) an Hbeta equivalent width greater than 100A and an [O III]/[O II] ratio >4 to select young stellar populations with intrinsically bright (i.e. observable) LyC, (4) no other bright galaxies within the COS safety limit, (5) no previous HST observations, (6) a representative and expansive range of observed Mg II/[O III] flux ratios to probe the full range of possible fesc(Mg II). The result of these selection criteria is a sample of 8 galaxies. None of these galaxies were previously observed or scheduled for observations with HST/COS. The galaxies are faint and satisfy safety conditions for observing with HST/COS. Furthermore, there are no sources brighter than the COS safety limits within a 43'' diameter centered on the selected galaxies.
NUV acquisition images of the targets will be obtained with the standard Mirror A and the ACQ/IMAGE mode to reach a S/N~20 inside a 9x9 pixel box centered on the brightest part of the galaxy. The adopted GALEX NUV magnitudes were used to estimate exposure times. We also assumed that the galaxy light is concentrated within 0.4'' in diameter, which is consistent with other Green Peas in the literature and is corresponding to the surface brightness NUV/0.4**2. The total estimated acquisition times vary in the range from 2x100s to 2x300s. However, keeping in mind that ETC estimates are uncertain for our type of objects (intermediate case between point-like and extended options in ETC) and based on the previous observations of similar objects with the COS we conservatively adopted acquisition exposure time 2x700s per object to be safe with successful pointing. Using these deeper acquisition images we will study the UV morphology (size, light distribution, etc.) of the selected objects.
The low-resolution G140L grating with central wavelength of 800A will be used to measure the LyC. The exposure time for each object is calculated to detect the LyC at the 3sigma significance level by binning in the spectral direction by 100-pixels at the observed wavelength of 912x(1+z) and by 20-pixels binning along the spatial axis, corresponding to SNR ~ 3/sqrt(100x20)~0.1 per pixel. We estimated the LyC flux assuming an escape fraction of 5% and that the intrinsic LyC flux density is equal to I(Hbeta)/I(912) ~ 9A, where I(Hbeta) is the extinction-corrected Hbeta flux. This value corresponds to a theoretical 3 Myr instantaneous burst, stellar population and acts as a conservative lower limit for the expected LyC flux density for galaxies with the large observed Hbeta equivalent widths.
For the medium-resolution Ly-alpha spectroscopy, the G160M grating on COS will be used to observe the Ly-alpha line. The resolution of G160M grating is required to resolve the Ly-alpha line profile and to measure features such as the narrow velocity separation between the Ly-alpha emission peaks. While the effective resolution of G160M is R = 16000, galaxies are not point sources and the G160M grating instead delivers observations with effective R ~ 4000 - 10000. We will compare the observed Ly-alpha profiles to medium-resolution (R ~ 8000) follow-up observations of the Mg II profile to determine how the line profile varies across transitions with optical depths that differ by 1e5 (the typical H/Mg ratio). This will constrain future radiative transfer simulations. If Ly-alpha is in absorption, we will derive N(H I) by fitting the Lorentzian wings of the Ly-alpha absorption profile. An intrinsic flux derived from the galaxy SED is used to calculate the exposure time needed to obtain a S/N ~ 3 in the continuum near Ly-alpha line by binning by 100-pixels and 20 pixels along spectral and spatial axes, respectively, corresponding to SNR~0.1 per pixel. This SNR is sufficient to determine the shape of the Ly-alpha profile with ample accuracy to constrain radiative transfer models and to derive velocity separations between the emission peaks.
For each target 0.5 orbits are allocated for acquisition, 1.5 orbits for the the medium-resolution G160M Ly-alpha spectrum, and 2 orbits for the low-resolution G140L spectrum that will determine the LyC, totalling 4 orbits per object.
Our observations do not require repeated visits to the same galaxy and do not require constraints on the HST orientation. Therefore, operating HST in reduced gyro mode would likely affect our program a little, slightly increasing the time for acquisition and slightly reducing the time for science observations.Our team is uniquely qualified to reduce, analyze, and publish the proposed observations. Our team includes experts in the determination of the LyC escape fraction (Izotov et al. 2016 a, b; Izotov et al. 2018 a,b). With 11 previously published LyC emitting galaxies and nine more scheduled in Cycle 26 (GO 15639), we will use this previous experience to rapidly measure the LyC escape fractions.
Members of our team have developed sophisticated HST/COS reduction techniques required to coadd the faint flux expected from LyC emitters (Worseck et al. 2011; Worseck et al. 2014). This technique is required for accurate flux estimates at these low fluxes. Our team also has extensive experience in the stellar continuum fitting required to determine the intrinsic LyC fluxes, to determine the LyC escape fractions. We also have extensive experience in the radiative transfer simulations required to determine the connection between Mg II and Lyman-alpha (Schaerer et al. 2011; Prochaska et al. 2011; Verhamme et al. 2015).
Our team has extensive experience with analysis of Mg II observations both from the SDSS (Guseva et al. 2019) and at higher redshifts (Prochaska et al. 2011). This experience was used to develop criteria used to select the galaxies and will help with our analysis of the proposed Mg II followup. Our team also has access to the large telescopes required for high-resolution, high-SNR Mg II follow-up on blue-sensitive spectrographs like Hi-res and KCWI on Keck (Co-I Prochaska). Our extensive experience will lead to rapid analysis and publication of the proposed data.Galaxies and the IGMCosmology6falsefalsetruefalsefalsefalsefalseSUPPORTEDGALAXYDWARF COMPACTEMISSION LINE NEBULASTAR FORMING REGIONSTARBURSTNOJ2000J2000FUV=22.42+/-0.16, NUV=22.15+/-0.14, frest(900)=4.0e-18 erg/s/cm2/A (5% of intrinsic flux), frest(1216)=7.0e-17 erg/s/cm2/AGALAXYDWARF COMPACTEMISSION LINE NEBULASTAR FORMING REGIONSTARBURSTNOJ2000J2000FUV=21.35+/-0.35, NUV=22.04+/-0.44, frest(900)=1.2e-17 erg/s/cm2/A (5% of intrinsic flux), frest(1216)=4.0e-16 erg/s/cm2/AGALAXYDWARF COMPACTEMISSION LINE NEBULASTAR FORMING REGIONSTARBURSTNOJ2000J2000FUV=21.99+/-0.53, NUV=21.61+/-0.49, frest(900)=5.0e-18 erg/s/cm2/A (5% of intrinsic flux), frest(1216)=2.2e-16 erg/s/cm2/AGALAXYDWARF COMPACTEMISSION LINE NEBULASTAR FORMING REGIONSTARBURSTNOJ2000J2000FUV=21.88+/-0.59, NUV=22.29+/-0.70, frest(900)=4.6e-18 erg/s/cm2/A (5% of intrinsic flux), frest(1216)=1.3e-16 erg/s/cm2/AGALAXYDWARF COMPACTEMISSION LINE NEBULASTAR FORMING REGIONSTARBURSTNOJ2000J2000FUV=20.92+/-0.37, NUV=21.29+/-0.35, frest(900)=3.0e-18 erg/s/cm2/A (5% of intrinsic flux), frest(1216)=1.3e-16 erg/s/cm2/AGALAXYDWARF COMPACTEMISSION LINE NEBULASTAR FORMING REGIONSTARBURSTNOJ2000J2000NUV=22.46+/-0.20, frest(900)=8.5e-18 erg/s/cm2/A (5% of intrinsic flux), frest(1216)=1.3e-16 erg/s/cm2/AGALAXYDWARF COMPACTEMISSION LINE NEBULASTAR FORMING REGIONSTARBURSTNOJ2000J2000NUV=22.94+/-0.37, frest(900)=4.7e-18 erg/s/cm2/A (5% of intrinsic flux), frest(1216)=1.1e-16 erg/s/cm2/AGALAXYDWARF COMPACTEMISSION LINE NEBULASTAR FORMING REGIONSTARBURSTNOJ2000J2000FUV=21.83+/-0.17, NUV=21.81+/-0.13, frest(900)=5.0e-18 erg/s/cm2/A (5% of intrinsic flux), frest(1216)=1.1e-16 erg/s/cm2/ACOS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG160M1611COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG160M1600The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.(Tic-Visit
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)true40