0Assigned ID: 601
----- Attempting Submission 1 (Fri Mar 06 17:55:54 GMT 2020) -----
HST Phase I Proposal 601 successfully submitted.
Receipt: # 601-1
----- Attempting Submission 2 (Fri Mar 06 23:14:51 GMT 2020) -----
HST Phase I Proposal 601 successfully submitted.
Receipt: # 601-2
----- Attempting Submission 3 (Fri Mar 06 23:16:55 GMT 2020) -----
HST Phase I Proposal 601 successfully submitted.
Receipt: # 601-3
----- Attempting Submission 4 (Fri Mar 06 23:18:49 GMT 2020) -----
HST Phase I Proposal 601 successfully submitted.
Receipt: # 601-4
----- Attempting Submission 5 (Fri Mar 06 23:21:48 GMT 2020) -----
HST Phase I Proposal 601 successfully submitted.
Receipt: # 601-5
----- Attempting Submission 6 (Fri Mar 06 23:59:26 GMT 2020) -----0----- Attempting Submission 1 (Tue Jun 30 19:45:43 GMT 2020) -----
----- Attempting Submission 2 (Mon Oct 12 20:16:01 GMT 2020) -----
----- Attempting Submission 3 (Tue Nov 03 19:02:21 GMT 2020) -----Extreme Star-Forming Galaxies: Local laboratories to constrain models of ionizing sources in the reionization epochThe rest-UV emission line spectra of star-forming galaxies (SFGs) at z>6 serves as a primary tool to reveal the nature of ionizing sources that are responsible for the cosmic reionization. Low-metallicity star-forming dwarf galaxies at z<0.3, show similar strong UV emission lines (eg; C IV, He II, O III], and C III]), and are being used to calibrate the UV diagnostics that can be applied to study galaxies in the reionization epoch. However, the high equivalent widths (EW > 20 Angstrom) seen for UV emission lines in z>6 galaxies, have not been observed in any of the local analogs. Such high EWs pose a challenge to the photoionization models, requiring the lowest metallicities, youngest stellar ages, and highest ionization parameters as model inputs to produce the required hard ionizing spectrum, and extreme emission lines. We propose to obtain HST COS (G140L) and STIS (G230L) spectra of a unique sample of 5 SFGs, recently identified as having extreme [OIII]/[OII] ratios (>22) with evidence for hard ionizing radiation from young, massive stars with ages < 3 Myrs. The photoionization models predict high nebular C IV and C III] EWs (> 15 Angstrom), comparable to galaxies in the reionization epoch. Our goal is to (1) compare the fluxes and EWs of the UV emission lines to the model predictions and infer the ISM conditions, (2) calibrate the UV diagnostics that predict potential Lyman continuum escape, and (3) obtain constraints on the ionizing sources (very massive stars, WR stars, or binaries) based on the hardness of the ionizing radiation. The results from our analysis of local analogs will offer crucial insights into the stellar populations and ISM conditions in extreme starbursts at high redshifts that are responsible for reionization.The observations in this program are designed to obtain the rest-UV spectra of a sample of 5 local compact star forming galaxies (CSFGs) at z = 0.03-0.07 that have high [OIII]/[OII] ratios = 23 - 43. The CSFGs are the best local analogs to study the extreme ionizing conditions observed in high redshift galaxies at the reionization epoch. All of these CSFGs have existing HST COS observations using the G130M grating that covers the Lyman-alpha emission line. The CSFGs are selected from the SDSS and their optical spectra are also available in the SDSS database. The CSFGs will be observed using the COS G140L grating for the FUV wavelengths, primarily for the C IV, He II, and O III] emission lines. Since the sensitivity of this instrument setup drops precipitously at wavelengths > 1800, we will use the STIS G230L grating to observe the C III] line which falls in wavelength range 1960 - 2026 Angstrom. We do not require to resolve the O III] and C III] doublet emission lines because we are interested in measuring the integrated line fluxes, and will use the low resolution gratings for both instruments. The overlap in the wavelengths around the weaker OIII] emission line is an added advantage, and also serves to cross-calibrate the derived fluxes.
We used the online exposure time calculator for COS and STIS to compute the exposure times required to achieve signal-to-noise (S/N) > 3 per resolution element. The information on the optical emission line fluxes from SDSS, were used to derive the predicted O III] and C III] UV emission line fluxes using the CLOUDY photoionization models (Jaskot & Ravindranath 2016; Nakajima et al. 2018). The predicted UV emission line fluxes and the continuum estimated using the GALEX magnitudes, along with the UV continuum information available from the HST COS G130M grism were used to derive the exposure times.
The ETC calculations were performed for COS using the G140L, with central wavelength 1280 Angstrom, and the primary science aperture (PSA). The CSFGs are compact with half-light radii less than 1", and we used a point source approximation for the exposure time calculations. The estimated exposure times range from 2000 - 6000s depending on the target brightness and the O III] line fluxes. We will use the TIME-TAG mode and FP-POS = ALL for the science exposures. The buffer times for the science exposures were adopted to be 2/3 of the values returned by the ETC as recommended by the COS instrument handbook. For the COS target acquisition, we assumed that the target is an extended source. All of our targets have COS acqusition images taken previously in HST-GO-14080 and HST-GO-15136. The COS acquisition images show that in most cases the source has multiple clumps of star formation, with one brightest clump centered on the source coordinates. We used the COS ETC to compute the acquisition exposure times required to obtain a S/N ~ 15 - 20 for an extended source, using the ACQ/IMAGE mode with MirrorA and PSA. The CSFGs are more extended than a point source, but may not fill the 1.25" radius of the COS aperture since they are unresolved in the SDSS images. We also followed the method in proposal HST-GO-14080 and assumed the case of a point source which only accounts for 10% of the total NUV flux within the COS PSF. The acquisition exposures times we derive from the ETC will yield S/N ~ 20 - 30 and was verified by using the acquisition images obtained for the same targets in previously executed COS programs (14080 and 15136).
For the STIS ETC calculations, we used the G230L grating, and the 52" x 0.5" aperture. We find that the exposure times for the required S/N range from 1000 - 5000s depending on the target brightness and the C III] line fluxes. We used the TIME-TAG mode and the buffer times were adopted to be 4/5 of the values returned by the ETC as recommended for use in the APT. For STIS target acquisition, we used the SDSS g-band magnitudes for an extended source and computed the exposure times required for S/N=40. Although the sources are unresolved at the SDSS resolution they are resolved on the STIS acquisition images. The acquisition exposure times were calculated for ACQ mode using the long pass F28X50LP aperture, and with MIRROR and STIS CCD.
We also used the Bright Object Tool to verify that there are no UV bright objects close to the targets that would cause health and safety concerns for the COS FUV, and STIS NUV-MAMA detectors.Our team has extensive expertise with HST COS and HST STIS observations, and use of CLOUDY photoionization models.
Anne Jaskot and Swara Ravindranath have used CLOUDY photoionization models to identify UV diagnostics that can be used to infer the nature of ionizing sources, and phyical conditions in the ISM of star-forming galaxies.
Swara Ravindranath, Anne Jaskot, and Harry Ferguson have used HST STIS (GO-14134) with the same configuration proposed here, to observe Green Pea Galaxies to test the predictions from the CLOUDY models. Anne Jaskot, Swara Ravindranath, and Harry Ferguson are carrying out HST COS survey to obtain the first large statistical sample of LyC measurements at low redshift, and an HST imaging program to look for Lyman continuum leakage from high redshift galaxies.
Anne Jaskot has used HST COS observations to study Lyman-alpha emission lines in Green Pea Galaxies.
Bethan James is an expert on UV spectroscopy, paticularly with HST COS. Bethan James is also an expert on low-metallicity galaxies, massive stars, and has carried out spatially-resolved emission line studies of star-forming galaxies.GalaxiesStellar Populations and the Interstellar Medium6falsefalsetruefalsefalsefalsefalsefalseSUPPORTEDGALAXYDWARF COMPACTEMISSION LINE NEBULASTARBURSTNOJ2000J2000FUV = 20.64, NUV = 20.43GALAXYDWARF COMPACTEMISSION LINE NEBULASTARBURSTNOJ2000J2000FUV = 20.26, NUV = 20.25GALAXYDWARF COMPACTEMISSION LINE NEBULASTARBURSTNOJ2000J2000FUV = 21.04, NUV = 20.58GALAXYDWARF COMPACTEMISSION LINE NEBULASTARBURSTNOJ2000J2000FUV = 20.54, NUV = 20.66GALAXYDWARF COMPACTEMISSION LINE NEBULASTARBURSTNOJ2000J2000FUV = 20.10, NUV = 20.40COS/FUVSpectroscopicNoNoG140L1280STIS/NUV-MAMASpectroscopicNoNoG230L2376COS/FUVSpectroscopicNoNoG140L1280STIS/NUV-MAMASpectroscopicNoNoG230L2376COS/FUVSpectroscopicNoNoG140L1280STIS/NUV-MAMASpectroscopicNoNoG230L2376COS/FUVSpectroscopicNoNoG140L1280STIS/NUV-MAMASpectroscopicNoNoG230L2376COS/FUVSpectroscopicNoNoG140L1280STIS/NUV-MAMASpectroscopicNoNoG230L2376The scheduling data was generated by CASM 28.2.CASM was run in Phase II mode.1632672518000257.57895064879375(Tic-Visit
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)true10This is a duplicate of failed visit 10 (impacted by HST safing)(Tic-Visit
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