0Assigned ID: 4892
----- Attempting Submission 1 (Tue Aug 22 11:20:40 GMT 2023) -----
HST Phase I Proposal 4892 successfully submitted.
Receipt: # 4892-1I changed to FLASH=20 for EELG-1 F225W exposure.-285397864----- Attempting Submission 2 (Tue Nov 07 21:25:50 GMT 2023) -----Eat Your Green Pea Galaxies!7The early Universe was re-ionized by high energy photons for which high-mass X-ray binaries (HMXBs) in low-metallicity, dwarf galaxies with high SFR might have contributed significantly to the process. Green Pea galaxies are believed to be low-z analogs to these cosmologically important ionizers, and are characterized by strong [OIII] emission indicative of a very young stellar population. As such, they are predicted to have a high L_{X,HMXB}/SFR ratio. We have identified seven new Green Pea galaxies with J-PLUS that are near enough to be detected with Chandra, and our sample will double the number of X-ray detected Green Peas. Our goal is to use the X-ray emission with joint HST imaging to trace the connection between HMXBs and star formation in such extreme emission line galaxies.In this proposal, we intend to analyze the morphology of low redshift Green Pea galaxies with high spatial resolution. First, we intend to study the spatial distribution of the ionized gas and thus the most recent star formation burst, using narrow band filters to image the Halpha line (F665W or F673W). We will also analyze the location and morphology of young stellar populations with the UV filter (F225W). Finally, we will target the redder part of the spectrum (with the F775W filter) to provide with a continuum image to subtract from the Halpha one, and to study the structure of the old stellar populations.
Combining this data with the Chandra observations, we will be able to search for clumps of star formation that are coincident with X-ray emission, and measure its specific properties, which may be different from other clumps. The HST data will also be helpful in determining the presence of an underlying disk, formed by the old stellar population. We will also potentially identify jets, holes, and tails in the ionized gas structure, with implications in the leakage of Lyman radiation. This is a key issue in the analysis of the very high redshift galaxies discovered by JWST (those responsible of the reionization of the Universe), which are analogues to our galaxies. We will obtain a much higher physical spatial resolution that what the JWST reaches at high redshift.
In order to do so, we intend to observe each galaxy during on HST orbit, with three different filters and three exposures in each filter. The different exposures will help us remove cosmic rays or bad pixels and, along with the dithering pattern, sample accurately the PSF. The exposure times of the F225W filter are longer than the other filters, due to the lower sentivity and therefore lower SNR in the bluer wavelengths. To a lesser extent, the F775W filter exposures are shorter than the Halpha filters (F665W or F673W). The exposures are short (114-300 s), but since the targets are relatively bright, we expect to reach high SNR. According to the ETC, we will reach SNR > 20 for 0.2 arcsec apertures in the optical filters, and SNR>10 in the UV.
To improve the efficiency of the observations, and given the small size of the targets (<20 arcsec), we have chosen to read only a sub-array of the CCD. We propose to use UVIS2-C1K1C-SUB for most of the sample, as it is roughly twice the size of the galaxies, and it allows us to extend significantly the exposure times and thus the SNR. For the largets galaxy we use UVIS2-2K2C-SUB, and for the smallest, UVIS2-C512C-SUB. We use postflash to avoit CTE issues.
The different Halpha filters are chosen depending on the redshift of each target.
The target EELG-6 has already been observed with F775W and F673W to get Halpha, so there is no need to repeat them. We chose to use the remaining time in the orbit to observe it with F547M and F621M to obtain an image of the [OIII]5007+4959 emission line. Combining it with the available Halpha, we will explore the different physical properties in the gas (ionization parameter and metallicity), traced by the [OIII]/Halpha ratio.naGalaxies6falsefalsefalsefalsefalsefalsefalsefalseSUPPORTEDGALAXYDWARF COMPACTEMISSION LINE NEBULAJ2000J2000uJAVA=21.99+-0.08 mag/arcsec^2, Halpha=5.9e-15 erg/s/cm^2/arcsec^2 , iSDSS=20.42+-0.01 mag/arcsec^2GALAXYDWARF COMPACTEMISSION LINE NEBULAJ2000J2000uJAVA=22.07+-0.08 mag/arcsec^2, Halpha=3.3e-15 erg/s/cm^2/arcsec^2 , iSDSS=20.57+-0.01 mag/arcsec^2GALAXYDWARF COMPACTEMISSION LINE NEBULAJ2000J2000uJAVA=22.21+-0.13 mag/arcsec^2, Halpha=4.8e-15 erg/s/cm^2/arcsec^2 , iSDSS=20.89+-0.03 mag/arcsec^2GALAXYDWARF COMPACTEMISSION LINE NEBULAJ2000J2000uJAVA=22.5+-0.18 mag/arcsec^2, Halpha=1.5e-15 erg/s/cm^2/arcsec^2 , iSDSS=21.18+-0.03 mag/arcsec^2GALAXYDWARF COMPACTEMISSION LINE NEBULAJ2000J2000uJAVA=21.1+-0.05 mag/arcsec^2, Halpha=7.8e-15 erg/s/cm^2/arcsec^2 , iSDSS=20.33+-0.01 mag/arcsec^2GALAXYDWARF COMPACTEMISSION LINE NEBULAJ2000J2000uJAVA=20.44+-0.02 mag/arcsec^2, Halpha=6.7e-15 erg/s/cm^2/arcsec^2 , iSDSS=20.08+-0.01 mag/arcsec^2GALAXYDWARF COMPACTEMISSION LINE NEBULAJ2000J2000uJAVA=25.35+-1.68 mag/arcsec^2, Halpha=5.8e-16 erg/s/cm^2/arcsec^2 , iSDSS=23.51+-0.19 mag/arcsec^2WFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF775WWFC3/UVISImagingNoNoF665NWFC3/UVISImagingNoNoF689MWFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF775WWFC3/UVISImagingNoNoF665NWFC3/UVISImagingNoNoF689MWFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF775WWFC3/UVISImagingNoNoF665NWFC3/UVISImagingNoNoF689MWFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF775WWFC3/UVISImagingNoNoF665NWFC3/UVISImagingNoNoF689MWFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF775WWFC3/UVISImagingNoNoF665NWFC3/UVISImagingNoNoF689MWFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF775WWFC3/UVISImagingNoNoF665NWFC3/UVISImagingNoNoF689MWFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF775WWFC3/UVISImagingNoNoF665NWFC3/UVISImagingNoNoF689MPOS-TARGDITHER0.135LINEfalsefalse346.84WFC3-UVIS-DITHER-LINE-3PT1false/private/var/folders/8t/mg1bkfyj20xf2vfc_9vyhfs80006z1/T/OPVisit5381463468967989118.xmlThe scheduling data was generated by CASM 32.1.CASM was run in Phase II mode.(Tic-Visit
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