0Assigned ID: 5618
----- Attempting Submission 1 (Tue Mar 26 20:25:10 GMT 2024) -----
HST Phase I Proposal 5618 successfully submitted.
Receipt: # 5618-1
----- Attempting Submission 2 (Tue Mar 26 23:03:34 GMT 2024) -----
HST Phase I Proposal 5618 successfully submitted.
Receipt: # 5618-2
----- Attempting Submission 3 (Tue Mar 26 23:18:31 GMT 2024) -----
HST Phase I Proposal 5618 successfully submitted.
Receipt: # 5618-3
----- Attempting Submission 4 (Tue Mar 26 23:28:58 GMT 2024) -----
HST Phase I Proposal 5618 successfully submitted.
Receipt: # 5618-4
----- Attempting Submission 5 (Tue Mar 26 23:40:48 GMT 2024) -----
HST Phase I Proposal 5618 successfully submitted.
Receipt: # 5618-5
----- Attempting Submission 6 (Tue Mar 26 23:50:22 GMT 2024) -----SAME POS MAY NOT BE APPROPRIATE
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SAME POS MAY NOT BE APPROPRIATE0----- Attempting Submission 1 (Tue Aug 13 22:36:11 GMT 2024) -----
----- Attempting Submission 2 (Sun Mar 02 23:00:34 GMT 2025) -----
HST Phase II Proposal 17719 successfully submitted.
Receipt: # 17719-2
----- Attempting Submission 3 (Sun Mar 02 23:01:11 GMT 2025) -----Warning (Orbit Planner): SAME POS MAY NOT BE APPROPRIATE
I want to observe the same target with 3 different filters with the same orientation. I think it is the right thing to do.Brighter than GN-z11? Grism Observations of the brightest z~11 Candidates found in COSMOS-WebWe have searched in the widest-field JWST survey (>0.5deg2) for rare, extremely bright high redshift candidates and we have identified several dozen candidates at z>10. Among these, two candidates could potentially surpass the brightness of GN-z11 (Oesch et al. 2016), the archetype "extremely bright" galaxy which happens to be the most luminous and distant galaxy ever found by HST with an absolute magnitude (M_UV) of -21.50 and a spectroscopic redshift of 10.6 (Bunker et al. 2023). We have found two spatially compact and isolated candidates at z~11 that we propose to target for WFC3/IR G141 grism observations. They are extremely bright, 10-50x brighter than other JWST sources at similar redshifts. With these observations we expect to distinguish between possible low-z interlopers (with strong emission lines) and a genuine z>10 source (via a Lyman break). This would allow us to ascertain the extent to which GN-z11 is unique or representative of these galaxies, and to unravel how these galaxies could form such substantial stellar mass only 500 million years after the Big Bang, challenging our current cosmological models. The confirmation of even one of these candidates is vital for testing these scenarios. However, without spectroscopy, definitive conclusions remain elusive, as the possibility of contamination from a low-redshift source with unusually strong emission lines cannot be entirely ruled out.For each galaxy, our observational strategy comprises three visits of two orbits each, employing two distinct orientations. We plan to capture a direct image with the F160W filter before each observation with the G141 grism. This will be instrumental for continuum/contamination modeling and to optimize data reduction. The same reference pixel will be utilized for both the F160W image and the G141 grism exposures.
To minimize the impact of background variations, we intend to execute the following pattern: direct F160W image, G141 grism exposure, followed by a dither offset, repeated four times per visit. This 4-point dithering strategy, coordinated with a variety of different orientations, will be effective in mitigating contamination from nearby sources.
This approach, mirroring successful methodologies from prior studies such as GN-z11 and the 3D-HST survey (e.g., Brammer et al. 2012), promises to deliver unprecedented insights into the nature and origins of these potentially groundbreaking z~10 candidates. A significant obstacle in grism spectroscopy is the systematic contamination of the target spec- trum by light emanating from adjacent galaxies. To avoid this, we carefully chose isolated galaxies where the range of available ORIENT angles will disperse the spectra in directions where the source spectrum will not be contaminated by neighbors. The Astronomer's Pro- posal Tool (APT) permits orientation angles for the COSMOS field ranging from 70 to 130 degrees. Given that the Wide Field Camera 3 (WFC3) instrument's position angle (PA) is fixed at 135.37 degrees, the allowable position angles on the sky for our observations fall within the range of 205.37 to 260.37 degrees.Our team brings together very strong skills in different fields which will allow us to successfully conduct this project. There are in particular experts in the manipulation of HST data, experts in very high redshift galaxies, experts in galaxy evolution, experts in simulations, experts in multiwavelength analysis and galaxy spectral energy distribution modeling.
Maximilien Franco (UT Austin) - expert in JWST/NIRCam data reduction, modelization and analysis of high redshift galaxies.
Caitlin Casey (UT Austin) is an expert in galaxy formation and evolution, co-PI of the COSMOS-Web survey, and has extensive experience in IR with ALMA.
Hollis Akins has extensive background in high-redshift galaxy evolution and is experienced working with a range of spectroscopic and photometric data products from HST, ALMA, and JWST.
Dr. Anton Koekemoer is an Observatory Scientist in the JWST NIRCam team at STScI, with scientific expertise in multiwavelength studies of distant galaxies and AGN, and has been the primary builder of the imaging mosaics and science data products for large HST programs including GOODS, CANDELS, COSMOS, HUDF, HFF, also involved with several large JWST surveys of the distant universe, incl CEERS, COSMOS-web, PRIMER, NGDEEP and others.
Steve Finkelstein is an expert in high-redshift galaxy evolution. He has significant experience in selection of high-redshift galaxies, measurement of their properties, and the evolution of the UV luminosity function. He is the PI of the CEERS Survey.
Andreas Faisst (Caltech/IPAC) is an expert in galaxy evolution studies and the formation of Epoch of Reionization galaxies. He has extensive expertise with imaging and grism data from HST
Jeyhan Kartaltepe (RIT) is an expert in the study of galaxy formation and evolution, co-PI of the COSMOS-Web survey, and has extensive experience with archival WFC3 grism spectroscopy in CANDELS.
Fabrizio Gentile is an expert in multi-band photometry and SED fitting, with a special expertise in the analysis of highly dust-obscured sourcesGalaxiesLarge Scale Structure of the Universe6falsefalsefalsefalsefalsefalseSUPPORTEDGALAXYHIGH REDSHIFT GALAXYNOJ2000J200025th mag at ~2um from JWST photometryGALAXYHIGH REDSHIFT GALAXYNOJ2000J2000~26 mag at 2um from JWST photometryWFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141ACS/WFCImagingNoNoF435WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF435WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141ACS/WFCImagingNoNoF435WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF435WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WHst Same orient constraint links visits (01 02 03)The scheduling data was generated by CASM 33.0.CASM was run in Phase II mode./Users/mf248874/Downloads/OP-cache/apt_hst-v01.xml(Tic-Visit
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)true20Hst Same orient constraint links visits (10 11 12)The scheduling data was generated by CASM 33.0.CASM was run in Phase II mode./Users/mf248874/Downloads/OP-cache/apt_hst-v12.xml(Tic-Visit
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:trans-version "20241216"
:date "19-Feb-2025 20:07:26.0"
:trans-errors '(:WARNINGS 2 :ERRORS 0 :HEALTH-AND-SAFETY 0
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(Tic-Obset
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)
(Tic-Orbit
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(Tic-Orbit
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)true20