0Assigned ID: 1936
----- Attempting Submission 1 (Fri Apr 09 14:39:49 GMT 2021) -----Please find attached the our submitted Phase II Proposal 16693. We have tried to limit each visit to a maximum of 3 orbits as per the support astronomer's instructions,
and have added comments to every visit highlighting the number of orbits, orient constraints, etc. Please let us know in case any clarifications may be needed.
Regards,
Aayush Saxena
Co-PI-1873780331----- Attempting Submission 1 (Mon Jul 26 19:54:29 GMT 2021) -----The host galaxy and environment of a radio galaxy near the epoch of reionizationRadio-loud active galactic nuclei (RLAGN) are the most luminous radio sources in the Universe, and RLAGN at high-z are important for studying the formation of massive galaxies and supermassive black holes (SMBHs). The discovery of a radio galaxy at z=5.72 (TGSS J1530+1049) has pushed studies of RLAGN closer to the epoch of reionization (EoR). HST imaging of other high-z radio galaxies has shown that such systems are massive, with intense star-formation. They exhibit complex morphologies, large sizes and are frequently surrounded by overdensities of faint galaxies, indicative of a forming cluster environment. TGSS J1530+1049 at z=5.72 offers an opportunity to now investigate these phenomena at z~6, and we propose deep multi-band HST imaging with ACS and WFC3 to image the radio galaxy and its close companions, searching for overdensities on scales of 5 Mpc (co-moving) in its environment.
TGSS J1530+1049 is a JWST NIRCam GTO target and is the subject of an approved Cycle 1 NIRSpec/IFU program. It benefits from high-resolution VLBI radio imaging of its AGN jets and is an approved Chandra target. The combination of these proposed HST observations with JWST data will result in maps of the distribution of stellar mass and measurements of star-formation rate, dust, ionisation state and metallicity of the gas. Correlating the rest-UV morphology with AGN jets and constraining the evolutionary stage of the stellar populations are crucial to understand AGN feedback in massive galaxies near the EoR. Further, rest-frame UV HST imaging will allow the identification of any nearby companions through Lyman break selection, which will not be possible from the NIRCam data alone.This is a proposal to obtain deep ACS and WFC3 images of the most distant radio selected galaxy currently known, TGSS J1530+1049 at z = 5.72.
The ACS observations will be done in F606W, F775W and F850LP, and the WFC3 observations in F105W, F125W and F160W. Our choice for these filters is driven by the need to: (i) obtain deep multi-wavelength imaging for accurate characterisation of the rest UV morphology and the physical properties of the host galaxy for TGSS1530, which will complement forthcoming JWST NIRCam and NIRSpec observations, and (ii) optimize the selection of z~6 galaxies in the vicinity of TGSS1530 using the standard (i775-z850) versus (Y105-H160) color diagram, with the V606 needed to identify foreground interlopers (i.e., S/N(V606) < 2 or V606-z850 > 2.7), and the J125 and H160 filters needed to identify background (i.e., z > 7) galaxies.
The WFC3 images in F105W, F125W and F160W will probe the UV continuum red- wards of Lya, giving crucial measures of the UV continuum slopes, and star-formation rates. We will perform standard dithered imaging with the ACS/WFC and WFC3/IR chan- nels to close the ACS/WFC gap, improve the PSF and remove bad pixels and cosmic rays. Besides this color-based selection, accurate multi-band photometry can be used to obtain reliable photometric redshifts, which are sufficient for making a first cut of galaxy candidates that are plausibly part of any large-scale structure associated with TGSS1530.
The depth of the filters are primarily motivated by the need to accurately constrain the size and morphology of TGSS1530 and robustly detect the radio galaxy host across a broad range of wavelengths. With these HST observations we will also be able to probe sufficiently down the luminosity function of z~6 star-forming galaxies in the vicinity of TGSS1530 to study large-scale structure around this RLAGN.
We require a limiting S/N ~ 2 down to 29AB in V606, and a S/N ~ 5 in i775 and z850 down to 27.7AB and 27.2AB, respectively. The IR bands will also be used to measure the sizes and morphologies of both TGSS1530 and nearby dropouts, and therefore, need to be slightly deeper with 5sigma point source sensitivities (AB) of: Y105 = 27.4, J125 = 27.3, and H160 = 27.0. These limiting depths have been indicated in Figure 4 (horizontal bars). Therefore, assuming a typical orbit duration with 2000s on-source exposures, we request 3 orbits in V606, 4 in i775, 5 in z850, 2 in Y105, 2 in J125, and 2 in H160, for a total of 18 orbits.
We will use dithering in all observations to improve image quality. For ACS observations, we use a "line" pattern to fill the detector gaps, and within each pattern we use a "box" dithering pattern to improve image quality. For WFC3 observations, we use a "blob" dithering pattern. These dithering patters are included in every visit/orbit, and help to maximise the science exposure time per orbit. Particularly for WFC3 exposures, the individual expososures are close to the optimum exposure times recommended in the intstrument handbook.
The ORIENT of the first ACS visit has been chosen to most closely reproduce the roll angle restrictions for planned JWST NIRCam GTO observations. The ORIENT of every subsequent ACS visit has been made to be the same as the first visit. There are no ORIENT constraints for WFC3 visits owing to the smaller field of view, but the ORIENT of subsequent WFC3 visits have been set to be the same as the first WFC3 visit.
Total time requested: 18 orbits are requested to observe one field in 6 filters.The team is highly experienced in the fields of observational cosmology and galaxy formation.
The PI, Dr. Overzier has 18 years of experience analysing and working with HST data (ACS, WFC3, COS), including many projects similar in nature to the current proposal.
The co-PI, Dr. Saxena - together with Prof. Best, Dr. Duncan, Prof. Miley, Dr. Overzier, Dr. Pentericci and Prof. Rottgering - discovered the target of this proposal and is involved with several follow-up campaigns across wavelengths.
Dr. Onoue, Dr. Banados, Dr. Mazzucchelli and Dr. Venemans are leading a VLT narrowband Lya imaging program on the proposed target and its environment, along with a NOEMA program on the target.
Prof. Heckman is an expert in studying the effects of feedback from starbursts and AGN on galaxies, and a is experienced HST user.
The entire team has broad experience in the selection and study of high redshift galaxies, including star-forming galaxies, quasars, and radio galaxies, their black holes, host galaxies and environments from a multi-wavelength perspective. Members of the team are also experienced in the processing of cosmological simulations that are used to interpret these HST data.Supermassive Black Holes and Active GalaxiesGalaxies6falsefalsefalsefalsefalsefalsefalseSUPPORTEDGALAXYHIGH REDSHIFT GALAXYRADIO GALAXYNOTGSS1530J2000J2000z-band 25 to 27 magACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF775WACS/WFCImagingNoNoF850LPWFC3/IRImagingNoNoF105WWFC3/IRImagingNoNoF125WWFC3/IRImagingNoNoF160WPOS-TARGDITHERDITHER43.034ACS-WFC-DITHER-BOXfalse68.14false0.1920.262385.29POS-TARGACS-WFC-DITHER-LINE18.391truePOS-TARGDITHERDITHER43.034ACS-WFC-DITHER-BOXfalse68.14false0.1920.262285.29POS-TARGACS-WFC-DITHER-LINE18.393truePOS-TARGDITHERDITHER42WFC3-IR-DITHER-BOX-MINfalse74.653true0.3650.5721241.859POS-TARGWFC3-IR-DITHER-BLOB18.5282falsePOS-TARGDITHERDITHER23.034ACS-WFC-DITHER-LINEfalsefalse0.145285.29POS-TARGACS-WFC-DITHER-LINE47.234trueHst Same orient constraint links visits (01 02 03 04 05)The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.Single visit using the F606W filter consisting of 3 orbits for the target TGSS J1530+1049. The dither line pattern has been used to fill the gap between the detectors, and a box sub-pattern has been used to improve image quality. The orient constraints have been introduced to match the JWST NIRCam GTO observations of TGSS J1530+1049. The orients of all subsequent visits using ACS are the same as F606_visit1.1660459542000107.0(Tic-Visit
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:si-vis-utilization 2480
:al-overhead-at-end 0
:internal-dur-at-end 690
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3149
:pcs-gap 0
)true20