0Assigned ID: 3178
----- Attempting Submission 1 (Fri Mar 25 10:03:17 GMT 2022) -----SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE
SAME POS MAY NOT BE APPROPRIATE0----- Attempting Submission 1 (Thu Jul 14 03:06:13 GMT 2022) -----
HST Phase II Proposal 17117 successfully submitted.
Receipt: # 17117-1
----- Attempting Submission 2 (Tue Feb 07 01:30:52 GMT 2023) -----
----- Attempting Submission 3 (Sat Feb 11 21:18:51 GMT 2023) -----We already consulted with our Contact Scientist (CS) about the remaining warnings.
These are our intentional setups, and we believe there shouldn't be a problem.A complete census of quiescent galaxies in the dense core of the Spiderweb protocluster at z=2.16We propose deep (7-orbit) WFC3/IR G141 spectroscopy of the central region of the best-studied galaxy cluster in formation - the "Spiderweb" protocluster at z=2.16 - to blindly search for and characterize quiescent members in the dense core of the protocluster. We will measure the stengths of the 4000A break (Dn4000) and the equivalent widths of the H-delta absorption line for all cluster member galaxies in the single WFC3 FoV (~1.5cMpc x1.5cMpc). This enables us to determine the formation redshifts (z_f) of individual cluster members and identify recently quenched galaxies (post-starbursts), allowing us to test if massive cluster galaxies are formed at much earlier epoch (at z>>4), or if a majority of them are recently quenched. Importantly, in addition to the rich multi-wavelength datasets collected over the last ~20 years, the scheduled JWST/NIRCam Cycle-1 GO program and ALMA Cycle-8 program for wide-field 1.1mm mapping will unveil the obscured star-formation in the Spiderweb protocluster through Paschen-beta and dust continuum. By mapping the internal distribution of star-forming and quenched/quenching pixels within the protocluster members - our ultimate goal is to reveal how the quenching event is triggered and propagated within massive cluster galaxies. Do the quenched region always propagate in an inside-out fashion? Or, does it happen simultaneously throughout the disk? The proposed WFC3 observations are critical to identify the quiescent members, and with the scheduled JWST observations, we will finally have a complete census of all cluster members of this structure at the peak epoch of star-formation, black hole and molecular gas activity.The aim of this proposal is to perform a slitless WFC3/IR G141 grism spectroscopy in the central region of the Spiderweb protocluster at z = 2.16. The primary spectrum order of the G141 grism covers lambda=1.07-1.72um with a spectral resolution of R~130. This wavelength range covers the major rest-optical spectral features of the protocluster member galaxies at z=2.16 such as [OII]3727, Hb4861, [OIII]5007, Hd4102, and the 4000A break. With a single pointing of WFC3 FoV (2'x2'; equivalently 1.5x1.5 Mpc^2 in the comoving scale), we can efficiently observe a variety of galaxies situated in the protocluster core environment. To avoid overlapping of the spectra in dense environments, we request three different ORIENT.
The proposed target is visible for 53min in one orbit. Following the standard overhead calculation described in the WFC3 Instrument Handbook, we will spend 9min for overheads per orbit, including guide star acquisition, filter change, camera setup, and readouts. Also we request a short direct imaging (undispersed) with F160W filter (~5-min) to calibrate target positions and wavelengths. By subtracting these overhead times from the available orbit visibility of the target (53min), we can take 38min science exposure for grism spectroscopy. Our goal is to obtain a total 234min science exposure with G141 grism. To achieve this goal, we need 7 orbits in total.The team is organized by co-PIs + co-Is of the scheduled JWST Cycle-1 GO 1572.
Co-PI Yusei Koyama is an assistant professor at the Subaru Telescope in Hawaii, USA. He has an expertise in observational astrophysics, and has led a number of research papers based on multi-wavelength wide-field observations of distant clusters/protoclusters over the last decade, including the target of this proposal (Spiderweb). He is the co-PI of the companion programs of the Spiderweb field: JWST/NIRCam Cycle-1 GO program (GO1572) and the ALMA deep fields scheduled in Cycle-8 (2021.1.00435.S).
Co-PI Helmut Dannerbauer is a staff researcher at the Instituto de Astrofisica de Canarias. He is an expert on the search of galaxy overdensities traced via dusty star-forming galaxies and characterization of their members via multi-wavelength datasets. He is also the co-PI of the companion of the Spiderweb field: JWST/NIRCam Cycle-1 GO program (GO1572) and the ALMA deep fields in Cycle-8 (2021.1.00435.S).
Co-I Tadayuki Kodama is professor and the head of Astronomical Institute, Tohoku University, who has been an expert on the research of clusters and protoclusters over the past 25 years, in particular on optical-NIR imaging (including narrow-band emitter imaging) and spectral evolution of stellar populations.
Co-I Rhythm Shimakawa is an assistant professor at National Astronomical Observatory of Japan. He has led analysis of protocluster galaxies at the cosmic noon based on optical and infrared data. Since he holds the master catalogue of our targets, our team can start the data analysis from a vantage point.
Co-I Jose Manuel Perez-Martinez is a postdoctoral researcher at Tohoku University with experience in the reduction and analysis of optical and NIR spectrophotometric data. His research is currently focused on the influence of the environment over cluster galaxy populations at intermediate to high redshift.
Co-I Rosa Calvi is a postdoctoral researcher at the Instituto de Astrofisica de Canarias. She is the PI of a new KMOS (VLT/ESO) program of the Spiderweb protocluster targeted in this HST proposal.
The team also includes two PhD students - Abdurrahman Naufal (Graduate School for Advanced Science in Japan) and Zhengyi Chen (the Instituto de Astrofisica de Canarias in Spain) - both working under the supervision of the co-PIs of this proposal (Yusei Koyama and Helmut Dannerbauer). They are expected to play leading roles in the data analyses of this program.GalaxiesLarge Scale Structure of the Universe6falsefalsefalsefalsefalsefalsefalsefalseSUPPORTEDCLUSTER OF GALAXIESGROUPRICH CLUSTERJ2000J2000J<23.9 (AB mag), H<23.0 (AB mag)CLUSTER OF GALAXIESGROUPRICH CLUSTERJ2000J2000J<23.9 (AB mag), H<23.0 (AB mag)CLUSTER OF GALAXIESGROUPRICH CLUSTERJ2000J2000J<23.9 (AB mag), H<23.0 (AB mag)CLUSTER OF GALAXIESGROUPRICH CLUSTERJ2000J2000J<23.9 (AB mag), H<23.0 (AB mag)CLUSTER OF GALAXIESGROUPRICH CLUSTERJ2000J2000J<23.9 (AB mag), H<23.0 (AB mag)CLUSTER OF GALAXIESGROUPRICH CLUSTERJ2000J2000J<23.9 (AB mag), H<23.0 (AB mag)CLUSTER OF GALAXIESGROUPRICH CLUSTERJ2000J2000J<23.9 (AB mag), H<23.0 (AB mag)WFC3/IRSpectroscopicNoNoG141WFC3/IRImagingNoNoF160WWFC3/IRSpectroscopicNoNoG141WFC3/IRImagingNoNoF160WWFC3/IRSpectroscopicNoNoG141WFC3/IRImagingNoNoF160WThe scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.168309267300080.0(Tic-Visit
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