no special comments.-1112066700Assigned ID: 422
----- Attempting Submission 1 (Fri Mar 06 08:33:43 GMT 2020) -----
HST Phase I Proposal 422 successfully submitted.
Receipt: # 422-1
----- Attempting Submission 2 (Fri Mar 06 13:51:24 GMT 2020) -----
HST Phase I Proposal 422 successfully submitted.
Receipt: # 422-2
----- Attempting Submission 3 (Fri Mar 06 15:03:26 GMT 2020) -----
HST Phase I Proposal 422 successfully submitted.
Receipt: # 422-3
----- Attempting Submission 4 (Fri Mar 06 22:56:35 GMT 2020) -----
HST Phase I Proposal 422 successfully submitted.
Receipt: # 422-4SAME 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 APPROPRIATEUpdated after first orbit conducted. Target is detected, suggesting a lower redshift than initially thought in the proposal. Hence, we require a change of grism to best target the Lyman-alpha line.
Using F098M for pre-imaging after consultation with co-investigators.
thanks,
Nick-714068895----- Attempting Submission 1 (Fri Jun 26 15:29:18 GMT 2020) -----
HST Phase II Proposal 16184 successfully submitted.
Receipt: # 16184-1
----- Attempting Submission 2 (Sat Jun 27 03:26:32 GMT 2020) -----
HST Phase II Proposal 16184 successfully submitted.
Receipt: # 16184-2
----- Attempting Submission 3 (Tue Jun 30 01:41:17 GMT 2020) -----
HST Phase II Proposal 16184 successfully submitted.
Receipt: # 16184-3
----- Attempting Submission 4 (Mon Jul 06 09:32:44 GMT 2020) -----
HST Phase II Proposal 16184 successfully submitted.
Receipt: # 16184-4
----- Attempting Submission 5 (Tue Jul 07 02:20:04 GMT 2020) -----
HST Phase II Proposal 16184 successfully submitted.
Receipt: # 16184-5
----- Attempting Submission 6 (Thu Nov 19 01:12:48 GMT 2020) -----
HST Phase II Proposal 16184 successfully submitted.
Receipt: # 16184-6
----- Attempting Submission 7 (Sat Nov 21 03:24:24 GMT 2020) -----SAME POS has been discussed and approved by contact scientistLyman-alpha Observations of a z=10.15 Powerful Radio GalaxyPowerful radio galaxies have been unique probes of the distant Universe for many decades. This proposal requests WFC3 grism and imaging observations to characterize the Lyman-alpha break/emission line in a redshift 10.15 powerful radio galaxy. This detection would be by far the most distant super-massive black hole (SMBH) and active galactic nucleus (AGN) known. At this redshift the radio galaxy would lie at the centre of a highly ionised Stromgren sphere ionised by star-formation, inverse Compton emission from the jets, and possibly accretion onto the SMBH. As well as reafirming the redshift of the host, these observations will potentially reveal the complex interaction of this radio-loud AGN with its local environment. Due to the poor transmission of the Earth's atmosphere, Hubble is the only facility which can conduct these observations.The aim of this proposal is to confirm the redshift of a candidate ultra-high redshift radio galaxy via a deep WFC3/IR grism spectrum. Far-infrared spectroscopy from ALMA initially suggested that it lies at z=10.1. However, an ALMA DDT, accepted after the Cycle 28 deadline, did not see the same lines. Furthermore, we have discovered deep optical data covering this source from the Subaray HSC-wide survey in which our target remains undetected up to i>25.5 (AB). Hence our source has an order of magnitude continuum break between 0.9um (i-band) and 2.2um (K-band). If this is the Lyman-alpha break, as we suspect, then this source must lie at z>7.3.
Our proposal consists of:
(i) one orbit of WFC3/IR imaging with F105W which was designed to be shortward of the Lyman-alpha break from the original redhift, thereby confirming the break. This is the first visit labelled F105Wimaging.
(ii) four orbits of WFC3/IR spectroscopy with G141 (using F160W for preimaging) comprised of two orbits in two different orientations. This is to obtain the Lyman-alpha line. Each orbit is contained in a separate visit and the visits labelled OR1x or OR2x for each of the two orientations, where x=a and b.
While this was not part of the original proposal we request that the one orbit of F105W imaging be conducted first. Then our choice of grisms for the spectroscopy will depend on whether the host galaxy is detected in that deep image or not as follows:
(a) if the host is detected in the F105W image then we request the grism is changed to G102 to cover the possibility of a lower redshift,
(b) if the host is not detected in the F105W then we stay with the original selection of G141.
In our deep K-band imaging from VLT/HAWKI, the host radio galaxy has another source nearby (likely at a lower redshift due to its detection at shorter wavelengths). Hence, we request our two orientations are chosen to avoid this source contaminating the spectrum of the host galaxy.
The position angles (east from north) from our deep K-band image we which to restrict the orientations to are:
70<PA<165
250<PA<245
Additionally we wish the second orientation to be offset from the first, but still within these original constraints. This is to avoid contamination of the spectrum by fainter sources we have not detected yet. We currently have this offset from OR1 at 30 to 150.This team has considerable experience in the study of distant radio galaxies, with core members having worked together on this subject for two decades. The team includes members who have studied radio galaxies across the electromagnetic spectrum including in the radio (100 MHz to 100 GHz), the far-infrared with ALMA and Herschel, the mid-infrared with Spitzer, the near-infrared from the ground and with HST, the optical from the ground and with HST, and in the X-ray. In particular, the team includes several members who have worked on publications using HST grism observations of radio galaxies and their environment. Hence, the team is well placed to rapidly exploit these observations once the data are obtained.Supermassive Black Holes and Active Galaxies6falsefalsefalsefalsefalsefalsefalseSUPPORTEDGALAXYHIGH REDSHIFT GALAXYRADIO GALAXYK_s flux from dedicated deep VLT/HAWKI imaging
Redshift unknown, but at least z>7.3NVSS091734-001242J2000J2000K_s(2.2um) = 3.07+/-0.12 uJyWFC3/IRSpectroscopicNoNoG141WFC3/IRImagingNoNoF105WPOS-TARGDITHER0.572LINE0.365falsefalse74.653418.528WFC3-IR-DITHER-BOX-MIN1false/Users/nseymour/work/proposals/proposed/hst/cycle28/z10_Lya_phase2.apt/z10_Lya_phase2_afterv1.apt/OP-cache/z10_Lya_phase2_afterv1-v01.xmlThe scheduling data was generated by CASM 28.2.CASM was run in Phase II mode.One orbit of imaging with WFC3/IR F105W:
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