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Assigned ID: 1695
----- Attempting Submission 1 (Wed Mar 21 23:31:46 GMT 2018) -----
HST Phase I Proposal 1695 (HST.apt) successfully submitted.
Receipt: # 1695-1
----- Attempting Submission 2 (Wed Mar 21 23:56:13 GMT 2018) -----
HST Phase I Proposal 1695 (HST.apt) successfully submitted.
Receipt: # 1695-2
0
----- Attempting Submission 1 (Wed May 30 23:20:29 GMT 2018) -----
HST Phase II Proposal 15464 (hstphaseII.apt) successfully submitted.
Receipt: # 15464-1
----- Attempting Submission 2 (Tue Sep 11 22:10:15 GMT 2018) -----
----- Attempting Submission 3 (Mon Sep 17 21:21:27 GMT 2018) -----
Visit Planner has been run for the new visit (Visit 10) which is a repeat observation of the failed visit 02.
0
Resolving the Stellar Histories of Herschel-Red Dusty Star Forming Galaxies at z~4
We have identified a sample of eight z~4 objects from a new class of powerful high-redshift dusty, star forming galaxies through their rising Herschel SPIRE flux densities and spectroscopic redshifts. A complete, multiwavelength analysis of these objects would increase the sample size of known z~4 SPIRE 'red' starbursts with accurate stellar mass profiles more than two times over, helping to bridge the evolutionary gap between z~2 and z~6 DSFGs, and between high redshift starburst galaxies and their massive 'red-and-dead' counterparts at z=1-2. The deep rest-frame optical observations required for the stellar mass estimates of these galaxies has not yet been observed. Moreover, we recently obtained deep corresponding IRAC images that show clear counterparts to the starbursts, but the true nature of this near-IR emission is elusive due to the blended IRAC image. With the large IRAC PSF, we cannot determine if the near-IR emission is in fact a massive lensing foreground galaxy, or indeed the rest-frame optical emission of the high-z star-forming galaxy(s). We also now have complementary high-resolution ALMA images that suggest complex structures and/or multiple objects are creating the extreme far-IR intensities. To fully understand the nature of these structures, we must understand both their stellar mass and dust mass distributions, the former of which requires high resolution WFC3 observations to de-blend, and potentially de-magnify, the IRAC images. The proposed high resolution WFC3 F125W imaging of each object is crucial to resolve IRAC counterparts, extend individual SEDs into the rest-frame optical regime, and measure more reliable stellar masses than ever before.
The goal of this program is to (a) detect and characterize the profile of any potential foreground lensing galaxy or galaxies, and/or (b) measure the rest-frame UV emission of z~4 dusty, starforming galaxies (DSFGs). HST data will also be used to de-blend/resolve the detected Spizter IRAC flux into the appropriate components, using gravitational lensing source plane reconstruction tools where necessary. Combined, these measurements will inform the optical/UV end of the DSFG spectral energy distributions, thereby constraining their stellar masses, gas masses and mass to light ratios.
To achieve these goals, we will use the WFC3 F125W band with an integration time of 48 minutes per target to achieve a S/N > 5 (WFC3IR.im.1155145), including a four-point dither pattern to better sample the PSF. This integration time is sufficiently long to capture a potential z = 1-2 foreground lensing elliptical galaxy at a S/N > 10. In ALMA imaging, the morphologies of each of the eight z~4 sources is different, with typical dust emission extending about 1 arcsec in diameter across.
Galaxies and the IGM
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