0
Assigned ID: 430
----- Attempting Submission 1 (Fri Aug 17 21:46:33 GMT 2018) -----
HST Phase I Proposal 430 (Wband_HST_cycle26.apt) successfully submitted.
Receipt: # 430-1
----- Attempting Submission 2 (Fri Aug 17 21:56:07 GMT 2018) -----
HST Phase I Proposal 430 (Wband_HST_cycle26.apt) successfully submitted.
Receipt: # 430-2
----- Attempting Submission 3 (Fri Aug 17 23:17:35 GMT 2018) -----
HST Phase I Proposal 430 (Wband_HST_cycle26.apt) successfully submitted.
Receipt: # 430-3
Update 18 December 2019: shortened visit 22 to improve schedulability
Update 4 February 2020: added repeat of visit 37
Update 26 November 2019: added repeat observation for Serpens 5
Update 9 July 2019: after change request accepted, replaced F850LP observations in Visit 2 (CFHT-Oph-WIR-57) with F105W and F153M.
Update 10 June 2019: reduced the exposure time for Visit 16 (Taurus 13) to make it schedulable with new scheduling changes.
This should be a complete submission for the whole program. Two outstanding concerns:
1) The Serpens objects are all in very extincted regions with few to no Gaia objects. Are there appropriate guide stars available for these targets?
2) I am not sure if I set the special requirements on ORIENT correctly for the Taurus followup visits. Orient ranges for Taurus followup visit 1 were set to avoid placing the candidate companion on a diffraction spike.
In Taurus followup visit 1, I set an "ORIENT from" requirement, by 90-120 degrees from Taurus followup visit 1. As long as the roll angle difference between visits is >5 degrees or so, it's not important what the actual
roll angle is -- I set 90-120 degrees to again try to avoid placing the candidate companion on a diffraction spike, so if the "ORIENT from" requirement should be set differently, please let me know.
236942954
----- Attempting Submission 1 (Tue Dec 04 20:35:59 GMT 2018) -----
----- Attempting Submission 2 (Tue Jun 11 00:21:29 GMT 2019) -----
----- Attempting Submission 3 (Tue Jul 09 14:12:57 GMT 2019) -----
----- Attempting Submission 4 (Tue Nov 26 13:19:10 GMT 2019) -----
----- Attempting Submission 5 (Wed Dec 18 16:24:28 GMT 2019) -----
----- Attempting Submission 6 (Tue Feb 04 13:44:14 GMT 2020) -----
I only ran the orbit and visit planner on visit 87, as all other visits have already been scheduled
A search for sub-Jupiter mass companions to young planetary mass brown dwarfs
We propose for HST WFC3 follow-up imaging of a newly discovered population of brown dwarf / planetary mass members of Taurus and Serpens, with the goal of imaging the lowest mass object to date, potentially down to sub-Jupiter mass objects. The number of known L-type planetary mass objects in Taurus has increased by an order of magnitude in the last two years, from 1 known L to 16. L-type members of Taurus have estimated masses of 2-7 MJup at ages of 1-10 Myr, thus any companions to these objects will have even lower masses. Thus, this is the first chance to probe multiplicity properties for a purely planetary mass population. This project potentially offers the opportunity to study the atmospheres of sub-Jupiter mass objects similar to those that will be eventually imaged around young stars with future ELT instrumentation and missions such as LUVOIR. HST is critical for this project. HST WFC3 is the only instrument capable of high-resolution imaging in and out of the 1.45 um water absorption feature which uniquely identifies substellar and planetary mass objects. Using a reddening insensitive index built from photometry in the F850LP, F127M, and F139M filters, we will be able to immediately distinguish bonafide companions from the reddened background stars that are the dominant source of contaminants.
This program has two main goals: 1) identify new planetary mass candidate companion to recently discovered brown dwarfs in young star-forming regions and 2) confirm / refute candidate companions detected to two young brown dwarfs, via either common proper motion confirmation or color analysis.
Strategy by target type:
1) First epoch targets: these are new brown dwarf members of Taurus or Serpens we've identified as part of an ongoing ground-based survey. The survey combined observations in J and H band with observations in a custom filter centered on the 1.45 um water absorption feature seen in objects with spectral types later than M6. Combining these filters, we defined a reddening insensitive index Q which acts as a proxy for spectral type (based on the depth of the water absorption feature). A similar reddening insensitive index can be set up using the F850LP, F127M, and F139M filters with WFC3 to use HST to search for clearly substellar or planetary mass companions to our new Taurus and Serpens brown dwarf objects. This requires that we obtain deep enough observations in each of these 3 filters within 1 orbit per target. To balance image quality / psf sampling and depth, we use 3-point line dithers with sub-arrays (to allow fast enough readout for multiple short exposures) in all three filters.
2) followup target Oph 57: this is a candidate companion with clear water absorption identified as part of GO 12944 -- in fact, it dropped out entirely in the F139M filter in the first epoch observation. Followup observations in program GO 14686 were ambiguous, but an additional astrometric point in 2019/2020 should unambiguously confirm or refute this candidate. We devote 2 orbits to this object: the first for a deep, full-frame 4-point dither in F850LP, the second for high S/N detections in F125W and F160W (full-frame, 4-point dither). F125W and F160W are the closest correlates to 2MASS J and H on HST. These colors will provide valuable characterization information for this candidate companion. Since we have J and H photometry for the primary already, if we can measure the contrast of the candidate companion, we can compare J-H colors for the primary vs. the candidate. If the candidate is bluer than the primary, then it's background, but if it has similar or redder colors that would be a good indication that it is a likely bound companion.
3) followup target Taurus 7: this has a close-in (<1"), faint candidate companion detected using adaptive optics on the Keck telescope.
The first epoch observation was in November 2017; given the small proper motion of Taurus, common proper motion confirmation is not yet possible for this object (that will probably require a 3-4 year baseline). The goal of the HST epoch, in contrast, is detection in F125M and F139M in order to detect water absorption and roughly determine the spectral type of this object. We also include an F850LP observation, but given the faintness of the primary and the dmag of the companion, if the companion is detected in F850LP it is almost certainly a background star (we predict an F850LP magnitude of ~25 if it is a bound companion). Thus, photometry is more important than astrometry here. We devote two orbits for this object as well, split into two visits, with the second visit in a different ORIENT range than the first, to enable higher contrasts via roll angle subtraction, as done for a similar (but brighter) brown dwarf - exoplanet binary 2M1207 in Song et al. 2006. We will acquire two dither positions per filter per visit, for four dithers total. POSTARG values for dither positions are taken from the WFC3-IR-DITHER-BOX-MIN pattern.
Planets and Planet Formation
Stellar Physics
6
false
false
false
false
false
false
false
SUPPORTED
STAR
BROWN DWARF
NO
J2000
J2000
J=17.5+-0.2, M9
STAR
BROWN DWARF
NO
J2000
J2000
J=17.9+-0.2, M9
STAR
BROWN DWARF
J2000
J2000
J=16.5+-0.1, M9
STAR
BROWN DWARF
J2000
J2000
J=17.4+-0.2, L0
STAR
BROWN DWARF
J2000
J2000
J=16.81+-0.17, L0 (Best et al. 2017)
STAR
BROWN DWARF
J2000
J2000
J=16.93+-0.14, L0 (Best et al. 2017)
STAR
BROWN DWARF
J2000
J2000
J=13.78+-0.02, L0 (Zhang et al. 2018)
STAR
BROWN DWARF
J2000
J2000
J=16.69+-0.12, L0.7 (Zhang et al. 2018)
STAR
BROWN DWARF
J2000
J2000
J=16.77+-0.12, M9.25 (Esplin & Luhman 2017)
STAR
BROWN DWARF
J2000
J2000
J=17.2, early L primary
STAR
BROWN DWARF
J2000
J2000
J=17.0, Late M / Early L
STAR
BROWN DWARF
J2000
J2000
J=17.6, L4
STAR
BROWN DWARF
J2000
J2000
J=16.5, M9.9 (Zhang et al. 2018)
STAR
BROWN DWARF
J2000
J2000
J=15.6, M9.1 (Zhang et al. 2018)
STAR
BROWN DWARF
J2000
J2000
J=16.1, M9.5 (Zhang et al. 2018)
STAR
BROWN DWARF
J2000
J2000
J=16.0, M9.7 (Zhang et al. 2018)
STAR
BROWN DWARF
J2000
J2000
Ks=14.5, M9.5 (Esplin & Luhman 2017)
STAR
BROWN DWARF
J2000
J2000
Ks=15.1, M9.5 (Esplin & Luhman 2017)
STAR
BROWN DWARF
J2000
J2000
Ks=15.9, M9-L2 (Esplin & Luhman 2017)
STAR
BROWN DWARF
J2000
J2000
Ks=15.2, M9.5 (Esplin & Luhman 2017)
STAR
BROWN DWARF
J2000
J2000
Ks=13.8, M8.5 (Esplin & Luhman 2017)
STAR
BROWN DWARF
J2000
J2000
Ks=15.4, M9.5 (Esplin & Luhman 2017)
STAR
BROWN DWARF
J2000
J2000
J=17.1, late M / early L
STAR
BROWN DWARF
J2000
J2000
J=16.6, late-M
STAR
BROWN DWARF
J2000
J2000
J=15.06, M7.25
STAR
BROWN DWARF
J2000
J2000
J=16.3, M9
STAR
BROWN DWARF
J2000
J2000
J=18.4, M8
STAR
BROWN DWARF
J2000
J2000
J=16.4, M6.5
STAR
BROWN DWARF
J2000
J2000
J=18.6, M6.5
STAR
BROWN DWARF
J2000
J2000
J=17.93, M8
STAR
BROWN DWARF
J2000
J2000
J=17.7, M8
STAR
BROWN DWARF
J2000
K=15.24+-0.03 (UKIDSS)
STAR
BROWN DWARF
J2000
J = 17.06+-0.03, K=15.58+-0.02 (UKIDSS)
STAR
BROWN DWARF
J2000
JHKs = 16.6, 15.8, 15.1, M9-L1
STAR
BROWN DWARF
J2000
JHKs = 17.2, 16.4, 15.5, M9-L1
STAR
BROWN DWARF
J2000
JHKs = 17.1, 16.2, 15.4, M9-L1
STAR
BROWN DWARF
J2000
JHKs = 17.2, 16.4, 15.4, M9
STAR
BROWN DWARF
J2000
JHKs = 15.7, 15.2, 14.6, M9
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/UVIS
Imaging
No
No
F850LP
POS-TARG
DITHER
0.572
LINE
0.365
false
false
74.653
4
18.528
WFC3-IR-DITHER-BOX-MIN
2
false
POS-TARG
DITHER
0.135
LINE
false
false
3
46.84
WFC3-UVIS-DITHER-LINE-3PT
3
false
POS-TARG
DITHER
3.25
LINE
false
false
3
41.788
WFC3-IR-DITHER-LINE-3PT
4
false
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