0
Assigned ID: 1209
----- Attempting Submission 1 (Fri Apr 07 23:59:32 GMT 2017) -----
0
----- Attempting Submission 1 (Sun Jul 30 13:41:45 GMT 2017) -----
HST Phase II Proposal 15355 (nao.apt) successfully submitted.
Receipt: # 15355-1
----- Attempting Submission 2 (Sun Jul 30 13:42:23 GMT 2017) -----
----- Attempting Submission 3 (Mon Sep 11 17:54:19 GMT 2017) -----
----- Attempting Submission 4 (Thu Jan 17 17:31:22 GMT 2019) -----
dropped visit start date
Perfect Blackbody Spectra for JWST and Next Generation UV-Opt-IR Standard Star Network
We propose to observe 18-19th magnitude objects with nearly perfect blackbody spectra discovered by the Sloan Digital Sky Survey. Follow-up observation by Keck/LRIS and Subaru/FOCAS confirmed no signs of absorption lines, and SDSS multi-epoch observation shows no time variation. With WFC3 (UVES/IR), we will establish a new network of Opt-IR Standards at 0.1% precision in magnitude from 0.1 micron through 5 micron. The identify of these objects are yet to be known. We conduct precise parallax measurements and find distances to these objects that enables us to infer the radius of these stars, and we may have a potential discovery of new type of objects.
Only two parameters (Effective Temperature and Normlization) are needed to describe the blackbody spectra, and we can predict magnitudes in any band from UV through IR with high precision. We will advance the way we peform the photometry by introducing the covariance matrix between the filter bands. This covariance matrix would reduce the errors in color and propagate systematic errors in an appropriate way, and we can reduce the systematic errors in SNIa cosmology today. The perfect blackbody spectrum is the most elegant solution for JWST photometric standards and next generation UV-Opt-IR photometry.
We will conduct precise photometry of 7 stars with the WFC3 camera.
During Cycle 25 we observe these stars in UVIS broad band filters (F225W, F275W, F336W, F438W, F555W, F606W, F814W and F850LP) in the C512C subarray in multiple dithers with each filter sufficient to achieve S/N of 200 at 18-19th magnitude. F606W is repeated in the second orbit for each star, 6 months apart so that we can measure parallax to infer distances to the stars.
Stellar Physics
Cosmology
0
false
false
true
false
true
false
false
SUPPORTED
STAR
DC
J2000
J2000
STAR
DC
J2000
J2000
STAR
DC
J2000
J2000
STAR
DC
J2000
J2000
STAR
DC
J2000
J2000
STAR
DC
J2000
J2000
STAR
DC
J2000
J2000
WFC3/UVIS
Imaging
No
No
F218W
WFC3/UVIS
Imaging
No
No
F225W
WFC3/UVIS
Imaging
No
No
F275W
WFC3/UVIS
Imaging
No
No
F336W
WFC3/UVIS
Imaging
No
No
F390W
WFC3/UVIS
Imaging
No
No
F438W
WFC3/UVIS
Imaging
No
No
F475W
WFC3/UVIS
Imaging
No
No
F555W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F775W
WFC3/UVIS
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/UVIS
Imaging
No
No
F218W
WFC3/UVIS
Imaging
No
No
F225W
WFC3/UVIS
Imaging
No
No
F275W
WFC3/UVIS
Imaging
No
No
F336W
WFC3/UVIS
Imaging
No
No
F390W
WFC3/UVIS
Imaging
No
No
F438W
WFC3/UVIS
Imaging
No
No
F475W
WFC3/UVIS
Imaging
No
No
F555W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F775W
WFC3/UVIS
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/UVIS
Imaging
No
No
F218W
WFC3/UVIS
Imaging
No
No
F225W
WFC3/UVIS
Imaging
No
No
F275W
WFC3/UVIS
Imaging
No
No
F336W
WFC3/UVIS
Imaging
No
No
F390W
WFC3/UVIS
Imaging
No
No
F438W
WFC3/UVIS
Imaging
No
No
F475W
WFC3/UVIS
Imaging
No
No
F555W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F775W
WFC3/UVIS
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/UVIS
Imaging
No
No
F218W
WFC3/UVIS
Imaging
No
No
F225W
WFC3/UVIS
Imaging
No
No
F275W
WFC3/UVIS
Imaging
No
No
F336W
WFC3/UVIS
Imaging
No
No
F390W
WFC3/UVIS
Imaging
No
No
F438W
WFC3/UVIS
Imaging
No
No
F475W
WFC3/UVIS
Imaging
No
No
F555W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F775W
WFC3/UVIS
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/UVIS
Imaging
No
No
F218W
WFC3/UVIS
Imaging
No
No
F225W
WFC3/UVIS
Imaging
No
No
F275W
WFC3/UVIS
Imaging
No
No
F336W
WFC3/UVIS
Imaging
No
No
F390W
WFC3/UVIS
Imaging
No
No
F438W
WFC3/UVIS
Imaging
No
No
F475W
WFC3/UVIS
Imaging
No
No
F555W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F775W
WFC3/UVIS
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/UVIS
Imaging
No
No
F218W
WFC3/UVIS
Imaging
No
No
F225W
WFC3/UVIS
Imaging
No
No
F275W
WFC3/UVIS
Imaging
No
No
F336W
WFC3/UVIS
Imaging
No
No
F390W
WFC3/UVIS
Imaging
No
No
F438W
WFC3/UVIS
Imaging
No
No
F475W
WFC3/UVIS
Imaging
No
No
F555W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F775W
WFC3/UVIS
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/UVIS
Imaging
No
No
F218W
WFC3/UVIS
Imaging
No
No
F225W
WFC3/UVIS
Imaging
No
No
F275W
WFC3/UVIS
Imaging
No
No
F336W
WFC3/UVIS
Imaging
No
No
F390W
WFC3/UVIS
Imaging
No
No
F438W
WFC3/UVIS
Imaging
No
No
F475W
WFC3/UVIS
Imaging
No
No
F555W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F775W
WFC3/UVIS
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F850LP
WFC3/UVIS
Imaging
No
No
F606W
WFC3/IR
Imaging
No
No
F105W
WFC3/IR
Imaging
No
No
F110W
WFC3/IR
Imaging
No
No
F125W
WFC3/IR
Imaging
No
No
F140W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/IR
Imaging
No
No
F105W
WFC3/IR
Imaging
No
No
F110W
WFC3/IR
Imaging
No
No
F125W
WFC3/IR
Imaging
No
No
F140W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/IR
Imaging
No
No
F105W
WFC3/IR
Imaging
No
No
F110W
WFC3/IR
Imaging
No
No
F125W
WFC3/IR
Imaging
No
No
F140W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/IR
Imaging
No
No
F105W
WFC3/IR
Imaging
No
No
F110W
WFC3/IR
Imaging
No
No
F125W
WFC3/IR
Imaging
No
No
F140W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/IR
Imaging
No
No
F105W
WFC3/IR
Imaging
No
No
F110W
WFC3/IR
Imaging
No
No
F125W
WFC3/IR
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No
No
F140W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/IR
Imaging
No
No
F105W
WFC3/IR
Imaging
No
No
F110W
WFC3/IR
Imaging
No
No
F125W
WFC3/IR
Imaging
No
No
F140W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/IR
Imaging
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No
F105W
WFC3/IR
Imaging
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No
F110W
WFC3/IR
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No
F125W
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F140W
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Spectroscopic
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Spectroscopic
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Spectroscopic
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No
G141
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Spectroscopic
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Spectroscopic
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No
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No
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G141
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G141
WFC3/UVIS
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WFC3/UVIS
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WFC3/IR
Spectroscopic
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G102
WFC3/IR
Spectroscopic
No
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G141
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