Merge pull request #408 from jasondrhodes/master

changed WFIRST files

Author: drphilmarshall

whitepaper/WFIRST/WFIRST_microlensing.tex

@@ -33,7 +33,7 @@ \section{Exoplanetary Microlensing with WFIRST and LSST}
 a qualitative confirmation of this result, as dozens of additional
 short timescale events have been discovered by the MOA and OGLE
 alert systems, but we await details of the implied rogue planet
-populations that will come from detailed analyses of bot the MOA
+populations that will come from detailed analyses of both the MOA
 and OGLE samples.
 
 A major weakness with the microlensing data that indicates this
@@ -235,8 +235,10 @@ \subsection{Metrics}
 
 We can see from the final column that the LSST observations should
 yield more than 30 rogue planet microlensing parallax measurements and
-more than 10 rogue planet mass measurements. And these are measurements
-that cannot be made by other methods. In addition, this program would
+more than 10 rogue planet mass measurements. These are measurements
+that cannot be made by other methods. 
+\textbf{THE PREVIOUS SENTENCE NEEDS MORE JUSTIFICATION.}
+In addition, this program would
 also yield masses for a somewhat larger number of bound planets
 (Gould, Gaudi \& Han 2003), although many of these will have their
 masses determined by other means as well.

whitepaper/WFIRST/WFIRST_weaklensing.tex

@@ -17,11 +17,6 @@
 \section{Cosmology with the WFIRST HLS and LSST}
 \def\secname{\chpname:weaklensing}\label{sec:\secname}
 
-% note to Phil-  I am not sure if there will be another section that
-% serves as an intro to WFIRST, but I am doing that here also, I think we
-% should make this about more than just WL.  Can we change the name and
-% focus of the section to the High Latitude Survey.  The driver %is still
-% probably weak lensing!
 
 \credit{jasondrhodes}
 
@@ -31,7 +26,7 @@ \section{Cosmology with the WFIRST HLS and LSST}
 measurements) and NIR grism spectroscopy.  The benefits of overlapping
 spectroscopic and photometric surveys for dark energy constraints and
 systematics mitigation are strong.  The primary scientific driver of the
-photometric portion of the WFIRST HLS is weakg gravitational lensing,
+photometric portion of the WFIRST HLS is weak gravitational lensing,
 but there is a wide range of ancillary science that will be possible
 with the publicly available WFIRST HLS data (see for instance, the SDT
 report mentioned above).  However, the requirements on the HLS are
@@ -42,20 +37,20 @@ \section{Cosmology with the WFIRST HLS and LSST}
 WFIRST weak lensing survey will require the full  10-year LSST depth in
 4 optical bands for optimal photometric redsfhift determination}.
 
-There is strong benefit not just to WFIRT, but to LSST, in coordinating
+There is strong benefit not just to WFIRST, but to LSST, in coordinating
 observations of the WFIRST HLS survey field. The combination of
 full-depth LSST data and WFIRST HLS NIR data will provide the gold
 standard in photo-zs.  Furthermore, WFIRST grism observations over the
 same area will provide many millions of high quality slitless spectra
-and WFIRST’s IFU can be run in parallel with WFI observations to provide
+and WFIRST's IFC can be run in parallel with WFI observations to provide
 many more very accurate spectroscopic redshifts in the survey area.
 Thus, the WFIRST photometric data will help to provide better LSST
-photo-zs and  WFIRST will also provide many of the spectra needed for a
+photo-zs and  WFIRST will also provide many of the spectra needed as a
 training set to calibrate the photo-zs for both missions.  A further
 benefit to LSST might be the reduced need for LSST observations at the
 reddest end of the LSST wavelength range (the z and y filters), where
 both the atmosphere and the physics of CCDs make ground-based
-observations less efficient than what WFIRST can achieve. Finally, the
+observations less efficient than what WFIRST can achieve. Further work is needed to quantify this benefit, especially as the WFIRST proposed filter set is evolving.Finally, the
 joint processing of LSST and WFIRST data will provide better object
 deblending parameters than LSST can achieve alone; WFIRST will be able
 to provide a morphological prior for the deblending of LSST images.
@@ -85,9 +80,9 @@ \subsection{Target measurements and discoveries}
 WFIRST HLS. As LSST and WFIRST progress, there is a mutual benefit in
 continuing discussions about the optimal joint observation schedule.
 
-It is possible that the WFIRST data might allow for shallower LSST data
-in the reddest LSST filter in the overlap region, and this must be
-quantified.
+%It is possible that the WFIRST data might allow for shallower LSST data
+%in the reddest LSST filter in the overlap region, and this must be
+%quantified.
 
 
 % --------------------------------------------------------------------
@@ -105,7 +100,7 @@ \subsection{Metrics}
 useful to the US community (or anyone with immediate access to both
 WFIRST and LSST data).  WFIRST data is unlikely to have any proprietary
 period.  Current plans call for the WFIRST HLS to be conducted in
-multple passes, but the exact survey pattern is still undecided, so this
+multiple passes, but the exact survey pattern is still undecided, so this
 metric is also not quantifiable yet.
 
 There may be some reduced need for the the LSST reddest bands in the
@@ -133,7 +128,7 @@ \subsection{Discussion}
 science.  Every effort should be made to coordinate all discussions of
 increased survey cadence (resulting in full LSST depth well before 10
 years) over sub-areas of the LSST survey footprint.  Specific attention
-should be paid to whether the accelerated portions of the LSSt survey
+should be paid to whether the accelerated portions of the LSST survey
 can completely overlap the WFIRST HLS, and whether the position of the
 WFIRST HLS can be determined, in part, by other science drivers within
 LSST.  This will require close LSST and WFIRST coordination at the

whitepaper/wfirst.tex

@@ -18,6 +18,7 @@ \section{Introduction}
 % Introduce, with a very broad brush, this chapter's science projects,
 % and why it makes sense for them to be considered together.
 
+
 The Wide Field Infrared Survey Telescope (WFIRST) is a NASA mission that
 entered Phase A in February 2016.  WFIRST was the highest recommendation
 for large space missions in the 2010 New Worlds New Horizons Decadal
@@ -40,28 +41,28 @@ \section{Introduction}
 Guest Observer program.
 \end{itemize}
 
-WFIRST will be at L2 to enable the thermal stability required for the
+WFIRST will be at L2 to enable the thermal stability needed for the
 precise astrometric, photometric, and morphological measurements
 required for these science goals. The baseline WFIRST mission
 architecture is described in detail in the final report of the WFIRST
-Science Definition Team (arxiv/1503.03757). The Wide Field
+Science Definition Team (arxiv/1503.03757). The WFIRST Wide Field
 Instrument(WFI) has a NIR focal plane with a $\sim0.28$ square degree
-field of view made up 18 4k$\times$4k Teledyne H4RG NIR detectors will
+field of view made up 18 4k$\times$4k Teledyne H4RG NIR detectors and will
 have imaging capabilities from $0.7-2$ microns and grism spectroscopy
 capabilities from $1.35-1.89$ microns with $R\sim461\lambda$.  The WFI
-also contains an Integral Field Unit (IFU) spectrometer with $R\sim100$
-resolution over the range $0.42-2$ microns for SN follow up. The exoplanet
+also contains an Integral Field Channel (IFC) spectrometer with $R\sim100$
+resoluton over the range $0.6-2$ microns for SN follow up. The exoplanet
 coronagraph will have imaging ($0.43-0.97$ microns) and spectroscopic
 ($0.6-0.97 $ microns) capabilities with a contrast ratio of 1 part in a
 billion.
 
-WFIRST's  6 year primary mission will have 2 years dedicated to a
+WFIRST's  6 year primary mission is envisioned to have 2 years dedicated to a
 $\sim2200$ square degree High Latitude Survey (HLS) for weak lensing and
 galaxy clustering,  1 year of microlensing observations divided into 6
 seasons, $0.6$ years of SN search and follow-up, one year dedicated to
 the coronagraph and 1.4 years dedicated to competitively selected Guest
 Observer observations. WFIRST has no expendables that would prevent an
-extended mission of 10 years or longer, and an extended mission would be
+extended mission of 10 years or longer, and an extended mission will likely be
 given over entirely to Guest Observer observations.
 
 The synergy with LSST is very promising indeed. In this chapter we aim
@@ -72,6 +73,7 @@ \section{Introduction}
 we propose as new \OpSim simulation runs.
 
 
+
 % --------------------------------------------------------------------
 
 \input{WFIRST/WFIRST_weaklensing.tex}