correcting a few typos before posting to ArXiv

paper/master.tex

@@ -153,7 +153,7 @@
 rotational behavior of stars whose rotation periods do not lengthen with the
 square-root of time, and parts of the Hertzsprung-Russell diagram where
 gyrochronology has not been calibrated.
-This publication is accompanied by an open source {\it Python} package (\sd)
+This publication is accompanied by an open source {\it Python} package, \sd,
 for inferring the ages of main-sequence and subgiant FGKM stars from rotation
 periods, spectroscopic parameters and/or apparent magnitudes and parallaxes.
 \end{abstract}
@@ -173,7 +173,7 @@ \section{Introduction}
 On the MS, isochrones are tightly spaced and, even with very precise
 measurements of effective temperature and luminosity, the position of a MS
 star on the HRD may be consistent with range of isochrones spanning several
-billion years.
+billion years \citep[see][for a review of stellar ages]{soderblom2010}.
 At the main-sequence turnoff however, isochrones are spread further apart, so
 that sufficiently precisely measured temperatures and luminosities can yield
 ages that are extremely precise (with minimum statistical uncertainties on the
@@ -389,12 +389,14 @@ \subsection{A new empirical gyrochronology relation}
 In order to fit a relation to Praesepe, we removed rotational outliers bluer
 than \gcolor\ = 2.7 via sigma-clipping and fit a 5th-order polynomial to the
 remaining FGK and early M stars.
-\racomment{We found that a 5th order polynomial provided a substantially
+% \racomment{
+    We found that a 5th order polynomial provided a substantially
 better fit than lower-order polynomials, which were not able to capture the
 sharp `elbow’ in the rotation period-color relation. Additional orders
 provided either a worse
 fit, tending towards extreme values at the boundaries, or diminishing returns
-in goodness-of-fit.}
+in goodness-of-fit.
+% }
 We also fit a straight line to the late M dwarfs (\gcolor\ $>$ 2.7), to
 capture the mass-dependent initial rotation periods of low mass stars
 \citep{somers2017}.
@@ -812,7 +814,7 @@ \subsection{Test 1: simulated stars}
 & D \sim U(10, 1000)~\mathrm{[pc]} \\
 & A_V \sim U(0, 0.1).
 \end{eqnarray}
-\teff, \logg, \fhat, parallax, and apparent magnitudes $B$, $V$, $J$, $H$, $K$,
+\teff, \logg, [Fe/H], parallax, and apparent magnitudes $B$, $V$, $J$, $H$, $K$,
 \gaia\ $G$, $G_{BP}$ and $G_{RP}$ were generated from these
 stellar parameters using the MIST stellar evolution models.
 We added a small amount of noise to the `observed' stellar properties in order
@@ -969,7 +971,7 @@ \subsection{Test 1: simulated stars}
 
 An important caveat associated with these results is that they strongly depend
 on the uncertainties adopted for all observables used in the analysis: \teff,
-\feh, \logg, $G$, $G_BP$, $G_RP$, $J$, $H$, $K$, $B$, $V$, and rotation
+\feh, \logg, $G$, $G_{BP}$, $G_{RP}$, $J$, $H$, $K$, $B$, $V$, and rotation
 period.
 Changing the uncertainties on these observables will affect the uncertainties
 on inferred ages in different ways.
@@ -1101,7 +1103,7 @@ \subsection{Test 2: Open clusters}
 cluster and figure \ref{fig:NGC6819_results} shows the results of inferring
 the ages of individual cluster members using a combination of gyrochronology
 and isochrone fitting (via \sd) and isochrone fitting alone.
-The ages of F stars in this cluster (\gcolor\ $\sim$ 5.5-6.5) were relatively
+The ages of F stars in this cluster (\gcolor\ $\sim$ 0.5-0.75) were relatively
 precisely constrained by isochrone fitting alone because, at 2.5 Gyr, they are
 approaching the MS turnoff.
 For these hot stars, ages inferred with gyrochronology and isochrones were
@@ -1201,7 +1203,8 @@ \subsection{Test 2: Open clusters}
 functions do not provide them.
 % In general, formal rotation period uncertainties should probably be calculated
 % empirically via simulations as in the \citet{aigrain2015} study.
-\racomment{Ideally, rotation period uncertainties should capture {\it both} the
+% \racomment{
+    Ideally, rotation period uncertainties should capture {\it both} the
 measurement precision, {\it and} the physical uncertainty introduced by the
 latitudinal movement of star spots on the surface of a differentially rotating
 star.
@@ -1223,10 +1226,12 @@ \subsection{Test 2: Open clusters}
 measurement uncertainty and physical variation, affect stellar ages via
 gyrochronology is key to understanding the power of gyrochronology as an
 age-dating method.
-For now, we leave this exploration for a future study.}
+For now, we leave this exploration for a future study.
+% }
 
 \subsection{Test 3: Kepler asteroseismic stars}
-\racomment{In order to test our method in the regime where both isochrone
+% \racomment{
+    In order to test our method in the regime where both isochrone
 fitting and gyrochronology become important, we recovered the ages of the 21
 asteroseismic stars analysed in \citet{vansaders2016}.
 These 21 stars were observed in \kepler's short cadence mode and are a mixture
@@ -1269,9 +1274,9 @@ \subsection{Test 3: Kepler asteroseismic stars}
 The white circles show ages inferred from isochrones only.
 Dashed lines connect the three different age measurements for the same
 stars.
-}
+% }
 
-\racomment{
+% \racomment{
 Although the ages of all 21 stars shown in figure \ref{fig:astero} were
 inferred with a joint isochronal and gyrochronal model, most (all but 8) were
 either too evolved, too metal poor, or too metal rich for gyrochronology to
@@ -1285,9 +1290,9 @@ \subsection{Test 3: Kepler asteroseismic stars}
 relatively hot.
 % Isochrones are information-rich for these hot and old stars, and this is
 % exactly where gyrochronology is at its most information-poor.
-}
+% }
 
-\racomment{
+% \racomment{
 In general, there is relatively poor agreement between the asteroseismic ages
 and the ages inferred using \sd.
 Much of this discrepancy is driven by differences in the isochronal ages,
@@ -1302,9 +1307,9 @@ \subsection{Test 3: Kepler asteroseismic stars}
 between the two sets of models can be as large as 1-2 billion years.
 The MIST isochrones lie above the BaSTI isochrones on the HR diagram, leading
 to a systematic underprediction of ages.
-}
+% }
 
-\racomment{
+% \racomment{
 The gyrochronal ages, where gyrochronology is applicable, do not show
 excellent agreement with the asteroseismic ages either.
 The four hot stars to the left in figure \ref{fig:astero} are rotating more
@@ -1330,7 +1335,7 @@ \subsection{Test 3: Kepler asteroseismic stars}
 It is the only clear SB1 in the \citet{vansaders2016} sample, although some
 others do have binary companions with long orbital periods, for which tidal
 interactions are not expected to be strong.
-}
+% }
 
 \begin{figure}
     \caption{ A comparison of stellar ages inferred using
@@ -1382,7 +1387,7 @@ \section{Conclusions}
 Although V-band extinction is marginalized over during inference, correcting
 photometry for dust-extinction before analysis, or including it as a
 prior can improve the accuracy of stellar ages measured with \sd.
-\racomment{
+% \racomment{
 We also tested \sd\ on a set of 21 \kepler\ asteroseismic stars
 \citep{vansaders2016}.
 We found that discrepancies between ages measured with \sd\ and ages measured
@@ -1397,7 +1402,7 @@ \section{Conclusions}
 period depends on age, mass, metallicity, surface gravity, etc), many stars
 with precise ages, spanning a range of properties, are still needed to
 reliably calibrate them.
-}
+% }
 
 In cases where gyrochronology predicts inaccurate stellar ages it is either
 because models are not correctly calibrated, because the rotation periods or

paper/ms.tex

@@ -80,14 +80,10 @@
 \newcommand{\Eep}{Equivalent evolutionary point}
 
 % \newcommand{\racomment}[1]{{\color{blue}#1}}
-\newcommand{\racomment}[1]{{\bf #1}}
+% \newcommand{\racomment}[1]{{\bf #1}}
 
 \begin{document}
 
-% \title{Inferring stellar ages by combining isochrone fitting with
-% gyrochronology}
-% \title{A new age-dating model for cool main sequence stars that combines
-% isochrone fitting with gyrochronology}
 \title{Towards precise stellar ages: combining isochrone fitting with
 empirical gyrochronology}