deletions | additions
diff --git a/Classification.tex b/Classification.tex
index 25e75a0..f582a24 100644
--- a/Classification.tex
+++ b/Classification.tex
...
luminosities for each event as a function of magnification and time of
peak (or, equivalently, the decline time).
Figure~\ref{fig:PeakLuminosityDeclineTimeWide} shows Figures~\ref{fig:PeakLuminosityDeclineTimeWide} and
\ref{fig:PeakLuminosityDeclineTime} show the resulting
constraints on the peak luminosity and the decline time, which we
quantify as $t_2$, the time over which the transient declines by 2
magnitudes. Shaded green and red bands represent the \spockone and
...
the most overlap) would be $L_{\rm pk}\sim10^{41}$ ergs/s and
$t_3\sim1.8$ days.
\subsection{Comparison to SN and SN-like Explosion Models}
In %In Figure~\ref{fig:PeakLuminosityDeclineTimeWide} we also demarcate
regions %regions of the
luminosity - decline luminosity--decline time phase space occupied by known
or %or theorized
SN-like transients.
\subsection{Supernova-like Transients}
The colored regions along the right side of
Figure~\ref{fig:PeakLuminosityDeclineTimeWide} mark the luminosity and
decline times for SNe and SN-like
transients, showing
that the very rapid rise and fall of both \spock light curves is
incompatible with any of the normal SN classes. For both
thermonuclear white dwarf explosions (Type Ia) and the core-collapse
explosions of massive stars (Type Ib, Ic, and II) the optical light
curve after reaching peak brightness is primarily powered by transients. This includes the
decay familiar luminosity-decline relation of
radioactive \NiFiftySix to \CoFiftySix, which leads to a minimum
decline rate of $\sim$0.1 mag day$^{-1}$. For Type
II Ia SNe
this decay
time can be extended into a plateau phase by the recession of the
photosphere via a recombination wave propagating inward through the
ionized H of the expanding outer shell. In no case can a normal SN
powered by the \NiFiftySix decay chain exhibit the decline rate of
$t_3<8$ days that has been observed for \spock. Furthermore, the
observed peak luminosities for both \spock events are too low for most
Type I or Type II SN, which peak at $\sim10^{42}$ to $10^{43}$ erg
s$^{-1}$.
Figure~\ref{fig:PeakLuminosityDeclineTimeWide} also shows that the
\spock events are far too faint \citep{Phillips:1993} and
far too fast to belong to the
broad heterogeneous class of Core
Collapse SNe, as well as less well-understood classes
of such as
Superluminous SNe \citep{Gal-Yam:2012,Arcavi:2016},
which have peak luminosities
$>10^{43}$ erg s$^{-1}$ and take at least 10's of days to decline by 2
magnitudes. \spockone and \spocktwo also decline too rapidly to match
the most common categories of peculiar SNe and ``SN-like'' transients
such as Type Iax SNe
\citep{Foley:2013a}, fast optical transients \citep{Drout:2014},
and
Ca-rich SNe \citep{Filippenko:2003,Perets:2011,Kasliwal:2012}, or
Luminous Red Novae \citep[also called intermediate luminosity red
transients][]{Munari:2002,Kulkarni:2007,Kasliwal:2011}. transients][]{Munari:2002,Kulkarni:2007,Kasliwal:2011b}. The \spock
events are incompatible with all of these explosion categories,
owing to the very rapid rise and fall of both \spock light curves, and
their relatively low peak luminosities of $\sim10^{41}$ erg s$^{-1}$.
Dashed boxes in Figure~\ref{fig:PeakLuminosityDeclineTimeWide}
represent categories of
``SN-like'' stellar explosions that have been
theoretically predicted and extensively modeled, but for which very
few viable candidates have actually been observed.
One Both of these
is
the ``.Ia'' class, due categories come closer to
explosions of a He shell on the surface of a
white dwarf \citep{Bildsten:2007}. Theoretical .Ia models suggest
that after an initial short peak (3-5 days) driven by the rapid
radioactive decay of \ion{Cr}{48} and \ion{Fe}{52} at matching the
exterior observed characteristics of the
ejecta, a secondary decline phase kicks in, powered by the slower
\ion{Ni}{56} decay chain \citep{Shen:2010}. There are only
two
.Ia
candidates in the literature \citep{Poznanski:2010,Kasliwal:2010}, so
we do not have enough objects to empirically constrain the range of
.Ia light curve shapes. The best we can do is to conclude from the
available models that a .Ia light curve would be brighter and slower
than the observed \spock
light curves.
A second dashed box in Figure~\ref{fig:PeakLuminosityDeclineTimeWide}
represents the ``kilonova'' class (also events, so they warrant closer scrutiny.
\subsubsection{Kilonova}
Also called
``Macronovae'' a ``macronova'' or
``mini-supernovae''), which are ``mini-supernova,'' this is theorized
to optical transients that may be generated by the merger of
two a neutron
stars (NSs). star (NS) binary. A NS+NS merger can drive a relativistic jet that may be
observed as a Gamma Ray Burst (GRB) and would emit gravitational
waves. These may also be accompanied by a very rapid optical light
curve (the kilonova component) that is driven by the radioactive decay
of r-process elements in the ejecta
\citep{Li:1998a,Kulkarni:2005}. \citep{Li:1998,Kulkarni:2005}. To
date there are two cases of fast optical transients associated with
GRB events, which have been interpreted as possible kilonovae
\citep{Perley:2009,Tanvir:2013}. The \spock transients fall within
the range of theoretically predicted peak luminosity and decline times
for kilonovae. However, the rise time for the \spockone event is at
least 5 days in the rest-frame, which is significantly longer than the
$<1$ day rise expected for a kilonova
\citep[e.g.][]{Metzger:2010,Barnes:2013,Kasen:2015}. Furthermore,
both \spock events are either significantly fainter or faster than the
optical light curves for the two existing kilonova candidates.
An additional challenge to all of \subsubsection{.Ia Supernova}
The dashed oval in Figure~\ref{fig:PeakLuminosityDeclineTimeWide}
represents the
models discussed above, from
supernova to .Ia ``.Ia'' class of He shell explosion
\citep{Bildsten:2007}. These are theorized to
kilonova, is arise from AM Canum
Venaticorum (AM CVn) systems, which are binary star systems
transferring He onto a C/O or O/Ne WD primary
\citep{Warner:1995,Nelemans:2005}. \citet{Bildsten:2007} showed that
all of
these
stellar explosions
are one-time events. For systems can build up enough He on the
common categories surface of
Type Ia, Type Iax,
Core Collapse, and Superluminous SNe, the
progenitor stars are
completely destroyed by WD to
trigger a thermonuclear runaway and possibly a detonation. A typical
AM CVn system could produce $\sim$10 He shell flashes over $\sim10^6$
yr, while the
explosion. Some SN-like explosions --
such as He mass transfer rate is slow enough to admit thermally
unstable burning in the
WD's accreted He shell. The final He shell
explosions in flash is the
.Ia SN model -- could leave brightest, and is what we refer to as the
progenitor star at least partially intact. However, even then .Ia event. This
last explosion may or may not lead to a detonation of the
mass lost from WD core
\citep[the double detonation
scenario][]{Nomoto:1982a,Nomoto:1982b,Woosley:1986;Woosley:1994}.
Theoretical .Ia models suggest that the
system light curves would be
sufficient quite
bright, reaching a peak luminosity of $\sim10^{42}$ erg s$^{-1}$.
That is comparable to
fatally disrupt the
mass accretion process, preventing brightness of a normal SN, but the
system from evolving back to
generate another similar explosion. These catastrophic stellar
explosions are also intrinsically rare (fewer than 1 event per century
per 10$^11$ \Msun), as they require progenitor systems .Ia light
curves would decline much more quickly. After an initial short peak
(3-5 days) driven by the rapid radioactive decay of \isotope{48}{Cr}
and \isotope{52}{Fe} at the exterior of the ejecta, a secondary
decline phase kicks in, powered by the slower \isotope{56}{Ni} decay chain
\citep{Shen:2010}. The optical emission is expected to fade by 2
magnitudes after $\sim10$ days. There have been a few viable .Ia
candidates presented in the literature
\citep{Kasliwal:2010,Perets:2010,Poznanski:2010}, but we do not have
enough objects to empirically constrain .Ia light curve shapes.
Although the \spock light curves were somewhat fainter and faster than
the expectations for a .Ia event, there is enough uncertainty about
the diversity of .Ia light curves that
start as high
mass stars and/or close binary systems this model should not be
dismissed on those merits alone.
\subsubsection{The Recurrence Problem}
An additional challenge for applying any SN-like transient model to
explain the \spock events is the problem of the apparent
recurrence. For all of these catastrophic stellar explosions we do
not expect to see repeated transient events: the kilonova progenitor
system is completely destroyed by the merger, and for the .Ia
explosions the principal observed transient event is the last
transient episode that
can sustain mass transfer. system produces. Even if we suppose that an AM
CVn system could produce repeated He shell flashes of similar
luminosity, the period of recurrence would be of order $10^5$ yr,
making these effectively non-recurrent sources.
Thus, the only way to reconcile
a these cataclysmic explosion
model models
with the two observed \spock events is to either (a)
invoke a highly
serendipitous occurrence of two unrelated explosions in the same host
galaxy in the same year, or (b) assert that the
two events are two images of the same
explosive event, explosion, appearing to us
separately only because of a gravitational lensing time delay
\citep[as was the case for the 5 images of SN
Refsdal][]{Kelly:2015a,Kelly:2016}.
For the former scenario of two unrelated explosions, we have already
ruled out all of the most common categories of stellar explosions
based on the properties of the light curve. The only models that can
accommodate the observed rapid light curves are the kilonova model and
perhaps the .Ia scenario. As there are no measured rates of .Ia Refsdal][]{Kelly:2015a,Kelly:2016}, or
kilonovae, it is difficult to accurately quantify the likelihood of
detecting such rare events. However, we have observed no other
transients with similar luminosity and light curve shapes in the
high-cadence surveys (b) invoke a highly
serendipitous occurrence of
5 other Frontier Fields clusters. Thus, it
appears unreasonable to allow that two
such unrelated peculiar explosions
would occur in the
same
host galaxy in
a single the same year.
Scenario (b), To evaluate scenario (a), in which a lensing time delay causes the
appearance of two
separate events,
is
also highly implausible. we must rely on the available lens
modeling. We have seen in Section~\ref{sec:LensingModels} that none of
the \macs0416 lens models predict an 8 month time delay between
appearances in image 11.1 and 11.2. This is represented in
Figure~\ref{fig:SpockDelayPredictions}, where we have plotted the
light curves for the two transient events, along with shaded vertical
bars marking the time delay predictions of all models.
%The lens models are broadly consistent with each other, predicting
%that the lensing time delay between images 11.1 and 11.2 is on the
%order of $\pm$60 days, far short of the 238 day lag that was observed
%between \spockone\ and \spocktwo.
To accept
the alternative single-explosion this time-delayed single explosion explanation for \spock,
we would have to assume that a large systematic bias is similarly
affecting all of the lens models. While we cannot rule out such a
bias, the consistency of the lens modeling makes
any catastrophic
(i.e., non-repeating) explosion model this scenario less
tenable.
For the latter scenario of two unrelated explosions, it is difficult
to assess the likelihood of such an occurrence quantitatively, as
there are no measured rates of .Ia or kilonovae. In a study of very
fast optical transients with the Pan-STARRS1 survey,
\citet{Berger:2013b} derived a limit of $\lesssim0.05$ Mpc$^{-3}$
yr$^{-1}$ for transients reaching $M\approx -14$ mag on a timescale of
$\sim$1 day. This limit, though several orders of magnitude higher
than the constraints on novae or SNe, is sufficient to make it
exceedingly unlikely that two such transients would appear in the same
galaxy in a single year. Furthermore, we have observed no other
transients with similar luminosities and light curve shapes in our
high-cadence surveys of 5 other Frontier Fields clusters. Indeed, all
other transients detected in the core Frontier Fields survey have been
fully consistent with normal SNe. Thus, we have no evidence to
suggest that transients of this kind are much more common at $z\sim1$.
\subsection{Luminous Blue Variable}
The transient events labeled as luminous blue variables (LBVs) are the
result of eruptions or explosive episodes on massive stars
($>10$\Msun) \citep[for an overview of recent work,
see][]{Smith:2011b}. Although the association with massive stars is
well established, this class is very heterogeneous and there is
currently a vigorous debate over the precise nature of the progenitor
pathway \citep{Smith:2015,Humphreys:2016,Smith:2016}. Examplified by
the well-studied galactic examples of P Cygni and $\eta$ Carinae
(\etacar), the ``Great Eruptions'' of such massive stars are sometimes
labeled as ``SN impostors.''
The transient episodes can exhibit light
curves reminiscent of core collapse SNe, reaching peak absolute
magnitudes of $\sim$-7 to -16 mag in optical bands, and lasting for
tens to hundreds of days.
The peak absolute magnitudes of observed giant LBV events span a range
of -10 to -18 mag, so the luminosities of the two \spock transients
are fully compatible. Most giant LBV eruptions have been
consistently observed to last much longer than the \spock events,
requiring tens to hundreds of days to fade by 2 magnitudes
\citep{Smith:2011b}. Some LBV stars
These stars commonly exhibit repeated
variability, with stochastic episodes of minor eruptions punctuated by
major SN impostor episodes, in some cases culminating with a final
true core collapse SN event
\citep[e.g.]{Mauerhan:2013,Tartaglia:2016}
Foley:2007,Pastorello:2007,Smith:2010b,GalYam:2009,}.
The LBV scenario does not
have any trouble accounting for the \spock events as two separate
episodes. However, in addition to the relatively short and very
bright giant eruptions, these massive stars also commonly exhibit a
slower underlying variability that has not been observed at the \spock
locations. P Cygni and \etaCar, for example, slowly rose and fell in
brightness by $\sim$1 to 2 mag over a timespan of several years before
and after their historic giant eruptions. Given the wide variation in
light curve properties for LBV events, this class must be held up as a possible
explanation for the \spock system, though the observed \spock events would stand out as the most rapid LBV major eruptions
\subsection{Recurrent
Nova Model} Nova}
Novae are represented in
Figure~\ref{fig:PeakLuminosityDeclineTimeWide} as a grey band, which
...
constraints from the two published kilonova candidates are shown,
which provide only lower limits on the peak luminosity
\citep{Tanvir:2013}, or the decline timescale \citep{Perley:2009}.
Two .Ia candidates are also plotted, SN 2002bj \citep{Poznanski:2010}
and SN 2010X \citep{Kasliwal:2010}. The sample of observed nova
outbursts (shown as solid points) demonstrates the observed scatter
about the MMRD relation.
One primary
first line of evidence supporting the nova hypothesis
comes from the \spock light curves.
Some Many RN light curves are similar
in shape to the \spock episodes, exhibiting a sharp rise ($<10$ days
in the rest-frame) and a similarly rapid decline.
Figure~\ref{fig:RecurrentNovaLightCurveComparison} compares the \spock
...
sudden disappearance of both of the \spock transient events is fully
consistent with the eruptions of known RNe in the local universe.
The
rise time of the \spock events is somewhat out of the ordinary for
nova outbursts. In particular, for recurrent nova eruptions that
decline rapidly ($t_2<10$ days) they tend to also reach peak
brightness very quickly, on timescales $<1$ day
\citep{Schaefer:2010}. The 2014 eruption of the rapid-recurrence nova
M31N 2008a-12 reached maximum brightness in a little under 1 day
\citep{Darnley:2015}. However, the rise time for nova eruptions is
poorly constrained, as rapid-cadence imaging is rarely secured until
after an initial detection near peak brightness. Unlike the situation
with a kilonova light curve, there is no a priori physical expectation
for an especially rapid rise to peak in nova light curves.
A second reason to consider the RN model is that it provides a
natural explanation for having two separate explosions that are
coincident in space but not in time. If \spock is a RN, then the two
observed episodes can be attributed to two distinct nova eruptions,
...
possible, classifying \spock as a RN would still require a very
extreme mass transfer rate to accommodate the $<1$ year recurrence.
A second Another major concern with the RN hypothesis for \spock is apparent
in Figure~\ref{fig:PeakLuminosityDeclineTime}, which shows that the
two \spock events are substantially brighter than all known novae --
perhaps by as much as 2 orders of magnitude. One might attempt to
...
{\rm more inconsistent} with observed nova peak luminosities.
\todo{Lpk vs recurrence period}
\subsection{Non-explosive \section{Non-explosive Astrophysical Transients}
There are several categories of astrophysical transients that we have
neglected so far, but which cannot accommodate the observations of the
diff --git a/HostGalaxy.tex b/HostGalaxy.tex
index d2f62ac..8dfe418 100644
--- a/HostGalaxy.tex
+++ b/HostGalaxy.tex
...
originated from the same physical location in the source plane. One
way to test this is to compare the properties of the \spock host
galaxy at the location of each event. To that end, we used the
techniques technique of ``pixel-by-pixel'' SED fitting as described in
\citet{Hemmati:2014} to determine rest-frame colors and stellar
properties in a single resolution element centered at each transient
location. For this purpose we used the deepest possible stacks of HST
diff --git a/bibliography/biblio.bib b/bibliography/biblio.bib
index 5380f71..49123dc 100644
--- a/bibliography/biblio.bib
+++ b/bibliography/biblio.bib
...
%% This BibTeX bibliography file was created using BibDesk.
%% http://bibdesk.sourceforge.net/
%% Created for rodney at
2016-07-14 17:45:44 2016-07-16 17:38:38 +0200
%% Saved with string encoding Unicode (UTF-8)
@article{Foley:2011,
Author = {{Foley}, R.~J. and {Berger}, E. and {Fox}, O. and {Levesque}, E.~M. and {Challis}, P.~J. and {Ivans}, I.~I. and {Rhoads}, J.~E. and {Soderberg}, A.~M.},
Journal = {\apj},
Month = may,
Pages = {32},
Title = {{The Diversity of Massive Star Outbursts. I. Observations of SN2009ip, UGC 2773 OT2009-1, and Their Progenitors}},
Volume = 732,
Year = 2011}
@article{Smith:2010,
Author = {{Smith}, N. and {Miller}, A. and {Li}, W. and {Filippenko}, A.~V. and {Silverman}, J.~M. and {Howard}, A.~W. and {Nugent}, P. and {Marcy}, G.~W. and {Bloom}, J.~S. and {Ghez}, A.~M. and {Lu}, J. and {Yelda}, S. and {Bernstein}, R.~A. and {Colucci}, J.~E.},
Journal = {\aj},
Month = apr,
Pages = {1451-1467},
Title = {{Discovery of Precursor Luminous Blue Variable Outbursts in Two Recent Optical Transients: The Fitfully Variable Missing Links UGC 2773-OT and SN 2009ip}},
Volume = 139,
Year = 2010}
@article{Smith:2016,
Author = {{Smith}, N.},
Journal = {ArXiv e-prints},
Month = jul,
Title = {{The isolation of Luminous Blue Variables: On subdividing the sample}},
Year = 2016}
@article{Smith:2011b,
Author = {{Smith}, N. and {Li}, W. and {Silverman}, J.~M. and {Ganeshalingam}, M. and {Filippenko}, A.~V.},
Journal = {\mnras},
Month = jul,
Pages = {773-810},
Title = {{Luminous blue variable eruptions and related transients: diversity of progenitors and outburst properties}},
Volume = 415,
Year = 2011}
@article{Smith:2011c,
Author = {{Smith}, N. and {Frew}, D.~J.},
Journal = {\mnras},
Month = aug,
Pages = {2009-2019},
Title = {{A revised historical light curve of Eta Carinae and the timing of close periastron encounters}},
Volume = 415,
Year = 2011}
@article{Davidson:2012,
Author = {{Davidson}, K. and {Humphreys}, R.~M.},
Journal = {\nat},
Month = jun,
Pages = {E1},
Title = {{The Great Eruption of {$\eta$} Carinae}},
Volume = 486,
Year = 2012}
@article{Foley:2007,
Author = {{Foley}, R.~J. and {Smith}, N. and {Ganeshalingam}, M. and {Li}, W. and {Chornock}, R. and {Filippenko}, A.~V.},
Journal = {\apjl},
Month = mar,
Pages = {L105-L108},
Title = {{SN 2006jc: A Wolf-Rayet Star Exploding in a Dense He-rich Circumstellar Medium}},
Volume = 657,
Year = 2007}
@article{Smith:2015,
Author = {{Smith}, N. and {Tombleson}, R.},
Journal = {\mnras},
Month = feb,
Pages = {598-617},
Title = {{Luminous blue variables are antisocial: their isolation implies that they are kicked mass gainers in binary evolution}},
Volume = 447,
Year = 2015}
@article{Humphreys:2016,
Author = {{Humphreys}, R.~M. and {Weis}, K. and {Davidson}, K. and {Gordon}, M.~S.},
Journal = {\apj},
Month = jul,
Pages = {64},
Title = {{On the Social Traits of Luminous Blue Variables}},
Volume = 825,
Year = 2016}
@article{Tartaglia:2016,
Author = {{Tartaglia}, L. and {Pastorello}, A. and {Sullivan}, M. and {Baltay}, C. and {Rabinowitz}, D. and {Nugent}, P. and {Drake}, A.~J. and {Djorgovski}, S.~G. and {Gal-Yam}, A. and {Fabrika}, S. and {Barsukova}, E.~A. and {Goranskij}, V.~P. and {Valeev}, A.~F. and {Fatkhullin}, T. and {Schulze}, S. and {Mehner}, A. and {Bauer}, F.~E. and {Taubenberger}, S. and {Nordin}, J. and {Valenti}, S. and {Howell}, D.~A. and {Benetti}, S. and {Cappellaro}, E. and {Fasano}, G. and {Elias-Rosa}, N. and {Barbieri}, M. and {Bettoni}, D. and {Harutyunyan}, A. and {Kangas}, T. and {Kankare}, E. and {Martin}, J.~C. and {Mattila}, S. and {Morales-Garoffolo}, A. and {Ochner}, P. and {Rebbapragada}, U.~D. and {Terreran}, G. and {Tomasella}, L. and {Turatto}, M. and {Verroi}, E. and {Wo{\'z}niak}, P.~R.},
Journal = {\mnras},
Month = jun,
Pages = {1039-1059},
Title = {{Interacting supernovae and supernova impostors. LSQ13zm: an outburst heralds the death of a massive star}},
Volume = 459,
Year = 2016}
@article{Gaskell:2003,
Author = {{Gaskell}, C.~M. and {Klimek}, E.~S.},
Journal = {Astronomical and Astrophysical Transactions},
...
Volume = 721,
Year = 2010}
@article{Smith:2011, @article{Smith:2011a,
Author = {{Smith}, N. and {Li}, W. and {Filippenko}, A.~V. and {Chornock}, R.},
Journal = {\mnras},
Month = apr,
diff --git a/figures/peakluminosity_vs_declinetime/caption.tex b/figures/peakluminosity_vs_declinetime/caption.tex
index c9dea31..da811a6 100644
--- a/figures/peakluminosity_vs_declinetime/caption.tex
+++ b/figures/peakluminosity_vs_declinetime/caption.tex
...
\label{fig:PeakLuminosityDeclineTime}
Peak luminosity vs. decline time for \spock and other rapidly
evolving declining transients. Constraints for \spockone
and \spocktwo are
plotted as overlapping
cyan and blue colored bands,
corresponding to independent constraints drawn from the F435W and F814W light curves, respectively. For \spocktwo the scarlet as in
Figure~\ref{fig:PeakLuminosityDeclineTimeWide}. Two .Ia candidates
are shown as stars \citep{Kasliwal:2010,Poznanski:2010}, and
maroon arrows
indicate lower limits for two kilonova
candidates \citep{Perley:2009,Tanvir:2013}. Grey bands show
constraints from the
F125W and F160W light curves, respectively. Each band encompass MMRD
relation for classical novae, as in
Figure~\ref{fig:PeakLuminosityDeclineTimeWide}. Circles mark the
range of possible observed peak luminosities and
time to decline
by 3 magnitudes. The width and height of these bands incorporates the uncertainty due to magnification (we adopt $10<\mu<100$) and the time of peak (using linear fits as shown in Figure~\ref{fig:LinearLightCurveFits}). Other examples of rapidly evolving transients are shown times for
comparison, with the "optical fast transients" classical novae from
the
Pan-STARRS1 survey appearing as circles in the upper right \citep{Drout:2014a}, Milky Way \citep{Downes:2000}, M31 \citep{Shafter:2011}, and
various novae in the
lower portion of local group \citep{Kasliwal:2011}. Black '+' symbols mark the
figure. Classical novae appear as cyan squares \citep{Downes:2000}, galactic recurrent novae as blue and cyan diamonds 7 rapidly declining Recurrent Novae from our own galaxy \citep{Schaefer:2010}, and the
rapid recurrence nova M31N200812a as large
cyan and orange diamonds. For all of these points the marker color indicates the band-pass of cross labeled at the
light curve used to derive bottom shows the
luminosity and decline time: blue indicates B band, cyan is V band, green is g band, and orange corresponds to r or R band.
\label{fig:PeakLuminosityDeclineTime} rapid recurrence nova
M31N 2008-12a \citep{Tang:2014,Darnley:2015}.
diff --git a/figures/peakluminosity_vs_declinetime/peakluminosity_vs_declinetime.pdf b/figures/peakluminosity_vs_declinetime/peakluminosity_vs_declinetime.pdf
index 4de4164..fe3aa99 100644
Binary files a/figures/peakluminosity_vs_declinetime/peakluminosity_vs_declinetime.pdf and b/figures/peakluminosity_vs_declinetime/peakluminosity_vs_declinetime.pdf differ
diff --git a/figures/peakluminosity_vs_declinetime/peakluminosity_vs_declinetime.png b/figures/peakluminosity_vs_declinetime/peakluminosity_vs_declinetime.png
index 5c3aec8..5f56747 100644
Binary files a/figures/peakluminosity_vs_declinetime/peakluminosity_vs_declinetime.png and b/figures/peakluminosity_vs_declinetime/peakluminosity_vs_declinetime.png differ
diff --git a/figures/peakluminosity_vs_declinetime_wide/caption.tex b/figures/peakluminosity_vs_declinetime_wide/caption.tex
index ccb4a51..df3fb5a 100644
--- a/figures/peakluminosity_vs_declinetime_wide/caption.tex
+++ b/figures/peakluminosity_vs_declinetime_wide/caption.tex
...
\label{fig:PeakLuminosityDeclineTimeWide}
Peak luminosity vs. decline time for \spock and other astrophysical
transients. Constraints for \spockone are plotted as overlapping cyan
and blue bands, corresponding to independent constraints drawn from
...
significant sample size: the ``.Ia'' class of white dwarf He shell
detonations \citep{Bildsten:2007,Shen:2010} and the kilonova class
from neutron star
mergers
\citep{Kulkarni:2005,Tanvir:2013,Kasen:2015}.
\label{fig:PeakLuminosityDeclineTimeWide} \citep{Li:1998,Kulkarni:2005,Kasen:2015}.
diff --git a/header.tex b/header.tex
index aba470e..db8d2e5 100644
--- a/header.tex
+++ b/header.tex
...
\def\Rv{\mbox{$R_V$}\xspace}
\def\Ha{\mbox{H$\alpha$}\xspace}
\newcommand\ionline[2]{#1{\scshape{#2}}}
\newcommand{\isotope}[2]{${}^{#1}$#2}
% Supernovae :
\def\CCSN{CC\,SN\xspace}
...
\def\dmfifteen{\ensuremath{\Delta\mbox{m}_{15}}\xspace}
\def\deltamfifteen{\ensuremath{\Delta\mbox{m}_{15}}\xspace}
% Other explosions:
\def\etacar{\ensuremath{\eta\,\mbox{Car}\xspace}
\def\etaCar{\ensuremath{\eta\,\mbox{Car}\xspace}
\def\m31n{M31N\,2008-12a\xspace}
\def\M31N{M31N\,2008-12a\xspace}
% Missions:
\def\HST{{\it HST}\xspace}
\def\Hubble{{\it Hubble}\xspace}
