text:
\section{Discovery of an Extreme Microlensing Event (EME)
\label{sec:intro}}

By several measures OGLE-2007-BLG-224 was the most
extreme microlensing event (EME) ever observed, having a substantially
higher magnification, shorter-duration peak, and faster angular speed
across the sky than any previous well-observed event.
These extreme features suggest an extreme lens.
Fortunately, the observations themselves had extreme characteristics,
and these permit one to test the nature of the lens.

OGLE-2007-BLG-224 (RA=18:05:41, Dec=$-28$:45:36)
was announced as a probable microlensing event
by the OGLE collaboration \citep{ews} on 9 May 2007 and independently by
the MOA collaboration \citep{bond02} on 12 May
as MOA-2007-BLG-163.  At discovery, it was
already recognized to be quite short, Einstein timescale $t_{\rm E}  \sim 7\,$days,
and was consistent with peaking at high magnification, although
with very low probability of doing so.  Such high-mag
events (typically defined as $A_{\rm max}>100$)
are extremely sensitive to planets, and hence planet-detection
groups attempt to predict these rare
events so as to intensively monitor them over their peak. This
is notoriously difficult, especially for short events,
because so little information is available before peak.  Indeed,
four of the five high-mag events that have to date yielded planet detections
had much longer-than-average Einstein timescales, $t_{\rm E}>40\,$days
\citep{ob05071,ob05169,ob06109,mb07192,mb07400}.
Nevertheless, 20 hours before peak, OGLE issued an alert calling this
a ``possible high-magnification event'', and 10 hours later,
by combining OGLE and MOA data, including points from MOA
just 12 hours before peak, the $\mu$FUN collaboration
was able to predict $A_{\rm max}>50$
and on this basis issued a general alert advocating intensive
observations.

As a result, on the night of the peak,
the $\mu$FUN Bronberg 0.35m telescope (South Africa) obtained 754
unfiltered images over 6.5 hours ending at UT 03:43 just 10 minutes
before peak, during which the magnified flux increased by a
factor 38.  The $\mu$FUN SMARTS 1.3 m telescope (Chile) obtained
a total of 304 images (52 in $I$ band, 8 in $V$, and 244 in $H$)
over 5.5 hours beginning 38 minutes before peak; and the OGLE 1.3m Warsaw
telescope obtained 62 images (57 in $I$ and 5 in $V$)
over 6.9 hours beginning 25 minutes before peak. The RoboNet 2m Liverpool
Telescope obtained 8 $R$ images whose number and timing were determined
by an automated program \citep{snodgrass08,tsapras09}
that queries several photometry databases and
attempts to optimize observations.  Critically, two of these observations
were about 35 minutes before peak and two others were 25 minutes after peak.

Additional observations were obtained by the MOA 1.8m telescope (New Zealand),
the $\mu$FUN 0.4m Auckland, 0.35m Farm Cove, and 0.4m Vintage Lane
telescopes (New Zealand), the $\mu$FUN 1.0m Mt.\ Lemon telescope (Arizona),
the PLANET 1.0m Canopus (Tasmania), 0.6m (Perth), 1.5m Boyden (South Africa)
and 1.54m Danish (Chile) telescopes, as well as the RoboNet Faulkes North 2m
(Hawaii), and Faulkes South 2m (New South Wales) telescopes.  These
observations helped in the determinations of the event's overall
parameters, but
not in the characterization of the peak, which is the central focus
of this {\it Letter}.

\section{EME Permits Measurement of Two Higher-Order Parameters
\label{sec:higher-order}}

Normally, microlensing events yield only one physical characteristic parameter,
the Einstein timescale $t_{\rm E}$, which is a degenerate combination of
three physical parameters of the system, i.e., the lens mass $M$, the
lens-source relative proper motion in the Earth frame,
${\bdv{\mu}}_{\rm geo}$, and the lens-source relative parallax $\pi_{\rm rel}=\au/D_l - \au/D_s$,
\begin{equation}
t_{\rm E} = {\theta_{\rm E}\over \mu_{\rm geo}}; \quad \theta_{\rm E} = {\pi_{\rm rel}\over \pi_{\rm E}};
\quad \pi_{\rm E}^2 = {\pi_{\rm rel}\over\kappa M},
\label{eqn:thetae}
\end{equation}
where $D_l$ and $D_s$ are the lens and source distances and
$\kappa = 4 G /(c^2\au) \sim 8.1\,{\rm mas}\,M_\odot^{-1}$.   Here,
$\pi_{\rm E}=\au/\tilde r_{\rm E}$ is the
``microlens parallax'', the ratio of the radius of the Earth's orbit
to the Einstein radius projected on the observer plane, $\tilde r_{\rm E}$.
See Figure 1 of \citealt{gould00} for a geometric derivation of the
relations between $(\pi_{\rm E},\theta_{\rm E})$ and $(M,\pi_{\rm rel})$.

Hence, if the lens is unseen, its mass and distance can be determined
only by measuring both $\theta_{\rm E}$ and $\pi_{\rm E}$ \citep{gould92}.
It is quite rare that
either of these parameters can be measured, and only three times (out of
$>4000$ events) have both been well-measured without seeing the lens itself
\citep{an02,jaros05,kubas05}.
However, as pointed out more
than a decade ago, EMEs present a unique
opportunity to measure both parameters \citep{gould97}.

\subsection{Angular Einstein Radius, $\theta_{\rm E}$, From Finite-Source Effects
\label{sec:thetae}}

First, during an EME peak, the lens is very likely to transit the
source, giving rise to distinctive ``finite-source'' effects that
yield $\rho = \theta_*/\theta_{\rm E}$, the ratio of the source radius to
the Einstein radius.  At high magnification, $A=1/u$, where $u$ is the
source-lens separation in units of $\theta_{\rm E}$.  Since typically
$\theta_{\rm E}\sim 0.5\,{\rm mas}$ and $\theta_*\sim 0.5\,{\mu\rm as}$, such effects
are expected for $A_{\rm max}\ga 1000$.  In the present case, we find that
the lens transited the source with an impact parameter of $\sim
\theta_*/3$, which permits a very accurate determination of
$\rho=8.50\pm 0.16\times 10^{-4}$.
We evaluate the source radius $\theta_*$ by extending the method
of \citep{ob03262}, to three bands, $VIH$ \citep{ob06109b}.
  We obtain calibrated
$VI$ data from OGLE-II, and calibrated $H$ data by aligning
SMARTS $H$-band to 2MASS \citep{2mass}.  We measure the
position of the clump and the source in 3 bands
$(V,I,H)_{\rm cl} = (17.32,15.28,13.33)\pm(0.1,0.1,0.1)$,
$(V,I,H)_{\rm s} = (20.58,18.91,17.50)\pm(0.02,0.02,0.02)$,
We adopt
$(M_V,M_I,M_H)=(0.79,-0.25,-1.41)\pm(0.08,0.05,0.04)$ based on
\citet{alves02} adjusted for the $\alpha$-enhanced environment
of the bulge \citep{salaris02}.  We perform a Monte Carlo Markov
Chain (MCMC) optimization of a model with 4 parameters: (1)
a \citet{cardelli89}
extinction law characterized by $R_V$, (2) the mean visual extinction
toward the clump $A_{V,\rm cl}$, (3) the mean distance to the clump, $R_0'$,
and (4) the extinction difference between the source and the clump
$\delta A_V$.  We assume (based on experience with high-resolution
spectra of bulge dwarfs) that $\delta A_V = 0 \pm 0.1$, and we demand
that the resulting $(V-I)_{0,\rm s}$ be consistent with that
predicted by \citet{bb88} from $(V-H)_{0,\rm s}$, with an error of 0.03 mag.
We then use the \citet{kervella04} $(V-H)$ color/surface-brightness
relation to derive $\theta_*=0.77\pm 0.03\,{\mu\rm as}$, where the error
also accounts for uncertainty in the model of the source flux
(which affects all three bands in tandem).  As a check, we note
that this procedure yields $R_{VI} \equiv A_V/E(V-I) = 2.01 \pm 0.10$,
a typical value for the bulge, and $R_0'= 7.8\pm 0.5\,$kpc, which is also
consistent with most estimates (keeping in mind that at
$\ell = 2.37^\circ$, the bar is about 200 pc closer than the Galactic
center).

This result implies $\theta_{\rm E} = \theta_*/\rho =
0.91\pm 0.04\,{\rm mas}$.  Combining this with the measured Einstein
timescale, $t_{\rm E}=6.91\pm 0.13\,$days, yields a proper motion in the
Earth frame \citep{an02,gould04a} of $\mu_{\rm geo} = \theta_{\rm E}/t_{\rm E} =
48\pm 2\,{\rm mas\,yr^{-1}}$.

\subsection{Projected Einstein Radius From Terrestrial Parallax, ${\bdv{\pi}}_{\rm E}$
\label{sec:pie}}

Second, and more dramatically, EMEs are subject to ``terrestrial parallax''
effects \citep{hardy95,holz96}.
If a microlensing event is observed from two different locations,
the source-lens relative trajectory will appear different: there will be
a different impact parameter $u_0$ and a different time of closest
approach $t_0$.  Since the projected Einstein radius $\tilde r_{\rm E}=\au/\pi_{\rm E}$
is typically of order AU, the second observer should typically be in solar
orbit to notice a significant effect, and indeed one such space-based
measurement has been made \citep{dong07}.
However, the main way that microlens parallax
has been measured in the past is to take advantage of the moving platform
of the Earth, but usually the event must last a large fraction of
a year for this to work \citep{poindexter05}.
For EMEs, the relevant spatial scale and
timescales are reduced by a factor $A_{\rm max}$.  For example, if the
projected velocity of the lens is $100\,{\rm km}\,{\rm s}^{-1}$ in the westward direction, then
$t_0$ will be about 80 seconds later in Chile than South Africa.
Measuring the peak time of a normal microlensing event (which typically
lasts $t_{\rm E}\sim 30\,$days) to this precision is virtually impossible.  But
since the peaking timescale of this event is roughly the source crossing time,
$t_*\equiv \rho\,t_{\rm E}=8.5\,$minutes, such measurements become quite
practical.  Indeed
the event passed both South Africa and the Canaries about 1 minute
earlier than Chile, with both time differences accurate to a few seconds.
See Figure \ref{fig:lc}.
In practice, we simultaneously account for the difference in impact
parameters and peak times at all locations \citep{an02}, as well as the Earth's
orbital motion (which turns out be negligible), to measure both the
microlens parallax $\pi_{\rm E} = 1.97 \pm 0.13$ and the direction of
lens-source relative motion, $52 \pm 5^\circ$
south of west.  See Figure \ref{fig:earth}.  The parallax measurement
can also be expressed in terms of the offsets,
${\bf \Delta t} \equiv (\Delta t_0,t_{\rm E}\Delta u_0)$, from which it is
ultimately derived:
$$
{\bf \Delta t}_{12}=(-18.1,54.0)s\pm (5.8,2.5)s
$$
$$
{\bf \Delta t}_{23}=(-43.1,-52.0)s\pm (2.6,7.0)s
$$
\begin{equation}
{\bf \Delta t}_{31}=(61.2,-2.0)s\pm (4.3,5.2)s,
\label{eqn:deltat}
\end{equation}
where 1 = South Africa, 2 = Canaries, 3 = Chile.

\subsection{Mass, Distance, and Transverse Velocity
\label{sec:mdpv}}

The determinations of $\pi_{\rm E}$ and $\theta_{\rm E}$ yield the mass and relative parallax
\begin{equation}
M = {\theta_{\rm E}\over \kappa\pi_{\rm E}} = 0.056\pm 0.004\,M_\odot
\quad \pi_{\rm rel} = \theta_{\rm E}\pi_{\rm E} = 1.78\pm 0.13\,{\rm mas}
\end{equation}
Assuming (as is consistent with its color and flux) that the source is
in the Galactic bulge $(\pi_s = 125\,{\mu\rm as})$, the lens parallax and distance
are $\pi_l = \pi_{\rm rel} + \pi_s = 1.90\,{\rm mas}$,
$D_l = \au/\pi_s = 525\pm 40\,{\rm pc}$.

The projected velocity of the lens in the Earth frame
is $\tilde v_{\rm geo} = \mu_{\rm geo}(\au/\pi_{\rm rel})= 127\,{\rm km}\,{\rm s}^{-1}$.  To find the
projected velocity in the frame of the Sun, we must remove the
motion of the Earth around the Sun ($23\,{\rm km}\,{\rm s}^{-1}$, almost due east).
We then find $\tilde v_{\rm hel}= 112\,{\rm km}\,{\rm s}^{-1}$ at $61^\circ$ south of west.
This means that the lens is moving against the direction of
Galactic rotation, just $1^\circ$ out of the Galactic plane
(toward Galactic south).  Taking account of the motion of the Sun relative
to the local standard of rest \citep{dehnen98} as well as the small
mean motion (and its uncertainty) of the source, we find that
the lens is moving at $\tilde v_{\rm hel}= 113\pm 21\,{\rm km}\,{\rm s}^{-1}$ relative to the
Galactic disk at its location, almost directly counter to Galactic rotation.
This motion is quite consistent with the kinematics of the Galactic
thick disk, which has an asymmetric drift of $43\,{\rm km}\,{\rm s}^{-1}$ and a dispersion
of $49\,{\rm km}\,{\rm s}^{-1}$ in the direction of Galactic rotation \citep{casertano90}.
(It is also consistent with Galactic halo stars, but
with a probability more than 100 times smaller.)\ \
Moreover, since the inferred mass is below the threshold for
burning hydrogen, the lens is almost certainly a brown dwarf.  While
nearby brown dwarfs of this mass have been detected
(e.g., \citealt{burgasser06,faherty09}), these are mostly
quite young and so still retain the heat generated during their collapse
from a cloud of gas.  The thick disk is of order 11 Gyrs old, and
hence brown dwarfs have had substantial time to cool.  Only those
very near the hydrogen burning limit are easy to see,
and then only if they are relatively nearby.

\section{Discussion
\label{sec:discuss}}

{\it Hubble Space Telescope (HST)} data were taken in $V$, $I$, $J$,
and $H$ bands $\Delta t_1 =29$ days
after peak when the source was magnified by a factor $A=1.005$, and again
almost exactly one year later, $\Delta t_2=1.08\,$ years.  At the
first epoch, the source and lens were virtually coincident, being
separated by only $\mu_{\rm geo} \Delta t_1\sim 4\,{\rm mas}$, i.e., $<0.1$
pixels, while at the second epoch they were separated by
$\mu_{\rm hel} \Delta t_2
\sim 47\,{\rm mas}\sim 1$ pixel, where $\mu_{\rm hel} =43\,{\rm mas\,yr^{-1}}$ is
the heliocentric proper motion.  These observations confirm that
the excess flux (above the source flux predicted from the microlensing
fit) is consistent with zero, but unfortunately not with very high
precision because an unrelated star lying 150 mas from the source
degrades the measurements.
 We discuss the prospect for future observations of the lens flux below.

We now ask, given a standard Galactic model \citep{han03,gould00}, how
likely it is that detailed information on a $t_{\rm E}=7\,$day (but otherwise
unconstrained) microlensing event toward this line of sight
$(l=2.37,\ b=-3.71)$ would turn out to imply a foreground ($D_l<4\,{\rm kpc}$)
thick-disk star rather than a star in the Galactic bulge?  The chance
is just 1/235.
Hence, either we were extremely lucky to have found this object,
or brown dwarfs are more common in the thick disk than our standard
model for the mass function would predict.  Specifically, our model
assumes a relatively flat power law mass function
for low-mass stars and brown dwarfs with $dN/d\log\,M \propto M^{-0.3}$ from
$M=0.7M_\odot$ down to $M=0.03\,M_\odot$.  This model is consistent
with results from observations of nearby thin disk brown dwarfs
\citep{pinfield06,metchev08}, and thus our detection would
imply that brown dwarfs must be an order of magnitude more
common in the thick disk than in the thin disk, in order that
the a priori probability of detecting this event be $\ga 10\%$.  This
possibility
should be considered seriously, since the prevalence of old brown
dwarfs is essentially unconstrained by any data, owing to their faintness.

In this light, we note that two other sets of investigators have concluded that
they must have been ``lucky'' unless old-population brown-dwarfs are more
common than generally assumed.  First, \citet{burgasser03} discovered a halo
brown dwarf, probably within 20 pc of the Sun, a volume that contains
only about 7 halo stars over the entire mass range from the hydrogen-burning
limit to a solar mass \citep{gould03}.
Yet the survey in which this object was discovered
would only be sensitive to halo brown dwarfs in an extremely narrow mass
range just below this limit \citep{burgasser04}.
Second, \citet{gaudi08}
analyzed a microlensing event of a nearby (1 kpc), bright ($V=11$) source
serendipitously discovered by an amateur astronomer hunting for comets,
finding that it was most likely a low-mass star or brown dwarf
moving at roughly $100\,{\rm km}\,{\rm s}^{-1}$.  Based on the low rate of such events
(and the non-systematic character of the search), they concluded that
they were ``probably lucky ... but perhaps not unreasonably so''
to have found this event.
See also \citet{fukui07}.
Finally, \citet{faherty09} found
14 high-velocity objects in a sample of 332 M, L, and T dwarfs,
which are consistent with thick-disk or halo kinematics.
Only one of these has $J-K<0$, which would be indicative of an old,
low-mass brown dwarf \citep{burrows01}, and with $v_{\rm tan}= 140\,{\rm km}\,{\rm s}^{-1}$
is most likely a halo brown dwarf, but could be in the high-velocity
tail of the
thick-disk.  At absolute magnitude $M_J=15.9$, it must be very close
to the hydrogen-burning limit $M>0.07\,M_\odot$ if it is as old as
the thick disk and halo: $\ga 11\,$Gyrs.  As this object was found
within 10 pc, it is yet another ``lucky find''
(compare to, e.g., \citealt{burgasser04}).
While the evidence from each of these studies is marginal,
collectively they point to the need for closer investigation of the
frequency of old brown dwarfs.

Brown dwarfs
are very blue in $H-K$ and somewhat red in $J-H$, so $H$ is the most
favorable band to observe them.
In the heliocentric frame, the lens is moving away from the source
at $\mu_{\rm hel}=43\,{\rm mas\,yr^{-1}}$.
Hence, just 3 years after the event, the lens should be well removed from the
source in Keck telescope $H$-band images (given its $40\,{\rm mas}$ adaptive-optics
point spread function). Equivalent angular resolution with {\it HST} would
require waiting four times longer, although it would profit from
the much fainter sky as seen from space as well as its better-defined
point-spread function.  From \citet{burrows01} (Figs.\ 1,8,9,24) and
\citet{burrows97} (Fig.\ 23) one finds that
the absolute magnitude of an 11 Gyr old,
$M=0.056\,M_\odot$ brown dwarf is $M_H=17.0$, implying $H=25.7$ at
525 pc (assuming extinction $A_H=0.1$).  By comparison, the source
is $H_{\rm s} = 17.5$.  In principle, the lens could be
younger, in which case it would be brighter and so easier to detect.
However, such high-velocity young stars are extremely rare, and
there is no known mechanism for preferentially accelerating brown
dwarfs to this speed.

If the lens is indeed in the thick disk, this would be
a challenging but not impossible observation, and would permit
a unique test of models of old brown dwarfs by comparison with
an object of known mass and well-constrained age.  The astrometry
associated with this measurement would yield  the lens-source relative proper
motion ${\bdv{\mu}}_{\rm hel}$, which would test both the
{\it magnitude} of the microlens-based proper-motion and
the {\it direction} of the microlens parallax, thereby confirming
and refining (or contradicting) the microlens-based mass estimate
\citep{gould04b}.

Looking further ahead, the space-based {\it James Webb Space Telescope}
(launch currently scheduled for 2013) will be able to take a spectrum
of this object, thereby testing more detailed atmospheric models.

\acknowledgments
We thank C.S. Kochanek, S.\ Poindexter and S.\ Kozlowski
for help with modeling the {\it HST} PSF.
We acknowledge the following support:
NSF AST-0757888 (AG,SD); NASA NNG04GL51G (DD,AG,RP);
Polish MNiSW N20303032/4275 (AU);
HST-GO-11311 (KS);
NSF AST-0206189, NASA NAF5-13042 (DPB);
Korea Science and Engineering Foundation grant 2009-008561 (CH)
Korea Research Foundation grant 2006-311-C00072 (B-GP)
Deutsche Forschungsgemeinschaft (CSB);
PPARC/STFC, EU FP6 programme ``ANGLES'' ({\L}W,NJR);
PPARC/STFC (RoboNet);
Dill Faulkes Educational Trust (Faulkes Telescope North);
Grants JSPS18253002 and JSPS20340052 (MOA);
Marsden Fund of NZ(IAB, PCMY); Foundation for Research Science and
Technology of NZ.

redpajama_set_name: RedPajamaArXiv


MBBS, MD (Physician), Robert Turner Diabetes Research Training, WHO/IDF/EASD Cambridge Diabetes Training, FCD (Diabetology), Certificate Course in Evidence Based Diabetes Management (CCEBDM), Post Graduate Diploma in Diabetology (PGDD).
Dr. Jayaprakashsai practices at Apollo Sugar Clinics in Banjara Hills, Hyderabad. He is well known in the medical community for the service he has rendered for spreading awareness on diabetes. He was given an appreciation award by the Rotary Club of Hyderabad (Central) in 2009. In 2014, he received the Diabetes Awareness Initiative Award, Bangalore from USV India Ltd.
Diabetes Education and Awareness through DEAR (Diabetes Education Awareness Reach).
Robert Turner Diabetes Research Training - Oxford University. U.K.
WHO/IDF/EASD Cambridge Diabetes Training - University of Cambridge.
I am a 63-year old man with diabetes. I have been visiting Apollo Sugar Clinics for the past 4 years. I consult Dr. J. Jayaprakashsai for my diabetes. I have to say that the doctor has taken exceptional care of my condition. I take my medications on time and walk daily as per the recommendation of the doctor. In fact, I have altered my diet as per the doctor's advice. The have to specially mention the help extended by the support staff in various aspects of my diabetes treatment. After coming to Apollo Sugar, my diabetes and blood pressure are well in control and I am very healthy.


QPR travel north to face Leeds at Elland Road on Saturday.
Simon Grayson has delivered a warning to former side Leeds United on LoveSport Radio, claiming QPR striker Nahki Wells can thrive off of the Elland Road atmosphere on Saturday afternoon.
Leeds take on Steve McClaren's QPR in Yorkshire on Saturday afternoon, as the Whites look to leapfrog Norwich City and go top of the Championship table with a fourth consecutive league win.
Marcelo Bielsa's men come into the match after three straight wins over Bristol City, Reading and Sheffield United, picking up three consecutive clean sheets along the way.
Grayson, who managed Leeds for just over three years before being sacked in 2012 after 169 games in charge, reckons Burnley loanee Wells could thrive off the hostile Elland Road atmosphere and put Leeds to the sword.
"Loftus Road is one of those ground where you've got to be on your game because of the atmosphere," Grayson said. "Elland Road is exactly the same. Players can thrive off of these sorts of atmospheres.
"The likes of Nahki Wells will be looking to go and prove to people that he has the mentality to deal with the big occasions, and look to cause an upset. QPR will go there in good spirits."
Wells, 28, joined QPR in the summer on loan from Premier League side Burnley and has netted three goals in 16 games as well as laying on two assists. Since his £5million move to Burnley (Mirror), he has managed just 10 appearances.
The Daily Mail claimed in the summer of 2017 that Leeds had enquired to sign Wells after losing Chris Wood to Burnley, but a move did not materialise. Now, he will be looking to show Leeds what they were missing.


text:
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text:
Paul Nortan (Paramaribo, 12 januari 1963) is een Nederlands oud-voetballer van Surinaamse afkomst die speelde voor AZ, Feyenoord, RKC Waalwijk en Top Oss. Hij stond vijf jaar bij Feyenoord onder contract maar een zware beenbreuk zorgde ervoor dat hij na twee en een half jaar niet meer in actie kwam voor de Stadionclub. Nortan was profvoetballer tussen 1984 en 1996 en is momenteel werkzaam als spelersmakelaar.

Nederlands voetballer
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text:
Q: Dataframe analysis by sample name and date in R I have a dataframe of groundwater sample results. The table could look like this:

Well Number
Sampling Date
Compound
Result

A
2020-01-01
a
0.5

A
2020-01-01
b
0.3

A
2020-01-01
a
0.6

A
2020-07-01
c
0.1

A
2020-07-01
c
0.1

A
2020-07-01
c
0.4

B
2020-02-01
a
0.1

B
2020-08-01
c
0.1

Now, I would like to analyse the data for each well and each sampling date. Specifically, I would like to determine, whether the wells have at least 2 compounds that have been measured with a result over 0.2 on the same date.
If yes, I would like to store this information. So, in this example well A has 3 compounds with a value of over 0.2 on 2020-01-01. So the stored information should look something like:
A 2020-01-01 -> true
A 2020-07-01 -> false
B 2020-02-01 -> false
B 2020-08-01 -> false
My table has thousnds of rows and non-linear data intervals. So the time and quantity of the measurements vary for each well.
How can I go through the data and make this anaysis and store it? I tried the split function to split the set into smaller sets by date and well number. But I did not really now how to work with the output format. Also, I remember in python I think I did something similar with a loop function (for i in...). Would that also work in R? And if yes, how?
Thank you very much even just for reading through my question :)

A: You can check whether all values per group are above 0.2 per case_when. You can use the following code:
library(dplyr)
df %>%
  group_by(Sampling_date) %>%
  mutate(info = case_when(all(Result > 0.20) ~ "true", TRUE ~ "false"))

Output:
# A tibble: 8 × 5
# Groups:   Sampling_date [4]
  Well_Number Sampling_date Compound Result info
  <chr>       <chr>         <chr>     <dbl> <chr>
1 A           2020-01-01    a           0.5 true
2 A           2020-01-01    b           0.3 true
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Nuno Mendes's plans to re-open his Michelin-starred restaurant Viajante have hit the rocks after the chef failed to reach his £1.75m crowdfunding target in the allotted time.
Mendes – who runs Taberna Do Mercado in Spitalfields and is executive chef at The Chiltern Firehouse – launched a funding campaign on Seedrs in November aiming to re-open the restaurant at Metropolitan Wharf in Wapping in Autumn 2016.
Investors were to be given a 33 per cent equity stake in the business with minimum investment starting at just £10.
But the chef has now taken down the page and is reportedly seeking funding elsewhere.
The Portuguese chef closed the original Bethnal Green Viajante site in February 2014 after four years.


At Vinnies we believe that empowering people, not blaming them, is the answer to combating the poverty that affects one in eight Australians.
Vinnies members, volunteers and employees assist over 1.8 million Australians each year and works directly with people experiencing poverty and homelessness . We also advocate for the rights of marginalised groups in the community and view Anti-Poverty Week as an opportunity to spread greater awareness of marginalisation in Australia.
Anti-Poverty Week is being held from Sunday, 14 October to Saturday 20 October 2018, and focuses on poverty across the world, including Australia .
In 2014 it was recorded that 2.9 million Australians are living below the poverty line.
Almost 35% of people experiencing poverty are employed or past retirement age.
12.3% of people with a disability are experiencing poverty.
More than 730,000 children in Australia living in poverty.
Vinnies has several events taking place in communities across Australia during Anti-Poverty Week. These events range from forums in the capital cities to sausage sizzles in regional centres.
For a full list of events taking place, visit the official website and click on 'Calendar of Events 2018'.
You can help fight poverty and hardship!
Not sure how you can make a difference and help people living below the poverty line?
Visit our Find Help page if you or somebody you know needs assistance.
Visit the Low-Income Support page to learn more about our advocacy and services.
You can volunteer for Vinnies frontline services, visit Become a Volunteer .
If you don't have time to volunteer you can make a donation to ensure our volunteers have the life changing resources they need.
Read the submissions Vinnies has made to government to bring about change for people experiencing inequality and poverty.
Visit the calendar of events on the Anti-Poverty Week website to see how you can get involved.
Use any of the social media tiles below to help promote Anti-Poverty Week and help us educate more Australians as to what poverty looks like in our country. Don't forget to use #APW2018 so we can see your posts and follow us on Facebook , Twitter and LinkedIn .
Vinnies has long campaigned for an increase in Newstart and Youth Allowance payments. We are calling for these payments to be raised so that people relying on them can meet their basic needs and live with dignity.
Every day, our members and volunteers witness first-hand the poverty and hardship experienced by people on Newstart and related payments.
Our social safety net should ensure people can afford a roof over their head and food on the table when they are unable to support themselves. Yet payments like Newstart are so low that many people cannot pay for essentials.
Newstart has not increased in real terms in 24 years and has failed to keep up with the rising costs of living. It has fallen ever further below the poverty line and behind average wages.
Today, over 800,000 people are struggling to live on as little as $39 per day. People locked out of paid work, carers, parents, and students are being forced to choose between eating a meal and paying the rent, or buying shoes for their children and maintaining their health.
Using the hashtag #RaisetheRate , a diverse coalition of charities, community organisations, business groups and individuals with lived experienced of poverty are urging the Commonwealth Government to recognise its responsibility to provide adequate income support – so that Newstart and other income support payments are a true support, not a pathway to poverty.


text:
About Mary Cummins
I have known Mary Cummins for about 18 months now. We met a total of four or five times, once at Boks office planning how to best support Ed and the department, two or three times at Boks/community meetings, and once at Mary's house for a planning meeting with Ed when he failed to show because he was afraid activists would blog about his hanging around his groupies. At that time, he didn't want anyone to know where he lived, so his place was out and I lived far away from either. Her "significant other" was there on that occasion.
We talked on the phone maybe ten times—tops. We have hundreds, maybe a thousand or more emails, mostly during the period when we were supporting Boks. We have hundreds of replies to or emailed from Boks re all kinds of things, from defending him and the department, to reviewing kill stats to commenting on his posts.
She was never his lover. She has been in a committed relationship ever since I met her. In the hundreds and thousands of emails,phone calls, or meetings was there even one indication of a romantic bond between them.
Nada. When attacks on Boks seemed to be going nowhere, the anti Boks people in the animal community attacked us to force us to stop defending Ed. She defended me and provided moral support.
She is one of the most intelligent woman I have ever met, and one of the most committed to the welfare of animals. She rescued and returned to the wild 1,400 wildlife in 2005. Her work and reputation were heavily damaged when she spent so much time and energy defending Boks. Then even Boks even went after her when he (allegedly) had two LAAS field people search her house.
She tried to prevent the killing of hundreds of ground squirrels poisoned by the City of Santa Monica. If you think she was obsessed, look at my postings about County Vector Control and Santa Monica officials killing squirrels. During her birth control project of the SM squirrels, there, she used to routinely rope and lower herself over the edge of the 200 ft cliffs in Palisades Park to treat the burrows with a cholesterol ingredient known to cause temporary sterility in small mammals.
Several of you have remarked to me as to how much she helped you when you had problems with wildlife or even with your animals. She can be relentless and selfless when it comes to helping animals or her friends.
Her only fault is her exuberance in the defense of friends. She pissed off a LOT of people when they attacked Boks and she responded in kind. She will counterattack to the same degree she and her friends are attacked. She was not afraid to go toe to toe with lots of people that attacked her friends of herself.
AND, she apologized to everyone that she had been overly enthusiastic when defending Boks.
I want to remind everyone that Mary is not your enemy. We all want to get rid of Boks. She has been providing statistics and information, including the transcript of Boks before Council when they reamed him for the way he went about the Pit Bull Academy.
Will you get off it and focus on the real problems at hand, saving animal lives at LAAS by whatever means needed, including exposing several general managers as the incompetents or liars that they are? Talk to her if you will to see if you can now get together for common goals.
I've never considered Mary an "enemy" nor you Ed. And when you think about it, the two of you individually have consistently provided way more information about what's going on at the LAAS city shelters than Boks ever has From the Desk of Ed Boks
( and yeah, that's a jab )
Cypress,CA
Thanks Ed
Nice to see support for Mary. You're helping to put the community back in the animal community.
This isn't the first time that being honest and bold had caused trouble for Mary. There are so many lies floating around that have used against her. If people stick to their own knowledge and experience, not the slander of some who is paid or crazed, they will conclude that she is a woman of great courage and will.
Mary has continued to rescue animals and to support other rescuers and assist the public with the wildlife they find, even through all these attacks on her reputation. It is tragic that a few liars can spin so much trouble with no concern for the damage they do to the people and animals that look to Mary for support. Let alone the damage done to her life and reputation. It's a crime.
Thanks for standing up, maybe a few brave souls will take note and follow suit.
We shouldn't be attacking any animal people. Infighting is the reason the animal movement is not stronger than it is. The enemy is the person who is abusing and neglecting animals, not each other. I can't think of a greater waste of effort than attacking people on our own side. Keep your own on the real goal, helping animals. Don't get distracted with pettiness.
The three people attacking Cummins are as follows:
Psycho-Bitch #1, whose only claims to fame are her ongoing divorce proceedings and the Bar Association's ongoing scrutiny of her questionable practices.
Psycho-Bitch #2, the agoraphobic, self-absorbed, unemployed scribe who brags about her gang ties in her rarely published articles and who's being ostracized by publishers across the country who don't want to be associated with someone so unstable and unprofessional.
Psycho-Putz, a certified loser with a cellphone videocam who can't hold down a job and who without his meds would be just another babbling bonehead at the corner of Van Nuys and Victory, if he could find his way there.
This insane clown posse (apologies to the band) is guilty of the very things each of them accuse Cummins of doing - lying, cyber-stalking, consorting with criminals...you name it.
Why do they hate Cummins? Like you say, she's smart and she stands up to people who attack her. They don't like that she doesn't suffer their foolishness, so, like other bullies who can dish it out but can't take it, they went on the warpath.
It would be nice if we would stop attacking each other and focus on helping the animals, but the three stooges (apologies to the comic geniuses) described above hardly qualify as animal activists. If we number them amongst us they will just continue to poison the entire humane community.
Atake Resigns! Blames Boks and Blackman
Apparently the Killing has begun big time
County Kill Numbers, stonewalling and Possible fraud
Interesting emails from Ed Boks to Animal Lover--A...
Yaroslavsky's email to Mayeda asking her to Explai...
Orlov is Number Impaired, But Boks May Be Doing So...
LAAS Lowers Killing by Refusing Neonates--Ammended
ABC Pulls Story About Boks National Honors
My Sources for Shelter Statistics
LA County's Dismal Failure at Saving Animals
Mayeda Goes Ballistic; Calls Boks Out
Mayor Antonio Villaraigosa fails Los Angeles' anim...
Boks' Claim of Being #1 Adoption Agency Exposed
Mayor Repeats Boks' Lie that LA Is Both No-Kill a...
Boks' Math; Vets
Two Excellent Sites on Catfood and Nutrition and a...
Friskies Bites Dust
Re Eric Jones Sweetheart Deal by Boks
The Fine Art of Moral Corruption
July Stats--Preliminary Analysis
ERIK JONES ITEM AT COMMISSION MEETING
Boks at Maricopa County
Mary Cummins' Lawsuit Against Boks
Parolees Fired
Santee Alley Illegal Animal Sales
Boksian Figure and Animal Juggling Create Another ...
Philly Continues to Outperform LAAS
Reno No-Kill Status
After Boks, Who?
Council Chastises Boks
Boks Illegally denying Requests for Public Records
Winograd Calls Boks a Fraud


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Ashly and Jeremy's spring wedding was one of my favorites to shoot yet! They have been dating since high school, which was when I first met them, and let me tell ya, these high school sweethearts were SO excited to be finally marrying one another!! The anticipation and joy was tangible all day long. One of my favorite features of this wedding was the bridesmaids' boho look with eucalyptus bouquets, woven lilac dresses, and chic gold headbands. They totally rocked it. But I'd have to say, the highlight of the day for me was watching Ashly exude light that poured out on the whole bridal party. She made the pictures absolutely radiate. I mean, look at that glowing bride!!
So many friends and family contributed to their special day in some form or fashion, from their friend who filled in as wedding coordinator to the bridesmaid that doubled as the calligrapher. Just goes to show how fun and seriously rewarding DIY weddings can be! I can't get enough of 'em. When I finished editing their wedding, I was thrilled to see how much Jeremy and Ashly's excitement came out in the photos and how surrounded with love and support they were throughout the whole thing. Truly a celebration of love.


Take a private tour Rabat/Sale and enjoy the VIP treatment. Your own driver guide, fully qualified and accredited, will allow you to experience Rabat and Sale in the best possible way.
During your guided tour, see the official residence of the king, as well as the Hassan Tower, the Mohammed V Mausoleum and the Kasbah of the Udayas.
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• Departure from your hotel in the morning after breakfast for Rabat.
Visit to the ruins of Chellah : housed on the site of the ancient city of Sale, Chellah is the quietest place in Rabat.
Visit to the Oudayas Kasbah, in its interior you can visit an ancient military prison , gardens, a museum and the famous blue and white Oudaya's streets.
Visit to the Hassan Tower: The symbol of Rabat(a height of 44m) . At first the minaret was built to accommodate up to 40,000 people. Its architecture is a masterpiece of traditional Moroccan art.
Visit to the Mohammed V mausoleum: the royal tomb which houses the tomb of Mohammed V and his son Moulay Abdellah and Hassan II.
Visit to the Archaeological Museum of Rabat one of the most sought in Morocco and the richest in everything related to prehistoric and pre-Islamic area.
Visit to the city of Sale, at just 3 km from Rabat and discover its ancient walls of ocher color, its pretty narrow streets, the architecture of its houses and its souks.
Back to Fez in the evening.


Here's a different frame on my Royal Botanic Gardens Water Lilies. . . I think the white window looks nicer. . What do you think?
When there are boot-washing stations near the bathrooms, you know you're in for it. It was worth wrecking my hiking boots for this view.
Here's somebody working on Australia Day in our garden. . making honey.
Seagulls over Sydney Harbour looking for some of their favourite seafood. . . Hot Chips. . or could this be a WWII fighter plane dogfight. .
This is a Brown Goshawk sitting in the open on a branch within the grounds of Taronga Zoo at Mosman on the lower north shore of Sydney with Harbour Bridge and the Sydney Opera House not far behind it.
Ladies & Gentlemen, This is Miss Annique Azure, world famous chanteuse, captured yesterday Sat. 22.12.18 at the Kirribilli Markets, on Sydney's lower north shore, right next to Sydney Harbour Bridge.
TRIPLE BOWTIE An oldie for your morning feeds. Bring more fire soon my babies.
--THE RIGHT WAY TO GET READY FOR THE FEAST-- I met these guys @emjayze_hempgoods in San Antonio and they made this in honor of the event. These prerolls are perfect for relaxing and vibing with the fam. Peep the ohmie @jelly.goddess in the beginning and Me closing it out.
Sendin this body vert out for @vapinsin ..Have you tried it yet?
-GRANDMASTER JELLYFISH- Throwing it back to over a year ago when I was hunting Big Jellys. Hooked this bad boy and wont forget that day:) @vaperz_girl behind the cam.
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Live on amazon. Search for "midnight murder plan" on amazon.
A baby Kookaburra, part of the terrestrial tree kingfishers, sitting in our backyard this afternoon, he was one of three looking for some worms. Shot on my Sony A7R II with the 24-105mm F4 zoom lens @ iso 200 f4 @ 1/60 sec. .